3,877 research outputs found
Radio emission at the centre of the galaxy cluster Abell 3560: evidence for core sloshing?
Previous radio observations of the galaxy cluster A3560 in the Shapley
Concentration showed complex radio emission associated with the brightest
cluster member.To understand its origin we observed it with the GMRT, the VLA
and ATCA at 240 and 610 MHz, 1.28,1.4, 2.3,4.8 and 8.4 GHz, and performed a
detailed morphological and spectral study of the radio emission associated with
the BCG. We also observed the cluster with XMM-Newton and Chandra to derive the
properties of the ICM. The radio emission of the N-E nucleus of the dumb-bell
BCG shows an active radio galaxy, plus aged diffuse emission, which is not
refurbished at present. Our Chandra data show that the radio active nucleus of
the BCG has extended X-ray emission, which we classify as a low-luminosity
corona. A residual image of the XMM-Newton brightness shows the presence of a
spiral-like feature, which we interpret as the signature of gas sloshing. The
presence of a subgroup is clear in the surface brightness residual map, and in
the XMM-Newton temperature analysis. The optical 2D analysis shows substructure
in A3560. A galaxy clump was found at the location of the X-ray subgroup, and
another group is present south of the cluster core, close to the spiral-like
feature. The aged part of the radio emission closely follows the spiral pattern
of the X-ray residual brightness distribution, while the two active radio lobes
are bent in a completely different direction. We conclude that the complex
radio emission associated with the cluster BCG is the result of a minor merger
event in A3560. The aged diffuse emission is strongly affected by the sloshing
motion in the ICM. On the other hand, the bent jets and lobes of the current
radio AGN activity may reflect a complex gas velocity field in the innermost
cluster regions and/or sloshing-induced oscillations in the motion of the cD
galaxy.Comment: 15 pages, 8 figures, 5 tables, A&A in pres
Estrutura de uma unidade organizacional de pesquisa agropecuária: proposta de um modelo conceitual.
The stripping of a galaxy group diving into the massive cluster A2142
Structure formation in the current Universe operates through the accretion of
group-scale systems onto massive clusters. The detection and study of such
accreting systems is crucial to understand the build-up of the most massive
virialized structures we see today. We report the discovery with XMM-Newton of
an irregular X-ray substructure in the outskirts of the massive galaxy cluster
Abell 2142. The tip of the X-ray emission coincides with a concentration of
galaxies. The bulk of the X-ray emission of this substructure appears to be
lagging behind the galaxies and extends over a projected scale of at least 800
kpc. The temperature of the gas in this region is 1.4 keV, which is a factor of
~4 lower than the surrounding medium and is typical of the virialized plasma of
a galaxy group with a mass of a few 10^13M_sun. For this reason, we interpret
this structure as a galaxy group in the process of being accreted onto the main
dark-matter halo. The X-ray structure trailing behind the group is due to gas
stripped from its original dark-matter halo as it moves through the
intracluster medium (ICM). This is the longest X-ray trail reported to date.
For an infall velocity of ~1,200 km s-1 we estimate that the stripped gas has
been surviving in the presence of the hot ICM for at least 600 Myr, which
exceeds the Spitzer conduction timescale in the medium by a factor of >~400.
Such a strong suppression of conductivity is likely related to a tangled
magnetic field with small coherence length and to plasma microinstabilities.
The long survival time of the low-entropy intragroup medium suggests that the
infalling material can eventually settle within the core of the main cluster.Comment: 11 pages, 7 figures, accepted for publication in A&
The two-component giant radio halo in the galaxy cluster Abell 2142
We report on a spectral study at radio frequencies of the giant radio halo in
A2142 (z=0.0909), which we performed to explore its nature and origin. A2142 is
not a major merger and the presence of a giant radio halo is somewhat
surprising. We performed deep radio observations with the GMRT at 608 MHz, 322
MHz, and 234 MHz and with the VLA in the 1-2 GHz band. We obtained high-quality
images at all frequencies in a wide range of resolutions. The radio halo is
well detected at all frequencies and extends out to the most distant cold front
in A2142. We studied the spectral index in two regions: the central part of the
halo and a second region in the direction of the most distant south-eastern
cold front, selected to follow the bright part of the halo and X-ray emission.
