2,778 research outputs found
The Variation of Integrated Star IMFs among Galaxies
The integrated galaxial initial mass function (IGIMF) is the relevant
distribution function containing the information on the distribution of stellar
remnants, the number of supernovae and the chemical enrichment history of a
galaxy. Since most stars form in embedded star clusters with different masses
the IGIMF becomes an integral of the assumed (universal or invariant) stellar
IMF over the embedded star-cluster mass function (ECMF). For a range of
reasonable assumptions about the IMF and the ECMF we find the IGIMF to be
steeper (containing fewer massive stars per star) than the stellar IMF, but
below a few Msol it is invariant and identical to the stellar IMF for all
galaxies. However, the steepening sensitively depends on the form of the ECMF
in the low-mass regime. Furthermore, observations indicate a relation between
the star formation rate of a galaxy and the most massive young stellar cluster
in it. The assumption that this cluster mass marks the upper end of a
young-cluster mass function leads to a connection of the star formation rate
and the slope of the IGIMF above a few Msol. The IGIMF varies with the star
formation history of a galaxy. Notably, large variations of the IGIMF are
evident for dE, dIrr and LSB galaxies with a small to modest stellar mass. We
find that for any galaxy the number of supernovae per star (NSNS) is suppressed
relative to that expected for a Salpeter IMF. Dwarf galaxies have a smaller
NSNS compared to massive galaxies. For dwarf galaxies the NSNS varies
substantially depending on the galaxy assembly history and the assumptions made
about the low-mass end of the ECMF. The findings presented here may be of some
consequence for the cosmological evolution of the number of supernovae per
low-mass star and the chemical enrichment of galaxies of different mass.Comment: 27 pages, accepted for publication by Ap
On the Similarity between Cluster and Galactic Stellar Initial Mass Functions
The stellar initial mass functions (IMFs) for the Galactic bulge, the Milky
Way, other galaxies, clusters of galaxies, and the integrated stars in the
Universe are composites from countless individual IMFs in star clusters and
associations where stars form. These galaxy-scale IMFs, reviewed in detail
here, are not steeper than the cluster IMFs except in rare cases. This is true
even though low mass clusters generally outnumber high mass clusters and the
average maximum stellar mass in a cluster scales with the cluster mass. The
implication is that the mass distribution function for clusters and
associations is a power law with a slope of -2 or shallower. Steeper slopes,
even by a few tenths, upset the observed equality between large and small scale
IMFs. Such a cluster function is expected from the hierarchical nature of star
formation, which also provides independent evidence for the IMF equality when
it is applied on sub-cluster scales. We explain these results with analytical
expressions and Monte Carlo simulations. Star clusters appear to be the relaxed
inner parts of a widespread hierarchy of star formation and cloud structure.
They are defined by their own dynamics rather than pre-existing cloud
boundaries.Comment: 22 pages, 2 figures, ApJ, 648, in press, September 1, 200
Effects of Simple Carbohydrate vs. Carbohydrate-Protein Intake on Glucose Homeostasis Following Intense Exercise
Kluka, J., Baskerville, J., Clifton, K., Fisher, K., Marks, D., Weidner, C., Veerabhadrappa, P. and Braun, W.A. (FACSM), Shippensburg University, Shippensburg, PA.
Purpose: To test the effects of simple carbohydrate (CHO) and the combination of CHO and protein on blood glucose (BG) clearance following intense anaerobic exercise. Methods: Eight members (age = 18.8 ± 1.4 years) of the Shippensburg University Football team participated in the study. On separate test days, subjects were given either a placebo (PL) drink, a CHO drink (74 g CHO in 473 ml), or a carbohydrate-protein (C-PRO) drink (58 g CHO and 16 g PRO in 473 ml), upon completing the exercise bout. Before exercise, baseline measurements were taken for BG and heart rate. The subject then completed a 90-sec modified Wingate protocol (resistance set at 70% of the individual’s Wingate protocol resistance). BG was tested post-exercise, and every ten minutes after ingestion of the solution for 60 min. Results: Neither total revolutions completed (PL = 123.0±5.0; CHO = 126.9±3.9; C-PRO = 125.4±2.8) nor post-exercise BG (mg.dl-1) differed across treatments (PL = 88.6±6.5; CHO = 93.1±4.0; C-PRO = 101.1±4.7). However, CHO elicited the highest (p\u3c0.05) mean BG during recovery and the lowest BG was found in the PL. Conclusion: While matching post-exercise energy intake, C-PRO elicited a smaller BG area than CHO but tended to be larger than that of PL (p=0.052). C-PRO may be a better choice for post-exercise intake if aiming to maintain glucose homeostasis during recovery
New Horizons Solar Wind Around Pluto (SWAP) Observations of the Solar Wind From 11-33 AU
The Solar Wind Around Pluto (SWAP) instrument on NASA's New Horizon Pluto
mission has collected solar wind observations en route from Earth to Pluto, and
these observations continue beyond Pluto. Few missions have explored the solar
wind in the outer heliosphere making this dataset a critical addition to the
field. We created a forward model of SWAP count rates, which includes a
comprehensive instrument response function based on laboratory and flight
calibrations. By fitting the count rates with this model, the proton density
(n), speed (V), and temperature (T) parameters are determined. Comparisons
between SWAP parameters and both propagated 1 AU observations and prior Voyager
2 observations indicate consistency in both the range and mean wind values.
