116 research outputs found
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
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
The Chandra Deep Group Survey -- cool core evolution in groups and clusters of galaxies
We report the results of a study which assembles deep observations with the
ACIS-I instrument on the Chandra Observatory to study the evolution in the core
properties of a sample of galaxy groups and clusters out to redshifts . A search for extended objects within these fields yields a total of 62
systems for which redshifts are available, and we added a further 24
non-X-ray-selected clusters, to investigate the impact of selection effects and
improve our statistics at high redshift. Six different estimators of cool core
strength are applied to these data: the entropy (K) and cooling time
() within the cluster core, the cooling time as a fraction of the age
of the Universe (), and three estimators based on the
cuspiness of the X-ray surface brightness profile. A variety of statistical
tests are used to quantify evolutionary trends in these cool core indicators.
In agreement with some previous studies, we find that there is significant
evolution in , but little evolution in , suggesting
that gas is accumulating within the core, but that the cooling time deep in the
core is controlled by AGN feedback. We show that this result extends down to
the group regime and appears to be robust against a variety of selection biases
(detection bias, archival biases and biases due to the presence of central
X-ray AGN) which we consider.Comment: Accepted by MNRAS, 24 pages, 11 figure
X-ray bright groups and their galaxies
Combining X-ray data from the ROSAT PSPC and optical data drawn from the
literature, we examine in detail the relationship between the X-ray and optical
properties of X-ray bright galaxy groups. We find a relationship between
optical luminosity and X-ray temperature consistent with that expected from
self-similar scaling of galaxy systems, L_B \propto T^{1.6 +/- 0.2}. The
self-similar form and continuity of the L_B : T relation from clusters to
groups and the limited scatter seen in this relation, implies that the star
formation efficiency is rather similar in all these systems. We find that the
bright extended X-ray components associated with many central galaxies in
groups appear to be more closely related to the group than the galaxy itself,
and we suggest that these are group cooling flows rather than galaxy halos. In
addition we find that the optical light in these groups appears to be more
centrally concentrated than the light in clusters. We also use the optical and
X-ray data to investigate whether early or late type galaxies are primarily
responsible for preheating in groups. Using three different methods, we
conclude that spiral galaxies appear to play a comparable role to early types
in the preheating of the intragroup medium. This tends to favour models in
which the preheating arises primarily from galaxy winds rather than AGN, and
implies that spirals have played a significant role in the metal enrichment of
the intragroup medium.Comment: 17 pages, accepted for publication in MNRA
The central elliptical galaxy in fossil groups and formation of BCGs
We study the dominant central giant elliptical galaxies in ``Fossil groups''
using deep optical (R-band) and near infrared (Ks-band) photometry. These
galaxies are as luminous as the brightest cluster galaxies (BCGs), raising
immediate interest in their link to the formation of BCGs and galaxy clusters.
However, despite apparent similarities, the dominant fossil galaxies show
non-boxy isophotes, in contrast to the most luminous BCGs. This study suggests
that the structure of the brightest group galaxies produced in fossil groups
are systematically different to the majority of BCGs. If the fossils do indeed
form from the merger of major galaxies including late-types within a group,
then their disky nature is consistent with the results of recent numerical
simulations of semi-analytical models which suggest that gas rich mergers
result in disky isophote ellipticals.
We show that fossils form a homogeneous population in which the velocity
dispersion of the fossil group is tightly correlated with the luminosity of the
dominant elliptical galaxy. This supports the scenario in which the giant
elliptical galaxies in fossils can grow to the size and luminosity of BCGs in a
group environment. However, the boxy structure of luminous BCGs indicate that
they are either not formed as fossils, or have undergone later gas-free mergers
within the cluster environment.Comment: 5 pages, 4 figures, Accepted for publication in MNRAS letter
Galaxies in Clusters: the Observational Characteristics of Bow-Shocks, Wakes and Tails
The dynamical signatures of the interaction between galaxies in clusters and
the intracluster medium (ICM) can potentially yield significant information
about the structure and dynamical history of clusters. To develop our
understanding of this phenomenon we present results from numerical modelling of
the galaxy/ICM interaction, as the galaxy moves through the cluster. The
simulations have been performed for a broad range, of ICM temperatures (kT =
1,4 and 8 keV), representative of poor clusters or groups through to rich
clusters. There are several dynamical features that can be identified in these
simulations; for supersonic galaxy motion, a leading bow-shock is present, and
also a weak gravitationally focussed wake or tail behind the galaxy (analogous
to Bondi-Hoyle accretion). For galaxies with higher mass-replenishment rates
and a denser interstellar medium (ISM), the dominant feature is a dense
ram-pressure stripped tail. In line with other simulations, we find that the
ICM/galaxy ISM interaction can result in complex time- dependent dynamics, with
ram-pressure stripping occurring in an episodic manner. In order to facilitate
this comparison between the observational consequences of dynamical studies and
X-ray observations we have calculated synthetic X-ray flux and hardness maps
from these simulations. These calculations predict that the ram-pressure
stripped tail will usually be the most visible feature, though in nearby
galaxies the bow-shock preceding the galaxy should also be apparent in deeper
X-ray observations. We briefly discuss these results and compare with X-ray
observations of galaxies where there is evidence of such interactions.Comment: 14 pages, 8 diagrams, MNRAS (in press
First results of the XI Groups Project: Studying an unbiased sample of galaxy groups
X-ray observations of hot, intergalactic gas in galaxy groups provide a
useful means of characterizing the global properties of groups. However, X-ray
studies of large group samples have typically involved very shallow X-ray
exposures or have been based on rather heterogeneous samples. Here we present
the first results of the XI (XMM/IMACS) Groups Project, a study targeting, for
the first time, a redshift-selected, statistically unbiased sample of galaxy
groups using deep X-ray data. Combining this with radio observations of cold
gas and optical imaging and spectroscopy of the galaxy population, the project
aims to advance the understanding of how the properties and dynamics of group
galaxies relate to global group properties. Here, X-ray and optical data of the
first four galaxy groups observed as part of the project are presented. In two
of the groups we detect diffuse emission with a luminosity of L_X ~ 10^41
erg/s, among the lowest found for any X-ray detected group thus far, with a
comparable upper limit for the other two. Compared to typical X-ray selected
groups of similar velocity dispersion, these four systems are all surprisingly
X-ray faint. We discuss possible explanations for the lack of significant X-ray
emission in the groups, concluding that these systems are most likely
collapsing for the first time. Our results strongly suggest that, unlike our
current optically selected sample, previous X-ray selected group samples
represented a biased picture of the group population. This underlines the
necessity of a study of this kind, if one is to reach an unbiased census of the
properties of galaxy groups and the distribution of baryons in the Universe.Comment: 14 pages, 8 figures, accepted for publication in MNRA
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