Access to Astronomical Catalogues

← Click to display the menu
J/A+A/600/A81      VLTS. 30Dor O giants and supergiants (Ramirez-Agudelo+, 2017)

The VLT-FLAMES Tarantula Survey. XXIV. Stellar properties of the O-type giants and supergiants in 30 Doradus. Ramirez-Agudelo O.H., Sana H., de Koter A., Tramper F., Grin N.J., Schneider F.R.N., Langer N., Puls J., Markova N., Bestenlehner J.M., Castro N., Crowther P.A., Evans C.J., Garcia M., Grafener G., Herrero A., van Kempen B., Lennon D.J., Maiz Apellaniz J., Najarro F., Sabin-Sanjulian C., Simon-Diaz S., Taylor W.D., Vink J.S. <Astron. Astrophys. 600, A81 (2017)> =2017A&A...600A..81R (SIMBAD/NED BibCode)
ADC_Keywords: Magellanic Clouds ; Stars, O ; Stars, giant ; Stars, supergiant ; Spectroscopy Keywords: stars: early-type - stars: evolution - stars: fundamental parameters - Magellanic Clouds - galaxies: star clusters: individual: 30 Doradus Abstract: The Tarantula region in the Large Magellanic Cloud contains the richest population of spatially resolved massive O-type stars known so far. This unmatched sample offers an opportunity to test models describing their main-sequence evolution and mass-loss properties. Using ground-based optical spectroscopy obtained in the framework of the VLT-FLAMES Tarantula Survey (VFTS), we aim to determine stellar, photospheric and wind properties of 72 presumably single O-type giants, bright giants and supergiants and to confront them with predictions of stellar evolution and of line-driven mass-loss theories. We apply an automated method for quantitative spectroscopic analysis of O stars combining the non-LTE stellar atmosphere model FASTWIND with the genetic fitting algorithm PIKAIA to determine the following stellar properties: effective temperature, surface gravity, mass-loss rate, helium abundance, and projected rotational velocity. The latter has been constrained without taking into account the contribution from macro-turbulent motions to the line broadening. We present empirical effective temperature versus spectral subtype calibrations at LMC-metallicity for giants and supergiants. The calibration for giants shows a +1kK offset compared to similar Galactic calibrations; a shift of the same magnitude has been reported for dwarfs. The supergiant calibrations, though only based on a handful of stars, do not seem to indicate such an offset. The presence of a strong upturn at spectral type O3 and earlier can also not be confirmed by our data. In the spectroscopic and classical Hertzsprung-Russell diagrams, our sample O stars are found to occupy the region predicted to be the core hydrogen-burning phase by state-of-the-art models. For stars initially more massive than approximately 60M the giant phase already appears relatively early on in the evolution; the supergiant phase develops later. Bright giants, however, are not systematically positioned between giants and supergiants at Minit>25M_☉. At masses below 60M_☉ the dwarf phase clearly precedes the giant and supergiant phases; however this behavior seems to break down at $Minit<18M. Here, stars classified as late O III and II stars occupy the region where O9.5-9.7V stars are expected, but where few such late O V stars are actually seen. Though we can not exclude that these stars represent a physically distinct group, this behaviour may reflect an intricacy in the luminosity classification at late O spectral subtype. Indeed, on the basis of a secondary classification criterion, the relative strength of SiIV to HeI absorption lines, these stars would have been assigned a luminosity class IV or V. Except for five stars, the helium abundance of our sample stars is in agreement