Äîêóìåíò âçÿò èç êýøà ïîèñêîâîé ìàøèíû. Àäðåñ îðèãèíàëüíîãî äîêóìåíòà : http://www.naic.edu/~astro/misc/ast_docs/07%20APRPP.pdf Äàòà èçìåíåíèÿ: Thu Aug 23 23:54:29 2007 Äàòà èíäåêñèðîâàíèÿ: Sat Dec 22 06:52:47 2007 Êîäèðîâêà: Ïîèñêîâûå ñëîâà: arp 220

NATIONALASTRONOMY&IONOSPHERECENTER
OperatedbyCornellUniversityundercooperativeagreementwiththeNationalScienceFoundation



MANAGEMENT OPERATIONS and ASTRONOMICAL SCIENCES




2006PROGRESSREPORT 2007PROGRAMPLAN

StudentsattheUniversityofTexas,Brownsillecontrolthe Arecibotelescopefromtheirremotecontrolcenter.

March2007



NATIONALASTRONOMY&IONOSPHERECENTER
OperatedbyCornellUniversityundercooperativeagreementwiththeNationalScienceFoundation

MANAGEMENT OPERATIONS and ASTRONOMICAL SCIENCES


2006PROGRESSREPORT 2007PROGRAMPLAN





March2007

CooperativeAgreementNo.AST-0431904



Table of Contents1
Section 1 Section 2 Section 3 Section 4 Section 5 Section 6 Section 7 Section 8 Section 9 IntroductionandOverview1 AnnualProgressSummary2 2.1SummaryofAchievementsinPY20062 2.2ProblemsEncountered,SolutionsandImpact7 2.3ListofObservingPrograms,Investigators,andHours-PY20068 2.4VisitingPublicattheObservatory 3.1Cosmology27 3.2EarlyGalaxies28 3.3ActiveGalaxies28 3.4NormalGalaxiesandClusters29 3.5IntergalacticGasandTidalRemnants30 3.6MilkyWayGalaxy31 3.7Pulsars33 3.8SolarSystem33 3.9FundamentalPhysics37 4.1RadioAstronomyInstrumentation38 4.2IF/LOSystem40 4.3Backends41 4.4Computing:StorageandNetworking42 43 5.1AngelRamosVisitorCenter 43 5.22006REUProgram46 5.3ConnectingtoArecibo52 5.4ALFALFAVisitingScientists52 27

AccomplishmentsandPlansoftheNAICScientificStaff27

TechnicalAccomplishmentsandExpectations38

NAICEducationandOutreachPrograms

AreciboObservatoryPublications-PY200654 NAICExternalFederalFundingandActiveSubcontracts65 DivisionofEffortforStaff67 NAICOrganizationChartandDescription71 9.1ManagementPlan:OrganizationCharts 9.2VitaeofNewProfessionalStaff74 71

1

The contents, headings and order of topics presented here are as specified in the NAIC Coopertative Agreement.


Table of Contents continued
APPENDIX A:Committees107 Section 10 Section 11 Section 12 StatusReportandPlanforPY200775 10.1ScientificPlans75 10.2TechnicalPlans87 10.3MajorProjectPlans92 10.4OperationalChangesinResponsetotheSeniorReview RecommendationsforNAIC93 11.1MajorProgramGoalsandEmphasis95 11.2RiskFactorsAffectingProgramGoals96 11.3Management,Contractual,FinancialandTechnicalIssues97 11.4RequirementsforSupportoftheScientificCommunity99

LongRangeReportandPlan95

BudgetReport103


1. Introduction and Overview
The National Astronomy and Ionosphere Center (NAIC) radio/radar telescope located in Arecibo, Puerto Rico, is the instrument that provides more collectingarea--more"lightgatheringpower"--for centimeter-wave radio science than any competitivetelescopeintheworld.Operatedasanational research facility by Cornell University for the National Science Foundation (NSF), the Arecibo telescope in fact provides nearly three times the collecting area of all the other NSF-sponsored radio telescopes combined. The sheer physical size of theArecibotelescopemakesitauniquelypowerful research instrument. Unique also to the Arecibo Observatoryisthe programof researchsupported bythetelescopeandthediversityofinterestsofthe scientificusercommunityitserves.Operationofthe AreciboObservatorytosatisfytherequirementsof thisinterdisciplinaryusercommunityistheprimary responsibility of the scientists, engineers and staff of the NAIC. Management of NAIC as a national facilityisprovidedbyCornellUniversityunderaCooperativeAgreementwiththeNSF2. Described in this PY2007 NAIC Annual Progress Report and Program Plan (APRPP) are the major achievements of the past program year, the plans to meet the major challenges of PY2007, and an outlineofNAICprioritiesthatinformitslong-range planning. HighlightsoftheNAICachievementsinPY2006describedinthisAPRPPinclude: · Completion of the first year of observations made by two of the legacy sky surveys to be done with the Arecibo LbandFeedArray(ALFA)bycommunitybased ALFA consortia. Scientific results publishedandsubmittedforpublication fromboththePALFApulsarsurvey,and the ALFALFA survey of HI in galaxies in thelocal(z<0.1)universe,demonstrate the fruitfulness of the survey programs. They also create data products that are accessibleon-line,andusefulasresearch
2 CooperativeAgreementNo.AST-0431904betweentheNational ScienceFoundation,Arlington,VA22230andCornellUniversity, Ithaca,NY,14853,datedOctober1,2005.

tools, to the much wider astronomical community. · Routine scheduling of "commensal" observations, simultaneous observations done by two or more academic research groups with different scientific objectives,eachprocessingthesameastronomical signal with its own purposespecificspectrometer; · Completion of the engineering design phase of two new spectrometers, the EALFA spectrometer, designed to enable sensitive spectroscopy of atomic hydrogeningalaxiestoz=0.2,andthe PALFA spectrometer that will triple the analyzed bandwidth used for pulsar searches and timing. Contracts for fabrication of the two new spectrometers have been let with delivery expected in thefirstquarterofcalendaryear2007. · Completionofthecontracttocleanand paint all of the structural steel on the telescope platform to remove accumulatedcorrosionandmillscale,andtoapplyacoatingspecificallyselectedtoprotectthesteelforatleast20years. In PY2007 the emphasis at NAIC is on making the programmatic and personnel changes necessary forNAICtofunctionwellatthelowerfundinglevel recommendedbytheSeniorReview,andtodevelop new scientific partnerships with the NAIC user community for archiving survey data and making the data products accessible for data mining. The highlightsinclude: · Tailoring Observatory services to the ALFA survey consortia to the downstreamneedsofdataarchivinganddata access through involvement with the Virtual Observatory. In the cost-constrained environment at NAIC imposed by the reduced funding recommended by the Senior Review, this means that the data archiving and data access support comes at the expense of services providedtotheconsortiainthedata-takingphaseoftheirsurveywork. · Using the recommendations of the Arecibo Users and Scientific Advisory Committee (AUSAC) to develop telescope scheduling procedures that assure the survey programs receive the time an 1

NAICAPRPP2007










nually they require for their successful execution, and the traditional commonuser programs maintain full access to the telescope and to Observatory user supportservices. · Assuring that the staff reductions imposed by the Senior Review are accompaniedbyacommensuratereductionin the scope of Observatory tasks so that the burden on the Observatory support staff members remains manageable for eachindividual. Onthelongerterm,prioritieswitha5-yearorgreaterhorizoninclude(a)organizationofacademicresearchers to specify the scientific and technical requirementsforacomprehensivesearchforsources oftransientcosmicradioemission;(b)organization of academic researchers to specify the scientific andtechnicalrequirementsforanincoherentscatter ionospheric radar facility to be located at the Arecibo magnetic conjugate point in Argentina; and (c) refinement of the U.S. participatory role in theinternationalSquareKilometerArrayproject. As a NSF National Center, the NAIC shares in the NSF mission: To promote the progress of science; to advance the national health, prosperity, and welfare; to secure the national defense; and for otherpurposes3.Overtheyearsthephrase"other purposes" has been defined by Congressional actiontoinclude(1)fosteringtheinterchangeofscientificandengineeringinformationnationallyand internationally; (2) supporting the development of computer and other methodologies; and (3) addressingissuesofequalopportunityinscienceand engineering.TheNAICPY2007ProgramPlanfully embracesallthesegoalswiththesuiteofprograms andcommunitysupportoutlinedinthisAPRPP.

NAIC Arecibo Observatory. There were more users of the NAIC facilities at the Arecibo Observatory, more prospective users proposing to use the facilities,morestudentsinvolvedwiththeresearch at NAIC, and more publications from research at NAICthanatanytimeinthepast.

Science Achievement Highlights. NAIC supports a multidisciplinary science program with research facilities for passive radio astronomy, active radio astronomy done using radar transmitters at 430MHzand2300MHztoilluminatesolarsystem objects, and upper atmospheric research. In the astronomy program, recent science highlights include:
· Best limits ever achieved on dipolar gravitational wave emission. Pulsar J1738+0333 is a 5.85-ms object in a binarysystemwithanorbitalperiodof8.5 hours; the companion object is a white dwarf. High precision timing of the pulsar orbital dynamics reveals that the orbit is decaying due to dipolar gravitational wave emission at a rate of 4.4 x 10-14s/s,avaluethatisexactlyconsistent with that expected from General Relativity. This is the most precise measurement ever made of the effect of dipolar gravitationalwaveemission. · Frequency structure has been observed in pulses from the Crab Nebula pulsar that is unresolved with a sampling rate of 0.4 nanoseconds; the corresponding physicalsizeoftheemissionregionmust be less than 13 cm, about the size of a grapefruit. This is, by far, the smallest astronomical object, a plasma cloud or plasma interaction region, ever detected beyond the solar system. During its short lifetime, the blasts of radio emission from the region have a luminosity that exceeds 10 percent of the total luminosityofthesun. · OHemissionwasobservedinthecomet 9P/Tempel1fortwomonthspriortothe NASA Deep Impact penetration of the comet nucleus, and for several weeks followingtheimpact.OHisasecondary product arising from the photodissociation of water. The OH production rate after Deep Impact was immeasurably different from the OH production rate prior to impact suggesting that the OH
NAICAPRPP2007

2. Annual Progress Summary
2.1 Summary of Achievements in PY2006
PY2006 was an exceptionally productive year for NAIC in all areas. By any objective measure, the NAICProgramYears2005and2006werethemost successful in the more than 40-year history of the
3

NationalScienceFoundationActof1950,PublicLaw810507.

2














·

·

·

·

emission is being quenched in the intems formed, the properties they share nercomaowingtotheincreasedabunandthedynamicsoftheirmotion. danceofwaterproducedintheimpact. · Using the highest resolution radar imThe supernova rate in the prototypical ages ever made of the moon, planetary ultraluminous infrared galaxy Arp 220 astronomers found no evidence for ice has been measured by means of VLBI in the craters at the lunar south pole. observationsofthenucleus.AcompariThere had been speculation that reserson of VLBI observations made on two voirsofwaterexistedintheformofperepoch separated by a year revealed the manent ice sheets in shadowed lunar presence of 4 new radio supernovae in craters at the pole. The radar images the later epoch that were not present made at Arecibo disprove this conjecin the earlier epoch. The implied star ture, a result that is important for those formation rate that follows from the planning extended human exploratory observed supernova rate is sufficient to missionsonthemoon. poweralltheinfraredemissionfromArp 220.ByincludingtheArecibotelescope Programmatic Achievements in Support of in the VLBI array, the VLBI observations Scientific Research. The number of scientific were the most sensitive ever made, a proposals scheduled on the Arecibo telescope sensitivity ~5 microJy/beam that was since the major Gregorian upgrade of the telecrucialtothedetectionofthenewradio scope was completed in 1999 is shown in Figure supernovae. 2.1.1.Thisplotincludesscheduledproposalsinall Discovery of the second relativistic bithree components of the NAIC scientific program at the Arecibo Observatory, astronomy, planetary nary pulsar, J1903+03, a system that is an ideal "laboratory" for precision tests radarandspaceandatmosphericsciences(SAS). ofGeneralRelativityandforinclusionin the pulsar timing array search for graviThegrowthinthenumberofproposalsscheduled tational waves originating in the big onthetelescopeannuallyderivesfromtwofactors. First, it reflects a deliberate management decision bang; Discovery of a "dark galaxy" near NGC to emphasize the research of new investigators, student investigators, investigators at small institu1156, a galaxy having the mass in neutral atomic hydrogen equivalenttothemass NAIC Scheduled Proposals by Year of the Milky Way, but 250 no apparent starlight. Radio Astronomy The newly discovered Planetary Radar galaxy is approxiSAS 200 Total mately 50 Mpc from theEarthandappears to be about 75 kpc in diameter. The rota150 tional kinematics are consistent with those expectedforagalaxy. 100 Researchers using the AreciboObservatory's powerful radar have 50 made the most detailed observations ever of a binary nearEarth asteroid--two 0 1998 1999 2000 2001 2002 2003 2004 2005 2006 clusters of rubble cirProgram Year cling each other--ofFigure 2.1.1. The of proposals scheduled on the Arecibo fering new clues a function of year. numberarescientificseparatelyfor the three components telescope as Figures shown of the NAIC about how such sys- scientificprogramattheAreciboObservatory.

Scheduled Observing Proposals

NAICAPRPP2007















3


NAIC Users by Year
350 NAIC Staff Cornell Other Users Total

300

250

200

150

100

50

0 1998 1999 2000 2001 2002 Program Year 2003 2004 2005 2006

Figure 2.1.2. The number of users of the NAIC Arecibo telescope in the period since completionoftheGregorianupgrade.

telescope annually and the numberofinstitutionsthese scientists represent has grownconsistentlysincethe completion of the Gregorianupgradeofthetelescope in1999.Thetelescopeuser statistics are shown in Figure 2.1.2. Each person is counted individually and only once in a year, even in thosecaseswhereaperson observesmultipletimesduring the year and/or participates on several scheduled observingproposals.Injust the three year period since 2002 the annual number of users increased by 71% (from193to331).

Number of Users

tionsandinvestigatorsproposingresearchthatcan onlybedonewiththeArecibotelescope(e.g.HIin low surface brightness dwarf galaxies or timing of faintpulsars).InanerawhentheALFAsurveyprograms are of high scientific importance and community agreed priority, the role of the individual investigator,curiosity-drivenresearchmustbeprotected.Second,aconsciouseffortismadetopack thetelescopescheduletightlysothatasmanyproposalsaspossiblewillhaveaccesstothetelescope. Often this involves careful consultation between the 90 proposers and the Observatory telescope scheduler to 80 compromiseonthetimelimitstobeallocatedtoparticu70 lar programs. The fact that the number of proposals 60 being scheduled has been increasing, when the total 50 telescope time for science 40 observations is nearly constant, is one objective mea30 sureofthecooperativespirit that exists between the Ob20 servatoryanditscommunity of users. Clearly, that spirit 10 of goodwill is improving to thebenefitofall. 0
Number of Students 1998 1999

At all the NSF national centersthereisanunmistakable trend for the number of scientists/students on observingproposalstoincrease.Thesametrendcan be easily seen in astronomical publications where theaveragenumberofauthorsperpaperhasbeen increasing steadily for two decades. This growth certainly results from many factors among them being the greater specialization of contemporary astrophysics owing to the expansion in the number and sophistication of research tools, including
NAIC Student Users by Year
Students

2000

2001

2002 Program Year

2003

2004

2005

2006

The number of scientists Figure 2.1.3. The number of graduate and undergraduate students conducting thesis using the NAIC Arecibo researchobservationsontheArecibotelescope.
4 NAICAPRPP2007


software and computational tools. Additionally, there is an unmistakable preference for many researchers to prefer to work in supportive teams ratherthantoworkindependently.Itisimportant that scientific journals, national research centers and funding agencies adapt their processes and procedurestochangessuchastheseastheyoccur. Hence,keepingtrackoftheuserstatisticsatNAICis vitaltothefuturesuccessoftheinstitution. NAIC provides encouragement by means of travel costreimbursementforgraduateandundergraduate students to become actively involved in their thesis research programs on the Arecibo telescope. At NAIC, students are encouraged to get their (trained) hands on the equipment, to make modifications to the observing procedures, and to experiment with novel observing techniques and dataprocessingalgorithms.Largelyforthisreason, there is an active and growing group of students who make use of Arecibo observations as a component of their thesis research. Figure 2.1.3 summarizes the number of graduate students whose observations were scheduled on the Arecibo telescope. Again, for each year an individual graduate student was counted only once, even in those cases where the student observed multiple times oronmultiplescheduledprograms.

sions.AsdescribedelsewhereintheAPRPP,NAIC initiates programs focused on student education involving use of the Arecibo telescope, and it providesinstitutionalsupportforprogramsdeveloped andimplementedbyfacultyadvisorsattheirhome colleges and universities. Often such NAIC institutionalsupportconsistsofassuringthatstudentprogramsarescheduledonthetelescopeatthehours thatareappropriateforclassroomactivities;inother cases NAIC makes its best efforts to assure that travel support, meeting facilities, data transport or softwaresystemsaremadeavailabletostudentresearchers. The success of the NAIC initiatives can beseenquantitativelyinthegrowthofstudentinvolvementwithNAIC(Fig.2.1.3). Thenumberofinstitutionsfromwhichtheusersof theArecibotelescopecomeasafunctionofyearis showninFigure2.1.4.Herethenumbersareseparated between institutions located in the U.S., and foreign institutions. In this plot a particular institution is counted only once a year, even in those caseswhereseveraltelescopeuserscomefromthe sameinstitutioninthatyear.

Programmatic Achievements in Support of Educational Programs in Puerto Rico. For many years, NAIC has exploited the fact that the Arecibo Observatory provides an inspirational setGrowthinthenumberofstudentusersalsoresults, tingforeducationalinitiativesofmanykinds.One of the most successful of these initiatives is the in part, from deliberate NAIC management deciAngel Ramos Foundation NAIC User Institutions by Year Teacher workshops, a num160 ber of one-day workshops areofferedfrequentlyduring US Institutions 140 Foreign Institutions the year. These are coordiTotal Institutions natedthroughlocaluniversities with the Puerto Rico De120 partmentofEducation.Participants at these workshops 100 include pre-service teachers, graduate students in educa80 tion and undergraduates who apply for the program 60 and are selected competitively. NAIC staff members 40 present an overview program of studies that empha20 sizes the scientific goals and methodologyoftheastronomy and aeronomy program 0 1998 1999 2000 2001 2002 2003 2004 2005 2006 at the Arecibo Observatory; Program Year age appropriate materials Figure 2.1.4. Thenumberofinstitutionsrepresentedannuallybyscheduledusersofthe are given to the teachers so NAICArecibotelescope.
5

NAICAPRPP2007

Number of Institutions


that they may communicate the information to theirstudents. ThesuccessoftheNAICteachereducationalworkshopsattheAreciboObservatoryhasledtoanincrease in the private funding we have received to support the workshops, which in turn has led to a further expansion of the program. Figure 2.1.5 illustratesthegrowthinthenumberofteachersin Puerto Rico served by this important NAIC educationalandoutreachprogram.

writtenformanyofthenon-exemptObservatorystaff; ·Improving communication materials to ensure that employees all have the same information regarding their benefits,especiallythehealthcareplan.Fully bilingual information is now being producedanddistributed; ·Implementation of the Cornell standard policy for filling staff vacancies, including internal postings followed by externalcompetition; ·Employee Performance Evaluation. All employees are now presented annually with a writtenevaluationandaperformance dialogue is conducted. The evaluations are linked to the employees' annual performance salary/wage increase. Thisisthesecondyearofformal performance management at NAIC.Manyroughspotsinthe processweresmoothedasaresultoftheexperiencelastyear.

Streamlining the personnel recruitment process has been a particular management objective over the past year. The goal is to eliminate the barriers that have led some reFigure 2.1.5. NumberofteachersinPuertoRicoattendingNAICscienceeducacentrecruitmentstobeunnecessartionworkshopsattheAreciboObservatoryshownasafunctionofyear. ily protracted. Briefly, the process Management Achievements in PY2006. In by which an open position is filled is coordinated PY2006 significant progress was again made toby the HR manager. She works with the involved ward assuring that management practices at the supervisor to update the job description, post the ObservatoryarefullycompliantwithCornellprocejob so that all interested have the opportunity to duresandprocess.Progressintheseareasbenefits apply for it, conduct the search, interview the apdirectly NAIC personnel, not visiting users, but it is plicants, and select the best qualified candidate. no less critical to the success of NAIC. Substantial This process assures transparency and equal opsteps were taken to assure that NAIC employees portunity. Each supervisor, individually, will learn sharefullyinCornellprogramsthatprovideopporthe steps through mentored experience in one of tunitiesforgreatereducational,health,andprofestheir actual recruitments. Delays in some recent sional advancement. Progress made in PY2006 in hiresarethepricewearepayingforeducatingour the area of improved employee benefits includes supervisorsintheprocess. thefollowing: ·Development of comprehensive posiProviding employee benefits, knowledge of those tion descriptions and classifications. All benefits,andprocessesbywhichaccesstothebenObservatorynon-academicpositionsare efitsareknowntoall,andappliedequitablytoall,is beingre-writtenandre-classifiedintothe a continuing task. Further meaningful progress is Cornell standard classification structure. expectedinallthesepersonnelmanagementareas InPY2006NAICcontinuedtoworkwith inPY2007. a private consultant to accelerate the process of getting position descriptions
6 NAICAPRPP2007


2.2 Problems Encountered, Solutions and Impact
Operationally, the biggest challenge to NAIC is the lack of budget stability. Figure 2.2.1 shows the change in NSF funding of NAIC, actual and projected, over a ten-year period relative to the fiducial year 1999. Shown on this plot is the actual funds received by NAIC (yellow), the actual funds received by the NSF division of astronomical sciences (red) and the effect of inflation year-by-year relativeto1999takenas3%peryear. InPY2007thepurchasingpoweroftheNSFfunds receivedbyNAIChaddecreasedbyapproximately 25% relative to 1999. With NSF as a whole in a dramatically expansive phase, the declining NAIC budgetisclearlytheresultofdecisionsbeingmade annually at NSF/AST that favor other activities at the expense of on-going NAIC operations. It is a seriousproblemforNAICthatNSF/ASThasnotexpressed with clarity the metric being used to determine NAIC annual funding at a time when the Observatory user-base has doubled in three years, theresearchopportunitieshaveneverbeengreaterandthescientificoutputisatanalltimehigh.

The report of the NSF/AST Senior Review has had severe consequences for NAIC staff morale. The NAIC staff members, press reporters doing stories ontheSeniorReview,governmentofficialsandthe U.S.communityofastronomersallfocusontheexpressionoftheSeniorReviewthattheAreciboObservatory should be closed in 2011. It is certainly true that the report expresses `closure' as a last resortoptiontobeusedonlyintheeventthat~$5M of annual operations funding cannot be found from sponsors other than NSF/AST. But the news oftheSeniorReviewreportistherecommendation that the Arecibo Observatory should be closed. It is for this reason that all stories in the print and broadcast media that discussed the Senior Review focusedonthisasTHEstory.Everyonewhoworks at NAIC and the Arecibo Observatory were stung bythisrecommendation.Particularlysobecauseit isreadilyapparenttotheNAICstaffthattheanalysispresentedinthereportleadingtotheSeniorReviewrecommendationtoclosetheAreciboObservatory has clear flaws. Namely, the ALFA surveys will require a decade or longer to be completed oncethefollowuptimeisincluded,notthe3years the SR used as the basis for their analysis; and no accountwastakenbytheSeniorReviewthattheir recommendations would terminate the Arecibo

Funding History Relative to FY1999
140.00 AST (%) NAIC (%) inflation (%)

120.00

Cumulative Percent Change from FY1999

100.00

80.00

60.00

40.00

20.00

0.00 2000 -20.00 2001 2002 2003 2004 2005 2006 2007 2008 2009 2010

-40.00 Fiscal year

Figure 2.2.1. Budget history of NAIC and AST, actual and projected, expressed as a percentage change fromFY1999.TheNAICbudgetisshowninyellow,ASTinredandinflationinblue(takenas3%peryear).

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7


Planetaryradar,auniquescientificprogramthatis theonlytechnologycapableofdeterminingtheorbitsofnear-Earthasteroidswithsufficientprecision toassesstheirpotentialthreattoimpacttheEarth. The investment of many hundreds of millions of dollars being made by NSF, DoD, DoE and several U.S.universitiesinIntegral,PanStarsandLSSTwith theobjectiveoflocatingnear-Earthasteroidsiscertainly called into question if the Arecibo planetary radarsystemwerenotavailabletodotheprecision orbitdetermination. ThereducedNSF/ASTbudgetforNAICthatfollows fromtheinitialSeniorReviewrecommendationthat

NAIC funding be reduced by 25% over the next 3 years has led to a staff reduction of approximately 30 positions at NAIC and a consequent reduction in the scope of activities supported by NAIC. An adjustment of such a large magnitude is a significantmanagementchallenge.NAICwillworkwith its user community to make the required changes inawaythatpreservesthescientificstrengthofthe Observatoryandcontinuesitsrecentgrowthpath butwithoutundulyinconveniencingtheusercommunity. Inevitably, this will require NAIC to have the flexibility to experiment and make corrections aswelearnbyexperience.

2.3 List of Observing Programs, Investigators and Hours - Program Year 2006
Experiment by Group RadioAstronomy SolarSystemStudies Space&AtmosphericSci. CommissioningTask Maintenance Unsched.Maintenance Total Total Hours Used 4301.00 488.75 1441.50 919.00 1462.00 147.75 8760.00
% of Total Used

49.10 5.58 16.45 10.49 16.69 1.69 100.00

RADIO ASTRONOMY











Graduatestudentsareunderlined Undergraduatestudentsareitalicized

NAIC staff members are bolded

SpectroscopicandContinuumObservations
Hours Observers
Lewis, B.M. (NAIC) Linz,H.(UPRRioPiedras) Hofner,P.(NewMexicoTech) Stecklum,B.(TLSTautenburg) Araya,E.(NewMexicoTech) Bacmann,A.(AIUJena) Lewis, B.M. (NAIC) Lewis, B.M. (NAIC) Ghosh, T. (NAIC) Salter, C. (NAIC) O'Neil, K. (NAIC) Kanekar,N.(Kapteyn) Chengalur,J.(NCRA-TIFR) Ghosh, T. (NAIC)

Project # Title
A1312 A1582 LightTravel-TimeDimensionsfor|b|>10deg OH/IRStars FromDarknesstoLight-StarFormationinInfrared DarkClouds

4.75 2.50 70.25 56.50 2.00 3.00 8

A1587 A1589 A1653 A1724

TheOHLight-CurveofIRAS22402+1045 OntheImminent"Death"oftheOH/IRStar 15060+0947 A-21cmSearchforLow-zDampedLy- SystemsTowardsCompactRadioSources HIandOHinDampedLyman-Systems









NAICAPRPP2007


Hours Observers
2.00 LebrÑn, M. (NAIC) Pantoja,C.(UPRRioPiedras)

Project # Title
A1767 A1785 A1852 A1908 A1965 A1969 HIandH2COObservationsofIVCswithStrong ContinuumBackgroundSources ASearchforHigh-zWaterVaporMasersin ObscuredAGNs ToContinuetheMonitoringofOHMasersin HighGalacticLatitudeOH/IRStars

3.75 Ghosh, T. (NAIC) Mathur,S.(OhioStateUniv.) Salter, C. (NAIC) 219.75 Lewis, B.M. (NAIC) 1.00 23.50 68.00 7.25 Momjian, E.(NAIC) Ghosh, T.(NAIC) Salter, C. (NAIC) Muller,E.M.(ANTF) Pandian,J.D.(Cornell) Goldsmith,P.F.(JPL) Deshpande,A.(RamanRes.)



HI21cmandOH18cmSpectralLineObservations ofthe2JyIRAS-NVSSSample AbsorptionbytheTidalHIFilamentsAssociatedwith NGC4631 TracingHigh-MassStarFormationintheGalaxy

Giovanelli,R.(Cornell) A2010 Haynes,M.(Cornell) Boselli,A.(MarseillesObs.) Brosch,N.(WiseObs.) Catinella, B.(NAIC) Charmandaris,V.(U.Crete) Darling,J.(Univ.Colorado) Davies,J.(CardiffUniv.) GarciaLambas,D.(U.Cordoba) Gavazzi,G.(U.StudidiMilano) Hoffman,L.(LafayetteCollege) Hunt,L.(ArcetriObs.) Iovino,A.(U.Milano-Brera) Karachentsev,I.(SpecialAstrophysical Observatory,Russia) Karachentsev,V.(Univ.Kiev) Kent,B.(Cornell) Koopmann,R.(UnionCollege) Marinoni,C.(U.Milano-Brera) Masters,K.(CfA) Minchin,R.(CardiffUniv.) Momjian, E.(NAIC) Muller,E.(ATNF) Pantoja,C.(UPRRioPiedras) Putman,M.(U.Michigan) Rosenberg,J.(U.Colorado) Salzer,J.(WesleyanUniv.) Saintonge,A.(Cornell) Scodeggio,M.(MilanoCNR) Skillman,E.(U.Minnesota) Solanes,J.(U.Barcelona) Spekkens,K.(RutgersUniv.) Springob,C.(NRL)

ALFALFA:TheAreciboLegacyFastALFASurvey

NAICAPRPP2007









9


Hours Observers
Stierwalt,S.(Cornell) Valotto,C.(U.Cordoba) vanDriel,W.(Obs.Paris) vanZee,L.(IndianaUniv.) (seelistabove) Davies,J.I.(CardiffUniv.) (seelistabove) Putman,M.(U.Michigan) Stanimirovic,S.(UCBerkeley) Heiles,C.(UCBerkeley) Goldston,J.E.(UCBerkeley) Arce,H.(Caltech) Bania,T.(BostonUniv.) Briggs,F.(AustraliaNat'lUniv.) Koo,B-C.(SeoulNat'lUniv.) Korpela,E.(UCBerkeley) Lockman,F.J.(NRAO) vanLoon,J.(KeeleUniv.) Goldston,J.E.(UCBerkeley) Heiles,C.(UCBerkeley)

Project # Title

49.25 1042.25 3.75 1.00 0.75 128.75 76.00

A2010 and A2048 A2010 and A2059

ALFALFA:TheAreciboLegacyFastALFASurvey TheAreciboGalaxyEnvironmentsSurvey(AGES) ALFALFA:TheAreciboLegacyFastALFASurvey MappingtheHIGalaxyandHalowithTOGS(Turn onGALFASurvey)

A2011 BipolarFlowsinthe21cmSky HIContentandDynamicsofLowLuminosity Galaxies

Blanton,M.R.(NewYorkUniv.) A2046 West,A.(U.Washington) Geha,M.(CarnegieObs.) Pizagno,J.(OhioStateUniv.) Weinberg,D.(OhioStateUniv.) Dalcanton,J.(U.Washington) Garcia-Appadoo,D.(CardiffUniv.) Davies,J.I.(CardiffUniv.) Davies,J.I.(CardiffUniv.) Putman,M.(U.Michigan) Stanimirovic,S.(UCBerkeley) Heiles,C.(UCBerkeley) Goldston,J.E.(UCBerkeley) Arce,H.(Caltech) Bania,T.(BostonUniv.) Briggs,F.(AustraliaNat'lUniv.) Koo,B-C.(SeoulNat'lUniv.) Korpela,E.(UCBerkeley) Lockman,F.J.(NRAO) vanLoon,J.(KeeleUniv.) Ghosh, T. (NAIC) Salter, C.(NAIC) Momjian, E.(NAIC) A2048 A2048 and A2059

TheAreciboGalaxyEnvironmentsSurvey(AGES) TheAreciboGalaxyEnvironmentsSurvey(AGES) MappingtheHIGalaxyandHalowithTOGS(Turn onGALFASurvey)

A2049

TheFateofCoolingFlowGas:AnAreciboHI21-cm AbsorptionSurvey

10



















NAICAPRPP2007


Hours Observers
35.00 30.25

Project # Title
TurbulenceandFeedbackintheDiffuseISM

Goldston,J.E.(UCBerkeley) A2050 Lazarian,A.(U.Wisconsin) Esquivel-Salazar,A.(U.Wisconsin) Heiles,C.(UCBerkeley) Heiles,C.(UCBerkeley) Stanimirovic,S.(UCBerkeley) Kanekar,N.(NRAOSocorro) A2052

TheThinnestColdHICloudsintheDiffuseISM

10.25 Henning,P.(U.NewMexico) Koo,B-C.,(SeoulNat'lUniv.) Bania,T.(BostonUniv.) Heiles,C.(UCBerkeley) Stanimirovic,S.(UCBerkeley) Kang,J.(SeoulNat'lUniv.) Lee,J-J.(SeoulNat'lUniv.) 33.25 Korpela,E.(UCBerkeley) Basketweave Koo,B-C.(SeoulNat'lUniv.) Heiles,C.(UCBerkeley) Goldston,J.E.(UCBerkeley) Stanimirovic,S.(UCBerkeley) Henning,P.A.(U.NewMexico) 34.00 69.75 105.00 Lubowich,D.(HofstraUniv.) Turner,B.(NRAO(C'Ville) Robert,H.(U.Manchester) Millar,T.(U.Manchester) Pasachoff,J.(WilliamCollege) Putman,M.(U.Michigan) Stanimirovic,S.(UCBerkeley) Heiles,C.(UCBerkeley) Goldston,J.E.(UCBerkeley) Arce,H.(Caltech) Bania,T.(BostonUniv.) Briggs,F.(AustraliaNat'lUniv.) Koo,B-C.(SeoulNat'lUniv.) Korpela,E.(UCBerkeley) Lockman,F.J.(NRAO) vanLoon,J.(KeeleUniv.)

A2053 and A2055

ALFAHISurveyoftheGalacticPlaneat1=38to45 deg:GalaxiesintheZoneofAvoidance ALFAHISurveyoftheGalacticPlaneat1=38to45 deg:FaintHI21-cmEmissionLineWingsat ForbiddenVelocities

A2056 and A2051 A2057

AnALFAProposal:TestingtheModified Technique(ACommensalProposalwiththeZOA Group)

ALFAHISurveyoftheGalacticPlaneat1=192deg: GalaxiesintheZoneofAvoidance,Testingthe ModifiedBasketweaveTechnique DIintheMostDeuteratedKnownMolecularCloud: AKeytoUnderstandingDeuteriumAstrochemistry

A2059

MappingtheHIGalaxyandHalowithTOGS(Turn onGALFASurvey)

Putman,M.(U.Michigan) A2060 Stanimirovic,S.(UCBerkeley) Lockman,F.J.(NRAO) Kerton,C.(IowaState) Esquivel-Salazar,A.(U.Wisconsin) Lazarian,A.(U.Wisconsin)

AGALFAStudyoftheDisk-HaloInterface

NAICAPRPP2007









11


Hours Observers
Goldston,J.E.(UCBerkeley) Muller,E.(ATNF) Gibson,B.(Swinburne) McClure-Griffiths,N.(ATNF)

Project # Title

50.25 77.00 17.75 84.50 66.00 22.25 8.75 1.50 45.50 12

Stanimirovic,S.(UCBerkeley) A2063 Weisberg,J.M.(CarletonCollege) Robishaw,T.(UCBerkeley) Heiles,C.(UCBerkeley) Quataert,E.(UCBerkeley) A2119

TheFifthSessionofPulsarHIAbsorptionMeasurementsofTiny-ScaleAtomicStructureintheInterstellarMedium OHMegamasersinULIRGs:TheMega-ObviousPlace toLookforZeemanSplitting! HiddenMolecularGasintheExtremeOuterDiskof M33?

Chomiuk,L.B.(U.Wisconsin) A2120 Strader,J.(UCO/LickObservatory) Allen,R.(STScI) Smith,G.(UCO/LickObservatory) Ho,L.C.(CarnegieObs.) Darling,J.(Univ.Colorado) Kanekar,N.(NRAO) Ghosh, T.(NAIC) Chengalur,J.N.(NCRA-TIFR) Kronberg,P.P.(LosAlamos) Salter, C.J.(NAIC) Kothes,R.(DRAO) Ensslin,T.(MPIfAGarching) Perillat, P.(NAIC) Brown, R.L. (NAIC) A2121 A2123

HIEmissioninAGNHosts:ANewStrategytoTest theBlackHole-HostGalaxyParadigm DotheFundamentalConstantsChangewithTime?

A2125

ImagingDiffuseIntergalactic430MHzEmissionin an8degx8degZoneofthePerseus-PiscesSupercluster

A2127

SearchforMolecularOxygeninthez=6.28QSO SDSSJ1030+0524 ALFALFA:TheAreciboLegacyFastALFASurvey. The2005SummerUndergraduateObserving Program

Stilp,A.(Univ.Wisconsin) A2140 Patel,N.(Cornell) Altaf,A.(LafayetteCollege) Ayala,J.(UPR) Forsyth,C.(Colgate&BrynMawr) Gillin,M.(UnionCollege) Goldstein,J.(LafayetteCollege) Mahmood,B.(UnionCollege) Mullan,B.(ColgateUniv.) Read,J.(UnionCollege) Walsh,B.(ColgateUniv.) Wortel,S.(ColgateUniv.)
Douglas,K.A.(UCBerkeley) Goldston,J.A.(UCBerkeley) Kregenow,J.M.(UCBerkeley) Heiles,C.E.(UCBerkeley) Edelstein,J.(UCBerkeley) Korpela,E.J.(UCBerkeley) Nishikida,K.(UCBerkeley) Magnani,L.(Univ.Georgia) A2143

TheMOlecularStateofGalacticTranslucentClouds: OHScientificJustification









NAICAPRPP2007


Hours Observers
13.00 5.00 14.75 38.50 54.00 20.75 46.75 17.75 20.50 25.50 11.50 32.50 Osten,R.A.(Univ.Maryland) Araya,E.(NewMexicoTech) Hofner,P.(NewMexicoTech) Olmi,L.(UPRSanJuan) Kurtz,S.(UNAM) Bieging,J.H.(StewardObs.) Goldston,J.(UCBerkeley) Heiles,C.(UCBerkeley) Buyle,P.(GhentUniv.) Pisano,D.(NRL) DeRijcke,S.(GhentUniv.) Michielsen,D.(GhentUniv.) Dejonghe,H.(GhentUniv.) Freeman,K.(Aust.Nat'lUniv.) Magnani,L.(Univ.Georgia) Wennerstrom,E.(U.Georgia) Douglas,K.A.(UCBerkeley) Onello,J.(SUNYCortland) Rosenberg,J.L.(CfA) Salzer,J.J.(WesleyanUniv.) Ashby,M.L.N.(CfA) Heiles,C.(UCBerkeley) Goldston,J.(UCBerkeley) Knee,L.B.(NRCofCanada) DiFrancesco,J.(NRC) Gibson, S.J.(NAIC) Goldston,J.(UCBerkeley) Heiles,C.(UCBerkeley) Li,D.(JPL) Krco,M.(Cornell)

Project # Title
A2145 A2146 WidebandDynamicSpectroscopyofCoherentRadio BurstsonActiveMDwarfs AnAreciboStudyoftheVariabilityoftheNew H2COMaserinIRAS18566+0408

A2147 A2149

HI21cmMappingoftheGemOB1Star-Forming Region HIDetectioninE+AGalaxies

A2154

OHObservationsofTwoTranslucentCloudEdges

A2156

AnHIStudyofStar-FormingDwarfGalaxies

A2172 A2174

MappingHIinaSpectacularShell AnHISurveyofthePerseusMolecularCloud Complex

Howell, E.(NAIC) A2185 Lovell,A.J.(AgnesScottCollege) Schloerb,F.P.(U.MassAmherst) Heiles,C.(UCBerkeley) Goldston,J.(UCBerkeley) Krco,M.(Cornell) Goldsmith,P.F.(JPL) Jones,T.J.(Univ.Minnesota) McQuinn,K.B.(Univ.Minnesota) Lewis,B.(NAIC) A2187 A2193 A2195

OHObservationsof73P/Schwassmann-Wachmann 3inSpringof2006 MappingHIinaSpectacularTrueFilament Completionofa2004ProjecttoObservetheTaurus MolecularCloudComplexwithGALFA ASearchforOH/IRStarsinM33

NAICAPRPP2007



















13


Hours Observers
22.75 23.75 13.50 28.50 17.75 14 Ho,L.C.(CarnegieObs.) Darling,J.(U.Colorado) Greene,J.E.(Harvard) Magnani,L.(Univ.Georgia) Lugo,S.K.(U.Georgia) Brand,J.(IRA-INAF) Wouterloot,J.(U.Hawaii) Terzian,Y.(Cornell) Chengalur,J.N.(NCRA-TIFR) B. Lewis(NAIC)

Project # Title
A2196 A2198 HIEmissionProfilesinAGNHosts:ANewStrategyto toTesttheBlackHole-HoseGalaxyParadigm TheDistributionofH2COintheFarOuterGalaxy

A2200

HIContentofDistantGalaxyClusters

Giovanelli,R.(Cornell) A2215 Kent,B.(Cornell) Haynes,M.(Cornell) Boselli,A.(MarseillesObs.) Brosch,N.(WiseObs.) Catinella, B. (NAIC) Charmandaris,V.(U.Crete) Darling,J.(Univ.Colorado) Davies,J.(CardiffUniv.) GarciaLambas,D.(U.Cordoba) Gavazzi,G.(U.StudidiMilano) Hoffman,L.(LafayetteCollege) Hunt,L.(ArcetriObs.) Iovino,A.(U.Milano-Brera) Karachentsev,I.(SpecialAstrophysical Observatory,Russia) Karachentsev,V.(Univ.Kiev) Koopmann,R.(UnionCollege) Marinoni,C.(U.Milano-Brera) Masters,K.(CfA) Minchin, R.(NAIC) Momjian, E.(NAIC) Muller,E.(ATNF) Pantoja,C.(UPRRioPiedras) Putman,M.(U.Michigan) Rosenberg,J.(U.Colorado) Salzer,J.(Wesleyan,Univ.) Saintonge,A.(Cornell) Scodeggio,M.(MilanoCNR) Skillman,E.(U.Minnesota) Solanes,J.(U.Barcelona) Spekkens,K.(RutgersUniv.) Springob,C.(NRL) Stierwalt,S.(Cornell) Valotto,C.(U.Cordoba) vanDriel,W.(Obs.Paris) VanZee,L.(IndianaUniv.) Dedes,L.(Univ.Bonn) Kalberla,P.(Univ.Bonn) Stanimirovic,S.(UCBerkeley) A2221

ALFALFAFollow-up:EnigmaticVirgoClouds

HIHaloCloudsintheOutskirtsoftheMilkyWay









NAICAPRPP2007


Hours Observers
32.75 5.00 3.75 4.50 Goldston,J.E.(UCBerkeley) Heiles,C.(UCBerkeley) Putman,M.(U.Michigan) Stanimirovic,S.(UCBerkeley) Hofner,P.(NewMexicoTech) Araya,E.(NewMexicoTech) Darling,J.(Univ.Colorado) Robishaw,T.(UCBerkeley) Heiles,C.(UCBerkeley)

Project # Title
A2222 TheAnti-CenterWaterfall

A2224 Urgent A2230 A2258 Urgent

RadioLineObservationsTowardStarForming RegionsAnUndergraduateEducationalProject UsingtheArecibo305mTelescope OHMasersinExtrasolarPlanetaryAtmospheres UrgentUpdateforA2119-OHMegamasersin ULIRGs:TheMega-ObviousPlacetoLookfor ZeemanSplitting!

