J/A+A/663/A148 OSTTA. I. 20 poorly studied open clusters (Carrera+, 2022)
One Star to Tag Them All (OSTTA). I.
Radial velocities and chemical abundances for 20 poorly studied open clusters.
Carrera R., Casamiquela L., Bragaglia A., Carretta E.,
Carbajo-Hijarrubia J., Jordi C., Alonso-Santiago J., Balaguer-Nunez L.,
Baratella M., D'Orazi V., Lucatello S., Soubiran C.
<Astron. Astrophys. 663, A148 (2022)>
=2022A&A...663A.148C 2022A&A...663A.148C (SIMBAD/NED BibCode)
ADC_Keywords: Clusters, open ; Abundances ; Optical
Keywords: stars: abundances - stars: evolution -
open clusters and association: general
Abstract:
Open clusters are ideal laboratories to investigate a variety of
astrophysical topics, from the properties of the Galactic disc to
stellar evolution models. For this purpose, we need to know their
chemical composition in detail. Unfortunately, the number of systems
with chemical abundances determined from high resolution spectroscopy
remains small.
Our aim is to increase the number of open clusters with radial
velocities and chemical abundances determined from high resolution
spectroscopy by sampling a few stars in clusters which had not been
previously studied.
We obtained high resolution spectra with the FIbre-fed Echelle
Spectrograph at Nordic Optical Telescope for 41 stars belonging to 20
open clusters. These stars have high astrometric membership
probabilities determined from the Gaia second data release.
We derived radial velocites for all the observed stars which were used
to confirm their membership to the corresponding clusters. For
Gulliver 37, we cannot be sure the observed star is a real member. We
derived atmospheric parameters for the 32 stars considered to be real
cluster members. We discarded five stars because they have very low
gravity or their atmospheric parameters were not properly constrained
due to low signal-to-noise ratio spectra. Therefore, detailed chemical
abundances were determined for 28 stars belonging to 17 clusters. For
most of them, this is the first chemical analysis available in the
literature. Finally, we compared the clusters in our sample to a large
population of well-studied clusters. The studied systems follow the
trends, both chemical and kinematical, described by the majority of
open clusters. It is worth mentioning that the three most metal-poor
studied clusters (NGC 1027, NGC 1750, and Trumpler 2) are enhanced in
Si, but not in the other α-elements studied (Mg, Ca, and Ti).
Description:
Effective temperatures, surface gravities, global metallicities and
abundances obtained from the spectroscopic analysis of the observed
stars.
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
tableb2.dat 354 30 Effective temperatures, surface gravities, and
global metallicities obtained from the
spectroscopic analysis of the observed stars
tableb5.dat 739 17 Average abundances for the observed clusters
--------------------------------------------------------------------------------
See also:
I/350 : Gaia EDR3 (Gaia Collaboration, 2020)
Byte-by-byte Description of file: tableb2.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 11 A11 --- Cluster Cluster name
13 A1 --- --- [G]
14- 32 I19 --- GaiaEDR3 Gaia EDR3 ot DR2 source_id
34- 40 F7.2 K Teff Effective temperature
42- 47 F6.2 K e_Teff Effective temperature error
49- 52 F4.2 [cm/s2] logg logarithmic surface gravity
56- 59 F4.2 [cm/s2] e_logg logarithmic surface gravity error
61- 65 F5.2 [-] [M/H] Global metallicity
70- 73 F4.2 [-] e_[M/H] Global metallicity error
75- 78 F4.2 km/s vmic Microturbulent velocity
82- 85 F4.2 km/s e_vmic Microturbulent velocity error
87- 92 F6.3 [-] [Na/H] Na abundance over H