with the initial LMC composition. This outcome is independent of their projected spin rates. The aforementioned five stars present moderate projected rotational velocities (i.e., vrot<200km/s) and hence do not agree with current predictions of rotational mixing in main-sequence stars. They may potentially reveal other physics not included in the models such as binary-interaction effects. Adopting theoretical results for the wind velocity law, we find modified wind momenta for LMC stars that are ∼0.3dex higher than earlier results. For stars brighter than 105L[sun, that is, in the regime of strong stellar winds, the measured (unclumped) mass-loss rates could be considered to be in agreement with line-driven wind predictions if the clump volume filling factors were fV∼1/8 to 1/6. Description: Measured stellar and wind parameters of 72 presumably-single O-type stars in the VLT-FLAMES Tarantula Survey, with luminosity class identifiers III-I. Also included are the stellar and wind parameters of 31 O-type stars without luminosity class identifier. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file tablec4.dat 244 72 Best fitting atmospheric and wind parameters of the O-giants, bright giants, and supergiants tablec5.dat 244 31 Best fitting atmospheric and wind parameters of the O-stars without luminosity class tablec1.dat 50 11 List of the hydrogen, helium, and nitrogen diagnostic lines used in the determination of the stellar and wind parameters of the O-giants, bright giants, and supergiants tablec2.dat 30 61 List of the hydrogen and helium diagnostic lines used in the determination of the stellar and wind parameters of the O-giants, bright giants, and supergiants tablec3.dat 30 31 List of the hydrogen and helium diagnostic lines used in the determination of the stellar and wind parameters of the O-stars without luminosity class
See also: J/A+A/530/A108 : VLT-FLAMES Tarantula Survey (Evans+, 2011) J/A+A/550/A107 : VFTS. RV catalogue of O stars in 30 Doradus (Sana+, 2013) J/A+A/560/A29 : VFTS. O-stars rotational velocities (Ramirez-Agudelo+ 2013) J/A+A/564/A39 : VFTS. OVz stars in 30 Dor (Sabin-Sanjulian+, 2014) J/A+A/564/A40 : VFTS. O-type stellar content of 30 Dor (Walborn+, 2014) J/A+A/575/A70 : VFTS. B supergiants (McEvoy+, 2015) J/A+A/600/A82 : VFTS. O giants & supergiants nitrogen abundances (Grin+, 2017) Byte-by-byte Description of file: tablec4.dat tablec5.dat
Bytes Format Units Label Explanations
1- 3 I3 --- VFTS VFTS identification number, [72/892] for tablec4 and [31/892] for tablec5 (2) 5- 27 A23 --- SpType Spectral type and luminosity classification by Walborn et al., (2014, Cat. J/A+A/564/A40) 29- 32 F4.1 mag KMAG Absolute K magnitude (3) 34- 38 F5.2 kK Teff Effective temperature 40 A1 --- nETeff [>] Note on E_Teff (4) 41- 44 F4.2 kK E_Teff ? Upper confidence interval of the effective temperature 46 A1 --- neTeff [<] Note on e_Teff (5) 47- 50 F4.2 kK e_Teff ? Lower boundary confidence interval of the effective temperature 52- 55 F4.2 [cm/s2] logg Surface gravity 57- 60 F4.2 [cm/s2] E_logg Upper boundary confidence interval of the surface gravity 62- 65 F4.2 [cm/s2] e_logg Lower boundary confidence interval of the surface gravity 67- 70 F4.2 [cm/s2] loggc Surface gravity corrected for rotation 72 A1 --- nEloggc [>] Note on E_loggc (4) 73- 76 F4.2 [cm/s2] E_loggc ? Upper boundary confidence interval of the surface gravity corrected for rotation 78 A1 --- neloggc [<] Note on e_loggc (5) 79- 82 F4.2 [cm/s2] e_loggc ? Lower boundary confidence interval of the surface gravity corrected for rotation 84- 88 F5.2 [Msun/yr] log(Mdot) Mass loss rate 90- 93 F4.2 [Msun/yr] E_log(Mdot) Upper boundary confidence