2909.75(TotalHours-SpectroscopicandContinuum)

PulsarAstronomy
7.25 3.00 17.75 116.50 7.25 5.00 49.00 Freire, P.(NAIC) Freire, P.(NAIC) Anderson,S.B.(Caltech) Freire, P.(NAIC) Jacoby,B.(NRL) P1567 P1681 P1684 HighPrecisionTimingofPulsarsinGlobluar Clusters TimingMillisecondPulsars.II.ThePSR J2016+1947BinarySystem TimingMillisecondPulsars.I.ThePSR J1738+0335BinarySystem

Freire, P. (NAIC) P1693 Cordes,J.(Cornell) Lorimer,D.R.(WestVirginiaU.) McLaughlin,M.(WestVirginiaU.) Kramer,M.(U.Manchester) Lyne,A.G.(U.Manchester) Bhat,R.N.D.(SwinburneUniv.) Gupta,Y.(NCRA/TIFR) Hankins,T.H.(NewMexicoTech) P1830 Kern,J.S.(NewMexicoTech) Popov,M.V.(AstroSpaceCtr) Soglasnov,V.A.(AstroSpaceCtr) Kondratiev,V.I.(AstroSpaceCtr) Hankins,T.(NewMexicoTech) Eilek,J.A.(NewMexicoTech) Crossley,J.(NewMexicoTech) Sheckard,J.(NewMexicoTech) Nice,D.J.(BrynMawrCollege) Backer,D.C.(UCBerkeley) Demorest,P.(UCBerkeley) P1976

PilotObservationsforaDrift-ScanPulsar Searchat327MHz

IntrinsicShapeofGiantPulsesfromthe MillisecondPulsarB1937+21



HighTimeResolutionMeasurementsofPulsar Microstructure

P2016

PrecisionMillisecondPulsarTiming

NAICAPRPP2007













15


Hours Observers
Ramachandran,R.(UCBerkeley) Stairs,I.(U.BritishColumbia) Ferdman,R.(U.BritishColumbia) Lommen,A.(Franklin&Marshall) Stairs,I.(U.BritishColumbia) Thorsett,S.(UCSantaCruz)

Project # Title

12.25 8.75 17.75 396.50 16

P2017

Long-TermTimingofPSRB1534+12 High-PrecisionTimingofParkesMultibeam MillisecondPulsars:VelocitiesandEvolution

Stairs,I.(U.BritishColumbia) P2019 Ferdman,R.(U.BritishColumbia) Faulkner,A.(U.Manchester) Lyne,A.G.(U.Manchester) Kramer,M.(U.Manchester) McLaughlin,M.(U.Manchester) Lorimer,D.(U.Manchester) Manchester,R.(ATNF-CSIRO) Hobbs,G.(ATNF-CSIRO) Camilo,F.(ColumbiaUniv.) D'Amico,N.(Oss.Ast.Cagliari) Possenti,A.(Oss.Ast.Cagliari) Burgay,M.(Oss.Ast.Cagliari) Nice,D.J.(BrynMawrCollege) Backer,D.C.(UCBerkeley) Ramachandran,R.(UCBerkeley) Demorest,P.(UCBerkeley) Stinebring,D.R.(OberlinCollege) P2020 Cordes,J.M.(Cornell) P2030 Camilo,F.(ColumbiaUniv.) Nice,D.J.(BrynMawrCollege) Ramachandran,R.(UCBerkeley) Freire, P.C.(NAIC) Thorsett,S.(UCSantaCruz) Kaspi,V.(McGillUniv.) Backer,D.C.(UCBerkeley) Arzoumanian,Z.(NASA/GSFC) Chatterjee,S.(CfA) Kramer,M.(U.Manchester) McLaughlin,M.(WestVirginiaU.) Xiluri,K.(StewardObs.) Gaensler,B.(CfA) Stairs,I.(U.BritishColumbia) Weisberg,J.(CarletonCollege) Lazio,J.(NRL) Han,J-L.(Nat'lAst.Obs.China) Lommen,A.(Franklin&Marshall) Lorimer,D.(WestVirginiaU.) Crawford,F.(HaverfordCollege) Stappers,B.(StichtingAstron) Deshpande, A.(RamanRes.) Bhat,R.(SwinburneUniv.) Ransom,S.(NRAO)

FurtherScintillationArcMonitoringofthePulsar B0834+06 AnALFAPulsarSurveyoftheGalacticPlane





NAICAPRPP2007


Hours Observers


Project # Title

Vlemmings,W.(U.Manchester) Hessels,J.(McGillUniv.) Giguere,C-A.(McGillUniv.) Deneva,J.(Cornell) Champion,D.(U.Manchester) Reid,B.(Princeton) vanLeeuwen,J.(U.BritishColumbia) Kasian,L.(U.BritishColumbia) Arzoumanian,A.(NASA/GSFC) Nice,D.J.(BrynMawrCollege) P2066 CharacterizingOrbitalTorquesandtheOriginof X-rayEmissionintheBlackWidowPulsar EstimationofPulseArrivalTimesforPSRB1937+21 UsingInterstellarHolography

14.50 9.00 12.00 6.25 15.25 34.00 1.25 11.50 39.75 49.75

Backer,D.C.(UCBerkeley) P2067 Ramachandran,R.(UCBerkeley) Demorest,P.(UCBerkeley) Walker,M.A.(KapteynInstitute) Jenet,F.(Univ.Texas) Johnston,S.(ATNF) Cordes,J.M.(Cornell) Champion,D.(U.Manchester) P2068 Lorimer,D.(WestVirginiaU.) McLaughlin,M.(WestVirginiaU.) Lorimer,D.(WestVirginiaU.) P2072 McLaughlin,M.(WestVirginiaU.) McLaughlin,M.(WestVirginiaU.) P2074 Lorimer,D.(WestVirginiaU.) Champion,D.(U.Manchester) Cordes,J.M.(Cornell) Arzoumanian,A.(NASA/GSFC) Xilouris,K.(StewardObs.) Stairs,I.(U.BritishColumbia) Stinebring,D.(OberlinCollege) Lorimer,D.(WestVirginiaU.) Cordes,J.M.(Cornell) P-ALFAConsortium P2076 P2099 Urgent

High-PrecisionTimingofTwoRecycledPulsars

OneMoreOrbit:Long-TermTimingofPSRJ0407+ 1607 PSRJ1453+19-AnotherPulsarPlanetarySystem?

ScintillationArcObservationsofPSRB1737+13 RapidObservationsoftheRelativisticBinaryPulsar J1906+07 InvestigatingNewTransientRadioSources

McLaughlin,M.(WestVirginiaU.) P2109 Lorimer,D.(WestVirginiaU.) Lyne,A.G.(U.Manchester) O'Brien,J.(U.Manchester) Rankin,J.M.(U.Vermont) Wright,G.A.E.(SussexUniv.) Srostlik,Z.(U.Vermont) Wolszczan,A.(PennState) P2110 P2111

PolarimetricPulse-SequenceObservationsofBright UnstudiedAreciboPulsars TimingObservationsofthePlanetsPulsar,PSR B1257+12

NAICAPRPP2007



















17


Hours Observers
8.75 30.00 13.50 30.00 18.25 7.50 7.50 99.00 37.50 70.50 9.50 13.00 18 Donovan,J.(ColumbiaUniv.) Camilo,F.(ColumbiaUniv.)

Project # Title
P2112 DeepSearchesforYoungPulsarsin"Shell" Supernova AnL-band(ALFA)SearchforGiantPulsesfromM33

Bhat,R.(SwinburneUniv.) P2113 Cordes,J.M.(Cornell) Deneva,J.(Cornell) Lazio,J.(NRL) McLaughlin,M.(WestVirginiaU.) Hankins,T.(NewMexicoTech) Nowakowski,L.(UPRMayaguez) P2115 Rankin,J.M.(Univ.Vermont) Bhat,R.(SwinburneUniv.) Sotero,N.(UPRArecibo) vanLeeuwen,J.(U.British P2116 Columbia) Stairs,I.(U.BritishColumbia) Ferdman,R.(U.BritishColumbia) Ramachandran,R.(UCBerkeley) Backer,D.(UCBerkeley) Demorest,P.(UCBerkeley) Nice,D.(BrynMawrCollege) Hankins,T.(NewMexicoTech) P2160 Sheckard,J.L.(NewMexicoTech) Hankins,T.(NewMexicoTech) P2161 Sheckard,J.L.(NewMexicoTech) Arzoumanian,Z.(NASA-GSFC) Cordes,J.(Cornell) Deneva,J.(Cornell) Freire, P.C.(NAIC) Stairs,I.H.(U.BritishColumbia) Nice,D.J.(BrynMawrCollege) Cordes,J.(Cornell) Nice,D.J.(BrynMawrCollege) Stairs,I.H.(U.BritishColumbia) Stairs,I.H.(U.BritishColumbia) Thorsett,S.E.(UCSantaCruz) Stairs,I.H.(U.BritishColumbia) Lorimer,D.(WestVirginiaU.) Arzoumanian,Z.(NASA-GSFC) Backer,D.(UCBerkeley) Bhat,R.(SwinburneUniv.) Camilo,F.(ColumbiaUniv.) Champion,D.(CfA) Chatterjee,S.(CfA) P2175

PossibleRadius-to-IntensityMappingandMode

ExposingDriftingSubpulsesfromtheSlowesttothe FastestPulsars

Ultra-HighTimeResolutionMeasurementsofthe Crab"Giant"RadioPulsars GiantPulsesfromJ1752+2359 APulsarSearchtoSolvea50Year-OldMystery

P2176 P2177 P2178 P2179 P2180

TimingthePSRJ1741+1354BinarySystem ExploringPulsarsDiscoveredbyPAL PrecisionMillisecondPulsarTiming Long-TermTimingofPSRB1534+12 TimingtheFirstRelativisticBinaryfromtheArecibo

NAICAPRPP2007


Hours Observers


Project # Title

Cordes,J.(Cornell) Crawford,F.(Franklin&Marshall) Deneva,J.(Cornell) Deshpande,A.(RamanRes.) Freire, P.C.(NAIC) Gaensler,B.(Harvard) Han,J.L.(Nat'lAst.Obs.ofChina) Hessels,J.(McGillUniv.) Kasian,L.(U.BritishColumbia) Kaspi,V.(McGillUniv.) Kramer,M.(U.Manchester) Lazio,J.(NRL) vanLeeuwen,J.(U.BritishColumbia) Lommen,A.(Franklin&Marshall) McLaughlin,M.(WestVirginiaU.) Nice,D.(BrynMawrCollege) Ransom,S.(NRAO) Stappers,B.(Astron.Inst.) Vlemmings,W.(U.Manchester) Weisberg,J.(CarletonCollege) Stinebring,D.(OberlinCollege) Stappers,B.(U.Amsterdam) P2189 50MHzScintillationObservationsofSeveralNearby Pulsars SearchforGiantPulsesinThreeHighEdotPulsars PolarimetricPulse-SequenceObservationsofBright UnstudiedAreciboPulsars High-PrecisionTimingofBinaryandMillisecond Pulsars

13.25 6.50 16.25 7.25 3.50

Ilardo,M.A.(N.CarolinaSchool P2201 ofScience&Math)
Rankin,J.M.(U.Vermont) Wright,G.A.E.(SussexUniv.) P2202

Stairs,I.H.(U.BritishColumbia) P2203 Ferdman,R.(U.BritishColumbia) Lyne,A.G.(U.Manchester) Faulkner,A.(U.Manchester) Kramer,M.(U.Manchester) McLaughlin,M.(WestVirginiaU.) Lorimer,D.(WestVirginiaU.) Manchester,R.(ATNF-CSIRO) Hobbs,G.(ATNF-CSIRO) Camilo,F.(ColumbiaUniv.) D'Amico,N.(Oss.Ast.Cagliari) Possenti,A.(Oss.Ast.Cagliari) Burgay,M.(Oss.Ast.Cagliari) Nice,D.(BrynMawrCollege) Backer,D.(UCBerkeley) Demorest,P.(UCBerkeley) vanLeeuwen,J.(U.British Columbia) Jonker,P.(CfA&SRON) Bildsten,L.(UCSantaBarbara) Ransom,S.(NRAOC'ville) Nelemans,G.(RadboudU.) Stairs,I.(U.BritishColumbia) P2204

SoftX-rayTransient1H1906+000:TheClosest CounterparttotheMillisecondRadioPulsars

NAICAPRPP2007













19


Hours Observers
9.50 51.00 10.50 McLaughlin,M.(W.VirginiaU.) Cordes,J.M.(Cornell) Lorimer,D.(WestVirginiaU.) Weisberg,J.(CarletonCollege) Nice,D.J.(BrynMawrCollege)

Project # Title
P2205 MonitoringandTimingofRRATSources

P2206

StudiesofRelativisticGravitationandPulsarPhysics withtheFirstBinaryPulsarB1913+16 TwoMassiveNeutronStars

Nice,D.J.(BrynMawrCollege) P2239 Stairs,I.H.(U.BritishColumbia) Backer,D.(UCBerkeley) Demorest,P.(UCBerkeley) Ferdman,R.(U.BritishColumbia) vanLeeuwen,J.(U.BritishColumbia)

1297.00(totalhours­PulsarAstronomy)

SpecialProjects
7.00
Salter, C.(NAIC) S1662 Ghosh, T. (NAIC) LebrÑn, M. (NAIC) Brooks,H.(ReedCollege) Buckley,S.(TrinityCollege) ColÑn,K..(CollegeofNewJersey) Graf,K.(Cornell) Hanson,H.(Univ.Wyoming) Mielke,C.(Univ.Arizona,Tucson) Ojalvo,I.(RensselaerPolytechnic) Rucker,D.(Univ.Arkansas) Bowen,D.(Cornell) Fernandez,M.X.(Dartmouth) Taylor,B.(Univ.Texas,Austin) Cabassa-Miranda,E.(UPRMayaguez) Gonzalez-Perez,I.(UPRMayaguez) Rivera,M.(UPRMayaguez) SummerStudentsHands-onProject TheDetectionofFormaldehydeinaMolecularCloud SeenatHalfthePresentAgeoftheUniverse

7.00(TotalHours­SpecialProjects)

20



















NAICAPRPP2007


Hours Observers

Project # Title

VLBI
2.75 2.75 4.50 4.50 3.75 6.25 1.75 4.00 3.75 6.00 1.25 1.25 6.75 7.50 15.75 5.75 5.25 1.25 1.50 1.00 Barvainis,R.(NSF) Ulvestad,J.(NRAO) Boyce,E.(MIT) Bietenholz,M.(YorkUniv.) Forbrich,J.(MPIfR,Bonn) Hough,D.H.(TrinityUniv.) Knudsen,K.(MPIfA,Heidelberg) More,A.(MPIfR,Bonn) BB191 BB217 BB219 BF089 BH139 BK127 BM241 6cmHAS CentralImageinGrav.LensB2319+051 2ndepochofobs.OfSN2001eminUGC11794: VLBA/MkIV4pol. TwoTaurusProtostars ImagingoftheExtremelyFaintNucleusinFRIIRadio Galaxy3C441 ResolvingtheAGNandtheStarburstinanIntensely StarformingQuasar HSA-4cm-2016+112 BrownDwarf2MASS0036

Doyle,G.(ArmaghObservatory, ED026 N.Ireland) Paragi,Z.(JIVE) Paragi,Z.(JIVE) Brisken,W.(NRAO) Diamond,P.(JodrellBank) Lonsdale,C.(NRAO) Orienti,M.(INAFBologna) Vermeulen,R.(NFRA) Paragi,Z.(JIVE) Paragi,Z.(JIVE) etest eVLBI F06L2 F06C2 GB057 GD021 GL028 GM062 GV017 N05L5 N06C2 VLBI

L-bandftptest C-bandftptest VLBIObservationofScintillationArcs Primaryfringefinder1613+341 HighSensitivityStudyofULIGs WhatCausestheVeryBroadHIAbsorptioninRadio Galaxies? OHMegamaseratz~0.25 NetworkMonitoringExperiment NetworkMonitoringExperiment

87.25(TotalHours­VLBI)

4301.00(RadioAstronomyTotalHours)
NAICAPRPP2007 21


Solar System Studies
Hours Observers
51.75 11.50 15.50 30.25 2.75 83.25 16.25 40.00 8.50 6.75 Magri,C.(U.Maine) Howell, E.S. (NAIC) Nolan, M.C.(NAIC) Ostro,S.J.(JPL) Giorgini,J.(JPL)

Project # Title
R1885 RadarandVisible/Near-InfraredInvestigationof PrimitiveMain-BeltAsteroids

Campbell,D.B.(Cornell) R2023 Campbell,B.A.(NASM) Carter,L.(NASM) Margot,J.L.(Cornell) Stacy,N.(DefenceScience&Tech) Shepard,M.K.(BloomsburgU.) Clark,B.E.(IthacaCollege) Harmon,J.K.(NAIC) Slade,M.A.(JPL) Nolan, M.C.(NAIC) Benner,L.A.M.(JPL) Howell, E.S. (NAIC) Ostro,S.J.(JPL) Giorgini,J.(JPL) Margot,J.L.(Cornell) Ostro,S.J.(JPL) Benner,L.A.M.(JPL) Magri,C.(Univ.Maine) Nolan, M.C.(NAIC) Giorgini,J.(JPL) Shepard,M.K.(BloomsburgU.) Howell, E.S. (NAIC) Margot,J.L.(Cornell) Campbell,B.A.(NASM) Campbell,D.B.(Cornell) Carter,L.M.(NASM) Campbell,D.B.(Cornell) Black,G.J.(Univ.Virginia) Carter,L.M.(NASM) Campbell,D.B.(Cornell) Black,G.J.(Univ.Virginia) Carter,L.M.(NASM) Campbell,D.B.(Cornell) Nolan, M.C.(NAIC) R2026 R2079 R2086

S-BandRadarMappingoftheLunarPoles

ARadarSurveyofX/M/E/TypeAsteroids:ASearch forMetallicCores RadarObservationsofMercuryDuringtheSummer 2005Conjunction RadarImagingofAsteroid1999RQ36

R2101

ProposalforRadarImagingofApollo,Phobos, Deimos,andSeveralMainbeltAsteroids

R2102 R2103 R2104 R2105 R2106

RadarMappingoftheMoonat70-cmWavelength UsingAreciboandtheGBT SurfacePropertiesofTitanfromAreciboRadar Observations S-BandRadarObservationsofEnceladus,Dione,and Tethys ARadarSearchforRegolithontheAsteroid2004 VG64 S-BandRadarMappingofSaturn'sRings

15.75 Nicholson,P.D.(Cornell) French,R.G.(WellesleyCollege) Campbell,D.B.(Cornell) 22









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Hours Observers
10.00 Campbell,B.A.(NASM) Campbell,D.B.(Cornell) Carter,L.M.(NASM) Harmon, J.K. (NAIC) Freeman,A.(JPL) 13.00 Haldemann,A.F.(JPL) Harmon, J.K. (NAIC) Larsen,K.W.(Univ.Colorado) Jurgens,R.F.(JPL) 7.25 Nolan, M.C.(NAIC) Howell, E.S. (NAIC) Benner,L.A.M.(JPL) Ostro,S.J.(JPL) Giorgini,J.D.(JPL) 11.00 Benner,L.A.M.(JPL) Nolan, M.C.(NAIC) Giorgini,J.D.(JPL) Ostro,S.J.(JPL) 0.75 Busch,M.W.(Caltech) Ostro,S.J.(JPL) 8.75 Margot,J.L.(Cornell) Giorgini,J.D.(JPL) 24.50 Shepard,M.K.(BloomsburgU.) Nolan, M.C.(NAIC) 18.50 Campbell,D.B.(Cornell) Campbell,B.A.(NASM) 35.75 Nolan, M.C.(NAIC) Harmon, J.K. (NAIC) Howell, E.S. (NAIC) Campbell,D.B.(Cornell) Margot,J.L.(Cornell) Ostro,S.J.(JPL) Benner,L.A.M.(JPL) Giorgini,J.D.(JPL) 23.75 Nolan, M.C.(NAIC) Howell, E.S. (NAIC) Benner,L.A.M.(JPL) Ostro,S.J.(JPL) Giorgini,J.D.(JPL) 2.00 Nolan, M.C.(NAIC)

Project # Title
R2107 70-cmWavelengthRadarObservationsofMars

R2108

Arecibo-GoldstoneMarsRadarInterferometric Mapping

R2137

RadarImagingofNear-EarthAsteroids1998ST49 and2002HW

R2167 R2168 R2169 R2170 R2182 R2183

RadarAstrometryofNear-EarthAsteroid99942 Apophis RadarImagingandShapeReconstructionof Asteroids10115(1992SK),23187(2000PN9), 9Metis,and105Artemis RadarObservationsofHighPerihelionAsteroid2000 BD19toQuantifyGeneralRelativityandSolar QuadrupoleMoments ObservationsofAsteroid68950(2002QF15)and ContinuationofaLong-TermXMEMain-BeltSurvey LunarSurfaceStudiesviaS-BandRadarImageryand Interferometry RadarObservationsofComet73P/SchwassmannWachmann3

R2184

RadarImagingofNear-EarthAsteroids2004WB1 and2001SG276

R2188 Urgent

RadarObservationsofAsteroid2005VS

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Hours Observers
3.00 Nolan, M.C.(NAIC) Benner,L.A.M.(JPL) 8.00 Howell, E.S. (NAIC) Magri,C.(Univ.Maine) Nolan, M.C.(NAIC) 10.00 Taylor,P.A.(Cornell) Margot,J.L.(Cornell) Nolan, M.C.(NAIC) Ostro,S.J.(JPL) Benner,L.A.M.(JPL) Giorgini,J.D.(JPL) Magri,C.(Univ.Maine) 8.25 Nolan, M.C.(NAIC) 3.00 Simpson,R.(Stanford) Nolan, M.C.(NAIC) 5.75 Benner,L.A.M.(JPL) Nolan, M.C.(NAIC) Giorgini,J.D.(JPL) 11.00 Jensen,E.(UCLA) Miralles,M-P.(CfA) 2.25 Nolan, M.C.(NAIC) Howell, E.S. (NAIC)

Project # Title
R2190 Urgent R2191 Urgent R2208 RadarObservationsofAsteroid2005WC1 RotationallyResolvedRadarObservationsof105 Artemis:Correlationwith3-micronSpectroscopy PhysicalCharacterizationofPotentiallyHazardous Asteroid2004DC

R2219 Urgent R2223 Urgent R2225 Urgent R2257 Urgent R2260

RadarObservationsofAsteroid2005TF49 BistaticMarsExpress-AreciboRadarObservationsof "Stealth"RegionofMars AreciboRadarImagingofNear-EarthAsteroid2006 GY2 FaradayRotationoftheCassiniS-BandTransponder fromSolarCorona RadarObservationsofAsteroid2006QV89

488.75(SolarSystemStudiestotalhours)

Space & Atmospheric Sciences
413.25 112.75 Zhou,Q.(MiamiU.,Ohio) Aponte, N. (NAIC) Friedman, J.(NAIC) GonzÀlez, S.(NAIC) MacPherson,B.(UPS) Sulzer, M.(NAIC) Tepley, C.(NAIC) Djuth,F.T.(GeospaceResearch) Sulzer, M.(NAIC) Mathews,J.D.(PennState) Tepley, C.(NAIC) Zhou,Q.(MiamiU.,Ohio) T1193 CoordinatedIncoherentScatterRadarand OpticalObservationsDuringtheWorldDays During1999-2000

T1892

AContinuumofGravityWavesintheArecibo Thermosphere?

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NAICAPRPP2007


Hours Observers
81.75 23.25 28.50 34.25 227.50 20.50 10.00 73.75 17.00 98.00 50.75 36.00 Zhou,Q.(MiamiU.,Ohio) Morton,Y.T.(MiamiU.,Ohio) Zhang,J.(MiamiU.,Ohio) Meisel,D.D.(SUNYGeneseo) Bauer,E.E.(SUNYGeneseo) Mathews,J.D.(PennState) Meriwether,J.W.(ClemsonU.) Tepley, C.(NAIC) Sulzer, M. (NAIC) Faivre,M.(ClemsonU.) Brown,B.(HarvardUniv.) Nikoukar,R.(U.Illinois) Sulzer, M. (NAIC) Waldrop,L.S.(U.Illinois) Noto,J.(SSI) Kerr,R.(NSF) Betremieaux,Y.(SSI) Bhatt,A.N.(Cornell) Kelley,M.C.(Cornell) Sulzer, M.P. (NAIC) Fernandez, J.(NAIC) Sulzer, M.P. (NAIC) Aponte, N. (NAIC) Riggin,D.(ColoradoResearch) Fritts,D.C.(ColoradoResearch) Janches,D.(ColoradoResearch) Zhou,Q.(MiamiUniv.-Ohio) Mathews,J.(PennState) Wiig, J.(NAIC) Janches,D.(ColoradoResearch) Chandran,A.(Univ.Colorado)

Project # Title
T2029 T2084 T2085 ObservationsofGravityWaveActivitiesintheMesosphereUsingtheDualBeamIncoherentScatter Radar StudiesofaNewlyDiscoveredAsteroidalDust Stream RadarandOpticalMappingoftheMidnight Temperature



T2090 T2091

ANewApproachtotheOptimalExtractionof IonosphericParametersfromIncoherentScatter RadarMeasurements ACharacterizationofEnergeticNeutralAtomsin ThermosphericalIonosphere/ExosphereCoupling

T2131 T2134 T2138

GyroLineObservationsinEandFRegionsDuring EveningHoursatArecibo E-RegionSeasonalObservationsofIon-Neutral CollisionFrequenciesUsingPlasmaandIonLine Measurements AreciboStudiesofGravityWaveMomentumFlux andMeteoricFluxintheMLTRegion

T2162 T2163

TestTimefor430MHzInterferometerProject AProposalforRadarMeteorObservationsduring theSeasonalMinimumoftheSporadicActivityat Arecibo:ACrucialNeedfortheConfirmationof ModeledPredictionsanditsRelationtothe AtmosphericCa,Ca+andKLayers DeterminationofIonCompositioninthe IntermediateLayers MeasurementofNegativeIonsintheD-Regionand ComparisonwithNewModels

Zhou,Q.(MiamiUniv.-Ohio) T2165 Brenneman,M.(MiamiUniv.-Ohio) Raizada, S. (NAIC) Sulzer, M.P. (NAIC) T2166

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25


Hours Observers
45.25 22.75 15.00 59.00 41.00 23.00 8.25 Nicolls,M.J.(Cornell) Aponte, N. (NAIC) Sulzer, M.P. (NAIC) Djuth,F.T.(GeospaceResearch) Carlson,H.C.(AFOSR) Sulzer, M.P. (NAIC) Kelley,M.C.(Cornell) Wong,V.K.(Cornell) Nicolls,M.J.(Cornell) Sulzer, M.P. (NAIC) Lee,M.C.(MIT) Sulzer, M.P. (NAIC) Burton,L.(MIT) Cohen,J.(MIT) Husmann,D.(MIT) Labno,A.(MIT) Pradipta,R.(MIT) Rokusek,D.(MIT) Waldrop,L.(Univ.Illinois) Sulzer, M.P. (NAIC) Waldrop,L.(Univ.Illinois) GonzÀlez, S.(NAIC) Rapp,M.(Inst.Atmos.Phys., Germany) Strelnikova,I.(Inst.Atmos.Phys.) Raizada, S.(NAIC) Sulzer, M.P. (NAIC)

Project # Title
T2211 T2212 T2213 T2214 High-ResolutionElectronTemperatureMeasure- mentsUsingthePlasmaLineAsymmetry TheNaturalPlasmaLineRevisitedasanAeronomical Diagnostic VerificationandCalibrationofOn-OrbitDetectionof IonosphericLayersandConductivityUsingtheGPS OccultationMethod OpticalandRadarDiagnosticsofEnergeticElectron PrecipitationOverArecibo,PuertoRico

T2226 Urgent T2250 T2253

ImprovedNeutralAtomicOxygenDensityEstimation UsingtheAreciboDual-BeamISR TheBurnsideFactorRevisited:AModel-Independent IonMomentumBalanceStudy SignaturesofChargedMeteoricSmokeParticlesin IncoherentScatterRadarSpectra

1441.50(Space&AtmosphericSciencestotalhours)

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NAICAPRPP2007


2.4 Visiting Public at the Observatory
Summary.Asinpreviousyears,theVisitorCenter hosted many special events for the general public andfortheNAIC/AreciboObservatorycommunity ingeneral.TheseincludedtheNAIC/NRAOSingle Dish Summer School, Geoscience Workshop, the Gordon Lecture, and other scientific and educational workshops. We updated 15 displays at the Visitor Center and are in the process of updating and adding new panels. Three educational workshops were offered (two for teachers and one for journalists) on the issue of pseudoscience, and we hostedanastronomysummercampfor25middle schoolstudents.ThenumberofvisitorstotheAreciboObservatorydeclinedby9%andwehavetaken several measures to make the operation more efficient. General Public. A trend that began in FY2005 reflecting an annual decrease in the number of visitorstotheAreciboObservatoryisalsoreflected in the figures for FY2006. The number of visitors to the facility in FY2006 was 99,496 as compared to109,108inFY2005.This9%decreaseisseenin both the general public, and the school children visiting A.O. But the main reason affecting the flowofvisitorsinFY2006wasthedropinthenumber of school groups visits. This issue is discussed inSection5.1.
ThePuerto Rico Hotel and Tourismindustryisalso reporting a 10% decrease in room occupancy for this period. Many businesses in Puerto Rico have been affected by the lack of economy growth in theregion.

3. Accomplishments and Plans of the NAIC Scientific Staff
NAIC Staff scientists are actively engaged in observational investigations and theoretical analysis in areas of astrophysical research from the cosmologicalstructureoftheuniversetotheshapeofasteroids passing in the vicinity of the Earth. Nearly all of the research projects involved collaborations between NAIC staff scientists and colleagues at universities and institutes elsewhere. And, nearly all of the research in progress now, or planned to begin this program year, will extend over several years as data are taken, reduced, analyzed and finally written up for publication. For that reason, the research reported here will not be completed in PY2007 but substantial progress is expected in alltheprojectsmentionedhere.

3.1 Cosmology
A VLBI visibility-survey of a complete sample of more than 1000 radio sources selected from the VLA-FIRST catalog to have 1.4 GHz flux density greater than 1 mJy has recently been completed. This VLBI survey used the ultra-high sensitivity achievable with the Arecibo and Efflesberg telescopes at 21-cm wavelength with each telescope being equipped with VLBA/Mk4 recording at 512 Mbits/s.Evenforon-sourceintegrationsofaslittle as1-second,allsourceswithcompactcomponents offluxdensitygreaterthan1-mJyaredetectableat 8-sigma or higher. This permits a cosmologically important statistical comparison to be made with the few extensive surveys done of brighter (> 10-mJy) sources, e.g. the Person-Readhead surveyandtheCaltech-JodrellBanksurvey. AlloftheVLA-FIRSTsourcesselectedforstudy liewithintheSloanDigitalSkySurveyareaand all are identified with SDSS objects brighter than V = 24 mag. Redshifts are available for all objects. Thus, the body of data for which inter-comparisons are possible is very extensive thereby leveraging the scientific value of the current dataset. Among the scientific results to be gathered from this work is a determination of the relative fraction of AGN and Starburst galaxies as a function of redshift for afaintsourcepopulationofobjects.[C.Salter, T.Ghosh]

Figure 2.4.1. NumberofObservatoryvisitorsperyear.

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27


3.2 Early Galaxies
Using the Arecibo telescope and the GMRT, HI and OH observations were made toward a radio sample of 27-objects, seventeen of which were "Gigahertz Peaked Spectrum" (GPS) objects and Compact Steep Spectrum (CSS) objects. No OH emission or absorption was detected toward any of the sources, but the HI detection rate was approximately25%,includingfourpreviously-known HIabsorptionsystems. When the new results are combined from other HI searches it is possible to compile a sample of 96 radio sources consisting of 27 GPS, 35 CSS, 13 compactflatspectrumand21large(LRG)sources. TheHIabsorptiondetectionrateishighest,~45%, for the compact GPS sources and it is lowest for theLRGsources.WefindHIcolumndensitytobe anticorrelated with source size, as reported earlier by Pihlstrom et al., a trend that is consistent with inferences from optical spectroscopy. The HI column density shows no significant dependence on eitherredshiftorluminosity,whicharethemselves stronglycorrelated.Theseresultssuggestthatthe environments of radio sources on GPS/CSS scales are similar at different redshifts. Further, in accordance with the unification scheme, the GPS/CSS galaxies have a HI detection rate, ~40%, that is significantlyhigherthanthedetectionrate,~20%, toward the GPS/CSS quasars. Also in accord with the unification scheme, the strongest absorption component detected toward GPS sourcesappears blue-shiftedinastrongmajority(65%)ofthecases. All of these results are in accord with a growing body of evidence supporting the model in which jet-cloud interactions play an important role in de-

terminingtheionizationandkinematicalproperties of the interstellar gas in early and active galaxies. [T.Ghosh,C.Salter]

3.3 Active Galaxies
As part of the NAIC summer research program for undergraduates, under the supervision of Tapasi Ghosh, Emmanuel Momjian, and Chris Salter (NAIC), MarÌa Ximena FernÀndez (Vassar and Dartmouth) worked on a project that focused on 85 galaxies from the 2 Jy IRAS-NVSS Sample with far-IR luminosities >109Lsun. This subsample contained objects that lay in the R.A. (B1950) range 20h-00h. The project resulted in several new HI and OH detections, both in emission and absorption.Amongthemostinterestingofthesewasthe discoveryofHIandOH-megamaseremissionfrom the ULIRG IRAS 23327+2913 (LIR=1.15â1012 Lsun; z~0.107). This ULIRG is a system of two galaxies separatedbyabout20kpcatthebeginningstages ofinteraction(Dinh-Vi-Trungetal.2001,ApJ,556, 141), see Figure 3.3.1. The northern galaxy is disturbed, while the southern one is a normal spiral with a very thick bar structure. Dinh-Vi-Trung et al. report the detection of CO(1-0) only from the apparentlyundisturbedsoutherncomponent. Follow-up observations of this ULIRG were made bythegroupinOctober2006.Figure3.3.2shows the HI spectrum from IRAS 23327+2913. The central velocity of the dominant spectral feature indicates that this HI emission is associated with the southerncomponent,whiletheweaker"shoulder" at ~32000 km/s corresponds to the redshift of the northern component. Figure 3.3.3 shows the OH megamaser spectrum, with the dominant feature from the 1667 MHz transition: this has a broad,

Figure 3.3.1. Left frame: the contour plots of the CO(1-0) emission from IRAS23327+2913 overlaid on the R-band image. Central frame: contour plot of the same R-band image at the same scale. Right frame: K-band image (Dinh-ViTrungetal.2001)

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2.5 Flux Density (mJy) 2.0 1.5 1.0 0.5 0.0

IRAS 23327+2913 HI

3.4 Normal Galaxies and Clusters
The evolution of the Tully-Fisher relation over cosmictimeismuchdebated.Ifgalaxiesweremore luminous in the past, we should observe an offset in the TFR derived independently at high and low redshiftz(i.e.,achangeofitszeropoint).However, studies based on optical spectroscopy (e.g. Flores et al. 2006, AAP, 455, 107) have reached conflictingconclusions.Resultsvaryfromsubstantialluminosity evolution (in excess of one magnitude with respecttothez=0TFR)evenatmodestz,tonosignificant change uptoz~1. Evidence forevolution oftheTFR,orlackthereof,remainsinconclusive. Barbara Catinella (NAIC-Arecibo) and collaboratorsatCornell(M.P.HaynesandR.Giovanelli)and the University of Pittsburgh (J.P. Gardner and A.J. Connolly)haveundertakenatargetedsurveywith the305-mAreciboradiotelescopetodetectHI-line emission from disk galaxies at z>0.16 (i.e. at frequenciesbelow1220MHz).Amongotherapplications, this dataset will be used to study the evolutionoftheTFRatintermediateredshifts.Compared toopticalwidths,HImeasurementssamplealarger fractionofthedisks,wheretherotationcurvesare typically flat, and are not affected by slit smearing, by misalignment, or by aperture effects. Thus, in contrast to studies based on optical spectroscopy, radio observations allow a direct, technique-independentcomparisonwiththelocalTFR. Naturally, detectionof21cmemissionfromgalaxies at z>0.1 is difficult: the signals are weak, accurate redshifts of the targets need to be known in advance, the presence of radio frequency interference restricts the accessible redshift windows, and the larger number of galaxies sampled by the antennabeamathigherredshiftleadstoincreased confusion problems. In fact, these observations haveonlyrecentlybecomefeasiblethankstotechnicalimprovementsatArecibo(Gregorianupgrade, a new L-wide receiver in 2003, with access to frequenciesdownto1.12GHz),andtotheavailability oftheSloanDigitalSkySurvey3.2.

31000

31500 32000 32500 33000 Heliocentric Velocity (km/s)

Figure 3.3.2. Spectrum of the HI 21-cm line emission from the ULIRG IRAS23327+2913. The velocity resolution is 29 km/s.

probablydouble-peaked,structure.The1665MHz transition is very tentatively detected and correspondstothefeatureat~32700km/s.Thecentral velocityoftheOH1667MHzlinesuggeststhatthe megamaseremissionfromthesystemismorelikely to be associated with the southern component. No megamaser emission is detected at the velocitycorrespondingtothenorthern,disturbed,component of this ULIRG. The results presented here, combined with the CO(1-0) observations of DinhVi-Trungetal.(2001),showthatIRAS23327+2913 does not fit into the commonly accepted scenario for ULIRGS of a merger between two disk galaxies, where the two progenitors of the merger are strongly disturbed during the interacting phase, with the final product of the merger resembling an elliptical galaxy (Mihos & Hernquist 1996, ApJ, 464, 641). [M. Fernandez, E. Momjian, T. Ghosh & C.Salter]
IRAS 23327+2913 OH

Flux Density (mJy)

1.0 0.5 0.0 31000 31500 32000 32500 33000 Heliocentric Velocity (km/s)

Figure 3.3.3. Spectrum of the OH 18-cm megamaser emission from IRAS23327+2913. The broad, probably doublepeaked, dominant spectral feature corresponds to the 1667 MHz transition from the southern component of the system. The1665MHzlineistentativelydetectedandcorrespondsto the spectral feature at ~32700 km/s. The velocity resolution is27km/s.

2 3 Funding for the Sloan Digital Sky Survey (SDSS) and SDSS-II has beenprovidedbytheAlfredP.SloanFoundation,theParticipating Institutions,theNationalScienceFoundation,theU.S.Department of Energy, the National Aeronautics and Space Administration, the Japanese Monbukagakusho, the Max Planck Society, and the HigherEducationFundingCouncilforEngland.TheSDSSWebsite at http://www.sdss.org/, hosts its database, which provides high quality photometric images, accurate redshifts, and line-emission informationforalargenumberofgalaxies.

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29


(a)

(b)

Figure 3.4.1. (Left) SDSS image of the galaxy J142735.69+033434.2 (from the SDSS Sky Server web page at http://cas.sdss. org/dr5/en/);thesizeofthefieldshownis1.3´.(Right)Calibrated,smoothedHIspectrumobtainedatArecibo.Theverticalred lineindicatesthefrequencycorrespondingtotheSDSSredshift(z=0.2455).Thetotalon-sourceintegrationtimeis176minutes. ThisrepresentsthehighestredshiftdetectionofHIemissionfromanormalgalaxytodate.

