626 research outputs found
The PASTEL catalogue of stellar parameters
The PASTEL catalogue is an update of the [Fe/H] catalogue, published in 1997
and 2001. It is a bibliographical compilation of stellar atmospheric parameters
providing (Teff,logg,[Fe/H]) determinations obtained from the analysis of high
resolution, high signal-to-noise spectra, carried out with model atmospheres.
PASTEL also provides determinations of the one parameter Teff based on various
methods. It is aimed in the future to provide also homogenized atmospheric
parameters and elemental abundances, radial and rotational velocities. A web
interface has been created to query the catalogue on elaborated criteria.
PASTEL is also distributed through the CDS database and VizieR. To make it as
complete as possible, the main journals have been surveyed, as well as the CDS
database, to find relevant publications. The catalogue is regularly updated
with new determinations found in the literature. As of Febuary 2010, PASTEL
includes 30151 determinations of either Teff or (Teff,logg,[Fe/H]) for 16649
different stars corresponding to 865 bibliographical references. Nearly 6000
stars have a determination of the three parameters (Teff,logg,[Fe/H]) with a
high quality spectroscopic metallicity.Comment: 5 pages, accepted for publication in A&A. The PASTEL catalogue can be
queried at http://pastel.obs.u-bordeaux1.fr/ or
http://vizier.u-strasbg.fr/viz-bin/VizieR?-source=B/paste
Catalogue of [Fe/H] determinations for FGK stars : 2001 edition
The catalogue presented here is a compilation of published atmospheric
parameters (Teff, logg, [Fe/H]) obtained from high resolution, high
signal-to-noise spectroscopic observations. This new edition has changed
compared to the five previous versions. It is now restricted to intermediate
and low mass stars (F, G and K stars). It contains 6354 determinations of
(Teff, logg, [Fe/H]) for 3356 stars, including 909 stars in 79 stellar systems.
The literature is complete between January 1980 and December 2000 and includes
378 references. The catalogue is made up of two tables, one for field stars and
one for stars in galactic associations, open and globular clusters and external
galaxies. The catalogue is distributed through the CDS database. Access to the
catalogue with cross-identification to other sets of data is also possible with
VizieR (Ochsenbein et al. 2000).Comment: 5 pages, 4 figures, published in A&A 373, 159. Data can be fetched
directly from: ftp://cdsarc.u-strasbg.fr/cats/III/22
A catalogue of [Fe/H] determinations : 1996 edition
The Catalogue of [Fe/H] determinations has been updated and now includes 5946
determinations for 3247 stars (with 751 stars in 84 associations, clusters or
galaxies). The 700 bibliographical references are complete up to December 1995
and refer only to [Fe/H] determinations obtained from high-resolution
spectroscopic observations. The Catalogue also gives the spectral type, the
object type, the visual magnitude and colour, as well as determinations of the
effective temperature and gravity for each star, when available. In this paper,
we comment on the Catalogue, the parameters listed in it, its stellar
content,and the precautions that should be observed when using it. The full
Catalogue is only available in electronic form at the CDS or upon request
([email protected]).Comment: 7 pages (Latex, A&A style), 4 PostScript figures, to be published in
A&A Supplement Series in jul
Searching for Planets in the Hyades. I. The Keck Radial Velocity Survey
We describe a high-precision radial velocity search for jovian-mass
companions to main sequence stars in the Hyades star cluster. The Hyades
provides an extremely well controlled sample of stars of the same age, the same
metallicity, and a common birth and early dynamical environment. This sample
allows us to explore the dependence of the process of planet formation on only
a single independent variable: the stellar mass. In this paper we describe the
survey and summarize results for the first five years.Comment: 8 pages, 3 figures; To appear in the July 2002 issue of The
Astronomical Journa
A Study of the B-V Colour Temperature Relation
We attempt to construct a B-V colour temperature relation for stars in the
least model dependent way employing the best modern data. The fit we obtained
with the form Teff = Teff((B-V)0,[Fe/H],log g) is well constrained and a number
of tests show the consistency of the procedures for the fit. Our relation
covers from F0 to K5 stars with metallicity [Fe/H] = -1.5 to +0.3 for both
dwarfs and giants. The residual of the fit is 66 K, which is consistent with
what are expected from the quality of the present data. Metallicity and surface
gravity effects are well separated from the colour dependence. Dwarfs and
giants match well in a single family of fit, differing only in log g. The fit
also detects the Galactic extinction correction for nearby stars with the
amount E(B-V) = 0.26 +/-0.03 mag/kpc. Taking the newly obtained relation as a
reference we examine a number of B-V colour temperature relations and
atmosphere models available in the literature. We show the presence of a
systematic error in the colour temperature relation from synthetic calculations
of model atmospheres; the systematic error across K0 to K5 dwarfs is 0.04-0.05
mag in B-V, which means 0.25-0.3 mag in Mv for the K star range. We also argue
for the error in the temperature scale used in currently popular stellar
population synthesis models; synthetic colours from these models are somewhat
too blue for aged elliptical galaxies. We derive the colour index of the sun
(B-V)sun = 0.627 +/-0.018, and discuss that redder colours (e.g., 0.66-0.67)
often quoted in the literature are incompatible with the colour-temperature
relation.Comment: AASLaTeX (aaspp4.sty),36 pages (13 figures included), submitted to
Astronomical Journal, replaced (typo in author name
First High Contrast Imaging Using a Gaussian Aperture Pupil Mask
Placing a pupil mask with a gaussian aperture into the optical train of
current telescopes represents a way to attain high contrast imaging that
potentially improves contrast by orders of magnitude compared to current
techniques. We present here the first observations ever using a gaussian
aperture pupil mask (GAPM) on the Penn State near-IR Imager and Spectrograph
(PIRIS) at the Mt. Wilson 100 telescope. Two nearby stars were
observed, Eridani and Her A. A faint companion was detected
around Her A, confirming it as a proper motion companion. Furthermore,
the observed H and K magnitudes of the companion were used to constrain its
nature. No companions or faint structure were observed for Eridani.
