Cross-calibrating X-ray detectors with clusters of galaxies: an IACHEC study

TL;DR

This study assesses the cross-calibration accuracy of major X-ray instruments using galaxy clusters, finding consistent energy dependence but notable normalization discrepancies, especially in flux measurements and soft energy bands.

Contribution

It provides a detailed comparison of X-ray instrument calibrations using galaxy clusters, highlighting systematic differences and validating the energy calibration accuracy.

Findings

No significant temperature differences between instruments in 2-7 keV band.

Energy dependence of effective area is well calibrated.

Flux normalization differences of 5-10% between EPIC and ACIS.

Abstract

We used a sample of 11 nearby relaxed clusters of galaxies observed with the X-ray instruments XMM-Newton (EPIC) pn and MOS, Chandra ACIS-S and ACIS-I and BeppoSAX MECS to examine the cross-calibration of the energy dependence and normalisation of the effective area of these instruments as of December 2009. We also examined the Fe XXV/XXVI line ratio temperature measurement method for the pn and MOS. We performed X-ray spectral analysis on the XMM-Newton and Chandra data for a sample of 11 clusters. We obtained the information for BeppoSAX from DeGrandi & Molendi (2002). We compared the spectroscopic results obtained with different instruments for the same clusters in order to examine possible systematic calibration effects between the instruments. We did not detect any significant systematic differences between the temperatures derived in the 2-7 keV band using the different instruments. Also, the EPIC temperatures derived from the bremsstrahlung continuum agreed with those obtained from the Fe XXV/XXVI emission line ratio, implying that the energy dependence of the hard band effective area of the above instruments is accurately calibrated. On the other hand, the hard band EPIC/ACIS fluxes disagreed by 5-10% (i.e. at 6-25 sigma level) which indicates a similar level of uncertainty in the normalisations of the effective areas of these instruments in the 2--7 keV band. In the soft energy band (0.5-2.0 keV) there are greater cross-calibration differences between EPIC and ACIS. Due to the high statistical weight of the soft band data, the 0.5-7.0 keV band temperature measurements of clusters of galaxies with EPIC or ACIS are uncertain by ~10-15% on average.