SIMBAD references

2012A&A...537A..83C - Astronomy and Astrophysics, volume 537A, 83-83 (2012/1-1)

Abundance analysis of the outer halo globular cluster Palomar 14.


Abstract (from CDS):

We determine the elemental abundances of nine red giant stars belonging to Palomar 14 (Pal 14). Pal 14 is an outer halo globular cluster (GC) at a distance of ∼70kpc. Our abundance analysis is based on high-resolution spectra and one-dimensional stellar model atmospheres. We derived the abundances for the iron peak elements Sc, V, Cr, Mn, Co, Ni, the α-elements O, Mg, Si, Ca, Ti, the light odd element Na, and the neutron-capture elements Y, Zr, Ba, La, Ce, Nd, Eu, Dy, and Cu. Our data do not permit us to investigate light element (i.e., O to Mg) abundance variations. The neutron-capture elements show an r-process signature. We compare our measurements with the abundance ratios of inner and other outer halo GCs, halo field stars, GCs of recognized extragalactic origin, and stars in dwarf spheroidal galaxies (dSphs). The abundance pattern of Pal 14 is almost identical to those of Pal 3 and Pal 4, the next distant members of the outer halo GC population after Pal 14. The abundance pattern of Pal 14 is also similar to those of the inner halo GCs, halo field stars, and GCs of recognized extragalactic origin, but differs from what is customarily found in dSphs field stars. The abundance properties of Pal 14, as well as those of the other outer halo GCs, are thus compatible with an accretion origin from dSphs. Whether or not GC accretion played a role, it seems that the formation conditions of outer halo GCs and GCs in dSphs were similar.

Abstract Copyright:

Journal keyword(s): stars: abundances - Galaxy: halo - globular clusters: individual: Pal 14

VizieR on-line data: <Available at CDS (J/A+A/537/A83): stars.dat tablea.dat>

Simbad objects: 31

goto Full paper

goto View the reference in ADS

To bookmark this query, right click on this link: simbad:2012A&A...537A..83C and select 'bookmark this link' or equivalent in the popup menu


© Université de Strasbourg/CNRS

    • Contact