.

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... The BL Lac objects found within DXRBS fall mostly in the range . ... A large fraction of the BL Lacs so far in our sample are at L X / L R < 10 -6.5 , the region of Figure 6 populated by LBLs. In this region of parameter space (to the left of the left-most dashed line in Figure 6), DXRBS includes objects up to two orders of magnitude fainter than the 1 Jy survey. ... For comparison, we have plotted the values for members of these three ROSAT-based surveys (DXRBS, HQS/RASS and RC) in Figure 7. ...

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Next: Using Linecatalog Up: Line Catalog Previous: Loading a Line Catalog Index . ... ASAP>jpl = linecatalog('jpl.tbl') ASAP>jpl.set_frequency_limits(80,115,'GHz') # Lines for 3mm receiver ASAP>jpl.set_name('*OH') # Select all alcohols ASAP>jpl.set_name('OH') # Select only OH molecules ASAP>jpl.summary() ASAP>jpl.reset() # Selections are accumulative ASAP>jpl.set_frequency_limits(80,115,'GHz') ASAP>jpl.set_strength_limits(-2,10) # Select brightest lines ASAP>jpl.summary() . ...

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• The Local Volume HI Survey (LVHIS)
• Old VLA
• User Parameters - Spectral-line Imaging CentralProcessor 0.11 documentation

... Here we will continue to look at line plots. We will go through steps, such as changing line colors and plot ranges, you can use to modify your line plots. Note: Beginner's IDL - Line Plots III will be posted after the Thanksgiving holidays. ... Below is an example on how you can change the color of your plot as well as the background. ... IDL> plot, num, line, color = 45, background = 200 . ... IDL> plot, num, line, color=45, background = 200, /nodata . ... IDL> plot, num, line, xstyle=4 . ...

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• Absorption line spectra of the UV bright z=2.4 QSO HE 1122-1649
• STScI Preprint #1250
• The Spitzer Infrared Nearby Galaxies Survey: A High-Resolution Spectroscopy

Next: Wavelength calibration Up: Getting Started Previous: Detecting lines in . ... and the Calibration Starting Row will be used for the lines identifications. ... After setting these parameters, click the button. to pop up the Identify window. ... The identification starts by clicking on , which plots one row of the spectrum in the graphic window, indicates the position of the detected arc lines with blue vertical traces and gives a cursor. ... Figure: Lines Identification Window . ...

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• Line search and interactive identification
• Blue Compact Galaxies from the Hambyrg/SAO Survey
• Selection effects

Next: Results & Discussion Up: Coronal Hole Diagnostics out Previous: Introduction . ... The dates of the observations discussed here, their locations, pointing, slit sizes and exposure times are given in BTDW. ... Line fits are given by the dotted line. ... An estimation of the errors in the derived parameters was obtained using the GA-derived parameters as an input for a ``classical'' IDL-CURVEFIT procedure (Peter, 1999; Peter & Judge, 1999). ...

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• Armagh Observatory
• IDLINES: identifying spectral lines

... The molecular lines group at Arecibo Observatory consists of Chris Salter, Tapasi Ghosh and Robert Minchin. ... The molecular line group at Arecibo Observatory started in 2006 with a proposal to carry out a spectral census of the star-burst galaxy Arp 220 . ... However, the most interesting discovery came from the observations of the polar ring galaxy, NGC 660. ... Molecular Lines in NGC 660 Arias de Saavedra Benitez et al., ... A cm-Wavelength Search for Pre-Biotic Molecules in Starburst Galaxies. ...

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• I-GALFA Survey Fields
• INTRODUCTION to Spectral Line Observing at AO
• Example Observing Projects

... Each point shows the 1 sigma photometric errors and the time span covered by the data; the dotted lines are the 3 sigma limits of each image. ... The solid thick lines are a fit obtained from a K-corrected, time-dilated SNIb light curve at z= 0.95 with tmax=34.0, E(B-V)=0.04 and omega=0.1. ... The three images on the left are the total HDF-N images by Williams et al. 1996 with a pixel scale of 0.04 arcsec/pixel. ... Each image is labelled by the filter and the time range of the observations in days....

