255 research outputs found
Non-LTE line-formation for CNO
Accurate atomic data have become available in the recent past due to the
demands of astrophysics and fusion research. We report on the impact of such
data on non-LTE line-formation calculations for CNO in early-type stars.
Considerable improvement is achieved by the derivation of consistent results
from practically all available spectroscopic indicators, regardless of
ionization stage or spin system, and the uncertainties in the analyses are
drastically reduced. Moreover, systematic trends are revealed, e.g. an increase
of the NI abundances from previous studies of BA-type supergiants by a factor
of two is indicated. The present work promises stringent observational
constraints on chemical mixing in the course of massive star evolution. First
results on BA-type supergiants in the Galaxy and the Magellanic Clouds are
discussed.Comment: 6 pages, 2 figures; to be published in "CNO in the Universe", ASP
Conf. Series, eds. C. Charbonnel, D. Schaerer & G. Meyne
Blue Supergiants as a Tool for Extragalactic Distances - Theoretical Concepts
Because of their enormous intrinsic brightness blue supergiants are ideal
stellar objects to be studied spectroscopically as individuals in galaxies far
beyond the Local Group. Quantitative spectroscopy by means of efficient
multi-object spectrographs attached to 8m-class telescopes and modern NLTE
model atmosphere techniques allow us to determine not only intrinsic stellar
parameters such as effective temperature, surface gravity, chemical composition
and absolute magnitude but also very accurately interstellar reddening and
extinction. This is a significant advantage compared to classical distance
indicators like Cepheids and RR Lyrae. We describe the spectroscopic
diagnostics of blue supergiants and introduce two concepts to determine
absolute magnitudes. The first one (Wind Momentum -- Luminosity Relationship)
uses the correlation between observed stellar wind momentum and luminosity,
whereas the second one (Flux-weighted Gravity -- Luminosity Relationship)
relies only on the determination of effective temperature and surface gravity
to yield an accurate estimate of absolute magnitude. We discuss the potential
of these two methods.Comment: 25 pages, 16 figures; Invited review at the International Workshop on
"Stellar Candles for the Extragalactic Distance Scale", held in Concepcion,
Chile, December 9-11, 2002, to be published in: "Stellar Candles", Lecture
Notes in Physics, Springer-Verla
The influence of galaxy surface brightness on the mass-metallicity relation
We study the effect of surface brightness on the mass-metallicity relation
using nearby galaxies whose gas content and metallicity profiles are available.
Previous studies using fiber spectra indicated that lower surface brightness
galaxies have systematically lower metallicity for their stellar mass, but the
results were uncertain because of aperture effect. With stellar masses and
surface brightnesses measured at WISE W1 and W2 bands, we re-investigate the
surface brightness dependence with spatially-resolved metallicity profiles and
find the similar result. We further demonstrate that the systematical
difference cannot be explained by the gas content of galaxies. For two galaxies
with similar stellar and gas masses, the one with lower surface brightness
tends to have lower metallicity. Using chemical evolution models, we
investigate the inflow and outflow properties of galaxies of different masses
and surface brightnesses. We find that, on average, high mass galaxies have
lower inflow and outflow rates relative to star formation rate. On the other
hand, lower surface brightness galaxies experience stronger inflow than higher
surface brightness galaxies of similar mass. The surface brightness effect is
more significant for low mass galaxies. We discuss implications on the
different inflow properties between low and high surface brightness galaxies,
including star formation efficiency, environment and mass assembly history
The Arches Cluster Mass Function
We have analyzed H and K_s-band images of the Arches cluster obtained using
the NIRC2 instrument on Keck with the laser guide star adaptive optics (LGS AO)
system. With the help of the LGS AO system, we were able to obtain the deepest
ever photometry for this cluster and its neighborhood, and derive the
background-subtracted present-day mass function (PDMF) down to 1.3 Msun for the
5 arcsec-9 arcsec annulus of the cluster. We find that the previously reported
turnover at 6 Msun is simply due to a local bump in the mass function (MF), and
that the MF continues to increase down to our 50 % completeness limit (1.3
Msun) with a power-law exponent of Gamma = -0.91 for the mass range of 1.3 <
M/Msun < 50. Our numerical calculations for the evolution of the Arches cluster
show that the Gamma values for our annulus increase by 0.1-0.2 during the
lifetime of the cluster, and thus suggest that the Arches cluster initially had
Gamma of -1.0 ~ -1.1, which is only slightly shallower than the Salpeter value.Comment: Accepted for publication in ApJ
The growth history of local M33-mass bulgeless spiral galaxies
NGC7793, NGC300, M33 and NGC2403 are four nearby undisturbed and bulgeless
low-mass spiral galaxies with similar morphology and stellar mass. They are
ideal laboratories to study disc formation scenarios and stellar mass growth
histories. We construct a simple chemical evolution model by assuming that
discs grow gradually with continuous metal-free gas infall and metal-enriched
gas outflow. By means of the classical methodology, applied to the
model predictions, the best combination of free parameters capable of
reproducing the corresponding present-day observations is determined, i.e. the
radial dependence of the infall timescale ( is the disc scale-length) and the gas outflow efficiency
. The model results are in excellent agreement with the
general predictions of the inside-out growth scenario for the evolution of
spiral galaxies. About 80\% of the stellar mass of NGC\,7793 is assembled
within the last 8\,Gyr and 40\% within the last 4\,Gyr. By comparing the
best-fitting model results of the three other galaxies we obtain similar
results, 72\% (NGC300), 66\% (NGC2403) and 79\% (M33) stellar mass were
assembled within the past (i.e. ). These four disc
galaxies simultaneously increase their sizes and stellar masses as time goes by
and they grow in size at times the rate at which they grow in
mass. The scale-lengths of these four discs are now 20\% -- 25\% larger than at
. Our best-fitting model predicted the stellar mass-metallicity
relation and the metallicity gradients, constrained by the observed
metallicities from HII-regions emission line analysis, agree well with the
observations measured from individual massive red and blue supergiant stars and
population synthesis of SDSS galaxies.Comment: 12 pages, 10 figures, accepted for publication in the A&
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