263 research outputs found
The Contribution of TP-AGB and RHeB Stars to the Near-IR Luminosity of Local Galaxies: Implications for Stellar Mass Measurements of High Redshift Galaxies
Using high spatial resolution HST WFC3 and ACS imaging of resolved stellar
populations, we constrain the contribution of thermally-pulsing asymptotic
giant branch (TP-AGB) stars and red helium burning (RHeB) stars to the 1.6 um
near-infrared (NIR) luminosities of 23 nearby galaxies. The TP-AGB phase
contributes as much as 17% of the integrated F160W flux, even when the red
giant branch is well populated. The RHeB population contribution can match or
even exceed the TP-AGB contribution, providing as much as 21% of the integrated
F160W light. The NIR mass-to-light (M/L) ratio should therefore be expected to
vary significantly due to fluctuations in the star formation rate over
timescales from 25 Myr to several Gyr. We compare our observational results to
predictions based on optically derived star formation histories and stellar
population synthesis (SPS) models, including models based on the Padova
isochrones (used in popular SPS programs). The SPS models generally reproduce
the expected numbers of TP-AGB stars in the sample. The same SPS models,
however, give a larger discrepancy in the F160W flux contribution from the
TP-AGB stars, over-predicting the flux by a weighted mean factor of 2.3 +/-0.8.
This larger offset is driven by the prediction of modest numbers of high
luminosity TP-AGB stars at young (<300 Myrs) ages. The best-fit SPS models
simultaneously tend to under-predict the numbers and fluxes of stars on the
RHeB sequence, typically by a factor of 2.0+/-0.6 for galaxies with significant
numbers of RHeBs. Coincidentally, over-prediction of the TP-AGB and
under-prediction of the RHeBs result in a NIR M/L ratio largely unchanged for a
rapid star formation rate. However, the NIR-to-optical flux ratio of galaxies
could be significantly smaller than AGB-rich models would predict, an outcome
that has been observed in some intermediate redshift post-starburst galaxies.
(Abridged)Comment: 28 Pages, 12 Figures, 5 Tables, Accepted for Publication in the
Astrophysical Journa
Runaway dilaton models: improved constraints from the full cosmological evolution
One of the few firm predictions of string theory is the existence of a
massless scalar field coupled to gravity, the dilaton. In its presence, the
value of the fundamental constants of the universe, such as the fine-structure
constant, will vary with the time-dependent vacuum expectation value of this
field, in direct violation of the Einstein Equivalence Principle. The
\emph{runaway dilaton} proposed by Damour, Piazza, and Veneziano provides a
physically motivated cosmological scenario which reconciles the existence of a
massless dilaton with observations, while still providing non-standard and
testable predictions. Furthermore, the field can provide a natural candidate
for dynamical dark energy. While this model has been previously constrained
from local laboratory experiments and low-redshift observations, we provide
here the first full self-consistent constraints, also including high redshift
data, in particular from the cosmic microwave background. We consider various
possible scenarios in which the field could act as quintessence. Despite the
wider parameter space, we make use of recent observational progress to
significantly improve constraints on the model's coupling parameters, showing
that order unity couplings (which would be natural in string theory) are ruled
out.Comment: Published in Phys. Rev.
Resolved Near-infrared Stellar Populations in Nearby Galaxies
We present near-infrared (NIR) color-magnitude diagrams (CMDs) for the resolved stellar populations within 26 fields of 23 nearby galaxies (âČ 4 Mpc), based on images in the F110W and F160W filters taken with the Wide-Field Camera 3 (WFC3) on the Hubble Space Telescope (HST). The CMDs are measured in regions spanning a wide range of star formation histories, including both old dormant and young star-forming populations. We match key NIR CMD features with their counterparts in more familiar optical CMDs, and identify the red core helium-burning (RHeB) sequence as a significant contributor to the NIR flux in stellar populations younger than a few 100 Myr old. The strength of this feature suggests that the NIR mass-to-light ratio can vary significantly on short timescales in star-forming systems. The NIR luminosity of star-forming galaxies is therefore not necessarily proportional to the stellar mass. We note that these individual RHeB stars may also be misidentified as old stellar clusters in images of nearby galaxies. For older stellar populations, we discuss the CMD location of asymptotic giant branch (AGB) stars in the HST filter set and explore the separation of AGB subpopulations using a combination of optical and NIR colors. We empirically calibrate the magnitude of the NIR tip of the red giant branch in F160W as a function of color, allowing future observations in this widely adopted filter set to be used for distance measurements. We also analyze the properties of the NIR red giant branch (RGB) as a function of metallicity, showing a clear trend between NIR RGB color and metallicity. However, based on the current study, it appears unlikely that the slope of the NIR RGB can be used as an effective metallicity indicator in extragalactic systems with comparable data. Finally, we highlight issues with scattered light in the WFC3, which becomes significant for exposures taken close to a bright Earth limb
News from the Swampland -- Constraining string theory with astrophysics and cosmology
Our current best guess for a unified theory of gravitation and quantum field
theory (string theory) generically predicts a set of requirements for a
consistently quantized theory, the Swampland criteria. Refined versions of
these criteria have recently been shown to be in mild tension with cosmological
observations. We summarize the status of the current impact of and constraints
