Calibration Statistics Working Group
The main page of the CalStats WG is at https://iachec.org/calibration-statistics/
The τ-matrix of effective area uncertainties
Based on Tables 1 and 2 of Marshall et al. (2021; AJ 162, 254), modified by H. Marshall during IACHEC XVI (2024-May)
| Instrument | 0.15-0.33 keV | 0.33-0.54 keV | 0.54-0.8 keV | 0.8-1.2 keV | 1.2-1.5 keV | 1.5-1.8 keV | 1.8-2.2 keV | 2.2-3.5 keV | 3.5-5.5 keV | 5.5-10 keV | 15-25 keV | 25-50 keV | 50-100 keV | 100-300 keV |
|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|
| AstroSat SXT | 15 | 15 | 10 | 10 | 10 | 10 | 10 | 10 | 10 | |||||
| AstroSat CZTI | 20 | 20 | 20 | 25 | ||||||||||
| AstroSat LAXPC | 15 | 15 | 15 | 15 | 20 | |||||||||
| Chandra ACIS | 3 | 3 | 3 | 3 | 2.6 | 3 | 3.3 | 3.3 | 4.9 | 5 | ||||
| Chandra ACIS-MEG | 20 | 10 | 5 | 4 | 4 | 4 | 4 | 5 | 7 | |||||
| Chandra ACIS-HEG | 5 | 4 | 4 | 4 | 4 | 5 | 7 | |||||||
| Chandra ACIS-LEG | 10 | 10 | 7 | 5 | 4 | 4 | 4 | 4 | 5 | 7 | ||||
| Chandra HRCS-LEG | 5 | 7 | 7 | 7 | 7 | 7 | 7 | 7 | 10 | 10 | ||||
| Chandra HRCI-LEG | 5 | 7 | 7 | 7 | 7 | 7 | 7 | 7 | 10 | 10 | ||||
| INTEGRAL IBIS | 8 | 15 | 20 | |||||||||||
| INTEGRAL SPI | 5 | 5 | 5 | |||||||||||
| NuSTAR | 4 | 3 | 3 | 15 | 20 | |||||||||
| ROSAT PSPC | 10 | 10 | 10 | 10 | 10 | 10 | 10 | |||||||
| RXTE PCA | 5 | 10 | 3 | 3 | 10 | 50 | ||||||||
| RXTE HEXTE | 5 | 5 | 5 | |||||||||||
| Suzaku HXD | 20 | 20 | 20 | 20 | ||||||||||
| Suzaku XIS1 | 20 | 15 | 10 | 10 | 10 | 15 | 5 | 5 | 5 | |||||
| Suzaku XIS0,2,3 | 15 | 10 | 10 | 10 | 15 | 5 | 5 | 5 | ||||||
| Swift BAT | 15 | 4 | 4 | 12 | ||||||||||
| Swift PC/WT | 15 | 10 | 7.5 | 7.5 | 7.5 | 10 | 5 | 5 | 5 | |||||
| XMM MOS1 | 20 | 10 | 6 | 6 | 6 | 6 | 6 | 6 | 6 | 10 | ||||
| XMM MOS2 | 20 | 10 | 6 | 6 | 6 | 6 | 6 | 6 | 6 | 10 | ||||
| XMM pn | 2 | 2 | 2 | 2 | 2 | 2 | 2 | 2 | 2 | 3 | ||||
| XMM RGS1 | 8 | 5 | 5 | 5 | 5 | |||||||||
| XMM RGS2 | 8 | 5 | 5 | 5 | 5 | |||||||||
Library of background models/scripts/packages
| Instrument | Package/Code | Description | Links/Resources | References |
|---|---|---|---|---|
| Chandra/ACIS | mkacispback | A software to generate spectral models for Chandra ACIS particle-induced background, by Hiromasa Suzuki (UTokyo) | https://github.com/hiromasasuzuki/mkacispback |
|
| Chandra/ACIS-I | Continuum modeled as a combination of power-law and exponential, amplitudes changing along y direction; 11 fluorescent lines, six of which are spatially variable | https://ui.adsabs.harvard.edu/abs/2014A%26A...566A..25B/abstract |
| |
| NICER | nicer_bkg_estimator | The nicer_bkg_estimator tool implements the "space weather" method (Gendreau et al., in prep.) which uses environmental data to parse the background database. This tool uses a model of the magnetic cut-off rigidity as well as space weather data in the form of the planetary Kennziffer Index, or Kp index | https://heasarc.gsfc.nasa.gov/docs/nicer/tools/nicer_bkg_est_tools.html Readme: https://heasarc.gsfc.nasa.gov/docs/nicer/tools/nicer_bkg_estimator_README.txt |
|
| NICER | nibackgen3C50 | The nibackgen3C50 tool (Remillard et al.) makes use of a number of background proxies in the NICER data to define the basis states of the background database. | https://heasarc.gsfc.nasa.gov/docs/nicer/tools/nicer_bkg_est_tools.html Readme: https://heasarc.gsfc.nasa.gov/docs/nicer/tools/README_nibackgen3C50_v7b.txt |
|
| NICER | SCORPEON | multi-component physically motivated background model whose parameters are tied to housekeeping data. | TBP |
|
| NuSTAR | nuskybgd | Broadband (3-160 keV) background with appropriate response. Produces background models for arbitrary source locations in FoV, and band-selected background images. Authored by Dan Wik, python-port by Qian Wang. | https://github.com/NuSTAR/nuskybgd-py |
|
| XMM/pn | https://ui.adsabs.harvard.edu/abs/2021ApJ...908...37M/abstract |
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| XMM/MOS | https://ui.adsabs.harvard.edu/abs/2008A%26A...478..575K/abstract |
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| AstroSAT/LAXPC | The LAXPC team have described an improved model for LAXPC background, which incorporates the diurnal variation that was observed earlier. It also identifies some time period in a few orbits just after SAA exit which are badly affected by SAA and are now eliminated from GTI. These coupled with some improvements in calculating the gain shift in LAXPC20 have improved the background estimate for both light curve These are incorporated in the latest version (3.4.3) of the software available from the LAXPC website https://www.tifr.res.in/~astrosat_laxpc/LaxpcSoft.html Accounts for latitudinal, longitudinal, and quasi-diurnal (84495 s) variations. | https://arxiv.org/abs/2205.03136 |
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