J/A+A/629/A114 sigma Ori GTC+INT spectroscopy (Caballero+, 2019)
Stars and brown dwarfs in the sigma Orionis cluster.
IV. IDS/INT and OSIRIS/GTC spectroscopy and Gaia DR2 astrometry.
Caballero J.A., de Burgos A., Alonso-Floriano F.J., Cabrera-Lavers A.,
Garcia-Alvarez D., Montes D.
<Astron. Astrophys. 629, A114 (2019)>
=2019A&A...629A.114C 2019A&A...629A.114C (SIMBAD/NED BibCode)
ADC_Keywords: Clusters, open ; Spectroscopy ; Stars, brown dwarf
Keywords: open clusters and associations: individual: sigma Orionis -
stars: early-type - stars: solar-type - stars: late-type -
stars: emission-line, Be - stars: pre-main sequence
Abstract:
Only a few open clusters are as important for the study of stellar and
substellar objects, and their formation and evolution, as the young
sigma Orionis cluster. However, a complete spectroscopic
characterisation of its whole stellar population is still missing. We
filled most of that gap with a large spectroscopic and astrometric
survey of targets towards sigma Orionis. Eventually, it will be one of
the open clusters with the lowest proportion of interlopers and the
largest of confirmed cluster members with known uncontrovertible youth
features. We acquired 317 low-resolution optical spectra with IDS at
the 2.5m Isaac Newton Telescope and OSIRIS at the 10.4m Gran
Telescopio Canarias. On them, we measured equivalent widths of LiI,
Hα, and other key lines, and determined spectral types. We
complemented the information with Gaia DR2 astrometric data and other
features of youth (mid-infrared excess, X-ray emission) compiled with
Virtual Observatory tools and from the literature. Of the 168 observed
targets, we determined for the first time spectral types of 39 stars
and equivalent widths of LiI and Hα of 34 and 12 stars,
respectively. We identified 11 close (ρ≲3-arcsec) binaries
resolved by Gaia, of which three are new, 14 strong accretors, of
which four are new and another four have Hα emission shifted by
over 120km/s, two juvenile star candidates in the sparse population of
the Ori OB1b association, and one spectroscopic binary candidate.
Remarkably, we found 51 cluster non-members, 35 of which were
previously considered as sigma Orionis members and taken into account
in high-impact works on, e.g., disc frequency and initial mass
function.
Description:
Mayrit identifier, discovery/recommended name, equatorial coordinates,
proper motions, parallax, IDS/INT and/or OSIRIS/GTC date(s) of
observation, exposure time(s), (pseudo-)equivalent widths of Ca H, Ca
K, Hγ, Hβ, HeI D3, Hα, LiI... , spectral types
(MILES, PyHammer, Standards, Literature -and corresponding reference-,
Adopted), youth features (OB spectral type, concordant proper motion
and parallax, LiI λ6708Å in absorption, Hα
λ6563Å in emission, mid-infrared flux excess, X-ray
emission) and membership classification.
File Summary:
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FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
tablea1.dat 266 142 Observations of targets with IDS/INT
tablea2.dat 128 47 Observations of targets with OSIRIS/GTC
tablea3.dat 126 140 Equivalent widths of IDS/INT spectra
tablea4.dat 201 46 Equivalent widths of OSIRIS/GTC spectra
tablea5.dat 108 165 Membership and youth features of investigated
stars
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See also:
J/A+A/478/667 : The Mayrit catalogue (Caballero, 2008)
J/ApJ/794/36 : sigma Orionis cluster stellar population (Hernandez+, 2014)
Byte-by-byte Description of file: tablea1.dat tablea2.dat
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Bytes Format Units Label Explanations
