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J/A+A/506/213       B6-B9.5 stars abundance analysis         (Niemczura+, 2009)

Abundance analysis of prime B-type targets for asteroseismology. II. B6-B9.5 stars in the field of view of the CoRoT. Niemczura E., Morel T., Aerts C. <Astron. Astrophys. 506, 213 (2009)> =2009A&A...506..213N
ADC_Keywords: Stars, early-type ; Stars, B-type ; Abundances ; Rotational velocities Keywords: stars: abundances - stars: atmospheres - stars: chemically peculiar Abstract: The CoRoT satellite is collecting precise time-resolved photometry for tens of asteroseismology targets. To ensure a correct interpretation of the CoRoT data, the atmospheric parameters, chemical compositions, and rotational velocities of the stars must be determined. The main goal of the ground-based seismology support program for the CoRoT mission was to obtain photometric and spectroscopic data for stars in the fields monitored by the satellite. These ground-based observations were collected in the GAUDI archive. High-resolution spectra of more than 200 B-type stars are available in this database, and about 45% of them is analysed here. To derive the effective temperature of the stars, we used photometric indices. Surface gravities were obtained by comparing observed and theoretical Balmer line profiles. To determine the chemical abundances and rotational velocities, we used a spectrum synthesis method, which consisted of comparing the observed spectrum with theoretical ones based on the assumption of LTE. Atmospheric parameters, chemical abundances, and rotational velocities were determined for 89 late-B stars. The dominant species in their spectra are iron-peak elements. The average Fe abundance is 7.24±0.45dex. The average rotational velocity is 126km/s, but there are 13 and 20 stars with low and moderate Vsini values, respectively. The analysis of this sample of 89 late B-type stars reveals many chemically peculiar (CP) stars. Some of them were previously known, but at least 9 new CP candidates, among which at least two HgMn stars, are identified in our study. These CP stars as a group exhibit Vsini values lower than the stars with normal surface chemical composition. Description: The observational material consists of the high-resolution (R∼40000-50000) spectroscopic observations of B-type stars obtained with the ELODIE and FEROS spectrographs. The ELODIE spectrograph was attached to the 1.93m telescope at the Observatoire de Haute-Provence, France. The FEROS spectrograph was installed on the 1.52m and 2.2m telescopes at La Silla, Chile. Both instruments are cross-dispersed, fibre-fed echelle spectrographs. Typical signal-to-noise ratios of the spectra range from 100 to 150 at 550nm. The wavelength intervals covered are 390-680nm and 380-910nm for ELODIE and FEROS, respectively. In our initial sample, we have 160 FEROS spectra and 62 ELODIE spectra of B-type stars. Only the spectroscopic observations of the B6-B9.5 stars available in the GAUDI archive are analysed in this paper. We also excluded Be stars, supergiants and spectroscopic binaries for which the lines of two stars were visible in the spectra. Basic information about the analysed stars, including spectral type, name of the spectrograph, observation date in UT, V magnitude, interstellar reddening, indications of binarity, and abundance determinations in the literature are given in Table 1. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table1.dat 137 93 Description of the analysed stars and their observations refs.dat 82 31 References of table1 table2.dat 337 89 Atmospheric parameters, abundances of chemical elements and rotation velocities of all analysed stars table3.dat 33 21 Average abundances for the entire sample and the non-CP stars
Byte-by-byte Description of file: table1.dat
Bytes Format Units Label Explanations
1- 6 I6 --- HD HD number 8- 15 A8 --- SpType MK spectral type 17- 22 A6 --- Inst Spectrograph 24- 33 A10 "YYYY/DD/MM" Obs.date Observation date 35- 42 A8 "h:m:s" Obs.time Obsertation time of the beginning of the exposure 44- 47 F4.2 mag Vmag ? V magnitude 49- 52 F4.2 mag E(B-V) ? Interstellar extinction 54- 74 A21 --- Bin Informations about binarity, in refs.dat file 76-137 A62 --- Abun Previous abundance analysis, in refs.dat file
Byte-by-byte Description of file: refs.dat
Bytes Format Units Label Explanations
1- 2 I2 --- Ref Reference number 4- 22 A19 --- BibCode BibCode 24- 43 A20 --- Aut Author's name 47- 82 A36 --- Com Comments
Byte-by-byte Description of file: table2.dat
Bytes Format Units Label Explanations
