J/AJ/169/214 Open clusters abundances from LAMOST/Gaia crossmatch (Yang+, 2025)
Chemical abundance gradients in open clusters from the Gaia/LAMOST sample.
Yang G., Zhao J., Yang Y., Liu N., Luo Y., Zhao G.
<Astron. J., 169, 214 (2025)>
=2025AJ....169..214Y 2025AJ....169..214Y
ADC_Keywords: Clusters, open; Abundances; Spectroscopy; Optical
Keywords: Galaxy abundances ; Galaxy evolution ; Open star clusters
Abstract:
Based on a large and homogeneous sample of 299 open clusters (OCs)
from Gaia DR3 and large sky area multiobject fiber spectroscopic
telescope DR11, we studied the abundance gradients of the
α-elements Mg and Si, and the iron-peak elements Fe and Ni to
explore the chemical evolution of the Galactic disk. A noticeable
downward trend in metallicities, with a slope of -0.048±0.008dex/kpc,
is observed as the Galactocentric distance (RGC) increases. The
abundance gradients of both α-elements and iron-peak elements in
our sample exhibit no apparent symmetry between the regions above and
below the Galactic plane. The metallicities in the sample, scaled to
the Galactocentric distance of the Sun, show an age-related increase
of 0.017±0.016dex/Gyr. [El/H] exhibits distinct downward trends
toward the outer Galaxy. In the inner Galaxy, younger OCs have lower
[El/H] values than older clusters, whereas in the outer Galaxy, this
trend is reversed. For OCs aged between 0.5 and 2.5Gyr, the number of
clusters migrating inward is approximately equal to those migrating
outward. However, the outward migration distances are notably greater
than the inward ones. Analyzing the impact of kinematic orbits on the
radial and vertical abundance gradients of the four elements, we found
that kinematic orbits exert minimal influence on the radial abundance
gradients for both α-elements and iron-peak elements. In
contrast, they have a pronounced effect on the vertical abundance
gradients.
Description:
In this study, we utilized the Gaia-based data provided by Hunt+2023
(J/A+A/673/A114) and the Large Sky Area Multi-Object Fiber
Spectroscopic Telescope (LAMOST) DR11 survey (DR7; V/156), both being
in the optical. We cross-matched the observational OC member stars in
Hunt+2023 with the spectroscopic catalog in LAMOST DR11 to obtain the
chemical abundances for common member stars of OCs. For each cluster,
we removed stars whose [Fe/H] deviated by more than three times the
standard deviation from the mean [Fe/H] of the cluster. Additionally,
clusters with only one member star were excluded owing to concerns
about reliability. Following the aforementioned selection criteria, we
identified 300 OCs for which both parameters and chemical abundances
were available.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 72 300 Basic parameters of the sample clusters in this work
table2.dat 80 300 Average abundances of the sample clusters in this
work
table3.dat 39 78 Comparisons of element abundances of clusters values
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See also:
I/355 : Gaia DR3 Part 1. Main source (Gaia Collaboration, 2022)
V/156 : LAMOST DR7 catalogs (Luo+, 2019)
J/A+A/377/911 : Age-metall. relation in solar neighbourhood (Feltzing+, 2001)
J/A+A/381/32 : Galactic Cepheid abundances (Andrievsky+, 2002)
J/AJ/125/1397 : Kinematics, age and abundances of open clusters (Chen+, 2003)
J/A+A/480/79 : Abund. of giants in five Galactic clusters (Bragaglia+, 2008)
J/A+A/480/91 : Gal. disk stars vertical distribution. IV. (Soubiran+, 2008)
J/AJ/139/1942 : Equivalent widths of red giants in 6 OCs (Friel+, 2010)
J/ApJ/724/341 : Nucleosynthesis of massive metal-free stars (Heger+, 2010)
J/AJ/142/51 : Galactic Cepheids abundance variations (Luck+, 2011)
J/AJ/144/95 : Abund. in stars of the outer galactic disk. IV. (Yong+, 2012)
J/A+A/566/A37 : Iron abundances for 42 Galactic Cepheids (Genovali+, 2014)
J/A+A/585/A150 : On the metallicity of open clusters. III. (Netopil+, 2016)
