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36001. http://www.stsci.edu/hst/stis/documents/isrs/2015_01.pdf
Operated for NASA by AURA SP CE A TELESCOPE SCIENCE INSTITUTE Instrument Science Report STIS 2015-01(v1) Improved Photometry for G750L R.C. Bohlin1, C.R. Proffitt1 1 Space Telescope Science Institute, Baltimore, MD 08 June, 2015 ABSTRACT The repeatability of STIS G750L spectrophotometry at the longer wavelengths is significantly worse than that at shorter wavelengths or for the STIS G430L grating. ... Instrument Science Report STIS 2015-01(v1) Page 4 Figure 2. ... As in Figure 2 but for EXTRSIZE=11. ...
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Ссылки http://www.stsci.edu/hst/stis/documents/isrs/2015_01.pdf -- 1838.7 Кб
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36002. http://www.stsci.edu/hst/stis/documents/isrs/2015_03.pdf
Instrument Science Report STIS 2015-03 STIS CCD CTI Column and Temperature Dependence John Biretta, Sean Lockwood, and John Debes September 26, 2015 A BSTRACT We derive column dependent CTI corrections for the STIS CCD detector which potentially could be used with a pixel-based CTI correction algorithm planned for the near future. ... Instrument Science Report STIS 2015-03 Page 23 CTI corrections were applied to the dark frames both with and without the column-dependent corrections. ...
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Ссылки http://www.stsci.edu/hst/stis/documents/isrs/2015_03.pdf -- 1178.8 Кб
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36003. http://www.stsci.edu/hst/stis/documents/isrs/2015_07.pdf
Instrument Science Report STIS 2015-07 Dark count rates in the STIS FUV MAMA ! ... Instrument Science Report STIS 2015-07 Page 2 ! Instrument Science Report STIS 2015-XX Figure 2: FUV MAMA dark rates measured following SM4 until October 2012. ... Instrument Science Report STIS 2015-XX Figure 4: FUV MAMA count rates as a function of time since turn-on for two separate visits. ... Instrument Science Report STIS 2015-XX Figure 5: Dark rates vs two temperatures with quadratic fits for a single visit. ...
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Ссылки http://www.stsci.edu/hst/stis/documents/isrs/2015_07.pdf -- 1314.0 Кб
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36004. http://www.stsci.edu/hst/wfc3/documents/ISRs/WFC3-2014-02.pdf
... As of early 2013, after about 4 years in orbit, the horizontal positions of bright stars are affected at the 0.0015-pixel level, and fainter stars are affected at the 0.004-pixel level. ... These eight exposures were acquired at orientations differing by ~10 degrees and/or dithers differing by 1000 pixels, such that stars that are close to the interamplifier boundary in one observation are far from it in the others. ... The typical exposure had 150,000 identifiable stars. ...
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Ссылки http://www.stsci.edu/hst/wfc3/documents/ISRs/WFC3-2014-02.pdf -- 547.1 Кб
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36005. http://www.stsci.edu/hst/wfc3/documents/ISRs/WFC3-2014-04.pdf
... Type 1 processing used un-flashed dark frames and files were typically delivered several months after observations. ... Input Darks Frame Averaged 14 12 21 14 14 14 13 14 18 11 13 15 11 15 13 5 18 13 14 15 Reference File Name w1h22005i_drk.fits w1h22006i_drk.fits w1i2014gi_drk.fits w1i2014hi_drk.fits w1i2014ii_drk.fits w1i2014ji_drk.fits w1i2014ki ... -Jan-2012 25-Jan-2012 25-Jan-2012 25-Jan-2012 25-Jan-2012 25-Jan-2012 25-Jan-2012 13-Feb-2012 13-Feb-2012 13-Feb-2012 13-Feb-2012 Reference File ...
