1,321 research outputs found
Chandra and optical/IR observations of CXOJ1415.2+3610, a massive, newly discovered galaxy cluster at z~1.5
(Abridged) We report the discovery of CXO J1415.2+3610, a distant (z~1.5)
galaxy cluster serendipitously detected in a deep, high-resolution Chandra
observation targeted to study the cluster WARP J1415.1+3612 at z=1.03. This is
the highest-z cluster discovered with Chandra so far. Moreover, the total
exposure time of 280 ks with ACIS-S provides the deepest X-ray observation
currently achieved on a cluster at z>1.5. We perform an X-ray spectral fit of
the extended emission of the intracluster medium (ICM) with XSPEC, and we
detect at a 99.5% confidence level the rest frame 6.7-6.9 keV Iron K_\alpha
line complex, from which we obtain z_X=1.46\pm0.025. The analysis of the
z-3.6\mu m color-magnitude diagram shows a well defined sequence of red
galaxies within 1' from the cluster X-ray emission peak with a color range [5 <
z-3.6 \mu m < 6]. The photometric redshift obtained by spectral energy
distribution (SED) fitting is z_phot=1.47\pm 0.25. After fixing the redshift to
z=1.46, we perform the final spectral analysis and measure the average gas
temperature with a 20% error, kT=5.8^{+1.2}_{-1.0} keV, and the Fe abundance
Z_Fe = 1.3_{-0.5}^{+0.8}Z_\odot. We fit the background subtracted surface
brightness with a single beta--model out to 35" and derive the deprojected
electron density profile. The ICM mass is 1.09_{-0.2}^{+0.3}\times 10^{13}
M_\odot within 300 kpc. The total mass is M_{2500}= 8.6_{-1.7}^{+2.1} \times 10
^{13} M_\odot for R_{2500}=(220\pm 55) kpc. Extrapolating the profile at larger
radii we find M_{500}= 2.1_{-0.5}^{+0.7} \times 10 ^{14} M_\odot for R_{500} =
510_{-50}^{+55}$ kpc. This analysis establishes CXOJ1415.2+3610 as one of the
best characterized distant galaxy clusters based on X-ray data alone.Comment: 12 pages, 9 figures, A\&A in press, minor modifications in the tex
Ground-based monitoring of comet 67P/Churyumov-Gerasimenko gas activity throughout the <i>Rosetta</i> mission
Simultaneously to the ESA Rosetta mission, a world-wide ground-based campaign provided measurements of the large scale activity of comet 67P/Churyumov-Gerasimenko through measurement of optically active gas species and imaging of the overall dust coma. We present more than two years of observations performed with the FORS2 low resolution spectrograph at the VLT, TRAPPIST, and ACAM at the WHT. We focus on the evolution of the CN production, as a tracer of the comet activity. We find that it is asymmetric with respect to perihelion and different from that of the dust. The CN emission is detected for the first time at 1.34 au pre-perihelion and production rates then increase steeply to peak about two weeks after perihelion at (1.00±0.10) ×1025 molecules s−1, while the post-perihelion decrease is more shallow. The evolution of the comet activity is strongly influenced by seasonal effects, with enhanced CN production when the Southern hemisphere is illuminated
Radio Signatures of HI at High Redshift: Mapping the End of the ``Dark Ages''
The emission of 21-cm radiation from a neutral intergalactic medium (IGM) at
high redshift is discussed in connection with the thermal and ionization
history of the universe. The physical mechanisms that make such radiation
detectable against the cosmic microwave background include Ly_alpha coupling of
the hydrogen spin temperature to the kinetic temperature of the gas and
preheating of the IGM by the first generation of stars and quasars. Three
different signatures are investigated in detail: (a) the fluctuations in the
redshifted 21-cm emission induced by the gas density inhomogeneities that
develop at early times in cold dark matter (CDM) dominated cosmologies; (b) the
sharp absorption feature in the radio sky due to the rapid rise of the Ly_alpha
continuum background that marks the birth of the first UV sources in the
universe; and (c) the 21-cm emission and absorption shells that are generated
on several Mpc scales around the first bright quasars. Future radio
observations with projected facilities like the Giant Metrewave Radio Telescope
and the Square Kilometer Array may shed light on the power spectrum of density
fluctuations at z>5, and map the end of the "dark ages", i.e. the transition
from the post-recombination universe to one populated with radiation sources.Comment: LateX, 19 pages, 5 figures, significantly revised version to be
published in the Ap
Cobertura de testes unitários no SIGI.
Técnicas de teste. Ferramenta para cobertura de testes unitários. Diretrizes para utilização da Discover. Cobertura dos testes unitários do SIGI.bitstream/CNPTIA/9884/1/comuntec25.pdfAcesso em: 30 maio 2008
Case report - coronary vasospasm in transplanted heart: a puzzling phenomenon.
Coronary artery spasm (CAS) is an underdiagnosed disease especially in heart transplant patients, and in those patients the etiology and pathophysiology remain largely unknown, although it has been associated with cardiac allograft vasculopathy or graft rejection.
We report the case of a heart-transplant patient whose cardiac graft experienced two coronary vasospasms: the first before transplantation, and the other at one-month of a postoperative course complicated by primary graft failure.
Our case illustrates that a transplanted heart predisposed with coronary vasospasm may suffer from early relapse in the recipient despite of complete post-surgical autonomic denervation. Exacerbated endothelial dysfunction of the donor heart after transplant, with the addition of systemic factors in the recipient may be involved in the genesis of this puzzling phenomenon
Revisão taxonômica das espécies de Mimosa ser. Leiocarpae sensu lato (Leguminosae - Mimosoideae).
