J/MNRAS/488/1090 Unclassified B[e] stars in the MW, SMC and LMC (Condori+, 2019)
The study of unclassified B[e] stars and candidates in the Galaxy and
Magellanic Clouds.
Condori C.A.H., Borges Fernandes M., Kraus M., Panoglou D., Guerrero C.A.
<Mon. Not. R. Astron. Soc., 488, 1090-1110 (2019)>
=2019MNRAS.488.1090C 2019MNRAS.488.1090C (SIMBAD/NED BibCode)
ADC_Keywords: Stars, Be ; Stars, emission ; Line Profiles ; Spectra, optical ;
MK spectral classification ; Extinction ; Rotational velocities ;
Radial velocities ; Equivalent widths ; Effective temperatures
Keywords: line: profiles - stars: emission-line, Be - stars: identification -
techniques: spectroscopic
Abstract:
We investigated 12 unclassified B[e] stars or candidates, 8 from the
Galaxy, 2 from the Large Magellanic Cloud (LMC), and 2 from the Small
Magellanic Cloud (SMC). Based on the analysis of high-resolution
spectroscopic (FEROS) and photometric data, we confirmed the presence
of the B[e] phenomenon for all objects of our sample, except for one
(IRAS 07455-3143). We derived their effective temperature, spectral
type, luminosity class, interstellar extinction and, using the
distances from Gaia DR2, we obtained their bolometric magnitude,
luminosity, and radius. Modelling of the forbidden lines present in
the FEROS spectra revealed information about the kinematics and
geometry of the circumstellar medium of these objects. In addition, we
analysed the light curves of four stars, finding their most probable
periods. The evolutionary stage of 11 stars of our sample is suggested
from their position on the HR diagram, taking into account
evolutionary tracks of stars with solar, LMC, and SMC metallicities.
As results, we identified B and B[e] supergiants, B[e] stars probably
at the main sequence or close to its end, post-AGB and HAeB[e]
candidates, and A[e] stars in the main sequence or in the pre-main
sequence. However, our most remarkable results are the identification
of the third A[e] supergiant (ARDB 54, the first one in the LMC), and
of an 'LBV impostor' in the SMC (LHA 115-N82).
Description:
Our sample comprises 12 objects: 8 from the Galaxy, 2 from LMC, and 2
from SMC, which exhibit or may exhibit the B[e] phenomenon, as seen in
Table 1. We analysed in a homogeneous way photometric and
high-resolution spectroscopic data of these objects. The sample can
also be divided in two groups: the first group is composed of Hen
3-938, SS 255, Hen 2-91, LHA 115-N82, ARDB 54, and LHA 120-S59, for
which the analysis of high-resolution spectra (public or ours) was
done for the first time; and the second one is composed of IRAS
07080+0605, IRAS 07377-2523, IRAS 07455-3143, V* FX Vel, IRAS
17449+2320, and [MA93] 1116 that were already studied by different
authors using high-resolution spectroscopy, but for which we provide
more details about their nature.
For our analysis, we obtained high-resolution spectra using the
Fibre-fed Extended Range Optical Spectrograph (FEROS, Kaufer et al.
1999Msngr..95....8K 1999Msngr..95....8K) attached to the 2.2-m ESO-MPI telescope, at La
Silla Observatory (Chile). FEROS is a bench-mounted echelle
spectrograph, which provides a resolution of 0.03Å/pixel (R∼48000)
and a spectral coverage from 3600 to 9200Å. The spectra of our
sample were observed in 12 different epochs between 2005 and 2016
(Table 1).
In addition to the spectroscopic data, we searched for public
photometric data, in order to derive the light curve (LC) of some of
our objects and identify any possible photometric variation and
periodicity. We collected data from VizieR
(http://vizier.u-strasbg.fr/viz-bin/VizieR), All Sky Automated Survey
(ASAS, Pojmanski 2003AcA....53..341P 2003AcA....53..341P, Cat. II/264), the Optical
Gravitational Lensing Experiment (OGLE III, Udalski et al.
2008AcA....58...69U 2008AcA....58...69U), and also from the literature, as can be seen in
Table 2.