on the Swampland conjectures from cosmology, and subject a variety of dark
energy quintessence models to recently released cosmological datasets. We find
that instead of tightening the tension, the new data allows for slightly more
freedom in the Swampland criteria. We further demonstrate that if there is no
theoretical argument made to prevent interactions of the moduli fields with the
electromagnetic sector, a novel fine-tuning argument arises from the extremely
tight current constraints on such interactions. Finally, we conclude with a
cautionary tale on model-independent reconstructions of the Swampland criteria
from expansion rate data.Comment: 35 pages, 20 figures, 4 tables. All comments are welcome! [v2: Added
citations, corrected eq. 2.6
The Panchromatic Hubble Andromeda Treasury XX: The Disk of M31 is Thick
We present a new approach to measuring the thickness of a partially face-on
stellar disk, using dust geometry. In a moderately-inclined disk galaxy, the
fraction of reddened stars is expected to be 50% everywhere, assuming that dust
lies in a thin midplane. In a thickened disk, however, a wide range of radii
project onto the line of sight. Assuming stellar density declines with radius,
this geometrical projection leads to differences in the numbers of stars on the
near and far sides of the thin dust layer. The fraction of reddened stars will
thus differ from the 50% prediction, with a deviation that becomes larger for
puffier disks. We map the fraction of reddened red giant branch (RGB) stars
across M31, which shows prominent dust lanes on only one side of the major
axis. The fraction of reddened stars varies systematically from 20% to 80%,
which requires that these stars have an exponential scale height h_z that is
0.14+/-0.015 times the exponential scale length (h_r~5.5kpc). M31's RGB stars
must therefore have h_z=770+/-80pc, which is far thicker than the Milky Way's
thin disk, but comparable to its thick disk. The lack of a significant thin
disk in M31 is unexpected, but consistent with its interaction history and high
disk velocity dispersion. We suggest that asymmetric reddening be used as a
generic criteria for identifying ``thick disk'' dominated systems, and discuss
prospects for future 3-dimensional tomographic mapping of the gas and stars in
M31.Comment: 22 pages. Accepted to the Astrophysical Journa
The Panchromatic Hubble Andromeda Treasury I: Bright UV Stars in the Bulge of M31
As part of the Panchromatic Hubble Andromeda Treasury (PHAT) multi-cycle
program, we observed a 12' \times 6.5' area of the bulge of M31 with the
WFC3/UVIS filters F275W and F336W. From these data we have assembled a sample
of \sim4000 UV-bright, old stars, vastly larger than previously available. We
use updated Padova stellar evolutionary tracks to classify these hot stars into
three classes: Post-AGB stars (P-AGB), Post-Early AGB (PE-AGB) stars and
AGB-manqu\'e stars. P-AGB stars are the end result of the asymptotic giant
branch (AGB) phase and are expected in a wide range of stellar populations,
whereas PE-AGB and AGB-manqu\'e (together referred to as the hot
post-horizontal branch; HP-HB) stars are the result of insufficient envelope
masses to allow a full AGB phase, and are expected to be particularly prominent
at high helium or {\alpha} abundances when the mass loss on the RGB is high.
Our data support previous claims that most UV-bright sources in the bulge are
likely hot (extreme) horizontal branch stars (EHB) and their progeny. We
construct the first radial profiles of these stellar populations, and show that
they are highly centrally concentrated, even more so than the integrated UV or
optical light. However, we find that this UV-bright population does not
dominate the total UV luminosity at any radius, as we are detecting only the
progeny of the EHB stars that are the likely source of the UVX. We calculate
that only a few percent of MS stars in the central bulge can have gone through
the HP-HB phase and that this percentage decreases strongly with distance from
the center. We also find that the surface density of hot UV-bright stars has
the same radial variation as that of low-mass X-ray binaries. We discuss age,
metallicity, and abundance variations as possible explanations for the observed
radial variation in the UV-bright population.Comment: Accepted for publication in Ap
Infrasound and Gravity Waves Over the Andes Observed by a Pressure Sensor on Board a Stratospheric Balloon
The study of infrasound (acoustic) and gravity waves sources and propagation in the atmosphere of a planet gives us precious insight on atmosphere dynamics, climate, and even internal structure. The implementation of modern pressure sensors with high rate sampling on stratospheric balloons is improving their study. We analyzed the data from the National Aeronautics and Space Administration Ultra Long Duration Balloon mission (16 May to 30 June 2016). Here, we focus on the balloon's transit of the Andes Mountains. We detected gravity waves that are associated to troposphere convective activity and mountain waves. An increase of the horizontal wavelengths from 50 to 70 km with increasing distance to the mountains is favoring the presence of mountain waves. We also report on the detection of infrasounds generated by the mountains in the 0.01â0.1 Hz range with a pressure amplitude increase by a factor 2 relative background signal. Besides, we characterized the decrease of microbaroms power when the balloon was flying away from the ocean coast. These observations suggest, in a way similar to microseisms for seismometers, that microbaroms are the main background noise sources recorded in the stratosphere even far from the ocean sources. Finally, we observed a broadband signal above the Andes, between 0.45 and 2 Hz, probably associated with a thunderstorm. The diversity of geophysical phenomena captured in less than a day of observation stresses the interest of high rate pressure sensors on board long-duration balloon missions
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