XMM-Newton Science Analysis System . ... A different approach is done via the setting withctisrcpos =Y: all event energy corrections do not use the actual RAWY coordinate but the corresponding RAWY location of the source ( SRCPOS ) as determined by the task epframes (either automatically or via setting withsrccoords =Y). ... The task epchain may be used with the setting ccds =4 withctisrcpos =Y to process only the CCD 4 where usually the bright source is located that causes the Out-of-Time events. ...

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• Conversion to DET coordinates

Next: Catalog Construction Up: Observations and Analysis Previous: Source Detections . ... It was assumed that the highest signal gives the most likely position of the source. ... Comparing the summed map with the maps from the individual energy ranges, the one which produced the smallest error box was chosen to represent the source position, as long as was greater than 4, a level chosen to reflect a reasonable degree of confidence in the detection. ...

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• What was measured?
• HyperLEDA documentation: compilation of surface brightness (a105)

... A photometric analysis was made of the simulated images using two of the widely available reduction programs, ROMAFOT (Buonanno et al. 1983) and DAOPHOT (Stetson 1987). ... The rebinned and expanded image gave better results (Fig. 7b), with the smallest errors in the order of = 0.04. ... Similarly to ROMAFOT, the image with the Moffat PSF gave significantly better results than the image generated with the Tiny Tim PSF; the errors in the magnitudes of the brighter stars were around = 0.02. ...

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• Chapter 3: Fixed and Generic Targets
• Fixed and Generic Targets
• Mode = ACQ/PEAKDConfig = COS/NUV

... Miriad has a couple of tasks available for finding positions of sources (see also cgcurs in Chapter 17 ). ... It fits a 2-D parabola to the image intensities in a 3 by 3 pixel box centred on the brightest pixel in a specified region and reports the fitted location and intensity. ... Input image . ... The quality of your fit can improve significantly by selecting a snug region, and/or using the clip keyword to keep pixel values with little signal (e.g. sidelobes and noise) out of the fitting process....

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• ellint
• impol
• imstat

... Using a simple 2-D Gaussian Point Spread Function (PSF) on a constant (flat) sky background, I derive a theoretical photometric and astrometric performance model for analytical and digital PSF-fitting stellar photometry. ... The photometric performance is maximized when either the effective background area or the effective-background-level measurement error is minimized. ... An important, but frequently ignored, noise source is the uncertainty of the measurement of the effective background level ( )...

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• Robust Data Analysis Methods for Spectroscopy
• The Co-Addition Technique Applied to Images of Galaxy Cores
• Classification of Objects in the Guide Star Catalog

... Posts tagged ?time series? ... Tags: AstroStat , computer science , job announcement , job market , time series , UC Berkeley . Category: Job , News | ... arxiv:0906.3662] The Statistical Analysis of fMRI Data by Martin A. Lindquist . ... ArXiv] Statistical Analysis of fMRI Data? Tags: data aquisition , experimental design , fMRI , ICA , image analysis , image processing , localization , modeling , pipeline , preprocessing , similarities , Spatial , temporal , time series , voxel . ... 2008? ...

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• The AstroStat Slog Blog Archive Use and Misuse of Chi-square
• *skypix* -- conversion of pixel position to sky coordinates
• The AstroStat Slog Blog Archive [Jobs] postdoc position at UC Berkeley

In this gallery are many images of Low Surface Brightness Galaxies which have recently been discovered and analyzed. ... The central surface brightness of this galaxy is 24.28 . Malin 2 This galaxy is another huge disk galaxy with a scale length of 15 kpc and a redshift of 15000 km/a. The high surface brightness knot in one of its spiral arms actually has the same color, luminosity and H-alpha equivalent width as the entire Large Magellanic Cloud . ... Truly it is a Low Surface Brightness Galaxy. ...

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Please enter the lightcurve file name and period search parameters: . Lightcurve file: . ... Apply the Heliocentric correction and convert all dates to Terrestrial Time (TT)? ... Also, the Heliocentric correction cannot be applied to such lightcurves. ... This period search service is also available at the mirror sites: Mirror 1 , Mirror 2 , Mirror 3 , Mirror 4 . You may download the latest source code distribution and install the period search service at your own web server. ...

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Many entry fields permit sexagesimal entry (h:m:s.s or :':"). ... Sexagesimal entry is flexible in that you can specify one to three fields, as you desire. ... Position entry widgets assume that a single field is decimal hours or degrees (h.h or . ... You may specify one to three fields: . ... Note: sexagesimal offsets and durations are entered in the same fashion, but a single field is decimal arc-seconds or seconds ('.' or s.s) and two fields are (arc) minutes and seconds (':"." or m:s.s). ...

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• sgs summary
• lsst.coordConv: coordConv: Astronomical Coordinate Conversions
• SDSS Engineering Papers

This WWW form allows the user to obtain "postage stamp" FITS or jpeg images or contour plots of selected, small fields from the The VLA Low-Frequency Sky Survey (VLSS, formerly VLSS). ... The specified region of the closest VLSS field is returned as a FITS or jpeg format image or a contour plot. ... The VLSS postage stamp server can return a FITS file with the MIME type of image/x-fits; your browser needs to be told a suitable display program for FITS files. ...

