J/A+A/603/A91 VLTS. B-type main-sequence binary systems (Garland+, 2017)
The VLT-FLAMES Tarantula Survey.
XXVII. Physical parameters of B-type main-sequence binary systems in the
Tarantula nebula.
Garland R., Dufton P.L., Evans C.J., Crowther P.A., Howarth I.D.,
de Koter A., de Mink S.E., Grin N.J., N.Langer, Lennon D.J., McEvoy C.M.,
Sana H., Schneider F.R.N., Simon-Diaz S., Taylor W.D., Thompson A.,
Vink J.S.
<Astron. Astrophys. 603, A91 (2017)>
=2017A&A...603A..91G 2017A&A...603A..91G (SIMBAD/NED BibCode)
ADC_Keywords: Magellanic Clouds ; Stars, double and multiple ; Stars, B-type ;
Rotational velocities
Keywords: stars: early-type - stars: abundances - binaries: spectroscopic -
ISM: individual objects: Tarantula Nebula (except planetary nebulae)
Abstract:
A spectroscopic analysis has been undertaken for the B-type multiple
systems (excluding those with supergiant primaries) in the VLT-FLAMES
Tarantula Survey (VFTS). Projected rotational velocities, vsini, for
the primaries have been estimated using a Fourier Transform technique
and confirmed by fitting rotationally broadened profiles. A subset of
33 systems with vsini≤80km/s have been analysed using a TLUSTY grid
of model atmospheres to estimate stellar parameters and surface
abundances for the primaries. The effects of a potential flux
contribution from an unseen secondary have also been considered. For
20 targets it was possible to reliably estimate their effective
temperatures (Teff) but for the other 13 objects it was only possible
to provide a constraint of 20000≤Teff≤26000K - the other parameters
estimated for these targets will be consequently less reliable. The
estimated stellar properties are compared with evolutionary models and
are generally consistent with their membership of 30 Doradus, while
the nature of the secondaries of 3 SB2 system is discussed. A
comparison with a sample of single stars with vsini≤80km/s obtained
from the VFTS and analysed with the same techniques implies that the
atmospheric parameters and nitrogen abundances of the two samples are
similar. However, the binary sample may have a lack of primaries with
significant nitrogen enhancements, which would be consistent with them
having low rotational velocities and having effectively evolved as
single stars without significant rotational mixing. This result, which
may be actually a consequence of the limitations of the pathfinder
investigation presented in this paper, should be considered as a
motivation for spectroscopic abundance analysis of large samples of
binary stars, with high quality observational data.
Description:
Rotational velocity estimates are presented for (near) main sequence
B-type stars that were observed in the VFTS and that are believed to
be the primary of a multiple system. For each star, estimates are
given from different lines are given deduced using both profile
fitting (PF) and Fourier Transform (FT) methodologies, together with
line central depths (CD). Also listed for each star are the means from
the two methodologies, together with standard deviation for the FT
estimates.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table6.dat 139 61 Narrow lined stars
table7.dat 115 44 Broad line stars
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See also:
J/A+A/530/A108 : VLT-FLAMES Tarantula Survey (Evans+, 2011)
J/A+A/550/A107 : RV catalogue of O stars in 30 Doradus (Sana+, 2013)
J/A+A/550/A108 : DIB in VLT-FLAMES Tarantula Survey (van Loon+, 2013)
J/A+A/550/A109 : VLT-FLAMES Tarantula Survey: vsini measures (Dufton+ 2013)
J/A+A/558/A134 : VLTS. 30 Dor luminous stars (Doran+, 2013)
J/A+A/560/A29 : O-stars in VLT-FLAMES Tarantula Survey (Ramirez-Agudelo+ 2013)
J/A+A/564/A39 : VLTS. OVz stars in 30 Dor (Sabin-Sanjulian+, 2014)
J/A+A/564/A40 : VLTS. O-type stellar content of 30 Dor (Walborn+, 2014)
J/A+A/564/L7 : VLT-FLAMES Tarantula Survey: VFTS 822 (Kalari+, 2014)
J/A+A/574/A13 : VLTS. B-type stars classification and RV (Evans+, 2015)
J/A+A/575/A70 : VLT-FLAMES Tarantula Survey: B supergiants (McEvoy+, 2015)
J/A+A/580/A93 : VLTS. B stars multiplicity (Dunstall+, 2015)
J/A+A/600/A81 : VLTS. 30Dor O giants and supergiants (Ramirez-Agudelo+, 2017)
J/A+A/600/A82 : VLTS. O giants & supergiants nitrogen abundances (Grin+, 2017)
Byte-by-byte Description of file: table6.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 3 I3 --- VFTS VFTS star number
7- 9 I3 km/s PF4120 ? vsini for HeI 4120Å from PF methodology
12- 14 I3 km/s FT4120 ? vsini for HeI 4120Å from FT methodology
16- 17 I2 % CD4120 ? Central depth for HeI 4120Å from
