1,168 research outputs found
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
Beyond Borders: Educating and Empowering Between Mexico and the United States. A biographical case study
Determinación de la estructura genética de las poblaciones silvestres españolas de Castanea sativa mediante isoenzimas
The genetic variability within and among 17 wild Spanish chestnut stands was examined by isozyme analysis, with the goals of describing their geographic structure and designing conservation and management strategies. Measures of genetic diversity such as allelic richness, heterozygosity, polymorphism, F-statistics, D-statistics, gene flow, clustering using Nei’s genetic distances and a method based on an Monte Carlo Markov Chain algorithm and the contributions of each stand to diversity and allelic richness were all used. Wild Spanish chestnut populations displayed heterogeneity of allele frequencies between them, high levels of genetic diversity and high differentiation (Fst = 0.15) compared with populations from other western European countries such as France and Italy. The two clustering methods allowed the identification of three clusters: a Mediterranean cluster, a northern Spanish cluster and the southern Galician cluster. The highest heterozygosity and allelic richness were found in the North, especially in the southern Galician cluster. Several areas can be recommended for inclusion in the network of Conservation Units: Fraga de Catasós, representing the southern Galician cluster; Fragas do Eume, representing the northern Spanish cluster; and Hervás or El Tiemblo, representing the Mediterranean cluster.La variabilidad genética entre y dentro de 17 rodales de castaño silvestre muestreados en poblaciones españolas se examinó mediante el análisis de polimorfismos isoenzimáticos con la finalidad de describir la estructura geográfica y diseñar estrategias de conservación y manejo. Se calcularon la riqueza alélica, heterocigosidad, polimorfismo, la estadística F y D, el flujo genético y se realizaron análisis de agrupación de poblaciones utilizando la distancia genética de Nei y un método basado en el algoritmo Monte Carlo Markov Chain, y finalmente se calcularon las contribuciones de cada rodal a la diversidad y riqueza alélica.
Las poblaciones silvestres de castaño españolas presentaron heterogeneidad de frecuencias alélicas entre ellas, elevados niveles de diversidad genética y de diferenciación (Fst = 0.15) comparadas con otras poblaciones del Oeste de Europa. Se identificaron tres grupos de poblaciones: el grupo Mediterráneo, el grupo del Norte y del Sur de Galicia. La mayor heterocigosidad y riqueza alélica está en el Norte, principalmente en el grupo del Sur de Galicia. Se recomiendan varias áreas para incluir en la red de Unidades de Conservación: Fraga de Catasós, en representación del grupo Sur de Galicia; las Fragas do Eume, representando el grupo del Norte; y Hervás o el Tiemblo en representación del grupo Mediterráneo
The Effect of Hot Gas in WMAP's First Year Data
By cross-correlating templates constructed from the 2 Micron All Sky Survey
(2MASS) Extended Source (XSC) catalogue with WMAP's first year data, we search
for the thermal Sunyaev-Zel'dovich signature induced by hot gas in the local
Universe. Assuming that galaxies trace the distribution of hot gas, we select
regions on the sky with the largest projected density of galaxies. Under
conservative assumptions on the amplitude of foreground residuals, we find a
temperature decrement of -35 7 K ( detection level,
the highest reported so far) in the 26 square degrees of the sky
containing the largest number of galaxies per solid angle. We show that most of
the reported signal is caused by known galaxy clusters which, when convolved
with the average beam of the WMAP W band channel, subtend a typical angular
size of 20--30 arcmins. Finally, after removing from our analyses all pixels
associated with known optical and X-ray galaxy clusters, we still find a tSZ
decrement of -96 37 K in pixels subtending about 0.8 square
degrees on the sky. Most of this signal is coming from five different cluster
candidates in the Zone of Avoidance (ZoA), present in the Clusters In the ZoA
(CIZA) catalogue. We found no evidence that structures less bound than clusters
contribute to the tSZ signal present in the WMAP data.Comment: 10 pages, 4 figures, matches accepted version in ApJ Letter
Adult-Onset Eccrine Angiomatous Hamartoma: A Case Report With Ultrasound Findings
