J/A+A/664/A66 Gaia EDR3 young stellar clusters membership (Mendigutia+, 2022)
Gaia EDR3 comparative study of protoplanetary disk fractions in
young stellar clusters.
Mendigutia I., Solano E., Vioque M., Balaguer-Nunez L., Ribas A.,
Huelamo N., Rodrigo C.
<Astron. Astrophys. 664, A66 (2022)>
=2022A&A...664A..66M 2022A&A...664A..66M (SIMBAD/NED BibCode)
ADC_Keywords: Milky Way ; Clusters, open ; Parallaxes, trigonometric ;
Proper motions
Keywords: open clusters and associations: general - protoplanetary disks -
proper motions - parallaxes - virtual observatory tools
Abstract:
The lifetime of protoplanetary disks around young stars limits the
timescale of planet formation. A disk dissipation timescale ≤10Myr
was inferred from surveys that count the relative number of stars with
disks - the disk fraction - in young stellar clusters with different
ages. However, most previous surveys focused on the compact region
within ∼2pc of the clusters' centers, for which the disk fraction
information about the outer part is practically absent.
We aim to test if disk fraction estimates change when inferred from an
extended region around the clusters' centers.
Gaia EDR3 data and a best-suited, Virtual Observatory (VO)-based tool
- Clusterix - are used to identify member stars for a representative
sample of 19 young stellar clusters considering two concentric fields
of view (FOVs) with radii of 20pc and 2pc. Inner-disk fractions
associated with each FOV are identically derived from 2MASS
color-color diagrams and compared to each other.
Although the density of members is smaller in the periphery, the
absolute number of member stars is typically ∼5 times larger at
distances farther than ∼2pc from the clusters' centers. In turn, our
analysis reveals that the inner disk fractions inferred from the
compact and the extended regions are equal within ~±10%. A list of
member and disk stars identified in each cluster is provided and
stored in a VO-compliant archive, along with their membership
probabilities, angular distances to the center, and Gaia and
near-infrared data. Averaged values and plots that characterize the
whole clusters are also provided, including Hertzsprung-Russell
diagrams based on Gaia colors and absolute magnitudes for the sources
with known extinction.
Our results cover the largest fields ever probed when dealing with
disk fractions for all clusters analyzed, and imply that their
complete characterization requires the use of wide FOVs. However, the
comparative study does not support a previous hypothesis that disk
fractions should be significantly larger when extended regions are
considered. The resulting database is a benchmark for future detailed
studies of young clusters, whose disk fractions must be accurately
determined by using multiwavelength analysis potentially combined with
data from upcoming Gaia releases.
Description:
The table includes data for the members within ∼20pc from the center
of 19 young stellar clusters. Membership identification was based on
kinematic and spatial segregation using proper motions and parallaxes
from Gaia EDR3 (Gaia Collaboration et al., 2021A&A...649A...1G 2021A&A...649A...1G, Cat.
I/350). Sources with Gaia magnitudes G > 17, parallaxes ≤ 0, parallax
relative error ≥ 0.1 and renormalized unit weight error (RUWE) ≥ 1.4
are not included. Gaia coordinates, proper motions, parallaxes and
magnitudes are listed for each source, along with membership
probabilities inferred from Clusterix (Balaguer-Nunez et al.,
2020MNRAS.492.5811B 2020MNRAS.492.5811B, Cat. J/MNRAS/492/5811), angular distances to the
center of the corresponding clusters, and near-infrared colors from
2MASS (Skrutskie et al., 2006AJ....131.1163S 2006AJ....131.1163S, Cat. VII/233). The stars
with inner disks identified from 2MASS color-color diagrams are also
indicated. The absence of such an indication does not necessarily mean