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Ссылки http://www.stsci.edu/hst/wfc3/documents/ISRs/WFC3-2014-04.pdf -- 1570.6 Кб
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36006. http://www.stsci.edu/hst/wfc3/documents/ISRs/WFC3-2014-07.pdf
... During Cycle 21 the WFC3 team is using 98 external and 1907 internal orbits of HST time divided into 33 different programs, grouped in eight categories: UVIS Detectors, IR Detector, CTE Characterization and Calibration, Astrometric Calibrations, Characterization of IR Traps, WFC3 Photometric Performances, WFC3 Grisms, and, Flatfields Calibrations. ... UVIS Grism: Flux Calibration: 2 external orbits are used to monitor the UVIS grism flux in chip2 and calibrate its flux in chip 1. ...
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Ссылки http://www.stsci.edu/hst/wfc3/documents/ISRs/WFC3-2014-07.pdf -- 1166.9 Кб
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36007. http://www.stsci.edu/hst/wfc3/documents/ISRs/WFC3-2014-09.pdf
Instrument Science Report WFC3 2014-009 Use of the Shutter Blade Side "A" for UVIS Short Exposures Kailash Sahu, Sylvia Baggett, J. MacKenty May 07, 2014 A BSTRACT WFC3 UVIS uses a shutter blade with two sides, A and B, consecutively in exposures. ... Fig. ... 2474 Fig. ... Fig. 7 shows the shutter position difference in all the WFC3 exposures taken with blade A (top) and the shutter position difference in all the commanded blade A exposures (bottom). ... No such effect is present in shutter A images. ...
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Ссылки http://www.stsci.edu/hst/wfc3/documents/ISRs/WFC3-2014-09.pdf -- 1510.6 Кб
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36008. http://www.stsci.edu/hst/wfc3/documents/ISRs/WFC3-2014-10.pdf
Instrument Science Report WFC3 2014-10 Improved TinyTIM Models for WFC3/IR J. Biretta May 08, 2014 AB STRACT We use TinyTIM version 7.4 to model a star image near the center of the WFC3/IR detector, subtract the model from the observed star, examine the residuals, and suggest changes to the TinyTIM parameters to improve the fit. The largest errors appear related to the pupil cold mask parameters and we derive improved values for those. ... Improved TinyTIM Cold Mask Parameters. ...
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Ссылки http://www.stsci.edu/hst/wfc3/documents/ISRs/WFC3-2014-10.pdf -- 652.7 Кб
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36009. http://www.stsci.edu/hst/wfc3/documents/ISRs/WFC3-2014-15.pdf
... Spectra of Vega are obtained using spatial scanning in the -1st order with the G102 and G141 grisms. ... ibtw04a8q ibtw04a9q ibtw04aaq ibtw04acq ibtw04adq ibtw04aeq ibtw04afq ibtw04agq ibtw04aiq ibtw04ajq ibtw04akq ibtw04alq V V V V Target DARK ALF-LYR ALF-LYR ALF-LYR ALF-LYR DARK ALF-LYR ALF-LYR ALF-LYR DARK ALF-LYR ALF-LYR ALF-LYR DARK ALF-LYR ALF-LYR ALF-LYR ALF-LYR DARK ALF-LYR ALF-LYR ALF-LYR ALF-LYR DARK ALF-LYR ...
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Ссылки http://www.stsci.edu/hst/wfc3/documents/ISRs/WFC3-2014-15.pdf -- 1070.0 Кб
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36010. http://www.stsci.edu/hst/wfc3/documents/ISRs/WFC3-2014-16.pdf
... However, these are a part of the definition of the photometric system. ... 0.004665 Table 1: Photometric Transformation Coefficients for Synthetic Stel Body Models Spectrum Color ABMAG STMAG BB(2500) I-( uvis1 , f814w ) 0.092 0.050 BB(2500) V-( uvis1 , f606w ) 0.629 0.473 BB(2500) V-( uvis1 , f555w ) -0.158 -0.089 BB(2500) B-( uvis1 , f475w ) 0.882 0.691 BB(2500) U-( uvis1 , f336w ) -1.094 -0.947 BB(2500) I-( uvis2 , f814w ) 0.089 0.048 BB(2500) V-( uvis2 , f606w ) 0.629 0.473 BB(2500) V-( uvis2 , ...
