343 research outputs found
Structure and stellar content of dwarf galaxies. III: B and R photometry of dwarf galaxies in the M101 group and the nearby field
We have carried out CCD photometry in the Cousins B and R bands of 21 dwarf
galaxies in and around the M101 group. Eleven are members and suspected members
of the group and ten are field galaxies in the projected vicinity of the group.
We have derived total magnitudes, effective radii, effective surface
brightnesses, as well as galaxy diameters at various isophotal levels in both
colours. Best-fitting exponential parameters and colour gradients are also
given for these galaxies. Some of the galaxies show a pronounced luminosity
excess above the best-fitting exponential at large radii, or surface
brightnesses fainter than approx 26 mag/sq_arcsec in R. This feature, while
non-significant for a single case and technically difficult to interpret, might
be an indication of the existence of an extended old stellar halo in dwarf
irregulars. The photometric parameters of the galaxies presented here will be
combined with previously published data for nearby dwarf galaxies and
statistically analysed in a forthcoming paper.Comment: 15 pages, 4 tables and 13 figures. For a full resolution version see
http://www.astro.unibas.ch/galaxies/papers.html To appear in A&A
Structure and stellar content of dwarf galaxies IV. B and R photometry of dwarf galaxies in the CVnI cloud
We have carried out CCD photometry in the Cousins B and R bands of 15
galaxies in the Canes Venatici I cloud. Total magnitudes, effective radii,
effective surface brightnesses, as well as galaxy radii at various isophotal
levels in both colors were determined. Best-fitting exponential parameters and
color gradients are also given for these galaxies. The photometric parameters
presented here will analyzed in a forthcoming paper, together with previously
published data for nearby dwarf galaxies.Comment: 10 pages, submitted to A&AS. For a full resolution version see
ftp://merkur.astro.unibas.ch/pub/bremnes/canesv.ps.g
Virgo cluster early-type dwarf galaxies with the Sloan Digital Sky Survey. IV. The color-magnitude relation
We present an analysis of the optical colors of 413 Virgo cluster early-type
dwarf galaxies (dEs), based on Sloan Digital Sky Survey imaging data. Our study
comprises (1) a comparison of the color-magnitude relation (CMR) of the
different dE subclasses that we identified in Paper III of this series, (2) a
comparison of the shape of the CMR in low and high-density regions, (3) an
analysis of the scatter of the CMR, and (4) an interpretation of the observed
colors with ages and metallicities from population synthesis models. We find
that the CMRs of nucleated (dE(N)) and non-nucleated dEs (dE(nN)) are
significantly different from each other, with similar colors at fainter
magnitudes (r > 17 mag), but increasingly redder colors of the dE(N)s at
brighter magnitudes. We interpret this with older ages and/or higher
metallicities of the brighter dE(N)s. The dEs with disk features have similar
colors as the dE(N)s and seem to be only slightly younger and/or less
metal-rich on average. Furthermore, we find a small but significant dependence
of the CMR on local projected galaxy number density, consistently seen in all
of u-r, g-r, and g-i, and weakly i-z. We deduce that a significant intrinsic
color scatter of the CMR is present, even when allowing for a distance spread
of our galaxies. No increase of the CMR scatter at fainter magnitudes is
observed down to r = 17 mag (Mr = -14 mag). The color residuals, i.e., the
offsets of the data points from the linear fit to the CMR, are clearly
correlated with each other in all colors for the dE(N)s and for the full dE
sample. We conclude that there must be at least two different formation
channels for early-type dwarfs in order to explain the heterogeneity of this
class of galaxy. (Abridged)Comment: 17 pages + 12 figures. Accepted for publication in A
Deep griz GMOS Imaging of the Dwarf Irregular Galaxy Kar 50
Images obtained with the Gemini Multi-Object Spectrograph (GMOS) are used to
investigate the stellar content and distance of the dwarf irregular galaxy Kar
50. The brightest object is an HII region, and the bright stellar content is
dominated by stars with g'-r' < 0. The tips of the main sequence and the red
giant branch are tentatively identified near r' = 24.9 and i' = 25.5,
respectively. The galaxy has a blue integrated color with no significant color
gradient, and we conclude that Kar 50 has experienced a recent galaxy-wide
episode of star formation. The distance estimated from the brightest blue stars
indicates that Kar 50 is behind the M81 group, and this is consistent with the
tentative RGB-tip brightness. Kar 50 has a remarkably flat central surface
brightness profile, even at wavelengths approaching 1um, although there is no
evidence of a bar. In the absence of another large star-forming episode, Kar 50
will evolve into a very low surface brightness galaxy.Comment: 17 pages of text and 8 postscript figures. Accepted for publication
in the PAS
Disks in Early-Type Dwarf Galaxies
We identify disk features (spiral arms, bars, or edge-on disks) in a significant fraction of Virgo cluster early-type dwarfs. These galaxies are disk-shaped and are an unrelaxed cluster population that possibly formed out of infalling progenitors. Some display spiral arms with grand design features that cannot be the mere remainders of potential late-type spiral progenitor
Temperature dependence of surface stress across an order-disorder transition: p(1x2)O/W(110)
Strain relaxations of a p(1x2) ordered oxygen layer on W(110) are measured as
a function of temperature across the disordering transition using low-energy
electron diffraction. The measured strains approach values of 0.027 in the
[1-10] and -0.053 in the [001] direction. On the basis of the measured strain
relaxations, we give quantitative information on temperature-dependent surface
stress using the results of ab initio calculations. From the surface formation
energy for different strains, determined by first-principles calculations, we
estimate that surface stress changes from -1.1 for the ordered phase to -0.2N/m
for the disordered one along [1-10], and from 5.1 to 3.4 N/m along [001].
