J/A+A/691/A226 Abundances of globular cluster stars (Ceccarelli+, 2024)
A comparative high-resolution spectroscopic analysis of in situ and
accreted globular clusters.
Ceccarelli E., Mucciarelli A., Massari D., Bellazzini M., Matsuno T.
<Astron. Astrophys. 691, A226 (2024)>
=2024A&A...691A.226C 2024A&A...691A.226C (SIMBAD/NED BibCode)
ADC_Keywords: Clusters, globular ; Abundances ; Optical
Keywords: stars: abundances - Galaxy: formation - globular clusters: general
Abstract:
Globular clusters (GCs) are extremely intriguing systems that help in
reconstructing the assembly of the Milky Way via the characterisation
of their chemo-chrono-dynamical properties. In this study, we use
high-resolution spectroscopic archival data from UVES and UVES-FLAMES
at the VLT to compare the chemistry of GCs dynamically tagged as
either Galactic (NGC 6218, NGC 6522, and NGC 6626) or accreted from
distinct merger events (NGC 362 and NGC 1261 from
Gaia-Sausage-Enceladus, and Ruprecht 106 from the Helmi Streams) in
the metallicity regime where abundance patterns of field stars with
different origin effectively separate (-1.3<[Fe/H]←1.0dex). We find
remarkable similarities in the abundances of the two
Gaia-Sausage-Enceladus GCs across all chemical elements. They both
display depletion in the alpha-elements (Mg, Si and Ca) and
statistically significant differences in Zn and Eu compared to in situ
GCs. Additionally, we confirm that Ruprecht 106 exhibits a completely
different chemical makeup from the other target clusters, being
underabundant in all chemical elements. This demonstrates that when
high precision is achieved, the abundances of certain chemical
elements can not only efficiently separate in situ from accreted GCs,
but can also distinguish among GCs born in different progenitor
galaxies. In the end, we investigate the possible origin of the
chemical peculiarity of Ruprecht 106. Given that its abundances do not
match the chemical patterns of the field stars associated with its
most likely parent galaxy (i.e. the Helmi Streams), being depleted in
the abundances of alpha-elements in particular, we believe Ruprecht
106 to originate from a less massive galaxy compared to the progenitor
of the Helmi Streams.
Description:
GC, star ID, Gaia DR3 ID, abundances of Fe, Mg, Si, Ca, TiI, TiII,
ScII, V, Cr, Mn, Co, Ni, Cu, Zn, YII, BaI, LaII, and EuII. Stellar
spectra were retrieved from the ESO archive. Stars were observed with
UVES or UVES-FLAMES at VLT using the Red Arm 580 CD3 grating.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 51 66 GC, star ID, atmospheric parameters and
flag for good photometry
table2.dat 91 66 GC, star ID, abundances of FeI, Mg, Si, Ca,
TiI, and TiII
table3.dat 114 66 GC, star ID, abundances of ScII, V, Cr, Mn,
Co, Ni, Cu, and Zn
table4.dat 72 66 GC, star ID, abundances of YII, BaII, LaII,
and EuII
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See also:
I/355 : Gaia DR3 Part 1. Main source (Gaia Collaboration, 2022)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 6 A6 --- GC Target globular cluster
8- 14 A7 --- StarID Literature star ID
