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main:nonbruce_instrument_info [2014/01/27 22:25]
bruce [UFOT Info] 		main:nonbruce_instrument_info [2022/01/15 01:37] (current)
bruce [GBM Localization]
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-**Non-Bruce GRB Instrumentation Information**+====== Non-Bruce GRB Instrumentation Information ====== 
 +---- 
 + 
 +====== Quick Links ====== 
 + 
 +[[https://www-astro.lbl.gov/~bruce/docuwikis/brucework/doku.php?id=infotree:general_astro:observing#x-gamma_instruments_characteristics|General X- and gamma-ray instrument info table]] - instruments better for 0.1-10 keV included. 
  
  
 ---- ----
 +
 +----
 +
 +
 +
 +====== Launches ======
 +
 +You can find information on Scheduled Space Launches on this page: http://www.satelliteonthenet.co.uk/index.php/2015
 +
  
 ====== Swift ====== ====== Swift ======
 +----
  
 +===== Swift BAT =====
  
  
 +[[public:swift_instrument|BAT info]] on a separate page
 +
 +===== Swift UVOT =====
 +
 +
 +==== UVOT Photometry ====
  
-===== UVOT Info ===== 
  
-UVOT Photometry:  
  
 The Swift UVOT Users's guide http://swift.gsfc.nasa.gov/analysis/UVOT_swguide_v2_2.pdf, P. 76 says, " look at http://heasarc.gsfc.nasa.gov/docs/heasarc/caldb/swift/docs/uvot/" for integrated PSFs. The Swift UVOT Users's guide http://swift.gsfc.nasa.gov/analysis/UVOT_swguide_v2_2.pdf, P. 76 says, " look at http://heasarc.gsfc.nasa.gov/docs/heasarc/caldb/swift/docs/uvot/" for integrated PSFs.
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 UVOT W band PSF is FWHM = 2.37 "  http://heasarc.gsfc.nasa.gov/docs/heasarc/caldb/swift/docs/uvot/uvot_caldb_psf_02.pdf UVOT W band PSF is FWHM = 2.37 "  http://heasarc.gsfc.nasa.gov/docs/heasarc/caldb/swift/docs/uvot/uvot_caldb_psf_02.pdf
 THERE IS AN IMPORTANT TRICK FOR CALDB: the curve-of-growth is normalized at 5"; ALL FLUX is really about 115% for W, not 100%. THERE IS AN IMPORTANT TRICK FOR CALDB: the curve-of-growth is normalized at 5"; ALL FLUX is really about 115% for W, not 100%.
- + 
 +=== Photometric Calibration of W band === 
 + 
 +http://heasarc.gsfc.nasa.gov/docs/heasarc/caldb/swift/docs/uvot/uvot_caldb_counttofluxratio_10wa.pdf describes the calibration of UVOT filters. 
 + 
 +Their procedure calculates the flux-weighted effective wavelength of vega (3470Å); then calculates ratios of expected count rate for f_nu~ nu^+2 spectrum;  (I use index= +0.75).   They give a "count rate to flux ratio" for various indices and extinctions of 2.6 to 4.4e-17.  I just assume use 3.5e-17.  They give errors on this of > 10%.    
 + 
 + 
 +====== Fermi GBM ====== 
 + 
 + 
 +Fermi GBM is like a smaller version of BATSE; scintillators on the corners of cube geometry give all-sky (with earth occulting a LOT of the sky) coverage and rough localization.   
 + 
 +===== GBM Localization ===== 
 + 
 +The reference here is Connaughton+15 ApJS https://iopscience.iop.org/article/10.1088/0067-0049/216/2/32#apjs506206s6.  
 + 
 +Ground-Automated GCN NOtices 30-60 s after trigger give 68% probability within (+/- or radius) 7.6 deg; there is a much larger tail for like 90% probability. BRIGHT SUB-SAMPLE: GRBs reported with only 1 deg.  statistical uncertainty, 68% radius=2.9 deg.  
 + 
 +one degree radius looks like it would get you about 10% of the Bright Sub-sample.  for a square FOV, that's 1.7 deg on a side - yuk.  two deg on a side gets you radius = 1.13 deg and around 17.5% of Bright sample events. So, that helps. 
 + 
 +HiTL (Human in the Loop) positions are available ~ 1 hr later. 68% prob. radius=5.3 deg.  BRIGHT SUB-SAMPLE: for For GRBs reported with only 1 deg. statistical uncertainty, 68% radius=3.4 deg (yes, worse than automated).  
 + 
 + 
 + 
main/nonbruce_instrument_info.1390861549.txt.gz · Last modified: 2021/01/12 00:50 (external edit)

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