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table1.dat 96 30 Our sample of unclassified B[e] stars and
candidates observed with FEROS
table2.dat 82 27 Photometric data of our sample collected from
the literature
table3.dat 39 14 The radial velocity of stars from our sample
that do not present sensible spectral
variability or for which we have just one
spectrum
table4.dat 68 13 Radial velocities, derived from permitted
absorption and forbidden emission lines, for
the objects with strong variability
table5a.dat 52 9 Spectral type, luminosity class, intrinsic
color index, and effective temperature for some
stars of our sample, obtained using method 1
table5b.dat 59 7 Spectral type, intrinsic color index, and
effective temperature for some stars of our
sample, obtained using method 2
table5c.dat 57 3 Effective temperature for some stars of our
sample, obtained using method 3
table6.dat 117 12 Interstellar, circumstellar, and total color
excess, E(B-V), and visual interstellar
extinction, AV, for the objects of our sample
table7.dat 112 5 Velocities needed for fitting the line profiles
for the stars with both [OI] and [CaII]
forbidden lines
table8.dat 34 16 Velocities needed for fitting the line profiles
for the stars with only the [OI] forbidden lines
table9.dat 100 11 Physical parameters of the stars of our sample
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Byte-by-byte Description of file: table1.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 6 A6 --- Loc Localisation (Galaxy/SMC/LMC)
8 A1 --- f_Name [ab] Flag on Name (G1)
10- 23 A14 --- Name Star name
25- 39 A15 --- ID IRAS object identifier (IRAS HHMMm+DDMM)
41- 42 I2 h RAh Right ascension (J2000)
44- 45 I2 min RAm Right ascension (J2000)
47- 50 F4.1 s RAs Right ascension (J2000)
52 A1 --- DE- Declination sign (J2000)
53- 54 I2 deg DEd Declination (J2000)
56- 57 I2 arcmin DEm Declination (J2000)
59- 62 F4.1 arcsec DEs Declination (J2000)
64- 73 A10 "Y:M:D" Date Date of observation
75- 83 F9.1 d JD Julian date of the start of the first exposure
85- 88 I4 s texp Exposure time of each spectrum in seconds
90 I1 --- N [1/2] Number of spectra at each observation
92 A1 --- f_N Flag on N (1)
94- 96 I3 --- S/N Signal to noise ratio around 5500Å of each
spectrum
--------------------------------------------------------------------------------
Note (1): Flag as follows:
* = Public spectra obtained from ESO Science Archive Facility
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table2.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 6 A6 --- Loc Localisation (Galaxy/SMC/LMC)
8 A1 --- f_Name [ab] Flag on Name (G1)
10- 24 A15 --- Name Star name
26- 41 A16 --- Date Date of observation
43- 48 F6.3 mag Umag ? U-band magnitude
50- 53 F4.2 mag e_Umag ? Error on Umag
55- 60 F6.3 mag Bmag ? B-band magnitude
62- 65 F4.2 mag e_Bmag ? Error on Bmag
67- 72 F6.3 mag Vmag ? V-band magnitude
74- 77 F4.2 mag e_Vmag ? Error on Vmag
79- 80 I2 --- refs References (1)
82 A1 --- f_Date [*] Flag on date (2)
--------------------------------------------------------------------------------
Note (1): References as follows:
1 = Vieira et al. (2003AJ....126.2971V 2003AJ....126.2971V, Cat. J/AJ/126/2971, Pico dos Dias
Survey)
2 = Torres et al. (1995AJ....109.2146T 1995AJ....109.2146T)
3 = Henden et al. (2015AAS...22533616H, Cat. II/336, AAVSO Photometric All
Sky Survey (APASS) DR9)
4 = Girard et al. (2011AJ....142...15G 2011AJ....142...15G, Cat. I/320, SPM 4.0 Catalog)
5 = Cutri et al. (2003yCat.2246....0C 2003yCat.2246....0C, Cat. II/246, 2MASS Catalog)
6 = Zacharias et al. (2004AAS...205.4815Z 2004AAS...205.4815Z, Cat. I/297, The NOMAD-1 Catalog)
7 = Heydari-Malayeri (1990A&A...234..233H 1990A&A...234..233H)
8 = Orsatti (1992AJ....104..590O 1992AJ....104..590O)