Thegroup'stargetsforHIspectroscopyatArecibo wereextractedfromtheSDSSdatabaseonthebasis oftheirredshift,opticalemission-linestrength,inclination, disk morphology, and relative isolation (to minimizeconfusionwithinthebeam).HIprofilesof adequate quality for velocity-width measurements were obtained for 20 galaxies with 0.17 z 0.25, with average total integration times between 2 and 6 hours. Figure 3.4.1 shows the highest redshiftdetectionofHIemissionfromanormalgalaxy to date (z=0.2455). The HI spectra of 12 of the 20 detections are presented in Figure 5. Analysis of the selection biases of this sample, necessary to establish if there is a change of the TF zero point basedonthisdataset,isinprogress.[B.Catinella] The Arecibo Galaxy Environment Survey recently covered five square degrees around the NGC 7332/7339 galaxy pair. The survey detected the large spiral galaxy, NGC 7339 along with two previously unknown dwarf galaxies in the group (AGES J2238+2352 and AGES J2236+2343). The lenticular galaxy NGC 7332 and the dwarf spheroidalgalaxyKKR73werenotdetected,butupper limitscanbesetontheirneutralhydrogenmasses. The survey also found at least twenty galaxies in the volume behind the group, out to a redshift of ~17,000km/s.Withthecommissioningofthenew E-ALFAcorrelatorearlynextyear,itisexpectedthat AGESwillfindmoreofthedistantsourcesinfuture fields.[R.Minchin]

3.5 Intergalactic Gas and Tidal Remnants
Damped Lyman Alpha (DLA) absorption systems areindicativeofalargecolumndensityofHIalong the line of sight to a distant object. Always, the interpretation is that DLA absorption arises in a disk galaxy and, depending on the angular scale ofthebackgroundsource,itcanbetheintegrated absorptionoftheentireinterveningdiskoritcould beabsorptionresultingfromasingledarkcloudin thedisk.Theabsorptionlinewidthallowsustodiscriminate between these two cases. DLA absorptionsystemsarecommonlyseenintheabsorption spectrumofz~1-3QSO,buttheyarenearlyabsent in the local, z<1 universe. Some of this is certainly a selection effect as the Ly- line is unobservable from the ground at z<1. Here is where the radio observationshaveuniqueutility. Recently, a search has been made of more for HI absorption searching for DLA systems toward more than 200 distant, compact, radio sources. The search is sensitivity to DLA systems at 0 < z < 0.3. Data are taken using the method of double positionswitchingwherethetargetobjectandthe calibrator object were both objects to be studied and, on the sky, they were a close pair of sources. DLAabsorptiontowardthe"target"wouldappear as absorption in the spectrum of the "reference" object whereas DLA absorption in the "reference" would appear as a peak in the ratio spectrum. Analysisofthedataisunderwaywithapreliminary indication that the detection rate is unlikely to exceedabout5%.
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When finalized, this study will help improve both DLAstatisticsatlowredshift,andknowledgeofthe HImassfractionatthepresentepoch.Importantly, theradiosearchesarenotaffectedbyobscuration intheinterveninggalacticdiskssothestatisticalinformationwillremainrobust.[T.Ghosh,C.Salter]

3.6 Milky Way Galaxy
An important gap in our understanding of the evolution of stars of modest mass, like our Sun, is theabsenceofanabinitiounderstandingofmassloss at their asymptotic giant branch (AGB) phase. We have no accepted theoretical constraints on the rate or on the evolution of dM/dt from AGB stars,andsoworkwithadhocrelationsadaptedto inferredratesofdM/dt. This has beenonereason for studying OH/IR stars. Recent work by Lewis shows that the problem has now become more complex, as when NIR and OH observations are combinedwithmodellingresults,theysuggestthat thedM/dtofOH/IRstarsisstronglymodulatedon amuchlongertime-scalethanthepulsationalperiodsofthestars. Previous pointers to this occur in CO mapping of the carbon star IRC+10216, and in Hubble images of the Cat's Eye and Egg nebulae, which exhibit a sequence of concentric rings underlying all of their other structure. The NIR colors of OH/IR starsdefineatightlinearlocusextendingoverfive orders of magnitude in a 2MASS two-color plot. Lewis(AJ132,489)modelsthisusingtheradiative transfercodeDUSTY,and findsthat theNIRcolors of a set of models froma rangeof constant dM/dt exactly trace the locus provided one uses a coldsilicate dust opacity, and starts with a stellar spectral energy distribution (SED) matching its bluest colors. It is then easy to model the detached shell thatgrowsunderthenormalexpansionofathick, dust-shell model when dM/dt is set to zero: these modelsalsofollowthelocus.Onebyproductisthe association of a chronology with their NIR colors, whichshowsthatittakes<100yrforashelltotraverse the entire color locus. And much the most rapidcolorevolutionnaturallyoccurswhiledustis departing from the vicinity of the dust-formation radius, where it has its maximum volume density. Thisisthekeyfinding. The first evidence for a general deep modulation ofdM/dtisfrommassiveOH/IRstars,andisbased on combining modelling results with the distribution of NIR colors of cohorts of stars selected on
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thebasisoftheirMIRcolors:80%ofthosewiththe reddestMIRcolorsfallnearthemiddleofthelocus ratherthanatitsredend,wheretheywouldoccur if their shells were generated by a constant dM/dt (Lewis et al., AJ, 127, 501). This is only explicable forthermallypulsingOH/IRstarsifthesestarshave astronglymodulateddM/dt. The second line of evidence comes from modelling the rapid loss of 1612 MHz masers from lowmass OH/IR stars. Four of those in the Arecibo skyhavecompletelylosttheir1612MHzmasersin thelast20yr,andone,fromthe472dayLPVIRAS 19479+2111, recently turned ON again. Gray, Howe and Lewis (MNRAS 364, 783) modelled the speed of the decline in maser intensity, by constructing the set of time-dependent OH column densities arising when dM/dt goes abruptly to zeroafterbeingconstantfor300yr,togetherwith a time-dependent radiative transfer model for the generationofthemasers.Thesemodelsmatchthe declineofthemasers,andshowtheyarepumped throughthe53µmtransitions.Thesearesensitive tothereprocessingofthestellarSEDbytheinnermostdustshell,whichisvacatedfirstwhendM/dt =0.Thisleadstoaweakeningofthepumpandto the loss of the maser. The rapid switching ON & OFFofthesemasersisthusshowntobeanartifact ofastronglymodulateddM/dtfromanOH/IRstar thathadamodestprogenitormass. With both massive and low-mass stars exhibiting stronglymodulatedmass-lossrates,stellarstructure calculations are doomed to rely for some time to come on an average dM/dt, and to infer this from observations.Thisfindingalsohelpsustointerpret theNIRcolor-magnitudeplotsofcarbonstarsfrom SpitzerobservationsofLocalGroupgalaxies,which show lightly populated "echo sequences" tracking thefundamentalandfirstovertonesequences. Coldatomicgasrepresents~30%oftheISMmassin ourpartoftheGalaxy.Sincehydrogenisthemost abundantelementininterstellargas,theHI21-cm lineisanaturalprobeofthecoldatomicphase,the coldest parts of which (T < 50 K) can be detected as HI self-absorption (HISA) against brighter backgroundHIemission(Figure3.6.1). Until recently, HISA studies of cold HI were hamperedbylowangularresolution,limitedskycoverage,orboth,makingitdifficulttomeasuretheabsorption properly and chart the cloud population inanunbiasedway.Buttheseproblemshavebeen overcome with new large-scale, arcminute-resolu 31


Figure 3.6.1. Left: Dark HISA clouds in the CGPS (Gibson et al., 2000). Some HISA features have CO emission (contours), but some do not. Right: Spectra of two HISA features at v=-40 km/s, with total H I emission (top), ONOFFabsorptionstrength(middle),andCOemission(bottom).

tion 21cm radio synthesis surveys of the Galactic disk. Recent work shows that (1) a rich and varied HISApopulationcanbeseenathighangularresolution, and (2) most of these cold HI clouds have no obvious counterparts in the standard 2.6mm CO J=1-0 line tracer of molecular gas. The latter contradicts traditional expectations that HISA gas traces the small fraction of molecular cloud gas that is atomic, unless the CO proxy for H2 is itself suspect. Algorithms have been developed to identify and analyzetheCGPSHISAfeaturessystematically(Gibsonetal.,2005a,2005b;seealsoGibson2002).We have found a faint, intricate HISA population that appearsubiquitousandmaytraceturbulentfluctuationsintheinterstellarmedium.Bycontrast,stronger HISA is concentrated into discrete complexes, manywithradialvelocitiesexpectedforthedensity wave of the Perseus spiral arm (Roberts, 1972). Indeed, the strong outer-Galaxy HISA we see in the CGPS requires spiral arm velocity perturbations in ordertoexist;otherwise,thevelocity-distancerelationship is monotonic, and no organized H I emission background can occur at the same velocity as the absorbing gas. HISA thus probes the spiral structure of our galaxy from the inside. We have also found that, statistically, most CGPS HISA does not correspond with significant CO emission. This does not rule out H2 untraced by CO, a possibility underinvestigationelsewhere.Or,someHISAmay
32

lackmoleculargasentirely.EquilibriumcloudmodelshavedifficultyexplainingthelowHISAtemperature without molecular cooling, but equilibrium maynotapply.Instead,theHISAmaytracecoldHI beforeorafteraphasechange.Inthestandardspiral shock picture, gas is compressed downstream of the shock, where it forms molecular clouds and thenthemassivestarsthatdefinethespiralarm.If this is correct, HISA is tracing evolving gas as well asspiralstructure. TheoriginalCGPSlongitudecoveragehasbeenextendedto65-175degrees,andwehavesubmitted a proposal for a second extension to 190 degrees. In addition, the VLA Galactic Plane Survey (VGPS; Taylor et al., 2002) has been observed over 18 - 67 degrees longitude, and the Southern Galactic Plane Survey (McClure-Griffiths et al., 2001) covering 252 - 358 degrees is being extended through the Galactic center to 20 degrees. Collectively, these and other projects to map molecular gas anddustinthesameareasarenowknownasthe International Galactic Plane Survey (IGPS). When the IGPS data are complete, they will allow HISA mapping over most of the Galactic disk. Already, these efforts are bearing fruit: a preliminary analysisofpartoftheVGPS(Gibsonetal.,2004)showed HISAisevenmorecommonherethanintheCGPS (Figure 3.6.2). The inner-Galaxy sightlines of the VGPSshouldbemorefavorableforHISA,sincegas on the near side of the Galactic center always has
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a far-side emission background at the same velocity. The VGPS HISA also shows an improved though still imperfect CO correspondence, perhaps because of the same geometric effect. Most intriguing is the prominent concentration of HISA along a number of velocity features that look suspiciously like spiral arms. Spiral structure has traditionally been more difficult to discern in the inner Galaxy, but HISA may helpwiththissituation. Most sightlines in the sky lack sufficiently bright backgrounds to produce self-absorption, and Figure 3.6.2. HISA line strength integrated over latitude for a 25-degree section of since the population of cold HI theVGPS,withdarkerfeaturesbeingstronger.ManyHISAfeaturesrunalmostparallel linesof constantGalactocentricradiusR(overplottedforaflatrotationcurvewithR0 clouds should be randomly dis- to8.5kpcandv =220km/s),whichisconsistentwiththeHISAtracingspiralstructure = 0 tributed with respect to such intheinnerGalaxy(Gibson,2004). backgrounds, the majority of cold HI features should manifest as narrow-line P-ALFAdatareduction.Theyworkedonaseriesof HI emission (NHIE) rather than HISA (one famous python scripts developed to automatically process the P-ALFA data with full resolution using Scott example is Verschuur's Cloud A; see Knapp & Verschuur,1972).ThealgorithmsusedtodetectHISA Ransom's (NRAO) PRESTO routines. These scripts in the CGPS dataset can also be run in an inverse also load the results into a database, to be hosted mode to identify NHIE features. Early tests of this bytheCornellTheoryCenter.Finally,Patrickdevelfacility on CGPS data show considerable promise, oped a viewer that connects to the database and allows candidates to be browsed and flagged. As with a great many NHIE features appearing as organized structures on the sky and in velocity. The part of the testing of the scripts and the pipeline, CGPS NHIE feature population outnumbers the several disks worth of data have been processed, CGPS HISA population considerably, as might be and thepulsarsseeninthe"quicklook"processing expected. Further work is planned to explore the wereagainreadilydetected.Inaddition,onenew spatial distributions of the NHIE features and to pulsar has been discovered, PSR J1903+03. It was constrain their properties with additional data. [S. detected with a S/N of 24.2, a spin period of 2.15 ms, and a DM of ~300 cm-3 pc. From the confirGibson] mationandtimingobservationsmadetodate,itis clearthatthismillisecondpulsar(MSP)isinabinary 3.7 Pulsars system with an orbital period of several hundred days. The P-ALFA survey has discovered 35 new pulsars to date. These were found using the "quicklook" Outside globular clusters this is the 5th fastest processing. This program degrades the data by spinningpulsarknown:whenglobularclusterpula factor of 16 in time and resolution to allow for sars are also included, it is the 11th. This object almostreal-timesearchingofpulsars.However,by has the highest DM known for any MSP. This is doingthis,thereductionprocesshassystematically extremely important --it confirms the fact that the degraded its sensitivity to fast pulsars and pulsars P-ALFA survey can see MSPs deep into the disk of at high dispersion measures (DMs). The P-ALFA the Galaxy, far from the Solar System, where the consortium intends to re-reduce all its data while vast majority of MSPs await discovery. MSPs, parexploitingitsfullfrequencyandtimeresolution. ticularly those in binary systems, are important for manyareasofastrophysics(see,forinstance,article Duringthepastsummer,PatrickLazarus,anunderonPSRJ1738+0333). graduatestudentatMcGillUniversity,workedwith DavidChampion,JasonHesselsandVickyKaspion
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Using models of the electron distribution of the Galaxyandthepulsarpopulation,DuncanLorimer (West Virginia Univ.) predicts that the present observing system (i.e. 100 MHz bandwidth, 268s integrations) will detect 120 MSPs in the area 32 34

"Stiff" EOSs predict that matter is highly incompressible. That would produce very large stars that cannot withstand large spin frequencies without breaking apart. Finding fastspinning pulsars could therefore disprovesuchEOSs. the contrary, the very "soft" EOSs On predict, because of their different micro-physical assumptions, lower pressures for a given density. More compressible matter translates into smaller, compact stars with very high gravitational fields, with upper mass limits of about 1.6 solar masses (above that limit, the star implodes and forms a black hole). Finding a more massive star, we can exclude such"soft"EOSs. · Binary pulsars give us the only strongfield tests of gravitational theories. Russell Hulse and Joe Taylor earned the Nobel Prize in Physics in 1993 for their discovery of the first binary pulsar, PSR B1916+13. The precise tracking of the motion of this object led to the confirmation of the existence of gravitational waves, a fundamental prediction of GeneralRelativity. These two astrophysics experiments are among the top priorities for research in astrophysics outlined in the report of the National Academies entitled"FromQuarkstotheCosmos:ElevenScience QuestionsfortheNewCentury"(BoardonPhysics and Astronomy, 2003, National Academies Press). Some of the specific investigations underway includethefollowing: · Ninenewpulsarshavesincebeenfound inTerzan5.Oneofthem,Terzan5ad,is aneclipsingbinarysystem,anditisnow the fastest spinning pulsar known. Although it is still not fast enough to constrain the equation of state seriously, other faster pulsars might still be found in globular clusters. Also, Terzan 5adalreadyconstrainsmodelsofgravitational wave emission, and it might be detectedbyLIGOinthenearfuture. · Continued timing observations will be made of the first double pulsar,
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PSR J0737-3039 A and B at ATNF. Timing this pulsar for only three years has already yielded the most precise strong-field tests of General Relativity ever!
· The ALFA pulsar survey will benefit from the increased processing bandwidth made possible by the new NAIC PALFA spectrometer (see also the Arecibo website of this survey and for information on the spectrometer). This has recently discovered the second most relativistic system known, PSR J1906+0746. This system is also about 1000 times younger than the double pulsar.Itbelongstoanew population of young, binary systems that could include even more eccentric and compacts orbits! This survey is expected to find many hundreds of new pulsars. It is specially sensitive to fastspinning pulsars and pulsars with short orbital periods, in fact it has just found its first MSP! · Timing the PSR J1738+0333 binary system at Arecibo have recently resultedinthe lowest limits ever on emission of dipolar gravitational waves. This is very important for constraining alternative theories of gravitation! [P. Freire]

probabilitywiththeEarthin2036byaboutafactor oftwotoabout1in40,000. A radar-derived shape model of the near-Earth asteroid binary system 1999 KW4 appears in two companionarticlestoappearinScience(seeFigure 3.8.1).Thefirstpaper,bySteveOstro(JPL)etal.(Science, 2006, doi: 10.1126/science.1133622), uses high resolution radar images allow the shape of the larger component ("Alpha") to be determined to within 3% in each dimension. Since the binary orbit determines the mass, they accurately determinedthedensity(1.97±0.24g/cm3). Together, Alpha's size, shape, spin, density, and porosity reveal it to be an unconsolidated gravitational aggregate close to its breakup point, suggestingthatKW4'sorigininvolvedspin-upanddisruptive mass shedding of a loosely bound precursor object, probably within the past million years, and perhaps much more recently. The disruption may have been caused by tidal effects of a close encounterwithaplanetorbytorquesduetothermal radiation of absorbed sunlight (the "YORP" effect).Thenear-circularityofAlpha'spole-onprofile further suggests that the disruption may have produced a quasi-circular disc of particles rather thanmerelyaprolateelongatedbody. The second paper, by Daniel Scheeres (Univ. of Michigan) and collaborators (Science, 2006, doi: 10.1126/science.1133599)examinesthedynamics of the binary system. They determined that solidbody effects and a coupling between rotational and orbital motion can be more pronounced and can have different time scales than with the other

3.8 Solar System
Comet 73P/Schwassmann-Wachmann 3madeacloseapproachtotheEarthin May 2006, and presented an excellent observing opportunity: The best since C/Iras-Araki-Alcock 1983. The comet has split into several fragments, and Mike Nolan and John Harmon (NAIC) obtained radar images of two of the nucleus fragments and the first-ever radar "image" of the coma of fragment "B". Ellen Howell (NAIC) obtained spatially-resolved OH spectra to determine wateroutflowfluxandvelocity.

Radar observations of asteroid (99942) Apophis in May By Lance Benner (JPL) and Mike Nolan reduced the uncerFigure 3.8.1.Shapeofasteroidbinarysystem1999KW4,asderivedfromthe taintyinitsorbit,reducingthepredicted range-DopplerechoesoftheAreciboS-bandradar.(Courtesy,MikeNolan)
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binariesthatnaturehasprovided(binarystars,the Earth-Moon and Pluto-Charon systems, and much larger binary asteroids like the Ida-Dactyl system). Previous studies of binary system dynamics have nothadtowrestlewithinteractionsofcomponents whose shapes are irregular and asymmetrical and whose interiors are nonrigid, porous assemblages ofgranularmaterials.Thenewresearchestablishes thetechniquesneeded to investigatebinaryNEAs anddisclosesphenomenacriticaltounderstanding howtheseasteroidsoriginatedandevolved. The 3-MW gas turbine generator that powers the S-band radar system was found to have a serious fault during a routine inspection in July this year. It has now been repaired, and operations should have resumed by the time of publication of this newsletter. Beginningin January2000, the Saturnsystemhas been observable for about half an hour per night at Arecibo: The transmitter is run for 30 minutes, then the telescope performs other observationsuntilitistimeto receive the echoes an hour andahalflater. A number of observing programs have been observing Saturn's rings and satellites. After the 2007 apparition, SaturnwillheadSouthofthe Arecibo declination range until 2028, and the observers are looking forward to a final observing season in January and February 2007. [M. Nolan, E. Howell and J. Harmon] The long-period Comet SWAN (C/2006 M4) was discovered 12 July 2006 on SOHO spacecraft images. The comet experienced an outburst on 25 October (IAUC 8766) and had brightened by more than 4 visual magnitudes. This brighteningbehaviorinalong-period comet often suggests a fragmentation of the nucleus.
36

Fragmentationeventsgenerallyresultinadramatic increase in gas production and could lead to total disruption of the body. Observations of split and fragmentingcometssuchasthisprovideanimportantviewofthefresh,unprocessedinterioricesthat arepreservedfromthetimeoftheformationofthe comet in the early solar system. Fortunately, the Arecibo Observatory is quite responsive to targets of opportunity, particularly during daytime hours when many astronomical observations cannot be done. We observed Comet SWAN on 27-29 October, and detected the 1665 and 1667 MHz OH lines. We observed using L-wide, centered on the nucleus position, and in a hexagonal pattern 4.1 arcminaway,whichcorrespondsto179,000kmat the distance of the comet. The 1667 MHz spectra areshowninFigure3.8.2,withmodelfitsshownas dottedlines.Thehexagonisorientedwiththesunward and tailward direction as projected on the sky. Over the three-day period, there were only

Figure 3.8.2. TheOH1667MHzlineofCometSWAN(C/2006M4)on27October2006. Thenucleuspositionisinthecenter,andeachouterpositionis4.1arcminutesawayfrom the nucleus in the coma, which corresponds to 179,000 km at the comet. The model spectra are shown as dotted lines along with the data. The model assumes hemispherical symmetry, so deviations in individual off spectra may indicate jets or asymmetries in the coma.(Courtesy,EllenHowell)











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vel (km/s)

minorchangesinobservedlinestrength,andthose couldbeattributedto expected changes inexcitation of the OH as the comet moved with respect to the sun. More detailed analysis is continuing. Additionalobservationsmayindicatewhetherthis newactivitywillcontinue,orifthiswasaone-time event and the comet will gradually fade back to previous brightness levels. These data will be particularlyinterestingforcomparisonwithourrecent observations of the fragments of periodic Comet 73P/Schwassmann-Wachmann3.

tioninawaythatisimpossiblefordoubleneutron starsystems.

100 0 -100 -200 -300 -400 -0.5 0 0.5 phase (Unitless) 1

3.9 Fundamental Physics
PSR J1738+0333 is a 5.85-ms pulsar in a binary system with an orbital period of 8.5 hours, and a companion white dwarf (WD) with a mass of ~0.2 solar masses. This millisecond pulsar (MSP) was found with the Parkes 64-m radio telescope in a search led by Bryan Jacoby (then at Caltech) andMatthewBailes(Swinburne).PauloFreirehas madetimingobservationsofthispulsarforthelast 3years,sopreliminaryresultshavebeenpresented herebefore.However,thisisnowoneofthemost precisely timed pulsars ever, with rms residuals of order 200 ns per WAPP per hour. Its orbit has a small apparent eccentricity of about 0.0000011, which implies that the orbit itself does not depart frombeingexactlycircular(witharadiusof102,000 kmsini,whereiistheinclination)bymorethan80 microns(and,yes,thisvalueiscorrect). Recent optical work constrains the masses of the pulsar and its companion. Using the Magellan telescope Marten van Kerkwijk identified the companion star and measured its spectrum, which is very similar to the 0.203 solar mass companion of PSR J1909-3744. Further, the radial-velocity curve was measured using Gemini South (see Fig. 3.9.1), from which one can derive its mass ratio of 8.1±0.3. The pulsar's mass is therefore ~1.6±0.2 solar masses (assuming a 10% uncertainty in the massofthecompanion).Thisisinterestingaswere it to be measured more precisely, it could exclude some models for the behaviour of matter at densities higher than that of the atomic nucleus. It is also important because it allows a calculation of theexpectedrateoforbitaldecayduetotheemission of quadrupolar gravitational waves (the sort predicted by GR) of ­(3.4±0.6)â10-14 s/s. This is very important, because asymmetric systems like this (where one of the components has a much largerself-gravitationalenergythantheother)can beusedtoconstrainalternativetheoriesofgravitaNAICAPRPP2007

Figure 3.9.1. Measured radial velocities of the white dwarf companiontoPSRJ1738+0333asafunctionoforbitalphase, from measurements of the Doppler shift of its spectral lines. The blue curve represents the best fit model. The red curve represents the line-of-sight velocity of the pulsar as a function oforbitalphase;theamplitudeofthiscurveisroughly8times smaller(MartenvanKerkwijk).

This calculated period derivative, which is ~60 times smaller than that of the Hulse-Taylor binary, suggests that the orbital period should shorten by ~1 microsecond/yr. After 3 years of timing Paulo findsameasuredvalueof­(4.4±2.9)â10-14s/s.The difference between the predicted and observed values is the smallest ever measured. This in turn introducesthetightestconstraintsyetonthedipolar gravitational wave emission predicted by alternative theories of gravitation. If we interpret the limit on the emission of gravitational waves as a constant "omega" in the Brans-Dicke formulation for gravity, we then obtain w>2300 (s/0.2)2: the previous pulsar limit is w>1300 (s/0.2)2 (the variable s is the change in the binding energy of the neutron star as a function of the gravitational constant G which is not fixed for the Brans-Dicke theory:itispredictedtobeintherange0.1to0.3, depending on the unknown equation of state). However, w is infinite in General Relativity (GR). Hence,Paulo'sresult,whilelessrestrictivethanthe w>40,000 derived from the Cassini spacecraft, is obtained in the strong-field regime, which is the onlyregimethatcanconstrainallalternativetheoriesofgravitation. There is considerable potential for improving this test of GR. Continued timing of PSR J1738+0333 overthenext5(10)yearsshouldincreasethepreci 37


sionofthemeasuredorbitalperiodderivativebya factor of 10(40). If the measured value then conforms to prediction, the uncertainty of the predictionitself(6â10-15s/s)becomesthelimitingfactor intheprecisionofthistest,asthekineticeffectscan beaccuratelycorrectedfrompreciseknowledgeof the proper motion and parallax. We would then achieve an order of magnitude improvement on all previous pulsar limits on dipolar gravitational waveemission,andanticipatealimitofw>15,000 (s/0.2)2. On the other hand, simply by improving our knowledge of the mass ratio through averaging more measurements, and by measuring the orbitaldecaymoreprecisely,weshouldbeableto determine the pulsar and companion masses very accurately, this might be very important for the studyoftheEOS.

tially assigned to protect the deuterium fine-structure line. DI searches at Arecibo are made with some regularity, but by far the primary use of the receiveratthisfrequencyisforpulsartimingobservations. Pulsar timing can be done uniquely well at the Arecibo Observatory because of the unsurpassedsensitivityofthe305-mtelescope.Roughly, the timing precision achievable is proportional to the sensitivity of the telescope being used for the timing. Here, sensitivity depends not just on the collectingareabutalsoonthesystemtemperature

4. Technical Accomplishments and Expectations
Figure 4.1.1. Photo of the new 327-MHz cryogenic receiverwiththecryostatremoved.

InPY2006progressonradioastronomyinstrumentation was made in completing the fabrication of a cryogenic receiver for the 327 MHz band primarily for pulsar timing applications, fabricating a new receiver for the Arecibo planetary radar system,contractswereletfortwonewspectrometers specializedfortheneedsofthePALFAandEALFA surveyconsortiarespectively,andtheIF/LOsystem bandwidth and flexibility were both increased in responsetouserrequirements. Progress in computing and data management (backup,archiving,access)wasfocusedonthedramatically increasing data rate from the telescope thatresultsfrombroaderbandreceiversandsignal processingequipment,andfromthedata-multiplyingeffectsofhavingmultiplesky-positionssampled simultaneouslyasoccursthroughuseoftheALFA multibeam receiver, and through the now-common commensal observing programs. Data managementeffortsarebudget-limitedatNAIC.

and the analyzed bandwidth. Pulsar astronomer users at Arecibo pointed out that still further sensitivity gains were possible if the existing 327-MHz receiverwerereplacedbyanewreceivercryogenically cooled to reduce the receiver temperature, and hence the system temperature, and the front endbandwidthwasincreased.Thesewerethedefiningspecificationsfortheproject,justcompleted inPY2006.

4.1 Radio Astronomy Instrumentation
327-MHz Cryogenic Receiver. Internationally, radioastronomysharesprimaryallocationofanarrowsliceofthespectrumat327-MHzthat wasini38

Figure 4.1.2. Photo of the new 327-MHz cryogenic receiver with the dewar installed for receiver testing in the lab.





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The completed receiver is shown in Figure 4.1.1 with its cryostat removed. It is a dual polarization receiver, linear polarization, that is cooled to 15 K. A filter bank has been installed to reject out-ofbandRFI.Thetotalbandwidthis50MHz.Testson the telescope have demonstrated that the entire bandwidth is usable at Arecibo, a result that arises because other spectrum users of the band that have caused RFI difficulties in the past appear to have moved their applications to other frequency bands. The 327 MHz cryogenic receiver will be in regular scheduledserviceforusersinPY2007.

performance with two new feed horns designed forhighergain,andanewlow-noisereceiver. Twonewfeedhornsweredesigned,carefullyanalyzed and constructed. Each one is optimized to its specific task, receive or transmit. The transmit horn has an edge taper of -15 db which is 2 db lessedgetaperthanthenominalof-17db.Transmit spillover is not an issue. The small amount of lost power on transmit is more than compensated by the increased forward gain that results from a more uniform aperture illumination. The receive horn has an edge taper of -17 db, the nominal value for the Gregorian optics. The receive horn optimizes G/T, balancing increased gain from less edgetaperwithincreasednoisetemperaturefrom morespillover.Theinputmatchofbothhornswas modeledandthenmeasuredasbetterthan-35db overa100MHzbandwidth.Thetransmithornwas tested and installed on the telescope in PY2006; it isperformingasdesigned. The new receiver is in its final stages of assembly. Allthecomponentsubassemblieshavebeenfabricated, assembled and tested. Photos are included hereasfigures4.1.3and4.1.4. The receiver is intended to have a receiver noise temperature of less than 5K. This will be achieved inpartbyplacingtheorthomodetransducer(OMT) in the dewar cooled to 16K. The present receiver has a turnstile junction at room temperature with associatedlossywaveguideruns.Thenewreceiver willonlyhaveashortrunofroundwaveguidefrom the horn leading directly to the cryogenic stages inthedewar. The new receiver has amplifiers utilizing InP transistors yielding an amplifier noise temperature of less than 2K. The amplifiers are an existing, advanced, Figure 4.1.4. Completed cryogenic design from the dewar for the planetary radar receivmicrowave de- er.
39

Planetary Radar Receiver.Theexistingreceiver andfeedhornsfortheplanetaryradarsystemwere constructed in the mid 1990's during the Arecibo Gregorian Upgrade. The receiver was built out of existing parts from the line feed system and other surplusequipment.Thefeedhornsforbothreceive andtransmitareidenticalandweredesigned,built

Figure 4.1.3.Planetaryradarreceiverunderassembly.

andinstalledwithoutextensiveanalysisoranypattern testing. It has become evident from observationsandmicrowavemodelingthatthefeedhorns have too much edge taper, about -20 db. at the edge of the tertiary. This under-illumination reducesthegainofthesystemonbothtransmitand receive.AsthescientificusersoftheS-bandplanetaryradarsystemseektoobservesmallerandmore distantobjectsincludingasteroidsandthesatellites ofSaturnandMars,highertelescopegainandthe greatersensitivityachievablewithalowernoisereceiver is required. The planetary radar system upgrade project was initiated to optimize the system
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velopment laboratory at Chalmers UniversityinSweden.Themeasured performance of the amplifiers meets specifications(seeFig.4.1.5) The OMT has a septum polarizer whichdirectlyyieldscircularpolarizations.Thepresentturnstilehasabout -30dbofdiscriminationbetweenRCP and LCP. The new septum OMT has apredictedperformanceof-33db.at band center. The round waveguide componentsthatmakethetransition from the feed horn to the 16K cryogenic stage are all completed and tested. Figure4.1.6showsthecurrentstatus of the S-band radar receiver assembly.Thereceiverwillbetestedonthe telescopeinthesummerof2007and available for visitor use immediately Figure 4.1.5.MeasuredperformanceoftheChalmersInP-basedLNAsthatare thereafter.
beingusedinthenewplanetaryradarreceiver.

vatoryIFandLOsystemshavetobecontinuallyexpanded. Presently, the fundamental mixing from RF to IF at Arecibo happens at the receiver; the IF is then brought down to the control room via optical fiber for further processing. Plans are being developed to make use of the rapidly expanding A/D capabilities of commercial hardware, and the declining costs of this hardware and optical fiber transmitters and receivers, to sample the RF at the receiver, bring the RF down to the control room and do all subsequent RF processing in the control room. This has many advantages including that of eliminating the need to maintain IF instrumentation on the telescope platform, there is an importantweightsavingsontheplatform,andthe convenienceoflocatingallsignalprocessingforall receivers in a single, climate-controlled, room. In PY2007 these plans will be further developed. No hardwarepurchasesareplannedinPY2007.
Figure 4.1.6. Assembly of the S-band radar receiver.

4.2 IF/LO System
The continuing interest of telescope users in analyzingwiderbandwidthsformanyscienceapplications has meant that the capabilities of the Obser40

The capabilities to process still more IF/LO signals in the control room were expanded significantly in PY2006 in anticipation of the need to support twonewspectrometersinPY2007.Specifically,the IF/LOcapabilitieswereaugmentedtoatotalof16 channels.Thesechannelsmaybedividedasneeded,butthedrivingrequirementwastosupportthe
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for user observations in PY2005.Ithasrunwithoutafaultfornearlytwo years.Constructionwas done under NAIC contract at the University of California, Berkeley, Space Sciences Laboratorybythegroupledby Dr.DanWerthimer. The two new spectrometers are designed for the applications of the PALFA and EALFA consortium groups respectively. The technical requirements for the instruments were established in meetings among the Arecibo technical staff, the AreFigure 4.2.1.IF/LOracksinthetelescopecontrolroomattheAreciboObservatory. cibo scientific staff and 7 ALFA dual-polarization beams with two spares. representatives of the PALFA and EALFA consorInaddition,hardwarewasinstalledtoenableasintia. The fundamental spectrometer specifications gle-pixelbeamtobeprocessedforspectroscopyat aregivenintheTable. 800-MHzbandwidth. The spectrometer project is a contract arrange4.3 Backends mentbetweenNAICandJeffMock.Thedivisionof responsibilitiesisthis: PALFA and EALFA Spectrometers. The primary motivation for the ALFA multibeam receiver · Mock delivers to Arecibo FPGA based is to facilitate large-scale surveys of the sky. Major hardware sufficient to process16 simullegacy surveys with three distinct scientific objectaneous IF signals. This includes the IF tivesareplannedbyconsortiaoftelescopeusers:a sampler, Xilinx processor, control firmsurveyofgalacticHI(GALFA),apulsarsurvey(PALware,GbitEthernetinterface. FA) and a survey of the local, z<0.2, extragalactic sky (EALFA). The signal processing requirements of these three consortia are sufficiently different that NAIC agreed to provide separate backends foreachconsortium.Thisgivesanopportunityfor the three groups to observe simultaneously: with the receiver IF split and sent separately to each of the three spectrometers, the three surveys can be conducted at the same time without any one surveyinterferingwiththeothers.Werefertothisas "commensal"observing. ThefirstofthethreeALFAspectrometers,theGALFAspectrometer,wasbuiltandinstalledinPY2004; it was commissioned and put into routine service
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Figure 4.3.1. Demonstration units for the PALFA and EALFAspectrometerhardwareatArecibofortesting,January2007.









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Table 4.3.1 P-ALFA and E-ALFA Basic Spectrometer Specifications
P-ALFA (Include GALFACTS) 7-beams,2-pols/beam 14IFsignalsnominallycovering100400MHz 14channelIFtoquadraturebasebandconverter Four12-bit300MHzADCs(2pols, basebanddata,IandQinputs) Sub-bandingin100MHz,orsmaller, bandstocoverthe300MHz Flexibilityforsteeringthesub-bands Selectablenumber(256,512,1024, 2048)spectralchannelsover300 MHzperpolarization Outputbits,12 Selectabletimesampling(16µsec, 32µsec,64µsec);1msecforGALFACTS CrossproductsforGALFACTSor polarizationsummingforpulsars Externalclockandsync Spectralnormalization Externalwinkingcal Capabilityforreprogrammablepolyphasefiltershapesshouldnotbe excluded ComputationsdoneinPCwhenever possible E-ALFA 7-beams,2-pols/beam 14IFsignalsnominallycovering100400MHz 14channelIFtoquadraturebasebandconverter Four12-bit200MHzADCs(2pols, basebanddata,IandQinputs) Sub-bandingin100MHz,orsmaller, bandstocoverthe200MHz Flexibilityforsteeringthesub-bands 8192spectralchannelsover 200MHzperpolarization Outputbits,12 ~3msectimesamplingforRFIexcision--fixed,notselectable CrossproductsforRFIIdentification Externalclockandsync Capabilityforradarblanking

Analog Input

Sampling

Outputs

Desirable Options

· NAIC is responsible for the 300 MHz bandwidthIFsplitin2bands,I&Qbasebandsignals,theclockandLOdistribution,andthenecessaryhigh-speeddata storage and data archive. This includes anynecessarycomputeservers. Mock delivered demonstration hardware to the ObservatoryinJanuary2007fortesting.Thetests revealed no major deficiencies. The project continuesontowarditsplannedoperationalreadiness dateofJune2007.

PY2007 the new spectrometers will cause this figuretoincreasebyatleastafactorofbetweenthree andten.Inpreparation,weareplanningoninstallingmuchlargercapacityRAIDvolumestosupport theongoingobservingprogramsandatape-based systemforlonger-termstorage. The Arecibo Observatory has no ambition to becomeacomputationaldatacenterthathostsdatasetstobeaccessedbyexternalusers.Recognizing that the needs of the astronomical community in the U.S. include access to data products from Arecibo, NAIC is making arrangements with the CornellTheoryCentertohosttheArecibodataandto serve the community of database users in accessingthesedatathroughtheVOprotocol.

4.4 Computing: Storage and Networking
In PY2006 the science data taken at the telescope andrecordedforarchivalstorageorbackupatthe Observatoryamountedtomorethan80TBytes,just fortheastronomyprogram.Wecanexpectthatin
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5. NAIC Education and Outreach Programs
5.1 Angel Ramos Visitor Center
Summary. Thisreportcoverstheperiodbetween July 1, 2005 and June 30, 2006. As in previous years,theVisitorCenterhostedmanyspecialevents for the general public and for the NAIC/Arecibo Observatory community in general. These included the NAIC/NRAO Single Dish Summer School, Geoscience Workshop, the Gordon Lecture, and other scientific and educational workshops. We updated 15 displays at the Visitor Center and are intheprocessofupdatingandaddingnewpanels. Three educational workshops were offered (two for teachers and one for journalists) on the issue of pseudoscience, and we hosted an astronomy summer camp for 25 middle school students. The number of visitors to the Arecibo Observatory declinedby9%andwehavetakenseveralmeasures tomaketheoperationmoreefficient. General Public. A trend that began in PY2005 reflecting an annual decrease in the number of visitorstotheAreciboObservatoryisalsoreflected in the figures for PY2006. The number of visitors to the facility in PY2006 was 99,496 as compared to109,108inPY2005.This9%decreaseisseenin both the general public, and the school children visitingA.O.Butthemainreasonaffectingtheflow ofvisitorsinPY2006wasthedropinthenumberof school groups visits. This issue is discussed in the nextsection. ThePuertoRicoHotel and Tourismindustryisalso reporting a 10% decrease in room occupancy for this period. Many businesses in Puerto Rico have

been affected by the lack of economy growth in theregion.

School Groups. The school visits program allows school groups, from both public and private institutions, to visit by appointment the Arecibo Observatory and tour its Angel Ramos Foundation Visitor Center. In PY2006, 350 school groups touredtheAreciboObservatory.Ascomparedto thepreviousyear,inPY2005therewasa21%decreaseinthenumberofschoolgroupsvisitingAO, andthisaccountsforabout8,000fewervisitors.In additiontotheschoolgroupsvisits,alargenumber ofadditionalgroupsarealsoscheduledeveryyear. These include university, industry, government, boy scouts, and other community organizations. InPY2006wehosted53specialgroups.

Scheduled Group Visits to the Arecibo Observatory 2000-2006
PY 2000 2001 2002 2003 2004 2005 2006 School Groups 515 548 532 563 525 444 350 Special Groups 77 128 84 102 125 66 53 Total Groups 592 676 616 665 650 516 403 No. of Visitors 29,234 36,544 34,446 35,838 31,896 28,546 20,439

ThegovernmentofPuertoRicohadalargebudget deficit in PY06. This problem forced many agencies, in particular de Department of Education, to either close or limit their activities. Many schools (andsummercamps)hadtocanceltheirscheduled visitstoAOduetolackoffunds.

Conferences and Special Events. During the year,weofferedanumberofspeciallectures,tours and workshops to schools, universities, and the community. We provided five (one-day session) workshops for science teachers, two for pre-service teachers, and three for high school students. In addition, we hosted a two-week summer workshop as part of the Arecibo Geoscience Diversity Project.
The Visitor Center also hosted a number of scientificmeetingsduringtheyear.Theseincludedthe NAIC/NRAO Single Dish Summer School, the Arecibo Conjugate Workshop, and the Gordon Lecture.

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From Arecibo to the Universe Summer Camp (UPR, NSF, Math-Science Partnerships). DuringtheweekofJune11to16,theAreciboObservatory hosted the residential summer camp "From Arecibo to the Universe" for 24 middle school students from participating ALACIMA schools. All participants completed the program successfully. As part of the summer camp activities, students had the opportunity to tour the Arecibo Observatory and meet scientists, engineers, and technical staff.Throughthese interactions, participants were able to enrich their experience and learn about professional careers.

sion by our summer camp staff and a professional lifeguard,participantsenjoyedourswimmingpool andbasketball/volleyballfacilities.

Pseudoscience Workshops (NASA-PR Space Grant). Inanefforttoimprovethelevelofscience literacy on the Island, a series of workshops were offeredonthetopicofpseudoscience.Thepresentationofpseudoscientifictopicsinthemedia(radio, TV, press, web) appears to be increasing. Topics include: UFO's, astrology, magnetic healing, and many others. Pseudoscientific ideas are many times presented as "scientific knowledge" and this creates a serious confusion in the general public; particularlyinstudents,teachersandjournalists.
We offered two residential workshops (3 days each) for science teachers and two workshops (1 day each) for journalists. Each session allowed participants to establish the difference between science and pseudoscience, and to identify the basic elements that are common to pseudoscientificideas.

From Arecibo to the Universe was designed as an introductory astronomy workshop developed through hands-on activities on the solar system, stars, galaxies, and the universe. Participants learned to use an optical telescope and performed astronomical observations on Saturn, Jupiter, and the Sun. In addition, they learned to identify the summer constellations and the names ofthebrighteststars. The program included a dedicated period of 2 hrs each day for recreation. Under constant supervi-

Arecibo Geoscience Diversity Project (NSF Geoscience Diversity Program). The third

Educational Workshops Offered at AO in PY2006
Date Oct12-14,'05 Nov30,`05 Jan9,`06 Feb24,`06 Mar3,`06 Mar18-19,`06 Mar22-25,`06 June11-16,`06 44 Time PseudoscienceWorkshop StellarEvolution SpaceWeather ScaleModelsin Astronomy Telescopes Pseudoscienceforthe Press PseudoscienceWorkshop FromArecibotothe UniverseSummerCamp No. of Participants 25teachers 30HSstudents 40teachers 25undergrads 20BoyScouts 15reporters 25teachers 25 middle school students Institution NASASpaceGrant VegaBajaSchool NASA/UPRMayagÝez UPRRioPiedras Troop261,Capitan Correa NASASpaceGrant NASASpaceGrant UPR(NSF-MSP) NAICAPRPP2007


Invited Lectures at AO in PY2006
Date July28,`05 Nov5,`05 Dec5,`05 Dec6,`05 Dec8,`05 Jan27,`06 Feb7,`06 Feb22,`06 Apr5,`06 Apr20,`06 Title RadioAstronomy Universe AreciboObservatory AreciboObservatory Universe SolarSystem Universe Universe HistoryofAstronomy SETI No. of Participants 60undergrads 300teachers 20 60 30students 30students 150students 45students 60undergrads 150HSstudents Institution UPRMayagÝez MSPTeacher Conference,SanJuan JobCorps,Isabela SanFelipeSchool CamuySchool LuisF.PerezSchool LaMilagrosaSchool Academia Discipulos de Cristo (VegaBaja) InteramericanUniv.,Bayamon InteramericanUniv.,Ponce

year of our NSF sponsored Geoscience Diversity program went very well. Students and teachers from four schools and 8 undergraduates from the UPRparticipatedintheprogram.Thisyearwehad participation from the Domingo Aponte Collazo School in Lares, Ferando Callejo School in Manati, the Esther Feliciano Mendoza School in Aguadilla, and the Enrique Borras School in Arecibo. Each schoolprovidedateamof5studentsandascience teacher. Two schools (Lares and Manati) worked with the UPR on a research program at the Cano Tiburones wetland. Here they measured water quality and identified bacteria in aquatic plants known to absorb metal ions. The Aguadilla and Arecibo schools worked at the Arecibo Observatory comparing different galaxy populations using datacollectedbytheALFALFAsurvey.Participants presented their research projects at the Arecibo Geoscience Congress, held at the Arecibo Obser-

vatoryonApril29,2006.

