J/A+A/643/A148 Lupus DANCe. Census and 6D structure with Gaia-DR2 (Galli+, 2020)
Lupus DANCe. Census of stars and 6D structure with Gaia-DR2 data.
Galli P.A.B., Bouy H., Olivares J., Miret-Roig N., Vieira R.G., Sarro L.M.,
Barrado D., Berihuete A., Bertout C., Bertin E., Cuillandre J.C.
<Astron. Astrophys. 643, A148 (2020)>
=2020A&A...643A.148G 2020A&A...643A.148G (SIMBAD/NED BibCode)
ADC_Keywords: Associations, stellar ; Clusters, open ; Stars, distances ;
Stars, ages ; Effective temperatures
Keywords: open clusters and associations: individual: Lupus - stars: formation -
stars: distances - methods: statistical - parallaxes - proper motions
Abstract:
Lupus is recognised as one of the closest star-forming regions, but
the lack of trigonometric parallaxes in the pre-Gaia era hampered many
studies on the kinematic properties of this region and led to
incomplete censuses of its stellar population.
We use the second data release of the Gaia space mission combined with
published ancillary radial velocity data to revise the census of stars
and investigate the 6D structure of the Lupus complex. Methods: We
performed a new membership analysis of the Lupus association based on
astrometric and photometric data over a field of 160deg2 around the
main molecular clouds of the complex and compared the properties of
the various subgroups in this region.
We identified 137 high-probability members of the Lupus association of
young stars, including 47 stars that had never been reported as
members before. Many of the historically known stars associated with
the Lupus region identified in previous studies are more likely to be
field stars or members of the adjacent Scorpius-Centaurus association.
Our new sample of members covers the magnitude and mass range from
G~=8 to G~=18mag and from 0.03 to 2.4M☉, respectively. We
compared the kinematic properties of the stars projected towards the
molecular clouds Lupus 1 to 6 and showed that these subgroups are
located at roughly the same distance (about 160∼pc) and move with the
same spatial velocity. Our age estimates inferred from stellar models
show that the Lupus subgroups are coeval (with median ages ranging
from about 1 to 3Myr). The Lupus association appears to be younger
than the population of young stars in the Corona-Australis
star-forming region recently investigated by our team using a similar
methodology. The initial mass function of the Lupus association
inferred from the distribution of spectral types shows little
variation compared to other star-forming regions.
In this paper, we provide an updated sample of cluster members based
on Gaia data and construct the most complete picture of the
3D structure and 3D space motion of the Lupus complex.
Description:
Kinematic properties and stellar parameters of the Lupus members selected
in our membership analysis using Gaia-DR2 data. We provide for each star
its identifier, position, proper motion, parallax, radial velocity,
distance, spatial velocity, SED classification, age and membership
probability. We also provide the membership probabilities for all sources
in the field region surveyed by our study and the empirical isochrone
of the Lupus association.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tablea1.dat 205 137 Properties of the 137 Lupus members
tablea2.dat 138 10946139 Membership probability for p_in thresholds
tablea3.dat 35 400 Empirical isochrone of the Lupus association
tablea4.dat 91 110 Stellar parameters of Lupus stars
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See also:
I/345 : Gaia DR2 (Gaia Collaboration, 2018)
J/A+A/320/185 : UBVRIcJHKL photometry in Lup (Wichmann+ 1997)
J/A+A/529/A108 : Lupus clouds proper motion study with VO (Lopez Marti+, 2011)
J/MNRAS/331/474 : ubvyβ photometry in the Lupus dark cloud (Franco, 2002)
J/A+A/580/A26 : T Tauri star population in Lupus (Galli+, 2015)
J/A+A/602/A33 : X-Shooter spectroscopy of YSOs in Lupus (Frasca+, 2017)
J/A+A/600/A20 : Lupus YSOs X-shooter spectroscopy (Alcala+, 2017)
J/A+A/619/A52 : Dense cores and YSOs in Lupus complex (Benedettini+, 2018)
J/AJ/159/200 : YSOs objects in Lupus star-forming region (Melton, 2020)
Byte-by-byte Description of file: tablea1.dat
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Bytes Format Units Label Explanations
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1- 9 A9 --- --- [Gaia DR2 ]
10- 28 I19 --- GaiaDR2 Source identifier from Gaia-DR2 catalogue