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• IBIS: Technical Description
• The Arcetri Spectral Code - E.Landi and M.Landini (2002)
• CHIANTI atomic database

... rev }; if ( $rev !~ /^\d{4}$/) { &print_obs_log_sum(" Revolution $rev invalid. ... TR /i) { # until end of row push @saved_lines, $lines[$i]; if ($lines[$i] =~ / (\d{2}):(\d{2}):(\d{2})\.\d{2} /) { # RA line my ($cur_ra) = 15 * $1 + $2 / 4.0 + $3 / 240.; if ($cur_ra = $ra1_min $cur_ra = $ra1_max) {$found_ obs = 1;} if ($split) { if ($cur_ra = $ra2_min $cur_ra = $ra2_max) {$found_ obs = 1;} } } $i++; } if ($found_ obs ) { print _found_row($n_hits, @saved_lines); $n_hits++; $found_ ...

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• Command line options

... This document and the attached postscript figure document an analysis that I did to determine the optimum midpoint and required ranges for both the rotator and azimuth for the 2.5 M telescope. ... I simulate a series of drift scans on the sky for tracks that cover the northern survey area. These tracks cover the range in survey latitude of -60 to +60 degrees, spaced by 10 degrees. ... Along each track the azimuth, elevation, and position angle of the CCD is computed at 1 minute intervals. ...

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• UW-WSU Nebular Emission-Line Filters
• lsst.tcc: python/tcc/axis/posRefCatalog.py Source File

OptInt PmWiki . ... Tech Meet 2 . ... Page History | ... MROI Delay Line Design Contract . ... Design Documentation . ... PmWiki . ... Return to Tech Meet 2 ( Edit ) . ... 1 pixel independent of pixel scale (avoids aliasing of high frequencies in speckled image) . ... ADR & CAH: Optical image quality tolerancing of OAP-based layout -} . ... ADR & CAH: Use tolerancing results to assign image quality and stability budgets by component . ... ADR & CAH: Think about how to apportion image quality budget . ...

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• OptInt PmWiki : Design Documentation | History
• OptInt PmWiki : Derived Requirements Document Outline | History

Static Fourier spectrometers are often used for spectral measurements of the ionosphere emissions. There are two main advantages of Fourier spectrometers (FS) - large geometric factor and high spectral resolution; these parameters are two orders better than for grating spectral instruments. ... In scanning Fourier spectrometer optical and electric modulation of signal is used to avoid this problem, for static Fourier spectrometer there are no such ways. ...

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• Eclipse map for Computer Ephemeris for 2016 (DE200/LE200).
• Eclipse map for Computer Ephemeris for 2015 (DE200/LE200).
• Eclipse map for Computer Ephemeris for 2014 (DE200/LE200).

... I present results from several seasons of photometric observations of X--ray sources in the Orion OB1a and OB1b star formation regions. The initial goal was to measure the rotational periods of several dozen pre--main sequence (PMS) stars. ... Infrared and optical data confirm that 90% of the X--ray sources are PMS and about 10% of the PMS stars may have disks. ... I find rotation periods for five stars at confidence of greater than 99.9/ greater than 99/ at much lower confidence. ...

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• Spectroscopic Data
• X--ray Quiet PMS Candidates
• The AstroStat Slog central limit theorem

... An interactive IRAF task for the analysis of Extreme Ultraviolet Explorer ( EUVE ) emission line spectra is presented. The line flux in extracted spectra may be measured by multiple techniques, including fitting individual lines. ... To aid in identifying lines, the positions of known lines may be marked on the spectrum during the fitting process. Also, model EUVE spectra may be constructed and overlaid using plasma emissivities and source emission measures supplied by the user. ...

