J/A+A/613/A65 Spectroscopic parameters of O-type stars (Holgado+, 2018)
The IACOB project.
V. Spectroscopic parameters of the O-type stars in the modern grid of standards
for spectral classification.
Holgado G., Simon-Diaz S., Barba R.H., Puls J., Herrero A., Castro N.,
Garcia M., Maiz Apellaniz J., Negueruela I., Sabin-Sanjulian C.
<Astron. Astrophys. 613, A65 (2018)>
=2018A&A...613A..65H 2018A&A...613A..65H (SIMBAD/NED BibCode)
ADC_Keywords: Stars, O ; Spectroscopy
Keywords: stars: early-type - stars: fundamental parameters -
techniques: spectroscopic - catalogs - Galaxy: general
Abstract:
The IACOB and OWN surveys are two ambitious complementary
observational projects which have made available a large multi-epoch
spectroscopic database of optical high resolution spectra of Galactic
massive O-type stars.
As a first step in the study of the full sample of (more than 350)
O stars surveyed by the IACOB and OWN projects, we have performed the
quantitative spectroscopic analysis of a subsample of 128 stars
included in the modern grid of O-type standards for spectral
classification. The sample comprises stars with spectral types in the
range O3-O9.7 and covers all luminosity classes.
We use the semi-automatized iacob-broad and iacob-gbat/fastwind tools
to determine the complete set of spectroscopic parameters that can be
obtained from the optical spectrum of O-type stars. A quality flag is
assigned to the outcome of the iacob- gbat/fastwind analysis for each
star, based on a visual evaluation of how the synthetic spectrum of
the best fitting fastwind model reproduces the observed spectrum. We
also benefit from the multi-epoch character of the IACOB and OWN
surveys to perform a spectroscopic variability study of the complete
sample, providing two different flags for each star accounting for
spectroscopic binarity as well as variability of the main wind
diagnostic lines.
Description:
Complete list of stars considered standards O-type stars for spectral
classification. We performed an exhaustive search for spectra of
these stars in modern high resolution spectroscopic databases. The
spectrum with best quality, in terms of signal-to-noise ratio, was
considered for the quantitative spectroscopic analysis and a
multi-epoch characterization.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tabled1.dat 158 131 Complete list of stars considered in this work
tabled2.dat 128 131 Spectroscopic parameters for the complete
sample of stars
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See also:
III/252 : Pulkovo radial velocities for 35493 HIP stars (Gontcharov, 2006)
III/254 : 2nd Cat. of Radial Velocities with Astrometric Data
(Kharchenko+, 2007)
J/A+A/562/A135 : Northern Galactic OB stars vsini (Simon-Diaz+, 2014)
J/A+A/597/A22 : Massive O- and B-type stars velocities (Simon-Diaz+, 2017)
J/A+A/613/A65 : Spectroscopic parameters of O-type stars (Holgado+, 2018)
J/A+A/613/A9 : Extinction towards Galactic O stars (Maiz Apellaniz+, 2018)
J/A+A/639/A157 : Massive O-type stars near ZAMS elusive detection
(Holgado+, 2020)
Byte-by-byte Description of file: tabled1.dat
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Bytes Format Units Label Explanations
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1- 17 A17 --- Target Name of the star
21- 34 A14 --- OName Alternative name of the star
36- 39 A4 --- SpType Spectral type
41- 45 A5 --- LumClass Luminosity class
47- 49 I3 --- NOT Number of available spectra with NOT
51- 53 I3 --- Mercator Number of available spectra with Mercator
55- 56 I2 --- FEROS/MPI2.2 Number of available spectra with FEROS
58- 59 I2 --- CAFE Number of available spectra with CAFE
61- 97 A37 --- SpecUsed Spectra used in the analysis
99-106 F8.3 d JD ?=- Julian date (JD-2450000)
108-110 I3 --- S/Nc ?=0 Signal-to-noise of the continuum
112-129 A18 --- Line Line used for the broadening parameter
131-133 I3 --- S/Nl ?=- Signal-to-noise of the line