16- 34 I19 --- GaiaDR3 Gaia DR3 source_id
36- 39 I4 K Teff Effective temperature
41- 44 F4.2 [cm/s2] logg Surface gravity
46- 49 F4.2 km/s vt Microturbulent velocity
51 I1 --- Flag [0/1] Flag for quality of the photometry
(0=good, 1=bad)
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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- 6 A6 --- GC Target globular cluster
8- 14 A7 --- StarID Literature star ID
16- 20 F5.2 [Sun] [Fe/H] Abundance [Fe/H]
22- 25 F4.2 [Sun] e_[Fe/H] Uncertainty on the [Fe/H] abundance
27- 32 F6.2 [Sun] [Mg/Fe] ?=999 Abundance [Mg/Fe]
34- 39 F6.2 [Sun] e_[Mg/Fe] ?=999 Uncertainty on the [Mg/Fe] abundance
41- 45 F5.2 [Sun] [Si/Fe] Abundance [Si/Fe]
48- 51 F4.2 [Sun] e_[Si/Fe] Uncertainty on the [Si/Fe] abundance
53- 57 F5.2 [Sun] [Ca/Fe] Abundance [Ca/Fe]
60- 63 F4.2 [Sun] e_[Ca/Fe] Uncertainty on the [Ca/Fe] abundance
65- 69 F5.2 [Sun] [TiI/Fe] Abundance [TiI/Fe]
73- 76 F4.2 [Sun] e_[TiI/Fe] Uncertainty on the [TiI/Fe] abundance
79- 83 F5.2 [Sun] [TiII/Fe] Abundance [TiII/Fe]
88- 91 F4.2 [Sun] e_[TiII/Fe] Uncertainty on the [TiII/Fe] abundance
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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- 6 A6 --- GC Target globular cluster
8- 14 A7 --- StarID Literature star ID
17- 21 F5.2 [Sun] [ScII/Fe] Abundance [ScII/Fe]
26- 29 F4.2 [Sun] e_[ScII/Fe] Uncertainty on the [ScII/Fe] abundance
31- 35 F5.2 [Sun] [V/Fe] Abundance [V/Fe]
37- 40 F4.2 [Sun] e_[V/Fe] Uncertainty on the [V/Fe] abundance
42- 46 F5.2 [Sun] [Cr/Fe] Abundance [Cr/Fe]
49- 52 F4.2 [Sun] e_[Cr/Fe] Uncertainty on the [Cr/Fe] abundance
54- 58 F5.2 [Sun] [Mn/Fe] Abundance [Mn/Fe]
61- 64 F4.2 [Sun] e_[Mn/Fe] Uncertainty on the [Mn/Fe] abundance
66- 70 F5.2 [Sun] [Co/Fe] Abundance [Co/Fe]
73- 76 F4.2 [Sun] e_[Co/Fe] Uncertainty on the [Co/Fe] abundance
78- 82 F5.2 [Sun] [Ni/Fe] Abundance [Ni/Fe]
85- 88 F4.2 [Sun] e_[Ni/Fe] Uncertainty on the [Ni/Fe] abundance
90- 94 F5.2 [Sun] [Cu/Fe] Abundance [Cu/Fe]
97-100 F4.2 [Sun] e_[Cu/Fe] Uncertainty on the [Cu/Fe] abundance
102-107 F6.2 [Sun] [Zn/Fe] Abundance [Zn/Fe]
109-114 F6.2 [Sun] e_[Zn/Fe] Uncertainty on the [Zn/Fe] abundance
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Byte-by-byte Description of file: table4.dat
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Bytes Format Units Label Explanations
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1- 6 A6 --- GC Target globular cluster
8- 14 A7 --- StarID Literature star ID
16- 20 F5.2 [Sun] [YII/Fe] Abundance [YII/Fe]
24- 27 F4.2 [Sun] e_[YII/Fe] Uncertainty on the [YII/Fe] abundance
30- 34 F5.2 [Sun] [BaII/Fe] Abundance [BaII/Fe]
39- 42 F4.2 [Sun] e_[BaII/Fe] Uncertainty on the [BaII/Fe] abundance
44- 49 F6.2 [Sun] [LaII/Fe] Abundance [LaII/Fe]
54- 57 F4.2 [Sun] e_[LaII/Fe] Uncertainty on the [LaII/Fe] abundance
59- 64 F6.2 [Sun] [EuII/Fe] Abundance [EuII/Fe]
69- 72 F4.2 [Sun] e_[EuII/Fe] Uncertainty on the [EuII/Fe] abundance
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Acknowledgements:
Edoardo Ceccarelli, edoardo.ceccarelli3(at)unibo.it
(End) Patricia Vannier [CDS] 16-Oct-2024