1,433 research outputs found
On the signature of superclusters and voids in the Integrated Sachs-Wolfe effect
Through a large ensemble of Gaussian realisations and a suite of large-volume
N-body simulations, we show that in a standard LCDM scenario, supervoids and
superclusters in the redshift range should leave a {\em small}
signature on the ISW effect of the order K. We perform aperture
photometry on WMAP data, centred on such superstructures identified from SDSS
LRGs, and find amplitudes at the level of 8 -- 11K -- thus confirming the
earlier work of Granett et al 2008. If we focus on apertures of the size
\sim3.6\degr, then our realisations indicate that LCDM is discrepant at the
level of . If we combine all aperture scales considered, ranging
from 1\degr--20\degr, then the discrepancy becomes , and it
further lowers to if only 30 superstructures are considered
in the analysis (being compatible with no ISW signatures at in this
case). Full-sky ISW maps generated from our N-body simulations show that this
discrepancy cannot be alleviated by appealing to Rees-Sciama mechanisms, since
their impact on the scales probed by our filters is negligible. We perform a
series of tests on the WMAP data for systematics. We check for foreground
contaminants and show that the signal does not display the correct dependence
on the aperture size expected for a residual foreground tracing the density
field. The signal also proves robust against rotation tests of the CMB maps,
and seems to be spatially associated to the angular positions of the supervoids
and superclusters. We explore whether the signal can be explained by the
presence of primordial non-Gaussianities of the local type. We show that for
models with \FNL=\pm100, whilst there is a change in the pattern of
temperature anisotropies, all amplitude shifts are well below K.Comment: 14 pages, 9 figures, matches accepted version in MNRA
A linear filter to reconstruct the ISW effect from CMB and LSS observations
The extraction of a signal from some observational data sets that contain
different contaminant emissions, often at a greater level than the signal
itself, is a common problem in Astrophysics and Cosmology. The signal can be
recovered, for instance, using a simple Wiener filter. However, in certain
cases, additional information may also be available, such as a second
observation which correlates to a certain level with the sought signal. In
order to improve the quality of the reconstruction, it would be useful to
include as well this additional information. Under these circumstances, we have
constructed a linear filter, the linear covariance-based filter, that extracts
the signal from the data but takes also into account the correlation with the
second observation. To illustrate the performance of the method, we present a
simple application to reconstruct the so-called Integrated Sachs-Wolfe effect
from simulated observations of the Cosmic Microwave Background and of
catalogues of galaxies.Comment: 8 pages, 6 figures, accepted for publication in the IEEE Journal of
Selected Topics in Signal Processin
The origin of the LMC stellar bar: clues from the SFH of the bar and inner disk
We discuss the origin of the LMC stellar bar by comparing the star formation
histories (SFH) obtained from deep color-magnitude diagrams (CMDs) in the bar
and in a number of fields in different directions within the inner disk. The
CMDs, reaching the oldest main sequence turnoffs in these very crowded fields,
have been obtained with VIMOS on the VLT in service mode, under very good
seeing conditions. We show that the SFHs of all fields share the same patterns,
with consistent variations of the star formation rate as a function of time in
all of them. We therefore conclude that no specific event of star formation can
be identified with the formation of the LMC bar, which instead likely formed
from a redistribution of disk material that occurred when the LMC disk became
bar unstable, and shared a common SFH with the inner disk thereafter. The
strong similarity between the SFH of the center and edge of the bar rules out
significant spatial variations of the SFH across the bar, which are predicted
by scenarios of classic bar formation through buckling mechanisms.Comment: MNRAS Letters, accepte
Characteristics of Disadvantaged Students. A Selection of Student Participants
© 2008 Copyright Education, Audiovisual & Culture Executive Agency.
The document may be freely copied and distributed provided that no modifications are made, that the
source is acknowledged and that this copyright notice is included
Impact of Scale Dependent Bias and Nonlinear Structure Growth on the ISW Effect: Angular Power Spectra
We investigate the impact of nonlinear evolution of the gravitational
potentials in the LCDM model on the Integrated Sachs-Wolfe (ISW) contribution
to the CMB temperature power spectrum, and on the cross-power spectrum of the
CMB and a set of biased tracers of the mass. We use an ensemble of N-body
simulations to directly follow the potentials and compare results to
perturbation theory (PT). The predictions from PT match the results to high
precision for k<0.2 h/Mpc. We compute the nonlinear corrections to the angular
power spectrum and find them to be <10% of linear theory for l<100. These
corrections are swamped by cosmic variance. On scales l>100 the departures are
more significant, however the CMB signal is more than a factor 10^3 larger at
this scale. Nonlinear ISW effects therefore play no role in shaping the CMB
power spectrum for l<1500. We analyze the CMB--density tracer cross-spectrum
using simulations and renormalized bias PT, and find good agreement. The usual
assumption is that nonlinear evolution enhances the growth of structure and
counteracts linear ISW on small scales, leading to a change in sign of the
CMB-LSS cross-spectrum at small scales. However, PT analysis suggests that this
trend reverses at late times when the logarithmic growth rate
f(a)=dlnD/dlna<0.5 or om_m(a)<0.3. Numerical results confirm these expectations
and we find no sign change in ISW-LSS cross-power for low redshifts.
Corrections due to nonlinearity and scale dependence of the bias are found to
be <10% for l<100, therefore below the S/N of the current and future
measurements. Finally, we estimate the CMB--halo cross-correlation coefficient
and show that it can be made to match that for CMB--dark matter to within 5%
for thin redshift shells, mitigating the need to model bias evolution.Comment: 27 pages, 19 figure. Hi-res. version:
http://www.itp.uzh.ch/~res/NonlinearISW.HiRes.pd
Development, Characterization, and In Vitro Evaluation of Tamoxifen Microemulsions
Microemulsions (MEs) were designed by an innovative rational development, characterized, and used to load up to 20 mM of Tamoxifen citrate (TMX). They were made with acceptable and well-characterized excipients for all the routes of administration. Some of their properties, such as nanometric mean size and long stability shelf life, make them interesting drug delivery systems. The results obtained after the in vitro inhibition of estradiol-induced proliferation in MCF-7 breast cancer cells demonstrated a significant effect in cell growth. A decreasing of at least 90% in viable cells was shown after the incubation with MEs containing 20 mM of TMX. Besides, two compositions which loaded 10 mM of drug showed a cytotoxic effect higher than 70%. These results encourage the evaluation of alternative protocols for this drug administration, not only for estrogen receptor (ER) positive tumors, but also for ER negative
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