[Abstract] Eccrine angiomatous hamartoma (EAH) is a rare, benign cutaneous tumor composed of vascular and eccrine elements. It is most commonly diagnosed during the first years of life, although there are reports of cases diagnosed in adults. We report the ultrasound findings of a 46-year-old patient with a left plantar lesion, histopathological diagnosis of which confirmed suspicion of EAH
The galaxy cluster Ysz-Lx and Ysz-M relations from the WMAP 5-yr data
We use multifrequency matched filters to estimate, in the WMAP 5-year data,
the Sunyaev-Zel'dovich (SZ) fluxes of 893 ROSAT NORAS/REFLEX clusters spanning
the luminosity range Lx,[0.1-2.4]keV = 2 10^{41} - 3.5 10^{45} erg s^{-1}. The
filters are spatially optimised by using the universal pressure profile
recently obtained from combining XMM-Newton observations of the REXCESS sample
and numerical simulations. Although the clusters are individually only
marginally detected, we are able to firmly measure the SZ signal (>10 sigma)
when averaging the data in luminosity/mass bins. The comparison between the
bin-averaged SZ signal versus luminosity and X-ray model predictions shows
excellent agreement, implying that there is no deficit in SZ signal strength
relative to expectations from the X-ray properties of clusters. Using the
individual cluster SZ flux measurements, we directly constrain the Y500-Lx and
Y500-M500 relations, where Y500 is the Compton y-parameter integrated over a
sphere of radius r500. The Y500-M500 relation, derived for the first time in
such a wide mass range, has a normalisation Y*500=[1.60 pm 0.19] 10^{-3}
arcmin^2 at M500=3 10^{14} h^{1} Msun, in excellent agreement with the X-ray
prediction of 1.54 10^{-3} arcmin^2, and a mass exponent of alpha=1.79 pm 0.17,
consistent with the self-similar expectation of 5/3. Constraints on the
redshift exponent are weak due to the limited redshift range of the sample,
although they are compatible with self-similar evolution.Comment: Version accepted for publication in Astronomy and Astrophysic
Global Antifungal Profile Optimization of Chlorophenyl Derivatives against Botrytis cinerea and Colletotrichum gloeosporioides
Twenty-two aromatic derivatives bearing a chlorine atom and a different chain in the para or meta
position were prepared and evaluated for their in vitro antifungal activity against the phytopathogenic
fungi Botrytis cinerea and Colletotrichum gloeosporioides. The results showed that maximum inhibition
of the growth of these fungi was exhibited for enantiomers S and R of 1-(40-chlorophenyl)-
2-phenylethanol (3 and 4). Furthermore, their antifungal activity showed a clear structure-activity
relationship (SAR) trend confirming the importance of the benzyl hydroxyl group in the inhibitory
mechanism of the compounds studied. Additionally, a multiobjective optimization study of the
global antifungal profile of chlorophenyl derivatives was conducted in order to establish a rational
strategy for the filtering of new fungicide candidates from combinatorial libraries. The MOOPDESIRE
methodology was used for this purpose providing reliable ranking models that can be
used later
Impact of Systematic Errors in Sunyaev-Zel'dovich Surveys of Galaxy Clusters
Future high-resolution microwave background measurements hold the promise of
detecting galaxy clusters throughout our Hubble volume through their
Sunyaev-Zel'dovich (SZ) signature, down to a given limiting flux. The number
density of galaxy clusters is highly sensitive to cluster mass through
fluctuations in the matter power spectrum, as well as redshift through the
comoving volume and the growth factor. This sensitivity in principle allows
tight constraints on such quantities as the equation of state of dark energy
and the neutrino mass. We evaluate the ability of future cluster surveys to
measure these quantities simultaneously when combined with PLANCK-like CMB
data. Using a simple effective model for uncertainties in the cluster mass-SZ
flux relation, we evaluate systematic shifts in cosmological constraints from
cluster SZ surveys. We find that a systematic bias of 10% in cluster mass
measurements can give rise to shifts in cosmological parameter estimates at
levels larger than the statistical errors. Systematic errors are
unlikely to be detected from the mass and redshift dependence of cluster number
counts alone; increasing survey size has only a marginal effect. Implications
for upcoming experiments are discussed.Comment: 12 pages, 6 figures; accepted to JCAP; revised to match submitted
versio
- …