. 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

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• Australian Long Baseline Array (LBA)
• Australia Long Baseline Array - 2002Jan Term schedule
• Australia Long Baseline Array - 2002May Term schedule

... 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. ...

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• ESO - Additional Scope for ALMA Long Baseline Science Verification Targets
• ALMA Performs Its First Very Long Baseline Observations
• E-ELT Baseline Meeting, March 2008

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 . ...

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• OptInt PmWiki : Baseline Solution Software | Attach
• OptInt PmWiki : Baseline Solution Software | History
• OptInt PmWiki : Baseline Solution Software | Edit

... 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! ...

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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. ...

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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 . ...

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• RadioAstron Monthly Notices

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. ...

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• Descriptor index

... 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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• Parallax--Lesson Plan #14
• Space Research Institute (IKI) Seminar
• Parallax

.

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... 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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... 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 . ...

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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. ...

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• Keywords_102
• Keywords_302
• Keywords_104

... 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. ...

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• Prototypical Operations Support Tools for NASA Interferometer Missions:
• Distribution of the OPUS Data Processing System
• The CARMA Data Viewer

... 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. ...

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• INTAS99.4

... Il comando gauss effettua il fit , che viene visualizzato con fit Lo spettro con baseline rimossa e fit incorporato viene infine scritto nel file di output con write Volendo recuperare il risultato del fit , bisogner`a ( una volta conclusa la riduzione di tutti gli spettri ) aprire in input quello che era il file di output con il comando ... La seconda (fit.class) permette di fittare tutti gli spettri contenuti in tale file. ...

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• http://www.arcetri.astro.it/~lt/projects/ovro/wams/WamsTalk.pdf

COPRATES CHASMA NORTH WALL INTERIOR LAYERED DEPOSIT: LAYER MEASUREMENTS AND COMPARISON WITH JUVENTAE CHASMA ILDS USING MARS EXPRESS HIGH RESOLUTION STEREO CAMERA (HRSC) DERIVED TOPOGRAPHY Michael, G.1, E. Hauber1, K. Gwinner1, R. Stesky2 ... Planets, Freie Universitaet, Berlin, Germany 5ESTEC, ESA, Noordwijk, The Netherlands Introduction: The interior layered deposit ( ILD ) in the north wall of Coprates ... The lesser section of the ILD is confined by a ridge of the chasma wall. ...

17. Introduction

18. Mauna Kea Observatories, AstroGuide Listing

19. http://hea.iki.rssi.ru/conf/hea2010/Presentations/22/Sokolovsky.pdf

20. NGC 4258