Jazz Band in AO.OnMarch31,2006,wehosted the school band from Xavier Highs School in New York for a special presentation to our staff. Many employeescametoenjoythispresentationoffered duringthelunchhourattheAOgazebo. Bring your Child to Work Day. TheVisitorCenterhosteda1-hourworkshopforAOstaffchildren as part of the "Bring your Child to Work Day". A general overview about AO was provided as well asahands-oncoloringbookactivityabouttheradiotelescope. Financial Report. In this section a summary of the financial activities associated with the operationoftheAngelRamosFoundationVisitorCenter is presented. The VC operating budget is com-

Scientific Meetings Offered at AO in PY2006
Date July10-16,`05 Feb14-16,`06 Feb27,`06 Mar8-9,`06 Apr2,`06 Apr17-19,`06 Apr29,`06 June27,`06 Title SingleDish SummerSchool NAICVCMeeting MicrowaveRadiometry AUSACMeeting NationalWeatherServiceMeeting AreciboConjugateWorkshop GeoscienceCongress WillianGordonLecture No. of Participants 50 50 40 50 30 50 60 80 Institution NAIC/NRAO NAIC UPR NAIC NWS-NOAA NAIC/NSF NAIC Cornell

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Special Visits and Events at AO in PY2006
Date Sept9,`05 Oct4,`05 Nov23,`05 Dec15,`05 Jan23-27,`06 Jan25,`06 Jan27,`06 Feb1,`06 Mar12,`06 Mar14,`06 Mar31,`06 Apr27,`06 Title Novo-NordiPharmaceuticalMeeting WorkersCompTraining Bristol-MyersTour AMGENMeeting&Tour CornellHRTraining TelescopePaintingProjectMeeting NSFDirectorVisit&Tour MedtronicMeeting FordhamUniversity PhilipsAcademy,Massachusetts XavierHighSchool(JazzBand) BringYourChildtoWorkDay No. of Participants 15 75 5 12 20 50 5 25 12 100 50 20

prisedbytheincomeobtainedthroughadmissions and store sales, and the operating expenses due to personnel, maintenance, and inventory. Salaries and wages account for 48 % of the operating costs, store merchandize and vending supplies for 34%, and the remaining operating costs for 18%.InPY2006,theVisitorCenterhadrevenues for$839,539,andoperatingexpensesof$796,932 foranetincomeof$42,603.

Plan of Action. On November 1, 2005 we increasedthecostofadmissiontotheVisitorCenter by$1.00.Thisactionwasnecessarygiventheimpactofhighgaspricesonouroperatingcosts.The new fee contributed about $50,000 in revenues forPY06.Wehavealsoreducedtonumberofparttimeemployees,andareintheprocessofbuilding a coffee shopthat will providea newsource ofincome.

5.2 2006 REU Program
The Arecibo Observatory organized its 2006 REU summer student program for 10 weeks from the end of May to mid August. This program exposes studentstovariousactivitieswiththeaimofmotivating them to pursue their future career in research. Theselectionprocessishighlycompetitivewith11 studentsgettingselectedfromdifferentuniversities outofnearly115applicants.Theseelevenstudents werefundedfromdifferentsources,(a)eightwere supported by the NSF REU grant, (b) two recent graduatessupportedbyNAIC,and(c)onewasselected on the basis of the Observatory Director's discretion. In addition, three students from UPRMayagÝez(UPR-M)workedattheObservatoryand
46

were funded by the Partnership for Space Science Education and Research (PaSSER) program, and one was supported by `FundaciÑn Comunitaria de Puerto Rico' and worked on a project related to education and outreach activity to promote science for the disabled. Apart from this, there were twograduatestudentsfromtheUniversityofColorado (CU) supported by Colorado Research Associates (CoRA), working with their Ph.D. supervisor Dr. Diego Janches (CoRA), who used the facilities at the Observatory for their research work. These students, Amal Chandran and Jonathan Fentzke, participatedintheREUactivitiesandalsogave20minute presentations towards the end of the program.Oneofthehighlightsofthisyear'sprogram was the participation of students from U.S. universities, and two from outside the U.S. One student (SoniaBuckley)attendscollegeintheU.K.andone (Ximena FernÀndez) is originally from Colombia, whichallowedstudentsfromdiversebackgrounds tointeract. ProfessorsJulioUrbina(PennStateUniversity)and JosÈ Rosado (UPR-M) visited the Observatory this summer and mentored a few REU students. Also, Prof. Carmen Pantoja (UPR Rio Piedras -- UPR-RP) andherstudentspentamonthworkingattheObservatory's àngel Ramos Visitor Center to develop techniquesforpromotingscienceamongthevision and hearing impaired. Several Observatory staff members gave lectures to the students with the objectiveofintroducingthemtothefundamentals and applications of the various instruments available on site. The talks included a variety of topics covering areas related to astronomy, ionospheric
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science,planetaryradar,andelectronicswithfocus onthecurrentresearchactivitiesusingthefacilities at the Observatory. This was complemented with avisittothe500-fthighplatformthatcontainsseveral receivers. The engineers and technical staff showed them the 430 MHz transmitters, which was beneficial to the engineering students. A very distinguished visitor, Dr. Jocelyn Bell, was invited totheObservatoryasthe2006WilliamE.andElva F.GordonDistinguishedLecturer.Duringhervisit, she gave a popular lecture on "Reflections on the Discovery of Pulsars" on 27 June 2006. A get-togetherwasarrangedthatallowedfemalescientists and students to interact with her and gave them anexcellentopportunitytodiscussissuesrelatedto womeninscience.Also,severalvisitorstotheObservatorygavetalksthatwereattendedbytheREU students. This list includes: D. Campbell, P. Taylor, Eliana Nossa (all Cornell), X. Chu (CU), G. CortÈs (NAIC, Cornell), D. Werthimer (UC Berkeley), and J.C.Morales(UniversityofTurabo). The research experience for REU students comprisedamandatoryproject(individual)andanoptional project (group of 3 to 4 students) as a part ofahands-onexperiment.Themandatoryproject involvedeitherrealtimeobservationsorpreviously obtained data and their analysis/interpretation. Those who wanted to obtain experience on the procedures related to observing were offered participation in hands-on experiments that were conducted by Arecibo staff members Mayra LebrÑn, Chris Salter and Tapasi Ghosh. Three runs were scheduled that provided students an excellent opportunity to get their `hands dirty'. A summary of the hands-on experiments is provided later in this document. Thestudentswereaskedtogive20-minutepresentations summarizing the project they worked on during their stay at the Observatory. Some of the studentswillpresenttheirworkinmeetings/conferences. The aeronomy students plan to participate intheCEDAR(Coupling,EnergeticsandDynamics of Atmospheric Regions) meeting in June 2007. Similarly,theastronomystudentswillpresentposters at the meetings of the American Astronomical Society in October 2006 and January 2007. It is worthmentioningthatoneofthestudents(Ms.X. FernÀndez)whoworkedwithT.Ghosh,C.S.Salter and E. Momijan discovered a new galaxy and has expressedherinterest in participating in follow-up work and to pursue astronomy as her future career.
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Thereisafamoussayingthat`Allworkandnoplay makesJackadullboy'.Tomakesurethatstudents got a chance to experience life outside the Observatory, a variety of activities were arranged that gave them an opportunity to explore the culture and nature of the Caribbean island. Many thanks to all the administrative staff, especially MarÌa-Judith RodrÌguez, Lucy LÑpez, Wilson Arias, Carmen Segarra, Carmen Torres, Eva Robles, JosÈ Cordero, and all the drivers for their cooperation and time. As a welcome to students, a BBQ was organized near the recreational area. We encouraged studentstogiveusfeedbackabouttheirinterestsand tried to organize events accordingly. Some students became certified for scuba diving and then visited places like the Mona and Vieques Islands thatarefamousfortheirbeautifulbeachesandsea life. This gave them a chance to camp, hike and snorkel in different locations. The students spent a weekend camping in the El Yunque Rain Forest. Also, a cultural trip to Old San Juan was arranged thatwascoupledwithavisittotheBacardÌfactory thatisfamousformanufacturingthemostpopular rumintheworld.Therewasaneducationaltripto the Institute of Tropical Ecosystem Studies located in the Rain Forest, which also hosts REU students andiscoordinatedbyDr.AlonsoRamÌrez.Thiswas later reciprocated by a visit to the Observatory by the Rain Forest REU students. A trip to a cultural festivalinthenearbytownofHatillowasorganized that exposed students to the local music, dance and food. On many occasions, students were accompanied by staff members (P. Freire, J. Wiig, P. Farias, and H. Vo), who followed along to several beachesandotherscenicspots.Wealsotookthem out to the cinema and dance establishments. Towardtheendofthesummer,anotherBBQwasarranged to welcome the Rain Forest REU students and also to give a farewell to our own students. The two groups played volleyball and exchanged their experiences. On several occasions, the studentsorganizedeveningget-togethersattheVSQ andinvitedstaffmembersandvice-versa.

2006 Summer Student Projects.
·SupportedbyNSFREUFunds:

Heidi Brooks is currently a senior at Reed College. AsanREUstudent,sheworkedwithDr.EllenHowellandstudiedtheorbitsofbinaryasteroidsinthe near-earth population as a means for obtaining measurements of their densities. She worked primarily with radar-obtained delay Doppler images
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of 2003 YT1, 2002 BM26, and 2006 GY2. She recordedtherangeseparationoftheprimaryandsecondaryasteroidsatvarioustimeintervals,aswellas their respective bandwidths. The values obtained forrangeseparationwereplottedversustimeand fitted to sine curves, as would result from the (assumed) circular orbits of the secondaries. They were found to exhibit the following periods: 2003 YT1,36.7±1.8hours;2002BM26,either12.5±0.2 or25.8±0.3;and2006GY2,11.7±0.2hours.AdditionaldataforYT1,alongwiththeuseofamodelingprogramcalledShapeallowedconstraintsto be placed on the geometry of the system. From these inputs, Heidi was able to calculate the mass and volume of the primary to be (1.27±0.39)â1012 kgand0.63±0.10km3,respectively,resultinginafinalestimateofthedensitytobe2.01±0.70g/cm3.

SoniaBuckleyisafirst-yearundergraduatestudent at Trinity College Dublin, Ireland, studying Natural Sciences. She worked with Johannes Wiig to calibrate the Pennsylvania State University all-sky imager.Theall-skyimagerisasensitivedigitalcamera that collects images of the entire night sky for the purpose of studying airglow events. Sonia's project involved the intensity calibration and flat-fielding of the imager. To do this, many images had to betakenofalightsourceofknownintensityunder different conditions. The imager was dismounted from its position in the airglow laboratory and set up underneath a C14 calibration source. The calibration data was collected over the course of several nights to avoid light contamination. Sonia then used IDL to analyze these results and carry out the calibration. The program doframe. pro for automatically flat-fielding and converting pixelcountstointensityvaluesofanyimagetaken with the camera was created using the results of the calibration. All the results and IDL programs will be posted on the web at http://allsky.ee.psu. edualongwiththeimagestakeneverynightwith the all-sky imager so that anyone can access the data. This means that the calibration data will be usedwhenstudyingtheimagestoobtainmoreaccurate,understandableimages. KnicoleColÑnisaseniorattheCollegeofNewJersey. She worked with Dr. Mayra LebrÑn on reducing and analyzing the 18 cm (1665, 1667, 1612, and1720MHz),6cm(4765,4751,and4660MHz) and 5 cm (6031, 6035, 6049, and 6017 MHz) OH lines,aswellasthe4830MHzH2COandthe6668 MHz CH3OH lines, all arising in the massive starforming region IRAS 19111+1048. All lines were
48

observedonJuly4-5,2005usingtheAreciboTelescope L-band, C-band and C-high receivers. The analysis was completed using Arecibo routines for reducing correlator data. Maser emission was confirmedinthe1665,1667,6031,and6035MHz OH lines, and each maser line was accompanied byanabsorptionfeature.Bycomparisonwithprevious studies, all but the 6031 MHz line appear to be highly variable. The 6 cm OH lines, the 18 cm (ground-state)and5cm(excited-state)OHsatellite lines,andtheabsorptionfeaturesinthefourmasing lines were found to exhibit weak and broad spectralprofileslocatedatvelocitiesslightlyhigherthan thatofthesource,indicatingthattheirappearance may be due to a form of quasi-thermal excitation rather than the masing process. Currently there is no evidence for either H2O or CH3OH masers, but massiveCOoutflowshavebeendetectedthrough previous studies. Along with the detection of OH masers,thesepropertiesplaceIRAS19111+1048in a late stage of protostellar evolution in which the HII region has expanded and developed enough toallowforconditionsthatareunabletogenerate H2O or CH3OH masers. As a separate result, the near and far kinematical distances to this source were determined to be, respectively, 4.4 and 7.6 kpc.

Kevin Graf is a senior at Cornell University and worked with Ganesh Rajagopalan. His work focused on the C-High Receiver at the Observatory that is mostly used for 6.7 GHz Methanol Maser line surveys. However, there is interest in upgrading the receiver to a dual-beam receiver for continuum observations. The receiver possesses two feed horns and two front-end receiver chains. The planned implementation of Dicke-switching at rates of approximately 10 Hz following the dewarshouldnullifythe1/f-noisefromfluctuating atmospheric emissions. The type WBA13 MMIC amplifiers used at the C-High Receiver front-end, however, possess Heterojunction-FETs, which are known for 1/f-noise that can limit the sensitivity of continuum observations. Using the test setups assembled and verified this summer, the stability of the type WBA13 MMIC amplifiers, as well as of the C-High Receiver as a whole, will be characterized.TheAllanVarianceofthesamplesshouldofferrecommendedintegrationtimesandswitching rates. These results should guide the process of the dual-beam upgrade as well as provide useful information to observers who use the receiver for continuumobservations.
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Heather Hanson is a senior at the University of Wyoming. She worked with Dr. Mike Nolan and her project focused on the asteroid 105 Artemis, whichisaC-typemain-belt asteroidthathasbeenobservedtocontainhydrated minerals on at least a portionofitssurface.Seventyfive percent of all asteroids belong to the C-type classification.Theseasteroids are often observed to have absorption bands near0.7micronsand3.0microns.The0.7-micron absorption feature indicates the presence of iron bearingphyllosilicatesthatarerelatedtohydrated minerals,whilethebroad3.0micronabsorptionis causedbyoverlappingabsorptionbandsfromH2O andOHlayersinhydratedminerals.Oftenthe0.7micronbandisnotobservedbuthydratedminerals are present and absorption at 3.0 microns is seen. To further understand the link between the absence and/or presence of the different bands, radardatafromtheAreciboObservatoryandspectra from the IRTF on Mauna Kea have been obtained foranumberofasteroids.Manyoftheradardata showirregular,non-symmetricbrightfeaturesthat maybelinkedtothereflectivityofthesurface,and therefore the composition instead of the shape of theasteroid.Bothradarobservationsandnear-infrared spectra of 105 Artemis have been obtained andanalyzed.Heathercoordinatedtheradarand spectral data using lightcurve data obtained from the amateur astronomy community. Through a modeling program called Shape, these data were usedtomakeasimplified3Dmodelof105Artemis in order to map the areas where hydrated minerals have been observed. Once mapped, the link between the hydrated minerals and radar-bright areascanbetested. Clinton Mielke is a senior at the University of Arizona,Tucson.HeworkedwithDr.PauloFreirethis summer,theresidentpulsarexpert.Paulogavehim the choice between two projects to work on, and steppinguptothechallenge,hedecidedtoundertake both. First, he worked on a numerical simulation of a particular binary pulsar system. By using the4thorderRungeKuttaalgorithm,hetestedthe general relativistic perturbation on the pulsar's orbit, and found a precession of the periastron over
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a specific timescale that agreed with theoretical models. Unfortunately, the amount of drift has beenfoundtobetoosmalltoobserve,soalthough his code worked well, the binary system is not a strongcandidatefortestingGeneralRelativity. On his second project, Clinton wrote an orbital fitting program that uses the Levenberg-Marquardt methodtoperformaleastsquaresfit.Whengiven an input file of epochs and periods, the algorithm findsKeplerianorbitalelementsandafewadditionalparametersfortheparticularsysteminquestion. Thisprogramwilllikelybecomeavaluabletoolfor astronomers in the pulsar community, as no open source alternative seems to exist for this particular application.Hewillbecoordinatinghiseffortswith Paulo over the upcoming few months to modify this application and bring it into use amongst all whoneedit.

IsobelOjalvoisaseniorstudentatRensselaerPolytechnic Institute in Troy, NY studying physics and mathematics.HerREUsummerprojectsupervisors wereDrs.StevenGibsonandRobertMinchin.Her REU project was to determine what is needed to put data obtained from the Arecibo L-Band Feed Array (ALFA) onto the Virtual Observatory (VO) and to implement a preliminary database and website. The VO is an international collaboration tomakelargeastronomicalsurveysavailabletothe public with a suite of search and intercomparison tools. Isobel's focus was on the VO interface for ALFA surveys of the Galactic interstellar medium (GALFA) and HI environments around other galaxies (AGES), both of which are generating large, 3-dimensional data sets. She used the scripting language Perl as a common gateway interface to access the data and investigated how to provide
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a web-interface that will allow users outside the Observatory to extract subsets of the data via the WorldWideWeb.

Daniel Rucker is a fourth-year undergraduate student at University of Arkansas at Little Rock, majoring in Systems Engineering. He worked under the supervision of Prof. Julio Urbina and Ryan Seal on the development and implementation of an FPGA-based radar controller for the Space and Atmospheric Sciences Group at the Arecibo Observatory. This device will be integrated with the recently developed multi-channel digital receiver acquisition system to conduct radar observations. The radar controller will provide up to 16 control signals: sample start trigger to the receiver board, T/R switching, RF pulse, blanking, coding, etc. It will also control two 8-bit digital-to-analog converters (DACs) for multi-frequency signal generation. The device is an external module that is programmedviatheUSB2.0portandoffersatotalof 50I/Opins.Configurationandoperationofthedevice is achieved with a general-purpose computer throughagraphicalinterfaceunderLinuxOS.
·SupportedbyNAICfunds:

ingcouldexistinamonitoringmodethatdoesnot require a runtime engine. Both methods were implementedandareavailable.TheJavaclient/server pairwasalsoimplemented.Javawouldnotrequire a runtime engine and offers a high refresh rate, at thecostofmoredifficultimplementationandmore difficult futureupgrades and modifications. Given a stable Java client/server pair, the Java version would be better for scientists who won't have the LabVIEWruntimeengine.

DavidBowengraduatedfromCornellUniversity inMay2006.ThissummerheworkedwithGanesh Rajagopalanonaprojectrelatedtosignalinterference.Broadbandsignalinformationisvitaltoidentifying and diagnosing signal interference in radio astronomy and radar experiments at the Arecibo Observatory. Previously, data available remotely hasbeenband-limitedandhasnotrevealedeffects of system problems and RFI from sources such as lightning.Datafromaninstrumentcapableofdisplayingthebroadbandsignalneedstobeavailable to remote users at the time of their experiments. These remote users include engineers in their homes in the Arecibo area as well as scientists in arbitrarylocationsaroundtheworld.
Using an Agilent E4403B ESA-L series spectrum analyzer, broadband signal information must be made available. Since the data must reach potentiallyaroundtheworld,thedatamustbeavailable throughaninternetgateway,orwebserver.Two solutions were implemented: LabVIEW programs using the web publishing utility and a Java client/ serverprogrampair.LabVIEWwasmoreeasilyimplemented,butrequiredtheoverheadofaruntime engine to be interactive (called embedded mode). At the cost of refresh rate, LabVIEW web publish50

MarÌa Ximena FernÀndez is a senior currently enrolled in a dual degree program, where she studies Physics and Astronomy at Vassar College and EngineeringSciencesatDartmouthCollege.Atthe Observatory, she worked with Drs. Tapasi Ghosh, Emmanuel Momjian, and Chris Salter analyzing HI 21cmandOH18cmspectrallineobservationsofa groupof luminousinfraredgalaxies (LIRGs). These galaxiesemitmostoftheirenergyatinfraredwavelengths and are found in interacting/merging systems. The intense infrared luminosity (Lir>1011Lo) is due to the dust heating from extreme starburst and/or active galactic nuclei energy sources. In 2004, Arecibo observations were made using the L-Band Wide receiver of 85 LIRGs from the 2 Jy IRAS-NVSS sample. The sample was observed with ON/OFF or double position switching (DPS) modes, depending on the radio continuum flux density of the target sources, and the data were reduced with IDL. The team detected HI in 82 galaxies (16 new detections), and OH in 7 galaxies (5 new detections). In some cases, the HI spectra showed the classic Gaussian or double horn distributions, while the majority exhibited distorted features indicating that they are in an interacting/ merging system. IRAS 23327+2913 is considered tobethemostintriguingsourceinthesample.This ultra-luminousinfraredgalaxy(ULIRG,Lir>1012Lo), which is described in the literature as a pair of nucleiinthebeginningstagesofinteraction,wasdetectedinbothneutralhydrogenandOHmegamaseremissionfromthesystem,whichhadnotbeen reportedbefore. Brandon Taylor graduated from the University of TexasatAustinthispastMaywithadegreeinElectricalEngineering.Whilethere,heworkedinionosphericresearchattheAppliedResearchLaboratories. Prior to coming to the Arecibo Observatory, he also spent a summer as an REU student at the MITHaystackObservatory.
This summer, he worked with Dr. Hien Vo on a
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project to statistically analyze Subauroral Polarization Streams(SAPS). SAPS,which can bedetected by elevated ion drifts equatorward of the auroral oval, are associated with disturbed ionospheric conditions.Abetterunderstandingoftheseevents canimproveionosphericmodelsandreduceerrors inGPSandothersatellitecommunications. Brandon'sprojectwasaimedatexploitingthecontinuous data collection of DMSP satellites to provide a better statistical analysis of SAPS than had previously been performed. He developed an algorithmtoautomatically processayear'sworthof satellite data and to detect and quantify high ion driftsasSAPS.AdditionalcodewaswrittentocomparevariouspropertiesoftheseSAPSinavarietyof geomagneticconditions.Inadditiontotheresults achievedthissummer,theprojectwillbeextended byDr.Vo. ·SupportedbyPaSSERfunds:

ments of the temperature and potassium content in the mesosphere during the daytime, utilizing LiDAR technology. The test bed is composed of a tunable single-mode external cavity diode laser, the filter, a potassium vapor cell in an oven with fluorescence detection, and a Fabry-Perot etalon. Theovenandcontrollercircuit,constructedduring the summer of 2005, heat a potassium spectrum cell, and we use the laser to excite fluorescence in a "Doppler-free" configuration. Since the emission linesofthepotassiumarewellknown,itispossible to use the system to tune the laser and obtain a reliable wavelength scale for the filter calibration measurements. The challenge for this past summer was to install the Fabry-Perot etalon and to detect fluorescence from the vapor cell in the "Doppler-free configuration". Unfortunately, in the course of these measurements it was discovered that the cell did not actually contain potassium. Another cell was bought for the system and a new oven fabricated in order to use it. The work for the summer was basicallythemodificationofthenewovenandthe constructionoftheFabry-Perotetalon.Asthesummer was ending, Israel was able to get an assignment to finish the project through the University ofPuertoRico,thankstoProf.JosÈRosado.Israelis now putting the working elements of this system intoastandardarrangementforlong-termuse.

Edvier Cabassa-Miranda, a sophomore at The UniversityofPuertoRico-MayagÝez,workedwithProf. Julio Urbina (PSU) and used Coqui II observations fromthe50MHzradarlocatednearSalinas,Puerto Rico, to measure observed counts of both specular and non-specular meteor trails in the E-region ionosphere. These observations were made over a time span ranging from 18:00 to 08:00 on various days in 1998 and 1999. The Coqui II radar has two sub-arrays, both pointed to the north in themagneticmeridianplane,perpendiculartothe magnetic field elevation angle of approximately 41degrees.Traditionalmeteorradarsrequiretrail specularity (trail perpendicular to radar beam) for a reflection, but over the last decade, two new typesofradar-meteorreflections,knownasmeteor headechoesandnon-speculartrails,havebecome known or widely used. He attempted to see if this radar is capable of detecting the head echoes. He analyzedthesignalsbyremovingunwantedinterference using some routines that he developed in IDL.NowthefutureworkistotrytogenerateRTI imagestoseetheheadechoes.Hewouldalsolike toconductsimulations. Israel GonzÀlez-PÈrez Jr., who is an undergraduate in electrical engineering at The University of Puerto Rico at MayagÝez, returned to Arecibo this summer to continue a project started during the previous summer under the tutelage of Dr. JonathanFriedman(NAIC).Thisistheconstructionofa testbedandcalibrationsystemforaFaradayfilter. ThepurposeofthefiltersystemistotakemeasureNAICAPRPP2007

Melissa Rivera is currently an undergraduate student in Electrical Engineering at The University of Puerto Rico at MayagÝez, with a strong interest in Communications, Physics and Astronomy. She is also the Vice-President of the Caribbean Astronomical Society of Puerto Rico. Her project at the ObservatoryfocusedonanalysisofdatafromJicamarcaObservatoryusingitsradarnamedJULIA(Jicamarca Unattended Long-term Investigations of theIonosphereandAtmosphere),andshewasadvisedbyProf.JosÈRosado(UPR-M).Thisstudyanalyzed perturbations in the electric field as a result ofgeomagneticsubstormsonequatoriallatitudes. The method that she used to obtain conclusions for these phenomena is called Superposed Epoch Analysis, which is a very powerful technique. It consists of sorting data into categories and comparingmeansfordifferentcategories.Thismethod mustbeappliedcarefullyandlogically.
The analysis of the radar data shows disturbances in the daytime equatorial geomagnetic H field associatedwithspecificphasesofisolatedsubstorms.
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Threewell-documentedsubstormswereexamined in India, but now with this investigation, she has found more than 102 days of perturbations at different hours and different days in 2004 and 2005. This pattern of response constitutes the first-time evidence for the occurrence of equatorial H-field perturbations related to the growth phase as well astheexpansionphaseofindividualsubstorms. ·FundingfromOtherSources: Gloria Isidro worked at the Visitor Center under the supervision of Drs. Carmen Pantoja and JosÈ Alonsowithascholarshipfromthe"FundacionComunitaria de Puerto Rico." She is a graduate studentattheDepartmentofMathematicsatTheUniversityofPuertoRico,RÌoPiedras.Thissummershe developed a guide for the Observatory for blind visitors. The guide consists of three documents in Braille with text and high relief figures describing thepartsofthetelescope,importanttermsusedin radio astronomy, and frequently asked questions. TogetherwithProf.CarlosLaRosa(UPR-Utuado)a tactilemodelofthetelescopewasalsodeveloped. These materials will help in making the Arecibo Observatory a more accessible facility and an Observatoryforall.

cility will allow high school, undergraduate, and graduate students to work in teams to perform actual observations of radio pulsars. They will use the data both to search for low-frequency gravitational waves and constrain the cosmic population of super-massive black hole binary systems. The firstprojectthestudentswillbeobservingforisthe PALFAproject. TheARCCstudentshavebeenworkingondesigns of the UTB Remote Command Center for the past sixweeks.Duringtheirplanning,studentsworked with limited budget and space while dreaming and designing a facility ideally suited for remote viewing. Student designs have incorporated items such as a star-field projection onto the ceiling of theroomtogiveavisualrepresentationoftheportionoftheskycurrentlybeingobserved.Theyalso designedaconferenceareaforpresentations.The myriad of control windows necessary will be displayedonaseriesofinterlinkedprojectionscreens andmonitors. One of the unusual aspects of the ARCC program is the level of integration of high school students. Currently, there are 13 high school junior and seniorstudentswhoareapartoftheARCCresearch group. These students are led by Andy Miller, a PorterHighSchoolphysicsandastronomyteacher. Thestudentsattendgroupmeetingsattheuniversity campus on Monday nights. These meetings give them the opportunity to collaborate with the undergraduate students, graduate students, and researchscientiststhatformthegroup. A special thanks to the people at Arecibo who helped with the camera installation: Phil Perillat, TimHankins,ArunVenkataraman,andReyVÈlez.

5.3 Connecting to Arecibo
Students in South Texas got their first glimpse into the Arecibo Observatory Control Room via a new webcamthatlinksUTBandthePuertoRicoobservatory. On October 23, 2006, operator Wilfredo Portalatin turned to the camera and waved at the students--theyroaredwithexcitementatthisfirst encounter. The cell phone and laptop connection is the first step for this group as they start to build anAreciboRemoteCommandCenter(ARCC).

5.4 ALFALFA Visiting Scientists
In a November 16 meeting in Ithaca, Jamie Lomax presented her senior thesis project based on ALFALFA. Oded Spector had just arrived from Tel AvivUniversityaswell.Heisgettingstartedonan ALFALFA-basedPh.D.thesis. Dr. Rebecca Koopmann, an Associate Professor in the Department of Physics & Astronomy at Union CollegeisonsabbaticalatCornellasavisitingNAIC scientist (through July 2007) and as a member of the ExtraGalactic group working on the ALFALFA survey. Becky is especially interested in the connection between HI and star formation in nearby spiral galaxies and has done extensive work on
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Rick Jenet, a professor at the University of Texas at Brownsville, received an NSF Career Grant that is funding the construction of the ARCC. This fa52


how galaxies in the Virgo cluster differ from their moreisolatedcounterparts.WhileatCornell,Becky has become immersed in the ALFALFA project, conducting observations, making grids and extracting sources. Her particular research focus is onthestudyofearly-typegalaxiesinVirgothatare detected by ALFALFA. This October, Becky visited GeorgiaSouthernUniversitywhereshegaveacolloquium on ALFALFA and helped Sarah and Jim Higdon install the ALFALFA IDL-based reduction pipeline. Sarah will travel to Arecibo for a week in January 2007 with two GSU undergraduate students to conduct the ALFALFA observations. Becky has hosted the very successful 2005 and 2006 undergraduate ALFALFA workshops held at UnionCollege.SheisleadingtheALFALFAundergraduate education team development of educationalmaterialsandactivitiesespeciallygearedfor undergraduates involved in ALFALFA. Through Becky,wearesuretherewillbeasteadystreamof undergraduateswhohavethethrillofdiscovering newgalaxies! Dr. Noah Brosch is on sabbatical from Tel Aviv University's School of Physics and Astronomy and from the Directorship of its Wise Observatory. His research interests range from star formation processes in dwarf galaxies to small objects in our Solar System (asteroids and meteors). Among his various tasks, one of the more challenging is being the Principal Investigator of the UV space telescope TAUVEX built in Israel and scheduled to be launchedin2007.ThevisittoCornellhasallowed NoahtobecomefamiliarwiththeALFALFAdataacquisitionandpipelineandtoplanoutthescientific
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studyofstarformation in extremely isolated galaxies, ones which are unlikely to have experienced interactions in recent cosmic times. He has been joined most recently by his graduate studentOdedSpector. Oded is working on the criteria by which the isolated sample will be selected;thestudyof these galaxies will serve as the basis forhisPh.D.dissertationresearch.NoahandOded will spend several weeks in Arecibo in December 2006 to conduct the ALFALFA observations. We wish Noah great success with TAUVEX and look forward to finding out just what triggers star formationingalaxiesthatdon'thaveanyneighbors. Dr. Thomas Balonek, a Professor of Physics & Astronomy at Colgate University, is on sabbatical at Cornell as a visiting NAIC scientist (through April 2007) and isamemberoftheExtraGalactic group toworkontheALFALFAsurvey.Hisresearchspecialty is the radio and optical variability of quasars and AGN but, since becoming involved in ALFALFA last year, he has gotten very excited about the studyofHIingalaxiesandgroupsofgalaxies.During his stay at Cornell, Tom has been participating in the ALFALFA observations both in Arecibo and remotely, and is now one of the ALFALFA "expert observers". He just spent Thanksgiving at Arecibo introducing ALFALFA (and Arecibo!) to Aileen O'Donoghue,JeffMillerandsenior JamieLomaxofSt.LawrenceUniversity.Tom'scurrent ALFALFA project is a study of the spiral-rich ZwickyClusterZwCL1400+0949anditsenvirons. Tom began this work last year as the senior research project of his student Brian Walsh, who is now a graduate student at Boston University. It mightberememberedthatTomwasasummerstudent at Arecibo in 1973, but we both promise to keeppicturestakenduringthatsummersecret!









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6. Arecibo Observatory Publications (PY2006)
October 1, 2005 ­ September 30, 2006
In PY2006, 36 astronomy papers were published in refereed journals that presented original observational data from the Arecibo Observatory. These papers are identified by a blue square (¢). In addition,theNAIC/AOstaffandotherscientistswere authors of another 24 papers (identified below by a redcircle)thatwerepublishedinrefereedjournals inPY2006thatexclusivelyinvolvedarchivaldatafrom AO, data from other telescopes, or were theoretical papers involving no new observational data. Eleven papers presenting original observations from the Arecibo Observatory are currently in press or have recentlybeensubmittedtorefereedjournals.Allthe papers are listed below. NAIC/AO staff names are bolded.

try of a Candidate Contact Binary, Icarus, 182(2), pp.474-481,June2006
Bogdanov,S., J.E. Grindlay,C.O. Heinke,F. Camilo,P.C.C. Freire,and W. Becker, Chandra XRay Observations of 19 Millisecond Pulsars in the GlobularCluster47Tucanae,Astrophys.J.,646(2), pp.1104-1115,Aug2006 Burgay,M., N. D'Amico,A. Possenti,R. N. Manchester,A.G. Lyne,M. Kramer,M.A. McLaughlin,D.R. Lorimer,F. Camilo,I.H. Stairs,P. C.C. Freire, and B.C. Joshi, The Double Pulsar SystemJ0737-3039,MemoriedellaSocietaAstronomicaItalianaSupplement,9,p.345,2006 urgay,M., .C. oshi,N. 'Amico,A. ossenti,A. B BJ D P G. Lyne,R.N. Manchester, M.A. McLaughlin,M. Kramer,F. Camilo, andP.C.C. Freire,The Parkes High-Latitude Pulsar Survey, MNRAS, 368(1), pp. 283-292,May2006 Busch,M.W., S.J. Ostro,L. A. M. Benner,J. D. Giorgini,R. F. Jurgens, R. Rose,C. Magri,P. Pravec,D. J. Scheeres,and S. B. Broschart, Radar and optical observations and physical modeling of near-Earth Asteroid 10115 (1992 SK), Icarus, 181(1),pp.145-155,March2006[TimesCited:2] ¢ Campbell, B.A. and D.B. Campbell, Regolith properties in the south polar region of the Moon from70-cmradarpolarimetry,Icarus,180(1),pp.17,Jan2006[TimesCited:2] ¢ Carter, L.M., D.B. Campbell and B.A. Campbell, Volcanic deposits in shield fields and highland regions on Venus: Surface properties from radar polarimetry, J. Geophys. Res., 111, E06005, June 2006 ¢ Catinella,B., R. Giovanelli,and M.P. Haynes,Template Rotation Curves for Disk Galaxies, Astrophys. J., 640(2), pp. 751-761, April 2006 [TimesCited:2] ¢ Champion,D.J., D.R. Lorimer,M.A. McLaughlin,K.M. Xilouris,Z. Arzoumanian,P. C.C. Freire,A.N. Lommen,J.M. Cordes,and F. Camilo,Arecibo Timing and Single-Pulse Observations of 17 Pulsars, MNRAS, 363(3), pp. 929-936, Nov2005[TimesCited:3] ¢ Champion,D.J., M.A. McLaughlin, and D.R. Lorimer,ASurveyforPulsarsinEGRETErrorBoxes, MNRAS, 364(3), pp. 1011-1014, Oct 2005 [Times Cited:1]
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ASTRONOMY
Araya, E., P. Hofner, L. Olmi, S. Kurtz, and H. Linz, Arecibo observations of formaldehyde in L1551, 2006,toappearinAstron.J. Auld,R.,R.F.Minchin,J.I.Davies,B.Catinella,W. van Driel, P.A. Henning, S. Kinder, E. Momjian, E. Muller, K. O'Neil, S. Sabatini, S. Schneider, G. Bothun, L. Cortese, M. Disney, G.L. Hoffman, M. Putman, J.L. Rosenberg, M. Baes, W.J.G. de Blok, A. Boselli,E.Brinks,N.Brosch,J.Irwin,I.D.Karachentsev,V.A.Kilborn,B.Koribalski,andK.Spekkens,The AreciboGalaxyEnvironmentSurvey:precursorobservationsoftheNGC628group,2006,toappear inMNRAS Beelen, A., P. Cox, J. Pety, C.L. Carilli, F. Bertoldi, E. Momjian,A.Omont,P.Petitjean,A.O.Petric,StarburstActivityintheHostGalaxyofthez=2.58Quasar J1409+5628, 2005, to appear in Astron. Astrophys. ¢ Benner,L.A.M., J.D. Giorgini,S.J. Ostro,M.C. Nolan,and M.W. Busch,(99942) Apophis, IAU Circ.,8711,2,Ed.Green,D.W.E.,May2006 ¢ Benner, A.M., M.C. Nolan, S.J. Ostro, J.D. Giorgini,D.P.Pray,A.W.Harris,andC.Magri,Near-Earth Asteroid 2005 CR37: Radar Images and Photome54


