2,686 research outputs found
Shock heating of the merging galaxy cluster A521
A521 is an interacting galaxy cluster located at z=0.247, hosting a low
frequency radio halo connected to an eastern radio relic. Previous Chandra
observations hinted at the presence of an X-ray brightness edge at the position
of the relic, which may be a shock front. We analyze a deep observation of A521
recently performed with XMM-Newton in order to probe the cluster structure up
to the outermost regions covered by the radio emission. The cluster atmosphere
exhibits various brightness and temperature anisotropies. In particular, two
cluster cores appear to be separated by two cold fronts. We find two shock
fronts, one that was suggested by Chandra and that is propagating to the east,
and another to the southwestern cluster outskirt. The two main interacting
clusters appear to be separated by a shock heated region, which exhibits a
spatial correlation with the radio halo. The outer edge of the radio relic
coincides spatially with a shock front, suggesting this shock is responsible
for the generation of cosmic ray electrons in the relic. The propagation
direction and Mach number of the shock front derived from the gas density jump,
M = 2.4 +/- 0.2, are consistent with expectations from the radio spectral
index, under the assumption of Fermi I acceleration mechanism
Comparing the temperatures of galaxy clusters from hydro-N-body simulations to Chandra and XMM-Newton observations
Theoretical studies of the physical processes guiding the formation and
evolution of galaxies and galaxy clusters in the X-ray are mainly based on the
results of numerical hydrodynamical N-body simulations, which in turn are often
directly compared to X-ray observations. Although trivial in principle, these
comparisons are not always simple. We demonstrate that the projected
spectroscopic temperature of thermally complex clusters obtained from X-ray
observations is always lower than the emission-weighed temperature, which is
widely used in the analysis of numerical simulations. We show that this
temperature bias is mainly related to the fact that the emission-weighted
temperature does not reflect the actual spectral properties of the observed
source. This has important implications for the study of thermal structures in
clusters, especially when strong temperature gradients, like shock fronts, are
present. Because of this bias, in real observations shock fronts appear much
weaker than what is predicted by emission-weighted temperature maps, and may
even not be detected. This may explain why, although numerical simulations
predict that shock fronts are a quite common feature in clusters of galaxies,
to date there are very few observations of objects in which they are clearly
seen. To fix this problem we propose a new formula, the spectroscopic-like
temperature function, and show that, for temperature larger than 3 keV, it
approximates the spectroscopic temperature better than few per cent, making
simulations more directly comparable to observations.Comment: Submitted for publication in MNRAS; 15 pages, 10 color figures and 13
BW figures,mn2e.cls. High resolution figures available here:
http://people.roma2.infn.it/~mazzotta/preprints/mazzotta.pd
Uniform Interpretation: Notice of Nonconformity
This Article is about uniform interpretation as it pertains to the nonconformity notices under CISG Article 39.1 Article 39, which is one of the most heavily-litigated provisions of the CISG, provides in relevant part:2 The buyer loses the right to rely on a lack of conformity of the goods if he does not give notice to the seller specifying the nature of the lack of conformity within a reasonable time after he has discovered it or ought to have discovered it.I will focus chiefly on two aspects of Article 39(1): (1) what constitutes a “reasonable time” within which buyers must notify sellers of a “lack of conformity” and (2) what level of specification is required to establish “the nature of the lack of conformity.
Is the Sunyaev-Zeldovich effect responsible for the observed steepening in the spectrum of the Coma radio halo ?
The spectrum of the radio halo in the Coma cluster is measured over almost
two decades in frequency. The current radio data show a steepening of the
spectrum at higher frequencies, which has implications for models of the radio
halo origin. There is an on-going debate on the possibility that the observed
steepening is not intrinsic to the emitted radiation, but is instead caused by
the SZ effect. Recently, the Planck satellite measured the SZ signal and its
spatial distribution in the Coma cluster allowing to test this hypothesis.
Using the Planck results, we calculated the modification of the radio halo
spectrum by the SZ effect in three different ways. With the first two methods
we measured the SZ-decrement within the aperture radii used for flux
measurements of the halo at the different frequencies. First we adopted the
global compilation of data from Thierbach et al. and a reference aperture
radius consistent with those used by the various authors. Second we used the
available brightness profiles of the halo at different frequencies to derive
the spectrum within two fixed apertures, and derived the SZ-decrement using
these apertures. As a third method we used the quasi-linear correlation between
the y and the radio-halo brightness at 330 MHz discovered by Planck to derive
the modification of the radio spectrum by the SZ-decrement in a way that is
almost independent of the adopted aperture radius. We found that the spectral
modification induced by the SZ-decrement is 4-5 times smaller than that
necessary to explain the observed steepening. Consequently a break or cut-off
in the spectrum of the emitting electrons is necessary to explain current data.
