Issue |
A&A
Volume 419, Number 2, May IV 2004
|
|
---|---|---|
Page(s) | 517 - 525 | |
Section | Extragalactic astronomy | |
DOI | https://doi.org/10.1051/0004-6361:20034477 | |
Published online | 03 May 2004 |
An X-ray review of MS 1054–0321: Hot or not?*
1
Istituto di Radioastronomia del CNR-INAF, via P. Gobetti 101, 40129 Bologna, Italy e-mail: gioia@ira.cnr.it
2
INAF - Osservatorio Astronomico di Brera, via Brera 28, 20121 Milano, Italy e-mail: braito@brera.mi.astro.it, e-mail: rdc@brera.mi.astro.it, e-mail: tommaso@brera.mi.astro.it
3
Dipartimento Astronomia Universitá di Bologna, via Ranzani 1, 40127 Bologna, Italy e-mail: mbranch@ira.cnr.it
4
Institute for Astronomy, ETH Hoenggerberg, HPF G4.2 8093 Zurich, Switzerland e-mail: vy@phys.ethz.ch
Corresponding author: I. M. Gioia, gioia@ira.cnr.it
Received:
8
October
2003
Accepted:
24
February
2004
XMM-Newton observations are presented for the
cluster of galaxies MS 1054-0321, the highest redshift
cluster in the Einstein Extended Medium Sensitivity Survey (EMSS).
The temperature inferred by the XMM-Newton data,
keV, is much lower than the temperature
previously reported from ASCA data,
keV
(Donahue et al. 1998), and a little lower than the Chandra temperature,
keV, determined by Jeltema et al. 2001.
The discrepancy between the newly derived temperature and the
previously derived temperatures is discussed in detail.
If one allows the column density to be a free parameter, then the best fit
temperature becomes
keV, and the best fit
column density becomes
atoms cm-2.
The iron line is well detected in the XMM-Newton spectrum
with a value for the abundance of
, in very good agreement with previous determinations. The derived XMM
X-ray luminosity for the overall cluster in the 2–10 keV
energy band is
erg s-1
while the bolometric luminosity is
erg s-1.
The XMM-Newton data confirm the substructure in the cluster X-ray
morphology already seen by ROSAT and in much more detail by Chandra.
We find that only two of the three clumps detected in the weak lensing
mass reconstruction image are visible in X-rays, as already noted by
[CITE]. The central weak lensing clump is
coincident with the main cluster component and has a
temperature
keV. The western weak lensing
clump coincides with the western X-ray component which is much
cooler with a temperature
keV.
The optically measured velocity dispersion, obtained from 145 cluster
redshifts, is consistent with the velocity dispersion expected from
the
relationship once the XMM-Newton temperature
is used. MS 1054-0321 fits well in the
correlation available in the literature and derived from information
collected for all clusters at redshfits of
known today and
with a measured X-ray temperature. The cluster temperature seems to be
commensurate with the predictions from its X-ray luminosity from the
relation of local clusters. Given the newly determined
temperature, MS 1054-0321 is no longer amongst the hottest clusters known.
Key words: galaxies: clusters: general / galaxies: clusters: individual: MS 1054-0321 / cosmology: dark matter / X-rays: galaxies: clusters / galaxies: intergalactic medium
© ESO, 2004
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