J/A+A/687/A66 Abundances in eight bulge stars (Da Silva+, 2024)
Abundances in eight bulge stars from the optical and near-infrared.
Da Silva P., Barbuy B., Ernandes H., Souza S.O., Fernandez-Trincado J.G.,
Gonzalez-Diaz D.
<Astron. Astrophys. 687, A66 (2024)>
=2024A&A...687A..66D 2024A&A...687A..66D (SIMBAD/NED BibCode)
ADC_Keywords: Milky Way ; Stars, fundamental ; Abundances ; Optical ;
Infrared ; Ultraviolet
Keywords: stars: abundances - Galaxy: bulge -
globular clusters: individual: NGC 6522 -
globular clusters: individual: NGC 6558 -
globular clusters: individual: HP 1 -
globular clusters: individual: Palomar 6
Abstract:
The abundances of the α-elements are key for understanding the
early chemical enrichment of the Galactic bulge. The elements of
interest present lines in different wavelength regions, and some of
them show lines only in part of the spectra. In the present work, the
CNO trio, the a-elements Mg, Si, Ca, and Ti, and odd-Z Na and Al are
examined as measured from optical and H-band lines.
The aim of this work is to carry out a detailed comparison of stellar
parameters and abundances derived in the optical and near-infrared
(H-band). We also inspect the best available lines for a list of bulge
stars previously analyzed by the Apache Point Observatory Galactic
Evolution Experiment (APOGEE) team in the H-band and by our group in
the optical. This work is mainly of interest to spectroscopists.
In the present work, we compared the stellar parameters and abundance
results derived from APOGEE H-band spectra with optical analyses based
on Ultraviolet and Visual Echelle Spectrograph at the Very Large
Telescope (VLT/UVES) data for eight bulge stars.
We point out the most suitable wavelength region for each of the
studied elements, and highlight difficulties in the derivation of
stellar parameters both in the optical and H-band. The near-infrared
will allow observations of a large number of stars in the near future
given new instruments soon to be available. The identification of
spectral lines in this spectral region and the investigation of their
reliability are ongoing efforts worldwide. New instruments will also
allow simultaneous observation of H-band and optical.
Description:
In this work, we compared abundance results obtained from optical
spectra (VLT/UVES) and H-band spectra (APOGEE) for eight bulge stars.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table2.dat 114 8 Sample stars: Identifications from internal name,
Gaia, 2MASS and OGLE numbers
table4.dat 108 38 Abundance ratios [X/Fe] for each star from
APOGEE ASPCAP DR17
table5.dat 107 23 *Abundance ratios [X/Fe] obtained from
UVES optical spectra
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Note on table5.dat: for sample stars from Barbuy et al. (2013A&A...559A...5B 2013A&A...559A...5B,
2014A&A...570A..76B 2014A&A...570A..76B, 2015A&A...580A..40B 2015A&A...580A..40B, 2016A&A...591A..53B 2016A&A...591A..53B,
2018ARA&A..56..223B 2018ARA&A..56..223B), Ernandes et al. (2018A&A...616A..18E 2018A&A...616A..18E,
2020A&A...640A..89E 2020A&A...640A..89E); Friaca & Barbuy (2017A&A...598A.121F 2017A&A...598A.121F); Lecureur et al.
(2007A&A...465..799L 2007A&A...465..799L); Souza et al. (2021A&A...656A..78S 2021A&A...656A..78S);
van der Swaelmen et al. (2016A&A...586A...1V 2016A&A...586A...1V).
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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 I1 --- Seq [1/8] Sequential number of the star
3- 13 A11 --- Field Field name
15- 19 A5 --- Name Name of the star (1)
22- 40 I19 --- GaiaDR3 Gaia DR3 identifier
42- 59 A18 --- 2MASS 2MASS name (2MHHMMSSss+DDMMSSs)
61- 66 I6 --- OGLE ?=- OGLE identification number
68- 69 I2 h RAh Right ascension (J2000)
71- 72 I2 min RAm Right ascension (J2000)
74- 79 F6.3 s RAs Right ascension (J2000)
81 A1 --- DE- Declination sign (J2000)
82- 83 I2 deg DEd Declination (J2000)
85- 86 I2 arcmin DEm Declination (J2000)
88- 93 F6.3 arcsec DEs Declination (J2000)
95-100 F6.3 mag Vmag V magnitude
102-107 F6.3 mag Imag I magnitude
109-114 F6.3 mag Hmag H magnitude
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Note (1): Star NGC 6522-402361 is also identified as B-107 in Barbuy et al.
(2014A&A...570A..76B 2014A&A...570A..76B), and stars OGLE-545277, -82 760 and -392 918 are also
identified as BW-b4, BW-b5 and BW-f6 in Lecureur et al. (2007A&A...465..799L 2007A&A...465..799L).
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Byte-by-byte Description of file: table4.dat table5.dat
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Bytes Format Units Label Explanations
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1- 2 A2 --- Code Code (1)
4- 7 A4 --- El Element
9- 14 F6.3 [-] [X/Fe]1 ?=- HP1-2 [X/Fe] abundance ratio
16- 20 F5.3 [-] e_[X/Fe]1 ? HP1-2 [X/Fe] abundance ratio error
22- 26 F5.2 [-] [X/Fe]2 ?=- NGC 6558-283 [X/Fe] abundance ratio
28- 31 F4.2 [-] e_[X/Fe]2 ? NGC 6558-283 [X/Fe] abundance ratio error
34- 38 F5.2 [-] [X/Fe]3 ?=- NGC 6558-1160 [X/Fe] abundance ratio
40- 43 F4.2 [-] e_[X/Fe]3 ? NGC 6558-1160 [X/Fe] abundance ratio error
46- 50 F5.2 [-] [X/Fe]4 ?=- OGLE 402361 [X/Fe] abundance ratio
52- 55 F4.2 [-] e_[X/Fe]4 ? OGLE 402361 [X/Fe] abundance ratio error
58- 63 F6.3 [-] [X/Fe]5 ?=- Palomar 6-401 [X/Fe] abundance ratio
65- 69 F5.3 [-] e_[X/Fe]5 ? Palomar 6-401 [X/Fe] abundance ratio error
71- 76 F6.3 [-] [X/Fe]6 ?=- OGLE 545277 [X/Fe] abundance ratio
78- 82 F5.3 [-] e_[X/Fe]6 ? OGLE 545277 [X/Fe] abundance ratio error
84- 89 F6.3 [-] [X/Fe]7 ?=- OGLE 82760 [X/Fe] abundance ratio
91- 95 F5.3 [-] e_[X/Fe]7 ? OGLE 82760 [X/Fe] abundance ratio error
97-102 F6.3 [-] [X/Fe]8 ?=- OGLE 392918 [X/Fe] abundance ratio
104-108 F5.3 [-] e_[X/Fe]8 ? OGLE 392918 [X/Fe] abundance ratio error
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Note (1): Code as follows:
Ap = result adopted as calibrated by the APOGEE project
As = spectroscopic ASPCAP abundance
U = UVES optical spectra
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History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 22-Aug-2024