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1- 9 A9 --- Mayrit Mayrit identifier
10 A1 --- n_Mayrit [)] ) for Mayrit identifier not
oldest identifier
12- 44 A33 --- AName Alternative star name (1)
45 A1 --- n_AName [*] Note (2)
46- 47 I2 h RAh Right ascension (J2000)
49- 50 I2 min RAm Right ascension (J2000)
52- 56 F5.2 s RAs Right ascension (J2000)
58 A1 --- DE- Declination sign (J2000)
59- 60 I2 deg DEd Declination (J2000)
62- 63 I2 arcmin DEm Declination (J2000)
65- 68 F4.1 arcsec DEs Declination (J2000)
70- 76 F7.3 mas/yr pmRA* Proper motion along RA (pmRA*cosDE)
78- 82 F5.3 mas/yr e_pmRA* rms uncertainty on pmRA*
84- 90 F7.3 mas/yr pmDE Proper motion along DE
92- 96 F5.3 mas/yr e_pmDE rms uncertainty on pmDE
98-103 F6.3 mas plx ?=- Parallax
105-109 F5.3 mas e_plx ?=- rms uncertainty on plx
111-121 A11 "DD/MMM/YYYY" Obs.date1 Date of observation
123-128 A6 s ExpTime1 Exposition time
129 A1 --- --- [,]
131-141 A11 "DD/MMM/YYYY" Obs.date2 Date of observation
143-146 I4 s ExpTime2 ? Exposition time
147 A1 --- --- [,]
149-159 A11 "DD/MMM/YYYY" Obs.date3 Date of observation
161-163 I3 s ExpTime3 ? Exposition time
164 A1 --- --- [,]
166-176 A11 "DD/MMM/YYYY" Obs.date4 Date of observation
178-180 I3 s ExpTime4 ? Exposition time
181 A1 --- --- [,]
183-193 A11 "DD/MMM/YYYY" Obs.date5 Date of observation
195-197 I3 s ExpTime5 ? Exposition time
198 A1 --- --- [,]
200-210 A11 "DD/MMM/YYYY" Obs.date6 Date of observation
212-214 I3 s ExpTime6 ? Exposition time
215 A1 --- --- [,]
217-227 A11 "DD/MMM/YYYY" Obs.date7 Date of observation
229-232 I4 s ExpTime7 ? Exposition time
233 A1 --- --- [,]
235-245 A11 "DD/MMM/YYYY" Obs.date8 Date of observation
247-249 I3 s ExpTime8 ? Exposition time
250 A1 --- --- [,]
252-262 A11 "DD/MMM/YYYY" Obs.date9 Date of observation
264-266 I3 s ExpTime9 ? Exposition time
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Note (1): The oldest designation is listed first except for stars with
variable star nomenclature
Note (2): Notes:
2MASS J05381494-0219532 : have poor quality spectra and, therefore,
were discarded from the analysis.
2MASS J05384652-0235479 : have poor quality spectra and, therefore,
were discarded from the analysis.
Mayrit 1500066 : was not tabulated by Gaia DR2, and its equatorial
coordinates are from 2MASS.
Mayrit 1245057AB : We took three spectra of Mayrit 1245057AB: one of
component A, one of B, and the two of them inside the slit in parallactic
angle.
Proper motions are taken from 2017A&A...600L...4A 2017A&A...600L...4A (HSOY, Cat. I/339)
sigma Ori AB : Proper motions are taken from 2005yCat.1297....0Z 2005yCat.1297....0Z
(UCAC4, Cat. I/322).
Mayrit 203283, : proper motions are taken from 2017A&A...600L...4A 2017A&A...600L...4A
(HSOY, Cat. I/339)
Mayrit 528005AB : proper motions are taken from 2017A&A...600L...4A 2017A&A...600L...4A
(HSOY, Cat. I/339)
Mayrit 1082115 : proper motions are taken from 2017A&A...600L...4A 2017A&A...600L...4A
(HSOY, Cat. I/339)
Mayrit 1500066 : proper motions are taken from 2017A&A...600L...4A 2017A&A...600L...4A
(HSOY, Cat. I/339)
Mayrit 1626148AB : We took two spectra of Mayrit 1626148AB: one of
component A and one of component B.
Proper motions are taken from 2005yCat.1297....0Z 2005yCat.1297....0Z (UCAC4, Cat. I/322)
Mayrit 180277 : was also observed on 06 Mar 2012 at an airmass of 1.25 for
900s with the volume-phase holographic grating R2500V
(R∼1400, Δλ∼4400-6000Å)
2E 1456 : is a galaxy previously thought to be a star. We did not account for
it in the analysis.
Mayrit 1298302 : was not tabulated by Gaia DR2 and its equatorial coordinates
are from 2MASS.
Proper motions are taken from 2017A&A...600L...4A 2017A&A...600L...4A (HSOY, Cat. I/339).
