... omgchain (omgchain-1.0.12) [xmmsas_20050815_1803-6.5.0] . Meta Index / Home Page / Grism chain procedure . The task omgprep introduces some changes into the grism image files which are necessary for running the source detection and spectral extraction tasks. ... The original unrotated image is shown in Fig. ... Images prepared for running the source detection and spectra extraction tasks are shown in Fig. 4 (for the visual grism) and 7 (for the UV-grism). ...

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• Grism chain capabilities

Next: Getting the Dispersion Up: Geometric Correction Previous: Geometric Correction . For optimum results, it is important to use a comparison spectrum with as high a signal-to-noise ratio of the lines as possible. ... The algorithm detects lines whose strength exceeds a certain threshold (parameter THRES ) above the local background. ... The command IDENTIFY/LONG allows an initial interactive identification, by wavelength, of some of the detected lines. ...

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• Fitting the dispersion curve
• Reduction of the KPNO 2.1m telescope data
• Wavelength calibration

... LABORATORY OF RADIO ASTRONOMICAL OBSERVATIONS . Radio sources identification is one of the most important tasks of the current radio astrophysics. ... Optical idetification. ... Optical identifications of subsample of steep spectra radio sources from RC catalog using 6m SAO telescope of SAO RAS: optical observations. ... Astronomy Reports. ... Identification of radio sources with data of various radio catalogs allows one to construct continual spectrum of the object and its radio structure. ...

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... HST . Adjustment to the alignment of two STIS central wavelength settings . ... Data . ... HST Overview . Overview . ... However, two settings have had unusually large offsets in the cross-dispersion direction since STIS was launched. ... Corrected alignments were installed in HST on March 4, 2010 and tested using internal exposures taken as part of the CAL/STIS program 12078. Operational workarounds when using small subarrays with these central wavelength settings are no longer required. ...

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• FAQ: How do I know that wavecal processing worked correctly?
• WFC3 Data Handbook
• Identification of Erroneous Doppler Compensation for Moving Targets

Next: Status of the BIMA Image Pipeline . ... We describe all the steps of the standard reduction including per pixel error propagation: Bias correction, treatment of bad pixels, flatfielding, and filtering of cosmic ray events. ... We build difference images via image convolution with a technique called OIS (optimal image subtraction, Alard & Lupton 1998), proceed with PSF-fitting, relative photometry on all pixels and finally apply an automatic detection of variable sources. ...

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• In-Orbit Calibration of the Distortion of the SOHO/LASCO-C2 Coronagraph
• NICMOSlook and Calnic C: Slitless Spectra Extraction Tools
• The Basic Calibrated Data Processing Pipeline for SIRTF IRS

Next: Identifications and Efficiency Up: THE DEEP X-RAY RADIO Previous: Source Classification . ... For some sources which did not have NVSS positions before the time of optical observations, arcsecond positions from the Texas survey (Douglas et al. 1996) and NED (typically based on VLA data) were used. ... All X-ray/radio sources without counterparts on the survey plates were imaged at either the KPNO 0.9m or the CTIO 0.9m telescopes. ... Previously Identified Sources . Sample Properties . ...

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• Identifications and Efficiency
• ESO - How good is HAWKI astrometry and how are PSF variations corrected?
• Nausicaa Delmotte's Homepage

system performance with all freq over plotted. system performance plotted separately for each freq. ... All of the heiles calibration scans 21nov02 through 31dec02 for the lband wide (lbw) receiver were used to plot the system performance. ... Fig 1 has the Gain in Kelvins/Jansky. ... Fig 2 plots the coma parameter, first sidelobe height below the peak, the main beam efficiency, followed by the main beam + 1st sidelobe beam efficiency. ... Fig 1 1175 Mhz Gain,Tsys. ... Fig 3 1300 Mhz Gain,Tsys. ...

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• http://www.naic.edu/~phil/callbn/sep02/lbnSysPerfSep02.html
• http://www.naic.edu/~phil/hardware/vertex/jonhagen/setencoder.pdf
• http://www.naic.edu/~phil/hardware/generator/networkdoc/Training%20Materials/Checklist%20for%20remote%20dialout.doc

Download Izmccd (~2.7 MB). Solution of problems at identification of star field. ... 2) Scale is not correct. ... In this case algorithm of identification will revise all values of scale from twice smaller up to twice greater. ... There should be more than value of the field "Number of stars in frame". ... The star field is considered identified if number of the identified stars more or equally to this value. It is necessary to set value from 4 up to value of field "Number of stars in frame". ...

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An OH survey for Post-Asymptotic Giant Branch stars P. te Lintel Hekkert, J.M. Chapman We present a survey for OH maser emission at 18 cm in the direction of 196 IRAS point sources. ... OH emission and/or absorption was detected in the direction of 77 sources of which 61 OH detections were previously unknown, giving an overall detection rate of 39 per cent. ... These included three \pn\ (two new OH detections), nine \ppn\ (three new OH detections) and two cold OH/IR stars (both previously known). ...

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• Unified Radio Catalog: results for Version 1.1
• Gain-Elevation and Opacity Corrections
• Neutral hydrogen absorption

... The files here will change whenever we have a new beta version that has had an error-free telescope run. ... A few things to note, however, about this "beta" edition: There is almost no error checking on the operation of the filter wheel. ... CCDops has better error checking than XmCCD, so if you have a Windows computer available, check your camera with CCDops when you use it for the first time. ... I have a built-in fixed delay to inhibit multiple requests too fast for the wheel. ...