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Ссылки http://www.stsci.edu/hst/wfc3/documents/ISRs/WFC3-2014-16.pdf -- 240.3 Кб
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36011. http://www.stsci.edu/hst/wfc3/documents/ISRs/WFC3-2014-19.pdf
Instrument Science Report WFC3 2014-19 Sink Pixels and CTE in the WFC3/UVIS Detector Jay Anderson and Sylvia Baggett June 13, 2014 ABSTRACT Post-flashed calibration products have highlighted a previously undocumented type of image defect, which we call "sink pixels" (SPs). These pixels apparently contain a number of charge traps, and as such they under-report the number of electrons that were generated in them during the exposure. ... DO SPS TRAP CHARGE FROM UPSTREAM PIXELS? ...
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Ссылки http://www.stsci.edu/hst/wfc3/documents/ISRs/WFC3-2014-19.pdf -- 2732.7 Кб
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36012. http://www.stsci.edu/hst/wfc3/documents/ISRs/WFC3-2014-24.pdf
Instrument Science Report WFC3 2014-24 Instrument Science Report ACS 2014-03 Local Pixel Bundles: Bringing the Pixels to the People Jay Anderson Dec 9, 2014 ABSTRACT The automated galaxy-based alignment software packaged developed for the Frontier Fields program (hst2galign, see Anderson & Ogaz 2014 and http://www.stsci.edu/hst/campaigns/frontier-fields/) produces a direct mapping from the pixels of the flt frame of each science exposure into a common master frame. ...
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Ссылки http://www.stsci.edu/hst/wfc3/documents/ISRs/WFC3-2014-24.pdf -- 1192.1 Кб
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36013. http://www.stsci.edu/hst/wfc3/documents/ISRs/WFC3-2015-03.pdf
... Flux loss due to CTE degradation is a function of the source's distance from the amplifier, the source signal level, the background within the image, and the epoch of the observations. The worst-case flux losses occur in images with extremely low backgrounds. ... Applying the empirical pixel-based CTE correction algorithm can also reduce flux losses: to ~10+/-1% and ~0+/-1% (unflashed images, no background) and to 3+/-1% and 0.5+/-1% (post-flashed), for the faint and bright sources, respectively. ...
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Ссылки http://www.stsci.edu/hst/wfc3/documents/ISRs/WFC3-2015-03.pdf -- 939.9 Кб
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36014. http://www.stsci.edu/hst/wfc3/documents/ISRs/WFC3-2015-07.pdf
Operated for NASA by AURA Instrument Science Report WFC3 2015-07 WFC3 Cycle 22 Calibration Program E. Sabbi & the WFC3 Team May 11, 2015 ABSTRACT The Cycle 22 WFC3 Calibration Program runs from November 2014 through October 2015 and is designed to measure and monitor the behavior of both the UVIS and IR channels. ... UVIS Grism: Flux Calibration: 2 external orbits are used to monitor the UVIS grism flux in chip2 and calibrate its flux in chip 1. ... The WFC3 team is using 282 internal orbits to: 1. ...
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Ссылки http://www.stsci.edu/hst/wfc3/documents/ISRs/WFC3-2015-07.pdf -- 792.7 Кб
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36015. http://www.stsci.edu/hst/wfc3/documents/ISRs/WFC3-2015-08.pdf
Instrument Science Report WFC3 2015-08 A Study of the Time Variability of the PSF in F606W Images taken with WFC3/UVIS Jay Anderson, Matthew Bourque, Kailash Sahu, Elena Sabbi, Alex Viana May 28, 2015 ABSTRACT This document is the first in a series designed to study how the F606W WFC3/UVIS Point-Spread Function (PSF) changes with focus. ... The PSF fit star's central pixels. ... Figure 13: The residual PSF as extracted from star images taken at various empirically identified focus levels. ...
