2015A&A...579A.104S


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.08CEST03:45:04

2015A&A...579A.104S - Astronomy and Astrophysics, volume 579A, 104-104 (2015/7-1)

Chemical abundances of giant stars in NGC 5053 and NGC 5634, two globular clusters associated with the Sagittarius dwarf spheroidal galaxy?

SBORDONE L., MONACO L., MONI BIDIN C., BONIFACIO P., VILLANOVA S., BELLAZZINI M., IBATA R., CHIBA M., GEISLER D., CAFFAU E. and DUFFAU S.

Abstract (from CDS):

The tidal disruption of the Sagittarius dwarf spheroidal galaxy (Sgr dSph) is producing the most prominent substructure in the Milky Way (MW) halo, the Sagittarius Stream. Aside from field stars, it is suspected that the Sgr dSph has lost a number of globular clusters (GC). Many Galactic GC are thought to have originated in the Sgr dSph. While for some candidates an origin in the Sgr dSph has been confirmed owing to chemical similarities, others exist whose chemical composition has never been investigated. NGC 5053 and NGC 5634 are two of these scarcely studied Sgr dSph candidate-member clusters. To characterize their composition we analyzed one giant star in NGC 5053, and two in NGC 5634. We analyze high-resolution and signal-to-noise spectra by means of the MyGIsFOS code, determining atmospheric parameters and abundances for up to 21 species between O and Eu. The abundances are compared with those of MW halo field stars, of unassociated MW halo globulars, and of the metal-poor Sgr dSph main body population. We derive a metallicity of [FeII/H]=-2.26±0.10 for NGC 5053, and of [FeI/H]=-1.99±0.075 and -1.97±0.076 for the two stars in NGC 5634. This makes NGC 5053 one of the most metal-poor globular clusters in the MW. Both clusters display an α enhancement similar to the one of the halo at comparable metallicity. The two stars in NGC 5634 clearly display the Na-O anticorrelation widespread among MW globulars. Most other abundances are in good agreement with standard MW halo trends. The chemistry of the Sgr dSph main body populations is similar to that of the halo at low metallicity. It is thus difficult to discriminate between an origin of NGC 5053 and NGC 5634 in the Sgr dSph, and one in the MW. However, the abundances of these clusters do appear closer to that of Sgr dSph than of the halo, favoring an origin in the Sgr dSph system.

Abstract Copyright:

Journal keyword(s): Galaxy: abundances - globular clusters: individual: NGC 5053 - globular clusters: individual: NGC 5634 - galaxies: active - stars: abundances - galaxies: individual: Sgr dSph

VizieR on-line data: <Available at CDS (J/A+A/579/A104): table1.dat alllines.dat allsynth.dat>

Simbad objects: 19

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Number of rows : 19

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 NAME Whiting 1 GlC 02 02 56.8 -03 15 10           ~ 100 0
2 NAME Sgr Stream St* 02 22 +00.0           ~ 644 0
3 Cl Berkeley 29 OpC 06 53 04.2 +16 55 39   14.3       ~ 139 0
4 NGC 5053 GlC 13 16 27.09 +17 42 00.9     9.96     ~ 533 0
5 2MASS J13163595+1741127 RG* 13 16 35.9679244606 +17 41 12.744574835   15.52 14.48   13.39 ~ 9 0
6 HD 122563 Pe* 14 02 31.8456299772 +09 41 09.942736952 7.47 7.10 6.19 5.37 4.79 G8:III:Fe-5 746 0
7 Cl* NGC 5634 BFI 2 * 14 29 30.06480 -05 58 39.3924     14.776   13.295 ~ 2 0
8 NGC 5634 GlC 14 29 37.28 -05 58 35.1   10.69 10.05     ~ 246 0
9 Cl* NGC 5634 BFI 3 * 14 29 40.52160 -05 57 09.5940     14.761   13.329 ~ 2 0
10 NGC 5897 GlC 15 17 24.40 -21 00 36.4   10.16 8.52     ~ 337 0
11 NGC 6397 GlC 17 40 42.09 -53 40 27.6   7.39 5.17     ~ 1798 1
12 NGC 6534 G 17 56 08.5680229969 +64 17 01.502898328   15.5       ~ 14 0
13 NAME SDG G 18 55 03.1 -30 28 42   4.5 3.6     ~ 1737 2
14 M 54 GlC 18 55 03.33 -30 28 47.5           ~ 898 0
15 Cl Terzan 7 GlC 19 17 43.92 -34 39 27.8           ~ 359 0
16 Cl Arp 2 GlC 19 28 44.11 -30 21 20.3     12.41     ~ 298 0
17 Cl Terzan 8 GlC 19 41 44.41 -33 59 58.1     11.54     ~ 256 0
18 Cl Pal 12 GlC 21 46 38.84 -21 15 09.4     11.89     ~ 449 0
19 NAME Local Group GrG ~ ~           ~ 6970 0

    Equat.    Gal    SGal    Ecl

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2020.07.08-03:45:04

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