346 research outputs found
XMM-Newton observations of the binary cluster system Abell 399/401
Abell 399 and Abell 401 are both rich clusters of galaxies, at temperatures
7.2keV and 8.5keV respectively. They lie at a projected separation of ~3Mpc,
forming a close pair. We have observed the system with the XMM-Newton
satellite. The data of each cluster show significant departures from our
idealised picture of relaxed rich clusters. There is also evidence for enhanced
X-ray flux in the region between the two, where the temperature is higher than
our expectations.
Although tidal or compression effects might affect the large scale structure
of the two clusters, we show that these cannot account for the distortions seen
in the inner regions. We argue that the reasonably relaxed morphology of the
clusters, and the absence of major temperature anomalies, argues against models
in which the two have already experienced a close encounter. The properties of
the intermediate region suggests that they are at an early stage of merging,
and are currently interacting mildly, because their separation is still too
large for more dramatic effects. The substructure we find in their inner
regions seems to point to their individual merging histories. It seems likely
that in the Abell 399/401 system, we are witnessing two merger remnants, just
before they merge together to form a single rich cluster. This picture is
consistent with recent numerical simulations of cluster formation. (abridged)Comment: 20 pages, 14 figures, to be published in MNRA
XMM-Newton observations of Abell 2255 : a test case of a merger after `core-crossing'
It has been known that Abell 2255 is not a relaxed cluster, but it is
undergoing a merger. Here, we report on the analysis of the XMM-Newton
observations of this cluster. The X-ray data give us the opportunity to reveal
the complexity of the cluster, especially its temperature distribution. The
integrated spectrum is well fitted by a single temperature thermal model,
indicating a mean temperature of ~7 keV. However, the cluster is not isothermal
at this temperature: its eastern regions are significantly cooler, at ~5.5 keV,
whilst towards the West the temperature reaches ~8.5 keV.
These temperature asymmetries can be explained if Abell 2255 has been
assembled recently by the merging of smaller subunits. It is now in the phase
after the cores of these subunits have collided (the `core-crossing' phase)
some 0.1-0.2 Gyr ago. A comparison with numerical simulations suggests that it
will settle down into a single relaxed cluster in ~(2-3) Gyr.Comment: 9 pages, 6 figures, accepted by MNRA
Are "Bondi-Hoyle Wakes" detectable in clusters of galaxies?
In clusters of galaxies, the reaction of the intracluster medium (ICM) to the
motion of the co-existing galaxies in the cluster triggers the formation of
unique features, which trace their position and motion. Galactic wakes, for
example, are an apparent result of the ICM/galaxy interactions, and they
constitute an important tool for deciphering the motion of the cluster
galaxies. In this paper we investigate whether Bondi-Hoyle accretion can create
galactic wakes by focusing the ICM behind moving galaxies. The solution of the
equations that describe this physical problem provide us with observable
quantities along the wake at any time of its lifetime. We also investigate
which are the best environmental conditions for the detectability of such
structures in the X-ray images of clusters of galaxies. We find that
significant Bondi-Hoyle wakes can only be formed in low temperature clusters,
and that they are more pronounced behind slow-moving, relatively massive
galaxies. The scale length of these elongated structures is not very large: in
the most favourable conditions a Bondi-Hoyle wake in a cluster at the redshift
of z=0.05 is 12 arcsec long. However, the wake's X-ray emission is noticeably
strong: the X-ray flux can reach ~30 times the flux of the surrounding medium.
Such features will be easily detectable in Chandra's and XMM-Newton's X-ray
images of nearby, relatively poor clusters of galaxies.Comment: 8 pages with 11 Postscript figures, accepted for publication in MNRA
The cool wake around 4C 34.16 as seen by XMM-Newton
We present XMM-Newton observations of the wake-radiogalaxy system 4C34.16,
which shows a cool and dense wake trailing behind 4C34.16's host galaxy. A
comparison with numerical simulations is enlightening, as they demonstrate that
the wake is produced mainly by ram pressure stripping during the galactic
motion though the surrounding cluster. The mass of the wake is a substantial
fraction of the mass of an elliptical galaxy's X-ray halo. This observational
fact supports a wake formation scenario similar to the one demonstrated
numerically by Acreman et al (2003): the host galaxy of 4C34.16 has fallen into
its cluster, and is currently crossing its central regions. A substantial
fraction of its X-ray halo has been stripped by ram pressure, and remains
behind to form the galaxy wake.Comment: 9 pages, 6 figures, accepted for publication in MNRA
X-Ray Wakes in Abell 160
`Wakes' of X-ray emission have now been detected trailing behind a few (at
least seven) elliptical galaxies in clusters. To quantify how widespread this
phenomenon is, and what its nature might be, we have obtained a deep (70 ksec)
X-ray image of the poor cluster Abell 160 using the ROSAT HRI. Combining the
X-ray data with optical positions of confirmed cluster members, and applying a
statistic designed to search for wake-like excesses, we confirm that this
phenomenon is observed in galaxies in this cluster. The probability that the
detections arise from chance is less than 0.0038. Further, the wakes are not
randomly distributed in direction, but are preferentially oriented pointing
away from the cluster centre. This arrangement can be explained by a simple
model in which wakes arise from the stripping of their host galaxies'
interstellar media due to ram pressure against the intracluster medium through
which they travel.Comment: 7 pages, 7 figures, accepted for publication in MNRA
Δούκα-Καμπίτογλου Αικατερίνη, Μυθιστόρημα Γυναίκας: Ποιήτριες του 20ου αιώνα
No abstract (available)
Simulations of the Effects of Stripping and Accretion on Galaxy Haloes in Clusters
We present results from a series of hydrodynamic simulations investigating
ram pressure stripping of galactic haloes as the host galaxy falls radially
into a cluster. We perform a parameter study comprising of variations in
initial gas content, gas injection rate (via stellar mass loss processes),
galaxy mass and amplitude of infall. From the simulation results we track
variations in both physical quantities (e.g. gas mass) and directly observable
quantities (e.g. X-ray luminosities). The luminosity of the galaxy's X-ray halo
is found to compare favourably with the observationally determined correlation
with optical blue band luminosity (L_X:L_B) relation. Factors affecting the
X-ray luminosity are explored and it is found that the gas injection rate is a
dominant factor in determining the integrated luminosity. Observational
properties of the material stripped from the galaxy, which forms an X-ray wake,
are investigated and it is found that wakes are most visible around galaxies
with a substantial initial gas content, during their first passage though the
cluster. We define a statistical skewness measure which may be used to
determine the direction of motion of a galaxy using X-ray observations.
Structures formed in these simulations are similar to the cold fronts seen in
observation of cluster mergers where a sharp increase in surface brightness is
accompanied by a transition to a cooler region.Comment: Accepted for publication in MNRAS. 19 pages, 21 figure
The origin and evolution of cluster magnetism
Random motions can occur in the intergalactic gas of galaxy clusters at all
stages of their evolution. Depending on the poorly known value of the Reynolds
number, these motions can or cannot become turbulent, but in any case they can
generate random magnetic fields via dynamo action. We argue that magnetic
fields inferred observationally for the intracluster medium require dynamo
action, and then estimate parameters of random flows and magnetic fields at
various stages of the cluster evolution. Polarization in cluster radio halos
predicted by the model would be detectable with the SKA.Comment: 4 pages, 1 figure, to be published by Astronomische Nachrichten
(proceedings of "The Origin and Evolution of Cosmic Magnetism", 29 August - 2
September 2005, Bologna, Italy); version updated to match the accepted tex
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