that the star is diskless.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tablea1.dat 125 19 Young stellar clusters: regions and membership
tablea2.dat 166 8699 Data for the members within ∼20pc from the
center of 19 young stellar clusters
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See also:
I/350 : Gaia EDR3 (Gaia Collaboration, 2020)
VII/233 : The 2MASS Extended sources (IPAC/UMass, 2003-2006)
J/MNRAS/492/5811 : Clusterix 2.0 (Balaguer-Nunez+, 2020)
Byte-by-byte Description of file: tablea1.dat
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Bytes Format Units Label Explanations
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1- 11 A11 --- Cluster Cluster name
13- 20 F8.4 deg RAdeg Cluster central right ascension (ICRS)
22- 29 F8.4 deg DEdeg Cluster central declination (ICRS)
31- 33 I3 arcmin RFOV20pc FOV20pc cluster associated angular radius
35- 38 I4 --- NmembFOV20pc Number of members for FOV20pc
39 A1 --- --- [/]
40- 45 I6 --- NtotFOV20pc Total number of sources within FOV20pc
having Gaia EDR3 proper motions and
reliable parallaxes (1)
47- 50 F4.2 mas plxFOV20pc FOV20pc inferred mean parallax
52- 55 F4.2 mas e_plxFOV20pc FOV20pc inferred mean parallax error
57- 62 F6.2 mas/yr pmRAFOV20pc FOV20pc inferred mean proper motion
along RA
64- 67 F4.2 mas/yr e_pmRAFOV20pc FOV20pc inferred mean proper motion
along RA error
69- 73 F5.2 mas/yr pmDECFOV20pc FOV20pc inferred mean proper motion
along DE
75- 78 F4.2 mas/yr e_pmDECFOV20pc FOV20pc inferred mean proper motion
along DE error
80- 83 F4.1 arcmin RFOV2pc FOV2pc cluster associated angular radius
85- 87 I3 --- NmembFOV2pc Number of members for FOV2pc
88 A1 --- --- [/]
89- 92 I4 --- NtotFOV2pc Total number of sources within FOV2pc
having Gaia EDR3 proper motions and
reliable parallaxes (1)
94- 97 F4.2 mas plxFOV2pc FOV2pc Inferred mean parallax
99-102 F4.2 mas e_plxFOV2pc FOV2pc Inferred mean parallax error
104-109 F6.2 mas/yr pmRAFOV2pc FOV2pc Inferred mean proper motion
along RA
111-114 F4.2 mas/yr e_pmRAFOV2pc FOV2pc Inferred mean proper motion
along RA error
116-120 F5.2 mas/yr pmDECFOV2pc FOV2pc Inferred mean proper motion
along DE
122-125 F4.2 mas/yr e_pmDECFOV2pc FOV2pc Inferred mean proper motion
along DE error
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Note (1): total number of sources within the FOV having Gaia EDR3 proper motions
and reliable parallaxes (as defined in Sect. 2.1).
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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- 11 A11 --- Cluster Name of the host young stellar cluster
13- 22 F10.6 deg RAdeg Gaia EDR3 right ascension (ICRS) at Ep=2016.0
24- 33 F10.6 deg DEdeg Gaia EDR3 declination (ICRS) at Ep=2016.0
35- 41 F7.3 mas/yr pmRA Gaia EDR3 proper motion in RA
43- 47 F5.3 mas/yr e_pmRA Gaia EDR3 error proper motion in RA
49- 55 F7.3 mas/yr pmDE Gaia EDR3 proper motion in DE
57- 61 F5.3 mas/yr e_pmDE Gaia EDR3 error proper motion in DE
63- 68 F6.4 mas Plx Gaia EDR3 parallax
70- 75 F6.4 mas e_Plx Gaia EDR3 error parallax
77- 83 F7.4 mag BPmag ?=- Gaia EDR3 BP magnitude
85- 90 F6.4 mag e_BPmag ?=- Gaia EDR3 error BP magnitude
92- 98 F7.4 mag RPmag ?=- Gaia EDR3 RP magnitude
100-105 F6.4 mag e_RPmag ?=- Gaia EDR3 error RP magnitude
107-113 F7.4 mag Gmag Gaia EDR3 G magnitude
115-120 F6.4 mag e_Gmag Gaia EDR3 error G magnitude
122-129 F8.6 deg dcent Angular distance to the center of the cluster
131-135 F5.3 --- Prob [0/1] Membership probability
137-142 F6.3 mag H-K ?=- 2MASS H-K color
144-148 F5.3 mag e_H-K ?=- 2MASS error H-K color
150-155 F6.3 mag J-H ?=- 2MASS J-H color
157-161 F5.3 mag e_J-H ?=- 2MASS error J-H color
163-166 A4 --- Disk Presence ("yes") or possible presence ("yes?")
of an inner disk
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Acknowledgements:
Ignacio Mendigutia, imendigutia(at)cab.inta-csic.es
(End) Patricia Vannier [CDS] 27-Jun-2022