98-101 F4.2 [-] e_[Na/H] Na abundance over H error
103-108 F6.3 [-] [Al/H] Al abundance over H
114-117 F4.2 [-] e_[Al/H] Al abundance over H error
119-124 F6.3 [-] [Mg/H] Mg abundance over H
130-133 F4.2 [-] e_[Mg/H] Mg abundance over H error
135-140 F6.3 [-] [Si/H] Si abundance over H
146-149 F4.2 [-] e_[Si/H] Si abundance over H error
151-156 F6.3 [-] [Ca/H] Ca abundance over H
162-165 F4.2 [-] e_[Ca/H] Ca abundance over H error
167-172 F6.3 [-] [Sc/H] Sc abundance over H
178-181 F4.2 [-] e_[Sc/H] Sc abundance over H error
183-188 F6.3 [-] [Ti/H] Ti abundance over H
194-197 F4.2 [-] e_[Ti/H] Ti abundance over H error
199-204 F6.3 [-] [V/H] V abundance over H
209-212 F4.2 [-] e_[V/H] V abundance over H error
214-219 F6.3 [-] [Cr/H] Cr abundance over H
225-228 F4.2 [-] e_[Cr/H] Cr abundance over H error
230-235 F6.3 [-] [Mn/H] Mn abundance over H
241-244 F4.2 [-] e_[Mn/H] Mn abundance over H error
246-251 F6.3 [-] [Fe/H] Fe abundance over H
257-260 F4.2 [-] e_[Fe/H] Fe abundance over H error
262-267 F6.3 [-] [Co/H] Co abundance over H
273-276 F4.2 [-] e_[Co/H] Co abundance over H error
278-283 F6.3 [-] [Ni/H] Ni abundance over H
289-292 F4.2 [-] e_[Ni/H] Ni abundance over H error
294-298 F5.2 [-] [Y/H] Y abundance over H
303-306 F4.2 [-] e_[Y/H] Y abundance over H error
308-313 F6.3 [-] [Ba/H] Ba abundance over H
319-322 F4.2 [-] e_[Ba/H] Ba abundance over H error
325-329 F5.2 [-] [Ce/H] Ce abundance over H
335-338 F4.2 [-] e_[Ce/H] Ce abundance over H error
340-345 F6.3 [-] [Nd/H] Nd abundance over H
351-354 F4.2 [-] e_[Nd/H] Nd abundance over H error
--------------------------------------------------------------------------------
Byte-by-byte Description of file: tableb5.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 11 A11 --- Cluster Cluster name
13- 31 F19.17 [-] [Na/H] Average Na over H
33- 52 F20.18 [-] e_[Na/H] Average Na over H dispersion
54- 75 F22.19 [-] [Mg/H] Average Mg over H
77- 96 F20.18 [-] e_[Mg/H] Average Mg over H dispersion
98-118 F21.18 [-] [Al/H] Average Al over H
120-139 F20.18 [-] e_[Al/H] Average Al over H dispersion
141-161 F21.18 [-] [Si/H] Average Si over H
163-182 F20.18 [-] e_[Si/H] Average Si over H dispersion
184-203 F20.17 [-] [Ca/H] Average Ca over H
205-224 F20.18 [-] e_[Ca/H] Average Ca over H dispersion
226-247 F22.19 [-] [Sc/H] Average Sc over H
249-268 F20.18 [-] e_[Sc/H] Average Sc over H dispersion
270-290 F21.18 [-] [Ti/H] Average Ti over H
292-311 F20.18 [-] e_[Ti/H] Average Ti over H dispersion
313-333 F21.18 [-] [V/H] Average V over H
335-354 F20.18 [-] e_[V/H] Average V over H dispersion
356-376 F21.18 [-] [Cr/H] Average Cr over H
378-397 F20.18 [-] e_[Cr/H] Average Cr over H dispersion
399-420 F22.19 [-] [Mn/H] Average Mn over H
422-441 F20.18 [-] e_[Mn/H] Average Mn over H dispersion
443-463 F21.18 [-] [Fe/H] Average Fe over H
465-484 F20.18 [-] e_[Fe/H] Average Fe over H dispersion
486-506 F21.18 [-] [Co/H] Average Co over H
508-527 F20.18 [-] e_[Co/H] Average Co over H dispersion
529-549 F21.18 [-] [Ni/H] Average Ni over H
551-570 F20.18 [-] e_[Ni/H] Average Ni over H dispersion
572-590 F19.16 [-] [Y/H] Average Y over H
592-609 F18.16 [-] e_[Y/H] Average Y over H dispersion
611-631 F21.18 [-] [Ba/H] Average Ba over H
633-652 F20.18 [-] e_[Ba/H] Average Ba over H dispersion
654-674 E21.18 [-] [Ce/H] Average Ce over H
676-695 F20.18 [-] e_[Ce/H] Average ce over H dispersion
697-717 F21.18 [-] [Nd/H] Average Nd over H
719-737 F19.17 [-] e_[Nd/H] Average Nd over H dispersion
739 I1 --- N Number of stars
--------------------------------------------------------------------------------
Acknowledgements:
Jimenez Carrera, jimenez.carrera(at)inaf.it
(End) Patricia Vannier [CDS] 17-Jul-2022