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).  eROSITA from K. Dennerl (2024-May).

Instrument0.15-0.33 keV0.33-0.54 keV0.54-0.8 keV0.8-1.2 keV1.2-1.5 keV1.5-1.8 keV1.8-2.2 keV2.2-3.5 keV3.5-5.5 keV5.5-10 keV15-25 keV25-50 keV

50-100 keV

100-300 keV
AstroSat SXT
151510101010101010



AstroSat CZTI









20202025
AstroSat LAXPC







1515151520
Chandra ACIS33332.633.33.34.95



Chandra HETGS

105444457



Chandra ACIS-MEG
20105444457



Chandra ACIS-HEG


5444457



Chandra ACIS-LEG101075444457



Chandra HRCS-LEG577777771010



Chandra HRCI-LEG577777771010



Chandra LETGS577777771010



eROSITA44444446815



Instrument0.15-0.33 keV0.33-0.54 keV0.54-0.8 keV0.8-1.2 keV1.2-1.5 keV1.5-1.8 keV1.8-2.2 keV2.2-3.5 keV3.5-5.5 keV5.5-10 keV15-25 keV25-50 keV

50-100 keV

100-300 keV
INTEGRAL IBIS










81520
INTEGRAL SPI










555
NuSTAR







4331520
ROSAT PSPC10101010101010






RXTE PCA






510331050
RXTE HEXTE









555
Suzaku HXD









20202020
Suzaku XIS1
201510101015555



Suzaku XIS0,2,3

1510101015555



Swift BAT









154412
Swift PC/WT
15107.57.57.510555



Instrument0.15-0.33 keV0.33-0.54 keV0.54-0.8 keV0.8-1.2 keV1.2-1.5 keV1.5-1.8 keV1.8-2.2 keV2.2-3.5 keV3.5-5.5 keV5.5-10 keV15-25 keV25-50 keV

50-100 keV

100-300 keV
XMM MOS12010666666610



XMM MOS22010666666610



XMM pn2222222223



XMM RGS1
85555







XMM RGS2
85555






















Library of background models/scripts/packages


InstrumentPackage/CodeDescriptionLinks/ResourcesReferences
Chandra/ACISmkacispbackA 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 variablehttps://ui.adsabs.harvard.edu/abs/2014A%26A...566A..25B/abstract
NICERnicer_bkg_estimatorThe 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

NICERnibackgen3C50The 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

NICERSCORPEONmulti-component physically motivated background model whose parameters are tied to housekeeping data.TBP
NuSTARnuskybgd

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
  • Marelli, M., Molendi, S., Rossetti, M., Gastaldello, F., Salvetti, D., De Luca, A., Bartalucci, I., Kuhl, P., Esposito, P., Ghizzardi, S., and Tiengo, A., 2021, AJ 908, 37, Analysis of the Unconcentrated Background of the EPIC pn Camera on Board XMM-Newton, https://ui.adsabs.harvard.edu/abs/2021ApJ...908...37M/abstract
XMM/MOS

https://ui.adsabs.harvard.edu/abs/2008A%26A...478..575K/abstract
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
and spectral analysis significantly.

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
  • Antia, H.M., Agrawal, P.C., Katoch, T., Manchanda, R.K., Mukerjee, K., and Shah, P., 2022, ApJS, accepted,

    Improved background model for the Large Area X-ray Proportional Counter (LAXPC) instrument on-board AstroSat, https://arxiv.org/abs/2205.03136


Attachments:

  File Modified
PDF File Intro.pdf A short list of topics for the IACHEC WG in Beijing. Apr 20, 2015 12:46 by Herman Lee Marshall
PDF File jdrake_caluncert.pdf MC cal uncert for XMM Apr 20, 2015 20:21 by Herman Lee Marshall
Microsoft Powerpoint Presentation CalUn_IACHEC2015.pptx Cal uncertainties for NuSTAR Apr 20, 2015 20:21 by Herman Lee Marshall
PDF File ChisqBias.pdf Use of ML preferable to chi-square. Apr 20, 2015 20:23 by Herman Lee Marshall
PDF File Meng_astronote_20150410.pdf Preliminary analysis for reconciling disparate instruments. Apr 21, 2015 03:42 by Herman Lee Marshall

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