9 = Massey (2002ApJS..141...81M 2002ApJS..141...81M, Cat. II/236)
10 = Ardeberg et al. (1972A&AS....6..249A 1972A&AS....6..249A)
11 = Zaritsky et al. (2004AJ....128.1606Z 2004AJ....128.1606Z, Cat. J/AJ/128/1606)
12 = Gummersbach, Zickgraf & Wolf (1995A&A...302..409G 1995A&A...302..409G)
13 = Miroshnichenko et al. (2007ApJ...671..828M 2007ApJ...671..828M)
14 = Kharchenko (2001KFNT...17..409K 2001KFNT...17..409K, Cat. I/280, ASCC-2.5 V3)
15 = de Winter et al. (2001A&A...380..609D 2001A&A...380..609D, Cat. J/A+A/380/609)
16 = Massey, Parker & Garmany (1989AJ.....98.1305M 1989AJ.....98.1305M, Cat. J/AJ/98/1305)
Note (2): Flag as follows:
* = No information about the exact dates of the photometric observations
is provided, thus, we decided to assume the year of the publication
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table3.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 6 A6 --- Loc Localisation (Galaxy/SMC/LMC)
8- 22 A15 --- Name Star name
24- 33 A10 "Y:M:D" Date Date of observation
35- 37 I3 km/s RV Average radial velocity obtained from [OI]
and [FeII] lines
39 I1 km/s e_RV Error on RV
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table4.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 6 A6 --- Loc Localisation (Galaxy/SMC/LMC)
8- 22 A15 --- Name Star name
24- 33 I10 "Y:M:D" Date Date of observation
35- 37 I3 km/s RVOFe Radial velocity derived from [OI] and [FeII]
39 I1 km/s e_RVOFe Error on RVOFe
41- 43 I3 km/s RVHe ? Radial velocity derived from [HeI]
45 I1 km/s e_RVHe ? Error on RVHe
47- 49 I3 km/s RVMg ? Radial velocity derived from [MgII]
51 I1 km/s e_RVMg ? Error on RVMg
53- 55 I3 km/s RVSi ? Radial velocity derived from [SiII]
57 I1 km/s e_RVSi ? Error on RVSi
59- 61 I3 km/s RVCa ? Radial velocity derived from [CaI]
63 I1 km/s e_RVCa ? Error on RVCa
65- 66 I2 km/s RVLi ? Radial velocity derived from [LiI]
68 I1 km/s e_RVLi ? Error on RVLi
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table5a.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 15 A15 --- Name Star name
17- 21 A5 --- SpType Spectral type
23- 30 A8 --- LC Luminosity class
32- 36 F5.2 mag (B-V)0 Intrinsic B-V colour index (1)
38- 41 F4.2 mag e_(B-V)0 Error on (B-V)0
43- 47 I5 K Teff Effective temperature
49- 52 I4 K e_Teff Error on Teff
--------------------------------------------------------------------------------
Note (1): Borges Fernandes et al. (2009A&A...508..309B 2009A&A...508..309B, Cat. J/A+A/508/309)
described a method to derive the intrinsic colour index (B-V)0 and
the total extinction of each object through the observed color index
(method 1)
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Byte-by-byte Description of file: table5b.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 15 A15 --- Name Star name
17- 26 A10 "Y:M:D" Date Date of observation
28- 31 F4.2 --- MgII/HeI MgII 4482Å/HeI 4471Å equivalent width
ratio
33- 36 F4.2 --- e_MgII/HeI Error on MgII/HeI
38- 39 A2 --- l_SpType [=<,< ,∼ ] Limit flag on SpType
41- 45 A5 --- SpType Spectral type (1)
47- 48 A2 --- l_Teff [=<,< ,∼ ] Limit flag on Teff
50- 54 I5 K Teff Effective temperature
56- 59 I4 K e_Teff ? Error on Teff
--------------------------------------------------------------------------------
Note (1): Based on empirical spectroscopic criteria, using equivalent width
ratios of photospheric lines, we can estimate the spectral
classification for B- and A-type stars in the Galaxy and in the
Magellanic Clouds. We chose the relation that associates the spectral
type to MgII 4482Å/HeI 4471Å (method 2), as done by
Lennon (1997A&A...317..871L 1997A&A...317..871L, Cat. J/A+A/317/871), Evans & Howarth
(2003MNRAS.345.1223E 2003MNRAS.345.1223E) and Kraus et al. (2008A&A...487..697K 2008A&A...487..697K).