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• NVSS Source Search (10-July-1998) Help for NVSS Source Catalog Search
• NVSS Image ftp service Documentation Help for NVSS Image ftp service
• NVSS Postage Stamp Server Documentation Help for NVSS Postage Stamp Server

... connection points . ... The point P3 is the connection between the horizontal and vertical actuators and is the axis of rotation for the tail gunner motion. processing: survey/020204/reduc We can compute P3,P5 (the moveable points) in dome centerline coordinates if we have the actuator distances and we know the positions of the above connection points in dome centerline coordinates for a given position of the tertiary (say the nominal focus position).(see actuator distances to dome centerline ). ...

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• http://www.naic.edu/vscience/schedule/tpfiles/RankintagP2202tp.pdf
• http://www.naic.edu/vscience/schedule/tpfiles/MitratagP2532tp.pdf
• http://www.naic.edu/vscience/schedule/tpfiles/HowelltagR2737tp.pdf

... From the peculiar shape of the light curve in the visible spectral region (a long phase interval of light constancy was observed by Hensberge et al. in 1981 ), HD 56022 had been expected to show unambiguously the nonequatorial symmetry of its surface brightness distribution. However, analysis of the light curve has yielded a possible equatorial position of a spot. ... A solution seems only possible, if the light constancy over the long phase interval in the visible is not observed in the UV. ...

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• http://jet.sao.ru/jet/~goray/2362/v2362cyg.htm
• http://mavr.sao.ru/hq/balega/PUBL_BAL/PUB_2006/2005_k3-50a_dina4.pdf
• di_eks

Central Astronomical Observatory at Pulkovo of Russian Academy of Sciences PUL Analysis Center Pulkovo IVS Analysis Center (PUL) 2009 Annual Rep ort Zinovy Malkin, Natalia Miller, Elena Popova Abstract This report briefly presents the PUL IVS Analysis Center activities during 2009 and plans for the coming year. The main topics of the investigations of PUL staff in that period were ICRF related studies, computation and analysis of EOP series, and VLBI2010 related issues. ...

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• http://www.gao.spb.ru/english/as/j2014/presentations/perepelkin.pdf
• Pulkovo Observatory
• Pulkovo NEO Page: Estimation of Observational Accuracy

. Next: Initial velocity Up: Space and velocity distributions Previous: Space and velocity distributions . Following Paczynsky (1990), we assume initial space distribution of young neutron stars to be varying exponentially with distance from the Galactic center and from the Galactic plane, that is probability distribution for young neutron star positions can be written in the form . with kpc, and pc. Mike E. Prokhorov . Fri Jul 19 19:16:07 MSD 1996

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• Initial velocity

polimodel -- Produce model linear polarization and position angle images . ... Whether to apply random errors to output polarization and position angle values. seed = "" [integer] . ... This task produces a model linear polarization image and corresponding position angle image from an input image assumed to represent intensity (Stokes I parameter). ... A threshold for the input image can be defined such that polarization and position angle are not computed for input values less than this threshold. ...

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• Some Experiments with the Restoration of NICMOS Camera 2 Images of OMC-1
• The Formation and Evolution of LMC Rich Star Clusters: NGC 1818
• NICMOS/HST H-band (F160W) Images of the 30 Dor Starburst Cluster

polimodel -- Produce model linear polarization and position angle images . ... Whether to apply random errors to output polarization and position angle values. seed = "" [integer] . ... This task produces a model linear polarization image and corresponding position angle image from an input image assumed to represent intensity (Stokes I parameter). ... A threshold for the input image can be defined such that polarization and position angle are not computed for input values less than this threshold. ...

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• VISTA view of the newly discovered globular cluster VVV CL001 and its brighter
• Wide-field view of the sky around the bright star cluster IC 4651 | ESO
• Bright Galaxies in the Virgo Cluster | ESO

ADC CATALOG HOLDINGS SHORT TITLE LIST March 29, 2002 (adapted from ftp://adc.gsfc.nasa.gov/pub/adc/archives/catalogs/key) Category 1: Astrometric and Positional Data - March 29, 2002 1090 Positions of 502 Stars in Pleiades Region (Eichhorn+ 1970) 1107A Washington Cat Visual Double Stars 1984.0 (Worley, Douglass 1984) 1131A SAO Star ...

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. Please standby and you will be automatically connected to the new location of the unframed Supernova page. Or, click on the link above. If you have questions or problems, please email me at David Bishop dbishop@vhdl.org . Last modified: Mon Aug 27 12:40:15 EDT 2001

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• Supernova 1999br in NGC 4900
• Supernova 2005W in NGC 691
• Bright Supernova - Archives

... R-band images obtained at 0.8 arcsec seeing conditions have allowed us to separate foreground star from point-like extragalactic source and estimate their brightness separately. ... To study the nature and properties of the source, we observed it under high spatial resolution. ... CONCLUSION RTT150 optical observations with sub-arcsecond seeing and low resolution spectra confirm the hypothesis of superposition of a radio source onto a `normal' F/G galactic star proposed by [1]. ...

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Tail Probe is one of the satellites of the INTERBALL program. ... Collection of the orbital elements | ... Flight situation analysis during operations scheduling . ... Two stages of the orbital situation analysis are presented: . ... The satellites motion calculation during the flight situation analysis is based on the orbital elements, determined by the Ballistic center at KIAM RAN. The modified (by backward integration) orbital elements are usedduring the aposteriory situation analysis. ...

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• Satellite position in the SE and GSM coordinate systems
• INTERBALL AURORAL PROBE SITUATION ANALYSIS
• Transits of Venus