. Next: Auto-baselining Up: Basic Processing Previous: Time average separate scans . To make a baseline fit, you must first create a mask of channels to use in the baseline fit. ASAP> msk = scans.create_mask([100,400],[600,900]) ASAP> scans.poly_baseline(msk, 1) . This will fit a first order polynomial to the selected channels and subtract this polynomial from the full spectra. Subsections . Auto-baselining . Malte Marquarding 2005-11-30

The purpose of these tools is to provide a control mechanism for flagging an LRP as baselined in ASSIST.. ... Viewgraph on Desired Baselining Procedure. Outline of New Baseline Tool Requirements (Investigated and documented by Tony Roman) . ... Bill W.?) which detail what notifications need to be sent to the LRPG account when a calendar is baselined. ... Below is a viewgraph (same author as previous viewgraphs?) detailing what notification needs to be sent to the PCs when the LRP is baselined. ...

... Science . ... Science Users Information > Science Publications > Science Announcements > Release of ALMA Long Baseline Campaign Science Verification Data . ... Observing with ESO Telescopes . ... A new installment of ALMA Science Verification (SV) data is available. This release contains several new datasets corresponding to four targets observed as part of the 2014 ALMA Long Baseline Campaign in order to demonstrate the long baseline (~10 km), high angular resolution, capability of ALMA. ...

OptInt PmWiki . MROI Delay Line SW / . Edit Page | Page History | ... MROI Delay Line Design Contract . ... MROI DL Production SW Contract . ... Software Design Documentation . ... MROI . ... MROI DL Design Contract Private Material . ... Baseline Solution Software . ... May be best to implement within a framework which is an embryonic form of the MROI offline software framework - but we need to design the framework! ISS Supervisor able to launch specific offline data analysis tasks . ...

Next: Submitting a Telescope Proposal Up: Astronomer's Guide to the Previous: Pulsars . Arecibo presently supports VLBI for up to a maximum of 4% of its astronomy observing time. ... Arecibo is equipped with a a VLBA4 recording system, compatible with the HSA, EVN and Global networks, and the 305-m telescope is available for scheduling with any of them. ... From 2004, Arecibo has used a VLBA4 Data-Acquisition Rack, together with a Mark-5A disk-based VLBI recording system. ...

... 50 Weirdest Objects . ... Observing springtime deep-sky objects with a large telescope . ... What is the baseline for determining the magnitude scale of celestial objects? Why do brighter objects have negative numbers? ... He called the brightest 1st magnitude and the faintest 6th magnitude. ... Also, to assign a magnitude to the brightest planets, the Moon, and especially the Sun, scientists would have to work with negative numbers. Get instant access to subscriber content on Astronomy.com! ...

Find Similar Abstracts (with default settings below ) . ... Translate Abstract . ... Bispectrum speckle interferometry and future long-baseline interferometry of the carbon star IRC+10216 . ... 2003SPIE.4838.1055B We present near-infrared (JHK) bispectrum speckle-interferometry monitoring of IRC+10216 obtained with the SAO 6m telescope. The present speckle observations covering baselines up to 6m provide important complementary informations for future long-baseline interferometry. ...

Orbit . ... The orbit of the RadioAstron provides four types of study: . rough images of radio sources with ultra-high angular resolution, using all baselines up to the radius of the apogee, that is much larger than Earth diameter; . ... high quality imaging of radio sources, with moderate resolution, by observing either with small projected base lines Earth-spacecraft, i.e. close to the orbital plane, or near the perigee. ... high accuracy orbit determination. ... Space Radio Telescope . ...

This diagram shows how the 'vertical-align' properties on cells combine to determine the height of the row containing the cells. The diagram also illustrates the meaning of some values of 'vertical-align' that apply to table cells: baseline, top, bottom, and middle. The diagram shows a row of five (labeled) table cells of varying heights and alignments. ... The first cell is aligned with the row baseline and extends to just below the row top. ...

... Each bin is associated with a start time (which is equal to the end time of the previous bin, if there is one), and end time (which is equal to the start time of the following bin, if there is one) and an attitude. ... This attempt is either successful or unsuccessful (logical returned value of the oal call, or null value in the atthkset column). evproject begins a new attitude bin if any of the following occur: . ... The attitude of each new `successful' bin is set to the baseline attitude. ...