¢ Cordes, J.M., B. Rickett, W. Coles, and D. Stinebring, Theory of Parabolic Arcs in Interstellar ScintillationSpectra,Astrophys.J.,637(1),pp.346-365, Jan2006 ¢ Cordes, J.M., P.C.C. Freire, D.R. Lorimer, F. Camilo, D.J. Champion, D.J. Nice, R. Ramachandran, J.W.T. Hessels, W. Vlemmings, J. van Leeuwen, S.M. Ransom, N.D.R. Bhat, Z. Arzoumanian, M.A. McLaughlin, V.M. Kaspi, L. Kasian, J.S. Deneva, B. Reid, S. Chatterjee, J.L. Han, D.C. Backer, I.H. Stairs,A.A.Deshpande,andC.-A.Faucher-GiguÕre, Arecibo Pulsar Survey Using ALFA. I. Survey StrategyandFirstDiscoveries,Astrophys.J.,637(1),pp. 446-455,Jan2006[TimesCited:2] ¢ Davies,J.I., M.J. Disney,R.F. Minchin,R. Auld,andR.Smith,Theexistenceanddetectionof optically dark galaxies by 21-cm surveys, MNRAS, 368(3),pp.1479-1488,May2006 Freire,P.C.C.,SolvingtheMysteryofIapetus,2005, submittedtoJ.Geophys.Res.-Planets ¢ Gavazzi, G., K. O'Neil, A. Boselli, and W. van Driel, HI Observations of Galaxies: The Coma Supercluster,Astron.Astrophys.,449(3),pp.929-935, April2006[TimesCited:2] Gibson,S.J. and K.H. Nordsieck,Erratum: The Pleiades Reflection Nebula. II. Simple Model Constraints on Dust Properties and Scattering Geometry, (ApJ, 589, 362 [2003]), Astrophys. J., 643(1), pp.582-583,May2006 ¢ Giovanelli,R., M.P. Haynes,B.R. Kent,P. Perillat, A. Saintonge,N. Brosch,B. Catinella,G.L. Hoffman,S. Stierwalt,K. Spekkens,M.S. Lerner,K. L. Masters, E. Momjian,J.L. Rosenberg, C.M. Springob,A. Boselli, V. Charmandaris, J.K. Darling, J. Davies, D. Garcia Lambas,G. Gavazzi,C. Giovanardi,E. Hardy,L.K. Hunt,A. Iovino, I.D. Karachentsev, V.E. Karachentseva, R.A. Koopmann, C. Marinoni, R. Minchin, E. Muller, M. Putman, C. Pantoja, J.J. Salzer, M. Scodeggio,E. Skillman, J.M. Solanes,C.Valotto,W.vanDriel,andL.vanZee,The Arecibo Legacy Fast ALFA Survey I. Science Goals, Survey Design and Strategy, Astron. J., 130(6), pp. 2598-2612,Dec2005[TimesCited:10] ¢ Giovanelli,R., M.P. Haynes, B.R. Kent, P. Perillat,B. Catinella, G.L. Hoffman, E. Momjian,J. L. Rosenberg, A. Saintonge, K. Spekkens, S. Stierwalt,N. Brosch,K.L. Masters, C.M. Springob,I.
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D. Karachentsev,V.E. Karachentseva, R.A. Koopmann, E. Muller,W. vanDriel, and L. vanZee,The AreciboLegacyFastALFASurveyII.Results,Astron. J., 130(6), pp. 2613-2624, Dec 2005 [Times Cited: 3] Gray, M.D., D.A. Howe and B.M. Lewis, Evolution of 1612-MHz maser emission in expanding circumstellarshells,MNRAS,364,pp.783-795,Dec 2005 ¢ Harmon,J.K., M.C. Nolan,J.L. Margot,D.B. Campbell,L.A.M. Benner, andJ.D. Giorgini,Radar observations of Comet P/2005 JQ5 (Catalina), Icarus,184(1),p.285-288,Sept2006 Hessels,J.W.T., S.M. Ransom,I.H. Stairs,P.C.C. Freire,V.M. Kaspi,and F. Camilo,A Radio Pulsar Spinning at 716 Hz, Science, 311(5769), pp. 19011904,March2006[TimesCited:7] Hodge, J.A. and A.A. Deshpande, HI Density DistributionDrivenbySupernovaEjecta:ASimulation Study, Astrophys. J., 646(1), pp. 232-239, July 2006 JimÈnez-Esteban,F.M., P. GarcÌa-Lario,D. Engels,andJ.V.PereaCalderÑn,AnInfraredStudy of Galactic OH/IR Stars. II. The `GLMP Sample' of Red Oxygen-Rich AGB Stars, Astron. Astrophys., 446(2),pp.773-783,February2006 Klaassen,P.D., R. Plume,S.J. Gibson,A.R. Taylor,and C.M. Brunt,CO in H I Self-absorbed Clouds in Perseus, Astrophys. J., 631(2), pp. 10011009,Oct2005[TimesCited:2] Koo,B-C., J. Kang,and C.J. Salter,A "Missing" Supernova Remnant Revealed by the 21 cm Line ofAtomicHydrogen,Astrophys.J.,643(1),pp.L49L52,May2006[TimesCited:2] Koopmann, R.A., M.P. Haynes, and B. Catinella,AComparisonofHandStellarScaleLengthsin Virgo and Field Spirals, Astron. J., 131(2), pp. 716735,Feb.2006[TimesCited:4] Kramer, M., I.H. Stairs, R.N. Manchester, M.A. McLaughlin, A.G. Lyne, R.D. Ferdman, M. Burgay, D.R. Lorimer, A. Possenti, N. D'Amico, J.M. Sarkissian, G.B. Hobbs, J.E. Reynolds, P.C.C. Freire, and F.Camilo,Testsofgeneralrelativityfromtimingthe doublepulsar,2006,toappearinScience
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LebrÑn,M., H. Beuther,P. Schilke,and Th. Stanke,The extremely high-velocity molecular outflow in IRAS 20126+4104, Astron. Astrophys., 448(3), pp.1037-1042, March 2006 [Times Cited: 1] Lee,S., R.T. Pappalardo,and N.C. Makris,Mechanics of Tidally Driven Fractures in Europa's Ice Shell, Icarus, 177(2), pp. 367-379, Oct 2005 [Times Cited:1] ¢ Lewis, B.M., On Modeling the Near-Infrared Two-Color Locus of OH/IR Stars with a Constant dM/dt,Astron.J.,132(2),pp.489-496,Aug2006 ¢ Lommen,A.N., R.A. Kipphorn,D.J. Nice,E.M. Splaver, I.H. Stairs,and D.C. Backer,The Parallax andProperMotionofPSRJ0030+0451,Astrophys. J., 642(2), pp. 1012-1017, May 2006 [Times Cited: 1] Lorimer, D.R., Binary and Millisecond Pulsars, LivingReviewsofRelativity,8(7),Nov2005 ¢ Lorimer,D.R., I.H. Stairs,P.C.C. Freire,J.M. Cordes,F. Camilo,A.J. Faulkner,A.G. Lyne,D.J. Nice,S.M. Ransom,Z. Arzoumanian,Z., and 26 coauthors, Arecibo Pulsar Survey Using ALFA. II. The Young, Highly Relativistic Binary Pulsar J1906+0746, Astrophys. J., 640(1), pp. 428-434, March2006[TimesCited:6] ¢Masters, K.L., C.M. Springob, M.P. Haynes, and R. Giovanelli, SFI++ I: A New I-band Tully-Fisher Template, the Cluster Peculiar Velocity Dispersion and H0,toappearinAstrophys.J.,Dec2006 McLaughlin,M.A., A.G. Lyne,D.R. Lorimer,M. Kramer,A.J. Faulkner,R.N. Manchester,J.M. Cordes,F.Camilo,A.Possenti,I.H.Stairs,G.Hobbs, N. D'Amico, M. Burgay, and J.T. O'Brien, Transient radio bursts from rotating neutron stars, Nature, 439(7078),pp.817-820,Feb2006 [TimesCited:12] Meech,K.J., N. Ageorges,M.F. A'Hearn,C. Arpigny,A. Ates,J. Aycock,J.,....Howell, E.S., plus 202 coauthors, Deep Impact: Observations from a Worldwide Earth-Based Campaign, Science, 310(5746), pp. 265-269, Oct 2005 [Times Cited: 14] Momjian,E., J.D. Romney,C.L. Carilli,and T.H. Troland,SensitiveVLBIStudiesoftheOHMegama56

ser Emission from IRAS 17208-0014, 2006, to appearinAstrophys.J.
¢ Nice,D.J.,E.M.Splaver,I.H.Stairs,O.LÆhmer,A. Jessner,M. Kramer,and J.M. Cordes,A 2.1 Msolar Pulsar Measured by Relativistic Orbital Decay, Astrophys.J.,634(2),pp.1242-1249,Dec2005[Times Cited:35] ¢ Nolan, M.C., J.K. Harmon, E.S. Howell, D.B. Campbell, and J.L. Margot, J.L., Detection of Large GrainsintheComaofCometC/2001A2(LINEAR) from Arecibo Radar Observations, Icarus, 181(2), pp.432-441,April2006[TimesCited:1] ¢ Osten, R.A. and T.S. Bastian, Wideband SpectroscopyofTwoRadioBurstsonADLeonis,Astrophys. J., 637(2), pp. 1016-1025, Feb 2006 [Times Cited:1] ¢ Ostro,S.J.,L.A.M.Benner,C.Magri,J.D.Giorgini, R.Rose,R.F.Jurgens,D.K.Yeomans,A.A.Hine,M.C. Nolan,D.J.Scheeres,S.B.Broschart,M.Kaasalainen, and J.L. Margot, Radar Observations of Itokawa in 2004andImprovedShapeEstimation,submittedto MeteoriticsandPlanetaryScience,40(11),pp.15631574,Nov2005[TimesCited:1] ¢ Ostro,S.J., L.A.M. Benner,J.D. Giorgini,M.C. Nolan,A.A. Hine,E.S. Howell,J.L. Margot, C. Magri,and M.K. Shepard,(1862) Apollo, IAU Circ., 8627, 2 (2005). Edited by Green, D. W. E., Nov 2005 Ostro,S.J., West,R.D., Janssen,M.A., Zebker,H.A., Wye,L.C., Lunine,J.I., Lopes,R.M., Kelleher,K., Hamilton,G.A., Gim,Y., Anderson, Y. Z., Boehmer, R. A., and Lorenz, R. D., Cassini RADAR Observations of Phoebe, Iapetus, Enceladus, and Rhea, Icarus, 183(2), pp. 479-490, Aug 2006 [TimesCited:1] Ostro,S.J.,J.L.Margot,L.A.M.Benner,J.D.Giorgini, D.J. Scheeres, E.G. Fahnestock, S.B. Broschart, J. Bellerose,M.C.Nolan,M.Magri,P.Pravec,P.Scheirich,R.Rose,R.F.Jurgens,E.M.DeJong,andS.Suzuki, Radar Imaging of binary near-Earth asteroid (66391)1999KW4,2006,toappearinScience ¢ Pandian, J.D., Baker, L., Cortes, G., Goldsmith, P.F., Deshpande, A.A., Ganesan, R., Hagen, J., Locke,L.,Wadefalk,N.,andWeinreb,S.,Low-Noise 6-8GHzReceiver,IEEEMicrowaveMagazine,7(6), 74,2006
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SymposiumonTelescopeScience.HeldMay23-25, 2006, atBigBear,CA.PublishedbytheSocietyfor AstronomicalSciences,p.168,May2006 Benner,L.A.,M.W.Busch,S.J.Ostro,J.D.Giorgini,A. A. Hine,J.K. Harmon,M.C. Nolan,R. Rose,R.F. Jurgens,J.S. Jao,C. Magri, and J.L. Margot, Radar ImagesofAsteroid100085(1992UY4),NearEarth Objects,OurCelestialNeighbors:Opportunityand Risk, International Astronomical Union. Symp. no. 236,held14-18August,2006inPrague,CzechRepublic,S236,#29,Aug2006 Black, G., D.B. Campbell, R. Treacy, and M.C. Nolan, Radar-Interferometric Asteroid Imaging Using a Flexible Software Correlator, American AstronomicalSocietyMeeting207,#04.14,BAAS,37,p. 1155,Dec2005 Black, G.J. and D.B. Campbell, Arecibo Radar Observations Of Enceladus, Tethys, Dione, and Rhea, American Astronomical Society, DPS meeting #38, #72.02,Sept2006 Burgay,M., N. D'Amico,A. Possenti,A. Lyne,M. Kramer,M. McLaughlin,D. Lorimer,R. Manchester,F. Camilo,J. Sarkissian,P. Freire, and B.C. Joshi, The Double Pulsar System J0737-3039: NewsandViews,inInteractingBinaries:Accretion, Evolution, and Outcomes. AIP Conference Proceedings,797,pp.523-530,Oct2005 Busch,M.W., S.J. Ostro,L.A.M. Benner,and J.D. Giorgini,Radar Images and Shape Models of Asteroids 10115 (1992 SK), 23187 (2000 PN9) and 29075(1950DA),TheSocietyforAstronomicalSciences 25th Annual Symposium on Telescope Science. Held May 23-25, 2006, at Big Bear, CA. Published by the Society for Astronomical Sciences, p. 169,May2006 Busch,M.,J.D.Giorgini,S.J.Ostro,L.A.M.Benner,R. F. Jurgens,R. Rose,P. Pravec,D.J. Scheeres,S.B. Broschart,C. Magri,M.C. Nolan, and A.A. Hine, Physical Modeling of Near-Earth Asteroid 29075 (1950 DA), American Astronomical Society, DPS meeting#38,#53.09,Sept2006 Camilo,F.; PALFACollaboration, Arecibo Multibeam Pulsar Surveys: Overview and Discovery of a Young Relativistic Binary, American Astronomical Society Meeting 207, #192.04; Bulletin of the American Astronomical Society, Vol. 37, p.1489, Dec2005
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Thesis:
Catinella, B., Internal kinematics of disk galaxies inthelocaluniverse,Ph.Ddissertation,CornellUniversity,Nov2005

Conference Proceedings:
Ayala,J.A.,A.Stilp,N.Patel,A.Altaf,J.Goldstein,C. Forsyth,M. Gillin,B. Mahmood,J. Read,L. Vucic, and 15 coauthors, An Undergraduate Research Project within the ALFALFA Collaboration, American Astronomical Society Meeting 207, #179.21; BulletinoftheAmericanAstronomicalSociety,Vol. 37,p.1457,Dec2005 Backer, D.C., On the Way to the ATA, From Clark Lake to the Long Wavelength Array: Bill Erickson's RadioScienceASPConferenceSeries,Vol.345,Proc. oftheConf.held8-11September,2004inSantaFe, New Mexico, USA. Edited by N. Kassim, M. Perez, M.Junor,andP.Henning,p.471,Jan2006 Benner,L.A.M.,AreciboandGoldstoneRadarImagingofNear-EarthandMain-BeltAsteroidsin2005, TheSocietyforAstronomicalSciences25thAnnual
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Campbell, B.A., L.M. Carter, D.B. Campbell, B.R. Hawke, R.R. Ghent, and J.L. Margot, 20-m Resolution Radar Studies of the Aristarchus Plateau and Reiner Gamma Formation, 37th Annual Lunar and PlanetaryScienceConf.,March13-17,2006,League City,TX,abstractno.1717,Mar2006 Campbell, D.B., J.K. Harmon, M.C. Nolan, and S.J. Ostro, Radar observations of comet nuclei and comae, Highlights of Astronomy IAU Symp. 13, p. 763,2005 Campbell, D.B. and B.A. Campbell, L.M. Carter, J.L. Margot, and N.J.S. Stacy, High Resolution Radar PolarimetricObservationsoftheLunarSouthPole, 37th Annual Lunar and Planetary Science Conf., March 13-17, 2006, League City, TX, abstract no. 1408,Mar2006 Carter, L.M., D.B. Campbell, J.L. Margot, and B.A. Campbell, Mapping the Topography of Maxwell MontesUsingGround-basedRadarInterferometry, 37th Annual Lunar and Planetary Science Conf., March 13-17, 2006, League City, TX, abstract no. 2261,Mar2006 Carter,L.M.,D.B.CampbellandM.C.Nolan,Regolith Cover on Near-Earth Asteroids: Radar PolarimetricImagingandAnalysis,AmericanAstronomicalSociety,DPSmeeting#38,#68.04,Sept2006 Catinella,B., M.P. Haynes,J.P. Gardner,A.J. Connolly,and R. Giovanelli,Evolution of the Massto-light Ratio of Galaxies to z~0.25, Galaxy Evolution Across the Hubble Time, International AstronomicalUnion.Symp.no.235,held14-17August, 2006 in Prague, Czech Republic, S235, #114, Aug 2006 Cordes,J.M., M. Kramer,D.C. Backer,T.J.W. L a z i o , S c i e n c e W o r k i n g G r o u pf o r t h e S q u a r e K i lometerArrayTeam, Key Science with the Square Kilometer Array: Strong-field Tests of Gravity using Pulsars and Black Holes, American Astronomical Society Meeting 207, #137.04; Bulletin of the American Astronomical Society, Vol. 37, p.1390, Dec2005 Cordes, J.M., The Square Kilometer Array: Key Science and Technology Development, From Clark Lake to the Long Wavelength Array: Bill Erickson's Radio Science ASP Conf. Series, Vol. 345, Proc. of the Conf. held 8-11 Sept 2004 in Santa Fe, New Mexico, N. Kassim, M. Perez, M. Junor, and P. HenNAICAPRPP2007

ning,eds.,p.461,Jan2006 Cordes, J.M., The Square Kilometer Array, American Astronomical Society Meeting 208, #73.02, June2006 Cortese,L., R. Minchin,J. Davies,R. Auld,B. Catinella, and E. Momjian, AGES observations of Abell1367 and its outskirts, Galaxy Evolution Across the Hubble Time, International AstronomicalUnion.Symp.no.235,held14-17August,2006 inPrague,CzechRepublic,S235,#127,Aug2006 Crutcher, R.M. and T.H. Troland, Magnetic Fields andStarFormation-ObservationalResults,inTriggered Star Formation in a Turbulent ISM, International Astronomical Union. Symposium no. 237, held 14-18 August, 2006 in Prague, Czech Republic,S237,#25,Aug2006 Day,F.M. and E. Momjian,The Impact of Arecibo's Sensitivity on VLBA Observations, American AstronomicalSocietyMeeting207,#29.07;Bulletin of the American Astronomical Society, Vol. 37, p. 1212,Dec2005 Deneva, J.S. and R.M. Shannon, The Pulsar ALFA SurveyandanNVO-EnabledSearchforPulsarJets and Bowshocks, American Astronomical Society Meeting207,#187.01;BulletinoftheAmericanAstronomicalSociety,Vol.37,p.1480,Dec2005 Deneva,J.S.,AssessmentofPulsarandRotatingRadio Transient Detection Rates for the Arecibo Pulsar-ALFA Survey, American Astronomical Society Meeting208,#4.06,June2006 deRijcke,S., P. Buyle,D. Michielsen,D. J. Pisano,K. Freeman,and H. Dejonghe, E+A Galaxies : Did They Lose the A to Become E?, GalaxyEvolutionAcrosstheHubbleTime,InternationalAstronomicalUnion.Symp.no.235,held1417 August, 2006 in Prague, Czech Republic, S235, #334,Aug2006 Edwards,P.G., J.S. Ulvestad,and E.B. Fomalont,A VLBA Survey of Flat-Spectrum FIRST Sources, FutureDirectionsinHighResolutionAstronomy:The 10thAnniversaryoftheVLBA,ASPConf.Proc.,Vol. 340, edited by J. Romney and M. Reid. San Francisco:ASP,p.83,Nov2005 Freire,P.; ALFAPulsarConsortiumCollaboration, ALFA Pulsar Surveys: Searching for Fundamental
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Laboratories of Extreme Physics, American AstronomicalSocietyMeeting207,#192.05,Dec2005 Freire,P.,PulsarSurveyswithALFA,36thCOSPAR Scientific Assembly. Held 16 - 23 July 2004, in Beijing,China,p.1431,2006 Freire,P., B. Jacoby,M. Bailes,I. Stairs,A. Mott,R. Ferdman,D. Nice,and D.C. Backer, Discovery And TimingofthePSRJ1741+1351BinaryPulsar,American Astronomical Society Meeting 208, #72.06, June2006 Freudling,W., L. Staveley-Smith,M. Calabretta,B. Catinella,W. vanDriel,S. Linder,R. Minchin,E. Momjian,M.Zwaan,AUDSTeam,TheALFAUltra DeepSurvey(AUDS),AmericanAstronomicalSocietyMeeting207,#88.08,Dec2005 Frey,S., L.I. Gurvits,D.C. Gabuzda,C.J. Salter,D.R. Altschuler,P.Perillat,M.F.Aller,H.D.Aller,H.Hirabayashi,andM.M.Davis,VSOPMonitoringofthe CompactBLLacObjectAO0235+164,Pub.ofthe Astron. Society of Japan, 58(2), pp. 217-222, April 2006 Ghent, R.R., B.A. Campbell, B.R. Hawke, and D.B. Campbell, Earth-based 70-cm radar observations ofthesoutheastlimboftheMoon,AmericanGeophysical Union, Fall Meeting, abstract P33D-02, Dec2005 Ghent, R.R., B.A. Campbell, B.R. Hawke, and D.B. Campbell,RemoteSensingandGeologicStudiesof the Southeastern Quadrant of the Moon, 37th AnnualLunarandPlanetaryScienceConf.,March1317, 2006, League City, TX, abstract no. 1815, Mar 2006 Gibson, S., GALFACTS: A Full-Stokes Continuum Survey of the Arecibo Sky, American Astronomical SocietyMeeting207,#192.07,Dec2005 Gibson,S.J., J.M. Stil, A.R. Taylor,C.M. Brunt,D.W. Kavars,andJ.M.Dickey,ColdGalacticHIintheFirst and Second Quadrants, American Astronomical SocietyMeeting207,#81.01,Dec2005 Gibson,S.J., Galactic Spiral Structure in HI Emission and Self-Absorption, American Astronomical SocietyMeeting208,#49.02,June2006 Gibson,S.J., A.R. Taylor,J.M. Stil,C.M. Brunt,D.W. Kavars,andJ.M.Dickey,ColdHIinTurbulentEddies and Galactic Spiral Shocks, Triggered Star Forma60

tioninaTurbulentISM,InternationalAstronomical Union. Symp. no. 237, held 14-18 August, 2006 in Prague,CzechRepublic,S237,#61,Aug2006 Giovanelli,R.,M.P.Haynes,B.Kent,A.Saintonge,S. Stierwalt,N. Brosch,L. Hoffman,J. Rosenberg,B. Catinella,and E. Momjian, ALFALFA Discovery ofanHICloudComplexintheVirgoCluster,American Astronomical Society Meeting 207, #179.22, Dec2005 Haynes, M.P., ALFA Surveys as Complements to other Major Surveys, American Astronomical SocietyMeeting207,#192.08;BulletinoftheAmerican AstronomicalSociety,Vol.37,p.1489,Dec2005 Haynes,M.P., . iovanelli,B.R. ent,A. aintonge,S. RG K S Stierwalt,B. Catinella,E.M. Momjian,G.L. Hoffman,J.R.Rosenberg,N.Brosch,J.I.Davies,and R.L. Minchin, Complex Structure in the ALFALFA HIDistributionAroundVirgoHI21,AmericanAstronomicalSocietyMeeting207,#179.23,Dec2005 Heinke,C.O., J.E. Grindlay,P.D. Edmonds, H.N. Cohn,P.M. Lugger,F. Camilo,S. Bogdanov,and P.C. Freire,X-ray Binaries in the Globular Cluster 47Tucanae,inInteractingBinaries:Accretion,Evolution,andOutcomes.AIPConf.Proc.,797,pp.4045,Oct2005 Henkel, C., K.M. Menten, J. Braatz, R. Mauersberger, A. Weiss, M. LebrÑn, A. Tarchi, A.B. Peck, C.L. Carilli,andD.A.Lubowich,Extragalacticammonia, Highlights of Astronomy, IAU Symp. 13, pp. 879881,2005 Henning,P.A., C.M. Springob,B. Catinella,E. Momjian,B. Koribalski,K. Masters,E. Muller,C. Pantoja,M. Putman,J.L. Rosenberg,S. Schneider, and L. Staveley-Smith, Surveying The Zone Of Avoidance With The Arecibo L-band Feed Array, American Astronomical Society Meeting 208, #53.04,June2006 Hessels,J.,S.Ransom,I.Stairs,P.Freire,S.Begin,V. Kaspi,andF.Camilo,Radiopulsarsinglobularclusters,36thCOSPARScientificAssembly.Held16-23 July2004,inBeijing,China,p.1436,2006 Howell,E.S.,A.J.Lovell,B.Butler,F.P.Schloerb,and S.A. Torchinsky,Radio OH Observations of Comet 9P/Tempel1BeforeandAfterDeepImpact,American Astronomical Society Meeting 207, #187.04, Dec2005
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Howell,E.S.,C.Magri,H.M.Hanson,andM.C.Nolan, Correlating IRTF Spectra and Arecibo Radar Observations of Low-Albedo Main-Belt Asteroids, American Astronomical Society, DPS meeting #38, #59.08,Sept2006 Kasian,L.E.;PALFAConsortium,NewObservations of the Young Relativistic Binary PSR J1906+0746, American Astronomical Society Meeting 208, #4.02,June2006 Keeney, B.A., Do Starburst Winds Escape Their Parent Galaxies?, American Astronomical Society Meeting 207, #43.04; Bulletin of the American AstronomicalSociety,Vol.37,p.1229,Dec2005 Kent,B.R., R. Giovanelli,M.P. Haynes,A. Saintonge,S. Stierwalt,N. Brosch,B. Catinella,G. L. Hoffman,E. Momjian,and J.L. Rosenberg,ALFALFA Observations of the Virgo cluster and its environs, American Astronomical Society Meeting 207,#179.20;BulletinoftheAmericanAstronomicalSociety,Vol.37,p.1457,Dec2005 Khachokian,E.Y., G.T. Ter-Kazarian,andY. Terzian,OnMulti-NucleiFeaturesofSomeMarkarian Galaxies, Galaxy Evolution Across the Hubble Time,InternationalAstronomicalUnion.Symp.no. 235,held14-17August,2006inPrague,CzechRepublic,S235,#223,Aug2006 Koopmann,R.A., M.P. Haynes,J. Alonso,R. Giovanelli,G.L. Hoffmann,B.R. Kent,S. Stierwalt,and J.J. Salzer,The ALFALFA Undergraduate Workshop: Promoting Undergraduate Participation in a Legacy Survey Project, American Astronomical Society Meeting 207, #179.24; Bulletin of the American Astronomical Society, Vol. 37, p.1458,Dec2005 Kornreich,D.A., A.W. Mitschang, andA.K. Furniss, Deep ALFALFA HI Mapping of the Anomalously Large Disk of NGC 5701, American Astronomical SocietyMeeting208,#14.17,June2006 Kouprianova,E.G., A.V. Stepanov,and V.V. Zaitsev,Radio pulsations from AD Leo: diagnostics ofelectriccurrentsandplasmaparametersinstellar flares,HighlightsofRecentProgressintheSeismology of the Sun and Sun-Like Stars, 26th meeting of the IAU, Joint Discussion 17, 23 August 2006, Prague,CzechRepublic,JD17,#24,Aug2006

Kramer, M., Future radio observatories for pulsar studies, On the Present and Future of Pulsar Astronomy,26thmeetingoftheIAU,JointDiscussion 2, 16-17 August, 2006, Prague, Czech Republic, JD02,#44,Aug2006 Kronberg, P.P., The Astrophysical Importance of Low-level, Low Frequency Intergalactic Radiometry,FromClarkLaketotheLongWavelengthArray: BillErickson'sRadioScienceASPConferenceSeries, Vol. 345, Proc. of the Conf. held 8-11 September, 2004 in Santa Fe, New Mexico, USA. Edited by N. Kassim,M.Perez,M.Junor,andP.Henning,p.276, Jan2006 Lewis, B.M., On the reemergence of 1612 MHz masersinIRAS19479+2111,AmericanAstronomical Society Meeting 207, #104.06; Bulletin of the American Astronomical Society, Vol. 37, p.1335, Dec2005 Lewis, B.M., Identifying the Youngest Proto Planetary Nebulae, Planetary Nebulae in our Galaxy and Beyond, Proc. of the International Astronomical Union, Symp. #234, M.J. Barlow and R.H. MÈndez, eds. Cambridge University Press, pp. 449-450, 2006 Lommen,A.N., R.A. Kipphorn,D.J. Nice,E.M. Splaver, I.H. Stairs,and D.C. Backer, The Parallax and Proper Motion of PSR J0030+0451, American Astronomical Society Meeting 207, #183.06; Bulletin of the American Astronomical Society, Vol. 37, p.1469,Dec2005 Lovell,A.J. E.S. Howell,H. Marine,B.J. Butler,and F.P. Schloerb,OH Radio Mapping Observations of Comet73P/Schwassmann-Wachmann3,American Astronomical Society, DPS meeting #38, #06.04, Sept2006 Mantovani,F.,A.Rossetti,W.Junor,D.J.Saikia,and C.J. Salter,VLBA Polarimetric Observations of Young Radio Sources, Future Directions in High Resolution Astronomy: The 10th Anniversary of the VLBA, ASP Conf. Proc., Vol. 340. Edited by J. Romney and M. Reid. San Francisco: Astronomical SocietyofthePacific,2005,p.186,Nov2005 Margot, J.L., P. Pravec, M.C. Nolan, E.S. Howell, L.A.M.Benner,J.D.Giorgini,R.F.Jurgens,S.J.Ostro, M.A. Slade, C. Magri, P.A. Taylor, P.D. Nicholson, andD.B.Campbell,HermesasanExceptionalCase Among Binary Near-Earth Asteroids, Near Earth
61

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Objects,OurCelestialNeighbors:Opportunityand Risk,InternationalAstronomicalUnion,Symp.236, held 14-18 August, 2006 in Prague, Czech Republic,S236,#35,Aug2006 Minchin,R.F., E-ALFAConsortiumCollaboration, AGES, AUDS, ALFALFA, ZOA--Surveying the Extragalactic Sky from A to Z, American Astronomical Society Meeting 207, #192.02; Bulletin of the American Astronomical Society, Vol. 37, p. 1488, Dec2005 Minchin,R.F., J.I. Davies,M.J. Disney,A.R. Marble,C.D. Impey,P.J. Boyce,D.A. Garcia,M. Grossi,C.A. Jordan,R.H. Lang,S. Roberts, S. Sabatini,andW.vanDriel,HighResolutionHIImaging of VIRGOHI 21 - A Dark Galaxy in the Virgo Cluster, American Astronomical Society Meeting 207, #188.13,Dec2005 Minchin,R.F., R. Auld,J.I. Davies,B. Catinella,S. Linder,E. Momjian,E. Muller,S. Sabatini,S.E. Schneider,M.D. Stage,W. van Driel, AGES Team, FirstResultsfromtheAreciboGalaxyEnvironment Survey, American Astronomical Society Meeting 208,#53.06,June2006 Minchin,R.F., R. Auld,R., J.I. Davies,B. Catinella, L. Cortese,S. Linder,E. Momjian,E. Muller,K. O'Neil,K., J. Rosenberg,S. Sabatini, S.E. Schneider, M.D. Stage, and W. van Driel, The Arecibo Galaxy Environments Survey - Description of the Survey andEarlyResults,GalaxyEvolutionAcrosstheHubble Time, International Astronomical Union. Symp. no.235,held14-17August,2006inPrague,Czech Republic,S235,#284,Aug2006 Momjian,E.,T.H.Troland,J.D.Romney,C.L.Carilli, andG.B.Taylor,SensitiveVLBIObservationsofthe ULIRGIRAS17208-0014,FutureDirectionsinHigh Resolution Astronomy: The 10th Anniversary of the VLBA, ASP Conference Proceedings, Vol. 340. EditedbyJ.RomneyandM.Reid.SanFrancisco:AstronomicalSocietyofthePacific,p.232,Nov2005 Momjian,E., J.D. Romney,C.L. Carilli,and T.H. Troland,HSAobservationsofOHMegamaserEmission from the ULIRG IRAS 17208-0014, American AstronomicalSocietyMeeting207,#21.04;Bulletin of the American Astronomical Society, Vol. 37, p. 1191,Dec2005 Momjian,E.,C.J.Salter,T.Ghosh,J.Chengalur,N. Kanekar,B.A. Keeney,and J.T. Stocke, Arecibo HI
62

Observations of the Sub-DLA at z=0.0063 towards PG1216+069, American Astronomical Society Meeting208,#15.03,June2006
Nice,D.J., J.M. Weisberg,and J.H. Taylor,Arecibo Measurement of the Proper Motion of Binary Pulsar B1913+16, American Astronomical Society Meeting207,#183.05;BulletinoftheAmericanAstronomicalSociety,Vol.37,p.1468,Dec2005 Nice, D.J., High precision millisecond and binary pulsar timing at Arecibo, 36th COSPAR Scientific Assembly.Held16-23July2004,inBeijing,China., p.3227,2006. Nice,D.J.,PulsarTiminganditsFuturePerspective, On the Present and Future of Pulsar Astronomy, 26thmeetingoftheIAU,JointDiscussion2,16-17 August, 2006, Prague, Czech Republic, JD02, #57, Aug2006 Nolan, M.C., L.A.M. Benner, G. Black, D.B. Campbell, J.D. Giorgini, A.A. Hine, E.S. Howell, J.L. Margot,andS.J.Ostro,Radarobservationsofnearearthasteroids,HighlightsofAstronomyIAUSymp. 13,p.759,2005 Nolan,M.C., A.A. Hine,E.S. Howell,L.A.M. Benner,J.D. Giorgini,S.J. Ostro,G.J. Black,D.B. Campbell,J.L. Margot,L.M. Carter,and C. Magri, Extreme Diversity of Near-Earth Asteroid Physical Properties from Arecibo Radar Imaging, American AstronomicalSocietyMeeting207,#04.15,Bulletin of the American Astronomical Society, Vol. 37, p. 1155,Dec2005 Nolan, M.C., J.K. Harmon, E.S. Howell, L.A.M. Benner,J.D.Giorgini,S.J.Ostro,D.B.Campbell,and J.L.Margot,RadarObservationsOfComet73P/Schwassmann-Wachmann 3, American Astronomical Society,DPSmeeting#38,#12.06,Sept2006 Ostro,S.J., L. Benner,J.D. Giorgini,C. Magri,J. L. Margot,M.C. Nolan,and M.K. Shepard, Radar Reconnaissance Of Near-Earth Asteroids, Near Earth Objects, Our Celestial Neighbors: Opportunity and Risk, International Astronomical Union. Symp.no. 236, held 14-18 August, 2006 in Prague,CzechRepublic,S236,#6,Aug2006 Ostro,S.J., J.L. Margot, L.A.M. Benner, J.D. Giorgini,D.J. Scheeres,E.G. Fahnestock,S.B. Broschart,J. Bellerose,M.C. Nolan,C. Magri,P. Pravec,P.Scheirich,R.Rose,R.F.Jurgens,S.Suzuki,
NAICAPRPP2007


and E.M. de Jong, Radar Investigation of Asteroid 66391 (1999 KW4), American Astronomical Society,DPSmeeting#38,#65.02,Sept2006 Pandian,J.D., P.F. Goldsmith,and A.A. Deshpande,The Arecibo Methanol Maser Galactic Plane Survey, American Astronomical Society Meeting207,#165.02;BulletinoftheAmericanAstronomicalSociety,Vol.37,p.1424,Dec2005 Possenti,A., M. Burgay, N. D'Amico,A. Lyne,M. Kramer,M.McLaughlin,D.Lorimer,R.Manchester, F.Camilo,J.Sarkissian,P.Freire,B.C.Joshi,I.Stairs, and R. Ferdman, Two Years of Work in the J07373039 Laboratory, in Astrophysical Sources of High Energy Particles and Radiation, AIP Conf. Proc., 801,pp.272-277,Nov2005 Ransom,S.M., J.W.T. Hessels,I.H. Stairs,P.C.C. Freire,V.M. Kaspi,and F. Camilo,A Globular Cluster Pulsar Renaissance with the Green Bank Telescope, American Astronomical Society Meeting 207,#32.05,Dec2005 Reddy,V., R.R. Dyvig,P. Pravec,P. Kusnirak,L. Kornos,J. Vilagi,A. Galad,S. Gajdos,D.P. Pray,L. A.M. Benner,M.C. Nolan, J.D. Giorgini, S.J. Ostro, and P.A. Abell, Photometric and Radar Observations of 2005 AB: A New Binary Near-Earth Asteroid,37thAnnualLunarandPlanetaryScienceConference, March 13-17, 2006, League City, Texas, abstractno.1755,March2006 Roshi,D.A.,High-frequencyCarbonRecombination LineasaProbetoStudytheEnvironmentofUltracompactHIIregions,inTriggeredStarFormationin aTurbulentISM,InternationalAstronomicalUnion. Symp.no.237,held14-18August,2006inPrague, CzechRepublic,S237,#202,Aug2006 Saintonge,A., C. Marinoni,K.L. Masters, M.P. Haynes,R. Giovanelli, and T. Contini,Multi-wavelength Study of Galaxy Rotation Curves and its Application to Cosmology, 2005, to appear in the proc.oftheVthMarseilleInternationalCosmology Conf. Saintonge,A., R. Giovanelli,M.P. Haynes,B. Kent,S. Stierwalt,N. Brosch,B. Catinella,and E. Momjian,ASignalExtractionUtilityfortheALFALFASurvey,AmericanAstronomicalSocietyMeeting 207,#187.02,Dec2005 Salzer,J.J., N.M. Tresser,J.L. Rosenberg,and S. Stevenson,S., An Optically Unbiased Look at the
NAICAPRPP2007

Local Universe: Properties of the ADBS HI-Selected SampleofGalaxies,AmericanAstronomicalSociety Meeting207,#179.19;BulletinoftheAmericanAstronomicalSociety,Vol.37,p.1457,Dec2005
Sarma,A.P., T.H. Troland,J.D. Romney,and T.H. Huynh,T.H., VLBA Zeeman effect observations of water masers in the star forming region OH43.80.1, American Astronomical Society Meeting 207, #195.01;BulletinoftheAmericanAstronomicalSociety,Vol.37,p.1492,Dec2005 Scheeres,D.J., E.G. Fahnestock,S.J. Ostro,J. L. Margot,L.A.M. Benner,S.B. Broschart,J. Bellerose,J.D. Giorgini,M.C. Nolan,C. Magri,P. Pravec,P.Scheirich,R.Rose,R.F.Jurgens,S.Suzuki, and E.M. DeJong, Dynamical Investigation of Asteroid 66391 (1999 KW4), American Astronomical Society,DPSmeeting#38,#65.03,Sept2006 Shepard,M.K., B.E. Clark,L.A.M. Benner,J.D. Giorgini,C. Magri,M.C. Nolan,and S.J. Ostro, More Results from a Long-Term Radar Survey of M-Class Asteroids, American Astronomical Society, DPSmeeting#38,#71.01,Sept2006 Shore,S.N., T.N. Larosa,L. Magnani,and F.Costagliola,Turbulence in High Latitude Clouds, in Triggered Star Formation in a Turbulent ISM, International Astronomical Union. Symp. no. 237, held 14-18 August, 2006 in Prague, Czech Republic,S237,#3,Aug2006 Simpson,R.A., G.L. Tyler,M.C. Nolan,M. PÄtzold,andB.HÄusler,MarsExpressBistaticRadar Explores Stealth, American Astronomical Society, DPSmeeting#38,#67.06,Sept2006 Spekkens,K., .Momjian,B.R. ent,R. iovanelli,M. E K G P. Haynes,B. Catinella,S. Stierwalt,and A. Saintonge,ALFALFA Discovery of an HI Cloud Complex in the Virgo Cluster: Aperture Synthesis Observations, American Astronomical Society Meeting207,#179.25,Dec2005 Stacey,G.J., S.R. Golwala,C.M. Bradford,C.D. Dowell,G. Cortes-Medellin,T. Nikola,J. Zmuidzinas,T.L. Herter,S.J. Radford,J.P. Lloyd,A. W. Blain, R.L. Brown, and 9 coauthors, Instrumentation for the CCAT Telescope, Millimeter and Submillimeter Detectors and Instrumentation for AstronomyIII,J.Zmuidzinas,W.S.Holland,S.Withington, and W.D. Duncan, eds., Proc. of the SPIE, Vol.6275,July2006
63


Stairs,I.H., M. Kramer,R. Manchester,M. McLaughlin,A. Lyne,R. Ferdman,M. Burgay,D. Lorimer,A.Possenti,N.D'Amico,B.Joshi,P.Freire, and F. Camilo, Recent Observations of the Double Pulsar, American Astronomical Society Meeting 208,#33.04,June2006 Stanimirovic,S., Recent Results From Galfa: `GoldenEye' On Disk/halo Interfaces, American AstronomicalSocietyMeeting208,#34.02,June2006 Stierwalt,S., M.P. Haynes,R. Giovanelli,B. Kent,A. Saintonge,I.D. Karachentsev,V. E. Karachentseva,N. Brosch,B. Catinella,L. Hoffman,andE.Momjian,ALFALFASurveyofthe Leo Region, American Astronomical Society Meeting207,#187.03,Dec2005 Taylor,P.A.,J.L.Margot,M.C.Nolan,L.A.Benner,S. J.Ostro,J.D.Giorgini,andC.Magri,RadarImaging of Binary Near-Earth Asteroid 2004 DC, American Astronomical Society, DPS meeting #38, #50.04, Sept2006 Toribio, M.C., First Results from VLA Observations of Five Spiral Galaxies in the Virgo Cluster Region, GalaxyEvolutionAcrosstheHubbleTime,InternationalAstronomicalUnion.Symp.no.235,held1417 August, 2006 in Prague, Czech Republic, S235, #390,Aug2006 Troland,T.H.,MagneticFieldStrengthsintheCold NeutralMediumoftheGalaxy,AstronomicalPolarimetry: Current Status and Future Directions ASP ConferenceSeries,Vol.343,Proc.oftheConf.held 15-19 March, 2004 in Waikoloa, Hawai'i, USA. A. Adamson, C. Aspin, C. J. Davis, and T. Fujiyoshi, eds.,p.64,Dec2005 Ulvestad,J.S., K.E. Johnson,and S.G. Neff,A VLBI Search for Radio Supernovae in Super Star Clusters, American Astronomical Society Meeting 207, #113.09;BulletinoftheAmericanAstronomicalSociety,Vol.37,p.1346,Dec2005 Wells, K., D.B. Campbell, B.A. Campbell, and L.M. Carter,TheSize-FrequencyDistributionofFar-Field Tycho Secondary Craters, American Astronomical Society,DPSmeeting#38,#57.12,Sept2006 Weltevrede, P.. B. Stappers, and J. Rankin, and G. Wright, Is PSR B0656+14 a very nearby RRAT source?, On the Present and Future of Pulsar Astronomy,26thmeetingoftheIAU,JointDiscussion
64

2, 16-17 August, 2006, Prague, Czech Republic, JD02,#46,Aug2006 West,A.A., D.A. Garcia-Appadoo,and J.J. Dalcanton,SDSS/HIPASS Volume Limited Galaxy Survey, American Astronomical Society Meeting 208,#53.01,June2006





NAICAPRPP2007


7. NAIC External Federal Funding & Active Subcontracts
External Funding
Sponsor $$$ $37,655 $412,000 PI S. Gibson Period of Award Title of Project

CURRENT
JPL Joint Institute for VLBI in Europe NASA NSF 9/13/06 - 9/30/08 Cold Diffuse Clouds: The Missing A. Venkataraman $244,700 D. Campbell $20,000 R. Brown

NSF

$58,842

J. Friedman

NSF

$167,899

J. Friedman C. Tepley J. Alonso S. Gonzalez

Link in Molecular Cloud Formation EXPReS: A Production Astronomy eVLBI Infrastructure 8/1/03 - 7/31/06 Surface Properties From Radar and Radio Observations 9/1/06 - 2/28/07 Community Workshop: Building the Foundation for US Astronomy at m/cm Wavelengths in 2010 and Beyond 4/1/05 - 3/31/10 Collaborative Research: HighResolution Resonance Lidar Detection of Meteor Trails 11/1/05 Collaborative Research: CEDAR 10/31/08 Daytime Potassium Lidar at Arecibo
TBD 5/1/03 - 12/31/06 The Arecibo Geoscience Diversity

NSF

$596,836

Space Environment Corp. (NSF)

$95,000

S. Gonzalez

University of Puerto Rico (NASA)

$239,349

C. Tepley

Program: Enhancing the Education of Hispanics Through Research Experiences 10/1/03 - 9/30/07 Investigation of the Accuracy of Ionospheric Models at MidLatitudes...Implementation of Ionospheric Metric at CCMC 3/13/02 - 8/31/05 Studies of Tropical Weather and Climate at the Arecibo Observatory
9/1/04 - 8/31/07 Further Studies of Aerosols and

University of Puerto Rico (NASA)

$72,884

C. Tepley

Climate at the Arecibo Observatory

PENDING
AFOSR/DURIP $942,000 M. Sulzer, S. Gonzalez 4/1/07 - 3/31/08 The Arecibo HF Facility: An

NSF

$289.08

S. Raizada, J. Friedman, C. Tepley

Instrument to Study Ionospheric and Plasma Physics in the NearEarth Space Environment 2/10/07 - 2/9/10 CEDAR: An Observational and Theoretical Study of the Climatology of the Ca/Ca+ Layer in the MLT at Arecibo and its Relation to the Sporadic Micrometeor Flux
5/1/07 - 4/30/10 The Arecibo Geoscience Diversity

NSF

$966,156

J. Alonso

Space Telescope Science Institute University of Puerto Rico (NASA)

$9,916 $146,690

R. Minchin C. Tepley

University of Puerto Rico (NASA)

$207,402

C. Tepley

Project: A Track 2 Initiative for a Mentored Research Experience for Pre-College, Teacher, and Undergraduate Hispanics 1/1/07 - 12/30/07 The Nearest Gas-Rich Giant Galaxy 7/1/07 - 6/30/10 Understanding Cloud and Aerosol Dynamics in Tropical Coastal Regions 6/1/05 - 5/31/08 Cloud Studies at the Arecibo Observatory

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65


NAIC External Federal Funding & Active Subcontracts continued

Active Subcontracts
Subcontractor Ammann & Whitney Consulting Engineers, PC Columbia University $$$ $50,000 $1,750 PI T. Anderson F. Camillo J. Mock D. Janches J. Breakall J. Mathews D.B. Backer X. Chu Period of Award Purpose 4/1/06 - 3/31/10 Engineering Consulting for the

Arecibo Telescope
4/1/05 - 3/31/07 Software Development on Behalf of

the p-ALFA Consortium
Jeff Mock $400,000 Northwest Research Associates, Inc. $87,399 Penn State University Penn State University University of California, Berkeley University of Colorado $60,000 $62,358 $16,336 $61,311 1/1/06 - 4/30/07 P/E ALFA Spectrometers 4/1/06 - 4/1/07 Developing New AO Programs 9/1/06 - 5/31/07 HF Design 1/1/06 - 9/30/07 Next Generation SAS 4/1/05 - 3/31/07 Software Development on Behalf of

the p-ALFA Consortium
9/1/06 - 11/30/07 Student Support for Collaborative

Research CEDAR Daytime Potassium Doppler Lidar at Arecibo
University of Colorado $14,499 X. Chu 6/1/06 - 7/31/07 Study of MLT Thermal Structure and

University of Puerto Rico

$234,916

M. Ramos

10/1/03 12/31/06

Dynamics in Tropical Area Using Arecibo Data The Arecibo Geoscience Diversity Program