135-137 I3 0.1pm EW ?=- Equivalent width of the line (mÅ)
139-142 I4 km/s RV ?=- Radial velocity
144 I1 km/s e_RV ? rms uncertainty on RV
146-151 F6.1 km/s RVlit ?=- Radial velocity in literature
153-156 F4.1 km/s e_RVlit ? rms uncertainty on RVlit
157-158 A2 --- r_RVlit [* ] Reference for RVlit (1)
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Note (1): References as follows:
* = Values from Gontcharov et al. (2006AstL...32..759G 2006AstL...32..759G, Cat. III/252)
** = Values from Kharchenko et al. (2007AN....328..889K 2007AN....328..889K, Cat. III/254)
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Byte-by-byte Description of file: tabled2.dat
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Bytes Format Units Label Explanations
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1- 17 A17 --- Target Name of the star
18 A1 --- n_Target [a] Note (1)
20- 24 A5 --- SpType Spectral type
26- 36 A11 --- LumClass Luminosity class
38- 40 I3 km/s vsini ?=- Projected rotational velocity
42- 44 I3 km/s vmac ?=- Macroturbulent velocity
46 A1 --- l_Teff Limit flag on Teff
47- 50 F4.1 kK Teff ?=- Effective temperature
52- 54 F3.1 kK e_Teff ? rms uncertainty on Teff
56 A1 --- l_logg Limit flag on logg
57- 60 F4.2 [cm/s2] logg ?=- logarithm of the surface gravity
62- 65 F4.2 [cm/s2] e_logg ? rms uncertainty on logg
67 A1 --- l_loggt Limit flag on loggt
68- 71 F4.2 [cm/s2] loggt ?=- Gravity corrected from rotational
effects (2)
73- 76 F4.2 [cm/s2] e_loggt ? rms uncertainty on loggt
78 A1 --- l_Y(He) Limit flag on Y(He)
79- 82 F4.2 [-] Y(He) ?=- Helium abundance
84- 87 F4.2 [-] e_Y(He) ? rms uncertainty on Y(He)
89 A1 --- l_vmic Limit flag on vmic
90- 93 F4.1 km/s vmic ?=- Microturbulence velocity or lower value
of microturbulence velocity interval
96 I1 km/s e_vmic ? rms uncertainty on vmic
97 A1 --- --- [-]
98-101 F4.1 km/s Bvmic ? Upper value of microturbulence velocity
interval
103 A1 --- l_logQ Limit flag on logQ
104-108 F5.1 --- logQ ?=- Wind-strength parameter
110-112 F3.1 --- e_logQ ? rms uncertainty on logQ
114-115 A2 --- Qual Quality flag (Q1-Q4) (3)
117-123 A7 --- Notes Multi-epoch notes (4)
125-128 A4 --- OWNNote OWN multi-epoch notes (4)
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Note (1): Note as follows:
a = For these three stars the luminosity class has changed from III to IV in
the new GOSSS OB2500 v3.0 grid of standards (Maiz Apellaniz et al.,
2016ApJS..224....4M 2016ApJS..224....4M)
Note (2): gtrue=g+gcent, gcent~(Vrot*sini)2)/R*
Note (3): Quality flag as follows:
Q1 = acceptable fit with no major remarks,
Q2 = HeII λ4686 appearing in the observed spectrum as an inverse
P-Cygni profile or showing a double peak
Q3 = Hα and HeII λ4686 not fitting at the same time
Q4 = no HeI available to properly constrain the effective temperature of
the star
Note (4): Notes as follows:
C = Constant
LPV = Line profile variability
WVa = Wind variable
WVe = Wind variable
MD0 = More Data needed, only 0 spectra available
MD1 = More Data needed, only 1 spectra available
MD2 = More Data needed, only 2 spectra available
SB1 = single-line eclipsing binary
SB2 = double-line eclipsing binary
VAR = Variable
VAR? = Variable ?
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Acknowledgements:
Gonzalo Holgado, gholgado(at)iac.es
References:
Simon-Diaz & Herrero, Paper I 2014A&A...562A.135S 2014A&A...562A.135S, Cat. J/A+A/562/A135
Simon-Diaz et al., Paper II 2014A&A...570L...6S 2014A&A...570L...6S
Simon-Diaz et al., Paper III 2017A&A...597A..22S 2017A&A...597A..22S, Cat. J/A+A/597/A22
Godart et al., Paper IV 2017A&A...597A..23G 2017A&A...597A..23G
Holgado et al., Paper V 2018A&A...613A..65H 2018A&A...613A..65H, Cat. J/A+A/613/A65
Maiz-Apellaniz & Barba, 2018A&A...613A...9M 2018A&A...613A...9M, Cat. J/A+A/613/A9
Holgado et al. Paper VI 2020A&A...639A.157H 2020A&A...639A.157H, Cat. J/A+A/639/A157
(End) Gonzalo Holgado [Univ. La Laguna], Patricia Vannier [CDS] 30-Nov-2017