2,613 research outputs found
Lyman-alpha radiative transfer during the Epoch of Reionization: contribution to 21-cm signal fluctuations
During the epoch of reionization, Ly-alpha photons emitted by the first stars
can couple the neutral hydrogen spin temperature to the kinetic gas
temperature, providing the opportunity to observe the gas in emission or
absorption in the 21-cm line. Given the bright foregrounds, it is of prime
importance to determine precisely the fluctuations signature of the signal, to
be able to extract it by its correlation power.
LICORICE is a Monte-Carlo radiative transfer code, coupled to the dynamics
via an adaptative Tree-SPH code. We present here the Ly-alpha part of the
implementation, and validate it through three classical tests. Contrary to
previous works, we do not assume that P_alpha, the number of scatterings of
Ly-alpha photons per atom per second, is proportional to the Ly-alpha
background flux, but take into account the scatterings in the Ly-alpha line
wings. The latter have the effect to steepen the radial profile of P_alpha
around each source, and re-inforce the contrast of the fluctuations. In the
particular geometry of cosmic filaments of baryonic matter, Ly-alpha photons
are scattered out of the filament, and the large scale structure of P_alpha is
significantly anisotropic. This could have strong implications for the possible
detection of the 21-cm signal.Comment: 13 pages, 9 figures. To be published in A&
Star formation efficiency in galaxy interactions and mergers: a statistical study
We investigate the enhancement of star formation efficiency in galaxy
interactions and mergers, by numerical simulations of several hundred galaxy
collisions. All morphological types along the Hubble sequence are considered in
the initial conditions of the two colliding galaxies, with varying
bulge-to-disk ratios and gas mass fractions. Different types of orbits are
simulated, direct and retrograde, according to the initial relative energy and
impact parameter, and the resulting star formation history is compared to that
occuring in the two galaxies when they are isolated. Our principal results are:
(1) retrograde encounters have a larger star formation efficiency (SFE) than
direct encounters; (2) the amount of gas available in the galaxy is not the
main parameter governing the SFE in the burst phase; (3) there is an
anticorrelation between the amplitude of the star forming burst and the tidal
forces exerted per unit of time, which is due to the large amount of gas
dragged outside the galaxy by tidal tails in strong interactions; (4) globally,
the Kennicutt-Schmidt law is retrieved statistically for isolated galaxies,
interacting pairs and mergers; (5) the enhanced star formation is essentially
occurring in nuclear starbursts, triggered by inward gas flows driven by
non-axisymmetries in the galaxy disks. Direct encounters develop more
pronounced asymmetries than retrograde ones. Based on these statistical
results, we derive general laws for the enhancement of star formation in galaxy
interactions and mergers, as a function of the main parameters of the
encounter.Comment: 22 pages, 37 figures, 4 tables. Accepted on Astronomy & Astrophysic
MOND and Cosmology
I review various ideas on MOND cosmology and structure formation beginning
with non-relativistic models in analogy with Newtonian cosmology. I discuss
relativistic MOND cosmology in the context of Bekenstein's theory and propose
an alternative biscalar effective theory of MOND in which the acceleration
parameter is identified with the cosmic time derivative of a matter coupling
scalar field. Cosmic CDM appears in this theory as scalar field oscillations of
the auxiliary "coupling strength" field.Comment: 8 pages, LaTeX, 2 figures, to appear in proceedings of IAP05 in
Paris: Mass Profiles and Shapes of Cosmological Structures, G. Mamon, F.
Combes, C. Deffayet and B. Fort (eds), (EDP-Sciences 2005
Formation and Evolution of Galactic Disks with a Multiphase Numerical Model
The formation and evolution of galactic disks are complex phenomena, where gas and star dynamics are coupled through star formation and the related feedback. The physical processes are so numerous and intricate that numerical models focus, in general, on one or a few of them only. We propose here a numerical model with particular attention to the multiphase nature of the interstellar medium; we consider a warm gas phase (> 10^4 K), treated as a continuous fluid by an SPH algorithm, and a cold gas phase (down to 10K), fragmented in clouds, treated by a low-dissipation sticky particles component. The two gas phases do not have the same dynamics, nor the same spatial distribution. In addition to gravity, they are coupled through mass exchanges due to heating/cooling processes, and supernovae feedback. Stars form out of the cold phase, and re-inject mass to the warm phase through SN explosions and stellar winds. The baryons are embedded in a live cold dark matter component. Baryonic disks, initially composed of pure gas, encounter violent instabilities, and a rapid phase of star formation, that slows down exponentially. Stars form in big clumps, that accumulate in the center to build a bulge. Exponential metallicity gradients are obtained. External infall of gas should be included to maintain a star formation rate in the disk comparable to what is observed in present disk galaxies
Gravitational Lensing & Stellar Dynamics
Strong gravitational lensing and stellar dynamics provide two complementary
and orthogonal constraints on the density profiles of galaxies. Based on
spherically symmetric, scale-free, mass models, it is shown that the
combination of both techniques is powerful in breaking the mass-sheet and
mass-anisotropy degeneracies. Second, observational results are presented from
the Lenses Structure & Dynamics (LSD) Survey and the Sloan Lens ACS (SLACS)
Survey collaborations to illustrate this new methodology in constraining the
dark and stellar density profiles, and mass structure, of early-type galaxies
to redshifts of unity.Comment: 6 pages, 2 figures; Invited contribution in the Proceedings of XXIst
IAP Colloquium, "Mass Profiles & Shapes of Cosmological Structures" (Paris,
4-9 July 2005), eds G. A. Mamon, F. Combes, C. Deffayet, B. Fort (Paris: EDP
Sciences
Signatures of radial migration in barred galaxies: Azimuthal variations in the metallicity distribution of old stars
By means of N-body simulations, we show that radial migration in galaxy
disks, induced by bar and spiral arms, leads to significant azimuthal
variations in the metallicity distribution of old stars at a given distance
from the galaxy center. Metals do not show an axisymmetric distribution during
phases of strong migration. Azimuthal variations are visible during the whole
phase of strong bar phase, and tend to disappear as the effect of radial
migration diminishes, together with a reduction in the bar strength. These
results suggest that the presence of inhomogeneities in the metallicity
distribution of old stars in a galaxy disk can be a probe of ongoing strong
migration. Such signatures may be detected in the Milky Way by Gaia (and
complementary spectroscopic data), as well as in external galaxies, by IFU
surveys like CALIFA and ATLAS3D. Mixing - defined as the tendency toward a
homogeneous, azimuthally symmetric, stellar distribution in the disk - and
migration turns out to be two distinct processes, the effects of mixing
starting to be visible when strong migration is over.Comment: 8 pages, 10 figures, accepted for publication on Astronomy and
Astrophysic
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