66



















NAICAPRPP2007


8. Division of Effort for Staff
Distribution of Effort ATM REU VC

N am e R.L. Brown

Title Director, NAIC Interim Site Director AO Dir of Operations Asst Dir, SAS Sub-total Asst Prof Deputy Director, NAIC Head, Astronomy Program Head, Tech Services; Head, SSS Post Doc Post Doc Post Doc Post Doc Res Assoc Res Assoc Res Assoc Res Assoc Res Assoc Res Assoc Res Assoc Res Assoc Sr Res Assoc Sr Res Assoc Sr Res Assoc Sr Res Assoc Sr Res Assoc Sr Res Assoc Sr Res Assoc Sr Res Assoc Sr Res Assoc, Dir OPUS Visiting Scientist Visiting Scientist Visiting Scientist Visiting Scientist Visiting Scientist Visiting Scientist Sub-total GRA GRA Pre-Doc Student Pre-Doc Student Research Intern Sub-total

FTE HQ Key Personnel 1.00 x 1.00 1.00 3.00 Scientific Staff 0.35 x x 1.00 1.00 1.00 1.00 1.00 1.00 1.00 1.00 1.00 1.00 1.00 1.00 1.00 1.00 x 1.00 1.00 1.00 1.00

AST 1.00 1.00 0.75 2.75 0.35 1.00 0.85

CU*

Total 1.00 1.00 1.00 3.00 0.35 1.00 1.00 1.00 1.00 1.00 1.00 1.00 1.00 1.00 1.00 1.00 1.00 1.00 1.00 1.00 1.00 1.00 1.00

T. Hankins
R. Kerr S. Gonzalez

0.25 0.25

0.00

0.00

0.00

J.L. Margot M. Haynes B.M. Lewis M. Nolan B. Catinella J. Fernandez P. Santos R. Minchin E. Howell E. Momjian H. Vo M. Lebron M. Lerner N. Aponte P. Freire S. Gibson C. Tepley C.J. Salter G. Cortes-Medellin J. Friedman J.K. Harmon M. Sulzer S. Raizada T. Ghosh D.R. Altschuler A. Lovell L.Waldrop N. Brosch R. Koopman T. Balonek W. Gordon

0.15 1.00 1.00

1.00 1.00 1.00 0.70 1.00 1.00 1.00 1.00 1.00 1.00 1.00 1.00 1.00 0.50 0.50 0.30

x x x x x 18.35 Graduate Students x x 1.00 1.00 1.00 3.00 Managers 1.00 x 1.00 1.00 1.00 x x x 10.20 7.35 0.00 0.00 0.80 x x 1.00 1.00 1.00 1.00 1.00 1.00 3.00 18.35

E. Nossa

J. Pandian
Vacant Vacant I. Seker

x 1.00

1.00

0.00

0.00

0.00

Admin Director Business Manager Chief Telescope Engineer EH&S Officer S. Bravo Guard-Security Suprv A.G. VenkataramanHead, Computer Dept G. Rajagopalan Head, Electronics Dept J. Alonso Head, Visitor Center M. Rodriguez HR Manager Sub-total

D. Marsh J. Cordero Vacant W. Arias

0.80 0.85 1.00 0.80 1.00 1.00

0.20 0.15 0.20

1.00 1.00 1.00 1.00 1.00 1.00 1.00 1.00 8.00

1.00 1.00 1.00 1.00 8.00

0.75 0.80 6.25 0.20 0.75 0.00 0.75

0.25 0.25

NAICAPRPP2007



















67


Division of Effort for Staff continued
Name Vacant A.M. Vazquez A. Hine E. Robles W. Greene M.A. Morales V. Iguina J. Acevedo G. Comes J.A. Jimenez F.O. Soberal D. Whitlow H. Camacho R. Seal T. Hall L.A. Baker Title ALFA Programmer Computer Programmer Data Analyst Data Analyst Electrical Engr (Transmitters) Electronics Maint Engr Electronics Maint Engr HR/Scientific Services Info Tech Engr II Mech Engr/Maintenance Platform Maint Supervisor Res Support Spec Res Support Spec-Digital Res Support Spec-Digital Res Support Spec-Digital Res Support Specialist FTE HQ AST Professional/Technical 1.00 1.00 1.00 1.00 1.00 1.00 Distribution of Effort ATM REU VC CU* Total 1.00 1.00 1.00 0.50 1.00 1.00

0.50

1.00 1.00 1.00 1.00 1.00 1.00 1.00 1.00 1.00

1.00 1.00 1.00 1.00 0.85 1.00 1.00 1.00

0.15 1.00

x

1.00 1.00 1.00 1.00 1.00 1.00 1.00 1.00 1.00

B. Genter
Vacant R. Velez G. Shankaran J.L. Rodriguez P.J. Perillat N. Despiau W. Portalatin K.D. Kabelac

Res Support Spec-Receivers
Res Support Spec-Receivers Res Support Spec-RFI Sr Compt Staff Supp Spec Sr Compt Staff Supp Spec Sr Compt Staff Supp Spec Sr Telescope Operator Sr Telescope Operator Tech Serv Supervisor Tech Support Spec Tech Support Spec Telescope Scheduler/SOS Sub-total Executive Staff Asst Executive Staff Asst Finance Specialist Head, Telescope Ops Purchasing Supv Store Manager Sub-total Admin Aide Admin Asst Admin Asst Asst. Store Manager Elect Sup Coord Executive Secty Executive Secty Executive Secty HR & Benefits Asst HR & Payroll Asst Library Asst Office Assistant Purchasing Aide Purchasing Aide VC Tour Guides Workstudy Student Sub-total 1.00 0.50 1.00 1.00 1.00 1.00 x 1.00 1.00 1.00 20.50 15. 60 Administrative/Clerical 1.00 0.75 1.00 x 1.00 x 1.00 1.00 1.00 1.00 1.00 5. 00 3.75 Clerical 1.00 1.00 1.00 x 0.80 1.00 1.00 1.00 1.00 1.00 1.00 1.00 1.00 1.00 6.00 0.30 17.30 1.00 4.90 0.25 0. 00 0. 00 0.00 1.00 1.00 20.50 1.00 1.00 1.00 1.00 1.00 5. 00 1.00 1.00 1.00 1.00 1.00 1.00 1.00 0.80 1.00 1.00 1.00 6.00 x 0.30 8. 90 0.40 0. 00 8. 00 0. 00 1.00 1.00 1.00 1.00 1.00 1.00 1.00 1.00 1.00 6.00 0.30 17.30 1.00 0.50 1.00 0.75 1.00 1.00 0.50 1.00 1.00 1.00 1.00

0.25 1.00

E.L. Ruiz
R. Garcia H. Hernandez

Vacant
W. Turner Vacant Jose Luis Cruz M. Santiago M. Irizarry

0. 25

0.00

1.00 1.00

0.00

C. Torres J. Tarbell

0.20

W. Perez
A. Ortiz S. Cuevas de Jesus C. Rosario M. Mercado W. Santiago L. Lopez M. Gerena C.G. Segarra M. Herrera C. Caban M. Lopez (19) UPR Students S. DeVaul

0.20

68



















NAICAPRPP2007


Division of Effort for Staff continued
Name Title FTE HQ Technical AST Distribution of Effort ATM RE U VC CU* Total

J.L. Padilla Vacant

E. DeJesus M. Alvarez
A. Nolla A. Santoni Ruiz C. Rios-Velez J. Capo J. Rosa J.A. Soto J.E. Vives J.M. Rios V. Negron W. Iguina D.W. Overbaugh E. Cruz Martinez E. Gonzalez J. Marrero W. Hernandez

W. Torres Rivera

Drafter Driver Electrician Electrician Electronics Tech Electronics Tech Electronics Tech Electronics Tech Electronics Tech Electronics Tech Electronics Tech Electronics Tech Electronics Tech Electronics Tech Equipment Tech Systems Operator I Systems Operator I Systems Operator I Systems Operator I Telescope Operator Sub-total Air Cond Mech Auto Mech Carpenter/Plumber Groundskeeper Groundskeeper Guard Guard Guard Guard Guard Guard Guard Guard Guard Guard Guard Guard-Asst Suprv Heavy Equip Operator Janitor Laborer Machine Shop Foreman Sr Mechanic Supply Clerk Telescope Maint Supv Telescope Mechanic Telescope Mechanic Telescope Mechanic Telescope Rigger/Painter Telescope Rigger/Painter

1.00 1.00 1.00 1.00

1.00 0.75 0.50 1.00 0.25 0.50

1.00 1.00 1.00 1.00

1.00 1.00 1.00 1.00 1.00 x 1.00 1.00 1.00 1.00 13.00 Maintenance 1.00

1.00 1.00 1.00 0.50

0.50 1.00

1.00 1.00 1.00 1.00 1.00 1.00 1.00 1.00 1.00

1.00 1.00 1.00 1.00 10.75 1.00 2.25 0.00 0 .0 0 0.00

13.00 1.00

J. Velez I. Perez

A. Alonzo
A. Rivera

1.00 1.00 1.00 1.00 1.00 1.00 1.00 1.00 1.00

1.00 1.00 1.00 1.00 1.00 1.00 1.00 1.00 1.00

1.00 1.00 1.00 1.00 1.00 1.00 1.00 1.00 1.00

Antonio Perez
A. Maldonado C. Lebron D. Padilla-Arce I. Chico Cruz J.E. Maldonado J.M. Velez M. Lopez P. Perez R. Robles Vacant Vacant

A. Correa
M. Rodriguez Angel Perez E. Batista A. Aquino J. Perez S. Chico J. Rosado E. Del Pilar E. Lopez Martinez O. Rodriguez C. Sein E. Gonzalez

1.00 1.00 1.00 1.00 1.00 1.00 1.00 1.00 1.00 1.00 1.00

1.00 1.00 1.00 1.00 1.00 1.00 1.00 1.00 1.00 1.00 1.00

1.00 1.00 1.00 1.00 1.00 1.00 1.00 1.00 1.00 1.00 1.00

NAICAPRPP2007



















69


Division of Effort for Staff continued
Name F. Rodriguez Perez H. Crespo J. Rodriguez-Sein J.M. Chacon M. Nieves N. Gonzalez Correa Title Telescope Rigger/Painter Telescope Rigger/Painter Telescope Rigger/Painter Telescope Rigger/Painter Telescope Rigger/Painter Telescope Rigger/Painter Trade Supervisor Trades Helper Util Maint Worker Util Maint Worker Util Maint Worker Util Maint Worker Welder/Mechanic Sub-total FTE 1.00 1.00 1.00 1.00 1.00 1.00 HQ AST 1.00 1.00 1.00 1.00 1.00 1.00 Distribution of Effort ATM RE U VC CU* Total 1.00 1.00 1.00 1.00 1.00 1.00

V. Santiago
O. Rolan G. Milian J.A. Rodriguez Jose Rodriquez R. Cajigas M. Cortes

1.00 1.00 1.00 1.00 1.00 1.00 1.00 1.00 1.00 1.00 1.00 33.00 31.00 VSQ/Cafeteria 1.00 1.00 1.00 1.00 4 .0 0 125.15 1.00 1.00 1.00 1.00 4.00 94.20

1.00 0.00 0 .0 0 0.00 2.00

1.00 1.00 1.00 1.00 1.00 1.00 4.00

Vacant G. Rosario C. Ruiz E. Santiago R. Roman

Asst Cook Head Cook Housekeeper Housekeeper Kitchen Helper Sub-total

0.00 17.15

0.00 0 .0 0

0.00 11.75

0 .0 0 1 .0 5

1.00 1.00 1.00 1.00 4.00 125.15

Total NAIC Employee Effort

*Includes Cornell funds and/or salaries paid by other internal or external funding sources. Note: This listing includes all staff employed at some point during the 2006 program year, up to the publication date of this APRPP. The names shown in italics indicate a staff member who has departed NAIC in the last program year. The positions underlined were eliminated with the November 2006 staff reduction. The sub-totals and totals shown include active positions, up to the publication date of this APRPP

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9. NAIC Organization Chart and Description
9.1 Management Plan: Charts Organization

The National Astronomy and Ionosphere Center is conducted in accordance with the Cooperative AgreementbetweentheNationalScienceFoundation and Cornell University42. The organizational hierarchy of the two institutions that are party to thisCooperativeAgreementisasshownonFigure 9.1. The NSF is responsible for providing funding, general oversight, monitoring and evaluation to help assure that the NAIC is being managed and operated in accordance with approved plans. In supportofastableoperationalenvironmentforNAIC, the NSF strives to make annual funding for NAIC available to Cornell University in a timely fashion and to provide the necessary document reviews andapprovalsasrequired. Within the NSF, the NAIC contact is the NAIC Program Manager who is appointed within the DivisionofAstronomicalSciences(AST);heorsheisresponsible for scientific, programmatic and budget review and for providing the NAIC Director with agency guidance. In addition, the NAIC Program Managerisresponsibleforestablishinganeffective liaison with the manager within the Upper AtmosphereDivisionwhohasresponsibilityfortheNAIC Aeronomy program to assure that information on NAIC programmatics and review is available and shared. The NSF Division of Acquisition and Cooperative Support (DACS) is responsible for Cooperative Agreement matters between the NSF and Cornell University.Formalcommunicationsrelatedtocontracts and required Cooperative Agreement designated approvals is accomplished by the DACS through communication with the NAIC Administration Director. Annual funding and contractual obligationsflowfromtheNSFDACStotheCornell University Office of Sponsored Programs as specifiedintheCooperativeAgreement.
2
4 CooperativeAgreementNo.AST-0431904betweenthe NationalScienceFoundation,Arlington,VA22230andCornell University,Ithaca,NY,14853,datedOctober1,2005.

Cornell University, as the Cooperative Agreement awardee,isresponsiblefortheperformanceofthe NAIC. As illustrated in Figure 9.1, within Cornell UniversitytheNAICreportstotheViceProvostfor Research. NAIC has the responsibility for scientific operationsoftheobservatory,staffingitandensuring adequate oversight of the execution and performance of the Observatory in accordance with therequirementsofitsusers. InthespiritoftheNSF-CornellUniversityCooperativeAgreementforNAIC,communicationbetween NSF and Cornell is maintained on all institutional levels from that of the Cornell President providing the annual report of the NAIC Visiting Committee to the NSF Director, to the day-to-day reporting and programmatic interaction of the NAIC Director with the NSF/AST Division Program Manager. Again,thisisshownonFigure9.1. The National Astronomy and Ionosphere Center is one of twenty-two research centers managed by Cornell University. The NAIC director reports through the Vice Provost for Research to the Cornell University President. This top level organization within the university structure is illustrated in Figure9.1. Ultimate responsibility for the management and operation of NAIC rests with the University President. To carry out this responsibility the President establishedanexternalVisitingCommitteetoconduct an annual review of the management effectiveness of NAIC with emphasis on the scientific program of the NAIC, long range planning, and budget. The Cornell University Vice Provost for Research hastheresponsibilitytooverseetheprogrammatic plan, staffing and budget of NAIC. He also serves astheResponsibleExecutiveunderthetermsofthe Cooperative Agreement. In this capacity, the Vice Provost is aided by a Cornell advisory committee, the Cornell NAIC Oversight Committee (CNOC), that regularly reviews the operation and managementofNAICmonitoringprogressandplans. Cornell management of NAIC is defined in the NAIC Management Plan53. The Senior NAIC management consists of the Director, Deputy Director andtheAdministrationDirector.Althougheachof
NAICManagementPlan,November2005.Preparedbythe NationalAstronomyandIonosphereCenter,CornellUniversity, Ithaca,NY,14853
5

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Figure 9.1. InstitutionalrelationshipsbetweenCornellUniversityandtheNSFformanagementoftheNAIC.

these individuals has different, well-defined primary responsibilities as specified in the Management Plan,theoverallmanagementtaskisaccomplished asthesumoftheirseparateandsharedefforts.An advisory committee, the Arecibo Users and Scientific Advisory Committee (AUSAC), meets annually to review the scope and specifics of the NAIC scientific program, to provide advice on observatory prioritiesandtorecommendnewinitiatives. Thus, Cornell University oversight of the NAIC is provided at three levels: The Visiting Committee assesses NAIC management structure and effectiveness and reports to the Cornell President's office; the CNOC reviews NAIC programmatics and reportstotheCornellofficeoftheViceProvostfor Research; and the AUSAC provides a users assessmentofNAICoperationstotheNAICdirector. TheoperationalmanagementstructureoftheAreciboObservatoryitselfisshownonFigure9.2.The Observatory Director is responsible for the scientific operation of the Arecibo telescope and all the observatoryinstrumentsthatfunctioninsupportof theObservatory'sscientificprogram.TheObserva72

toryDirectorisassistedbyDepartmentHeadswho are the responsible managers for the tasks shown in Figure 9.2. All of the Department Heads report to the Observatory Director. The Observatory DirectorreportstotheNAICDirector. The organizational structure of the Arecibo Observatory enables the observatory staff to serve the diverse needs of the multidisciplinary science program at the observatory. Task prioritization is establishedbytheObservatorydirectorworkingin weekly, scheduled, consultation with the departmentheads. Major projects at the Observatory require special management attention. Each of these projects, as approvedforfundingbytheObservatorydirector, hasitsownprojectplan(tasks,resourcesandschedule).Projectmanagementisprovidedbyaproject managerselectedbytheObservatorydirector.For eachproject,thedirectoralsoselectsanindividual toserveasprojectscientist.Theroleoftheproject scientististogivescientificguidancetothemanager for any project decisions that have implications related to the project scope or to the interface of
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Figure 9.2.OrganizationChartfortheNAICAreciboObservatory

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the project to the Arecibo system. Every project hasaprojectmanagerandaprojectscientist,even those concerned with site building/remodeling. Such a management structure helps reinforce the ideathatthingsdoneattheNAICshouldbedone tobenefitscientificobjectives.Communicatingthis understandingtoallthoseinvolvedwiththeNAIC is one of the underlying Cornell management goals. Comprehensive accounting and management of all NAIC activities--operations and projects--is made possible by the NAIC Work Breakdown Structure (WBS). The WBS is a tool used by the NAIC director's office to track progress and monitor personnel assignhments. The WBS allows the NAIC director to measure progress by comparing the annual plan for budget allocation and personnelassignmentagainsttheyear-endactualbudget expenditure and actual personnel effort assigned foreachactivity. At NAIC, personnel assignments and budgets are madeandtrackedatWBSlevel-2. NAIC Work Breakdown Structure 1. NAIC Management 1.1 Director'sOffice 1.2 Administration 1.3 ProgramDevelopment 1.4 EngineeringDesignServices 1.5 US SKA Technology Development Project 2. Arecibo Observatory Operations 2.1 ManagementandAdministration 2.2 BusinessServicesandHumanResources 2.3 ScientificSupport 2.4 SiteServicesandTrades 2.5 Telescope 2.6 Electronics 2.7 Computing 2.8 Environment,SafetyandHealth 2.9 SpectrumManagement 3. Arecibo Observatory Technical Program 3.1 Telescope 3.2 Electronics 3.3 ComputingandCommunications 3.4 OpticalInstrumentation 3.5 BuildingInfrastructure
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3.6 MajorMaintenance 4. Scientific Research Program 4.1 Radio/RadarAstronomy 4.2 SpaceandAtmosphericSciences 5. HF 5.1 5.2 5.3 5.4 5.5 5.6 5.7 Project ProjectManagement Transmitter FeedSystem Electronics TelescopeSuspensionSystem MonitorandControl SystemEngineering

6. Platform Painting Project 6.1ProjectManagement 6.2EngineeringOversight 6.3ContractsandLabor 7. Angel Ramos Foundation Visitors Center 7.1 EducationandStudentPrograms 7.2 CommunityOutreachPrograms 7.3 NewInitiatives 8. Office for the Public Understanding of Science 8.1 TeacherandPublicWorkshops 8.2 Publications 8.3 NewInitiatives 9. Major New Initiatives 9.1 U.S. SKA Technology Development Project 9.2 Arecibo Geomagnetic Conjugate FacilityProject

9.2 List and Vitae of New Professional Staff
No new professional staff were hired during programyear2006.







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10. Status Report and Plan for PY2007
10.1 Scientific Plans
Scientific proposals made to NAIC for research on theArecibotelescopeinPY2007includestudiesof the gas content, distribution and dynamics of distantgalaxies,studiesoftheMilkyWaygalaxy,studies of stars and star-forming regions in the Milky Way, and detailed studies of solar system objects. These peer-reviewed proposals received from users and local staff together comprise the scientific plansforNAICinPY2007.Noindividualorinstitution can secureaccess to the telescope otherthan by means of submitting a peer-reviewed research proposal.

the Local and nearby superclusters, it will allow measurement of the HI diameter function, and it willenableafirstwide-areablindsearchforHItidal features,HIabsorbersatz<0.06,andOHmegamasersinthewavelengthrange0.16
Galaxies. Three major surveys of the HI gas content in galaxies, and in the environment shared among galaxies, are in progress. These two surveys are (1) ALFALFA, the Arecibo Legacy Fast ALFASurveythatbeganinPY2005withanobserving program that will continue through PY2013; (2) a deeper imaging survey, the Arecibo Galaxy Environment Survey (AGES), that begin a sevenyear program of observations in PY2006, and (3) theALFAUltra-DeepSurvey(AUDS)thatwillbegin inPY2007andfinishitsobservationalstagein2013 or2014.Allthreesurveysarebeingdonewiththe newALFAmultibeamimagingarrayreceiver.
Overthecourseofthenext5-7years,ALFALFAwill survey7000squaredegreesoftheskyandwilldetectsome16,000extragalacticHIsources.Itisspecifically designed to probe the faint end of the HI mass function in the very local universe and it will provide a complete census of HI in the surveyed sky area, making it especially useful in synergy withotherwideareasurveysconductedatoptical and infrared wavelengths, such as the Sloan Digital Sky Survey (SDSS), and the 2-micron University of Massachusetts survey (2MASS). In conjunction with optical studies of comparable volumes, ALFA will explore the "missing satellite problem", the apparent contradiction between the number of lowmasshaloesobservedintheLocalgroup,and surrounding groups, with that predicted from numericalsimulations.ALFALFAwillalsoprovidethe basisforstudiesofthedynamicsofgalaxieswithin
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· Investigate the HI mass function in different environments--around large galaxies, in groups of galaxies, clusters of galaxiesandbeyondtheLocalSupercluster--for comparison with galaxy evolutionmodels. · Giventheexcellentcorrelationbetween star formation rate and 20-cm continuumluminosity,AGESwillusethecontinuumemissiontomeasurethestarformation rates of a large number of galaxies selected by their gaseous rather than theiropticalorfar-infraredproperties. · Probe the contribution of neutral gas to the baryonic mass density--the "missing"baryonicmatterproblemwillbeexplored to greater depth than previously possible. · Studythenatureof,andpossiblelinkbetween,HVCsanddwarfgalaxiessearching for a solution to the CDM sub-structureproblem. · Identify gaseous tidal features as signatures of galaxy interactions and mergers.Seektounderstandtheimportance of mergers as a mechanism for the assembly of galaxies, and for gas removal mechanismsinclustersandgroups. · Probethenatureofdarkmatterbystudyingthevelocitydispersionsofgalaxiesin groupsandclusters. · Probe the nature of dark matter by studyingthedynamicalmassesofgalaxiescalculatedfromthemeasuredgalaxy rotationcurves. · Compute the magnitude of the metagalactic ionizing radiation field by measuring the truncation of the HI halos of largegalaxies. · Identify isolated neutral gas clouds and relate their surroundings to their formation either as remnants or precursors of thegalaxyformationprocess. · Compare the HI detected by QSO absorption line and 21-cm emission line observations.Arethesetwodeterminationsconsistentwitheachother? · UnderstandthespatialdistributionofHIselectedgalaxies. · Compare the AGES galaxy distribution with numerical models of galaxy formation providing input and tests of the validityofthesimulations.
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· Serendipitous findings: a large survey suchasAGEScoveringlargeareasofsky to low mass limits and column densities has great potential for making unexpecteddiscoveries. AUDS will use the new NAIC EALFA spectrometer to analyze the entire frequency band 1420 MHz ­ 1225 MHz carrying out a blind HI survey with unprecedented sensitivity, approximately 50 µJy/ beam. The frequency coverage corresponds to a rangeofHIredshiftsof0 0.1 will be larger than that of all previoustargetedandblindsurveyscombined. TheAUDSobservingprogramwillbeginatArecibo withthenewEALFAspectrometerinPY2007. ApartfromthemajorALFAsurveys,severalimportant `traditional' programs are planned in PY2007 to address specific scientific questions. One such program will conduct mapping observations of both HI and OH towards and surrounding the extended, bright, continuum region associated with NGC 383 (3C 31; Arp 331) in the Pisces-Perseus Supercluster. This group is exceptional for its extendedcontinuumbrightnessandlargespatialextent comprising eight galaxies which form a long galaxy chain. Continuum emission is occasionally detected with inter-group gas implying dynamic flows and/or high magnetic fields. These observations will be the first of their type: in addition to probing the usual three-dimensional (positionposition-velocity) neutral gas distribution, velocity dispersion and halo extent, they will provide two dimensionalgastemperaturedatathroughoutthe continuum emission region. The group is suitably nearby that it will be useful as a test-bed for probinghigherredshift,dampedLymanalphasystems.
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The observing program will map the large scale distribution of the intra-cluster HI of the NGC 383 group.Thespecificscientificobjectivesincludethe following: · Ascertain the full distribution of intracluster gas, and therefore the shape of the supporting gravitational potential field which results from the mass of the constituentgalaxies. · Probe the distribution and strength of the absorbed component that will uniquely provide information on the temperature and pressure of the intragroupgas. · Reveal the connectivity of the intragroupgas,andtherebyforthefirsttime, understand the complex dynamics and relationships of the large number of group members and their tidal interactions. Finally, the observations will form part of a larger long term project aimed at generating a database of absorption measurements through extended HI features of a number of perturbed systems and throughintra-galaxyclustergas.Systematicdifferences between the characteristics of profiles observed through tidal features, outflow processes andintra-galaxyclustergascanbeanalyzedonthe basisofmorerobuststatisticsultimatelyhelpingto discover fundamental differences and similarities of the thermal conditions of gas in these environments. The primary research targets for the HI 21-cm observations are gas-rich spiral galaxies. Elliptical galaxies, characterized by their old stellar population and little gas content, are more challenging, but equally interesting, targets. Several studies in PY2007 are focused on understanding the history of elliptical galaxies by means of observations of their atomic (HI) and molecular (CO) gas. As the telescopes used for the millimeter-wavelength CO observations improve the quality of their instrumentation, and hence improve their sensitivity, studiesofgasinellipticalgalaxiesislimitedprimarily by the paucity of sufficiently sensitive HI 21-cm observations.InPY2007 this deficiencywill beaddressed through long integrations with the Arecibotelescope. A complete sample of elliptical galaxies selected fromtheNearbyGalaxiesCatalogwillbesearched
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for both CO emission and HI emission. The HI observations will be made at Arecibo. An important objectiveoftheseobservationsistoassessthepossibility recently discussed that the molecular and atomic gas in elliptical gas has different physical origins. Of the 46 elliptical and SO galaxies in the sample, all but 7 have been searched for HI emission but only 13 have been detected previously. COemissionhasbeendetectedinall46.TheAreciboobservationswillimprovetheHIsensitivitylimits by more than an order of magnitude allowing manymoreofthegalaxiestobedetectedortoproduceupperlimitsthatarephysicallymeaningfulfor answeringthefundamentalquestions. Weak, redshifted. Ly- absorption lines are ubiquitous in far-UV spectra of nearby quasars. While notascommonasthehigh-zLy-forest,theseline nonetheless hold important clues to the baryon contentofthelocaluniverse.Somelow-zLy-absorbers are broad and weak, and may be directly associatedwithwarm-hotfilamentsofintergalactic gas. Narrow absorption lines are more common: the strongest often appear to be associated with galaxies and may trace extended halo gas, while weaker absorbers are distributed more randomly, suggestinganintergalacticorigin. The association between galaxies and absorbers is important for many reasons. Galaxies and intergalactic hydrogen are expected to trace the same filamentary distribution of dark matter seen in cosmological simulations. Thus, such correlations can provide a strong test for predictions of the CDM model. Furthermore, the gas probed by the quasar sight-line, if directly associated with a nearbygalaxy, providesinformationonthespatial andkinematicdistributionsofmatterinthegalaxy itself.Incaseswherethequasarsight-lineliesrelative far (> 100 kpc) from the center of the galaxy, the observed absorption systems may be probing gas in the far reaches of the galaxy's dark matter haloandcanthenbeusedtoplaceconstraintson thegalaxies'rotationcurvesatlargeradiiaswellas potentially serving as a hallmark of spiral galaxies withextremelyextendedHIdisksand/orhalos. Although the correlation between galaxies and Ly- absorbers at low redshifts has been studied observationally, not much is known about the morphologies and dynamical properties of the absorbinggalaxiesthemselves.Inparticular,dataon the HI morphologies and dynamical properties is still lacking. Deep observations of the absorbing
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galaxies themselves such as can be obtained only with the Arecibo telescope are needed to provide detailed information on the galaxies' extended HI morphologies and dynamics, and would be complementarytothespatialinformation. In PY2007 a systematic study of Ly- absorbing galaxieswillbedonetoaddressthreecriticalquestions: · Do the HI properties of galaxies associatedwithLy-absorbersdifferquantitatively compared to those of field galaxies? · Foredge-ongalaxies,istheLy-absorption line velocity consistent with the associatedgalaxy'sHIrotationvelocity? · Does the presence of Ly- absorption relatively far (~170 kpc) from a galaxy indicatetheexistenceofanextendedHI diskorhalo? ByobservingseveralgalaxiesinavarietyofconfigurationsrelativetotheLy-absorbers,theArecibo observations will provide needed insight into the natureoftheLy-/galaxyconnection. By number, dwarf galaxies are the most common type. Their star forming environments are simpler than those in massive spirals, making them excellentsystemsforthestudyofstarformationtriggeringandregulation.Asmallsubsetofdwarfgalaxies has been found to be extraordinarily bright in the IR PAH lines indicative of a large reservoir of very small dust grains. Why are these few dwarf galaxies so unusual? In PY2007 an attempt will be made to answer this question by means of HI 21-cm observations at Arecibo. The results will be combined with 8-µ PAH emission maps to determinethephysicalpropertiesofthestarformingregions, such as the atomic gas to stellar mass ratio, gastodustratio,starformationefficiency,andgas depletiontimescales. Thedeterminationofrotationalparametersofdisk galaxies is crucial to understanding disk galaxy formation and evolution over cosmic time, and to constrain models of galaxy structure. In particular, N-body simulations of cosmological scenarios must be able to reproduce observed scaling relations such as the Tully-Fisher relation. Presently, a very lively issue is the question of the evolution of the Tully-Fisher relation over cosmic time. Observations suggest that the co-moving star formation
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ratewashigherinthepast.Luminosityevolutionis also expected based on cosmological simulations. If galaxies were more luminous in the past, we shouldobserveanoffsetintheTully-Fisherrelation derived independently at high and low redshifts. However, studies based on optical spectroscopy havereachedconflictingconclusions.Resultsvary from substantial luminosity evolution in excess of one magnitude with respect to the Tully-Fisher relation derived for galaxies at z = 0, even at modest redshiftstonosignificant changeatz~1. EvidenceforevolutionoftheTully-Fisherrelation,ora lackthereof,isinconclusive. Studying the change in the Tully-Fisher relation at intermediate redshifts using radio HI velocity widthsoffersmanyimportantadvantagesoverthe optical studies. Compared to optical widths, HI measurements same a larger fraction of the galaxy disks, where the rotation curves are typically flat.Theradioobservationsarenotaffectedbyslit smearingandmisalignmentorbyapertureeffects. Thus, in contrast to studies based on optical spectroscopy,HIspectroscopyallowsustoperformadirectcomparisonwiththelocalTully-Fisherrelation thatistechniqueindependent.InPY2007observationswillbemadewiththeArecibotelescopeofa sample of 24-galaxies selected from the SDSS that willprovideasuitablydiscriminatingtest. Ultraluminous infrared galaxies are a population of galaxies that emit far-IR radiation with energies comparabletothoseofthemostluminousquasars. Nearly every ULIRG appears to have undergone a merger/interaction and contains massive star formation and/or an active galactic nucleus induced by gravitational interactions. The extraordinarily high gas densities and energy densities in ULIRGs makethemnaturallocationstoexpectverystrong magnetic fields. Minimum energy arguments suggestcharacteristicfieldstrengthsmaybe~100µG, twenty-timesgreaterthanthemagneticfieldinthe disk of the Milky Way. An alternate approach to estimatingthemagneticfieldinULIRGsistoappeal to the equipartition argument that applies in the Milky Way between magnetic field and ISM surface density. This would suggest a magnetic field strength as great as 1-10 mG. In either case, the estimated field strengths should be detectable by theZeemaneffectintheirOHmegamaserspectral lines. In PY2007 all the OH megamaser galaxies visible fromArecibowillbeobservedintheirOHspectral
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lines in a systematic search for the Zeeman effect. Positive detections will enable one or another of thesimplescalingrelationsnotedabovetobeconfirmedforuseinothergalaxieslackingsuchintense OHspectrallines. Understanding the relationship between HI and stars in the ISM of galaxies is critical to the study ofgalaxyevolution.Becausestellarpopulationsin galaxies form from collapsed clouds of hydrogen, wecanpresumethatgalaxiesevolvebyconverting theirgasintostarsandthatgalaxieswithfewstars and large quantities of gas must be less evolved than those with little gas and many stars. However,howagalaxyfollowsthisevolutionarypathis farmorecomplicated.Factorssuchasmass,metal content, gas fraction, internal motions, and other environmentalconditionsplayanimportantrolein determining the rate at which HI gets converted intostars. The extremes of galaxy evolution are particularly illustrative.Galaxiesthathavefewornostars,but possess large quantities of HI represent the most primitivestageofevolution.Galaxieswithlittlegas but many stars are some of the most evolved galacticsystemsintheuniverse,whichhavepresumablyconsumedalloftheirHI.Mostobservedgalaxies fall somewhere between these two extremes. Theyhavesomereservoirsofgasandhavealready accumulated populations of stars, and therefore represent a continuum of intermediately evolved galaxies.Bycollectingalargesameofgalaxies,using different techniques, it is possible to cover the entirerangeofevolutionarystates. Until recently, the ability to create such a sample was impossible. The required observing time placedseriouslimitsonthenumberofgalaxiesone couldincludeinanysample.Fortunately,thereare manylarge,unbiased,surveysnowunderway,givingastronomerstheabilitytoaccesslargeamounts ofdatainareasonableamountoftime.Inparticular, a comparison has been made between galaxiesdetectedbytheirHIemissionintheHIPASSsurveydoneattheParkestelescope,andthegalaxies found in that same region of sky detected by the Sloan Digital Sky Survey. There are 131 galaxies cataloged by the SDSS with optical redshifts less than 3000 km/s that cannot be identified in the HIPASS survey data. Many of these galaxies have opticalspectrathatsuggestactivestarformationis occurring.Thesesystemsareespeciallyinteresting becauseonewouldexpectanappreciablereservoir
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ofgastoaccompanystarformation.Observations willbemadeatAreciboinPY2007with~25times thesensitivityoftheHIPASSsurveyobservationsto tryandresolvethislogicalinconsistency. Theseobservationswillbecriticalalsoinconstrainingthebaryoncontentofnearbygalaxies.HIPASS and SDSS together do a good job of measuring most of the baryons in the joint dataset, either throughtheirHImassorthestellarmasscomputed from their colors. However, for the many galaxies notdetectedinHIPASSonlythestellarmasscanbe known.Yet,particularlyatthelow-luminosityend, themassinHIcouldstillbesignificant.Thisproject will address the missing data, either detecting or setting strong upper limits on the HI content of all galaxiesinthesample.

The Milky Way Galaxy. Theconsortiumofusers interested in surveying the Milky Way galaxy with ALFA,theGALFAconsortium,hasalsobeguninitial survey observations that will continue in PY2007. The GALFA emphasis in PY2007 includes study of turbulence in the ISM and the energy sources for that turbulence, a comparison of the atomic and molecularcomponentsin"molecular"clouds,careful large-scale mapping of clouds/regions in the MilkyWayofspecialastrophysicalinterest.
If the Milky way was a uniformly-rotating galaxy large-scale longitude-velocity, (l,v), HI maps would reflect that uniform rotation in smooth contours. This is not what is seen. In fact, the (l,v) diagrams of HI 21-cm emission in the Galactic plane usually show small high-velocity bumps protruding from their surroundings. These bumps represent line wings that extend to velocities beyond the maximumorminimumvaluespermittedbyGalacticrotation.These"forbiddenvelocity"wingsaredifferentfromhigh-velocity cloudsinthe sensethat the wings are extended and not separated from the GalacticHIemission.Sincethehigh-velocitywings exist at velocities forbidden by Galactic rotation, they must result from local dynamical processes, e.g. supernova explosions, stellar winds, collisions of high-velocity clouds, and such phenomenon. Severalexamplesofsuchlocalizedforbidden-velocity line wings are known in existing data sets, but theirrootcauseisunknown.ALFAwillbeusedto probe this phenomenon by examining with much better angular resolution the location and extent of the forbidden-velocity line wings and, with this information, to identify the underlying source of the turbulent energy input to the ISM. With this
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understandingintheknowncases,alargersurvey willbeconductedtomapthephenomenoninthe GalacticplanevisiblefromArecibo. In ourGalaxy,molecularcloudcomplexesand the atomic disk are distinct entities. The molecular cloudsaremoreconcentratedinspace,havemore than one order of magnitude higher density, and are generally much colder than atomic gas. The linewidth of the atomic ISM is determinedby pressure balance and is on the order of tens of km/s. The linewidth of molecular clouds, on the other hand,isontheorderofonekm/sandisdominated byturbulenceincloseequipartitionwiththecloud gravitationalenergy.Thus,unlikeatomicgas,molecular clouds are self-gravitating, turbulent objects.Thechangeofbalancebetweengravityand internal turbulence leads to star formation. This is the conventional understanding; clearly many points need verification and clarification. The primary goal of one of the key GALFA projects is to improve our understanding of the formation and age of molecular clouds by studying the relationshipbetweenneutralandmolecularhydrogen. ALFA will be used to map the HI distribution and velocity structure in the Taurus molecular cloud. These observations will be used to complement a CO data set that traces the molecular hydrogen distributioninthiscloud.InordertoisolatetheHI in the Taurus cloud from that in the foreground andbackground,observationswillbemadeofthe narrow HI self-absorption lines that arise from HI gaswithinthecloud.TheHI/H2ratioisasensitive measure of the elapsed lifetime of the molecular cloud. Hence the Arecibo observations will place a critical constraint on the evolution of the Taurus cloud. Specifically, column densities of both cold HIandH2willbecomputedfromtheobservations and that ratio will be studied as a function of total gas density, kinematic environment, and other parameters. The observations will enable the investigators to disentangle the atomic-molecular relationshipintheTauruscloud. InPY2007theGALFAconsortiumwillmakefurther progress on a complete, Nyquist-sampled, survey of the whole inner Galactic plane to |b| 10° in HI 21-cmlineemissionusingALFA.ALFAisuniquely abletoaddressmanyoutstandingquestionsinthe field of Galactic astronomy. Its fast mapping ability, high angular resolution, and unparalleled sensitivity allow the systematic study of whole cloud populations,structuresandphysicalprocessesover
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many size scales and across a range of interstellar environments. To understand these inter-related phenomena, it is necessary to map the inner Galaxythoroughlyoveralatituderangeofatleast|b| 10°. Such coverage shows the many disk features in context, features such as star-forming regions, superbubbles, and the HI envelopes of molecular clouds.Italsoallowscloudpopulations,HIrelicsof supernovae,anddiskturbulencetobeexaminedas a functionofheightabovethe plane toelevations oforder1kpc,thusprobingthetransitionfromthe thintothethickdisk.Mostimportantly,abroadlatitude range is essential for discerning the Galactic chimney structures that form the base of the diskhaloenergyexchange;thesefeaturesoftenextend many degrees off the plane and are impossible to studywithoutproperlatitudecoverage. The major scientific areas of investigation for the GALFAinnerGalaxyHIsurveyarethefollowing: · Characterizationofthephysicalcauseof faint,extended,emission-linewings; · Understanding the causal relation between the cold neutral medium as seen inemissionandinabsorption; · Probingthephysicsofinterstellar"chimneys","worms"andtheenergytransport fromtheGalacticdisktothehalo; · Investigating the origin and evolution of molecular clouds by establishing the spatial and kinematic association of GMCswithHIfeatures; · Seeking for the physical cause of interstellar turbulence using statistical analysesofHIlinekinematicsandcorrelations withsourcesofenergeticfeaturesinthe Galaxy. AsisthecasewiththestudyofgalaxiesatArecibo, researchers investigating phenomena in the Milky Waynotonlydosobymeansofwideareasurveys butalsobystudyingsmallareasofspecialinterest. InPY2007observationswillbemadeofatomicand moleculargasinawidevarietyofenvironmentsincludingHIinaspectacularGalacticfilament,"dark" gasinthelocal ISM,and OHintheedgesoftranslucentclouds. Lastyearanewpopulationofcoldneutralmedium (CNM)HIcloudswasdiscoveredthatarecharacterized by very low HI column densities, the so-called "low-N(HI)" clouds. The clouds have peak HI optical depths of only 0.1% to 2%, and column densi NAICAPRPP2007


ties no more than 1018 cm-2, 30-50 times lower thancharacteristicofthelargerensembleofgalactic HI clouds. How are these clouds related to the traditional spectrum of CNM clouds? To answer this questions observations were made at Arecibo in PY2006 toward 22 extragalactic continuum sources. At least 18 new low-N(HI) clouds were discovered. InPY200719additionalcontinuumsourceswillbe observed searching for additional examples of the low-N(HI)cloudphenomenon.Thefocusofthese new observations will be on a detailed comparison of the observational data with several recent theoreticalmodelsfortheproductionoflow-N(HI) cloudsthathaveappearedintheliterature.

pared with similar parameters from the coincident gamma ray event. Scheduling will be challenging fortheArecibotelescope. TheSGRareexoticstars, perhapsas exoticasstars come in the Milky Way. At the other extreme are dMe stars that, by number, account for more than 75%ofthestellarpopulationinthesolarneighborhood. Many dMe stars exhibit significant levels of coronal activity due to the strong magnetic fields that cover most of their surface. A recent survey oflate-typedwarfsshowedthatmorethan50%of thestarsofspectralclassM4toM9havehighlevels ofmagneticactivity. Flares on the Sun and on dMe stars are now believed to be basically similar in their origin and development. In general, both phenomena are believed to arise from the rupture of a stressed magnetic structure which by magnetic buoyancy is forced upwards through the photosphere into the corona/transition region where reconnection of magnetic field occurs followed by considerable energy release. In this model, the parameters of the radio emission that derives from the flare can beusedreliablytoinferthepropertiesoftheflare. In PY2007 the Arecibo telescope will be used to monitorthewell-knowndMeflarestarADLeoobserving simultaneously at both radio frequencies (atArecibo)andatvisualwavelengthsfromobservatoriesinEurope.Theobservationsofoscillations in the optical and radio during flares will enable theresearcherstoinvestigatethepropertiesofthe emissionandtoconstrainbetterthesourcesizevia the techniques emerging from solar coronal seismology.