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Byte-by-byte Description of file: tablea3.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 20 A20 --- Name Star name (1)
21 A1 --- n_Name [*] *: observed also with the R150V grism
22- 26 F5.1 0.1nm EWHb ?=- Equivalent width of Hbeta 4861.33A line
28 A1 --- --- [-]
29- 31 F3.1 0.1nm e_EWHb ?=- Lower error of Hbeta equivalent width
33 A1 --- --- [+]
34- 36 F3.1 0.1nm E_EWHb ?=- Upper error of Hbeta equivalent width
38- 42 F5.2 0.1nm EWHeI ?=- Equivalent width of He I D3 5875.67A line
44 A1 --- --- [-]
45- 48 F4.2 0.1nm e_EWHeI ?=- Lower error of He I D3 equivalent width
50 A1 --- --- [+]
51- 54 F4.2 0.1nm E_EWHeI ?=- Upper error of He I D3 equivalent width
56- 62 F7.2 0.1nm EWHa ?=- Equivalent width of Halpha 6562.80A line
64 A1 --- --- [-]
65- 69 F5.2 0.1nm e_EWHa ?=- Lower error of Halpha equivalent width
71 A1 --- --- [+]
72- 75 F4.2 0.1nm E_EWHa ?=- Upper error of Halpha equivalent width
77- 81 F5.2 0.1nm EWLiI ?=- Equivalent width of Li I 6707.80A line
83 A1 --- --- [-]
84- 87 F4.2 0.1nm e_EWLiI ?=- Lower error of Li I equivalent width
89 A1 --- --- [+]
90- 93 F4.2 0.1nm E_EWLiI ?=- Upper error of Li I equivalent width
95- 97 A3 --- SpTypeMIL Spectral type derived from MILES
99-101 A3 --- SpTypePyH Spectral type derived from PyHammer
103-135 A33 --- AName Alternative star name
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Note (1): The oldest or variable designation is listed except for
sigma Orionis members with Mayrit identifier.
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Byte-by-byte Description of file: tablea4.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 16 A16 --- Name Star name (1)
17 A1 --- n_Name [*] *: were observed by Caballero et al.,
2012A&A...546A..59C 2012A&A...546A..59C
18 A1 --- l_EWCaK Limit flag on EWCaK
19- 24 F6.2 0.1nm EWCaK ?=- Equivalent width of Ca K 3933.66Å line
25 A1 --- --- [-]
26- 30 F5.2 0.1nm e_EWCaK ?=- Lower error of Ca K equivalent width
31 A1 --- --- [+]
32- 36 F5.2 0.1nm E_EWCaK ?=- Upper error of Ca K equivalent width
38 A1 --- l_EWCaH Limit flag on EWCaH
39- 43 F5.1 0.1nm EWCaH ?=- Equivalent width of Ca H 3968.47Å line
45 A1 --- --- [-]
46- 49 F4.1 0.1nm e_EWCaH ?=- Lower error of Ca H equivalent width
51 A1 --- --- [+]
52- 55 F4.1 0.1nm E_EWCaH ?=- Upper error of Ca H equivalent width
57 A1 --- l_EWHg Limit flag on EWHg
58- 62 F5.1 0.1nm EWHg ?=- Equivalent width of Hγ
4340.47Å line
64 A1 --- --- [-]
65- 68 F4.1 0.1nm e_EWHg ?=- Lower error of Hγ equivalent width
72 A1 --- --- [+]
73- 76 F4.1 0.1nm E_EWHg ?=- Upper error of Hγ equivalent width
78 A1 --- l_EWHb Limit flag on EWHb
79- 84 F6.2 0.1nm EWHb ?=- Equivalent width of Hβ
4861.33Å line
85 A1 --- --- [-]
86- 90 F5.2 0.1nm e_EWHb ?=- Lower error of Hβ equivalent width
92 A1 --- --- [+]
93- 97 F5.2 0.1nm E_EWHb ?=- Upper error of Hβ equivalent width
100-105 F6.2 0.1nm EWHeI ?=- Equivalent width of He I D3
5875.67Å line
107 A1 --- --- [-]
108-111 F4.2 0.1nm e_EWHeI ?=- Lower error of HeI D3 equivalent width
114 A1 --- --- [+]
115-118 F4.2 0.1nm E_EWHeI ?=- Upper error of HeI D3 equivalent width
121-126 F6.1 0.1nm EWHa ?=- Equivalent width of Hα
6562.80Å line
128 A1 --- --- [-]
129-132 F4.1 0.1nm e_EWHa ?=- Lower error of Hα equivalent width
135 A1 --- --- [+]
136-139 F4.1 0.1nm E_EWHa ?=- Upper error of Hα equivalent width
142 A1 --- l_EWLiI Limit flag on EWLiI
143-147 F5.2 0.1nm EWLiI ?=- Equivalent width of LiI 6707.80Å line
149 A1 --- --- [-]
150-153 F4.2 0.1nm e_EWLiI ?=- Lower error of LiI equivalent width
155 A1 --- --- [+]
156-159 F4.2 0.1nm E_EWLiI ?=- Upper error of LiI equivalent width
161-165 A5 --- SpTypeMIL Spectral type derived from MILES
167-168 A2 --- SpTypePyH Spectral type derived from PyHammer
170-202 A33 --- AName Alternative star name
--------------------------------------------------------------------------------
Note (1): The oldest or variable designation is listed except for
sigma Orionis members with Mayrit identifier.
