J/A+A/646/A46 Chamaeleon DANCe. Stellar population with Gaia-DR2 (Galli+, 2021)
Chamaeleon DANCe. Revisiting the stellar populations of Chamaeleon I and
Chamaeleon II with Gaia-DR2 data
Galli P.A.B., Bouy H., Olivares J., Miret-Roig N., Sarro L.M., Barrado D.,
Berihuete A., Bertin E.. Cuillandre J.C.
<Astron. Astrophys. 646, A46 (2021)>
=2021A&A...646A..46G 2021A&A...646A..46G (SIMBAD/NED BibCode)
ADC_Keywords: Associations, stellar ; Clusters, open ; Stars, distances
Keywords: open clusters and associations: individual: Chamaeleon -
stars: formation - stars: distances - methods: statistical -
parallaxes - proper motions
Keywords:
Chamaeleon is the southernmost low-mass star-forming complex within
200 pc from the Sun. Its stellar population has been extensively
studied in the past, but the current census of the stellar content is
not complete yet and deserves further investigation.
We take advantage of the second data release of the Gaia space mission
to expand the census of stars in Chamaeleon and to revisit the
properties of the stellar populations associated to the Chamaeleon I
(Cha I) and Chamaeleon II (Cha II) dark clouds.
We perform a membership analysis of the sources in the Gaia catalogue
over a field of 100 deg2 encompassing the Chamaeleon clouds, and
use this new census of cluster members to investigate the 6D structure
of the complex.
We identify 188 and 41 high-probability members of the stellar
populations in Cha I and Cha II, respectively, including 19 and 7 new
members. Our sample covers the magnitude range from G=6 to G=20 mag in
Cha I, and from G=12 to G=18 mag in Cha II. We confirm that the
northern and southern subgroups of Cha I are located at different
distances (191.4+0.8-0.8pc and 186.7+1.0-1.0pc), but they
exhibit the same space motion within the reported uncertainties. Cha
II is located at a distance of 197.5+1.0-0.9pc and exhibits a
space motion that is consistent with Cha I within the admittedly large
uncertainties on the spatial velocities of the stars that come from
radial velocity data. The median age of the stars derived from the
Hertzsprung-Russell diagram (HRD) and stellar models is about 1-2Myr,
suggesting that they are somewhat younger than previously thought. We
do not detect significant age differences between the Chamaeleon
subgroups, but we show that Cha II exhibits a higher fraction of
disc-bearing stars compared to Cha I.
This study provides the most complete sample of cluster members
associated to the Chamaeleon clouds that can be produced with Gaia
data alone. We use this new census of stars to revisit the 6D
structure of this region with unprecedented precision.
Description:
Kinematic properties and stellar parameters of the Chamaeleon stars
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 fields surveyed by our study and
the empirical isochrone of the Cha I and Cha II subgroups.
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
tablea1.dat 196 188 Properties of the 188 cluster members in Cha I
tablea2.dat 195 41 Properties of the 41 cluster members in Cha II
tablea3.dat 136 177150 Probabilities for p_in thresholds in Cha I
tablea4.dat 136 50707 Probabilities for p_in thresholds in Cha II
tablea5.dat 15 400 Empirical isochrone of Cha I
tablea6.dat 15 400 Empirical isochrone of Cha II
tablea7.dat 151 172 Stellar parameters of Chamaeleon stars
--------------------------------------------------------------------------------
See also:
J/A+A/470/281 : WFI optical photometry in Cha II dark cloud (Spezzi+, 2007)
J/ApJ/675/1375 : IRAC/MIPS photometry in Cha I (Luhman+, 2008)
J/A+A/601/A97 : Gaia-ESO Survey: Cha I members (Sacco+, 2017)
J/AJ/154/46 : Cha I members proper motions and photometry (Esplin+, 2017)
Byte-by-byte Description of file: tablea1.dat tablea2.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 7 A7 --- --- [GaiaDR2]
8- 26 I19 --- GaiaDR2 Gaia-DR2 source identifier
28- 29 I2 h RAh Right ascension (ICRS) at Ep=2015.5
31- 32 I2 min RAm Right ascension (ICRS) at Ep=2015.5
34- 38 F5.2 s RAs Right ascension (ICRS) at Ep=2015.5
40 A1 --- DE- Declination sign (ICRS) at Ep=2015.5
41- 42 I2 deg DEd Declination (ICRS) at Ep=2015.5
44- 45 I2 arcmin DEm Declination (ICRS) at Ep=2015.5
47- 50 F4.1 arcsec DEs Declination (ICRS) at Ep=2015.5
