300 likes | 454 Views
Chandra Calibration Status. CUC Meeting Oct. 13, 2011. Calibration updates since the 2010 CUC meeting Internal Chandra cross-calibration status Current calibration issues. Chandra Calibration Status. Recent Calibration Products and Software Releases. ACIS.
E N D
Chandra Calibration Status CUC Meeting Oct. 13, 2011
Calibration updates since the 2010 CUC meeting • Internal Chandra cross-calibration status • Current calibration issues Chandra Calibration Status
Recent Calibration Products and Software Releases ACIS • ACIS temperature-dependent gain correction software for timed-event (TE) mode data was released in CIAO 4.4.1 on Dec. 15, 2010. • ACIS cti-correction software for TE data in graded (G) telemetry mode was released in CIAO 4.3 • A new contamination model for the ACIS-I was released in CALDB 4.4.1 • Time-dependent gain corrections for epochs 43-46 ( Aug 2010 – July 2011)
Recent Calibration Products or Software Releases HRC • An update to the HRC-I QE to improve cross-calibration between HRC-I/HRC-S/ACIS-S was released in CALDB 4.4.1 • HRC-I gain map for 2010 was released in CALDB 4.4.1 • HRC-S rmf (using SAMP) was released in CALDB 4.4.1 • A series of time-dependent HRC-S QE maps (one for each year) were released in CALDB 4.4.5 (June 30, 2011)
Recent Calibration Products or Software Releases LETG • Updated extraction regions and the clocking angle for dispersed LETG/ACIS-S spectra were released in CALDB 4.1.1 • Revised LETG transmission efficiencies for orders m=2-10 were released in CALDB 4.4.3 (April 26, 2011)
Internal Chandra Cross-Calibration Calibration products derived from ground-based data. • HRMA effective area • ACIS-S and ACIS-I QE • LETG first order efficiency • MEG first order efficiency for E<1 keV • HEG first order efficiency for E>1 keV • Shape of HRC QE Calibration products derived in-flight data and internal cross-calibration • HRC-I and HRC-S QE • LETG higher order efficiencies • ACIS contamination model • MEG first order efficiency for E>1keV • HEG first order efficiency for E<1keV
Internal Chandra Cross-Calibration Bare ACIS-S/ACIS-I cross-calibration Abell 1795 phabs*apec 0.5-7.0 keV 5% Abundance Temperature 3% Flux
Bare ACIS-S/ACIS-I cross-calibration NHS=3.07 NHI=2.91 Gs=1.84 GI=1.78 G21.5-09 phabs*pow Column density Power-law index Filled symbols – full-frame Open symbols – sub-array Flux
Bare HRC-I/HRC-S/ACIS-S cross-calibration G21.5-09 3%
Mirror Vignetting and ACIS QE MAP Abell 1795 ACIS-I3 aim point X ACIS-S read-out
Current ACIS Calibration Issues ACIS contamination model ACIS-I3 X Simultaneous two-temperature fit to 13108, 13112 and 13113
ACIS contamination model 13108 and 13109 Simultaneous two-temperature fit to 13108 and 13111
Spectral fit to the July 2011 LETG/ACIS-S observation of Mkn 421
Time-dependent ACIS QE ACIS-S3
Time-dependent ACIS QE ACIS-I3 Solution – a set of time sorted QEU maps
ACIS-S1 Gain E0102-72 observations on S1 node 2
ACIS-S1 Gain Near default LETG/ACIS-S configuration E0102-72
Feature near the Si-K edge in bright sources Cyg X-2 TE Mode CC Mode
CC-F mode calibration Required products for CC-F mode calibration • Trap maps for CC mode data - done • Gain tables for CC mode data – done • QE tables for CC mode data After Dec. 2009 – done Before Dec. 2009 – being worked
Current LETG/HRC-S Calibration Issues Result of current grey correction – broad band flux
Current HETG Calibration Issues Sample of about 30 HETG/ACIS-S AGN observations CALDB CALDB version
Current Imaging Issues Dithered SAOTrace simulation of an HRC-I observation of AR Lac
HRC-I intrinsic spatial response Raw Gaussian Gaussian plus Lorentzian
Summary of Present Calibration Activities • Release CC- F mode calibration products • Release MEG/HEG first order transmission correction • Release updated ACIS contamination model • Investigate low energy HRC-S QE losses • Investigate Si-K edge feature in ACIS data of very bright sources • Improve the low energy gain calibration of S1 • Incorporate dithered SAOTrace rays and updated HRC-I spatial response into MARX • Revise SAOTrace to produce better agreement between the raytrace simulations and the observed power in the wings of the PSF