260 research outputs found
Studying the WHIM Content of the Galaxy Large-Scale Structures along the Line of Sight to H 2356-309
We make use of a 500ks Chandra HRC-S/LETG spectrum of the blazar H2356-309,
combined with a lower S/N spectrum of the same target, to search for the
presence of warm-hot absorbing gas associated with two Large-Scale Structures
(LSSs) crossed by this sightline at z=0.062 (the Pisces-Cetus Supercluster,
PCS) and at z=0.128 ("Farther Sculptor Wall", FSW). No statistically
significant (>=3sigma) individual absorption is detected from any of the strong
He- or H-like transitions of C, O and Ne at the redshifts of the structures.
However we are still able to constrain the physical and geometrical parameters
of the associated putative absorbing gas, by performing joint spectral fit of
marginal detections and upper limits of the strongest expected lines with our
self-consistent hybrid ionization WHIM spectral model. At the redshift of the
PCS we identify a warm phase with logT=5.35_-0.13^+0.07 K and log N_H
=19.1+/-0.2 cm^-2 possibly coexisting with a hotter and less significant phase
with logT=6.9^+0.1_-0.8 K and log N_H=20.1^+0.3_-1.7 cm^-2 (1sigma errors). For
the FSW we estimate logT=6.6_-0.2^+0.1 K and log N_H=19.8_-0.8^+0.4 cm^-2. Our
constraints allow us to estimate the cumulative number density per unit
redshifts of OVII WHIM absorbers. We also estimate the cosmological mass
density obtaining Omega_b(WHIM)=(0.021^+0.031_-0.018) (Z/Z_sun)^-1, consistent
with the mass density of the intergalactic 'missing baryons' for high
metallicities.Comment: 29 pages, 8 figures, 4 tables. Accepted for publication in Ap
A changing inner radius in the accretion disc of Q0056-363?
Q0056-363 is the most powerful X-ray quasar known to exhibit a broad, likely
relativistic iron line (Porquet & Reeves 2003). It has been observed twice by
XMM-, three and half years apart (July 2000 and December 2003). In the
second observation, the UV and soft X-ray fluxes were fainter, the hard X-ray
power law flatter, and the iron line equivalent width (EW) smaller than in the
2000 observation. These variations can all be explained, at least
qualitatively, if the disc is truncated in the second observation. We report
also on the possible detection of a transient, redshifted iron absorption line
during the 2003 observation.Comment: Accepted for publication in A&
The Absence of Adiabatic Contraction of the Radial Dark Matter Profile in the Galaxy Cluster A2589
We present an X-ray analysis of the radial mass profile of the radio-quiet
galaxy cluster A2589 between 0.015-0.25 r_vir using an XMM-Newton observation.
Except for a ~16 kpc shift of the X-ray center of the R=45-60 kpc annulus,
A2589 possesses a remarkably symmetrical X-ray image and is therefore an
exceptional candidate for precision studies of its mass profile by applying
hydrostatic equilibrium. The total gravitating matter profile is well described
by the NFW model (fractional residuals <~10%) with c_vir=6.1 +/- 0.3 and M_vir
= 3.3 +/- 0.3 x 10^{14} M_sun (r_vir = 1.74 +/- 0.05 Mpc) in excellent
agreement with LCDM. When the mass of the hot ICM is subtracted from the
gravitating matter profile, the NFW model fitted to the resulting dark matter
(DM) profile produces essentially the same result. However, if a component
accounting for the stellar mass (M_*) of the cD galaxy is included, then the
NFW fit to the DM profile is substantially degraded in the central r ~50 kpc
for reasonable M_*/L_V. Modifying the NFW DM halo by adiabatic contraction
arising from the early condensation of stellar baryons in the cD galaxy further
degrades the fit. The fit is improved substantially with a Sersic-like model
recently suggested by high resolution N-body simulations but with an inverse
Sersic index, alpha ~0.5, a factor of ~3 higher than predicted. We argue that
neither random turbulent motions nor magnetic fields can provide sufficient
non-thermal pressure support to reconcile the XMM mass profile with adiabatic
contraction of a CDM halo assuming reasonable M_*/L_V. Our results support the
scenario where, at least for galaxy clusters, processes during halo formation
counteract adiabatic contraction so that the total gravitating mass in the core
approximately follows the NFW profile.Comment: 15 pages, 11 figures, accepted for publication in ApJ. Minor changes
to match published versio
Marcadores moleculares para el estudio de la variabilidad dentro del complejo Eragrostis curvula
211-220Weeping lovegrass is well adapted for forage production and useful for soil conservation in semiarid regions, constituting a morphologically diverse group. Diploid genotypes are unfrequent and reproduce sexually, whereas the tetraploids and plants of higher ploidy levels reproduce by apomixis. In the present work RAPD, AFLP and EST-SSR were used in order to assess the reproductive mode through progeny tests, to determine intracultivar homogeneity or seed purity, to establish genetic relationships among the cultivars within the complex and to characterize the new materials obtained by our group. Eight commercial cultivars and three new plant materials were analyzed. Uniform and variable patterns were observed in progenies of apomictic and sexual plants, respectively. Seed purity was evaluated in seed bulks, observing a certain degree of contamination with seeds from different sources. AFLP were the markers with the highest potential for cultivar identification. The clustering using SSR and AFLP was consistent with previous studies using isozymes and morphological traits. The new tetraploid materials developed by our own group should be included within the curvula type. We also proposed the creation of a new morphological type for the diploid, because it posses morphological characteristics of robusta and molecular profiles of the conferta type
On the importance of special relativistic effects in modelling ultra-fast outflows
Outflows are observed in a variety of astrophysical sources. Remarkably,
ultra-fast (), outflows in the UV and X-ray bands are often seen in
AGNs. Depending on their energy and mass outflow rate, respectively
, such outflows may play a key role in regulating
the AGN-host galaxy co-evolution process through cosmic time. It is therefore
crucial to provide accurate estimates of the wind properties. Here, we
concentrate on special relativistic effects concerning the interaction of light
with matter moving at relativistic speed relatively to the source of radiation.
Our aim is to assess the impact of these effects on the observed properties of
the outflows and implement a relativistic correction in the existing spectral
modelling routines. We define a simple procedure to incorporate relativistic
effects in radiative transfer codes. Following this procedure, we run a series
of simulations to explore the impact of these effects on the simulated spectra,
for different and column densities of the outflow. The observed optical
depth is usually considered a proxy for the wind , independently on its
velocity. However, our simulations show that the observed optical depth of an
outflow with a given column density decreases rapidly as the velocity of
the wind approaches relativistic values. This, in turn, implies that when
estimating from the optical depth, it is necessary to include a
velocity-dependent correction, already for moderate velocities (e.g. ). This correction linearly propagates to the derived . As an example of these effects, we calculate the
relativistically corrected values of and for a
sample of Ultra-Fast Outflows taken from the literature, and find
correction factors of within the observed range of outflowing
velocities.Comment: 6 pages, 5 figures. Accepted for publication in A&
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