160 research outputs found
Exploring the formation of spheroidal galaxies out to z ⌠1.5 in GOODS
The formation of massive spheroidal galaxies is studied on a visually classified sample extracted from the Advanced Camera for Surveys/Hubble Space Telescope (ACS/HST) images of the Great Observatories Origins Deep Survey north and south fields, covering a total area of 360 arcmin . The sample size (910 galaxies brighter than i = 24) allows us to explore in detail the evolution over a wide range of redshifts (0.4 10 M galaxies by a factor of 2 between z = 1 and 0, in contrast with a factor of âŒ50 for lower mass galaxies (10 <M / M <10 ). One-quarter of the whole sample of early types are photometrically classified as blue galaxies. On a volume-limited sample out to z <0.7, the average stellar mass of the blue ellipticals is 5 Ă 10 M compared to 4 Ă 10 M for red ellipticals. On a volume-limited subsample out to z = 1.4 probing the brightest galaxies (M <-21), we find the median redshift of blue and red early types: 1.10 and 0.85, respectively. Blue early types only amount to 4 per cent of this sample (compared to 26 per cent in the full sample). The intrinsic colour distribution correlates overall bluer colours with blue cores (positive radial gradients of colour), suggesting an inside-out process of formation. The redshift evolution of the observed colour gradients is incompatible with a significant variation in stellar age within each galaxy. The slope of the Kormendy relation in the subsample of massive galaxies does not change over 0.4 <z <1.4 and is compatible with z = 0 values. The 'zero-point' of the Kormendy relation (i.e. the surface brightness at a fixed half-light radius) is 1 mag fainter (in the B band) for the subsample of low-mass (M <3.5 Ă 10 M ) early types.Peer reviewe
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
Internal convection in thermoelectric generator models
Coupling between heat and electrical currents is at the heart of
thermoelectric processes. From a thermal viewpoint this may be seen as an
additional thermal flux linked to the appearance of electrical current in a
given thermoelectric system. Since this additional flux is associated to the
global displacement of charge carriers in the system, it can be qualified as
convective in opposition to the conductive part associated with both phonons
transport and heat transport by electrons under open circuit condition, as,
e.g., in the Wiedemann-Franz relation. In this article we demonstrate that
considering the convective part of the thermal flux allows both new insight
into the thermoelectric energy conversion and the derivation of the maximum
power condition for generators with realistic thermal coupling.Comment: 8 pages, 3 figure
The young stellar population at the center of NGC 205
Context. NGC 205 is a peculiar dwarf elliptical galaxy hosting in its center
a population of young blue stars. Their origin is still matter of debate, the
central fresh star formation activity possibly being related to dynamical
interactions between NGC 205 and M31. Aims. The star formation history in the
central 30\arcsec (120 pc) around the NGC 205 central nucleus is
investigated in order to obtain clues to the origin of the young stellar
population. Methods. Deep HST/ACS CCD photometry is compared with theoretical
isochrones and luminosity functions to characterize the stellar content of the
region under study and compute the recent SF rate. Results. Our photometry
reveals a previously undetected blue plume of young stars clearly
distinguishable down to I26. Our analysis suggests that 1.9
M were produced between approximately 62 Myr and 335 Myr ago in the NGC
205 inner regions, with a latest minor episode occurring 25 Myr ago. This
implies a star formation rate of M/yr over this
period. Conclusions. The excellent fit of the observed luminosity function of
young main sequence stars obtained with a model having a constant star
formation rate argues against a tidally triggered star formation activity over
the last 300 Myr. Rather, a constant SF may be consistent with NGC 205
being on its first interaction with M 31.Comment: 5 pages, 2 figures, accepted for publication in A&A letter
The Herschel Virgo Cluster Survey: VII. Dust in cluster dwarf elliptical galaxies
We use the Science Demonstration Phase data of the Herschel Virgo Cluster
Survey to search for dust emission of early-type dwarf galaxies in the central
regions of the Virgo Cluster as an alternative way of identifying the
interstellar medium.We present the first possible far-infrared detection of
cluster early-type dwarf galaxies: VCC781 and VCC951 are detected at the 10
sigma level in the SPIRE 250 micron image. Both detected galaxies have dust
masses of the order of 10^5 Msun and average dust temperatures ~20K. The
detection rate (less than 1%) is quite high compared to the 1.7% detection rate
for Hi emission, considering that dwarfs in the central regions are more Hi
deficient. We conclude that the removal of interstellar dust from dwarf
galaxies resulting from ram pressure stripping, harassment, or tidal effects
must be as efficient as the removal of interstellar gas.Comment: Letter accepted for publication in A&A (Herschel special issue
