33 research outputs found
Escenarios cosmológicos con distintos parámetros de densidad
Se están analizando diferentes escenarios cosmológicos con distintos parámetros de densidad compatibles con las determinaciones del espectro primordial de fluctuaciones, el contenido de material bariónico en cúmulos de galaxias y los resultados de la teoría de nucleosíntesis, el campo de velocidades peculiares de galaxias y su distribución espacial. Además, se está trabajando en la elaboración de un programa de cálculo de N-cuerpos basado en el esquema particle - mesh y que permite un tratamiento mas exacto de las interacciones partícula - partícula en escalas menores que la resolución numérica del potencial de la red.Asociación Argentina de Astronomí
Dependencia de la longitud de correlación de galaxias con el tipo morfológico y la velocidad circular
Utilizando el catálogo de velocidades radiales CfA investigamos la dependencia entre la longitud de correlación r. de galaxias con el tipo morfológico t y la velocidad circular Vc. Adoptando una ley de potencia para la función de correlación bipuntual x(r) =(r/r₀) con g = 1.8 y r₀ = 6 h Mpc (valor medio), se determina una relación entre r₀ y t que resulta: r₀ = (6.7 - 0.3 t) h Mpc. Encontramos una dependencia significativa entre el número medio de vecinos y la velocidad circular de las galaxias. Objetos con Vc mayor que 250 km/s presentan un exceso en el número medio de vecinos dentro de esferas de radio R, R < 6 h Mpc. Este exceso implica un incremento del 20% en el valor de r. respecto a su valor medio. Por otra parte no se encuentra evidencia estadística de una dependencia similar para objetos con velocidades Vc < 250 km/s.Asociación Argentina de Astronomí
Indirect Dark Matter Detection from Dwarf Satellites: Joint Expectations from Astrophysics and Supersymmetry
We present a general methodology for determining the gamma-ray flux from
annihilation of dark matter particles in Milky Way satellite galaxies, focusing
on two promising satellites as examples: Segue 1 and Draco. We use the
SuperBayeS code to explore the best-fitting regions of the Constrained Minimal
Supersymmetric Standard Model (CMSSM) parameter space, and an independent MCMC
analysis of the dark matter halo properties of the satellites using published
radial velocities. We present a formalism for determining the boost from halo
substructure in these galaxies and show that its value depends strongly on the
extrapolation of the concentration-mass (c(M)) relation for CDM subhalos down
to the minimum possible mass. We show that the preferred region for this
minimum halo mass within the CMSSM with neutralino dark matter is ~10^-9-10^-6
solar masses. For the boost model where the observed power-law c(M) relation is
extrapolated down to the minimum halo mass we find average boosts of about 20,
while the Bullock et al (2001) c(M) model results in boosts of order unity. We
estimate that for the power-law c(M) boost model and photon energies greater
than a GeV, the Fermi space-telescope has about 20% chance of detecting a dark
matter annihilation signal from Draco with signal-to-noise greater than 3 after
about 5 years of observation
Pregnancy in women with perinatally acquired HIV-infection: Outcomes and challenges
This is a retrospective comparison of pregnant women with perinatally acquired HIV-infection (PAH) with a cohort of pregnant women with behaviorally acquired HIV-infection (BAH). PAH cases (11 women) included all pregnant adolescents followed at our HIV clinic from January 2000 to January 2009. BAH cases (27 women) were randomly selected from all deliveries within the study period at the same institution. Demographics, mode of delivery, CD4+ counts, and viral loads (VLs) before, during, and six months postpartum, as well as neonatal outcomes, were reviewed
Dark Matter Direct Detection Signals inferred from a Cosmological N-body Simulation with Baryons
We extract at redshift z=0 a Milky Way sized object including gas, stars and
dark matter (DM) from a recent, high-resolution cosmological N-body simulation
with baryons. Its resolution is sufficient to witness the formation of a
rotating disk and bulge at the center of the halo potential. The phase-space
structure of the central galactic halo reveals the presence of a dark disk
component, that is co-rotating with the stellar disk. At the Earth's location,
it contributes to around 25% of the total DM local density, whose value is
rho_DM ~ 0.37 GeV/cm^3. The velocity distributions also show strong deviations
from pure Gaussian and Maxwellian distributions, with a sharper drop of the
high velocity tail.