interval of the mass loss rate (4) 95 A1 --- nelog(Mdot) [<] Note on e_log(Mdot) (5) 96- 99 F4.2 [Msun/yr] e_log(Mdot) ? Lower boundary confidence interval of the mass loss rate 101-104 F4.2 --- Y Surface Helium abundance in mass fraction 106-109 F4.2 --- E_Y Upper boundary confidence interval of the surface helium abundance 111 A1 --- neY [<] Note on e_Y (5) 112-115 F4.2 --- e_Y ? Lower boundary confidence interval of the surface helium abundance 117-118 I2 km/s vturb Micro-turbulent velocity 120 A1 --- nEvturb [>] Note on E_vturb (4) 121-122 I2 km/s E_vturb ? Upper boundary confidence interval of the micro-turbulent velocity 124 A1 --- nevturb [<] Note on e_vturb (5) 125-126 I2 km/s e_vturb ? Lower boundary confidence interval of the micro-turbulent velocity 128-130 I3 km/s vsini Projected rotational velocity 132 A1 --- nEvsini [>] Note on E_vsini (4) 133-135 I3 km/s E_vsini ? Upper boundary confidence interval of the projected rotational velocity (6) 137 A1 --- nevsini [<] Note on e_vsini (5) 138-140 I3 km/s e_vsini ? Lower boundary confidence interval of the projected rotational velocity (6) 142-145 I4 km/s vinf Terminal wind velocity 148-151 I4 km/s E_vinf Upper boundary confidence interval of the terminal wind velocity 154-157 I4 km/s e_vinf Lower boundary confidence interval of the terminal wind velocity 159-162 F4.2 [Lsun] logL Luminosity 164 A1 --- nElogL [>] Note on E_logL (4) 165-168 F4.2 [Lsun] E_logL ? Upper boundary confidence interval of the luminosity 170 A1 --- nelogL [<] Note on e_logL (5) 171-174 F4.2 [Lsun] e_logL ? Lower boundary confidence interval of the luminosity 176-180 F5.2 Rsun R Radius in solar units 182 A1 --- nER [>] Note on E_R (4) 183-186 F4.2 Rsun E_R ? Upper boundary confidence interval of the radius 188 A1 --- neR [<] Note on e_R (5) 189-192 F4.2 Rsun e_R ? Lower boundary confidence interval of the radius 194-198 F5.2 [g.cm/s2] log(Dmom) Modified wind-momentum 201-204 F4.2 [g.cm/s2] E_log(Dmom) Upper boundary confidence interval of the modified wind-momentum 206 A1 --- nelog(Dmom) [<] Note on e_log(Dmom) (5) 207-210 F4.2 [g.cm/s2] e_log(Dmom) ? Lower boundary confidence interval of the modified wind-momentum 212-216 F5.1 Msun Mspec Spectrocopic mass computed with newtonian gravity 218 A1 --- nEMspec [>] Note on E_Mspec (4) 219-222 F4.1 Msun E_Mspec ? Upper boundary confidence interval of the spectroscopic mass 224 A1 --- neMspec [<] Note on e_Mspec (5) 225-228 F4.1 Msun e_Mspec ? Lower boundary confidence interval of the spectroscopic mass 230-233 F4.1 Msun Mevol Evolutionary mass 235 A1 --- nEMevol [>] Note on E_Mevol (4) 236-239 F4.1 Msun E_Mevol ? Upper boundary confidence interval of the evolutionary mass 241 A1 --- neMevol [<] Note on e_Mevol (5) 242-244 F3.1 Msun e_Mevol ? Lower boundary confidence interval bar the evolutionary mass
Note (2): The last six entries of each table are excluded from the analysis. They are newly detected binaries (i.e., tableC4) or their fits have been rated as poor-quality (tableC5; see Sect. 3.6). The stellar and wind parameters of the stars: VFTS 016, 087, 125, 178, 180, 259, 267, 518,566, 599, and 764 include nitrogen diagnostic lines. Note (3): Values taken from Maiz-Apellaniz et al. (in prep). Note (4): A '>' indicates that the upper boundary of the confidence interval is not constrained (i.e., the lower boundary represents a lower limit). Note (5): A '<' indicates that the lower boundary of the confidence interval is not constrained (i.e., the upper boundary represents an upper limit). Note (6): A '---' is adopted when no uncertainty is available. It means that the parameter has been left fixed. This is the case for VFTS 051 and 711.