A deep view on the Virgo cluster core
In this study we investigate the optical photometric properties of early-type
galaxies in the Virgo cluster core region, by analysing their location on the
colour magnitude relation (CMR) and the structural scaling relations down to
faint magnitudes, and by constructing the luminosity function to compare it
with theoretical expectations. We visually select potential cluster members
based on morphology and angular size, excluding spiral galaxies. A photometric
analysis has been carried out for 295 galaxies, using surface brightness
profile shape and colour as further criteria to identify probable background
contaminants. 216 galaxies are considered to be certain or probable Virgo
cluster members. Our study reveals 77 galaxies not catalogued in the VCC (with
13 of them already found in previous studies) that are very likely Virgo
cluster members because they follow the Virgo CMR and exhibit low Sersic
indices. Those galaxies reach -8.7 mag in V band. The CMR shows a clear change
in slope from dEs to dSphs, while the scatter of the CMR in the dSph regime
does not increase significantly. Our sample might, however, be somewhat biased
towards redder colours. The scaling relations given by the dEs appear to be
continued by the dSphs indicating a similar origin. The observed change in the
CMR slope may mark the point at which gas loss prevented significant metal
enrichment. The almost constant scatter around the CMR possibly indicates a
short formation period, resulting in similar stellar populations. The
luminosity function shows a Schechter function's faint end slope of
-1.50\pm0.17, implying a lack of galaxies related to the expected number of
low-mass dark matter haloes from theoretical models. Our findings could be
explained by suppressed star formation in low-mass dark matter halos or by
tidal disruption of dwarfs in the dense core region of the cluster.Comment: A&A accepted, photometry of newly identified dwarf galaxies is
provided in Table 3, 17 pages, 8 figure
Relating basic properties of bright early-type dwarf galaxies to their location in Abell 901/902
We present a study of the population of bright early-type dwarf galaxies in
the multiple-cluster system Abell 901/902. We use data from the STAGES survey
and COMBO-17 to investigate the relation between the color and structural
properties of the dwarfs and their location in the cluster. The definition of
the dwarf sample is based on the central surface brightness and includes
galaxies in the luminosity range -16 >= M_B >~-19 mag. Using a fit to the color
magnitude relation of the dwarfs, our sample is divided into a red and blue
subsample. We find a color-density relation in the projected radial
distribution of the dwarf sample: at the same luminosity dwarfs with redder
colors are located closer to the cluster centers than their bluer counterparts.
Furthermore, the redder dwarfs are on average more compact and rounder than the
bluer dwarfs. These findings are consistent with theoretical expectations
assuming that bright early-type dwarfs are the remnants of transformed
late-type disk galaxies involving processes such as ram pressure stripping and
galaxy harassment. This indicates that a considerable fraction of dwarf
elliptical galaxies in clusters are the results of transformation processes
related to interactions with their host cluster.Comment: 12 pages, 8 figures, accepted for publication in A&A, typo corrected
in abstrac
Evolution of field early-type galaxies: The view from GOODS/CDFS
(Abridged) We explore the evolution of field early-type galaxies on a sample
extracted from GOODS/CDFS. The galaxies are selected by means of a
non-parametric analysis followed by visual inspection. We exclude those
galaxies which are not consistent with an evolution into the Kormendy relation.
The final set comprises 249 galaxies with a median redshift z=0.7. The
distribution of number counts versus apparent magnitude suggests a substantial
decrease of the comoving number density with redshift. The majority of the
galaxies feature passively evolving old stellar populations. One third of those
in the upper half of the redshift distribution have blue colors, in contrast to
only 10% in the lower redshift subsample. An adaptive binning of the color maps
is performed to explore the internal color distribution. We find that most blue
galaxies in our sample feature blue cores whereas most of the red early-types
are passively evolving stellar populations with red cores. The color gradients
and scatter do not evolve with redshift and are compatible with the
observations at z=0 assuming a radial dependence of the metallicity within each
galaxy. This work emphasizes the need for a careful sample selection, as we
found that most of those galaxies which were visually classified as early types
-- but then rejected based on the Kormendy relation -- feature blue colors
characteristic of recent star formation.Comment: 14 pages, 16 figures. Uses emulateapj. Accepted for publication in
ApJ. Some figures in low resolutio
Maternal knowledge of the risk of vertical transmission and offspring acquisition of hepatitis B.
