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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 (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:
FileName Lrecl Records Explanations
ReadMe 80 . This file table6.dat 139 61 Narrow lined stars table7.dat 115 44 Broad line stars
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 References: Evans et al., Paper I 2011A&A...530A.108E, Cat. J/A+A/530/108 Taylor et al., Paper II 2011A&A...530L..10T Bestenlehner et al., Paper III 2011A&A...530L..14B Bressert et al., Paper IV 2012A&A...542A..49B Dunstall et al., Paper V 2012A&A...542A..50D Henault-Brunet et al., Paper VI 2012A&A...545L...1H Henault-Brunet et al., Paper VII 2012A&A...546A..73H Sana et al., Paper VIII 2013A&A...550A.107S, Cat. J/A+A/550/A107 van Loon et al., Paper IX 2013A&A...550A.108V, Cat. J/A+A/550/A108 Dufton et al., Paper X 2013A&A...550A.109D, Cat. J/A+A/550/A109 Doran et al., Paper XI 2013A&A...558A.134D, Cat. J/A+A/558/A134 Ramirez-Agudelo et al., Paper XII 2013A&A...560A..29R, Cat. J/A+A/560/A29 Sabin-Sanjulian et al., Paper XIII 2014A&A...564A..39S, Cat. J/A+A/564/A39 Walborn et al., Paper XIV 2014A&A...564A..40W, Cat. J/A+A/564/A40 Kalari et al., Paper XV 2014A&A...564L...7K, Cat. J/A+A/564/L7 Maiz Apellaniz et al., Paper XVI 2014A&A...564A..63M Bestenlehner et al., Paper XVII 2014A&A...570A..38B Evans et al., Paper XVIII 2015A&A...574A..13E McEvoy et al., Paper XIX 2015A&A...575A..70M, Cat. J/A+A/575/A70 Clark et al., Paper XX 2015A&A...579A.131C Ramirez-Agudelo et al., Paper XXI 2015A&A...580A..92R Dunstall et al., Paper XXII 2015A&A...580A..93D, Cat. J/A+A/580/A93 Howarth et al., Paper XXIII 2015A&A...582A..73H Ramirez-Agudelo et al., Paper XXIV 2017A&A...600A..81R, Cat. J/A+A/600/A81 Grin et al., Paper XXV 2017A&A...600A..82G, Cat. J/A+A/600/A82
(End) Ryan Garland [University of Oxford], Patricia Vannier [CDS] 11-Apr-2017
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