132 research outputs found
The photoheating of the intergalactic medium in synthesis models of the UV background
We compare cosmological hydrodynamical simulations combined with the
homogeneous metagalactic UV background (UVB) of Haardt & Madau (2012) (HM2012)
to observations of the Lyman-alpha forest that are sensitive to the thermal and
ionization state of the intergalactic medium (IGM). The transition from
optically thick to thin photoheating predicted by the simple one-zone,
radiative transfer model implemented by HM2012 predicts a thermal history that
is in remarkably good agreement with the observed rise of the IGM temperature
at z~3 if we account for the expected evolution of the volume filling factor of
HeIII. Our simulations indicate that there may be, however, some tension
between the observed peak in the temperature evolution and the rather slow
evolution of the HeII opacities suggested by recent Hubble Space Telescope/COS
measurements. The HM2012 UVB also underpredicts the metagalactic hydrogen
photoionization rate required by our simulations to match the observed opacity
of the forest at z>4 and z<2
Diagnosing galactic feedback with line broadening in the low redshift Lyα forest
We compare the low-redshift (z 0.1) Lyα forest from hydrodynamical simulations with data from the Cosmic Origins Spectrograph. We find the tension between the observed number of lines with b-parameters in the range of 25â45 km sâ1 and the predictions from simulations that incorporate either vigorous feedback from active galactic nuclei or that exclude feedback altogether. The gas in these simulations is, respectively, either too hot to contribute to the Lyα absorption or too cold to produce the required linewidths. Matching the observed b parameter distribution therefore requires feedback processes that thermally or turbulently broaden the absorption features without collisionally (over)ionizing hydrogen. This suggests that the Lyα forest b-parameter distribution is a valuable diagnostic of galactic feedback in the low-redshift Universe. We furthermore confirm that the low-redshift Lyα forest column density distribution is better reproduced by an ultraviolet background with the H I photoionization rate a factor of 1.5â3 higher than predicted by Haardt and Madau
Bispectrum of the Sunyaev-Zel'dovich Effect
We perform a detailed study of the bispectrum of the Sunyaev-Zel'dovich
effect. Using an analytical model for the pressure profiles of the intracluster
medium, we demonstrate the SZ bispectrum to be a sensitive probe of the
amplitude of the matter power spectrum parameter sigma_8. We find that the
bispectrum amplitude scales as B_SZ ~ sigma_8^{11-12}, compared to that of the
power spectrum, which scales as A_tSZ ~ sigma_8^{7-9}. We show that the SZ
bispectrum is principally sourced by massive clusters at redshifts around
z~0.4, which have been well-studied observationally. This is in contrast to the
SZ power spectrum, which receives a significant contribution from less-well
understood low-mass and high-redshift groups and clusters. Therefore, the
amplitude of the bispectrum at l~3000 is less sensitive to astrophysical
uncertainties than the SZ power spectrum. We show that current high resolution
CMB experiments should be able to detect the SZ bispectrum amplitude with high
significance, in part due to the low contamination from extra-galactic
foregrounds. A combination of the SZ bispectrum and the power spectrum can
sharpen the measurements of thermal and kinetic SZ components and help
distinguish cosmological and astrophysical information from high-resolution CMB
maps.Comment: 12 pages, 8 figures, published in The Astrophysical Journa
Measurement of the intracluster light at z ~ 1
A significant fraction of the total photospheric light in nearby galaxy
clusters is thought to be contained within the diffuse intracluster light
(ICL), which extends 100s of kpc from cluster cores. The study of the ICL can
reveal details of the evolutionary histories and processes occurring within
galaxy clusters, however since it has a very low surface brightness it is often
difficult to detect. We present here the first measurements of the ICL as a
fraction of total cluster light at z \sim 1 using deep J-band (1.2 {\mu}m)
imaging from HAWK-I on the VLT. We investigate the ICL in 6 X-ray selected
galaxy clusters at 0.8< z <1.2 and find that the ICL below isophotes {\mu}(J) =
22 mag/arcsec2 constitutes 1-4% of the total cluster light within a radius