We also show that, if a steepening is absent from the emitted spectrum, future
deep observations at 5 GHz with single dishes are expected to measure a halo
flux in a 40 arcmin radius that would be 7-8 times higher than currently seen.Comment: 8 pages, 6 figures, accepted in Astronomy and Astrophysics (date of
acceptance 19/08/2013
One Actor, Multiple Roles: The Performances of Cryptochrome in Drosophila
Cryptochromes (CRYs) are flavoproteins that are sensitive to blue light, first identified in Arabidopsis and then in Drosophila and mice. They are evolutionarily conserved and play fundamental roles in the circadian clock of living organisms, enabling them to adapt to the daily 24-h cycles. The role of CRYs in circadian clocks differs among different species: in plants, they have a blue light-sensing activity whereas in mammals they act as light-independent transcriptional repressors within the circadian clock. These two different functions are accomplished by two principal types of CRYs, the light-sensitive plant/insect type 1 CRY and the mammalian type 2 CRY acting as a negative autoregulator in the molecular circadian clockwork. Drosophila melanogaster possesses just one CRY, belonging to type 1 CRYs. Nevertheless, this single CRY appears to have different functions, specific to different organs, tissues, and even subset of cells in which it is expressed. In this review, we will dissect the multiple roles of this single CRY in Drosophila, focusing on the regulatory mechanisms that make its pleiotropy possible
Antioxidant and Anti-Inflammatory Activities of Flavanones from Glycyrrhiza glabra L. (licorice) Leaf Phytocomplexes: Identification of Licoflavanone as a Modulator of NF-kB/MAPK Pathway
Inflammation represents an adaptive response generated by injuries or harmful stimuli. Natural remedies represent an interesting alternative to traditional therapies, involving several biochemical pathways. Besides, the valorization of agrochemical wastes nowadays seems to be a feasible way to reduce the health spending and improve the accessibility at bioactive natural compounds. In this context, the chemical composition of three Glycyrrhiza glabra L. (licorice) leaf extracts, obtained through maceration or ultrasound-assisted method (fresh and dried leaves) was investigated. A guided fractionation obtained three main components: pinocembrin, glabranin and licoflavanone. All the extracts showed similar antioxidant properties, evaluated by 2,2'-diphenyl-1-picrylhydrazyl (DPPH) or 2,2'-azino-bis(3-ethylbenzothiazoline-6-sulfonic acid) Diammonium Salt (ABTS) assay, while, among the isolated compounds, licoflavanone exhibited the best antioxidant activity. The anti-inflammatory activity of the extracts and the purified compounds was investigated in lipopolysaccharide (LPS)-stimulated RAW 264.7 murine macrophages. Extract C and licoflavanone showed a good anti-inflammatory activity without affecting cell viability, as they decreased nitrite levels even when used at 12.5 ÎĽg/mL (p < 0.005) and 50 ÎĽM concentration (p < 0.001), respectively. Interestingly, licoflavanone markedly decreased pro-inflammatory cytokines and cyclooxygenase 2/inducible nitric oxide synthase (COX-2/iNOS) expression levels (p < 0.001). A modulation of nuclear factor kappa B/mitogen-activated protein kinases (NF-kB/MAPK) pathway underlay such behavior, highlighting the potential of this natural compound as a new scaffold in anti-inflammatory drug research
Kinetic SZ effect and CMB polarization from subsonic bulk motions of dense gas clouds in galaxy cluster cores
Recent CHANDRA observations have revealed the presence of cold fronts in many
clusters of galaxies. The cold fronts are believed to be produced by the bulk
motions of massive, dense, cold gas clouds with respect to the hotter, more
rarefied ambient gas at velocities that can be as high as the speed of sound.
This phenomenon may produce a significant contamination of both the kinetic SZ
effect and the CMB polarization pattern observed in the direction of a cluster.
We estimate the contributions to the kinetic Sunyaev-Zel'dovich (SZ) effect and
to the CMB polarization toward galaxy clusters produced by the bulk motions of
the gas in the inner parts of galaxy clusters. The observed cold fronts probe
the absolute velocities of the gas motion while the induced polarization and
the kinetic SZ effect probe the transverse and the radial components,
respectively. We show that these signals may be easily detected with sensitive
future experiments, opening an exciting new window for studies of galaxy
cluster internal dynamics, and eventually facilitating reconstruction of the
intrinsic cluster polarization of the CMB and the associated measure of the
local CMB quadrupole.Comment: Accepted version. To be published in ApJ
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