Byte-by-byte Description of file: tablec1.dat
Bytes Format Units Label Explanations
1- 3 I3 --- VFTS [11/892] VFTS identification number 5- 6 I2 --- Lines Number of diagnostic lines used 8 A1 --- delta [X0] Hdelta line used (G1) 10 A1 --- gamma [X0] Hgamma line used (G1) 12 A1 --- beta [X0] Hbeta line used (G1) 14 A1 --- alpha [X0] Halpha line used (G1) 16 A1 --- 4026 [X0] HeI+II 4026 line used (G1) 18 A1 --- 4387 [X0] HeI 4387 line used (G1) 20 A1 --- 4471 [X0] HeI 4471 line used (G1) 22 A1 --- 4713 [X0] HeI 4713 line used (G1) 24 A1 --- 4922 [X0] HeI 4922 line used (G1) 26 A1 --- 4200 [X0] HeII 4200 line used (G1) 28 A1 --- 4541 [X0] HeII 4541 line used (G1) 30 A1 --- 4686 [X0] HeII 4686 line used (G1) 32 A1 --- 3995 [X0] N III 3995 line used (G1) 34 A1 --- 4097 [X0] N III 4097 line used (G1) 36 A1 --- 4195 [X0] N III 4195 line used (G1) 38 A1 --- 4379 [X0] N III 4379 line used (G1) 40 A1 --- qua [X0] N III 4511, 4515, 4518 lines used (G1) 42 A1 --- 4523 [X0] N III 4523 line used (G1) 44 A1 --- trip [X0] N III 4634, 4640 lines used (G1) 46 A1 --- 4058 [X0] N IV 4058 line used (G1) 48 A1 --- 4603 [X0] N V 4603 line used (G1) 50 A1 --- 4619 [X0] N V 4619 line used (G1)
Byte-by-byte Description of file: tablec2.dat tablec3.dat
Bytes Format Units Label Explanations
1- 3 I3 --- VFTS VFTS identification number, [61/892] tablec2, [31/682] tablec3 (2) 5- 6 I2 --- Lines Number of diagnostic lines used 8 A1 --- delta [X0] Hdelta line used (G1) 10 A1 --- gamma [X0] Hgamma line used (G1) 12 A1 --- beta [X0] Hbeta line used (G1) 14 A1 --- alpha [X0] Halpha line used (G1) 16 A1 --- 4026 [X0] HeI+II 4026 line used (G1) 18 A1 --- 4387 [X0] HeI 4387 line used (G1) 20 A1 --- 4471 [X0] HeI 4471 line used (G1) 22 A1 --- 4713 [X0] HeI 4713 line used (G1) 24 A1 --- 4922 [X0] HeI 4922 line used (G1) 26 A1 --- 4200 [X0] HeII 4200 line used (G1) 28 A1 --- 4541 [X0] HeII 4541 line used (G1) 30 A1 --- 4686 [X0] HeII 4686 line used (G1)
Note (2): The last six entries of each table are excluded from the analysis. They are newly detected binaries (i.e., tableC4) or their fits have been rated as poor-quality (tableC5; see Sect. 3.6). For the star VFTS 125, the following Nitrogen lines have also been used: N III 4634, 4640, N IV 4058, N V 4603, 4619.
Global notes: Note (G1): Flag as follows: X = line has been used in the determination of the stellar and wind parameters 0 = line has not been used
Acknowledgements: Oscar Hernan Ramirez Agudelo, oscar.ramirez(at)stfc.ac.uk References: Evans et al., Paper I 2011A&A...530A.108E, Cat. J/A+A/530/A108 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...542A..49B 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 2012A&A...550A.108V, Cat. J/A+A/550/A108 Dufton et al., Paper X 2012A&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 2013A&A...564A..39S, Cat. J/A+A/564/A39 Walborn et al., Paper XIV 2014A&A...564A..40W, Cat. J/A+1/564/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 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 Grin et al., Paper XXV 2017A&A...600A..82G, Cat. J/A+A/600/A82
(End) Oscar Hernan Ramirez Agudelo [UK ATC], Patricia Vannier [CDS] 18-Jan-2017
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

catalogue service

© UDS/CNRS

Contact