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. Departement of Quantum Astrophysics . Head: Kurt V.G. , Prof. ultraviolet spectroscopy of planetary upper atmospheres and interplanetary/interstellar medium; . observations of gamma-bursts and optical identification of their sources; . long-base optical interferometry. Staff: .

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... Each day a different image or photograph of our fascinating universe is featured, along with a brief explanation written by a professional astronomer. 2004 September 13 . Identify this Phenomenon . Credit: Walter Lewin ( MIT ) . ... At the time of this writing, MIT Physics Professor Walter Lewin had yet to find someone who can give the correct explanation. ... Additionally, Professor Lewin will answer appropriate e-mail questions and guesses sent to asklewin@space.mit.edu . ...

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• Презентация PowerPoint
• APOD: 2005 July 1 - Ring Around Fomalhaut
• APOD: 2014 June 9 - How to Identify that Light in the Sky

Astronomy Picture of the Day . ... Credit Copyright: Walter Lewin ( MIT ) Explanation: What caused this ring of colors? At the time of this writing, MIT Physics Professor Walter Lewin had yet to find someone who can give the correct explanation. ... Not APOD editors . ... Shortly after he gives the explanation on December 7 during a lecture in his course Vibrations and Waves at MIT, APOD will carry a link to it. ... NASA Web Site Statements, Warnings, and Disclaimers . ... The Solar Spectrum . ...

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• Астронет > Identify this Phenomenon
• Journal "Peremennye Zvezdy"
• XWare > APOD

The main steps in the reduction of NIR spectroscopic data are flat-field correction, subtraction of sky emission, wavelength calibration, correction for telluric absorption and correction for optical system plus detector efficency. ... Sky subtracted frames are corrected computing analitically the tilt angle from the instrumental calibration parameters or directly measuring it from the data. ... The same procedures are applied to the reference stars frames to obtain the calibration spectra. ...

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• mod_speling - Apache HTTP Server
• Educator's Guide to Robotic Spacecraft
• mod_xml2enc - Apache HTTP Server

Next: Imaging Polarimetry with NICMOS Up: NICMOS Data Calibration and Previous: The Photometric Performance of . ... NICMOSlook and Calnic C . ... Extracting spectra from a large number of NICMOS grism images requires a convenient interactive tool which allows a user to manipulate direct/grism image pairs. ... NICMOSlook and Calnic-C are two programs that were designed to take advantage of the fact that the NICMOS grism mode typically consists of taking both a direct and a grism image. ...

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• NICMOS Data Calibration and Analysis
• SLITLESS (Oct97) --- ST_ECF --- SLITLESS (Oct97)

... Perform rst run and assign all tracks with parent in wrong Jet to the other Jet Perform second run and see what changes: 6 ґ1 ґ 0.5 0 0.5 1 ґ1 ґ 0.5 0 0.5 1 cosJet1 : cosJet2 {bInSameJet == 1} ґ1 ґ 0.5 0 0.5 1 ґ1 ґ 0.5 0 0.5 1 cosJet1 : cosJet2 {vertexNumber == 77} ґ1 ґ 0.5 0 0.5 1 ґ1 ґ 0.5 0 0.5 1 cosJet1 : cosJet2 {( cosJet1 cosJet2 ) (jetNumber==1)} ґ1 ґ ... Unfortunately, the number of events with a p t - corrected mass > 2.0 GeV seems to go down ! ...

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• Rainfall in Eugene Oregon

... are preliminary IAU-style names for ChaMP objects. Finalization of names awaits the final systematization of optical coordinates and source identification. ... The yellow regions highlight atmospheric telluric bands at ~6900A and ~7600A. The optical ID, X-ray ID, classification, and redshift are given at the top of each plot, and a series of lines are shown that are often found in sources of that given classification. ... HS limit? ... g' band magnitude; calibrated SExtractor Kron mag or limit . ...

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• HST/FOS Atlas of AGN and Quasars
• The AstroStat Slog identification
• Spectroscopic Data

Microsymposium 38, MS067, 2003 (A4 format) SURVEY OF MARS CRATER TOPOGRAPHY FROM MOLA DATA. Michael G. G., European Space Agency, Research and Scientific Support Department, ESA/ESTEC, Noordwijk, The Netherlands, greg.michael@esa.int An algorithm for autonomous identification of crater centres from topography data has been improved in accuracy since [1,2] by taking account of the slope direction on the interior of the crater rim. ... References: [1] Michael G. G. (2002) Vernadsky-Brown 36, abs. ...

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ALMA | ... In this section, we explain why we need to correct phase fluctuations and ALMA's strategy to do this. Rapid fluctuations will be corrected with water vapour radiometers (WVRs). The Cavendish Astrophysics Group was also a leading contributor to the ALMA prototype WVRs, which were put through their paces in tests at the Submillimeter Array (SMA). ... The Cavendish Astrophysics Group in partnership with the Onsala Space Observatory built two prototype WVRs for the ALMA project. ...

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• OptInt PmWiki : MROIFastTipTilt / Interface Control
• OptInt PmWiki : MROIFastTipTilt / Tech Meet 10
• How to create a new tool in CASA Bojan Nikolic web pages (r. 329)

... About half an hour after the BAT trigger, the first images were obtained with the SAO RAS Zeiss-1000 telescope in four BVRI filters (see Fig.1). ... The spectrum of the optical transient was obtained with the SAO RAS 6-m BTA telescope 1.54 hours after the burst, using the SCORPIO instrument in the spectroscopic mode (Fig.2). ... The spectrum of the optical transient GRB090726 with identified lines, obtained with the BTA 1.54 hours after the burst. ...

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