These comparisons as well as our additional findings confirm that small and
midsized solar wind structures are worn down with increasing distance due to
dynamic interaction of parcels of wind with different speed. For instance, the
T-V relationship steepens, as the range in V is limited more than the range in
T with distance. At times the T-V correlation clearly breaks down beyond 20 AU,
which may indicate wind currently expanding and cooling may have an elevated T
reflecting prior heating and compression in the inner heliosphere. The power of
wind parameters at shorter periodicities decreases with distance as the longer
periodicities strengthen. The solar rotation periodicity is present in
temperature beyond 20 AU indicating the observed parcel temperature may reflect
not only current heating or cooling, but also heating occurring closer to the
Sun.Comment: 55 pages, 29 Figures, accepted for publication in The Astrophysical
Journal Supplements (ApJS
The Sparsest Clusters With O Stars
There is much debate on how high-mass star formation varies with environment,
and whether the sparsest star-forming environments are capable of forming
massive stars. To address this issue, we have observed eight apparently
isolated OB stars in the SMC using HST's Advanced Camera for Surveys. Five of
these objects appear as isolated stars, two of which are confirmed to be
runaways. The remaining three objects are found to exist in sparse clusters,
with <10 companion stars revealed, having masses of 1-4 solar mass. Stochastic
effects dominate in these sparse clusters, so we perform Monte Carlo
simulations to explore how our observations fit within the framework of
empirical, galactic cluster properties. We generate clusters using a simplistic
-2 power-law distribution for either the number of stars per cluster (N_*) or
cluster mass (M_cl). These clusters are then populated with stars randomly
chosen from a Kroupa IMF. We find that simulations with cluster lower-mass
limits of M_cl,lo >20 solar mass and N_*,lo >40 match best with observations of
SMC and Galactic OB star populations. We examine the mass ratio of the
second-most massive and most massive stars (m_max,2/m_max), finding that our
observations all exist below the 20th percentile of our simulated clusters.
However, all of our observed clusters lie within the parameter space spanned by
the simulated clusters, although some are in the lowest 5th percentile
frequency. These results suggest that clusters are built stochastically by
randomly sampling stars from a universal IMF with a fixed stellar upper-mass
limit. In particular, we see no evidence to suggest a m_max - M_cl relation.
Our results may be more consistent with core accretion models of star formation
than with competitive accretion models, and they are inconsistent with the
proposed steepening of the integrated galaxy IMF (IGIMF).Comment: 19 pages, 12 figures, accepted for publication in Ap
Protein sets define disease states and predict in vivo effects of drug treatment
Gaining understanding of common complex diseases and their treatments are the main drivers for life sciences. As we show here, comprehensive protein set analyses offer new opportunities to decipher functional molecular networks of diseases and assess the efficacy and side-effects of treatments in vivo. Using mass spectrometry, we quantitatively detected several thousand proteins and observed significant changes in protein pathway (dys-) regulated in diet-induced obesity mice. Analysis of the expression and posttranslational modifications of proteins in various peripheral metabolic target tissues including adipose, heart and liver tissue generated functional insights in the regulation of cell and tissue homeostasis during high fat diet and medication with two anti-diabetic compounds. Protein set analyses singled out pathways for functional characterization, and indicated for example early on potential cardiovascular complication of the diabetes drug rosiglitazone. In vivo protein set detection can provide new avenues for monitoring complex disease processes, and for evaluating preclinical drug candidates
The scale-free character of the cluster mass function and the universality of the stellar IMF
Our recent determination of a Salpeter slope for the IMF in the field of 30
Doradus (Selman and Melnick 2005) appears to be in conflict with simple
probabilistic counting arguments advanced in the past to support observational
claims of a steeper IMF in the LMC field. In this paper we re-examine these
arguments and show by explicit construction that, contrary to these claims, the
field IMF is expected to be exactly the same as the stellar IMF of the clusters
out of which the field was presumably formed. We show that the current data on
the mass distribution of clusters themselves is in excellent agreement with our
model, and is consistent with a single spectrum {\it by number of stars} of the
type with beta between -1.8 and -2.2 down to the smallest clusters
without any preferred mass scale for cluster formation. We also use the random
sampling model to estimate the statistics of the maximal mass star in clusters,
and confirm the discrepancy with observations found by Weidner and Kroupa
(2006). We argue that rather than signaling the violation of the random
sampling model these observations reflect the gravitationally unstable nature
of systems with one very large mass star. We stress the importance of the
random sampling model as a \emph{null hypothesis} whose violation would signal
the presence of interesting physics.Comment: 9 pages emulateap
Intermediate Old Star Clusters in a Young Starburst: The case of NGC 5253
We investigate the star cluster population in the outer parts of the
starburst galaxy NGC 5253 using archive images taken with the Hubble Space
Telescope's Advanced Camera for Surveys. Based on the F415W, F555W, and F814W
photometry ages and masses are estimated for bona-fide star cluster candidates.
We find three potentially massive (\ge 10 \time 10^5 \Msun) star clusters at
ages of order of 1-2 Gyr, implying, if confirmed, a high global star formation
rate in NGC 5253 during that epoch. This result underlines earlier findings
that the current star burst is just one episode in an very active dwarf galaxy.Comment: accepted for publication in MNRAS - The definitive version is (will
be) available at www.blackwell-synergy.co
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