J/A+A/701/A289 Stellar Population Astrophysics with the TNG (Dal Ponte+, 2025)
Stellar Population Astrophysics (SPA) with the TNG.
Non-local thermodynamic equilibrium atmospheric parameters and abundances of
giant stars in 33 open clusters.
Dal Ponte M, D'Orazi V., Bragaglia A., Casey A. R., Storm N., Spina L.,
Alonso-Santiago J., Andreuzzi G. Frasca A., Kos J., Lucatello S.,
Romano D., Vallenari A., Vernekar N.
<Astron. Astrophys. 701, A289 (2025)>
=2025A&A...701A.289D 2025A&A...701A.289D (SIMBAD/NED BibCode)
ADC_Keywords: Clusters, open ; Abundances ; Optical
Keywords: stars: abundances - stars: evolution - Galaxy: abundances -
Galaxy: disk - Galaxy: evolution -
open clusters and associations: general
Abstract:
Open clusters serve as important tools for accurately studying the
chemical evolution of the Milky Way. By combining precise chemical
data from high-resolution spectra with information on their distances
and ages, we can effectively uncover the processes that have shaped
our Galaxy.
This study aims to derive non-local thermodynamic equilibrium (NLTE)
atmospheric parameters and chemical abundances for approximately one
hundred giant stars across 33 open clusters with near-solar
metallicity. The clusters span a wide range of ages, enabling an
assessment of the presence and extent of any age-related abundance
gradients.
In the Stellar Population Astrophysics (SPA) project, we acquired new
high-resolution spectra of giant stars in a sample of open cluster
giants using the HARPS-N echelle spectrograph at the Telescopio
Nazionale Galileo. We chemically characterized nine open clusters for
the first time and reanalyzed previously studied SPA clusters,
resulting in a consistent and homogeneous sample.
We determined NLTE atmospheric parameters using the equivalent width
method and derived NLTE chemical abundances through spectral synthesis
for various elements, including alpha elements (Mg, Si, and Ti), light
odd-Z elements (Na, Al), iron-peak elements (Mn, Co, and Ni), and
neutron-capture elements (Sr, Y, and Eu). Our findings are compared
with the existing literature, revealing good agreement. We examine the
trends of [X/Fe] versus age, confirming previous observations and the
enrichment patterns predicted by nucleosynthesis processes. Positive
correlations with age are present for alpha elements such as Mg, Si,
Ti, odd-Z Al, and iron-peak elements Mn, Co, Ni, and Sr, while Na and
neutron-capture Y and Eu show a negative trend. This study emphasizes
the significance of NLTE corrections and reinforces the utility of
open clusters as tracers of Galactic chemical evolution. Furthermore,
we provide a benchmark sample of NLTE abundances for upcoming open
cluster surveys within large-scale projects such as 4MOST and WEAVE.
Description:
The table table2.dat contains the stellar parameters obtained with
LOTUS and the table table3.dat provides the chemical abundances
obtained with TSFitPy for the 95 stars presented in our work.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table2.dat 215 95 Stellar parameters from LOTUS
table3.dat 492 95 Chemical abundances from TSFitPy
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See also:
I/355 : Gaia DR3 Part 1. Main source (Gaia Collaboration, 2022)
Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 17 A17 --- Cluster Cluster name
19- 39 A21 --- Star Cluster star name
41- 59 I19 --- GaiaDR3 Gaia DR3 source identifier
61- 78 F18.13 K Teff LOTUS - Effective temperature
80- 97 F18.15 K e_Teff LOTUS - Effective temperature error
99-116 F18.16 [cm/s2] logg LOTUS - Surface gravity
118-135 F18.16 [cm/s2] e_logg LOTUS - Surface gravity error
137-156 E20.12 [-] [Fe/H] LOTUS - Metallicitty
158-177 F20.18 [-] e_[Fe/H] LOTUS - Metallicity error
179-196 F18.16 km/s Vmic LOTUS - Microturbulence
198-215 F18.16 km/s e_Vmic LOTUS - Microturbulence error
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Byte-by-byte Description of file: table3.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 17 A17 --- Cluster Cluster name
19- 39 A21 --- Star Cluster star name
41- 59 I19 --- GaiaDR3 Gaia DR3 source identifier
61- 82 F22.19 --- [Mg/Fe] ? TSFitPy - Magnesium abundance
84- 87 F4.2 --- e_[Mg/Fe] ? TSFitPy - Magnesium abundance error
89-109 E21.19 --- [Si/Fe] ? TSFitPy - Silicon abundance
111-130 F20.18 --- e_[Si/Fe] ? TSFitPy - Silicon abundance error
132-152 F21.18 --- [Ti/Fe] ? TSFitPy - Titanium abundance
154-173 F20.18 --- e_[Ti/Fe] ? TSFitPy - Titanium abundance error
175-195 E21.19 --- [Na/Fe] ? TSFitPy - Sodium abundance
197-217 F21.19 --- e_[Na/Fe] ? TSFitPy - Sodium abundance error
219-240 E22.19 --- [Al/Fe] ? TSFitPy - Aluminium abundance
242-262 E21.19 --- e_[Al/Fe] ? TSFitPy - Aluminium abundance error
264-285 F22.19 --- [Mn/Fe] ? TSFitPy - Manganese abundance
287-306 F20.18 --- e_[Mn/Fe] ? TSFitPy - Manganese abundance error
308-328 E21.19 --- [Co/Fe] ? TSFitPy - Cobalt abundance
330-349 F20.18 --- e_[Co/Fe] ? TSFitPy - Cobalt abundance error
351-372 F22.19 --- [Ni/Fe] ? TSFitPy - Nickel abundance
374-393 F20.18 --- e_[Ni/Fe] ? TSFitPy - Nickel abundance error
395-416 F22.19 --- [Sr/Fe] ? TSFitPy - Strontium abundance
418-421 F4.2 --- e_[Sr/Fe] ? TSFitPy - Strontium abundance error
423-443 F21.18 --- [Y/Fe] ? TSFitPy - Yttrium abundance
445-465 F21.19 --- e_[Y/Fe] ? TSFitPy - Yttrium abundance error
467-487 F21.19 --- [Eu/Fe] ? TSFitPy - Europium abundance
489-492 F4.2 --- e_[Eu/Fe] ? TSFitPy - Europium abundance error
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Acknowledgements:
Marina Dal Ponte, mari.dalponte(at)gmail.com
(End) Patricia Vannier [CDS] 15-Jul-2025