Hubble Space Telescope Imaging in the Chandra Deep Field South: III. Quantitative Morphology of the 1Ms Chandra Counterparts and Comparison with the Field Population
We present quantitative morphological analyses of 37 HST/WFPC2 counterparts
of X-ray sources in the 1 Ms Chandra Deep Field-South (CDFS). We investigate:
1) 1-D surface brightness profiles via isophotal ellipse fitting; 2) 2-D, PSF-
convolved, bulge+disk+nucleus profile-fitting; 3) asymmetry and concentration
indices compared with all ~3000 sources in our three WFPC2 fields; and 4) near-
neighbor analyses comparing local environments of X-ray sources versus the
field control sample. Significant nuclear point-source optical components
appear in roughly half of the resolved HST/WFPC2 counterparts, showing a narrow
range of F_X/F_{opt,nuc} consistent with the several HST-unresolved X-ray
sources (putative type-1 AGN) in our fields. We infer roughly half of the
HST/WFPC2 counterparts host unobscured AGN, which suggests no steep decline in
the type-1/type-2 ratio out to the redshifts z~0.5-1 typical of our sources.
The concentration indices of the CDFS counterparts are clearly larger on
average than those of the field distribution, at 5-sigma, suggesting that the
strong correlation between central black hole mass and host galaxy properties
(including concentration index) observed in nearby galaxies is already evident
by z~0.5-1. By contrast, the asymmetry index distribution of the 21 resolved
CDFS sources at I<23 is indistinguishable from the I<23 field. Moreover, the
frequency of I<23 near neighbors around the CDFS counterparts is not
significantly different from the field sample. These results, combined with
previous similar findings for local samples, suggest that recent merger/
interaction history is not a good indicator of AGN activity over a substantial
range of look-back time.Comment: 30 pages, incl. 8 figures; accepted for publication in the
Astrophysical Journa
A Puzzling X-Ray Source Found in the chandra Deep Field South
In this letter we report the detection of an extremely strong X-ray emission
line in the 940ks chandra ACIS-I spectrum of CXO CDFS J033225.3-274219. The
source was identified as a Type1 AGN at redshift of z = 1.617, with 2.0 -- 10.0
keV rest frame X-ray luminosity of ~ 10^44 ergs s^-1. The emission line was
detected at 6.2^{+0.2}_{-0.1} keV, with an equivalent width (EW) of
4.4^{+3.2}_{-1.4} keV, both quantities referring to the observed frame. In the
rest frame, the line is at 16.2^{+0.4}_{-0.3} keV with an EW of
11.5^{+8.3}_{-3.7} keV. An X-ray emission line at similar energy (~ 17 keV,
rest frame) in QSO PKS 2149-306 was discovered before using ASCA data. We
reject the possibility that the line is due to a statistical or instrumental
artifact. The line is most likely due to blueshifted Fe-K emission from an
relativistic outflow, probably an inner X-ray jet, with velocities of the order
of ~ 0.6-0.7c. Other possible explanations are also discussed
Mentalization-based treatment in clinical high risk for psychosis: A rationale and clinical illustration
Developmental clinical research in recent years has highlighted the value treating psychotic disorders at the earliest stage to reduce long-term morbidity. It is now suggested that treatment during the clinical high risk states (CHR), preceding by 1 to 4 years the onset of psychotic disorders, may delay or prevent the onset of psychosis, and contribute to a more positive prognosis. In this article, we wish to provide a rationale and clinical illustration of mentalization-based treatment (MBT) as an indicated preventive treatment for CHR. We will first review the notion of high-risk for psychosis, providing a trans-theoretical developmental framework for conceptualizing the clinical progression from sub-clinical towards clinical psychotic states. Second, we address the commonalities and differences between the constructs of mentalization and metacognition, and discuss their relevance in preventive psychotherapeutic treatment for CHR. Thirdly, we provide a clinical illustration of MBT to emerging psychosis. Finally, we conclude by discussing the specific contributions of MBT approach in youths at CHR, and the necessary research for evaluating its relevance in the context of risk for developing psychosis
Simulating the WFXT sky
We investigate the scientific impact of the Wide Field X-ray Telescope
mission. We present simulated images and spectra of X-ray sources as observed
from the three surveys planned for the nominal 5-year WFXT lifetime. The goal
of these simulations is to provide WFXT images of the extragalactic sky in
different energy bands based on accurate description of AGN populations, normal
and star forming galaxies, groups and clusters of galaxies. The images are
realized using a detailed PSF model, instrumental and physical
backgrounds/foregrounds, accurate model of the effective area and the related
vignetting effect. Thanks to this comprehensive modelization of the WFXT
properties, the simulated images can be used to evaluate the flux limits for
detection of point and extended sources, the effect of source confusion at very
faint fluxes, and in general the efficiency of detection algorithms. We also
simulate the spectra of the detected sources, in order to address specific
science topics which are unique to WFXT. Among them, we focus on the
characterization of the Intra Cluster Medium (ICM) of high-z clusters, and in
particular on the measurement of the redshift from the ICM spectrum in order to
build a cosmological sample of galaxy clusters. The end-to-end simulation
procedure presented here, is a valuable tool in optimizing the mission design.
Therefore, these simulations can be used to reliably characterize the WFXT
discovery space and to verify the connection between mission requirements and
scientific goals. Thanks to this effort, we can conclude on firm basis that an
X-ray mission optimized for surveys like WFXT is necessary to bring X-ray
astronomy at the level of the optical, IR, submm and radio wavebands as
foreseen in the coming decade.Comment: "Proceedings of "The Wide Field X-ray Telescope Workshop", held in
Bologna, Italy, Nov. 25-26 2009. To appear in Memorie della Societa
Astronomica Italiana 2010 (arXiv:1010.5889)
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