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Byte-by-byte Description of file: tablea5.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 21 A21 --- Name Star name (1)
22 A1 --- n_Name [*] Note on Name (4)
23- 34 A12 --- SpTypeLit Spectral type from the literature
35- 40 A6 --- r_SpTypeLit Reference for SpTypeLit (2)
41- 47 A7 --- SpTypeAdo Spectral type adopted from this work
50 A1 --- fOB [o] Flag for early-type O and B stars (3)
53 A1 --- fmu [oya] Flag for concordant total proper
motion (3)
56 A1 --- fpi [oya] Flag for concordant parallax (3)
59 A1 --- fLiI [oxb] Flag for LiI detection in absorption (3)
62 A1 --- fHalpha [ob] Flag for Halpha detection in emission (3)
65 A1 --- fmIR [o] Flag for mid-infrared flux excess (3)
69 A1 --- fX-ray [o] Flag for X-ray emission (3)
74 A1 --- fMember [+z] Flag for membership in sigma Orionis (3)
76-108 A33 --- AName Alternative star name
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Note (1): The oldest or variable designation is listed except for
sigma Orionis members with Mayrit identifier
Note (2): References as follows:
GK58 = Greenstein & Keenan, 1958ApJ...127..172G 1958ApJ...127..172G
Gue81 = Guetter, 1981AJ.....86.1057G 1981AJ.....86.1057G
Nes95 = Nesterov et al., 1995A&AS..110..367N 1995A&AS..110..367N< Cat. III/182
Wol96 = Wolk, 1996PhDT........63W 1996PhDT........63W
HS99 = Houk & Swift, 1999mctd.book.....H 1999mctd.book.....H, Cat. III/214/
ZO02 = Zapatero Osorio et al., 2002A&A...384..937Z 2002A&A...384..937Z
Sac08 = Sacco et al., 2008A&A...488..167S 2008A&A...488..167S, Cat. J/A+A/488/167
Cab08 = Caballero et al., 2008A&A...491..515C 2008A&A...491..515C
Cab12 = Caballero et al., 2012A&A...546A..59C 2012A&A...546A..59C
Man13 = Bonnefoy et al., 2013A&A...551A.107M 2013A&A...551A.107M
Her14 = Hernandez et al., 2014ApJ...794...36H 2014ApJ...794...36H, Cat. J/ApJ/794/36
SD15 = Morgan and Keenan, 1973ARA&A..11...29M 1973ARA&A..11...29M
Note (3): Flags as follows:
a = stars inside the cluster member boundaries;
b = stars for which we measured such lines for the first time
o = stars with previous measurements from the literature
+ = sigma Orionis members in this work
y = stars outside the cluster member boundaries;
x = stars for which we have not found LiI in absorption;
z = fore- or background stars
& = ?????
Note (4): Notes:
Mayrit 873229AB = parallaxes are affected by close binarity
Mayrit 359179AB = parallaxes are affected by close binarity
Mayrit 528005AB = parallaxes are affected by close binarity
Mayrit 1285339 = have discordance in radial velocity
Mayrit 1275190 = have discordance in radial velocity
Mayrit 822170 = have discordance in radial velocity
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Acknowledgements:
Jose A. Caballero, caballero(at)cab.inta-csic.es
References:
Caballero, Paper I 2008A&A...478..667C 2008A&A...478..667C, Cat. J/A+A/478/667
Caballero, Paper II 2010A&A...514A..18C 2010A&A...514A..18C
Caballero et al., Paper III 2012A&A...546A..59C 2012A&A...546A..59C
(End) J. aballero [CAB], A. de Burgos [INT], P. Vannier [CDS] 19-Aug-2019