PF methodology
19- 21 I3 km/s PF4169 ? vsini for HeI 4169Å from PF methodology
23- 25 I3 km/s FT4169 ? vsini for HeI 4169Å from FT methodology
28- 29 I2 % CD4169 ? Central depth for HeI 4169Å from
PF methodology
31- 33 I3 km/s PF4267 ? vsini for CII 4267Å from PF methodology
35- 37 I3 km/s FT4267 ? vsini for CII 4267Å from FT methodology
40- 41 I2 % CD4267 ? Central depth for CII 4267Å from
PF methodology
43- 45 I3 km/s PF4437 ? vsini for HeI 4437Å from PF methodology
47- 49 I3 km/s FT4437 ? vsini for HeI 4437Å from FT methodology
52- 53 I2 % CD4437 ? Central depth for HeI 4437Å from
PF methodology
55- 57 I3 km/s PF4481 ? vsini for MgII 4481Å from PF methodology
59- 61 I3 km/s FT4481 ? vsini for MgII 4481Å from FT methodology
64- 65 I2 % CD4481 ? Central depth for MgII 4481Å from
PF methodology
67- 69 I3 km/s PF4552 ? vsini for SiIII 4552Å from PF methodology
71- 73 I3 km/s FT4552 ? vsini for SiIII 4552Å from FT methodology
76- 77 I2 % CD4552 ? Central depth for SiIII 4552Å from
PF methodology
79- 81 I3 km/s PF4567 ? vsini for SiIII 4567Å from PF methodology
83- 85 I3 km/s FT4567 ? vsini for SiIII 4567Å from FT methodology
88- 89 I2 % CD4567 ? Central depth for SiIII 4567Å from
PF methodology
91- 93 I3 km/s PF4574 ? vsini for SiIII 4574Å from PF methodology
95- 97 I3 km/s FT4574 ? vsini for SiIII 4574Å from FT methodology
100-101 I2 % CD4574 ? Central depth for SiIII 4574Å from
PF methodology
103-105 I3 km/s PF4661 ? vsini for OII 4661Å from PF methodology
107-109 I3 km/s FT4661 ? vsini for OII 4661Å from FT methodology
112-113 I2 % CD4661 ? Central depth for OII 4661Å from
PF methodology
115-117 I3 km/s PF4713 ? vsini for HeI 4713Å from PF methodology
119-121 I3 km/s FT4713 ? vsini for HeI 4713Å from FT methodology
124-125 I2 % CD4713 ? Central depth for HeI 4713Å from
PF methodology
128-130 I3 km/s FTM ? Weighted mean of the FT estimates (1)
132-134 I3 km/s FTSD ? Standard deviation of the FT estimates (2)
137-139 I3 km/s PFM ? Unweighted mean of the PF estimates
--------------------------------------------------------------------------------
Note (1): Value of 40km/s is an upper limit.
Note (2): Null value: FTM is either an upper value or assigned to a 40km/s bin.
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table7.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 3 I3 --- VFTS VFTS star number
5 I1 --- Status [1]? indicates status uncertain if 1
7- 9 I3 km/s PF4009 ? vsini for HeI 4009Å from PF methodology
11- 13 I3 km/s FT4009 ? vsini for HeI 4009Å from FT methodology
16- 17 I2 % CD4009 ? Central depth for HeI 4009Å from
PF methodology
19- 21 I3 km/s PF4026 ? vsini for HeI 4026Å from PF methodology
23- 25 I3 km/s FT4026 ? vsini for HeI 4026Å from FT methodology
28- 29 I2 % CD4026 ? Central depth for HeI 4026Å from
PF methodology
31- 33 I3 km/s PF4120 ? vsini for HeI 4120Å from PF methodology
35- 37 I3 km/s FT4120 ? vsini for HeI 4120Å from FT methodology
40- 41 I2 % CD4120 ? Central depth for HeI 4120Å from
PF methodology
43- 45 I3 km/s PF4143 ? vsini for HeI 4143Å from
PF methodology
47- 49 I3 km/s FT4143 ? vsini for HeI 4143Å from FT methodology
52- 53 I2 % CD4143 ? Central depth for HeI 4143Å from
PF methodology
55- 57 I3 km/s PF4387 ? vsini for HeI 4387Å from PF methodology
59- 61 I3 km/s FT4387 ? vsini for HeI 4387Å from FT methodology
64- 65 I2 % CD4387 ? Central depth for HeI 4387Å from
PF methodology
67- 69 I3 km/s PF4471 ? vsini for HeI 4471Å from
PF methodology
71- 73 I3 km/s FT4471 ? vsini for HeI 4471Å from FT methodology
76- 77 I2 % CD4471 ? Central depth for HeI 4471Å from
PF methodology
79- 81 I3 km/s PF4713 ? vsini for HeI 4713Å from PF methodology
83- 85 I3 km/s FT4713 ? vsini for HeI 4713Å from FT methodology
88- 89 I2 % CD4713 ? Central depth for HeI 4713Å from
PF methodology
91- 93 I3 km/s PF4921 ? vsini for HeI 4921Å from PF methodology
95- 97 I3 km/s FT4921 ? vsini for HeI 4921Å from FT methodology
100-101 I2 % CD4921 ? Central depth for HeI 4921Å from
PF methodology
104-106 I3 km/s FTM ? Weighted mean of the FT estimates
108-110 I3 km/s FTSD ? Standard deviation of the FT estimates (2)
113-115 I3 km/s PFM ? Unweighted mean of the PF estimates
--------------------------------------------------------------------------------
Note (2): Null value: FTM assigned to a 40km/s bin.
--------------------------------------------------------------------------------
Acknowledgements:
Ryan Garland, ryan.garland(at)physics.ox.ac.uk
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(End) Ryan Garland [University of Oxford], Patricia Vannier [CDS] 11-Apr-2017