We complemented our observations with a preliminary LOFAR image at 118 MHz and
with the re-analysis of archival VLA data at 1.4 GHz. The two components of the
radio halo show different observational properties. The central brightest part
has higher surface brightess and a spectrum whose steepness is similar to those
of the known radio halos, i.e. . The ridge, which fades into the larger scale emission, is broader in
size and has considerably lower surface brightess and a moderately steeper
spectrum, i.e. . We propose that
the brightest part of the radio halo is powered by the central sloshing in
A2142, similar to what has been suggested for mini-halos, or by secondary
electrons generated by hadronic collisions in the ICM. On the other hand, the
steeper ridge may probe particle re-acceleration by turbulence generated either
by stirring the gas and magnetic fields on a larger scale or by less energetic
mechanisms, such as continuous infall of galaxy groups or an off-axis merger.Comment: 18 pages, 10 figures, 4 tables - A&A, accepte
Deep Chandra observations of the stripped galaxy group falling into Abell 2142
In the local Universe, the growth of massive galaxy clusters mainly operates
through the continuous accretion of group-scale systems. The infalling group in
Abell 2142 is the poster child of such an accreting group, and as such, it is
an ideal target to study the astrophysical processes induced by structure
formation. We present the results of a deep (200 ks) observation of this
structure with Chandra, which highlights the complexity of this system in
exquisite detail. In the core of the group, the spatial resolution of Chandra
reveals the presence of a leading edge and a complex AGN-induced activity. The
morphology of the stripped gas tail appears straight in the innermost 250 kpc,
suggesting that magnetic draping efficiently shields the gas from its
surroundings. However, beyond kpc from the core, the tail flares and
the morphology becomes strongly irregular, which could be explained by a
breaking of the drape, e.g. because of turbulent motions. The power spectrum of
surface-brightness fluctuations is relatively flat (),
which indicates that thermal conduction is strongly inhibited even beyond the
region where magnetic draping is effective. The amplitude of density
fluctuations in the tail is consistent with a mild level of turbulence with a
Mach number . Overall, our results show that the processes
leading to the thermalization and mixing of the infalling gas are slow and
relatively inefficient.Comment: Accepted for publication in A&
Novel RNA-binding properties of the MTG chromatin regulatory proteins
Background: The myeloid translocation gene (MTG) proteins are non-DNA-binding transcriptional regulators capable of interacting with chromatin modifying proteins. As a consequence of leukemia-associated chromosomal translocations, two of the MTG proteins, MTG8 and MTG16, are fused to the DNA-binding domain of AML1, a transcriptional activator crucial for hematopoiesis. The AML1-MTG fusion proteins, as the wild type MTGs, display four conserved homology regions (NHR1-4) related to the Drosophila nervy protein. Structural protein analyses led us to test the hypothesis that specific MTG domains may mediate RNA binding. Results: By using an RNA-binding assay based on synthetic RNA homopolymers and a panel of MTG deletion mutants, here we show that all the MTG proteins can bind RNA. The RNA-binding properties can be traced to two regions: the Zinc finger domains in the NHR4, which mediate Zinc-dependent RNA binding, and a novel short basic region (SBR) upstream of the NHR2, which mediates Zinc-independent RNA binding. The two AML1-MTG fusion proteins, retaining both the Zinc fingers domains and the SBR, also display RNA-binding properties. Conclusion: Evidence has been accumulating that RNA plays a role in transcriptional control. Both wild type MTGs and chimeric AML1-MTG proteins display in vitro RNA-binding properties, thus opening new perspectives on the possible involvement of an RNA component in MTG-mediated chromatin regulation
Clinical evolution after a non-reactive hypothermic EEG following cardiac arrest.
BACKGROUND: Lack of electroencephalography (EEG) background reactivity during therapeutic hypothermia (TH) has been associated with poor outcome in post-anoxic comatose patients. However, decision on intensive care withdrawal is based on normothermic (NT) evaluations. This study aims at exploring whether patients showing recovery of EEG reactivity in NT after a non-reactive EEG in TH differ from those remaining non-reactive.
METHODS: Patients with non-reactive EEG during TH were identified from our prospective registry of consecutive comatose adults admitted after successful resuscitation from CA between April 2009 and June 2014. Variables including neurological examination, serum neuron-specific enolase (NSE), procalcitonin, and EEG features were compared regarding impact on functional outcome at 3 months.