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Byte-by-byte Description of file: table5c.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 15 A15 --- Name Star name
17- 26 A10 "Y:M:D" Date Date of observation
28- 31 F4.2 --- HeIa/SiII ? HeI 4713Å/SiII 6347Å equivalent
width ratio
33- 36 F4.2 --- e_HeIa/SiII ? Error on HeIa/SiII
38- 41 F4.2 --- HeIb/SiII HeI 5875Å/SiII 6347Å equivalent width
ratio
43- 46 F4.2 --- e_HeIb/SiII Error on HeIb/SiII
48- 52 I5 K Teff Effective temperature (1)
54- 57 I4 K e_Teff Error on Teff
--------------------------------------------------------------------------------
Note (1): In order to estimate the effective temperature, we used the
HeI 4713Å/SiII 6347Å and HeI 5875Å/SiII 6347Å equivalent
width ratios, as in Khokhlov et al. (2017ApJ...835...53K 2017ApJ...835...53K) (method 3)
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table6.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 6 A6 --- Loc Localisation (Galaxy/SMC/LMC)
8- 22 A15 --- Name Star name
24 A1 --- f_Name Flag on Name (1)
26- 29 F4.2 0.1pm EWDIBs ? Equivalent width of the diffuse
interstellar band (DIB) at 5780Å in
mÅ
31- 34 F4.2 mag E(B-V)DIBsIS ? Interstellar color excess derived from
the DIB
36- 39 F4.2 mag e_E(B-V)DIBsIS ? Error on E(B-V)DIBsIS
41- 44 F4.2 mag E(B-V)IRSAIS Interstellar color excess taken from
IRSA (2)
46- 49 F4.2 mag e_E(B-V)IRSAIS Error on E(B-V)IRSAIS
51 A1 --- f_E(B-V)IRSAIS Flag on E(B-V)IRSAIS (3)
53- 56 F4.2 mag E(B-V)3DIS ? Interstellar color excess taken from 3D
dust mapping (4)
58- 61 F4.2 mag e_E(B-V)3DIS ? Error on E(B-V)3DIS
63- 66 F4.2 mag E(B-V)IS Interstellar color excess adopted in this
work
68- 71 F4.2 mag e_E(B-V)IS Error on E(B-V)IS
73- 76 F4.2 mag E(B-V)CS ? Circumstellar color excess (5)
78- 81 F4.2 mag e_E(B-V)CS ? Error on E(B-V)CS
83- 86 F4.2 mag E(B-V)T ? Total color excess (6)
88- 91 F4.2 mag e_E(B-V)T ? Error on E(B-V)T
93- 96 F4.2 mag Av Visual interstellar extinction (7)
98-101 F4.2 mag e_Av Error on Av
103 A1 --- u_E(B-V)lit1 [~] Uncertainty flag on E(B-V)lit1
105-108 F4.2 mag E(B-V)lit1 ? Interstellar color excess from the
literature
110 A1 --- r_E(B-V)lit1 Reference for E(B-V)lit1 (8)
112-115 A4 mag E(B-V)lit2 ? Other interstellar color excess from the
literature
117 A1 --- r_E(B-V)lit2 Reference for E(B-V)lit2 (8)
--------------------------------------------------------------------------------
Note (1): Flag as follows:
* = The total colour excess is negative using the colours from Table 2,
thus, we decided to consider only its interstellar extinction
Note (2): For the objects that do not present the diffuse interstellar band
(DIB) at 5780Å and objects located in the SMC and LMC, we used
values from IRSA/Galactic Dust Reddening and Extinction
(Schlafly & Finkbeiner 2011ApJ...737..103S 2011ApJ...737..103S)
(http://irsa.ipac.caltech.edu/applications/DUST/)
Note (3): For objects with declination ≥-30°, we used 3D dust mapping
(Green et al. 2018MNRAS.478..651G 2018MNRAS.478..651G) (http://argonaut.skymaps.info/)
Note (4): Flag as follows:
* = Minimum value of interstellar color excess from IRSA
Note (5): For the circumstellar extinction, we used the relation:
E(B-V)CS=E(B-V)T-E(B-V)IS
Note (6): For the total extinction of each object, we used the relation:
E(B-V)T=(B-V)-(B-V)0. These color indices are obtained from
Tables 2 and 5, respectively.
