2018A&A...616A..18E


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.08CEST04:14:18

2018A&A...616A..18E - Astronomy and Astrophysics, volume 616A, 18-18 (2018/8-1)

Iron-peak elements Sc, V, Mn, Cu, and Zn in Galactic bulge globular clusters.

ERNANDES H., BARBUY B., ALVES-BRITO A., FRIACA A., SIQUEIRA-MELLO C. and ALLEN D.M.

Abstract (from CDS):


Aims. Globular clusters are tracers of the history of star formation and chemical enrichment in the early Galaxy. Their abundance pattern can help understanding their chemical enrichment processes. In particular, the iron-peak elements have been relatively little studied so far in the Galactic bulge.
Methods. The main aim of this work is to verify the strength of abundances of iron-peak elements for chemical tagging in view of identifying different stellar populations. Besides, the nucleosynthesis processes that build these elements are complex, therefore observational data can help constraining theoretical models, as well as give suggestions as to the kinds of supernovae that enriched the gas before these stars formed.
Results. The abundances of iron-peak elements are derived for the sample clusters, and compared with bulge field, and thick disk stars. We derived abundances of the iron-peak elements Sc, V, Mn, Cu, and Zn in individual stars of five bulge globular clusters (NGC 6528, NGC 6553, NGC 6522, NGC 6558, HP 1), and of the reference thick disk/or inner halo cluster 47 Tucanae (NGC 104). High resolution spectra were obtained with the UVES spectrograph at the Very Large Telescope over the years.
Conclusions. The sample globular clusters studied span metallicities in the range -1.2≥[Fe/H]≥0.0. V and Sc appear to vary in lockstep with Fe, indicating that they are produced in the same supernovae as Fe. We find that Mn is deficient in metal-poor stars, confirming that it is underproduced in massive stars; Mn-over-Fe steadily increases at the higher metallicities due to a metallicity-dependent enrichment by supernovae of type Ia. Cu behaves as a secondary element, indicating its production in a weak-s process in massive stars. Zn has an alpha-like behaviour at low metallicities, which can be explained in terms of nucleosynthesis in hypernovae. At the metal-rich end, Zn decreases with increasing metallicity, similarly to the alpha-elements.

Abstract Copyright: © ESO 2018

Journal keyword(s): globular clusters: general - galaxies: abundances

CDS comments: Tables : star 2115 not identified. Table 1 stars 283, 364,1072 and 1160 are 2MASS J18102223-3145435, 2MASS J18102150-3145268, 2MASS J18101520-3146014 and 2MASS J18101768-3145246 in SIMBAD.