Stars and Nebulae. Soft Gamma-ray Repeaters (SGRs) are a class of unusual sources thought to be very young neutron stars. They are characterized primarily by occasional repeating bursts of low energy (soft) gamma rays, as well as by rare giantgammarayflaresthatareatleasttwoorders of magnitude higher in fluence than the smaller events.Themorecommonsmallamplitudebursts have durations less than ~ 1 sec, have rise times of a few tens of msec, and have fluences that are roughly correlated with duration. In quiescence, SGRs display X-ray pulsations with periods in the range 5-8 sec, spin-down rates in the range 10-11 ­ 10-12, and X-ray emission below 10 keV that is well described by a power law with photon index ~2.SomeSGRsmaybeassociatedwithsupernova remnantsbutthisisstillcontroversial.
SGRshavebeenarguedasbeing"magnetars",isolated ultra-highly magnetized neutron stars. The pulsed emission mechanism was conceived of as beinganalogoustotheradiopulsarmechanismin which the rotational spin-down powers the radiationprocess.Analternativeviewrecentlypresented argues instead that the gamma ray bursts are a result of magnetic energy stored in the non-potential magnetic fields in the magnetosphere that periodically lead to reconnection-type events such asiscommoninthesun. In PY2007 these two models will be tested by simultaneous radio and gamma-ray observations of SGR 1900+14 scheduled as target-of-opportunity sessions triggered by spacecraft such as Swift and RXTE. The rise time of the radio event, the time of its peak brightness and its duration are the observationalparametersofgreatestinteresttobecomNAICAPRPP2007

Pulsars.ThethirdoftheALFAscientificconsortia isthePALFAgroupthatisconductingalarge-scale pulsar survey of the Galactic plane. These survey observationsbeganinPY2005andwillcontinuein PY2007. The survey is expected to lead to other spinoff proposals, including a proposal for timing observationsofthepulsarsdiscovered.
Radio pulsars continue to provide unique opportunities for testing theories of gravity and probing states of matter otherwise inaccessible to experimentalscience.Inlargesamples,theyalsoallowdetailed modeling of the magnetoionic components of the interstellar medium. For these and other reasonsalarge-scalesurveythatbegaininPY2005 aims todiscoverrareobjectsespecially suitable for
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their physical and astrophysics payoffs. Of particular importance are pulsars in short-period orbits with relativistic companions, ultrafast milli-second pulsars(MSPs)withperiodsP<1.5msthatprovide important constraints on the nuclear equation of state and MSPs with stable spin rates that can be used as detectors of long-period (> years) gravitational waves. Long period pulsars (> 5 sec) are of interestforunderstandingtheirconnection,ifany, withmagnetars.Additionally,anyobjectswithespeciallylargespacevelocities,asrevealedthrough subsequentastrometry,willhelpconstrainaspects of the formation of neutron stars in core-collapse supernovae. While particular, rare objects will be the initial focus of survey follow up observations, long-termpayoffwilloccurfromthetotalityofpulsar detections, that can be used to map the electron density and its fluctuations and the Galactic magnetic field. Finally, multi-wavelength analyses ofselectedobjectswillprovidefurtherinformation onhowneutronstarsinteractwiththeISM,onsupernovae-pulsar statistics, and on the relationship of radio pulsars to unidentified sources found in surveysathighenergies. ThePALFAconsortiumwillconductaGalacticcensusofradiopulsarsthataimstodetectatleasthalf of the active radio pulsars that are beamed at us. Taking beaming and the radio lifetimes of pulsars intoaccount,thefiducialbirthrateofneutronstars, onepercentury,impliesthatthereare2x104detectablepulsarsintheGalaxy.Approximatelyonequarter of these pulsars are in the Arecibo sky so thereareabout5000pulsarsaccessibletoArecibo, halfofwhichareatlowGalacticlatitudes. One can describe three primary motivations for a largescalepulsarsurvey: 1.Thelargerthenumberofpulsardetectionsthe morelikelyitistofindrareobjectsthatprovide the greatest opportunities for use as physical laboratories. These include binary pulsars as described above, and also those with black hole companions; MSPs that can be used as detectors of cosmological gravitational waves; MSPs spinning faster than 1.5 ms, possibly as fastas0.5ms,thatprovetheequationofstate under extreme conditions; hypervelocity pulsars with translations speeds in excess of 1000 km/s,whichconstrainbothcore-collapsephysics and the gravitational potential of the Milky Way;andobjectswithunusualspinproperties, suchasthoseshowing"glitches"andapparent
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precessionalmotions. 2. In a full Galactic census the large number of pulsarscanbeusedtodelineatetheadvanced stagesofstellarevolutionthatleadtosupernovae and compact objects. In particular, with a largesamplethebranchingratiocanbedeterminedfortheformationofpulsarsandmagnetars.Fromalargesample,onecanalsoestimate theeffectivebirthrateforMSPsandforthosebinary pulsars that are likely to coalesce on time scalesshortenoughtobeofinterestassources ofperiodic,chirpedgravitationalwaves. 3.Amaximalpulsarsurveycanbeusedtoprobe andmaptheISMatanunprecedentedlevelof detail.Measurablepropagationeffectsinclude dispersion,scattering,Faradayrotation,andHI absorption that provide, respectively, line-ofsight integrals of the free electron density, of thefluctuatingelectrondensity,oftheproduct of electron density and line of sight magnetic field,andoftheneutralhydrogendensity.Together,theseparameterswillallowmoreaccuratemodelsoftheGalaxytobeconstructed. CanonicalpulsarsandMSPsaccountfor~90%and ~10%ofallpulsars,respectively,withrelativisticbinaries and high-field pulsars comprising < 1%. It wouldnotbesurprisingtofindadditionaltypesof pulsarsinahigh-yieldsurvey.Thatexpectationisa primarydriverforthePALFAsurvey. Pulsars, as extremely precise "clocks" fully embeddedinavarietyofastrophysicalenvironments,are usedtoprobethoseenvironmentsandthephysics that applies in that environment. This is done by repeatedlytimingthepulsars--comparingthemeasured arrival time of a pulsar's signal to the time expectedonthebasisofpriormeasurements.Any departure from these two times can be attributed to motion of the pulsar resulting from local forces; the nature of those forces can be investigated. In PY2007 the following pulsar timing programs are planned: 1. High precision timing of the double neutron star system J1829+2456 over the next year willenableadirectmeasurementoftheproper motionofthesystemtobemadeandfromthat one can establish how much of the dP/dt results from secular acceleration. A value of dP/ dt corrected for proper motion will permit the ageofthepulsartobecalculated.Alreadythe
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agelowerlimitis12.9Gyr.SuchalargeagealreadyimpliesthatJ1829+2456hadabirthspin period close to its current value, 40.1 msec. Knowledge of the transverse velocity can also be used to model the kick produced by the birth of the neutron star and so constrain the initialconditionsofthesystem. 2. TimingobservationswillbeginofPSRJ1903+03, the first millisecond pulsar to be discovered in the Arecibo PALFA survey. With a period of 2.15 ms and a dispersion measure of 297 pc cm-3,thisisaperfectexampleofashortperiod, high DM pulsar to which the PALFA survey is uniquely sensitive. PSR J1903+03 is a uniquely distant and precise pulsar which will allow changesinDMtobetrackedaccurately.Variations in DM provide a direct measurement of the integrated spectrum of electron density fluctuations in the ISM along the line-of-sight. Conventionalwisdomholdsthattheamplitude ofDMvariationsisrelatedtothesquarerootof thedistancetoapulsar;timingofPSRJ1903+03 willallowthistobetestedoveramuchgreater distancethancouldbedonewithanyprevious mspulsar. 3. Overthepastyear,severalmysteriousneutron starshavebeenfoundwithveryunusualproperties. Among these is the new population of Rotating Radio Transients (RRATs). These objectsarecharacterizedbyradioburstswithdurations between 2 and 30 ms and average intervalsbetweenburstsrangingfrom4minutes to3hours.PSRJ0628+09isaRRATdiscovered in the Arecibo PALFA survey with a period of 1.2 s; timing observations will help greatly in establishing its nature. PSR B1931+24, a 813mspulsarwithatypicalageandmagneticfield, is another mysterious transient pulsar. This "sometimes pulsar" mysteriously turns off and on in a quasi-periodic fashion, with intervals between "on" and "off" periods ranging from 25 to 35 days and on intervals lasting 5 to 10 days. This is the first time that something like this has been seen for any pulsar and it points to a massive increase in magnetospheric outflowwhenthepulsarison.Thisobjectandthe RRATs together have challenged our understanding of pulsar emission mechanisms and highlighted how little we know about pulsar properties and populations. Timing observationsinPY2007willaddressthisdeficiency.

4. Timing of the double neutron star system PSR B1534+12 will (a) improve the measurement of profile variation on orbital timescales, and hencerefinetheuniquemeasurementofspinorbit coupling in a strongly self-gravitating system; (b) improve the measurements of the post-Kepleriantimingparameterssandrtoimprovethepurelyquasi-statictestofgeneralrelativity--animportantcomplementtothemixed quasi-static/radiativetestinPSRB1913+16(the Hulse-Taylorpulsar);(c)betterdeterminedP/dt and hence the GR-derived distance to the pulsar, an important input to the expected event ratesforLIGO;(d)monitordispersionmeasure changes and provide ephemerides for VLBI observations; and (e) produce a calibrated 2dimensionalmapofthepulsarbeamshape. 5. Continued timing of the young relativistic binary pulsar PSR J1906+0746 discovered in the PALFA survey. This young pulsar is in an eccentric 4-hour orbit. Timing observations over thelastyearhavefacilitatedameasurementof the time dilation as well as the shift of periastron passage, resulting in mass estimates for the pulsar and its companion. These indicate thtthecompanionismostlikelyasecondneutronstar.Onthetimescaleofyears,weexpect tomeasuretheorbitalperioddecay,whichwill overconstrain the system and provide a test of strong-field gravity. The pulsar shows strong profileevolutionwithtime,whichisbeingused to investigate the pulsar's 2-dimensional beam shape and the phenomenon of geodetic precession. Finally, an attempt will be made to identify radio pulsations from the companion star. 6. High precision timing of nine millisecond pulsarsatmonthlyintervalsovertwoyearswillbe used to establish improved determinations of neutronstarmasses,measurepulsarparallaxes andpropermotions,setlimitsonthepresence of a gravitational wave background, and test and measure terrestrial clocks, ephemeredes, andreferenceframes.Differentapplicationsrequire different observing strategies. For some applications, such as measurement of relativisticsecularchangesinorbitalelements,intense campaignsatseveralwidelyspacedepochsare optimal. For other applications, most notably astrometryandgravitationalwavebackground measurements, it is best that the observations be made continuously and uniformly over
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manyyears. Pulsarsarestrikingsourcesofcoherentradioemission but the nature of their radio emission is far from understood. The physics of the process by whichradiofrequencyemissionisgeneratedinthe magnetospheres of neutron stars will be explored inPY2006throughseveralobservationalprograms atArecibo,twoofwhicharethefollowing. 1. PSRB1951+32isayoung39.5-mspulsarinthe core of the supernova remnant CTB 80. The pulsar's spin-down age of 107 kyr is comparable to the age determined from its proper motion and to the dynamical age of CTB 80. LocatedneartheedgeofthecoreofCTB80and moving rapidly away from the center of the remnant,thesystemrepresentstheinteresting stage of pulsar evolution when the neutron star penetrates and interacts with the interstellar medium swept up by the remnant. The pulsar'srelativisticwindtheninteractswiththe supernovashell,re-energizinganddistortingit and causing the emission of electromagnetic radiation over a broad range of wavelengths. One would expect that PSR B1951+32 would exhibit giant pulses because it shares many similarities with the prototypical giant pulse pulsarintheCrabnebula.Theobservationsto be conducted at Arecibo in PY2007 aim to improveoutknowledgeofgiantpulsesbysearchingforsuchemissionfromPSRB1951+32.Besides being very energetic, giant pulses are characterized by narrow pulse widths, high degreesofpolarization,andpowerlawenergy distributions.Itwillbeveryinterestingtoseeif PSRB1951+32hasallofthesecharacteristics. 2. The question of whether the same physical mechanism operates to produce pulses in all pulsars is a challenging one to answer. One approachtotheanswerbeingpursuedatArecibo in PY2007 is to study the giant pulses in the pulsar in the Crab nebula and compare them with high time resolution observations of three other bright pulsars. In previous observationsoftheCrabpulsarstrikingandunexpected intrinsic differences were found in the dynamic spectrum of the main pulse and the interpulse. The time and spectral signatures of the main pulse are consistent with one proposed model of pulsar radio emission; those of the interpulse cannot be explained by any currentmodel.Thenewobservationsofother
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brightpulsarssimilartotheCrabpulsarwilldeterminewhetherthedynamicspectraofother, more `normal' pulsars resemble either type of spectralbehaviorseenintheCrabpulsar.

Solar System Studies. TheNAICAreciboObservatory has the unique capability to offer its users theopportunitytostudysolarsystemobjectsusing passive radio astronomy techniques and using active radar observations. Both capabilities will be usedextensivelybyresearchgroupsinPY2006.
Comets are a primary target as they offer us a glimpseofprimitivematerialfromthesolarnebula that has had little or no chemical or thermal processing since its formation as part of the pre-solar nebula.Manyofthetracegasesincometiceshave spectral lines in the visible and near-infrared, but thebulkofthecometnucleusismadeupofwater ice, which is difficult to observe from the ground. The radio OH lines at 18-cm wavelength are one ofthefewways to measurethewater abundance in the coma of a comet, and to infer the mass loss rate. ThefluxofOHemissionisrelatedtothetotalnumberofOHmolecules,whichinturnisrelatedtothe watersublimatedfromthecometnucleus.Passive radiospectroscopyhastwoadvantagesoversmall aperture optical and UV spectroscopy. First, the large radio beam provides an integrated measurementoftheamountofOHinthecomaandisless affectedbytimevariabilityoroutgassingmorphology.Second,measurementsofthewidthandshape oftheOHlinesmaybeusedtoinferthevelocityof gases in the coma and to assess the uniformity of water production over the nucleus. Determining the water production rate and outgassing velocity is important to determine the production rates of trace gases in the coma. The water production rate is also needed in order to compare comets to eachotherandtodetermineabsoluteabundances oftracegasesanddust. Interpretation of radio OH observations depends on the line excitation mechanism. The excitation of the OH ground state doublet in comets is accomplishedbyabsorptionofsolarUVphotonsfollowed by cascade back to the ground state. The rateofexcitationdependscriticallyonhowthesolarspectrumisDopplershiftedasseenbythecomet. At some radial velocities, the doublet may have its population inverted or anti-inverted, providing a natural amplification or absorption of the
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cosmicmicrowavebackgroundbehindthecomet. Atotherheliocentricradialvelocities,however,the populationinthedoubletisthermalandthelines becomedifficultorimpossibletodetect.Whileitis best to observe at times in the comet's orbit when the excitation is favorable, it is also a good constraintontheinversionpredictionstoobservenear the time when the excitation crosses from inversiontoanti-inversion,orzero-crossingvelocities. In highly productive comets, OH spectral lines in the inner coma appear weaker than expected because gas collisions thermalize and quench the maseremission.Inlessproductivecomets,thedegreeofquenchingshouldbelower--itdependsinversely on the square root of the production rate. Quenching can strongly affect the water production rate inferred from the line flux and hence it is importanttogainabetterobservationalandtheoreticalunderstandingofthismechanism. Opportunities to observe comets are rare. In PY2007 extending into PY2008 OH observations will be made of the following seven comets: C/2006 VZ13 LINEAR, 46P/Wirtanen, 8P/Tuttle, 6P/d'Arrest, 15P/Finlay, 144P/Kushida and 19P/ Borrelley.Forallthesecometsobservationswillbe made three times on two adjacent days over the 3 weeks or so that each comet is visible from Arecibo. Experience with previous OH observations of comets done at Arecibo has shown that repetitive observations are indispensable for separating short-termvariabilityfromoutgassing,whileobservational spacing by a week or more are necessary tocharacterizelong-termvariations. Comet Tuttle that will be in the 2007 winter sky will be the subject of a worldwide observational campaign;theAreciboOHobservationswillbean important contribution to the "big picture" for this object.CometBorrellywasthetargetoftheDeep Space 1 mission, so it has a known shape, spin period and surface geology. This information makes observationsofOHinthiscometparticularlydesirable:aknownnucleussizeallowsthegasproduction rates to be used to estimate what fraction of the surface is active, and a known spin period can be used to link periodic changes in outgassing to changingsolarfluxontoactiveregions. Thesampleofsevencometsinthenext18-months or so will provide a fortuitous sample of objects fromwhichimportantdiagnosticcomparisonscan bemade.
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The unique capability at the Arecibo Observatory to make radar observations of solar system objects--planets, satellites, comets and asteroids--facilitatespreciseorbitaldynamicsmeasurementsbecause ofthe exceptionalrange(timeofflight) and radialvelocityprecisioninherentinradarmeasurements.SeveralobservingprogramsinPY2007will exploit this capability for innovative astrophysical measurements. Oneobservingprogramwillobtainpreciseastrometry of the NearEarth Object (NEO) 2000 EE14 to test general relativity. Briefly,NEO 2000 EE14 has aperihelionshiftrateof15arcsecondspercentury due to general relativity and the oblate Sun. The measurementsplanningforPY2007constituteone componentofalargerobservingprograminwhich theorbitsofadozenNEOsaremonitoredoverseveralyearstoreduceuncertaintiesonGRparameters andtoprovideadynamicalmeasurementorupper bound on the gravitational quadrupole moment of the Sun (J2). Considerable improvements over previous studies involving measurements of the perihelion shift of Mercury and Icarus are expectd because (1) several newly-discovered asteroids have orbits offering a better sensitivity to the solar J2; (2) the sample of NEOs incorporates a range of heliocentric distances and inclinations that can unambiguouslyseparateGRandJ2effects;and(3) thecenterofmasslocationsofsmallbodiesismore accuratelydeterminedthanthatofMercury. Simulations show that radar measurements of a dozen NEOs to be accumulated over the next 15 yearscandiscriminatechangesinthePPNparameteratthe10-4levelandchangesinJ2atthe10-8 level.Thiswouldimproveuncertaintiesonbyan order of magnitude and would put the preferred helioseismology value of J2 to a very serious test with a direct dynamical measurement. The radar measurements offer clear prospects for improved and independent estimates of the GR and J2 parameters. Radar is an exceptionally powerful probe of the surfacecompositionofasteroidsandplanetarysurfaces. In PY2007 radar observations will be made of the asteroids 2005 NW444, 2005 GL and 2005 WJ56inordertostudythesurfacephysicalproperties and to search for the presence or absence of regolith on these objects. These asteroids make close approaches to Earth in the coming year; observations will also provide precise rotation rates andsizemeasurements.Iftheincidentradarwave
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refracts into a surface and is reflected by buried scatterers, the return echo will have a net linearly polarized component that can be measured using throughafullpolarimetricanalysis.Thistechnique has been used to study the lunar regolith and Venus volcanic deposits, and has been successfully applied to the astroids 1999 JM8 and 4179 Toutatis,bothofwhichshowevidenceforregolith.The PY2007 observations are part of a larger project to observe a sample of asteroids and correlate the radar polarimetric properties with different sizes, shapesandcompositions. Asteroids in general constitute an enormous, diverse population of solid bodies whose study is essential to our understanding of the origin and evolutionofthesolarsystem.Somemightberemnants of the first material to accrete from condensatesintheprimitivesolarnebula,whileothersare thought to have undergone varying degrees of melting, internal differentiation, and chemical alteration. Virtually all have suffered collisions, and many are probably either pieces of ancient disrupted bodies or gravitationally bound collections offragments.Asteroidsdemonstrateprimaryprinciples governing planetary evolution at accessible scales, and a comprehensive understanding of asteroid formation circumstances and evolutionary histories is one of the fundamental goals driving planetaryscience. Radar is the most powerful ground-based techniqueforphysicalcharacterizationofasteroids,primarilybecausemeasurementsofthedistributionof echopowerintimedelay(range)andDopplerfrequency (radial velocity) provide spatially resolved images that can be inverted to yield global topographic and shape information. The accuracy of radar-based shape reconstruction depends on the echo signal-to-noise ratio and the images' coverageinorientationaswellasonthetarget'sshape, spin state, and scattering properties in a manner thathasbeenexploredandcalibrated. Many NEOs have been imaged with the Arecibo radar,and3-Dshapemodelshavebeenpublished for twelve of them. However, echoes from mainbeltasteroids(MBAs)aremuchweakerfromclosely approachingNEOs,andaradar-derived3-Dshape modelhasbeenpublishedforonlyoneMBA.The observations planned for PY2007 will greatly expandthestateofourunderstanding.Twenty-one largeMBAswillbeobservedthatpresentradarobservingopportunitieswithlargesingle-datesignal86

to-noise. Arecibo is the only radar system in the world that has sufficient power and sensitivity for such a project. The objective is to obtain unprecedentedinformationaboutthelarge-scale(several kilometer) structure of the radar-facing portions of the surface. Under ideal circumstances, inversion of the images to estimate a global 3D shape model may be warranted. However, even if too muchofthesurfaceremainshiddenfromtheradar (because of a high subradar latitude or a rotation period that precludes thorough Arecibo rotation phasecoverage),theshapeinversionsoftwarestill can estimate the topography of well-imaged portions of the surface and can simultaneously use lightcurvedatatoplaceconstraintsontheoverall shape. These observations will produce the first comprehensiveshapeinformationdatasetonmain beltasteroids. Again,inPY2007,NEOobservationsprovidesome important targets. Specifically, observations will be made of the asteroids (3200) Phaethon, (4954) Eric,(11500)1989URand2005WJ56.Theseprecisionobservationswillbeusedtoconstructphysical shape models, understand their surface properties, search for satellites and refine the orbital parameters. Phaethon and Eric are among the largest objects in the NEO population. Phaethon istheparentbodyoftheGeminidsmeteorsbutunlikeothermeteorparentbodies,itisclassifiedasan asteroid and not a comet. Searches for cometary activity have been negative, so its origin remains enigmatic. The observations planned for PY2007 will resolve a controversy concerning its diameter and optical albedo. 1989 UR has a very slow rotation period suggestive of non-principal axis rotation, the origins of which are poorly understood. 2005 WJ56 will be an extremely strong target; radar imaging will place thousands of pixels on its surfaceandwillrevealsurfacefeaturesinspectaculardetail. Finally, the Moon will be imaged once again in PY2007 at ever higher angular resolution. The increased angular resolution comes from developmentofmoresophisticatedwaysoffocusingradar images collected over long integration periods yielding spatial resolution as fine as 20-m at 12.6cm radar wavelength and 150-m at 70-cm radar wavelength. At 20-m resolution, the images are comparable to the best existing large-are spacecraft photos. The observations planned for the Arecibo telescope this year will address significant outstanding questions regarding the geologic his NAICAPRPP2007


toryoftheMoon'ssurfaceandtheresourcepotential of volcanic ash deposits and shaded polar areas.Theworkproposedforthisyearbuildsonthe analysisofsimilarobservationsoverthepastseveral yearsthathaveaddressedissuessuchasiceatthe lunar south pole, the origin of dark haloes around many impact craters, and the distribution of Mare Orientale related cryptomaria. These subjects are ofkeeninteresttothoseplanningexploratoryvisits to the Moon. It is satisfying to be able to provide the fundamental insight from ground-based radar observationsmadeattheAreciboObservatory.

pointtowhichthetertiarymirrorcanbedrivenreliablyandrepeatedlyintheeventapowerfailureor a computer failure should occur while the tertiary is in motion. In addition, calibrating the physical motion of the tertiary in terms of its effect on the telescope pointing is a major task for which Phil Perillat's involvement and experience will be indispensable.Thiswillbedoneaspartofthetelescope re-pointing following completion of the platform paintingproject. Thetertiarymirrorcontrolprojectrequiresapproximately$50kinmaterialsexclusiveofanymaterials required to correct RFI problems. Operationally, theplanistomovethetertiarymirrorinfrequently among two, or a small number of `optimum' positions chosen for the requirements of particular weatherconditions.Thedrivemotorswillbepowereddownbetweenmotionstoeliminatethepossibility of spurious RFI. NAIC PY2007 funds have been allocated to this project as has the priority time of engineer Comacho. The project is scheduledforcompletionearlyinPY2008.

10.2 Technical Plans
Telescope: Tertiary Mirror Motion and Control. With the addition of the Gregorian, it was understood that the telescope focus would be difficult to maintain to high precision during the day when solar heating of the main platform suspension cables caused the cables to lengthen and the platform to descend slightly. This effect, together withtheasymmetricalloadoftheGregoriandome at high zenith angles causes the tie downs to lose tension and, of course, when the tie downs lose tension they lose their ability to position the platform at the correct height necessary to keep the Gregorian receivers in focus. The problem is most acuteathighfrequencieswhereagivenheighterrorisalargerfractionalwavelengtherror.ThedesignsolutiontothisrecognizedproblemintheGregorian upgrade project was to drive the position of the tertiary mirror changing the focal position by the amount necessary to compensate exactly fortheslackinthetiedowns.Allthetertiarydrive motorsandcontrollerswereinstalledaspartofthe Gregorian upgrade project. But they were never calibrated and have never been used because the drivemotorswerefoundtobesourcesofRFI.
With the increased demand for observations at Xband, and especially for the increasingly frequent useofbothX-bandandC-bandduringthedayfor VLBIobservations,itwasapparentthatitwastime to implement the capability to move and control thetertiarymirror.InPY2007aprojecthasbegun forthistask.HectorComacho,thenewleadofthe AO digital engineering group, has project responsibility. He is working in close collaboration with Mike Nolan and Phil Perillat to define the problem andeffectasolution. Thescopeofworkincludesestablishingahardfiducial on the tertiary drive, a fundamental reference
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Telescope: Platform Painting Project. Concerned about the condition of the coating on the platformoftheArecibotelescope,NAICcontracted with the consulting firm of KTA-Tator, Inc. of Pittsburgh, PA to conduct a condition analysis of the coating on the structural steel platform. The KTA reporthighlightedanumberofconcerns,themost important of which is that the steel in the original telescope construction is covered with mill scale that was not removed at the time the steel was fabricated in the early 1960s. The mill scale peels offovertime,andhasdonesoontheArecibotelescope, allowing moisture to seep under the mill scale and cause corrosion in the base metal. The only remedy for this situation is to clean the steel abrasively(e.g.sandblastit)removingthemillscale downto"whitemetal"andthenprimeandrecoat thesteel.
NAIC worked with the KTA consultant to define carefully the scope of work for the entire cleaning and coating task including the choice of primer and finish coat to be used. Recommendations as to the tools to be used for the job, and the techniques necessary to apply a durable coating were alsosuppliedtoNAICbytheKTAconsultant.With the help of KTA, a bid package was prepared and distributed to potential contractors: six bids were received. Spensieri painting of Syracuse, NY was selected. The contract with Spensieri was negoti 87


atedandsignedinJanuary2007. TheplatformpaintingprojectwillbegininPY2007. Work on the telescope will require approximately 12 weeks. Funding has been arranged from a combinationofNAICcarryoverfundsandNSFnew funds provided through the Cooperative AgreementinPY2007.

of the critical items mentioned in the A&W 2003 conditionreportarebeinginspectedregularlywith no problems noted. A crack prone sharp corner mentioned in the A&W condition report was discussed in the last meeting and recommended for modification. Felipe will make this modification in thenearfuture." Owing to the extensive experience of the people ontheTigerTeam,theTigerTeamismeanttoidentify concerns and propose maintenance tasks that theteamitselfbelievestobeinthebestinterestof NAIC'sstewardshipoftheArecibotelescope.They dothis.Whatfollowsisthediscussion,recommendations and actions from the Tiger Team meeting ofFebruary2007. Thestressesinthemaincableselicitedseveralcomments. Don Campbell reminded [the Tiger Team] that we agreed to remeasure the catenary in several cables, especially the ones with unbalanced loads to double check the results from the previous tension survey. Phil Perillat emphasized that the measurements be made with consistent settings of all drives (dome, carriage house, azimuth arm, tie downs) and consistent temperature. The cabletensiondataistakenatafixed,balancedcondition. A study by A&W to quantify the effect of thedynamic,unbalancedloadsthecablesencounter during operations is planned. This study has beendelayedbypreparationsforthepaintingproject which also has been delayed. Included in this studywillbeareviewofthemaximumunbalanced torque allowed (Phil Perillat). The unbalanced torque limit has been repeatedly discussed and probably changed since the Gregorian upgrading andshouldbefinallyclarified. FelipeSoberalraisedaconcernaboutpossiblecorrosionjustinsidethecableendsockets.Onebackstaycablehasbeenreplacedinthepastbecauseof broken strands. The broken strands in that cable were probably due to corrosion inside the socket, especially in the outer layer of strands. The corrosion arises because the zinc potting material does not "wet out" the individual strands near the exit point from the socket. The cable interior has dry airpumpedintoitandthereisdryairpumpedinto the socket itself which should eliminate the corrosionbutthesehiddenareasremainaconcern.On apositivenote,therehasnotbeenabrokenstrand reportedsinceJuly2003. Felipe discussed the Gregorian dome elevation wheels.Therehavebeentwowheelsthatcracked
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Telescope: Structural Condition. In 2003 NAIC contracted with Ammann & Whitney to performathoroughsurveyofthestructuralcondition of the Arecibo telescope. The resultant A&W report,AreciboRadioTelescopeStructuralCondition Survey2003,concluded"Thesurveyfindsthatthe telescopeasawholeisingoodcondition butthat thecablesandthefeedsupportsystemareinneed of a complete painting"..."Secondary deficiencies and recommendations can be found in the body of this report". As described in the above section of this APRPP, NAIC has contracted for the structural steel platform to be completely cleaned and painted;inthiswaytheprincipalrecommendation of the A&W telescope condition survey will be implemented. The "secondary deficiencies" noted in the A&W report have been addressed with high priority by the Arecibo Observatory site platform crewinthecourseoftheirroutinetelescopemaintenancetasksoverthepastthreeyears.
In response to external concerns about the efficacy of the NAIC responses to the A&W "secondary deficiencies", NAIC established a telescope "Tiger Team"inMarch2006toreviewtheNAICresponses andtoprovideoversightforfuturetelescopestructural maintenance tasks. The Tiger Team is made up of seven NAIC and Cornell engineers and scientists whose combined experience working with the Arecibo telescope exceeds 150-years. These peopleare:

AreciboTelescopeTigerTeam DonCampbell FelipeSoberal HalCraft MichaelNolan PhilPerillat WilsonArias LynnBaker(Chair)

The Tiger Team meets every other month or more frequently as required. At the most recent meeting,February2007,theTigerTeamminutesrecord the following: "Felipe Soberal confirmed that all
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in service. These wheels were analyzed by Lucius Pitkin, a firm that specializes in inspection and failure analysis. Their conclusion was the failures were due to poor quality control in the induction hardening of the exterior. Felipe is sending more wheels, two operational and two spares for analysis byLuciusPitkin tocheck the quality ofthemetallurgy. Part of the wheel failure problem may be duetothepoorweightdistributionoftheoriginal bogeydesign.Thebogieswereupgradedin2001 toanimproveddesignwithbetterweightdistribution. One of the cracked wheels occured before this upgrade and one after, although the second cracked wheel was in service on the old bogies. There have been no further cracked wheels since then. Thewheelsareinspected and lubricatedoften and microswitches have been fitted to detect anywheelfailures. FelipeSoberalalsoreviewedthestateoftheelevation rail rolling surface. There are some cracks in therollingsurfaceinareaswherethedomespends themajorityofitstimeinoperation.Thesesections will be replaced after the painting project. The cracks primarily arise where the rail is over a panel point which is a very stiff and narrow support point. Felipe recommends welding in a support plate which will spread the support loading over a longer length of rail and reduce the cracking. The committee recomended that Felipe provide a drawingtoA&Wsotheycanreviewthereinforcementconcept. FelipeSoberaldiscussedlooseboltsthatattachthe secondary backup structure to the collar truss in the Gregorian dome. A few of these have been found loose and retightened. Felipe expressed some concern that the bolts may have been overstressedandthatiswhytheywereloose.Thesuggestion was made to replace some of the bolts foundlooseandhavetheremovedboltstestedfor an overstress condition. If the bolts are working loose from vibration or thermal cycling then some methodofholdingthemtightshouldbeapplied. DonCampbellremindedthatanewconditionsurvey should be performed soon, later in 2007 or early2008.Considerationshouldbegiventohaving another firm besides A&W perform the condition survey. Whoever does the survey should be guided by a detailed list of items from NAIC and theTigerTeamcommittee. ThetelescopeTigerTeamisfunctioningeffectively in an oversight capacity to assure Cornell that the
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structural condition of the Arecibo telescope remainssound.

Receivers. As described in Section 4 of this APRPP, two new receivers will be completed and madeavailabletotelescopeusersinPY2007.Both receivers represent new generation technology applied to frequency bands of high priority to the U.S. astronomical community: both replace existingAOreceivers.
Anew2380MHzradarreceiverwasdesignedand builttotherequirementsoftheplanetaryradarsystem. It's primary design specification is to achieve a system temperature on the sky of less than 20K, and improvement of more than 25% over the systemtemperatureofthepresentradarreceiver.This will be the lowest noise receiver on the Arecibo telescope. Further, an advanced feed design will betterilluminatethetelescopeleadingtoanetimprovementintheratiooftelescopegaintosystem temperature, G/T, of nearly 50%. All components of the receiver are complete; assembly is proceedingattheObservatory.Testsonthetelescopewill beginaftercompletionofthepaintingproject;the receiver will be available for visitor use in the third quarterof2007. The second new receiver to be made available to users in PY2007 is the cryogenically cooled 327 MHz receiver also described in Section 4 of this APRPP.Thisreceiveriscompleteandinitscommissioning phase on the telescope. It's primary applicationisexpectedtobeforprecisionpulsartiming programs. The heavily-constrained PY2007 NAIC budget receivedfromNSFASTdoesnotallowforanyfurther receiver design, construction or upgrade maintenanceatNAICinPY2007.

Planetary Radar Transmitter. The 2380 MHz transmitter operates at a peak power of approximately 1MW with the RF power supplied by two klystrons each of which generates 500 kW. Both oftheseklystronshaveneededrepairoverthelast two program years resulting in an extraordinary expense of nearly $250k each year. Fortunately, thebest-effortrepairsweresuccessfulforbothklystrons and the RF transmitter is now running routinelyforallscheduledobservations.
The2380MHzplanetaryradartransmitterisaCW (continuous wave) transmitter that must be sup 89


plied with uninterrupted electrical power of approximately 2 MW. At the Arecibo Observatory this is done using a purpose-specificdieselturbinegenerator.Thegenerator, built by Sun Turbines, a division of Caterpillar Inc, has reached the point in its usage cycle--a combination of run-time and number of starts--that routine major overhaul is required. We have solicited budgetary estimatesfortheturbineoverhaulfromCaterpillar and from third-party vendors. The cost will exceed $350k. The heavily-constrained PY2007NAICbudgetreceivedfromNSFAST doesnotallowfortheupgradetobedonein PY2007.Forbudgetaryreasonsonly,wewill defertheturbinemaintenanceuntilPY2008.

Figure 10.2.1.SpectrometersetupintheArecibocontrolroom.

Backends: Spectrometers. Two new spectrometers will be delivered to AO in PY2007 that are designed for the special requirements of the PALFA survey and the EALFA survey respectively. Each of these spectrometers was built by Jeff Mock under contract to NAIC. The technical specificationsofeacharetabulatedinSection4of this APRPP. The hardware configuration of both is identical. The spectrometers use FPGA-based processors that realize the frequency separation usingdigitalpolyphasefilterswithshapesspecified by the PALFA and EALFA consortium respectively. Both spectrometers process all 14 IF inputs from ALFA (with 2 spares) using 7 processor `boxes', eachofwhichanalyzes2polarizationsfromoneof thesevenALFAbeams.
Jeff Mock brought two `boxes' to Arecibo in January 2007 to test the functionality of these prototypeinstruments,andtochecktheinterfacesfrom theboxestotheobservatoryIFanddatamanagementsystems.Thetestingwasentirelysuccessful. A brief report of the January 2007 testing at AO from Jeff follows below (http://www.mock.com/ pdev/fl_ealfa.html).

Barbara Catinella and Emmanuel Momjian picked outafewknownEALFAobjectsthatwereobservableduringthetelescopetestingtime.Theypointed the telescope to collect both on-source and off-source integrations for three objects. All three objects were reasonably easy to identify, Phil Perillat told me how to properly extract the baseline using the off-source signal to produce these plots. The A&B polarities are summed after integration, thebaselinewasremovedusingtheoff-sourceobservation. NGC 1156 is a reasonably bright object. This is a 60-second integration using two overlapping 8kpoint PFB transforms, each covers 170MHz, the result covers the 300MHz of ALFA. Data was collected with 10ms integrations and assembled into longerintegrationsduringpostprocessing.

Figure10.2.1showsthespectrometersetupinthe Arecibocontrolroom.Therackintheforeground is temporary. Two spectrometers are mounted in the top of the rack. The middle of the rack contains some random attenuators and test signal generators. The two prototype mixers are in the lowerthirdoftherack,andtheservermachinefor Figure 10.2.2. A60-secondintegrationusingtwooverlapdumpingdataisinthebottomoftherack.Thein- ping8k-pointPFBtransforms.(Courtesy:JeffMock) terfacetothetelescopeisthroughconnectionsto UGC 1291isasomewhatdimmerobject.Thisisa theracksinthebackground.Thesignalgenerators 120-second integration using two overlapping 8kin the background racks are used for the 2nd LOs pointPFBtransforms,eachcovers170MHz. andADCclockforthespectrometers.
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Observational Research Program PALFA GALFA EALFA OtherPulsarPrograms Aeronomy

Data Storage Backup Requirements 50.67TB 3.03TB 1.54TB 22.13TB 5.16TB

Figure 10.2.3. A 120-second integration using two overlapping8k-pointPFBtransforms.(Courtesy:JeffMock)

AGC 110443wasthedimmestobjectweattempted to observe. This is a 120-second integration usingtwooverlapping8k-pointPFBtransforms,each covers170MHz.

The server storage at the Observatory is based on scaleable RAID clusters fed by a gigabit Ethernet network. Presently, the RAID volumes cost about $1.50 per GB; removable standalone drives used by many observing teams to transport their data totheirhomeinstitutionscostabout$0.40perGB. Longtermarchiving/backupfacilitiesattheObservatorymakeuseof½-inchcartridgetapetechnologiesandroboticlibraries.Twosuchsystemsarein useatAO: · SDLT-1 (160 GB/tape, write at 15 MB/s, cost$0.25/GB) · UltriumLTO-3(400GB,writeat25MB/s, cost$0.20/GB) Computing clusters are being upgraded to use 64-bit processorsincluding the AMD Opteron and CPUsbasedonthePower5coresystem.Network infrastructure will be expanded to support highbandwidth "spigots" (e.g. USB2 and Firewire) for copying data to portable media so as to facilitate users'desirestotransportextremelylargedatasets totheirhomeinstitutions.

Figure 10.2.4.A120-secondintegrationusingtwooverlapping8k-pointPFBtransforms.(Courtesy:JeffMock)

The competed PALFA and EALFA spectrometers will be commissioned at AO following completion of the platform painting project and will be made available for scheduled use in the third quarter of 2007.

The new PALFA and EALFA spectrometers discussed in the previous section of this APRPP will increase the data flow generated at the telescope many times over. The PALFA spectrometer drives ourrequirementsfordatamanagement;itwillroutinely produce data at a rate of 0.5 TB/hour. Our plans for coping with this enormous flow are to providethefollowing: · · · · · Dual-coreXeonCPU 8-channelSATAIIRAID 6x750GBSATAIIdisks Ultra320SCSIfortapedrive DualGigabitEthernet

Data Management, Backup and Archive at the Arecibo Observatory. The primary goal in PY2007 for computing hardware and data managementistoprovidethestoragecapacityneeded fortheALFAlegacysurveys.Toillustratethescale of the data management problem at AO quantitatively, here are the data flow statistics at the Observatory from the major user programs run in PY2006:

This is all purchased hardware. The heavily-constrained PY2007 NAIC budget received from NSF ASTdoesnotallowforthesepurchasestobemade inPY2007.ThismeansthatschedulingofthePALFA spectrometer will have to be artificially limited
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in PY2007 and/or that the staff assigned to copyingdatafromdisktotapewillhavetobeincreased inordertocopewiththedataflow.Itisaproblem that sufficient, one-time, capital funds can readily solve. One of the major institutional challenges of the ALFA surveys is to provide long-term archival data storageandcommunityaccess.ThevariousALFA surveysrequiretheconstructionoflargedatabases at all stages of data reduction from raw data to finished data product. These databases require permanent archiving, management and access by the science team, construction of data products andtoolstotheiraccessandusebyotherscientists andtheinterestedpublic.Mostofthesurveyswill deliver irreplaceable datasets, irreplaceable either becausetheyareuniquetotheepochatwhichthe observations were made (astronomical phenomena change!) or because they are not likely to be supercededbyfutureonesfortheseveraldecades that it will take before superior observing facilities are operational. For these reasons, in PY2007 NAIC will continue its major initiative to secure archivaldatabasestorageandaccessfacilitiesforthe ALFAsurveydata,anddosobymeansofpartnershipsformedwiththeCornellTheoryCenter(CTC). The CTC has the interest and the expertise to satisfy the ALFA archive requirements. An important consideration for NAIC is that the databases are constructed in full compliance with the guidelines of the Virtual Observatory (VO) so that the ALFA surveys can be "mined" in conjunction with other large astronomical survey datasets constructed at otherwavelengths. Because database management is a skill new to NAIC, and because it is the intent of NAIC to partnerwiththeCTCthatreceivesNSFsupporttomanage scientific data, NAIC will recruit for and hire a database expert to organize and implement this functionality for the ALFA survey teams. The individual hired for this position must be experienced inworkingwiththeVO.