R500. This is broadly consistent with simulations of the ICL at a similar
redshift and when compared to nearby observations suggests that the fraction of
the total cluster light that is in the ICL has increased by a factor 2 - 4
since z\sim1. We also find the fraction of the total cluster light contained
within the Brightest Cluster Galaxy (BCG) to be 2.0-6.3% at these redshifts,
which in 5 out of 6 cases is larger than the fraction of the ICL component, in
contrast to results from nearby clusters. This suggests that the evolution in
cluster cores involves substantial stripping activity at late times, in
addition to the early build up of the BCG stellar mass through merging. The
presence of significant amounts of stellar light at large radii from these BCGs
may help towards solving the recent disagreement between the semi-analytic
model predictions of BCG mass growth (e.g. De Lucia & Blaziot, 2007) and the
observed large masses and scale sizes reported for BCGs at high redshift.Comment: 12 pages, 12 figures. Accepted for publication in MNRA
Non-parametric modeling of the intra-cluster gas using APEX-SZ bolometer imaging data
We demonstrate the usability of mm-wavelength imaging data obtained from the
APEX-SZ bolometer array to derive the radial temperature profile of the hot
intra-cluster gas out to radius r_500 and beyond. The goal is to study the
physical properties of the intra-cluster gas by using a non-parametric
de-projection method that is, aside from the assumption of spherical symmetry,
free from modeling bias. We use publicly available X-ray imaging data from the
XMM-Newton observatory and our Sunyaev-Zel'dovich Effect (SZE) imaging data
from the APEX-SZ experiment at 150 GHz to de-project the density and
temperature profiles for the relaxed cluster Abell 2204. We derive the gas
density, temperature and entropy profiles assuming spherical symmetry, and
obtain the total mass profile under the assumption of hydrostatic equilibrium.
For comparison with X-ray spectroscopic temperature models, a re-analysis of
the recent Chandra observation is done with the latest calibration updates.
Using the non-parametric modeling we demonstrate a decrease of gas temperature
in the cluster outskirts, and also measure the gas entropy profile. These
results are obtained for the first time independently of X-ray spectroscopy,
using SZE and X-ray imaging data. The contribution of the SZE systematic
uncertainties in measuring T_e at large radii is shown to be small compared to
the Chandra systematic spectroscopic errors. The upper limit on M_200 derived
from the non-parametric method is consistent with the NFW model prediction from
weak lensing analysis.Comment: Replaced with the published version; A&A 519, A29 (2010
A relationship between AGN jet power and radio power
Using Chandra X-ray and VLA radio data, we investigate the scaling
relationship between jet power, P_jet, and synchrotron luminosity, P_rad. We
expand the sample presented in Birzan et al. (2008) to lower radio power by
incorporating measurements for 21 gEs to determine if the Birzan et al. (2008)
P_jet-P_rad scaling relations are continuous in form and scatter from giant
elliptical galaxies (gEs) up to brightest cluster galaxies (BCGs). We find a
mean scaling relation of P_jet approximately 5.8x10^43 (P_rad/10^40)^(0.70)
erg/s which is continuous over ~6-8 decades in P_jet and P_rad with a scatter
of approximately 0.7 dex. Our mean scaling relationship is consistent with the
model presented in Willott et al. (1999) if the typical fraction of lobe energy
in non-radiating particles to that in relativistic electrons is > 100. We
identify several gEs whose radio luminosities are unusually large for their jet
powers and have radio sources which extend well beyond the densest parts of
their X-ray halos. We suggest that these radio sources are unusually luminous
because they were unable to entrain appreciable amounts of gas.Comment: Accepted for publication in the Astrophysical Journal; 8 pages, 3
color figures, 1 tabl
Combining Semi-analytic Models with Simulations of Galaxy Clusters: the Need for Heating from Active Galactic Nuclei
We present hydrodynamical N-body simulations of clusters of galaxies with
feedback taken from semi-analytic models of galaxy formation. The advantage of
this technique is that the source of feedback in our simulations is a
population of galaxies that closely resembles that found in the real universe.