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Ссылки http://www.stsci.edu/hst/wfc3/documents/ISRs/WFC3-2015-08.pdf -- 2576.0 Кб
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36016. http://www.stsci.edu/hst/wfc3/documents/ISRs/WFC3-2015-10.pdf
... The accuracy caused by any non-linearity in the dispersion is estimated at ~0.1 pixel or ~2.5 е for G102 and ~5 е for G141. ... Name FILTER F098M F127M F105W G102 G102 G102 G102 F098M F127M F105W G102 F098M F127M F105W G102 F140W F167N F160W G141 G141 G141 G141 F140W F167N F160W G141 F140W F167N F160W G141 F098M G102 F098M G102 F098M G102 G102 F098M G102 F098M G102 F098M G102 F098M ...
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Ссылки http://www.stsci.edu/hst/wfc3/documents/ISRs/WFC3-2015-10.pdf -- 1717.8 Кб
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36017. http://www.stsci.edu/hst/wfc3/documents/ISRs/WFC3-2015-12.pdf
Instrument Science Report WFC3 2015-12 WFC3/UVIS Shutter Characterization Kailash Sahu, C.M. Gosmeyer, Sylvia Baggett July 08, 2015 A BSTRACT A series of internal flat field images and standard star observations were obtained to check the shutter performance. ... Our observations are consistent with the earlier finding that the variation in exposure time across the detector due to shutter shading is less than 0.1%. ... In Fig. 6 we plot the photometry for different exposure times in separate bins. ...
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Ссылки http://www.stsci.edu/hst/wfc3/documents/ISRs/WFC3-2015-12.pdf -- 587.9 Кб
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36018. http://www.stsci.edu/hst/wfc3/documents/meeting_posters/aas_224/anderson_UVIScte.pdf
HST WFC3: UVIS Charge-Transfer Efficiency Losses: Mitigation and Correction! ... BACKGROUND The WFC3/UVIS CCD detector started showing signs of charge-transfer efficiency This has been traced to the fact that CTE losses are even worse than expected images can be extremely low, on account of its extremely low dark current and the narrow-band filters, more efficient short exposures, etc.) ... THE INITIAL ACS PIXEL BASED CTE MODEL 1) Assume that warm pixels (WPs) are initially delta functions. ...
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Ссылки http://www.stsci.edu/hst/wfc3/documents/meeting_posters/aas_224/anderson_UVIScte.pdf -- 2062.7 Кб
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36019. http://www.stsci.edu/hst/wfc3/documents/meeting_posters/aas_224/bourque_UVISdark.pdf
HST WFC3: UVIS Dark Calibration! ... We present the various procedures and results of the WFC3/UVIS dark calibration, which monitors the health and stability of the UVIS detector, provides characterization of hot pixels and dark current, and produces calibration files to be used as a correction for dark current in science images. ... We outline the current algorithm for creating UVIS dark calibration files, which includes aggressive cosmic ray masking, image combination, and hot pixel flagging. ...
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Ссылки http://www.stsci.edu/hst/wfc3/documents/meeting_posters/aas_224/bourque_UVISdark.pdf -- 2342.5 Кб
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36020. http://www.stsci.edu/hst/wfc3/documents/meeting_posters/spie_2014/Deustua_Poster_SPIE_2014.pdf
... 8·10 Vega: coadded spectra G141 1995 for a detailed discussion) with uncertainties on the order of a few ! ... 1st order calibrations. ... Ratio of - 1st to + 1st order at Postion 1 for P330E 0.04 0.03 ratio Ratio of - 1st to + 1st order at Postion 2 for P330E 0.04 0.03 ratio of spectra 0.01 0.00 -0.01 1.1· 104 1.2 · 104 1.3· 104 1.4· 104 1.5· 104 1.6 · 104 1.7·10 Wavelength (angstroms) 4 ratio 0.02 0.02 0.01 0.00 -0.01 1.1· 104 1.2 · 104 1.3· 104 1.4· 104 1.5· 104 ...
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Ссылки http://www.stsci.edu/hst/wfc3/documents/meeting_posters/spie_2014/Deustua_Poster_SPIE_2014.pdf -- 1450.4 Кб
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