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• EMSAO: Radial Velocities from Emission Lines in Spectra
• Analysis Tools for Nebular Emission Lines
• VLT Data Quality Control

Focal line of the feed cabin No. ... Figure 1. The input parts of radiometers with primary feeds are placed on secondary mirror focal line taking into account a task to minimize losses in the front-end waveguides and reduce aberrational scatter at short wavelength range. ... From the right of the picture is a new developed three-frequency feed with matched phase center at the wavelengths 13, 31 and 49 cm, from the left is a new version radiometric system "MARS-2". ...

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• Optimization of spectroscopic observations
• Bus Hound
• Atlas and list of identified lines

RadioAstron AO-2 prop osal Submission dead line: 27 January 2014, 23:59 UT. ... Team contact name and e-mail address: Ivan Petrov (e-mail: Ivan.Petrov@gmail.com ) Total observing time request: 60 hrs Should be < 100 hours if GOT. ... Introduction -- providing concise background information necessary to assess the scientific merits of the research proposed; outlining the reasons for the project to constitute key science area for RadioAstron if the KSP-type is selected. ...

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• http://www.asc.rssi.ru/RadioAstron/ao-1/radioastron_ao1_proposal_template.pdf
• http://www.asc.rssi.ru/RadioAstron/ao-3/radioastron_ao3_proposal_template.pdf
• http://www.asc.rssi.ru/RadioAstron/ao-4/radioastron_ao4_proposal_template.pdf

... It was discovered during 1970's that radiation from electrical power transmission lines is one source of whistler-mode waves in the magnetosphere . Most of the world's power systems use 50 Hz or 60 Hz, but their harmonics in the kHz range (due to mechanical imperfections, nonlinear loads, etc.) can be radiated by transmission lines and leak into the magnetosphere with sufficient intensity to stimulate wave growth and emission generation, much like the VLF transmitter signals. ...

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• FLR [Oulu]
• Magnetic Field Lines
• Magnetic Field Lines -- History

The Mars Flag has a different design on the reverse side. obverse side of flag . ... The orbit lines on the obverse cross the Sun on the lower half of the flag and appear to go behind the Sun on the upper half of the flag. The reverse side has the orbits lines continuing around the Sun on the upper half of the flag. ... The Mars Flag reverse side is a continuation of the obverse side and not just a different design on the back and not a mirror image of the obverse. Main Flag Background Color . ...

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• ASP: A Good Definition of the Word "Planet": Mission Impossible?
• ASP: Running the Line: The Astronomy of Mason and Dixon
• ASP: Point: Where Is the Best Place to View a Solar Eclipse?

... The spatially resolved structure near the hydrogen emission H line was found in the spectrum taken with the BTA/SCORPIO in June, 2013. ... The fragment of the Nova V1494 Aql spectrum is shown in Fig.1. ... The Nova V1494 Aql has passed the stage of the supersoft X-ray source (SSS) in the period between 218 and 516 days after the visible light maximum (Schwarz et al., ... The spectrum of Nova V1494 Aql taken on 2013 June 9 with BTA/SCORPIO . ... The vertical lines are the lines of night sky emission....

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• New data on the cpmplex field structure of chemically peculiar stars
• Lack of Dwarf Galaxies in the Local Volume Compared to Conventional Cosmology
• Solar system sector, archive 2011

... Вид: пожарная мотопомпа ; . ... Коллекция: Осень-зима 2015/2016 . ... Пол: Женский . ... Коллекция: Весна-лето 2016 . ... title='Molokai Sunset - Quiksilver' border='0' align='left' width='120' style='margin-right: 20px;' hspace='7' vspace='5'/> Сланцы для мужчин от Quiksilver - новинка из коллекции "Весна 2015". ...

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• Покрывало-гобелен SL 220х240. 10394 - Soft Line - Soft Line 10394 Катушка
• Swiss Line Cell Shock White Маска для лица очищающая и выравнивающая тон кожи,
• Брюки спортивные для мальчика G0144 разноцветный Gas - Gas - Gas Защитная