Simbad objects: 41

goto Full paper

goto View the reference in ADS

Number of rows : 41

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 NGC 104 GlC 00 24 05.359 -72 04 53.20   5.78 4.09     ~ 3547 0
2 Cl* NGC 104 HH 3006 * 00 24 47.2 -71 47 44   14.10 12.82     ~ 8 0
3 Cl* NGC 104 MEN 21 * 00 25 57.2 -71 49 28   14.96 14.10     ~ 5 0
4 [TSA2014] 5968 RG* 00 26 27.2101784729 -71 47 44.066383358 15.2 13.584 12.191   10.6 ~ 11 0
5 2MASS J00262847-7150127 RG* 00 26 28.4777692076 -71 50 12.803925706 15.3 13.808 12.4   11.0 ~ 10 0
6 [TSA2014] 5265 s?r 00 26 57.4520553905 -71 49 13.916021905 15.4 13.6 12.1   10.6 ~ 11 0
7 NAME LMC G 05 23 34.6 -69 45 22     0.4     ~ 14826 1
8 NAME Dwarf Elliptical Galaxy in Sex G 10 13 02.9 -01 36 53   12 10.4     ~ 706 0
9 * alf Boo RG* 14 15 39.67207 +19 10 56.6730 2.46 1.18 -0.05 -1.03 -1.68 K1.5IIIFe-0.5 2132 0
10 NAME UMi Galaxy G 15 09 11.34 +67 12 51.7   13.60 10.6     ~ 1178 0
11 NAME Dra dSph G 17 20 14.335 +57 55 16.39   12.40 10.6     ~ 1165 1
12 2MASS J17310273-2958544 * 17 31 02.7283284721 -29 58 54.737981773     17.327   14.721 ~ 2 0
13 2MASS J17310347-2958259 * 17 31 03.478 -29 58 25.96     17.101   14.487 ~ 2 0
14 ESO 455-11 GlC 17 31 05.20 -29 58 54.0           ~ 131 0
15 Cl* Haute-Provence 1 BZO 2 * 17 31 05.85 -29 58 35.5     16.982     ~ 4 0
16 Cl* Haute-Provence 1 BZO 3 * 17 31 05.87 -29 59 18.1     17.003     ~ 4 0
17 2MASS J17310729-2959021 * 17 31 07.295 -29 59 02.16     17.131   14.394 ~ 2 0
18 2MASS J17310817-2958147 * 17 31 08.173 -29 58 14.70     17.116   14.710 ~ 2 0
19 2MASS J17310822-2959108 * 17 31 08.225 -29 59 10.85     17.115   14.628 ~ 2 0
20 NAME Gal Center reg 17 45 40.04 -29 00 28.1           ~ 11535 0
21 [BZO2009] B-122 * 18 03 33.3582320567 -30 01 58.747401711     16.00   14.280 ~ 8 0
22 NGC 6522 GlC 18 03 34.08 -30 02 02.3   10.68 9.48     ~ 455 1
23 UCAC3 120-361873 * 18 03 36.5963155073 -30 02 16.463106350     15.98 15.56 15.40 ~ 12 0
24 Cl* NGC 6522 ARP 2091 * 18 03 41.0126109802 -30 03 03.411884262     16.302   14.642 ~ 9 0
25 Cl* NGC 6522 ARP 2008 * 18 03 44.6345452534 -30 02 10.845200999     16.260 16.06 14.35 ~ 9 0
26 2MASS J18044775-3003469 RG* 18 04 47.76 -30 03 47.0     16.42     ~ 9 0
27 NGC 6528 GlC 18 04 49.61 -30 03 20.8   12.12 10.65     ~ 465 0
28 Cl* NGC 6528 VY I-18 * 18 04 49.7 -30 03 02           ~ 2 0
29 Cl* NGC 6528 VY I-36 RG* 18 04 50.92 -30 03 48.0     16.41     ~ 4 0
30 Cl* NGC 6553 HAR 3008 * 18 09 13.06 -25 55 30.1           ~ 2 0
31 Cl* NGC 6553 WFI 267092 * 18 09 13.420 -25 55 01.85           ~ 2 0
32 NGC 6553 GlC 18 09 15.68 -25 54 27.9   9.08       ~ 535 0
33 Cl* NGC 6553 GOM 40056 * 18 09 17.960 -25 55 04.89   17.86 15.32     ~ 12 0
34 Cl* NGC 6553 HAR 2064 * 18 09 18.310 -25 55 01.15           ~ 2 0
35 Cl* NGC 6558 BZO F97 * 18 10 15.20 -31 46 01.5     16.037   14.467 ~ 5 0
36 2MASS J18101768-3145246 IR 18 10 17.68464 -31 45 24.6636           ~ 2 0
37 NGC 6558 GlC 18 10 18.38 -31 45 48.6   12.39 11.29     ~ 179 0
38 Cl* NGC 6558 BZO B73 * 18 10 21.5037029738 -31 45 26.770206814     15.709   14.187 ~ 8 0
39 2MASS J18102223-3145435 IR 18 10 22.23432 -31 45 43.5132           ~ 2 0
40 NAME SDG G 18 55 03.1 -30 28 42   4.5 3.6     ~ 1737 2
41 NAME Galactic Bulge reg ~ ~           ~ 3389 0

    Equat.    Gal    SGal    Ecl

To bookmark this query, right click on this link: simbad:objects in 2018A&A...616A..18E and select 'bookmark this link' or equivalent in the popup menu


2020.07.08-04:14:18

© Université de Strasbourg/CNRS

    • Contact