RESULTS: Seventy-two of 197 patients (37 %) had a non-reactive EEG background during TH with thirteen (18 %) evolving towards reactivity in NT. Compared to those remaining non-reactive (n = 59), they showed significantly better recovery of brainstem reflexes (p < 0.001), better motor responses (p < 0.001), transitory consciousness improvement (p = 0.008), and a tendency toward lower NSE (p = 0.067). One patient recovering EEG reactivity survived with good functional outcome at 3 months.
CONCLUSIONS: Recovery of EEG reactivity from TH to NT seems to distinguish two patients' subgroups regarding early neurological assessment and transitory consciousness improvement, corroborating the role of EEG in providing information about cerebral functions. Understanding these dynamic changes encourages maintenance of intensive support in selected patients even after a non-reactive EEG background in TH, as a small subgroup may indeed recover with good functional outcome
Programming DNA-Based Systems through Effective Molarity Enforced by Biomolecular Confinement
The fundamental concept of effective molarity is observed in a variety of biological processes, such as protein compartmentalization within organelles, membrane localization and signaling paths. To control molecular encountering and promote effective interactions, nature places biomolecules in specific sites inside the cell in order to generate a high, localized concentration different from the bulk concentration. Inspired by this mechanism, scientists have artificially recreated in the lab the same strategy to actuate and control artificial DNA-based functional systems. Here, it is discussed how harnessing effective molarity has led to the development of a number of proximity-induced strategies, with applications ranging from DNA-templated organic chemistry and catalysis, to biosensing and protein-supported DNA assembly
South-West extension of the hard X-ray emission from the Coma cluster
We explore the morphology of hard (18-30 keV) X-ray emission from the Coma
cluster of galaxies. We analyze a deep (1.1 Ms) observation of the Coma cluster
with the ISGRI imager on board the \emph{INTEGRAL} satellite. We show that the
source extension in the North-East to South-West (SW) direction ()
significantly exceeds the size of the point spread function of ISGRI, and that
the centroid of the image of the source in the 18-30 keV band is displaced in
the SW direction compared to the centroid in the 1-10 keV band. To test the
nature of the SW extension we fit the data assuming different models of source
morphology. The best fit is achieved with a diffuse source of elliptical shape,
although an acceptable fit can be achieved assuming an additional point source
SW of the cluster core. In the case of an elliptical source, the direction of
extension of the source coincides with the direction toward the subcluster
falling onto the Coma cluster. If the SW excess is due to the presence of a
point source with a hard spectrum, we show that there is no obvious X-ray
counterpart for this additional source, and that the closest X-ray source is
the quasar EXO 1256+281, which is located from the centroid of the
excess. The observed morphology of the hard X-ray emission clarifies the nature
of the hard X-ray "excess" emission from the Coma cluster, which is due to the
presence of an extended hard X-ray source SW of the cluster core.Comment: 7pages, 10 figure
Recent extension driven by mantle upwelling beneath the Admiralty Mountains (East Antarctica)
Northern Victoria Land is located at the boundary
between an extended, presumably hot, region (West
Antarctic Rift System) and the thick, possibly cold,
East Antarctic craton. The style and timing of Tertiary
deformation along with relationships with the
magmatic activity are still unclear, and contrasting
models have been proposed. We performed structural
and morphotectonic analyses at the NE termination of
northern Victoria Land in the Admiralty Mountains
area, where the relationship between topography,
tectonics, and magmatism is expected to be well
pronounced. We found evidence of two subsequent
episodes of faulting, occurring concurrently with the
Neogene McMurdo volcanism. The first episode is
associated with dextral transtension, and it is
overprinted by extensional tectonics during the
emplacement of large shield alkaline volcanoes.
Upper mantle seismic tomography shows that the
extensional regime is limited to regions overlying a
low-velocity anomaly. We interpret this anomaly to be
of thermal origin, and have tested the role of largescale
upwelling on lithosphere deformation in the area.
The results of this integrated analysis suggest that the
morphotectonic setting of the region and the
magmatism is likely the result of upwelling flow at
the boundary between the cold cratonic and the hot
stretched province (WARS), at work until recent time
in this portion of the northern Victoria Land
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