We found that our observations with the GAPM achieved contrast levels similar
to our coronographic images, without blocking light from the central star. The
mask's performance also nearly reached sensitivities reported for other ground
based adaptive optics coronographs and deep HST images, but did not reach
theoretically predicted contrast levels. We outline ways that could improve the
performance of the GAPM by an order of magnitude or more.Comment: 8 pages, 4 figures, accepted by ApJ letter
Survey for Transiting Extrasolar Planets in Stellar Systems. II. Spectrophotometry and Metallicities of Open Clusters
We present metallicity estimates for seven open clusters based on
spectrophotometric indices from moderate-resolution spectroscopy. Observations
of field giants of known metallicity provide a correlation between the
spectroscopic indices and the metallicity of open cluster giants. We use \chi^2
analysis to fit the relation of spectrophotometric indices to metallicity in
field giants. The resulting function allows an estimate of the target-cluster
giants' metallicities with an error in the method of \pm0.08 dex. We derive the
following metallicities for the seven open clusters: NGC 1245,
[m/H]=-0.14\pm0.04; NGC 2099, [m/H]=+0.05\pm0.05; NGC 2324, [m/H]=-0.06\pm0.04;
NGC 2539, [m/H]=-0.04\pm0.03; NGC 2682 (M67), [m/H]=-0.05\pm0.02; NGC 6705,
[m/H]=+0.14\pm0.08; NGC 6819, [m/H]=-0.07\pm0.12. These metallicity estimates
will be useful in planning future extra-solar planet transit searches since
planets may form more readily in metal-rich environments.Comment: 38 pages, including 12 figures. Accepted for publication in A
The Structure of Stellar Coronae in Active Binary Systems
A survey of 28 stars using EUV spectra has been conducted to establish the
structure of stellar coronae in active binary systems from the EMD, electron
densities, and scale sizes. Observations obtained by the EUVE during 9 years of
operation are included for the stars in the sample. EUVE data allow a
continuous EMD to be constructed in the range log T~5.6-7.4, using iron
emission lines. These data are complemented with IUE observations to model the
lower temperature range. Inspection of the EMD shows an outstanding narrow
enhancement, or ``bump'' peaking around log T~6.9 in 25 of the stars, defining
a fundamental coronal structure. The emission measure per unit stellar area
decreases with increasing orbital (or photometric) periods of the target stars;
stars in binaries generally have more material at coronal temperatures than
slowly rotating single stars. High electron densities (Ne>10^12 cm^-3) are
derived at ~10 MK for some targets, implying small emitting volumes. The
observations suggest the magnetic stellar coronae of these stars are consistent
with two basic classes of magnetic loops: solar-like loops with maximum
temperature around log T~6.3 and lower electron densities (Ne>10^9-10.5), and
hotter loops peaking around log T~6.9 with higher electron densities
(Ne>10^12). For the most active stars, material exists at much higher
temperatures (log T>6.9) as well. However, current ab initio stellar loop
models cannot reproduce such a configuration. Analysis of the light curves of
these systems reveals signatures of rotation of coronal material, as well as
apparent seasonal changes in the activity levels.Comment: 45 pages, 9 figures (with 20 eps files). Accepted for its publication
in ApJ
The r-Process Enriched Low Metallicity Giant HD 115444
New high resolution, very high signal-to-noise spectra of ultra-metal-poor
(UMP) giant stars HD 115444 and HD 122563 have been gathered with the
High-Resolution Echelle Spectrometer of the McDonald Observatory 2.7m
Telescope. With these spectra, line identification and model atmosphere
analyses have been conducted, emphasizing the neutron-capture elements. Twenty
elements with Z > 30 have been identified in the spectrum of HD 115444. This
star is known to have overabundances of the neutron-capture elements, but it
has lacked a detailed analysis necessary to compare with nucleosynthesis
predictions. The new study features a line-by-line differential abundance
comparison of HD 115444 with the bright, well-studied halo giant HD 122563. For
HD 115444, the overall metallicity is [Fe/H]~ -3.0. The abundances of the light
and iron-peak elements generally show the same pattern as other UMP stars (e.g.
overdeficiencies of manganese and chromium, overabundances of cobalt), but the
differential analysis indicates several nucleosynthesis signatures that are
unique to each star.Comment: To Appear in the Astrophysical Journa
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