2,034 research outputs found
Draco -- A Failure of the Tidal Model
We test whether the structural properties of the nearby dwarf spheroidal
(dSph) galaxy Draco, a well-studied Milky Way companion, can be reconciled with
the suggestion that dSphs are unbound tidal remnants with a large depth extent
along the line of sight. In order to apply the observational test of this
hypothesis suggested by Klessen & Zhao, we use public photometric data from the
Sloan Digital Sky Survey (SDSS) to explore the width of Draco's blue horizontal
branch over a range of areas covering 0.06 square degrees to 6.25 square
degrees centered on Draco. The SDSS database is the only currently existing
database with sufficient depth and area coverage to permit a stringent test of
the tidal models. We show that blue horizontal branch stars extend beyond the
previously inferred limiting radii of Draco, consistent with the observed
absence of a truncated stellar surface density profile of this dSph. We
calculate new models for a galaxy without dark matter, using Draco's
morphological properties as constraints. The resulting models are unable to
reproduce the narrow observed horizontal branch width of Draco, which stays
roughly constant regardless of the field of view. We conclude that Draco cannot
be the remnant of a tidally disrupted satellite, but is probably strongly
dark-matter dominated. (ABSTRACT ABBREVIATED)Comment: 26 pages, 9 figures included, accepted for publication in ApJ,
high-resolution version available at
http://www.aip.de./~ralf/Publications/p22.abstract.htm
Observational Comparison of Star Formation in Different Galaxy Types
Galaxies cover a wide range of masses and star formation histories. In this
review, I summarize some of the evolutionary key features of common galaxy
types. At the high-mass end, very rapid, efficient early star formation is
observed, accompanied by strong enrichment and later quiescence, well-described
by downsizing scenarios. In the intermediate-mass regime, early-type galaxies
may still show activity in low-mass environments or when being rejuvenated by
wet mergers. In late-type galaxies, we find continuous, though variable star
formation over a Hubble time. In the dwarf regime, a wide range of properties
from bursty activity to quiescence is observed. Generally, stochasticity
dominates here, and star formation rates and efficiencies tend to be low.
Morphological types and their star formation properties correlate with
environment.Comment: Invited review to appear in IAU Symposium 270 on "Computational Star
Formation". Editors: J. Alves, B.G. Elmegreen, J.M. Girart, and V. Trimble
(Cambridge University Press). 12 pages, no figure
Metal-poor Galaxies in the Local Universe
A galaxy's mean metallicity is usually closely correlated with its luminosity
and mass. Consequently the most metal-poor galaxies in the local universe are
dwarf galaxies. Blue compact dwarfs and tidal dwarfs tend to deviate from the
metallicity-luminosity relation by being too metal-poor or too metal-rich for
their luminosity, respectively. A less pronounced offset separates dwarf
spheroidal (dSph) and dwarf irregular galaxies, making the former too
metal-rich for their luminosity, which indicates different formation conditions
for these two types of dwarfs. While environment (photo-evaporation through
local re-ionization by massive galaxies, tidal and ram pressure stripping)
govern the observed morphology-distance relation, intrinsic properties (in
particular total mass) play a decisive role in dwarf galaxy evolution with
respect to the time and duration of star formation and the amount of
enrichment. The metallicity distribution functions of nearby dwarfs can be
understood taking pre-enrichment, gas infall, and winds into account. Many
dwarfs show evidence for inhomogeneous, localized enrichment. Ultra-faint
dSphs, which may have formed their metal-poor stars at high redshift via H2
cooling, show an overabundance of metal-deficient stars as compared to the
(inner) Galactic halo, but may, along with classical dSphs, have contributed
significantly to the build-up of the outer halo. The abundance ratios measured
in the irregular Large Magellanic Cloud are consistent with the postulated
early accretion of irregulars to form the inner Galactic halo.Comment: Invited review, "First Stars IV" in Kyoto, Japan, 2012. 12 pages. To
appear in AIP Conference Proceeding
Stellar Populations in the Local Group of Galaxies
The characteristics and properties of the stellar populations and
evolutionary histories of Local Group galaxies are summarized and compared to
predictions of cosmological models. No clear signature of the re-ionization
epoch is observed; in particular, there is no cessation of star formation
activity in low-mass dwarf galaxies at the end of re-ionization. Arguments
against the morphological transformation of dwarf irregular into dwarf
spheroidal galaxies are derived from their pronounced evolutionary differences
at early epochs as evidenced by the offset in the metallicity-luminosity
relation between gas-rich and gas-poor dwarfs. While there is increasing
evidence for past and ongoing accretion events the overall importance of dwarf
galaxies as building blocks remains unclear considering their differences in
modes of star formation and detailed chemistry.Comment: Invited talk at the first international workshop on "Stellar
Astrophysics with the World's Largest Telescopes", Torun, Poland, 7-10
September 2004, 14 pages, 2 figure
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