J/A+A/589/A115 : Na and Al abundances of 1303 stars (Smiljanic+, 2016)
J/A+A/603/A2 : Gaia-ESO Survey abundances radial distribution (Magrini+, 2017)
J/MNRAS/465/3203 : GALAH observational overview (Martell+, 2017)
J/AJ/156/142 : Precision clust. abund. for APOGEE with SDSS DR14 (Donor+, 2018)
J/A+A/623/A80 : Open clusters in APOGEE and GALAH surveys (Carrera+, 2019)
J/MNRAS/490/1821 : Abund. for stars in 18 open clusters (Casamiquela+, 2019)
J/A+A/643/A12 : Chemical abundances of 6 open cluster stars (Casali+, 2020)
J/AJ/159/199 : OCCAM. IV. Open cluster abund. using APOGEE DR16 (Donor+, 2020)
J/ApJ/891/23 : Stellar abundances from LAMOST MRS (SPCAnet) (Wang+, 2020)
J/A+A/640/A127 : Open cluster properties with Gaia and LAMOST (Zhong+, 2020)
J/MNRAS/503/3279 : GALAH surv. Galactic disc with open clusters (Spina+, 2021)
J/A+A/661/A104 : Physical parameters of classical Cepheids (da Silva+, 2022)
J/MNRAS/509/421 : Gal. metallicity gradient with open clusters (Netopil+ 2022)
J/A+A/666/A121 : Cluster target Giraffe HR15N RV precision (Randich+, 2022)
J/A+A/678/A195 : O, S, and Fe abund. in classical Cepheids (da Silva+, 2023)
J/A+A/673/A114 : Improving the open cluster census. II. (Hunt+, 2023)
J/A+A/669/A119 : Radial abund. gradient with open clusters (Magrini+, 2023)
J/A+A/690/A334 : Restricted sample of Gaia-ESO open clusters (Palla+, 2024)
http://www.lamost.org/dr11/v2.0/ : LAMOST DR11 v2.0
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 20 A20 --- Cluster Cluster identifier
22- 29 F8.4 kpc X [-12.9/-6.09] Galactic X position (1)
31- 37 F7.4 kpc Y [-1.13/3.9] Galactic Y position (1)
39- 45 F7.4 kpc Z [-0.44/0.81] Galactic Z position (1)
47- 52 F6.4 Gyr Age [3e-3/3.81] Cluster age (1)
54- 58 F5.2 kpc Rad [6.18/12.92] Current radius from galactic
center
60- 64 F5.2 kpc Rad0 [6.42/13.12] Birthplace radius from galactic
center
66- 72 F7.4 kpc Z0 [-0.93/0.76] Birthplace distance from galactic
plane
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Note (1): Adopted from Hunt+2023 (J/A+A/673/A114)
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Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1- 20 A20 --- Cluster Cluster identifier
22- 26 F5.2 [-] [Mg/H] [-0.62/0.4]? Log Mg/H abundance ratio
28- 31 F4.2 [-] e_[Mg/H] [0/0.23]? Uncertainty in [Mg/H]
33- 35 I3 --- o_[Mg/H] [2/275]? Number of stars used to determine
[Mg/H]
37- 41 F5.2 [-] [Si/H] [-0.6/0.3]? Log Si/H abundance ratio
43- 46 F4.2 [-] e_[Si/H] [0/0.17]? Uncertainty in [Si/H]
48- 50 I3 --- o_[Si/H] [2/275]? Number of stars used to determine
[Si/H]
52- 56 F5.2 [-] [Fe/H] [-0.63/0.3] Log Fe/H abundance ratio
58- 61 F4.2 [-] e_[Fe/H] [0/0.47] Uncertainty in [Fe/H]
63- 65 I3 --- o_[Fe/H] [2/313] Number of stars used to determine
[Fe/H]
67- 71 F5.2 [-] [Ni/H] [-0.5/0.3]? Log Ni/H abundance ratio
73- 76 F4.2 [-] e_[Ni/H] [0/0.24]? Uncertainty in [Ni/H]
78- 80 I3 --- o_[Ni/H] [2/275]? Number of stars used to determine
[Ni/H]
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Byte-by-byte Description of file: table3.dat
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Bytes Format Units Label Explanations
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1- 13 A13 --- Cluster Cluster identifier
15- 19 F5.2 [-] [Mg/H] [-0.58/0.39]? log Mg/H abundance ratio
21- 25 F5.2 [-] [Si/H] [-0.52/0.32]? log Si/H abundance ratio
27- 31 F5.2 [-] [Fe/H] [-0.48/0.31] log Fe/H abundance ratio
33- 37 F5.2 [-] [Ni/H] [-0.48/0.33]? log Ni/H abundance ratio
39- 39 I1 --- Ref [1/4] Literature reference (1)
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Note (1): Reference as follows:
1 = This work; 36 occurrences
2 = Myers+ (2022AJ....164...85M 2022AJ....164...85M); 34 occurrences
3 = Reddy+ (2016MNRAS.463.4366R 2016MNRAS.463.4366R); 5 occurrences
4 = Magrini+2023 (J/A+A/669/A119); 3 occurrences
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History:
From electronic version of the journal
(End) Prepared by [AAS], Robin Leichtnam [CDS] 14-Jan-2026