889 research outputs found
Astrometric orbits of SB9 stars
Hipparcos Intermediate Astrometric Data (IAD) have been used to derive
astrometric orbital elements for spectroscopic binaries from the newly released
Ninth Catalogue of Spectroscopic Binary Orbits (SB9). Among the 1374 binaries
from SB9 which have an HIP entry, 282 have detectable orbital astrometric
motion (at the 5% significance level). Among those, only 70 have astrometric
orbital elements that are reliably determined (according to specific
statistical tests discussed in the paper), and for the first time for 20
systems, representing a 10% increase relative to the 235 DMSA/O systems already
present in the Hipparcos Double and Multiple Systems Annex.
The detection of the astrometric orbital motion when the Hipparcos IAD are
supplemented by the spectroscopic orbital elements is close to 100% for
binaries with only one visible component, provided that the period is in the 50
- 1000 d range and the parallax is larger than 5 mas. This result is an
interesting testbed to guide the choice of algorithms and statistical tests to
be used in the search for astrometric binaries during the forthcoming ESA Gaia
mission.
Finally, orbital inclinations provided by the present analysis have been used
to derive several astrophysical quantities. For instance, 29 among the 70
systems with reliable astrometric orbital elements involve main sequence stars
for which the companion mass could be derived. Some interesting conclusions may
be drawn from this new set of stellar masses, like the enigmatic nature of the
companion to the Hyades F dwarf HIP 20935. This system has a mass ratio of 0.98
but the companion remains elusive.Comment: Astronomy & Astrophysics, in press (16 pages, 12 figures); also
available at http://www.astro.ulb.ac.be/Html/ps.html#Astrometr
SB9: The Ninth Catalogue of Spectroscopic Binary Orbits
The Ninth Catalogue of Spectroscopic Binary Orbits
(http://sb9.astro.ulb.ac.be) continues the series of compilations of
spectroscopic orbits carried out over the past 35 years by Batten and
collaborators. As of 2004 May 1st, the new Catalogue holds orbits for 2,386
systems. Some essential differences between this catalogue and its predecessors
are outlined and three straightforward applications are presented: (1)
Completeness assessment: period distribution of SB1s and SB2s; (2) Shortest
periods across the H-R diagram; (3) Period-eccentricity relation.Comment: Accepte for publication in A&A, 6 pages, 6 figure
Spectroscopic Orbits for 15 Late-Type Stars
Spectroscopic orbital elements are determined for 15 stars with periods from 8 to 6528 days with six orbits computed for the first time. Improved astrometric orbits are computed for two stars and one new orbit is derived. Visual orbits were previously determined for four stars, four stars are members of multiple systems, and five stars have Hipparcos G designations or have been resolved by speckle interferometry. For the nine binaries with previous spectroscopic orbits, we determine improved or comparable elements. For HD 28271 and HD 200790, our spectroscopic results support the conclusions of previous authors that the large values of their mass functions and lack of detectable secondary spectrum argue for the secondary in each case being a pair of low-mass dwarfs. The orbits given here may be useful in combination with future interferometric and Gaia satellite observations
Spectroscopic Orbits for 15 Late-Type Stars
Spectroscopic orbital elements are determined for 15 stars with periods from 8 to 6528 days with six orbits computed for the first time. Improved astrometric orbits are computed for two stars and one new orbit is derived. Visual orbits were previously determined for four stars, four stars are members of multiple systems, and five stars have Hipparcos G designations or have been resolved by speckle interferometry. For the nine binaries with previous spectroscopic orbits, we determine improved or comparable elements. For HD 28271 and HD 200790, our spectroscopic results support the conclusions of previous authors that the large values of their mass functions and lack of detectable secondary spectrum argue for the secondary in each case being a pair of low-mass dwarfs. The orbits given here may be useful in combination with future interferometric and Gaia satellite observations
Spectroscopic Orbits for Late-type Stars. II
We have determined spectroscopic orbital elements for 13 systems—10 single-lined binaries and three double-lined binaries. For the three binaries with previously published spectroscopic orbits, we have computed improved or comparable elements. While two systems have relatively short periods between 10 and 19 days, the remaining systems have much longer periods ranging from 604 to 9669 days. One of the single-lined systems, HD 142640, shows both short-period and long-period velocity variations and so is triple. For three systems—HD 59380, HD 160933, and HD 161163—we have combined our spectroscopic results with Hipparcos astrometric observations to obtain astrometric orbits. For HD 14802 we have determined a joint orbital solution from spectroscopic velocities and interferometric observations. The orbits given here will be useful in combination with future interferometric and Gaia satellite observations
Photoelectrochemical Behavior of n-Type GaAs(100) Electrodes Coated by a Single Layer of Graphene
Methods for cell-selective analysis of proteome dynamics will facilitate studies of biological processes in multicellular organisms. Here we describe a mutant murine methionyl-tRNA synthetase (designated L274GMmMetRS) that charges the noncanonical amino acid azidonorleucine (Anl) to elongator tRNA^(Met) in hamster (CHO), monkey (COS7), and human (HeLa) cell lines. Proteins made in cells that express the synthetase can be labeled with Anl, tagged with dyes or affinity reagents, and enriched on affinity resin to facilitate identification by mass spectrometry. The method does not require expression of orthogonal tRNAs or depletion of canonical amino acids. Successful labeling of proteins with Anl in several mammalian cell lines demonstrates the utility of L274GMmMetRS as a tool for cell-selective analysis of mammalian protein synthesis
Gaia: Organisation and challenges for the data processing
Gaia is an ambitious space astrometry mission of ESA with a main objective to
map the sky in astrometry and photometry down to a magnitude 20 by the end of
the next decade. While the mission is built and operated by ESA and an
industrial consortium, the data processing is entrusted to a consortium formed
by the scientific community, which was formed in 2006 and formally selected by
ESA one year later. The satellite will downlink around 100 TB of raw telemetry
data over a mission duration of 5 years from which a very complex iterative
processing will lead to the final science output: astrometry with a final
accuracy of a few tens of microarcseconds, epoch photometry in wide and narrow
bands, radial velocity and spectra for the stars brighter than 17 mag. We
discuss the general principles and main difficulties of this very large data
processing and present the organisation of the European Consortium responsible
for its design and implementation.Comment: 7 pages, 2 figures, Proceedings of IAU Symp. 24
Large-scale environments of binary AGB stars probed by Herschel. II: Two companions interacting with the wind of pi1 Gruis
Context. The Mass loss of Evolved StarS (MESS) sample observed with PACS on
board the Herschel Space Observatory revealed that several asymptotic giant
branch (AGB) stars are surrounded by an asymmetric circumstellar envelope (CSE)
whose morphology is most likely caused by the interaction with a stellar
companion. The evolution of AGB stars in binary systems plays a crucial role in
understanding the formation of asymmetries in planetary nebul{\ae} (PNe), but
at present, only a handful of cases are known where the interaction of a
companion with the stellar AGB wind is observed.