We give a detailed study of the impact of these features on the predictions
for DM signals in direct detection experiments. In particular, the question of
whether the modulation signal observed by DAMA is or is not excluded by limits
set by other experiments (CDMS, XENON and CRESST...) is re-analyzed and
compared to the case of a standard Maxwellian halo, in both the elastic and the
inelastic scattering scenarios. We find that the compatibility between DAMA and
the other experiments is improved. In the elastic scenario, the DAMA modulation
signal is slightly enhanced in the so-called channeling region, as a result of
several effects. For the inelastic scenario, the improvement of the fit is
mainly attributable to the departure from a Maxwellian distribution at high
velocity.Comment: 39 page
The outer halos of elliptical galaxies
Recent progress is summarized on the determination of the density
distributions of stars and dark matter, stellar kinematics, and stellar
population properties, in the extended, low surface brightness halo regions of
elliptical galaxies. With integral field absorption spectroscopy and with
planetary nebulae as tracers, velocity dispersion and rotation profiles have
been followed to ~4 and ~5-8 effective radii, respectively, and in M87 to the
outer edge at ~150 kpc. The results are generally consistent with the known
dichotomy of elliptical galaxy types, but some galaxies show more complex
rotation profiles in their halos and there is a higher incidence of
misalignments, indicating triaxiality. Dynamical models have shown a range of
slopes for the total mass profiles, and that the inner dark matter densities in
ellipticals are higher than in spiral galaxies, indicating earlier assembly
redshifts. Analysis of the hot X-ray emitting gas in X-ray bright ellipticals
and comparison with dynamical mass determinations indicates that non-thermal
components to the pressure may be important in the inner ~10 kpc, and that the
properties of these systems are closely related to their group environments.
First results on the outer halo stellar population properties do not yet give a
clear picture. In the halo of one bright galaxy, lower [alpha/Fe] abundances
indicate longer star formation histories pointing towards late accretion of the
halo. This is consistent with independent evidence for on-going accretion, and
suggests a connection to the observed size evolution of elliptical galaxies
with redshift.Comment: 8 pages. Invited review to appear in the proceedings of "Galaxies and
their Masks" eds. Block, D.L., Freeman, K.C. & Puerari, I., 2010, Springer
(New York
Metal enrichment processes
There are many processes that can transport gas from the galaxies to their
environment and enrich the environment in this way with metals. These metal
enrichment processes have a large influence on the evolution of both the
galaxies and their environment. Various processes can contribute to the gas
transfer: ram-pressure stripping, galactic winds, AGN outflows, galaxy-galaxy
interactions and others. We review their observational evidence, corresponding
simulations, their efficiencies, and their time scales as far as they are known
to date. It seems that all processes can contribute to the enrichment. There is
not a single process that always dominates the enrichment, because the
efficiencies of the processes vary strongly with galaxy and environmental
properties.Comment: 18 pages, 8 figures, accepted for publication in Space Science
Reviews, special issue "Clusters of galaxies: beyond the thermal view",
Editor J.S. Kaastra, Chapter 17; work done by an international team at the
International Space Science Institute (ISSI), Bern, organised by J.S.
Kaastra, A.M. Bykov, S. Schindler & J.A.M. Bleeke
Evolución de sistemas de galaxias en el modelo CDM
Se realizaron simulaciones numéricas de N-cuerpos para estudiar la evolución de sistemas de galaxias en el contexto teórico del modelo CDM (Cold Dark Matter) con la normalización impuesta por la reciente determinación de las fluctuaciones en la temperatura de la radiación de fondo. Se implementaron modelos de formación de galaxias suponiendo un enfriamiento instantáneo del gas en regiones cuyo contraste de densidad local es alto. Los modelos analizados incluyen los efectos de fusión de galaxias, la acreción de gas y la inyección de energía al medio intergaláctico debido a vientos de supernovas. Los resultados obtenidos permiten dar cuenta de la relación observacional Tully-Fisher para galaxias espirales y del extremo débil de la función de luminosidad; como así también de la aparente disminución en la eficiencia de formación de galaxias en sistemas ricos. Los modelos no sustentan la existencia de efectos sistemáticos entre la dispersión de velocidades peculiares de las galaxias y la materia oscura indicando una gran dificultad del modelo CDM para reproducir las observaciones.Asociación Argentina de Astronomí
Chemical evolution of the galactic disk: evidence of an abundance gradient perpendicular to the galactic plane
Using a revised DDO abundance scale for the galactic open cluster system, the existence and size of the radial and axial abundance gradients, as well as the existence of a global age-metallicity relation in the galactic disk are investigated.Asociación Argentina de Astronomí