Telescope Platform Painting Project. This project was described in Section 10 of the APRPP. It will begin and be completed in PY2007 with funds provided by NSF/AST that are in addition to thefundsbudgetedinSection12ofthisAPRPP. U.S. SKA Technology Development Project. (a)ProjectPurpose
TheU.S.SKATDPisthefirststepinaprogressionof well-defined steps leading to the next generation radio telescope for meter and centimeter wavelengths,theSquareKilometerArray(SKA). TheSKAwilltransformradioastronomythrougha revolutionary design that combines an increase in sensitivityofafactorof20ormoreoverexistingradiotelescopeswiththecapabilitytoimagelargeregionsoftheskyinstantaneouslyoverawiderange ofangularresolution.TheSKAdesignincorporates asuiteofoperationalmodesthatenablesurveyobservations, targeted studies for imaging and spectroscopic analysis, and time-domain sampling for studies of transient or variable objects. The wide variety of SKA operational modes, its planned frequency coverage from ~100 MHz to 22 GHz or higher,andtheunrivaledsensitivityresultingfrom its enormous collecting area, assures that the SKA discovery space is extremely rich. Key science objectives of the SKA emphasize probes of fundamental physics such as those encapsulated in the eleven questions noted in the National Research Council publication Connecting Quarks with the Cosmos.TheSKAscienceobjectivesincludeprecisiontestsoftheoriesofgravityandexplorationsof thenatureofdarkmatterandofdarkenergy.They also include the cosmic origins of magnetic fields, the origins of black holes and the role played by the galactic nuclei that harbor supermassive black holes in generating through bursts of star formationthelightthatfirstilluminatedthecosmos.Additionally, the SKA will lead us to targets that providekeystoanunderstandingoftheoriginsoflife, keyssuchasorganicmoleculesandaminoacidsin space,theformationofplanetarysystemsand,perhaps, radio signals tracing communications from civilizationselsewhere. Development of the SKA is an international endeavor that is coordinated through the International SKA Steering Committee (ISSC), one third of whose members are affiliated with institutions in theUnitedStates.Presently,severalradicallydiffer NAICAPRPP2007

10.3 Major Project Plans
In PY2007 NAIC is engaged in two major projects, a project to clean (sandblast) and paint the structuralsteelonthetelescopeplatform,andinitiation of work on the 5-year U.S. Square Kilometer Array TechnologyDevelopmentProject(TDP)shouldthe TDPproposalbeacceptedandfundedbytheNSF.

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ent designs for the SKA are being investigated in different countries. In the U.S., nine research universities and seven research institutes have joined together as the U.S. SKA Consortium to pursue a telescope concept meeting the science requirementsoftheSKAthatisasynthesisarraycomprised ofalargenumberofsmalldiameterantennas.This LNSD concept provides the requisite SKA collecting area by utilizing approximately 4400 12-meter diameter parabolic antennas. Each antenna is equippedwithlownoisereceiversandbroadband dataacquisitionanddatatransmissionsystems.By using such conventional technology the technical risk inherent in the LNSD concept is low. But the necessity to cover the enormous SKA frequency range,thenecessitytocombinethesignalsfromall theantennasoverawidereceivedbandwidth,and the necessity to construct and operate such an arrayatanaffordablecostaresignificantchallenges. NAIC, as the managing organization for the TDP, will lead the partnership of U.S. academic institutions to demonstrate that these challenges can be met through the concepts developed in the U.S. SKATechnologyDevelopmentProject. (b)ProjectScope The primary objectives of the TDP are the following: · To design and construct a prototype 12m antenna that meets the SKA requirements and can be used as a cost basisfortheSKAprojectbaseline; · To design and construct prototype receiving systems, including cryocoolers and optical components, covering the entireSKAfrequencyrange; · To demonstrate, through tests on an off-the-shelf 6m antenna built using the technology planned for the 12m prototype, that the SKA requirement for collecting area divided by system temperature(A/Tsys)ismetforthatoneantenna; · To develop algorithms suitable for the LNSD concept for array calibration, imaging,formingofmultiplebeamssimultaneously, radio frequency interference management, and data transport. This work will leverage and extend ongoing studiesbyothersonsimilarissuesforthe Low Frequency Array (LOFAR) and the ExpandedVeryLargeArray(EVLA); · To use a 6m test antenna at the Allen TelescopeArray(ATA)toverifythrough
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observations the performance of feeds, low noise amplifiers and LNSD concept algorithms; · TodevelopamodelofLNSDconceptarrayoperations; · To use experience gained with ATA operations and detailed studies of the prototypeLNSDhardware,todevelopa thoroughcostestimateforconstruction andoperationofthefullSKALNSDprojectbaseline. The successful execution of the TDP will yield a complete project baseline for the LNSD SKA from which construction can begin. As a means to reachthisend,theLNSDtechnologydevelopment projectprovidesaframeworkthateffectivelybrings together a team of experts from many institutions allworkingtoassurethattheSKA,asthenextgeneration radio telescope, will be a worthy research complement to existing and planned telescopes across the electromagnetic spectrum as well as to non-photonic facilities such as gravitational-wave observatories. Together, these facilities will allow scientists and students of the next decades to untanglethecomplexityofthecosmos. (c)ProjectPlan,ScheduleandBudget

The TDP is a stand-alone proposal submitted to theNSFbyNAIC/CornellonbehalfoftheU.S.SKA Consortium. The TDP project plan, schedule and budgetisthoroughlyoutlinedintheTDPproposal. The TDP does not depend on resources provided throughtheNAICCooperativeAgreement,andas suchthebudgetfortheTDPisnotincludedinthe NAICbudgetpresentedinthisPY2007APRPP. ShouldtheTDPbefunded,theprojectwillusefull cost accounting so that the effort of existing NAIC staff working on the project will be properly, and fully,chargedtotheproject.

10.4 Operational Changes in Response to the Senior Review Recommendations for NAIC
The NSF division of astronomical sciences (AST) released the report of the Senior Review panel on November 3rd. The report, http://www.nsf.gov/ mps/ast/ast_senior_review.jsp, includes three recommendationsforNAIC.Theseare: 1. Reduce NSF astronomy division support for Areciboto$8Moverthenext3years;
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2. Schedule the survey programs for 80% of the time used for astronomy on the telescopethrough2010; 3. In 2011, plan either to close Arecibo or operate it with a much smaller astronomy budget; additional funds to be provided by othersources. TheCornell/NAICstatementinresponsetotheSeniorReviewreportfollows.

telescope platform must be removed and the platform re-painted. NSF has endorsed this view and a plan is in place to clean and paint the platform in 2007, a multi-million dollar project to be done via a financial partnership between NSF and Cornell. The platform painting will give the telescope astructurallifetimeof20years. The Senior Review is less sanguine about the priority NSF astronomy funding for NAIC deserves in competition with that of other facilities, particularly new facilities, in the period beyond 2010. The SR report mentions that NSF may want to reduce NAIC astronomy operations funding even further, below$8M/year,in2011.Thereportalsosuggests thatNSFmaywanttoconsiderclosingtheArecibo Observatory after 2011. And finally the SR report notes that the SR charge is to advise NSF for the periodbetweendecadalsurveys,andhenceissues that apply to the post-2010 years are subjects for the next decadal survey committee to consider; they are not issues on which the SR recommendationsaregermane.Clearly,thereisnocommunity consensusyetontheprioritiesforthenextdecade, andtherecannotbeuntilthedecadalsurveyisconducted. In light of this situation, Cornell/NAIC will take no actions that will limit the options available tothedecadalsurveycommittee.Inparticular,no planningwillbedone,oractionstaken,leadingto closureoftheAreciboObservatory. The primary recommendation of the SR report for NAIC/AreciboObservatory,thatfundingfortheastronomy program be reduced from $10.5M annually to $8M annually over 3 years, is one that Cornell/NAIC will implement by reducing the scope of the astronomy program. Although this cut of nearly 25% in the budget of the NAIC astronomy program will necessitate that major changes be made,itwillalsomotivateNAICtofocusondeveloping new research capabilities, particularly those that enable high-priority, community-based, radio science initiatives such as the international Square Kilometer Array to proceed expeditiously to completion. In order to accommodate the $8M annual budget for the astronomy program, the scope of the astronomy program will change from one in which the NAIC Arecibo Observatory offers a full range of instrumentation and support services for radio astronomical research, to a more limited program that focuses on the unique ability of the world's largestradiotelescopetosurveyandstudyfaintob NAICAPRPP2007

Cornell/NAIC Statement. Cornellfullysupports thegoalstheSeniorReviewandsharesintheview that science is a forward-looking enterprise; new research facilities are essential to future progress. Cornellisalsoproudofthescientificachievements thathavebeenmadeattheNAICAreciboObservatorybycreativeresearchersoverthemorethan40 years that Cornell has managed and operated the Observatory.Weappreciatethesupportivewords ofpraiseintheSRreportcongratulatingCornellon itseffectiveoperationofthefacility.
The NAIC Arecibo Observatory is a facility of the National Science Foundation. Cornell manages NAIConbehalfoftheU.S.scientificcommunityfor the advancement of radio science. The principal stakeholder in NAIC is the U.S. scientific community. If the U.S. scientific community, through the Senior Review or some similar community-based, informed, process recommends that changes should be made in the way NAIC is funded or in thescopeoftheservicesitprovidestothecommunity, Cornell/NAIC will work conscientiously with the community and its NSF sponsor to implement thosechanges. TheSeniorReviewrecommendsthatoverthenext 3 years the NSF funding for support of the NAIC astronomyprogramshouldbedecreasedbynearly 25%, from an annual budget of $10.5M to annual budgetof$8M.Cornell/NAICispreparedtomake the changes in the scope of the NAIC astronomy program, and in the operating structure of the Arecibo Observatory, that will enable the adjustment to a much reduced astronomy program to bemade.Inplanningforsuchchangeswerecognize, as did the Senior Review report, that there is every reason to expect that the Arecibo Observatorycanbescientificallyproductiveforthenextdecadeandevenfurtherintothefuture.Inorderfor thistohappen,CornellhaspointedouttotheNSF that the long-term safety of the Arecibo telescope requires that the accumulated corrosion on the
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jectsintheuniverse.Specificreductionsinscopeof theastronomyprogramincludethefollowing: WewilleliminateallAST-supportedNAICprogram elements that are not directly related to operation oftheNAICastronomyresearchprogram.Wewill reduce the number of telescope observing hours for astronomy to approximately 3800 hours per year.(Nowitis4800hoursperyear). · Nearly all astronomy observations on thetelescopewillbescheduledatnight, leaving the days free for maintenance activities. · We will do telescope and instrument maintenance 8-hours per day, 5-days perweek(Monday-Friday). · Because80%oftheastronomyobservationswillbeforsurveyobservations,we willreducethenumberofreceiversavailableforastronomyobservationsfrom13 to6.Thiswillmakeiteasiertomaintain theremainingreceivers. · The survey observations require less local support. Accordingly, scientific and support services in many areas will be reduced. · Wewillencourageremoteobservations to reduce the number of on-site visitors requiring Observatory assistance. This will enable us to reduce the cafeteria hours,andtripstotheairport,forexample.Studentvisitsfortrainingstillwillbe encouraged. · WewillcontinuetooperatetheArecibo Planetary Radar in FY2007 as we seek additional support for it from NSF and othersources.

moreyearsimmediatelyfollowingthat,theNAICis working in partnership with the U.S. academic research community toward the following common goals: · Operate and maintain the first highthroughput survey instrument at the Observatory, the Arecibo L-band Feed Array(ALFA),thatisdesignedtoenable rapid,large-scale,skysurveys.Thisproject is being done as a cooperation betweenNAICandthreeverylarge(50-75 member) topical consortia of academic researchers; · Develop and provide funding for backend instrumentation and software for ALFA as joint initiatives between NAIC and experienced university-based researchers. This includes, but is not limited to, fabrication, commissioning and operation of the PALFA and EALFA spectrometers; · Implement and augment "commensal" observing,asharingoftelescopetimein which the signals from the ALFA front ends are analyzed simultaneously by twoormorespectrometersoperatedby groupswithdifferentscienceobjectives, but with a common need to survey the skyatL-band; · Develop and assure the implementation of ALFA legacy databases that are accessible to all researchers through the Virtual Observatory so that use of the ALFA data products are a primary mechanism for students and scientists of all disciplines to benefit by the programmaticmissionofNAIC; · Build on the multibeam experience of ALFA for the design, prototype and construction of the next generation of phased array focal plane receivers for the Arecibo telescope as informed by thedesiresandinvolvementoftheuser community. This technology development initiative has relevance to the technicalrequirementsoftheSKA; · DevelopfurthertheAreciboresearchcapabilities in support of Very Long BaselineInterferometry(VLBI)inpartnership with the U.S. community of researchers using the VLBA and the HSA, and the communityofEuropeanresearchersusing the EVN. The cornerstone task in
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11. Longe Range Report and Plan
11.1 Major Program Goals and Emphasis
TheoverridingprogramgoalofNAIC,ontheshort term as well as on a much longer term, is not to build and operate large research facilities for the academicresearchcommunity,butrathertobuild, operate and manage major research facilities with thecommunity.InPY2007,andinthefiveyearsor
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·

·

·

·

·

·

·

· · ·

thenextfiveyearsisafour-foldincrease in the data rate from Arecibo to the internetbackboneinthemainlandU.S.; Evaluate concept designs for low-cost radio antennas of modest aperture, a prototype of which would be connected interferometrically with the 305-m Arecibo telescope as the foundation of a major initiative to search for cosmic sourcesoftransientradioemission; Install, operate and maintain an ionospheric heating facility (HF) on the Arecibo telescope with technical specification established through consultation withtheU.S.aeronomycommunity; Develop and fund the HF feed design and fabrication as a joint initiative betweenNAICandexperienceduniversity researchers; Maintain, operate and enhance the unique 2.380 GHz planetary radar system at Arecibo in response to community-generated needs. As noted in section 10 of this APRPP a near-term goal is to assure that the required overhaul of the turbine electric generator can be completedinthenextprogramyear. Serveasthemanagingorganizationfor U.S. participation in the International Square Kilometer Array (SKA) project, the next generation facility for radio astronomicalresearch; EstablishaProjectOfficeatNAICforthe U.S.SKATechnologyDevelopmentProject (TDP) and provide the project management for the TDP needed for the successful execution of all participating universityeffortsontheTDP; Createaneffectiveoutreachstructureto foster greater interest and involvement insciencebyunderservedminoritypopulations in Puerto Rico and throughout theU.S.Hispaniccommunity; Developprogramsthatenhancetheresearch participation of undergraduate studentsinresearchatNAIC; EnhanceNAICinvolvementinSpectrum Management,internationally,nationally andlocally; Organize community meetings to define the scientific requirements and technical specifications for an incoherent scatter radar research facility to be builtattheArecibomagneticconjugate


pointinArgentina. Noneoftheseobjectivescanbeachievedwithout effective partnerships. In the case of the major scientific initiatives--ALFA, SKA, HF--these partnerships are with the U.S. and international scientific communities. Other partnerships, such as the initiative to implement an interferometric capability at Arecibo, are with colleges and universities in Puerto Rico. Cornell University, through its faculty involvement in NAIC, is an effective partner in fosteringthemulti-institutionalcollaborationsneeded to promote research endeavors. In particular, the Cornell faculty provide NAIC with an important interface to the U.S. university-based scholars and students because they work in the same environment and have the same needs as their peers at institutionselsewhere.Theyfacilitatepartnerships. Cornell provides the intellectual framework to fosterthegrowthofseveralofthesepartnerships.

11.2 Risk Factors Affecting Program Goals
The primary risk factors limiting NAIC ability to achieve its partnership goals are budget and the widely-read recommendations in the NSF/AST Senior Review report that refer to NAIC as a facility "in transition" from a viable national research institution to one slated for closure. Fostering partnerships is an investment in trust. If one potential partnerhastheimpressionthattheotherpotential partner cannot be trusted to carry out his responsibilities in the partnership, that partnership will never get off the ground. The Senior Review recommendation that NAIC be closed in 2011 badly eroded the confidence of NAIC partners and potentialpartnersinthelong-termstabilityofNAICas anationalcenterwithwhichmajorprogramsmay bedevelopedandimplemented. TheNAICbudgetisarelatedconcern.InSection2 of this APRPP we showed the NSF funding history of NAIC, and of the NSF Division of Astronomical Sciences (AST), for the decade beginning in 1999. WereproducethatplotinFig.11.2.1.Intheeightyear period 2000-2007 in which the AST budget doubled,ASTfundingforNAICdeclinedsteadilyin real terms, never once in those eight years meeting the rate of inflation. These were the 8-years inwhichNAICtookfinancialresponsibilityfortwo majornewresearchprograms--theAreciboplanetaryradarprogram(formerlyfundedbyNASA),and the ALFA program of legacy sky surveys--both of which require expenditures of approximately $1M
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Figure 11.2.1. FundinghistoryofNAICandNSF/ASTexpressedasacumulativepercentagechangefrom FY1999. Projections beyond 2007 are based on the Presidential request for FY2008 and the recommendationsoftheSeniorReview.

annually.ThenetresultisthattheannualASToperatingbudgetfortheAreciboObservatory,about $10.5M,expressedasafractionofthereplacement costoftheAreciboObservatory,>$250M,is<4.2%. The management guideline for a research facility is that this ratio should be about 10%. Other AST national centers operate on annual budgets that areabout6%oftheObservatoryreplacementcost. NAICisbeingasked,annually,tooperateonfundingthatissignificantlylessthantheotherobservatoriesandasaconsequenceNAIChasbeenforced to implement cost-saving operational procedures that are unique. This is a significant management challenge, especially so as it is one that is re-presentedtoNAICeachandeveryyear! ThespecificmanagementconcernstoAOoverthe budgetincludethefollowing: · The AO head of electronics asks how it is possible for NAIC to keep pace with advancing technology with a shrinking technical staff and declining instrumentationbudget. · The AO head of computing asks how NAICcanaffordtheon-linedatastorage requirements of the ALFA (especially
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PALFA)legacyskysurveys. · All AO technical leaders ask how can NAIC retain its superb engineering staff membersiftheengineerscannotbegivenintellectually-challengingdesign/construction projects and are instead only givenroutinemaintenancetasks. · The AO head of the planetary radar systemwouldlikeassurancethatiftheoverhauloftheturbineelectricgeneratorhas tobepostponedbeyondPY2007owing to a lack of the funds necessary for the job (~$350k) that the overhaul can be fundedinPY2008.

11.3 Management, Contractual, Financial and Technical Issues
In confronting the management, contractual, financial and technical issues that inevitably arise in the operation of a research facility of the size of NAIC, NAIC has access to the extensive problemsolvingresourcesthatareavailabletoitbyvirtueof itsbeingpartofCornellUniversity. CornellUniversityisoneofthecornerstonesofU.S. higher education and research. It is a private, endowed university and also the federal land-grant
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institution of New York State. It is composed of fourteenschoolsandcolleges--sevenundergraduate units and four graduate and professional institutions in Ithaca, two medical schools and professional institutions in New York City, and one in Qatar, in the middle east. The university owns, leases or uses approximately 18,000,000 square feet of classroom, laboratory, office, building and residential space. Corporately, Cornell is a big institution with an annual budget that exceeds $2 billion. The administrative services of Cornell University--human resources, legal services, business services,etc.--functiontohandlethis$2billionper year institution. This is the scale of the framework that supports the $12 million per year institution that is NAIC. It is very sturdy support. The NAIC benefits directly and tangibly from Cornell's management;theNSFbenefitsindirectlyfromhavinga successfully managed research facility. This forms thebasisforacooperativerelationshipthatbrings successtobothparties--awin-winpartnership. Without question, the greatest benefit to NAIC being part of Cornell University is the intellectual guidance the university faculty have brought to the management of the observatory for 40 years. In addition to providing the inspiration for the observatory, the faculty has fostered continued development of the Arecibo research capabilities by providingconsistentandsteadyadvice.Theyhave alsoservedasaninterfacetotheU.S.researchcommunitybothbyprovidingleadershipinintellectual pursuits and in forging effective multi-institutional collaborations for research endeavors at Arecibo. TheCornellfacultycanbeaneffectiveinterfaceto USuniversity-basedscholarsandstudentsbecause the Cornell faculty work in the same environment and have the same needs as their peers at institutionselsewhere.TheNAICcommunityisenlarged and enriched by the involvement of the Cornell facultyandtheirstudents. From a business perspective, Cornell brings to the NAIC an extensive infrastructure of corporate support services, including: payroll, accounting, purchasing,humanresources,legal,internalaudit,environmenthealthandsafety,projectmanagement, and risk management. Since these are central administrativefunctionstheyarefundedmainlyfrom the University's general budget, which includes facilities and administrative cost recoveries. There are very few support services which the NAIC finances directly from NSF funds (legal expertise in PuertoRicoisonesuchexample).
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All NAIC employees are employees of Cornell University. As a result, they too share in the benefits of being part of a large institution. Among the most utilitarian of such benefits to the individual employeesarehumanresourcesservices(counseling, retirement planning, etc.) and computer access to the university library services. The latter is indispensable to the technical staff and, indeed, it isthisserviceprovidedbyCornellthatmakesitpossible for NAIC to manage a sophisticated research facility thousands of miles from Ithaca and to consider managing new initiatives that could well be locatedevenfurtherremoved. By NAIC being an integral part of Cornell University,theresourcesoccasionallyneededinmanyareastomanageriskisavailable. InitiatedinPY2006andcontinuingnowinPY2007, theCornellUniversityArchives,whichispartofthe Cornell University Library System, has initiated a project to establish a formal NAIC/Arecibo ObservatoryArchive.Thisprojectincludes: · Identifying Cornell offices with relevant archivalmaterial; · Working with the administrative staff within NAIC to develop a records and information management system to ensure that records of enduring value are collected, organized, preserved and madeaccessible; · Identifying and contacting former staff members, directors, and other key personnel who have relevant papers and collections appropriate for transfer to theArchives; · Transferring historically significant material to the Archives where it will be housedinasecure,temperatureandhumidity controlled environment, enhancing access for staff and researchers by creatinganonlineguidetothematerial; and, · Identifyingexistingcollectionswithinthe Division of Rare and Manuscript Collections that have material relevant to this projectandlinkingthesesitestothenew NAIC/AreciboObservatoryArchive.

11.4 Requirements for Support of the Scientific Community
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GenerationoftheplanforNAICsupportofthescientific community is informed by two principal requirements. First is the recognition that the NAIC, asaNSF-fundednationalresearchcenter,supports a multi-disciplinary program of research serving mainly the U.S. university community for which education of the next generation of scholars is a primary responsibility. The multi-disciplinary characterofNAICistruenowfortheAreciboObservatorywhereresearchfacilitiesareprovidedforradio astronomy, radar probes of solar system objects, ionosphericradarstudies,andopticalstudiesofthe upperatmosphere.Theadditionofthemajornew initiatives currently being pursued by NAIC, the SKAinparticular,is,potentially,amajornewobservatory that will further increase the multi-disciplinary character of NAIC. They will also greatly enhanceeducationalopportunitiesatNAIC.Second, is the point frequently highlighted in this APRPP, that the Cornell vision for NAIC has no provision in it for NAIC to become a NSF facility that is so large and so independent that it can create a researchstructure(facilities,instrumentsandpeople) with the mission of developing research initiatives for the community. Instead, the NAIC mission is to develop research initiatives with the community.Asaresearchuniversityitself,Cornellsharesthe educational goals, and understands first-hand the concerns, and needs, of the university community servedbyNAIC. As noted in section 11.1 above, the motivating goal for NAIC is to develop partnerships with the U.S. academic research community toward common goals. We recognize that a national center such as NAIC is a natural forum for promoting research and education partnerships. On the largest scale, university-based scientists and students have access to all the research facilities of NAIC, and the NAIC support staff, without charge. On an entire range of smaller scales, the NAIC facilitates the research and education initiatives of the university community by providing technical and educational services, technical designs, and managementleadershiptailoredtospecificcommunity needs. In return, community researchers bring instruments, ideas and software to the Observatory and make them available for the benefit of others. This makes for the foundation of a sound partnership, each party sharing its expertise with the others. Provision of sufficient NSF funding to enable NAIC to facilitate such partnerships is the primary NAICrequirementforsupportoftheU.S.academic researchcommunity.
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On a much larger scale, NAIC has been playing a leadership role in organizing the U.S. community to promote its interests in developing the future of meter/centimeter-wavelength astronomy in the U.S. In August 2006, NAIC lead a community-based workshop called "Building the Foundation for U.S. Astronomy at m/cm Wavelengths in 2010 and Beyond". The meeting was co-hosted byNAIC,NRAOandtheU.S.SKAConsortiumwith much-appreciatedfinancialsupportfromNSF/AST. The meeting was one of a series designed to lead toathoughtfulpositionpaperforU.S.radioastronomers to present to the next decadal survey. The final report of this workshop, reproduced below, hasimportantimplicationsforthefutureofAOand other long-wavelength U.S. facilities. Community leadership is an essential role for NAIC; NAIC will organize a follow up community meeting in the second half of calendar year 2007 to be held in Washington,D.C.

Building the Foundation for U.S. Astronomy at m/cm Wavelengths in 2010 and Beyond ­ A meeting held 3-4 August 2006 Tucson, AZ
Recommendations and Actions 21August2006
The meeting succeeded in bringing together an inter-disciplinary cross section of the astronomy community interested in the future development of m/cm astronomy in the U.S. A discussion of science opportunities for which observations at long wavelengths can provide unique scientific insight provided the starting point for the meeting. This discussionwasaidedbyreferencetothesetofkey science areas identified for the Square Kilometre Array. These areas include topics in fundamental physics and cosmology (Epoch of Reionization, dark matter and dark energy, gravity and pulsars, cosmicmagnetism),galaxyevolutionasprobedby HIobservationsandobservationsofredshiftedCO emission, and the important Cradle of Life topics (protostellar and protoplanetary disks and young stars, molecules and SETI). Additionally, contributed talks on more recent conceptual ideas stimulatedevenbroaderdiscussion. Withinthesebroadsciencecategories,keyscience objectives were identified at the meeting by four topicalworkinggroups.Throughdiscussionofthe
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working group reports in a meeting of the whole, two specific key projects of extremely broad scientific interest were highlighted as priority opportunities for which m/cm observations are uniquely required: · Detection and imaging of HI emission andabsorptionfromtheEoR; · A massive sky survey for HI emission from galaxies as a function of redshift. The goal of this "billion-galaxy" survey to redshifts of z=1.5 or higher is to parameterizethepropertiesofdarkenergy primarily by studying the signature of baryon oscillations. A determination of thecosmicevolutionofthegascontent in galaxies with unprecedented completenessisalsoenabled. Severalotherexcitingopportunitieswerediscussed andnotedasimportantdriversforfuturetelescopes andinstrumentationneeds,including: · Large sky-area, unbiased searches for radio transient sources on time scales rangingfromnanosecondstoyears; · Large sky-area searches dedicated to identifying as much of the pulsar population in the Milky Way as possible, up to ~20,000 pulsars. The primary goals are: (a) to establish a large sample of millisecondpulsarsthatcanbeusedasa long-term timing array for the detection of the nano-Hertz gravity waves, which result from cosmic strings and from supermassive black-hole mergers; (b) to discoverandconductprecisetimingobservations of those rare, compact, relativistic binary pulsars (with neutron star and black-hole companions), which will allow us to probe gravity over a wide range of environmental conditions, extending to the strong gravity regime of lines-of-sight that graze the event horizonoftheblackhole;(c)todiscoverand conduct precise timing observations of pulsarsorbitingSgrA*inordertoprobe space-time close to a rotating, massive, blackhole. · Imagingprotostellarandprotoplanetary disks at the earliest stages of formation, and edge-on systems at all evolutionary stages, where the disks are opaque at millimeter wavelengths and at all short100

er wavelengths owing to dust obscuration. · Imaginglower-ordermolecularlinetransitionsfromthefirstgalaxies.Thelower order CO transitions provide the cleanest measure of the total molecular gas mass--the fuel for galaxy formation, as wellasthebestmethodfordetermining galaxy dynamics, and hence total (gravitating) mass. Further, cm-wave telescopes are the most appropriate for studying emission from high dipolemoment molecules, such as HCN and HCO+, in the first galaxies, due to the large critical densities required for excitation.Thesemoleculesarethebesttracersofdensegasdirectlyassociatedwith starformation. · Large area polometric sky surveys to studycosmicmagnetisminastrophysical environmentsatallepochs. Thescienceareasmapintoobservationalopportunities throughout the 250:1 range of frequencies (0.1 to 25 GHz) that comprise the m/cm wavelength spectral band. Several Workshop speakers highlighted the fact that covering this enormous frequency range necessarily demands that we think in terms of multiple technical solutions. As a specific example, an array of inexpensive dipole antennas was agreed to be an optimal technical solution for constructing the very large collecting area needed at frequencies below ~300 MHz for imaging EoR/HI in emission and absorption. At higherfrequencies,from~300MHzto25GHz,an array (or arrays) of parabolic antennas appears to betheoptimalwaytocoverthenearly100:1broad spectralbandwidth. The discussion on how to realize the key science opportunities for the U.S. community was framed aroundthreespectralregions.

Low-frequency band, 100 ­ 300 MHz. TheenthusiasticsupportfortheEoR/HIprojectasa"must do"projectwasconsideredintwophases.Thefirst phaseisdedicatedtodetectionofthephenomenon andcharacterizationofitssignature.Thisphase,it was agreed, is best done by means of the many experiments currently underway (LOFAR, MWA, PAPER, 21CMA). The second phase, after detection, would be dedicated to imaging EoR/HI emissionandabsorptionoveraverylargeskyarea.This would require an array of much larger collecting
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area, and one with higher resolution, than those plannedforthepathfinderexperiments.Thearray must be one that is optimized for surface brightness sensitivity. It must be located on a site with the lowest possible RFI contamination. Currently, anEoRarrayisstillconsideredtobepartoftheSKA project because EoR imaging science is expected to require the square kilometer of collecting area and because it is directly germane to the cosmological history of atomic hydrogen, another major emphasis of the SKA. However, technology for EoR science can be developed much more quickly than for the rest of the SKA frequency range. For this reason, the workshop participants considered itappropriatethatEoRarraysbeconstructedindependently.Givenstronginterestandactivityinthe U.S., a roadmap for EoR science should be developed for presentation to the next decadal survey thatoutlinesadecisiontreefordecidingwhethera largerarrayneedstobebuiltinthe2010-2020decade,andifso,whatarethestepstoitsrealization. Theroadmapshouldbedevelopedincooperation withourinternationalcolleagueswhoareworking on EoR experimental arrays such as LOFAR and MWA.

CMBpolarization,forredshiftedlineemissionfrom CO, HCN and HCO+, for astrometric observations of redshifted H2O masers, and for "Cradle of Life" enterprises. There is clear interest in reaching 25 GHz(orevenhigher,ifaffordable)forthepurpose of understanding protoplanetary and debris disks that are too dense to probe with ALMA. Longbaselinecapability(1000sofkm)isessentialforimaging the details of disks (and for making movies ofdisksundergoingplanetformationoveraperiod of many years), and of the stellar black holes and neutron stars that reveal the same energy collimationandjetflowsthataresoubiquitousinquasars. The radio astrometric precision of 10 microarcsec will rival the accuracy of future space-based opticaltelescopesandallowustoobtainfundamental parametersofstellarmassesanddistances.Inaddition,relativeastrometricmeasurementsofextragalacticwatermegamasersmayleadtovaluesofthe Hubble constant more accurate than 3%, providing a critical constraint on the equation of state of darkenergy. The SKA technical plans for research capability at frequencies > 3 GHz are still being developed. However, high frequency technical development is a particular strength of the U.S. community owingtoworkbeingdoneforALMA,EVLA,ATAand the DSN array. There are many examples in the U.S of innovation and development underway or planned with a solid focus on reducing the cost of receiving, detecting and processing cosmic signalsatfrequencies>3GHz.Forthisreason,itwas agreed that this band was the best of the three important wavebands for the U.S. to take a leadingrole.TDPworkforthisfrequencybandwould build upon the existing U.S. technical and scientific foundation and focus on maximizing A/T as a function of frequency for a fixed cost budget. The implementationroadmapforthesecapabilitieswill be developed based on the achievements of the TDP, again in close consultation with the international SKA project. An important question for the U.S. community is whether the key science at frequencies > 3 GHz requires a new ~$1B telescope orwhetherexistingU.S.facilities,augmentedwith additionalcollectionarea,isasuitablealternative. Recommendations: 1. Encourage strong NSF support for EoR/HI pathfinder experiments such as that currently being provided to MWA and other initiatives. The science is extremely com 101

Mid-frequency band, 300 MHz ­ 3 GHz. Anarray that covers the mid-frequency band is of great interest particularly for the large-area survey of HI emission from galaxies at redshifts to 1.5, or higher. In addition, this band appears to be extremely promisingasalargeradiosynopticsurveytelescope (LRSST) that would provide a powerful probe of the transient radio universe. LRSST would deliver large samples from radio-only populations as well assynergisticcapabilitiestotheopticalLSSTandto gravitational wave observatories. Finally, two of the key science areas for the SKA, gravity studies with pulsars and cosmic magnetism, are also enabled with the extension of this band beyond the 1.4 GHz rest frequency of HI to about 3 GHz. The international SKA project has also focused major emphasisontheHIredshiftsurvey,andhereagain itisintheU.S.interesttoworkwiththeSKAproject toconstructaroadmap,includingdefinitionofthe U.S. implementation role, leading to this capability.TheworkplanfortheUSTechnologyDevelopmentProject(TDP)fortheSKAwillincludeprojects thatarerelevanttothisfrequencyrange. High-frequency band, 3 GHz to 25 GHz. Frequenciesabove3GHzareofgreatinterestforusing pulsarstoprobethemetricaroundSgrA*,formapping Galactic foregroundsrelevant to detection of
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2.

3.

4.

5.

pelling, and vital, to studies of the physics oftheearlyuniverse. Encourage the U.S. representatives to the International SKA Steering Committee (ISSC) to promote development of a roadmap for EoR/HI science. The plan should include a meaningful participatory and contributoryroleforU.S.researchersanda realisticassessmentoftheU.S.timescalefor majorfinancialcommitment. Encourage the U.S. representatives to the ISSC to promote the development of a roadmapleadingtoanarrayoptimizedfor a very large-scale survey of HI in galaxies toz=1.5(orhigherredshift)andforsurveys for transients, pulsars, and Faraday rotation.Theplanshouldincludeameaningful participatory and contributory role for U.S. researchers and a realistic assessment of the U.S. timescale for major financial commitment. Develop the scope of work for the TDP within the U.S. community such that the TDP supports the role agreed for U.S. involvement in item 3 without duplication of efforts underway by other SKA internationalgroups. Developaroadmapforactivitieswithinthe TDP that builds on existing capabilities in the U.S. at frequencies > 3 GHz, including capabilities at Arecibo, ATA, EVLA, VLBA, and GBT, that can be used to inform planningbytheinternationalSKAproject.The roadmap planning should be done in cooperation with the international SKA project.

achieve exceptionally high angular resolutiononlongbaselines. · Dark Energy and the Radio LSST. Thetaskistooutlineindetailthescientific and technical requirements for the HI sky survey extending to high redshifts, along with an all sky Faraday rotation survey, a Galactic census of pulsars, and a synoptic surveyofthetransientradiosky. · Optimization of pulsar timing for probing Sgr A* and for use of millisecond pulsars as gravitational wavedetectors. · Definition of the requirements for imaging nearby protoplanetary disks and for detecting redshifted molecular lines in the early universe.



Action Items: 1. Identify a work plan for the NSF-funded TDP that takes into account activities takingplacewithinthenationalcenters(NAIC and NRAO), and at U.S. universities and institutes, following the recommendations notedabove. 2. SetupUSWorkingGroupson: · EoR (to establish an EoR/HI roadmap for defining the context and plan for a large telescope to image theEoR/HI.) · Precision astrometry that exploits thecapabilityofm/cmastronomyto
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12. Budget Report
2007 Funding Request
All Programs
AST 340,000 1,170,000 1,550,000 20,000 7,000 240,940 1,275,000 4,602,940 1,518,970 6,121,910 149,030 150,000 40,000 ATM 90,000 355,500 220,000 10,000 115,000 790,500 260,865 1,051,365 10,000 55,000 5,000 REU Total 430,000 1,525,500 1,770,000 20,000 7,000 250,940 1,390,000 5,393,440 1,779,835 7,173,275 159,030

Senior Personnel Other Personnel Post Docs/RAs Other Prof Graduate Students Undergrad Students Secretarial-Clerical Other Total Personnel Fringe Benefits Total Salaries, Wages & Benefits Equipment/Capital Travel Domestic Foreign Participant Support Costs Stipends Travel Subsistence Other Total Participant Support Costs Other Direct Costs Materials and Supplies Pub/Doc/Diss Consultant Services Computer Services Subawards Other Total Other Direct Costs Total Direct Costs Indirect Costs Total Direct and Indirect Costs

205,000 45,000

16,000 6,000 3,000 25,000 599,060 30,000 20,000 100,000 25,000 1,800,000 2,574,060 9,060,000 1,400,000 10,460,000*

110,000 15,000 15,000 120,000 248,635 508,635 1,630,000 170,000 1,800,000

39,600 20,800 550 11,000 71,950

39,600 36,800 6,550 14,000 96,950

709,060 45,000 20,000 115,000 145,000 2,048,635 3,082,695 71,950 $71,950 10,761,950 1,570,000 1,871,950

* Note: This AST budget for new funds does not include additional funds to be provided by the NSF for the telescope painting
project, estimated at ~$2.9M.

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Budget Report continued
PY 2007 Budget Justification
New NSF Funds (all programs)
· Salaries and Wages Fundsarebudgetedasdetailedontheeffortdistributionchart,Section8.Inadditiontobasesalaries, fundsareprovidedforovertime,shiftdifferential,4%meritincreases,andthemandatedPuertoRican Christmasbonus. · Fringe Benefits ThefringebenefitrateappliedhasbeenapprovedbytheDepartmentofHealthandHumanServices forapplicationtofederallysponsoredprograms.Arateof33%hasbeenappliedfromOctober2006 throughSeptember2007forallbenefits-eligibleemployees. · Participant Support Costs REUfundsrepresent$71,950.AdditionalASTfunds($25K)arebudgetedforaworkshop(topicTBD)to behostedattheAreciboObservatory. · Equipment/Capital ThefollowingisabreakdownoftheestimatedexpendituresintheASTequipment/capitalbudgetline: InstrumentationDevelopment $19,030 S-BandRadarSystem 50,000 FocalPhaseArray 80,000 TOTAL 149,030 Atthistime,noindividualequipmentitemsinexcessof$25KareplannedfortheATMprogram. · Indirect Costs TherateshavebeenapprovedbytheDepartmentofHealthandHumanServicesforapplicationtosponsoredprograms.TheIDChasbeenestimatedasfollows: AST AO HQ Total ATM AO HQ Total MTDC 5,800,000 1,300,000 7,100,000 MTDC 1,360,000 35,000 1,395,000 IDC rate 11% 58/59% IDC rate 11% 58/59% IDC 640,000 760,000 1,400,000 IDC 149,700 20,300 170,000

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Budget Report continued

PY 2006 Subagreements
AST ATM PennStateUniversity NorthwestResearchAssociates UniversityofColorado PennStateUniversity

AmmannandWhitneySubcontract

Carryover Funds
FundsremainingatthecloseofPY2006total$3.3Mandareallocatedasfollows: PlatformPainting ALFASpectrometers MaintenanceTrailerInstallation MiscCommitments TurbineMaintenanceandRepair InstrumentationDevelopment PayrollTimekeepingUpgrade TertiaryDriveSystemUpgrade 2,000,000 500,000 250,000 250,000 135,000 80,000 50,000 35,000







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Budget Report continued

PY 2006 Final Financial Report
Cooperative Agreement #9809484/0431904 A Senior Personnel B Other Personnel Post Docs/Research Assoc Other Professionals Graduate Students Undergraduate Students Secretarial-Clerical Other Total Personnel (A+B) C Fringe Benefits Total Salaries, Wages & Benefits D Equipment/Capital Construct. E Travel Travel-domestic Travel-foreign F Participant Support Costs Stipends Travel Subsistence Other G Other Direct Costs Materials and Supplies Pub/Doc/Diss Consultant Services Subawards Computer Services Other Total Other Direct Costs H Total Directs Costs (A - G) I Indirect Costs J Total Direct and Indirect AST 305,904 1,040,776 1,946,361 19,502 6,592 283,675 1,679,065 5,281,875 1,641,722 6,923,597 499,757 201,805 48,733 0 863 -3,918 5,943 872,831 37,948 15,559 124,121 58,165 944,630 2,053,254 9,730,034 1,367,871 11,097,905

Expenses by SSOW/CSA
ATM 29,930 427,514 402,361 0 1,000 12,600 143,903 1,017,308 315,134 1,332,442 -14,290 74,425 4,328 0 18,284 0 3,848 152,439 16,496 0 71,224 50,540 143,422 434,121 1,853,158 194,433 2,047,591 38,035 10,749 686 14,324 REU Total Expenses 335,834 1,468,290 2,348,722 19,502 7,592 296,275 1,822,968 6,299,183 1,956,856 8,256,039 485,467 276,230 53,061 38,035 29,896 -3,232 24,115 1,025,270 54,444 15,559 195,345 108,705 1,088,052 2,487,375 11,646,986 1,562,304 13,209,290

0 63,794 63,794

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APPENDIX A:

2007 COMMITTEES
NAIC Visiting Committee (VC): PhilipDiamond,JodrellBankObservatory DavidFritts,ColoradoResearchAssocatesdivision/ NorthwestResearchAssociates GillianKnapp,PrincetonUniversity RichardKron,UniversityofChicago RobertSchunk,UtahStateUniversity RichardSimpson,StanfordUniversity RussTaylor,UniversityofCalgary PaulVandenBout,NRAO

Arecibo Users & Scientific Advisory Committee (AUSAC): FrankDjuth,GeospaceResearch,Inc. SheperdDoeleman,HaystackObservatory LyleHoffman,LafayetteCollege FarzadKamalabadi,UniversityofIllinois AmyLovell,AgnesScottCollege DavidNice,BrynMawrCollege MaryPutman,UniversityofMichigan ScottRansom,NRAO LiesevanZee,UniversityofIndiana

Cornell-NAIC Oversight Committee (CNOC): JamesAlexander,DepartmentofPhysics JosephBurns,DepartmentofAstronomy JamesCordes(Chair),DepartmentofAstronomy DonaldFarley,SchoolofElectricalEngineering JosephVeverka,DepartmentofAstronomy

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