Aims. We probe the environment of the very evolved AGB star Gruis on
large and small scales to identify the triggers of the observed asymmetries.
Methods. Observations made with Herschel/PACS at 70 m and 160 m
picture the large-scale environment of Gru. The close surroundings of
the star are probed by interferometric observations from the VLTI/AMBER
archive. An analysis of the proper motion data of Hipparcos and Tycho-2
together with the Hipparcos Intermediate Astrometric Data help identify the
possible cause for the observed asymmetry.
Results. The Herschel/PACS images of Gru show an elliptical CSE whose
properties agree with those derived from a CO map published in the literature.
In addition, an arc east of the star is visible at a distance of
from the primary. This arc is most likely part of an
Archimedean spiral caused by an already known G0V companion that is orbiting
the primary at a projected distance of 460 au with a period of more than 6200
yr. However, the presence of the elliptical CSE, proper motion variations, and
geometric modelling of the VLTI/AMBER observations point towards a third
component in the system, with an orbital period shorter than 10 yr, orbiting
much closer to the primary than the G0V star.Comment: 13 pages, 11 figures, accepted for publication in Astronomy &
Astrophysic
Search for brown-dwarf companions of stars
The discovery of 9 new brown-dwarf candidates orbiting stars in the CORALIE
and HARPS radial-velocity surveys is reported. New CORALIE radial velocities
yielding accurate orbits of 6 previously-known hosts of potential brown-dwarf
companions are presented. Including targets selected from the literature, 33
hosts of potential brown-dwarf companions are examined. Employing innovative
methods, we use the new reduction of the Hipparcos data to fully characterise
the astrometric orbits of 6 objects, revealing M-dwarf companions with masses
between 90 M_Jup and 0.52 M_Sun. Additionally, the masses of two companions can
be restricted to the stellar domain. The companion to HD 137510 is found to be
a brown dwarf. At 95 % confidence, the companion of HD 190228 is also a brown
dwarf. The remaining 23 companions persist as brown-dwarf candidates. Based on
the CORALIE planet-search sample, we obtain an upper limit of 0.6 % for the
frequency of brown-dwarf companions around Sun-like stars. We find that the
companion-mass distribution function is rising at the lower end of the
brown-dwarf mass range, suggesting that in fact we are detecting the high-mass
tail of the planetary distribution.Comment: 24 pages, 21 figures, 10 tables. Accepted for publication in
Astronomy and Astrophysics. Abridged abstrac
Analysis of alpha Centauri AB including seismic constraints
Detailed models of alpha Cen A and B based on new seismological data for
alpha Cen B by Carrier & Bourban (2003) have been computed using the Geneva
evolution code including atomic diffusion. Taking into account the numerous
observational constraints now available for the alpha Cen system, we find a
stellar model which is in good agreement with the astrometric, photometric,
spectroscopic and asteroseismic data. The global parameters of the alpha Cen
system are now firmly constrained to an age of t=6.52+-0.30 Gyr, an initial
helium mass fraction Y_i=0.275+-0.010 and an initial metallicity
(Z/X)_i=0.0434+-0.0020. Thanks to these numerous observational constraints, we
confirm that the mixing-length parameter alpha of the B component is larger
than the one of the A component, as already suggested by many authors (Noels et
al. 1991, Fernandes & Neuforge 1995 and Guenther & Demarque 2000): alpha_B is
about 8% larger than alpha_A (alpha_A=1.83+-0.10 and alpha_B=1.97+-0.10).
Moreover, we show that asteroseismic measurements enable to determine the radii
of both stars with a very high precision (errors smaller than 0.3%). The radii
deduced from seismological data are compatible with the new interferometric
results of Kervella et al. (2003) even if they are slightly larger than the
interferometric radii (differences smaller than 1%).Comment: 13 pages, 9 figures, accepted for publication in A&
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