52- 58 F7.3 mas/yr pmRA Proper motion (right ascension), pmRA*cosDE
60- 64 F5.3 mas/yr e_pmRA Uncertainty of proper motion (right ascension)
66- 71 F6.3 mas/yr pmDE Proper motion (declination)
73- 77 F5.3 mas/yr e_pmDE Uncertainty of proper motion (declination)
79- 83 F5.3 mas plx Parallax
85- 89 F5.3 mas e_plx Uncertainty of parallax
91- 95 F5.2 --- RUWE RUWE
97-102 F6.4 --- prob Membership probability (from zero to one)
104-108 F5.2 km/s RV ?=0 Radial velocity
110-113 F4.2 km/s e_RV ?=0 Uncertainty of radial velocity
115 I1 --- r_RV [1/7]?=0 Reference for radial velocity (1)
117-121 F5.1 pc d Distance
123-125 F3.1 pc E_d Upper uncertainty of the distance
128-130 F3.1 pc e_d Lower uncertainty of the distance
132-136 F5.1 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
162-166 F5.1 km/s Wgal W-velocity component
168-170 F3.1 km/s E_Wgal Upper uncertainty of W-velocity component
173-175 F3.1 km/s e_Wgal Lower uncertainty of W-velocity component
177-187 A11 --- Cloud Molecular cloud of the Chamaeleon complex
189-196 A8 --- SED SED classification
--------------------------------------------------------------------------------
Note (1): References for radial velocities:
1 = Sacco et al. (2017A&A...601A..97S 2017A&A...601A..97S, Cat. J/A+A/601/A97)
2 = Nguyen et al. (2012ApJ...745..119N 2012ApJ...745..119N, Cat. J/ApJ/745/119)
3 = Guenther et al. (2007A&A...467.1147G 2007A&A...467.1147G)
4 = Joergens & Guenther (2001A&A...379L...9J 2001A&A...379L...9J)
5 = Biazzo et al. (2012A&A...547A.104B 2012A&A...547A.104B)
6 = Torres et al. (2006A&A...460..695T 2006A&A...460..695T, Cat. J/A+A/460/695)
7 = Gaia-DR2 (2018A&A...616A...1G 2018A&A...616A...1G), Cat. I/345)
--------------------------------------------------------------------------------
Byte-by-byte Description of file: tablea3.dat tablea4.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 7 A7 --- --- [GaiaDR2]
8- 26 I19 --- GaiaDR2 Gaia-DR2 source identifier
28- 48 E21.17 --- P050 [0/1] Probability derived from p_in=0.5 solution
50- 70 E21.17 --- P060 [0/1] Probability derived from p_in=0.6 solution
72- 92 E21.17 --- P070 [0/1] Probability derived from p_in=0.7 solution
94-114 E21.17 --- P080 [0/1] Probability derived from p_in=0.8 solution
116-136 E21.17 --- P090 [0/1] Probability derived from p_in=0.9 solution
--------------------------------------------------------------------------------
Byte-by-byte Description of file: tablea5.dat tablea6.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 7 F7.4 mag RPmag RP magnitude from Gaia-DR2
9- 15 F7.4 mag G-RP G-RP colour from Gaia-DR2
--------------------------------------------------------------------------------
Byte-by-byte Description of file: tablea7.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 7 A7 --- --- [GaiaDR2]
8- 26 I19 --- GaiaDR2 Gaia-DR2 source identifier
28- 29 I2 h RAh Right Ascension (ICRS) at Ep=2015.5
31- 32 I2 min RAm Right Ascension (ICRS) at Ep=2015.5
34- 38 F5.2 s RAs Right Ascension (ICRS) at Ep=2015.5
40 A1 --- DE- Declination sign (ICRS) at Ep=2015.5
41- 42 I2 deg DEd Declination (ICRS) at Ep=2015.5
44- 45 I2 arcmin DEm Declination (ICRS) at Ep=2015.5
47- 50 F4.1 arcsec DEs Declination (ICRS) at Ep=2015.5
52- 57 F6.3 mag Jmag 2MASS magnitude in J filter
59- 63 F5.3 mag e_Jmag ? Uncertainty of 2MASS magnitude in J filter
65- 68 F4.2 mag AJ Extinction in J-band
70- 73 F4.2 mag e_AJ ? Uncertainty of extinction in J-band
75- 79 A5 --- SpType Spectral type
81- 85 I5 K Teff Effective temperature
87- 89 I3 K e_Teff Uncertainty of effective temperature
91- 96 F6.3 Lsun L Luminosity
98-102 F5.3 Lsun E_L Upper uncertainty of L
105-109 F5.3 Lsun e_L Lower uncertainty of L
111-114 F4.1 Myr tBHAC15 ? Age from BHAC15 models
116-118 F3.1 Myr E_tBHAC15 ? Upper uncertainty in the age from BHAC15
121-123 F3.1 Myr e_tBHAC15 ? Lower uncertainty in the age from BHAC15
125-128 F4.1 Myr tSDF00 ? Age from SDF00 models
130-133 F4.1 Myr E_tSDF00 ? Upper uncertainty in the age from SDF00
136-138 F3.1 Myr e_tSDF00 ? Lower uncertainty in the age from SDF00
141-151 A11 --- Cloud Molecular cloud of the Chamaeleon complex
--------------------------------------------------------------------------------
Acknowledgements:
Phillip Galli, phillip.galli(at)u-bordeaux.fr
(End) Phillip Galli [LAB, France], Patricia Vannier [CDS] 04-Dec-2020