30- 31 I2 h RAh Right ascension (ICRS) at Ep=2015.5
33- 34 I2 min RAm Right ascension (ICRS) at Ep=2015.5
36- 40 F5.2 s RAs Right ascension (ICRS)at Ep=2015.5
42 A1 --- DE- Declination sign (ICRS)at Ep=2015.5
43- 44 I2 deg DEd Declination (ICRS) at Ep=2015.5
46- 47 I2 arcmin DEm Declination (ICRS)at Ep=2015.5
49- 52 F4.1 arcsec DEs Declination (ICRS)at Ep=2015.5
54- 60 F7.3 mas/yr pmRA Proper motion in right ascension, pmRA*cosDE
62- 66 F5.3 mas/yr e_pmRA Uncertainty of proper motion in right ascension
68- 74 F7.3 mas/yr pmDE Proper motion in declination
76- 80 F5.3 mas/yr e_pmDE Uncertainty of proper motion in declination
82- 86 F5.3 mas plx Parallax
88- 92 F5.3 mas e_plx Uncertainty of parallax
94- 98 F5.2 --- RUWE RUWE
100-105 F6.4 --- prob [0/1] Membership probability (from zero to one)
107-110 F4.1 km/s RV ? Radial velocity
112-114 F3.1 km/s e_RV ? Uncertainty of radial velocity
116 I1 --- r_RV [1/5]? Reference for radial velocity (1)
118-122 F5.1 pc d Distance
124-126 F3.1 pc E_d Upper uncertainty of the distance
129-131 F3.1 pc e_d Lower uncertainty of the distance
133-136 F4.1 km/s Ugal ? U-velocity component
138-140 F3.1 km/s E_Ugal ? Upper uncertainty of U-velocity component
143-145 F3.1 km/s e_Ugal ? Lower uncertainty of U-velocity component
147-151 F5.1 km/s Vgal ? V-velocity component
153-155 F3.1 km/s E_Vgal ? Upper uncertainty of V-velocity component
158-160 F3.1 km/s e_Vgal ? Lower uncertainty of V-velocity component
162-165 F4.1 km/s Wgal ? W-velocity component
167-169 F3.1 km/s E_Wgal ? Upper uncertainty of W-velocity component
172-174 F3.1 km/s e_Wgal ? Lower uncertainty of W-velocity component
176-184 A9 --- Cloud Molecular cloud of the Lupus complex
186-190 F5.2 --- alpha ? SED spectral index
192-195 F4.2 --- e_alpha ? Uncertainty of the SED spectral index
197-205 A9 --- SED SED classification
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Note (1): References for radial velocities:
1 = Frasca et al. (2017A&A...602A..33F 2017A&A...602A..33F, Cat. J/A+A/602/A33)
2 = Guenther et al. (2007A&A...467.1147G 2007A&A...467.1147G)
3 = Wichmann et al. (1999MNRAS.307..909W 1999MNRAS.307..909W)
4 = Gontcharov et al. (2006AstL...32..759G 2006AstL...32..759G, Cat. III/252)
5 = Galli et al. (2013A&A...558A..77G 2013A&A...558A..77G)
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Byte-by-byte Description of file: tablea2.dat
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Bytes Format Units Label Explanations
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1- 9 A9 --- --- [Gaia DR2 ]
10- 28 I19 --- GaiaDR2 Source identifier from Gaia-DR2 catalogue
30- 50 E21.16 --- P050 Probability derived from p_in=0.5 solution
52- 72 E21.16 --- P060 Probability derived from p_in=0.6 solution
74- 94 E21.16 --- P070 Probability derived from p_in=0.7 solution
96-116 E21.16 --- P080 Probability derived from p_in=0.8 solution
118-138 E21.16 --- P090 Probability derived from p_in=0.9 solution
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Byte-by-byte Description of file: tablea3.dat
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Bytes Format Units Label Explanations
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1- 17 F17.14 mag RPmag RP magnitude from Gaia-DR2
19- 35 F17.15 mag G-RP G-RP colour from Gaia-DR2
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Byte-by-byte Description of file: tablea4.dat
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Bytes Format Units Label Explanations
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1- 9 A9 --- --- [Gaia DR2 ]
10- 28 I19 --- GaiaDR2 Source identifier from Gaia-DR2 catalogue
30- 33 I4 K Teff Effective temperature
35- 37 I3 K e_Teff Uncertainty of effective temperature
39- 44 F6.3 [Lsun] logL Logarithm of the luminosity
46- 50 F5.3 [Lsun] E_logL Upper uncertainty of logL
53- 57 F5.3 [Lsun] e_logL Lower uncertainty of logL
59- 61 F3.1 mag Av Extinction
63- 66 F4.1 Myr tBHAC15 ? Age from BHAC15 models
68- 71 F4.1 Myr E_tBHAC15 ? Upper uncertainty in the age from BHAC15
74- 77 F4.1 Myr e_tBHAC15 ? Lower uncertainty in the age from BHAC15
79- 82 F4.1 Myr tSDF00 ? Age from SDF00 models
84- 86 F3.1 Myr E_tSDF00 ? Upper uncertainty in the age from SDF00
89- 91 F3.1 Myr e_tSDF00 ? Lower uncertainty in the age from SDF00
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Acknowledgements:
Phillip Galli, phillip.galli(at)u-bordeaux.fr
(End) Phillip Galli [LAB, France], Patricia Vannier [CDS] 02-Oct-2020