J/A+A/701/A100 Cluster Members in the APOGEE DR17. I. (Guerco+, 2025)
Open cluster members in the APOGEE DR17. I. Dynamics and star members.
Guerco R., Souto D., Fernandez-Trincado J.G., Daflon S., Cunha K.,
Sales-Silva J.V., Loaiza-Tacuri V., Smith V.V., Ortigoza-Urdaneta M.,
Roriz M.P.
<Astron. Astrophys. 701, A100 (2025)>
=2025A&A...701A.100G 2025A&A...701A.100G (SIMBAD/NED BibCode)
ADC_Keywords: Milky Way ; Clusters, open ; Infrared sources
Keywords: surveys - Galaxy: kinematics and dynamics -
open clusters and associations: general
Abstract:
Open clusters (OCs) are groups of stars formed from the same cloud of
gas and cosmic dust. They play an important role in studying stars'
formation and evolution and understanding galaxies' structure and
dynamics. The main objective of this work is to identify stars that
belong to open clusters using astrometric data from Gaia EDR3 and
spectroscopic data from APOGEE DR17. Furthermore, we investigate the
metallicity gradients and orbital properties of the open clusters in
our sample. By applying the HDBSCAN clustering algorithm to this data,
we identified observed stars in our galaxy with similar dynamics,
chemical compositions, and ages. The orbits of the open clusters were
also calculated using the GravPot16 code. We found 1987 stars
belonging to 49 open clusters, and 941 of these stars have
probabilities above 80% of belonging to open clusters. Our metallicity
gradient presents a two-slope shape for two measures of different
Galactic center distances, the projected Galactocentric distance, and
the guiding center radius to the Galactic Center, as already reported
in previous work. However, when we separate the open clusters by age,
we observe no significant difference in the metallicity gradient slope
beyond a certain distance from the Galactic center. Our results show a
shallower gradient for clusters younger than 2Gyr than those older
than 2Gyr. All our OCs dynamically assemble the Disk-like population
very well, and they are in prograde orbits, which is typical for
disk-like populations. Some OCs resonate with the Galactic bar at the
Lagrange points L4 and L5.
Description:
Open clusters are groups of stars formed from the same cloud of gas
and cosmic dust. They play an important role in studying stars'
formation and evolution and understanding galaxies' structure and
dynamics. This table contains the stars belonging to the open clusters
studied, along with their respective membership probabilities. The
column 'OC' indicates the cluster to which the star, identified in the
'ID' column, belongs.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tablea1.dat 85 1987 Stars belonging to the OCs
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Byte-by-byte Description of file: tablea1.dat
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Bytes Format Units Label Explanations
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1- 23 A23 --- ID Identification of stars (2MASS JHHMMSSss+DDMMSSs)
25- 37 A13 --- OC Identification of open clusters
39- 51 F13.9 deg RAdeg Right Ascension (J2000)
53- 66 F14.10 deg DEdeg Declination (J2000)
68- 85 F18.14 % Pmemb Probability of the star belonging to the
open cluster
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Acknowledgements:
Rafael Guerco, rafael.fraga(at)ucn.cl
(End) Rafael Guerco [Univ. Cat. del Norte], Patricia Vannier [CDS] 24-Jun-2025