J/A+A/698/A295 Selected open clusters for validating APs (Tang+, 2025)
Selected open cluster sample for validating atmospheric parameters:
Application to Gaia and other surveys.
Tang T., Qin S., Zhong J., Jiang Y., Chen L.
<Astron. Astrophys. 698, A295 (2025)>
=2025A&A...698A.295T 2025A&A...698A.295T (SIMBAD/NED BibCode)
ADC_Keywords: Clusters, open ; Effective temperatures
Keywords: surveys - stars: fundamental parameters -
Hertzsprung-Russell and C-M diagrams -
open clusters and associations: general
Abstract:
Reliable stellar atmospheric parameters are essential for probing
stellar structure and evolution, and for stellar population studies.
However, various deviations appear in comparisons with different
ground-based spectroscopic surveys.
We aim to select high-quality open cluster members and employ the
atmospheric parameters provided by the theoretical isochrones of open
clusters as a benchmark to assess the quality of stellar atmospheric
parameters from Gaia DR3 and other ground-based spectroscopic surveys,
such as LAMOST DR11, APOGEE DR17, GALAH DR4.
We selected 130 open clusters with well-defined main sequences within
500pc of the solar neighborhood as a benchmark sample to estimate the
reference atmospheric parameters of the members from the best-fit
isochrones of those clusters. By comparing the atmospheric parameters
provided by different spectroscopic surveys to the theoretical
parameters, the atmospheric parameter deviation and the corresponding
dispersions exhibit different variations. The atmospheric parameter
deviations of F, G, and K-type stars are smaller than those of B, A,
and M-type stars for most surveys. For most samples, the dispersion of
Teff decreases as temperature decreases, whereas the dispersion of
logg shows an opposite trend.
Description:
We have selected 130 open clusters with well-defined main
sequences within 500pc in the solar neighborhood. We carried
out quality control using the corrected flux excess factor
of the BP and RP flux C*, and at the same time, we removed
the member stars whose binary mass ratio is greater than 0.5.
Then, we matched the remaining member stars to the best
isochrones in the color-magnitude diagram in the way of the
shortest distance to obtain their theoretical atmospheric
parameters. Ultimately, we provide the catalog with atmospheric
parameters of the member stars used for reference.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tablea1.dat 181 20780 Catalog of the member stars with theoretical
atmospheric parameters we used
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See also:
I/355 : Gaia DR3 Part 1. Main source (Gaia Collaboration, 2022)
Byte-by-byte Description of file: tablea1.dat
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Bytes Format Units Label Explanations
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1- 8 A8 --- Name The name of clusters we selected
11- 29 I19 --- GaiaDR3 Gaia DR3 identifier [source_id]
32- 49 F18.14 deg RAdeg Right ascension, Gaia DR3 (ICRS) at Ep=2016
52- 69 F18.14 deg DEdeg Declination, Gaia DR3 (ICRS) at Ep=2016
72- 80 F9.6 mag Gmag Gaia DR3, G magnitude
83- 90 F8.6 mag e_Gmag Gaia DR3, G magnitude error
93-101 F9.6 mag BPmag Gaia DR3, BP magnitude
104-111 F8.6 mag e_BPmag Gaia DR3, BP magnitude error
114-122 F9.6 mag RPmag Gaia DR3, RP magnitude
125-132 F8.6 mag e_RPmag Gaia DR3, RP magnitude error
135-144 F10.4 K Teffiso Estimated effective temperature
from isochrones
147-154 F8.4 K e_Teffiso Uncertainty in Teffiso
157-162 F6.4 [cm/s2] loggiso Estimated surface gravity from isochrones
165-171 F7.5 [cm/s2] e_loggiso Uncertainty in loggiso
174-181 F8.5 mag Distmin The minimum distance (1)
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Note (1): A positive value indicates that the member star is on the right side
of the isochrone, while a negative value indicates that it is on the left side.
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Acknowledgements:
Tong Tang, tangtong(at)shao.ac.cn
(End) Tong Tang [SHAO, China], Patricia Vannier [CDS] 13-May-2025