J/A+A/685/A10 Heavy element in Galactic GC (Schiappacasse-Ulloa+, 2024)
Heavy element abundances in galactic globular clusters.
Schiappacasse-Ulloa J., Lucatello S., Cescutti G., Carretta E.
<Astron. Astrophys. 685, A10 (2024)>
=2024A&A...685A..10S 2024A&A...685A..10S (SIMBAD/NED BibCode)
ADC_Keywords: Milky Way ; Clusters, globular ; Abundances
Keywords: stars: abundances - stars: AGB and post-AGB - stars: Population II -
Galaxy: abundances - globular clusters: general - Galaxy: halo
Abstract:
Globular clusters are considered key objects for understanding the
formation and evolution of the Milky Way. In this sense, the
characterisation of their chemical and orbital parameters can provide
constraints on chemical evolution models of the Galaxy. We use the
heavy element abundances of globular clusters to trace their overall
behaviour in the Galaxy, with the aim to analyse potential relations
between the hot H-burning and s-process elements. We measured the
content of CuI and s- and r-process elements (YII, BaII, LaII, and
EuII) in a sample of 210 giant stars in 18 galactic globular clusters
from high-quality UVES spectra. These clusters span a broad
metallicity range and the sample is the largest that has been
uniformly analysed to date, with respect to heavy elements in globular
clusters. The Cu abundances did not show a considerable spread in the
sample, nor any correlation with Na, indicating that the Na
nucleosynthesis process does not affect the Cu abundance. Most GCs
closely follow the Cu, Y, Ba, La, and Eu field stars' distribution,
revealing a similar chemical evolution. The Y abundances in
mid-metallicity regime GCs (-1.10dex<[Fe/H]←1.80dex) display a mildly
significant correlation with the Na abundance, which ought to be
further investigated. Finally, we do not find any significant
difference between the n-capture abundances among GCs with either
Galactic and extragalactic origins.
Description:
Data of 210 star belonging to 18 Galactic Globular Clusters. We used
data from UVES spectra available on the ESO archive. The present
tables display our results (Table 2) for the abundances of Cu, Y, Ba,
La, and Eu and the sensitivity matrix (Table 3) showing the effect of
the variation of the stellar parameters on the abundance determination.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table2.dat 52 210 Abundance of Cu, Y, Ba, La, and Eu for a sample
of 210 stars
table3.dat 46 90 Element sensitivity to the stellar parameter
variations
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See also:
J/A+A/505/139 : Abundances of red giants in 17 globular clusters
(Carretta+, 2009)
J/A+A/600/A118 : Abundances of red giant stars in NGC6093 (M80)
(Carretta+, 2017)
Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1- 8 A8 --- Cluster NGC number
10- 16 I7 --- Star Star ID
17 A1 --- n_Star [*] Note on Star (1)
18 I1 --- l_[Cu/Fe] [0/1] Cu abundance flag (2)
20- 24 F5.2 [Sun] [Cu/Fe] Cu abundance
26- 30 F5.2 [Sun] [Y/Fe] Y abundance
32- 36 F5.2 [Sun] [Ba/Fe] Ba abundance
38 I1 --- l_[La/Fe] [0/1] La abundance flag (2)
40- 44 F5.2 [Sun] [La/Fe] La abundance
46 I1 --- l_[Eu/Fe] [0/1] Eu abundance flag (2)
48- 52 F5.2 [Sun] [Eu/Fe] Eu abundance
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Note (1): * for the star not in previous papers, initially named 99.999
set to 9999999.
Note (2): Limit flag as follows:
0 = actual measurement of the element
1 = upper limit in abundance determination
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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- 8 A8 --- Cluster NGC number
10- 14 A5 --- Element Element analysed
16- 20 F5.2 K Teff Effective temperature
22- 26 F5.2 [cm/s2] logg Gravity
28- 32 F5.2 [Sun] [Fe/H] Metallicity
34- 38 F5.2 km/s vm Microturbulent velocity
40- 46 I7 --- Star Star ID
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Acknowledgements:
Jose Schiappacasse-Ulloa, jschiappacasseu(at)gmail.com
(End) Jose Schiappacasse-Ulloa [PD, Italy], Patricia Vannier [CDS] 22-Mar-2024