We demonstrate that, to achieve the high entropy levels found in clusters,
active galactic nuclei must inject a large fraction of their energy into the
intergalactic/intracluster media throughout the growth period of the central
black hole. These simulations reinforce the argument of Bower et al., who
arrived at the same conclusion on the basis of purely semi-analytic reasoning.Comment: 25 pages and 10 colour figures. Accepted by Ap
Exploring the Energetics of Intracluster Gas with a Simple and Accurate Model
The state of the hot gas in clusters of galaxies is investigated with a set
of model clusters, created by assuming a polytropic equation of state
(Gamma=1.2) and hydrostatic equilibrium inside gravitational potential wells
drawn from a dark matter simulation. Star formation, energy input, and
nonthermal pressure support are included. To match the gas fractions seen in
non-radiative hydrodynamical simulations, roughly 5% of the binding energy of
the dark matter must be transferred to the gas during cluster formation; the
presence of nonthermal pressure support increases this value. In order to match
X-ray observations, scale-free behavior must be broken. This can be due to
either variation of the efficiency of star formation with cluster mass M_500,
or the input of additional energy proportional to the formed stellar mass M_F.
These two processes have similar effects on X-ray scalings. If 9% of the gas is
converted into stars, independent of cluster mass, then feedback energy input
of 1.2e-5*M_Fc^2 (or ~1.0 keV per particle) is required to match observed
clusters. Alternatively, if the stellar mass fraction varies as M_500^-0.26
then a lower feedback of 4e-6*M_Fc^2 is needed, and if the stellar fraction
varies as steeply as M_500^-0.49 then no additional feedback is necessary. The
model clusters reproduce the observed trends of gas temperature and gas mass
fraction with cluster mass, as well as observed entropy and pressure profiles;
thus they provide a calibrated basis with which to interpret upcoming SZ
surveys. One consequence of the increased gas energy is that the baryon
fraction inside the virial radius is less than roughly 90% of the cosmic mean,
even for the most massive clusters.Comment: Accepted by ApJ; 28 pages, 12 figure
Probing the thermal state of the intergalactic medium at z > 5 with the transmission spikes in high-resolution Ly α forest spectra
We compare a sample of five high-resolution, high S/N Ly forest
spectra of bright QSOs aimed at spectrally resolving the
last remaining transmission spikes at with those obtained from mock
absorption spectra from the Sherwood and Sherwood-Relics suites of
hydrodynamical simulations of the intergalactic medium (IGM). We use a profile
fitting procedure for the inverted transmitted flux, , similar to the
widely used Voigt profile fitting of the transmitted flux at lower
redshifts, to characterise the transmission spikes that probe predominately
underdense regions of the IGM. We are able to reproduce the width and height
distributions of the transmission spikes, both with optically thin simulations
of the post-reionization Universe using a homogeneous UV background and full
radiative transfer simulations of a late reionization model. We find that the
width of the fitted components of the simulated transmission spikes is very
sensitive to the instantaneous temperature of the reionized IGM. The internal
structures of the spikes are more prominant in low temeperature models of the
IGM. The width distribution of the observed transmission spikes, which require
high spectral resolution ( 8 km/s) to be resolved, is reproduced for
optically thin simulations with a temperature at mean density of K at . This is weakly
dependent on the slope of the temperature-density relation, which is favoured
to be moderately steeper than isothermal. In the inhomogeneous, late
reionization, full radiative transfer simulations where islands of neutral
hydrogen persist to , the width distribution of the observed
transmission spikes is consistent with the range of caused by spatial
fluctuations in the temperature-density relation
The soft supersymmetry breaking in D=5 supergravity compactified on S_1/Z_2 orbifolds
We study the origin of the supersymmetry breaking induced by the mediation of
gravity and the radion multiplet from the hidden to the visible brane in the
context of the N=2, D=5 supergravity compactified on S_1/Z_2 orbifolds. The
soft supersymmetry breaking terms for scalar masses, trilinear scalar couplings
and gaugino masses are calculated to leading order in the five dimensional
Newton's constant k_5^2 and the gravitino mass m_{3/2}. These are finite and
non-vanishing, with the scalar soft masses be non-tachyonic, and are all
expressed in terms of the gravitino mass and the length scale R of the fifth
dimension. The soft supersymmetry breaking parameters are thus correlated and
the phenomenological implications are discussed.Comment: 16 pages, 3 figures, 1 Table, final version to appear in Physics
Letters B, slightly shortened, comments added, typos correcte
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