Note (7): In order to derive the visual interstellar extinction, AV, we
assumed AV/E(B-V)IS=3.1 for Galaxy (Cardelli, Clayton & Mathis
1989ApJ...345..245), 2.74 for SMC and 2.76 for LMC stars
(Gordon et al. 2003ApJ...594..279G 2003ApJ...594..279G)
Note (8): References as follows:
a = Vieira et al. (2011A&A...526A..24V 2011A&A...526A..24V)
b = Pereira, Franco & de Araujo (2003A&A...397..927P 2003A&A...397..927P)
c = Cidale, Zorec & Tringaniello (2001A&A...368..160C 2001A&A...368..160C)
d = Miroshnichenko et al. (2007ApJ...671..828M 2007ApJ...671..828M)
e = Chen, Liu & Shan (2016MNRAS.463.1162C 2016MNRAS.463.1162C, Cat. J/MNRAS/463/1162)
f = Orsatti (1992AJ....104..590O 1992AJ....104..590O)
g = Wisniewski et al. (2007ApJ...670.1331W 2007ApJ...670.1331W)
h = Kamath et al. (2014MNRAS.439.2211K 2014MNRAS.439.2211K, Cat. J/MNRAS/439/2211)
i = Heydari-Malayeri (1990A&A...234..233H 1990A&A...234..233H)
j = Levato et al. (2014A&A...568A..28L 2014A&A...568A..28L)
k = Gummersbach et al. (1995A&A...302..409G 1995A&A...302..409G)
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Byte-by-byte Description of file: table7.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 15 A15 --- Name Star name
17 A1 --- f_Name [a] Flag on name (1)
19- 20 I2 km/s vrOI5577 ? Component of the rotational velocity
projected to the line of sight for the
[OI]5577Å line
22- 24 F3.1 km/s e_vrOI5577 ? Error on vrOI5577
26- 29 F4.1 km/s vgOI5577 ? Gaussian component of the velocity for
the [OI]5577Å line
31- 33 F3.1 km/s e_vgOI5577 ? Error on vgOI5577
35- 36 I2 km/s vrOI6300a Component of the rotational velocity
projected to the line of sight for the
[OI]6300Å line (1st ring) (2)
38- 40 F3.1 km/s e_vrOI6300a Error on vrOI6300a
42- 45 F4.1 km/s vgOI6300a Gaussian component of the velocity for the
[OI]6300Å line (1st ring) (2)
47- 49 F3.1 km/s e_vgOI6300a Error on vgOI6300a
51- 52 I2 km/s vrOI6300b ? Component of the rotational velocity
projected to the line of sight for the
[OI]6300Å line (2nd ring) (2)
54- 56 F3.1 km/s e_vrOI6300b ? Error on vrOI6300b
58- 60 F3.1 km/s vgOI6300b ? Gaussian component of the velocity for
the [OI]6300Å line (2nd ring) (2)
62- 64 F3.1 km/s e_vgOI6300b ? Error on vgOI6300b
66- 67 I2 km/s vrCaII7291a Component of the rotational velocity
projected to the line of sight for the
[CaII]7291Å line
69- 71 F3.1 km/s e_vrCaII7291a Error on vrCaII7291a
73- 76 F4.1 km/s vgCaII7291a Gaussian component of the velocity for the
[CaII]7291Å line (1st ring) (2)
78- 80 F3.1 km/s e_vgCaII7291a Error on vgCaII7291a
82- 84 F3.1 km/s vgCaII7291b ? Gaussian component of the velocity for
the [CaII]7291Å line (2nd ring) (2)
86- 88 F3.1 km/s e_vgCaII7291b ? Error on vgCaII7291b
90- 91 I2 km/s vrCaII7324a Component of the rotational velocity
projected to the line of sight for the
[CaII]7324Å line
93- 95 F3.1 km/s e_vrCaII7324a Error on vrCaII7324a
97-100 F4.1 km/s vgCaII7324a Gaussian component of the velocity for the
[CaII]7324Å line (1st ring) (2)
102-104 F3.1 km/s e_vgCaII7324a Error on vgCaII7324a
106-108 F3.1 km/s vgCaII7324b ? Gaussian component of the velocity for
the [CaII]7324Å line (2nd ring) (2)
110-112 F3.1 km/s e_vgCaII7324b ? Error on vgCaII7324b
--------------------------------------------------------------------------------
Note (1): Flag as follows:
a = First ring with a gap. In some cases where the profiles are very
asymmetric, we allow for gaps in the rings.
