In the bottom of this page you find the spectra, responses and background files necessary to reproduce the spectral analysis in Nevalainen et al., 2010 (A&A, 523, 22) which yielded results summarised in Fig 1.
Fig.1: The average relative difference (diamonds) +- the error of the mean of the fluxes (solid line) and temperatures (dotted line) for different instrument pairs in the soft band (left side of the plot) and in the hard band (right side of the plot)
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For most clusters the Chandra data are obtained with ACIS-S, but for some ACIS-I is used, and marked accordingly.
The script files bestfit....xcm will set up the best fit. In more detail:
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- *hard*, *soft* and *wide* refer to the fits done in 2.0-7.0 keV, 0.5-2.0 keV and 0.5-7.0 keV bands, respectively.
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For flux comparison, scale the measured fluxes to the full annulus by dividing with the fraction of the covered full annulus
The following links provide a single tar file for each cluster-instrument combination, containing the spectral analysis material described above:
Cluster Instrument
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MKW3S XMM-Newton/pn XMM-Newton/MOS Chandra/ACIS-I
The following links contain some tabulated data from Nevalainen et al., 2010 paper in electronic form.
The first column gives the number X the of the cluster name AX, except for non-Abell names:
Coma = 1111, HydraA = 2222, MKW3S = 3333Data of Table A.1 in electronic form
pn
Note that for A262 the soft and wide band temperatures are not presented, but instead marked with -999
XMM-Newton pn temperatures obtained within Chandra-driven regions
XMM-Newton pn, MOS1 and MOS2 wide band temperatures with large XMM-only regions
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Attachments
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