1- 6 I6 --- HD HD number 8- 12 I5 K Teff Effective temperature 14- 16 F3.1 [cm/s2] logg Surface gravity 18- 20 I3 km/s Vsini Rotational velocity 22- 26 F5.2 [-] He ?=- He abundance log(epsilon_He) 28- 31 F4.2 [-] C ?=- C abundance log(epsilon_C) 33- 36 F4.2 [-] N ?=- N abundance log(epsilon_N) 38- 41 F4.2 [-] O ?=- O abundance log(epsilon_O) 43- 46 F4.2 [-] Ne ?=- Ne abundance log(epsilon_Ne) 48- 51 F4.2 [-] Mg ?=- Mg abundance log(epsilon_Mg) 53- 56 F4.2 [-] Al ?=- Al abundance log(epsilon_Al) 58- 61 F4.2 [-] Si ?=- Si abundance log(epsilon_Si) 63- 66 F4.2 [-] P ?=- P abundance log(epsilon_P) 68- 71 F4.2 [-] S ?=- S abundance log(epsilon_S) 73- 76 F4.2 [-] Cl ?=- Cl abundance log(epsilon_Cl) 78- 81 F4.2 [-] Ca ?=- Ca abundance log(epsilon_Ca) 83- 86 F4.2 [-] Sc ?=- Sc abundance log(epsilon_Sc) 88- 91 F4.2 [-] Ti ?=- Ti abundance log(epsilon_Ti) 93- 96 F4.2 [-] V ?=- V abundance log(epsilon_V) 98-101 F4.2 [-] Cr ?=- Cr abundance log(epsilon_Cr) 103-106 F4.2 [-] Mn ?=- Mn abundance log(epsilon_Mn) 108-111 F4.2 [-] Fe ?=- Fe abundance log(epsilon_Fe) 113-116 F4.2 [-] Ni ?=- Ni abundance log(epsilon_Ni) 118-121 F4.2 [-] Ga ?=- Ga abundance log(epsilon_Ga) 123-126 F4.2 [-] Sr ?=- Sr abundance log(epsilon_Sr) 128-131 F4.2 [-] Y ?=- Y abundance log(epsilon_Y) 133-136 F4.2 [-] Zr ?=- Zr abundance log(epsilon_Zr) 138-141 F4.2 [-] Ba ?=- Ba abundance log(epsilon_Ba) 143-144 I2 km/s e_Vsini The error of Vsini 146-149 F4.2 [-] e_He ?=- The error of He abundance 151-154 F4.2 [-] e_C ?=- The error of C abundance 156-159 F4.2 [-] e_N ?=- The error of N abundance 161-164 F4.2 [-] e_O ?=- The error of O abundance 166-169 F4.2 [-] e_Ne ?=- The error of Ne abundance 171-174 F4.2 [-] e_Mg ?=- The error of Mg abundance 176-179 F4.2 [-] e_Al ?=- The error of Al abundance 181-184 F4.2 [-] e_Si ?=- The error of Si abundance 186-189 F4.2 [-] e_P ?=- The error of P abundance 191-194 F4.2 [-] e_S ?=- The error of S abundance 196-199 F4.2 [-] e_Cl ?=- The error of Cl abundance 201-204 F4.2 [-] e_Ca ?=- The error of Ca abundance 206-209 F4.2 [-] e_Sc ?=- The error of Sc abundance 211-214 F4.2 [-] e_Ti ?=- The error of Ti abundance 216-219 F4.2 [-] e_V ?=- The error of V abundance 221-224 F4.2 [-] e_Cr ?=- The error of Cr abundance 226-229 F4.2 [-] e_Mn ?=- The error of Mn abundance 231-234 F4.2 [-] e_Fe ?=- The error of Fe abundance 236-239 F4.2 [-] e_Ni ?=- The error of Ni abundance 241-244 F4.2 [-] e_Ga ?=- The error of Ga abundance 246-249 F4.2 [-] e_Sr ?=- The error of Sr abundance 251-254 F4.2 [-] e_Y ?=- The error of Y abundance 256-259 F4.2 [-] e_Zr ?=- The error of Zr abundance 261-264 F4.2 [-] e_Ba ?=- The error of Ba abundance 266-267 I2 --- o_He ?=- Number of lines for He abundance determination 269-270 I2 --- o_C ?=- Number of lines for C abundance determination 272-273 I2 --- o_N ?=- Number of lines for N abundance determination 275-276 I2 --- o_O ?=- Number of lines for O abundance determination 278-279 I2 --- o_Ne ?=- Number of lines for Ne abundance determination 281-282 I2 --- o_Mg ?=- Number of lines for Mg abundance determination 284-285 I2 --- o_Al ?=- Number of lines for AL abundance determination 287-288 I2 --- o_Si ?=- Number of lines for Si abundance determination 290-291 I2 --- o_P ?=- Number of lines for P abundance determination 293-294 I2 --- o_S ?=- Number of lines for S abundance determination 296-297 I2 --- o_Cl ?=- Number of lines for Cl abundance determination 299-300 I2 --- o_Ca ?=- Number of lines for Ca abundance determination 302-303 I2 --- o_Sc ?=- Number of lines for Sc abundance determination 305-306 I2 --- o_Ti ?=- Number of lines for Ti abundance determination 308-309 I2 --- o_V ?=- Number of lines for V abundance determination 311-312 I2 --- o_Cr ?=- Number of lines for Cr abundance determination 314-315 I2 --- o_Mn ?=- Number of lines for Mn abundance determination 317-319 I3 --- o_Fe ?=- Number of lines for Fe abundance determination 321-322 I2 --- o_Ni ?=- Number of lines for Ni abundance determination 324-325 I2 --- o_Ga ?=- Number of lines for Ga abundance determination 327-328 I2 --- o_Sr ?=- Number of lines for Sr abundance determination 330-331 I2 --- o_Y ?=- Number of lines for Y abundance determination 333-334 I2 --- o_Zr ?=- Number of lines for Zr abundance determination 336-337 I2 --- o_Ba ?=- Number of lines for Ba abundance determination
Byte-by-byte Description of file: table3.dat
Bytes Format Units Label Explanations
1- 2 A2 --- El Name of the element 5- 9 F5.2 [-] log(eps)all Average abundance for the entire sample 12- 15 F4.2 [-] e_log(eps)all Standard deviation 17- 21 F5.2 [-] log(eps)nor Average abundance for non-CP stars 24- 27 F4.2 [-] e_log(eps)nor Standard deviations 29- 33 F5.2 [-] log(eps)sun Abundance of the Sun (1)
Note (1): The solar abundances are taken from Grevesse et al. (2007SSRv..130..105G)
Acknowledgements: Ewa Niemczura, eniem(at)astro.uni.wroc.pl References: Morel et al., Paper I 2006A&A...457..651M, Cat. J/A+A/457/651
(End) Patricia Vannier [CDS] 27-Oct-2009
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