... Sighting the telescope, first at the tree and then at pole B, you measure the angle A of the triangle ABC, equal to the difference between the numbers you have read from the azimuth plate.. ... Why triangles? ... One large surveying project of the 1800s was the " Great Trigonometric Survey " of British India. ... Everest was the one who commisioned and first used those giant theodolites; they are now on display in the Museum of the Survey of India in Dehra Dum. ... Everest . ...

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Note that these are 'General' ICDs giving information about protocols, not specific ICDs giving details of the full interfaces between specific Gemini systems. ... Document . ... The System Command Interface (PS) . ... The Baseline Attribute/Value Interface (PS) . ... Baseline DHS interface (PS) . ... System Status and Alarms Interface (PS) . ... Wavefront Sensing Information Interface (PS) . ... ICS/TCS Direct Control Interface (PS) . ... Telescope Tube Mass Balance f/16 IR Top End Config. ...

. Comment on J2206-1835 . Resolved: the source is extended, and has been detected only on the short Australian baselines at 2.3 GHz by Preston et al. (1989). Moellenbrock et al. (1996) did not detect the source in the 22 GHz VLBI survey. The correlated flux density is 1.2 Jy on the shortest VLBA baseline (see Figure 3). VLBApls home page . Last modified: 16 Oct 2000

TIME EVENT # EVENT DATE DATE START - END (UT) 001 28 February 1942 420228 002 07 March 1942 420307 003 25 July 1946 460725 004 19 November 1949 491119 005 23 February 1956 560223 020000 - 030000 006 31 August 1956 560831 110000 - 120000 007 17 July 1959 590716 220000 - 240000 008 04 May 1960 600504 090000 - 100000 009 03 September 1960 600902 230000 - 240000 010 12 November 1960 601112 120000 - 130000 011 15 November 1960 601115 010000 - ...

... Sighting the telescope, first at the tree and then at pole B, you measure the angle A of the triangle ABC, equal to the difference between the numbers you have read from the azimuth plate.. ... Why triangles? ... One large surveying project of the 1800s was the " Great Trigonometric Survey " of British India. ... Everest was the one who commisioned and first used those giant theodolites; they are now on display in the Museum of the Survey of India in Dehra Dum. ... Everest . ...

... Астронет | ... Обзоры astro-ph | ... A&ATr | ... планета Астронет | ... Словарь | ... О словаре . ... Термин "baseline" . baseline : . базис . ... east-west baseline : . базис (радиоинтерферометра), ориентированный в направлении запад-восток . ... fixed baseline : . постоянный базис (радиоинтерферометра) . long baseline : . большой базис (радиоинтерферометра) . Вернуться в словарь . ...

Высокоточные определения длин баз РСДБ-сети "Квазар-КВО" . ... Сравнение длин баз между опорными точками РСДБ-антенн комплекса "Квазар-КВО" с базами, полученными по координатам маркеров антенн ГНСС-приемников на обсерваториях, показывает, что расхождения не превышают 1 cм. ... Precise Determinations of VLBI Network Baselines . ... Baselines of the VLBI network are determined from all available observations. ... The comparison shows that the differences do not exceed 1 cm. ...

... Also the measured signals are affected by detector transients, altering the final results considerably. We present the design and the main features of a software package, developed in order to support the absolute calibration of the instrument. ... In case the fit is not successful, the average of the last 30% of the data is taken as the final signal. ... The two different symbols represent individual calibrations of the final background signals, using the first or the second FCS-signal. ...

... Left: A POSSM plot of the uncalibrated spectrum of DA 193 at 1.66 GHz on a baseline Bear Lakes to Noto. ... The phase slope as a function of frequency is clear evidence for a small delay error in the correlator model. Right: The same data as shown on the left, but corrected for a delay error and a residual fringe rate. ... Left: A VPLOT plot of the uncalibrated amplitude (upper frame) and uncalibrated phase (lower frame) as a function of time for the source DA 193 on a baseline HartRAO to Noto. ...