2010A&A...523A..22N


C.D.S. - SIMBAD4 rel 1.7 - 2019.10.15CEST19:57:24

2010A&A...523A..22N - Astronomy and Astrophysics, volume 523, A22-22 (2010/11-2)

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

NEVALAINEN J., DAVID L. and GUAINAZZI M.

Abstract (from CDS):

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 FeXXV/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 (2002ApJ...567..163D). 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 2-7keV band using the different instruments. Also, the EPIC temperatures derived from the bremsstrahlung continuum agreed with those obtained from the FeXXV/XXVI emission line ratio, implying that the energy dependence of the hard band effective area of the above instruments is accurately calibrated. This also indicates that deviations from ionisation equilibrium and a Maxwellian electron velocity distribution are negligible in the regions studied in the cluster sample. We thus consider the IACHEC sample of clusters of galaxies as standard candles for the calibration of the energy dependence of the hard band (2-7keV) effective area of X-ray telescopes. On the other hand, the hard band EPIC/ACIS fluxes disagreed by 5-10% (i.e. at 6-25σ level) which indicates a similar level of uncertainty in the normalisations of the effective areas of these instruments in the 2-7keV band. In the soft energy band (0.5-2.0keV) there are greater cross-calibration differences between EPIC and ACIS. We found an energy-dependent increase of ACIS versus pn bias in the cross-calibration of the effective area by ∼10% in the 0.5-2.0keV band. This amounts to a systematic difference of (∼20%) in the temperatures measured by the ACIS and the EPIC-pn cameras in this band. Due to the high statistical weight of the soft band data, the 0.5-7.0keV band temperature measurements of clusters of galaxies with EPIC/XMM-Newton or ACIS/Chandra are uncertain by ∼10-15% on average. These uncertainties will also affect the analysis of the wide band continuum spectra of other types of objects using ACIS or EPIC.

Abstract Copyright:

Journal keyword(s): instrumentation: miscellaneous - techniques: spectroscopic - galaxies: clusters: intracluster medium - X-rays: galaxies: clusters

Simbad objects: 12

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Number of rows : 12

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2019
#notes
1 ACO 85 ClG 00 41 37.8 -09 20 33           ~ 766 0
2 ACO 262 ClG 01 52 50.4 +36 08 46           ~ 645 1
3 ACO 3112 ClG 03 17 52.4 -44 14 35           ~ 283 1
4 NAME Hya A LIN 09 18 05.651 -12 05 43.99   14.38 14.8     ~ 877 1
5 NGC 4874 LIN 12 59 35.709 +27 57 33.80 13.01 13.7 11.40 12.122 11.386 ~ 698 3
6 ACO 1656 ClG 12 59 48.7 +27 58 50           ~ 4095 2
7 ACO 3571 ClG 13 47 28.9 -32 51 57           ~ 260 2
8 ACO 1795 ClG 13 49 00.5 +26 35 07           ~ 1133 0
9 ACO 2029 ClG 15 10 58.7 +05 45 42           ~ 835 0
10 ACO 2052 ClG 15 16 45.5 +07 00 01           ~ 664 1
11 NAME NGC 5920 Group ClG 15 21 50.7 +07 42 18     15.13     ~ 281 0
12 ACO 2199 ClG 16 28 37.0 +39 31 28           ~ 1084 1

    Equat.    Gal    SGal    Ecl

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2019.10.15-19:57:24

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