Moreover, our observation that the strains scale inversely with domain size
confirms that the strain relaxation takes place at the domain boundaries.Comment: 8 pages, 5 figure
Embedded disks in Fornax dwarf ellipticals
We present photometric and kinematic evidence for the presence of stellar
disks, seen practically edge-on, in two Fornax dwarf galaxies, FCC204 (dS0(6))
and FCC288 (dS0(7)). This is the first time such structures have been
identified in Fornax dwarfs. FCC2088 has only a small bulge and a bright
flaring and slightly warped disk that can be traced out to 23" from the center
(2.05 kpc for H_0=75 km/s/Mpc). FCC204's disk can be traced out to 20" (1.78
kpc). This galaxy possesses a large bulge. These results can be compared to the
findings of Jerjen et al. (2000) and Barazza et al. (2002) who discovered
nucleated dEs with spiral and bar features in the Virgo Cluster.Comment: 8 pages, 8 figures, accepted for publication in A&
A Collision of Subclusters in Abell 754
We present direct evidence of a collision of subclusters in the galaxy
cluster Abell 754. Our comparison of new optical data and archival ROSAT PSPC
X-ray data reveal three collision signatures predicted by n-body/hydrodynamical
simulations of hierarchical cluster evolution. First, there is strong evidence
of a non-hydrostatic process; neither of the two major clumps in the galaxy
distribution lies on the off-center peak of the X-ray emission from the
intracluster gas. Second, the peak of the X-ray emission is elongated
perpendicular to the collision axis defined by the centroids of the two galaxy
clumps. Third, there is evidence of compression-heated gas; one of A754's two
X-ray temperature components (Henry & Briel 1995) is among the hottest observed
in any cluster and hotter than that inferred from the velocity dispersion of
the associated galaxy clump. These signatures are consistent with the
qualitative features of simulations (Evrard 1990a,b) in which two subclusters
have collided in the plane of the sky during roughly the last Gyr. The
detection of such collisions is crucial for understanding both the dynamics of
individual clusters and the underlying cosmology. First, for systems like A754,
estimating the cluster X-ray mass from assumptions of hydrostatic equilibrium
and isothermality is incorrect and may produce the discrepancies sometimes
found between X-ray masses and those derived from gravitational lens models
(Babul & Miralda-Escude 1994). Second, the fraction of nearby clusters in which
subclusters have collided in the last Gyr is especially sensitive to the mean
mass density parameter Omega_0 (cf. Richstone et al. 1992; Evrard et al. 1993;
Lacey & Cole 1993). With a large, well-defined cluster sample, it will be
possible to place a new and powerful constraint on cosmological models.Comment: 4 pages + 1 color figure (Postscript). Accepted for Publication in
ApJ Letter
Surface stress of Ni adlayers on W(110): the critical role of the surface atomic structure
Puzzling trends in surface stress were reported experimentally for Ni/W(110)
as a function of Ni coverage. In order to explain this behavior, we have
performed a density-functional-theory study of the surface stress and atomic
structure of the pseudomorphic and of several different possible 1x7
configurations for this system. For the 1x7 phase, we predict a different, more
regular atomic structure than previously proposed based on surface x-ray
diffraction. At the same time, we reproduce the unexpected experimental change
of surface stress between the pseudomorphic and 1x7 configuration along the
crystallographic surface direction which does not undergo density changes. We
show that the observed behavior in the surface stress is dominated by the
effect of a change in Ni adsorption/coordination sites on the W(110) surface.Comment: 14 pages, 3 figures Published in J. Phys.: Condens. Matter 24 (2012)
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