INTRODUCTION AND OBJECTIVES: Universal vaccination at birth and in infancy is key to the elimination of chronic hepatitis B infection. We aimed to assess hepatitis B immune-prophylaxis and perinatal transmission knowledge, in a large and ethnically diverse cohort of previously pregnant North American women, chronically infected with hepatitis B.
MATERIALS AND METHODS: The Hepatitis B Research Network (HBRN) is comprised of 28 Clinical Centers in the United States and Canada. Female cohort participants were administered a questionnaire to assess: (1) their assertion of knowledge regarding HBV prophylaxis at birth, testing, and diagnosis of hepatitis B in their children, and (2) the percentage of affirmative to negative responses for each of the HBV-related interventions her child may have received. The relationship between asserted knowledge, actions taken and maternal demographics were assessed.
RESULTS: A total of 351 mothers with 627 children born in or after 1992 were included. Median age at enrollment was 39.8 years. Mothers were mostly foreign-born with the largest percentage from Asia (73.4%) and Africa (11.7%). Of the 627 children, 94.5% had mothers who asserted that they knew whether their child had received HBIG or HBV vaccine at birth, for 88.8% of the children, their mothers indicated that they knew if their child was tested for HBV and for 84.5% of children, their mothers knew if the child was diagnosed with HBV infection. Among children whose mothers asserted knowledge of their HBV management, 95.3% were reported to have received HBIG or HBV vaccine, 83.4% of children were said to have been tested for HBV, and 4.8% of children were said to have been diagnosed with HBV. Younger maternal age was the only factor significantly associated with higher percentage of children for whom mothers reported knowledge of testing (p=0.02) or diagnosis of HBV (p=0.02).
CONCLUSIONS: While high percentages of North American children had mothers asserting knowledge of HBV prophylaxis and testing, knowledge gaps remain, with mothers of 5.5-15.5% of children lacking knowledge of key components of the HBV prevention and diagnosis in the perinatal setting. Targeted education of HBsAg-positive mothers may aid in closing this gap and reducing vertical transmission
HST Morphologies of z ~ 2 Dust-Obscured Galaxies II: Bump Sources
We present Hubble Space Telescope (HST) imaging of 22 ultra-luminous infrared
galaxies (ULIRGs) at z~2 with extremely red R-[24] colors (called dust-obscured
galaxies, or DOGs) which have a local maximum in their spectral energy
distribution (SED) at rest-frame 1.6um associated with stellar emission. These
sources, which we call "bump DOGs", have star-formation rates of 400-4000
Msun/yr and have redshifts derived from mid-IR spectra which show strong
polycyclic aromatic hydrocarbon emission --- a sign of vigorous on-going
star-formation. Using a uniform morphological analysis, we look for
quantifiable differences between bump DOGs, power-law DOGs (Spitzer-selected
ULIRGs with mid-IR SEDs dominated by a power-law and spectral features that are
more typical of obscured active galactic nuclei than starbursts),
sub-millimeter selected galaxies (SMGs), and other less-reddened ULIRGs from
the Spitzer extragalactic First Look Survey (XFLS). Bump DOGs are larger than
power-law DOGs (median Petrosian radius of 8.4 +/- 2.7 kpc vs. 5.5 +/- 2.3 kpc)
and exhibit more diffuse and irregular morphologies (median M_20 of -1.08 +/-
0.05 vs. -1.48 +/- 0.05). These trends are qualitatively consistent with
expectations from simulations of major mergers in which merging systems during
the peak star-formation rate period evolve from M_20 = -1.0 to M_20 = -1.7.
Less obscured ULIRGs (i.e., non-DOGs) tend to have more regular, centrally
peaked, single-object morphologies rather than diffuse and irregular
morphologies. This distinction in morphologies may imply that less obscured
ULIRGs sample the merger near the end of the peak star-formation rate period.
Alternatively, it may indicate that the intense star-formation in these
less-obscured ULIRGs is not the result of a recent major merger.Comment: Accepted to ApJ; 22 pages, 8 Figures, 7 Table
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