Note (2): In cases where a single ring is insufficient to reproduce the
observed profile shape, we add one or more rings.
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Byte-by-byte Description of file: table8.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 15 A15 --- Name Star name
17- 20 F4.1 km/s vrot ? Component of the rotational velocity
projected to the line of sight
22- 24 F3.1 km/s e_vrot ? Error on vrot
26- 28 F3.1 km/s vgauss Gaussian component of the velocity
30- 32 F3.1 km/s e_vgauss Error on vgauss
34 A1 --- f_vgauss [a] Flag on vgauss (1)
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Note (1): Ring with a gap
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Byte-by-byte Description of file: table9.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 6 A6 --- Loc Localisation (Galaxy/SMC/LMC)
8- 22 A15 --- Name Star name
24 A1 --- f_Name [ab] Flag on Name (G1)
26- 33 F8.2 pc Dist ? Distances
35- 41 F7.2 pc E_Dist ? Upper error on Dist
43- 49 F7.2 pc e_Dist ? Lower error on Dist
51- 52 A2 --- f_Dist Flag on Dist (1)
54- 58 F5.2 mag BC Bolometric correction from Humphreys & McElroy
(1984ApJ...284..565H 1984ApJ...284..565H)
60- 64 F5.2 mag Mbol Bolometric magnitude
66- 69 F4.2 mag e_Mbol Error on Mbol
71- 75 I5 K Teff Effective temperature
77- 80 I4 K e_Teff Error on Teff
82 A1 --- r_Teff Reference for Teff (2)
84- 87 F4.2 [Lsun] logL Logarithm of the star luminosity
89- 92 F4.2 [Lsun] e_logL Error on logL
94 A1 --- u_Rad [~] Uncertainty flag on Rad
96- 97 I2 Rsun Rad Star radius
99-100 I2 Rsun e_Rad ? Error on Rad
--------------------------------------------------------------------------------
Note (1): Flag as follows:
* = Distances from Gaia DR2 for Galactic stars provided by
Bailer-Jones et al. (2018AJ....156...58B 2018AJ....156...58B, Cat. I/347). We caution that
the values for objects further away than 4kpc have high uncertainties.
These values might considerably change with Gaia DR3.
** = Distance modulus for SMC taken from Graczyk et al. (2014ApJ...780...59G 2014ApJ...780...59G,
Cat. J/ApJ/780/59) and for LMC taken from Udalski et al.
(1998ApJ...509L..25U 1998ApJ...509L..25U)
Note (2): Reference as follows:
L = Effective temperature from Levato et al. (2014A&A...568A..28L 2014A&A...568A..28L)
--------------------------------------------------------------------------------
Global Notes:
Note (G1): Flag as follows:
a = First group composed of Hen 3-938, SS 255, Hen 2-91, LHA 115-N82,
ARDB 54, and LHA 120-S59, for which the analysis of high-resolution
spectra (public or ours) was done for the first time
b = Second group composed of IRAS 07080+0605, IRAS 07377-2523,
IRAS 07455-3143, V* FX Vel, IRAS 17449+2320, and [MA93] 1116 that were
already studied by different authors using high-resolution spectroscopy,
but for which we provide more details about their nature
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History:
From electronic version of the journal
(End) Ana Fiallos [CDS] 25-Nov-2022