s#c#_#.rsp

caldb/data/asca/sis/cpf/93apr22

Unknown

(Andy Rasmussen, MIT, 1993 Apr 22)

A total of 16 files using a naming convention s$i$c$j$_$xxx$.rsp where

• $i$ represents the SIS sensor ($i$ = 0 or 1)
• $j$ represents the CCD chip ($j$ = 0, 1, 2 or 3)
• $xxx$ gices the number of detector channels in the matrix ($xxx$ = 512 or 1024)

These response matrices include chip-to-chip differences in gain and also in readout noise (all ground-measured values). It has be noticed that these gains are often off by 1-2% when attempting to fit sources seen with ASUKA using XSPEC. .. So don't be surprised if you have to use the `gain' task to adjust the gain and yield a better fit. Chip-to-chip differences in `chip architecture' have not been employed on these matrices; therefore they should be considered correct to `first order. More precise matrices will be made available as soon as the CRAB data analysis is completed.

Supplementary explanation:
(Koji Mukai, NASA/GSFC Asuka GOF, 1993 Apr 22)

These files seem to use effective area curve for 2 telescopes, even though each file is for a single CCD chip. Also the area used is on-axis values, no vignetting is included. Both 512 and 1024 channel files have equal sized pha bins. Note that the bright & fast mode data are compressed into 2048 bins where higher energy channels are compressed more. Real data files have a threshold below which 0 is output. Use ignore 1-12 or thereabout (with the 512 matrices).
SUMMARY:
files includes 2 XRT effective area; CCD QE for photon event grades 0-4; Thermal Shield transmission; Read-out-noise and other factors that determines spectral resolution, including fluorescence...

Koji Mukai (NASA/GSFC ASCA GOF) in SF format, reformatted to OGIP standard by Ian M George.

OGIP format RMFVERSN = 1992a (see CAL/GEN/92-002).

See above

• Ian M George (HEASARC) 1993 Apr 22
  • (see above)
• Ian M George (HEASARC) 1995 Dec 08
  • Dataset renamed from s$i$c$j$_$xxx$.rmf and moved to current location at the request of the ASCA GOF at NASA/GSFC