2022A&A...666A..62L


Query : 2022A&A...666A..62L

2022A&A...666A..62L - Astronomy and Astrophysics, volume 666A, 62 (2022/10-1)

High-resolution near-infrared spectroscopy of globular cluster and field stars toward the Galactic bulge.

LIM D., KOCH-HANSEN A.J., CHUN S.-H., HONG S. and LEE Y.-W.

Abstract (from CDS):

Globular clusters (GCs) play an important role in the formation and evolution of the Milky Way. New candidates are continuously found, particularly in the high-extinction low-latitude regions of the bulge, although their existence and properties have yet to be verified. In order to investigate the new GC candidates, we performed high-resolution near-infrared spectroscopy of stars toward the Galactic bulge using the Immersion Grating Infrared Spectrometer (IGRINS) instrument at the Gemini-South telescope. We selected 15 and 10 target stars near Camargo 1103 and Camargo 1106, respectively, which have recently been reported as metal-poor GC candidates in the bulge. In contrast to the classical approaches used in optical spectroscopy, we determined stellar parameters from a combination of line-depth ratios and the equivalent width of a CO line. The stellar parameters of the stars follow the common trends of nearby APOGEE sample stars in a similar magnitude range. We also determined the abundances of Fe, Na, Mg, Al, Si, S, K, Ca, Ti, Cr, Ni, and Ce through spectrum synthesis. There is no clear evidence of a grouping in radial velocity - metallicity space that would indicate the characterization of either object as metal-poor GCs. This result emphasizes the necessity of follow-up spectroscopy for new GC candidates toward the bulge, although we cannot completely rule out a low probability that we only observed nonmember stars. We also note discrepancies between the abundances of Al, Ca, and Ti when derived from the H- versus the K-band spectra. Although the cause of this discrepancy is not clear, the effects of atmosphere parameters or nonlocal thermodynamic equilibrium are discussed. Our approach and results demonstrate that IGRINS spectroscopy is a useful tool for studying the chemical properties of stars toward the Galactic bulge with a statistical uncertainty in [Fe/H] of ∼0.03 dex, while the systematic error through uncertainties of atmospheric parameter determination, at ∼0.14 dex, is slightly larger than in measurements from optical spectroscopy.

Abstract Copyright: © D. Lim et al. 2022

Journal keyword(s): techniques: spectroscopic - stars: abundances - Galaxy: bulge - globular clusters: individual: Camargo 1103 - globular clusters: individual: Camargo 1106 - infrared: stars

Simbad objects: 29

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Number of rows : 29
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2024
#notes
1 2MASS J17322736-3015592 * 17 32 27.3599981264 -30 15 59.371749671           ~ 1 0
2 2MASS J17323002-3018086 * 17 32 30.0146473291 -30 18 08.615484238           ~ 1 0
3 2MASS J17323290-3015096 * 17 32 32.9133052762 -30 15 09.619509773           ~ 1 0
4 Camargo 1106 Cl? 17 32 34 -30 16.8           ~ 4 0
5 2MASS J17323462-3017160 * 17 32 34.6304573058 -30 17 16.140354635           ~ 1 0
6 2MASS J17323474-3018303 * 17 32 34.7549726263 -30 18 30.384730416           ~ 1 0
7 2MASS J17323499-3017565 * 17 32 34.9841636943 -30 17 56.580049009           ~ 1 0
8 2MASS J17323628-3016451 * 17 32 36.2812908689 -30 16 45.205023592           ~ 1 0
9 2MASS J17323719-3016402 * 17 32 37.1723672444 -30 16 39.904292527           ~ 1 0
10 2MASS J17323720-3016566 * 17 32 37.2036752420 -30 16 56.591459937           ~ 1 0
11 2MASS J17323744-3018101 * 17 32 37.4463790609 -30 18 10.255715141           ~ 2 0
12 2MASS J18061926-2509341 * 18 06 19.2509807400 -25 09 34.078792480           ~ 1 0
13 2MASS J18062118-2511170 * 18 06 21.1826302818 -25 11 16.987141521           ~ 1 0
14 2MASS J18062575-2512006 * 18 06 25.7248649601 -25 12 00.303533072           ~ 1 0
15 2MASS J18062579-2509180 * 18 06 25.7938692144 -25 09 18.089270113           ~ 1 0
16 2MASS J18062652-2510405 * 18 06 26.5213078146 -25 10 40.384367634           ~ 1 0
17 2MASS J18062911-2512308 * 18 06 29.1266607673 -25 12 30.681583281           ~ 1 0
18 2MASS J18062918-2509590 * 18 06 29.1775368102 -25 09 59.106240696           ~ 1 0
19 2MASS J18062981-2510484 * 18 06 29.8120641705 -25 10 48.428133655           ~ 1 0
20 Camargo 1103 Cl? 18 06 31 -25 09.7           ~ 5 0
21 2MASS J18063151-2508510 * 18 06 31.5167268678 -25 08 50.918319933           ~ 1 0
22 2MASS J18063174-2511530 * 18 06 31.7371774351 -25 11 52.989573312           ~ 1 0
23 2MASS J18063241-2507052 * 18 06 32.4084094530 -25 07 05.262142833           ~ 1 0
24 2MASS J18063474-2509181 * 18 06 34.7380110119 -25 09 18.026783033           ~ 1 0
25 2MASS J18063694-2509100 * 18 06 36.9389439004 -25 09 10.020246248           ~ 1 0
26 2MASS J18063694-2510048 * 18 06 36.9485497545 -25 10 04.880087638           ~ 1 0
27 2MASS J18063977-2509023 * 18 06 39.7686105656 -25 09 02.338178339           ~ 1 0
28 NGC 6544 GlC 18 07 20.58 -24 59 50.4   11.36 9.90     ~ 299 0
29 NAME Galactic Bulge reg ~ ~           ~ 4309 0

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