Galactic globular cluster relative ages

被引:224
作者
Rosenberg, A
Saviane, I
Piotto, G
Aparicio, A
机构
[1] Osservatorio Astron Padova, Telescopio Nazl Galileo, I-35122 Padua, Italy
[2] Univ Padua, Dipartimento Astron, I-35122 Padua, Italy
[3] Inst Astrofis Canarias, E-38200 La Laguna, Tenerife, Spain
关键词
color-magnitude diagrams; Galaxy : evolution; Galaxy : formation; globular clusters : general; stars : Population II;
D O I
10.1086/301089
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
Based on a new large, homogeneous photometric database of 34 Galactic globular clusters (GGCs; plus Palomar 12), a set of distance- and reddening- independent relative age indicators has been measured. The observed delta(V-I)(2.5) and Delta V-TO(HB) versus metallicity relations have been compared with the relations predicted by two recently updated libraries of isochrones. Using these models and two independent methods, we have found that self-consistent relative ages can be estimated for our GGC sample. In turn, this demonstrates that the models are internally self-consistent. Based on the relative age versus metallicity distribution, we conclude that (1) there is no evidence of an age spread for clusters with [Fe/H] < -1.2, all the clusters of our sample in this range being old and coeval; (2) for the intermediate-metallicity group (-1.2 I [Fe/H] < -0.9), there is a clear evidence of age dispersion, with clusters up to similar to 25% younger than the older members; and (3) the clusters within the metal-rich group ([Fe/H] greater than or equal to -0.9) seem to be coeval within the uncertainties (except Pal 12) but younger (similar to 17%) than the bulk of the GGCs. The latter result is totally model dependent. From the Galactocentric distribution of the GGC ages, we can divide the GGCs in two groups: the old, coeval clusters and the young clusters. The second group can be divided into two subgroups: the "really young clusters" and the "young, but model dependent," which are within the intermediate- and high-metallicity groups, respectively. From this distribution, we can present a possible scenario for the Milky Way's formation: The globular cluster formation process started at the same zero age throughout the halo, at least out to similar to 20 kpc from the Galactic center. According to the present stellar evolution models, the metal-rich clusters are formed at a later time (similar to 17% lower age). Finally, significantly younger halo GGCs are found at any R-GC > 8 kpc. For these, a possible scenario associated with mergers of dwarf galaxies to the Milky Way is suggested.
引用
收藏
页码:2306 / 2320
页数:15
相关论文
共 44 条
[1]   THE PROPERTIES OF THE DISK SYSTEM OF GLOBULAR-CLUSTERS [J].
ARMANDROFF, TE .
ASTRONOMICAL JOURNAL, 1989, 97 (02) :375-389
[2]  
BERTELLI G, 1994, ASTRON ASTROPHYS SUP, V106, P275
[3]   CCD PHOTOMETRY OF THE GLOBULAR-CLUSTER NGC 1261 [J].
BOLTE, M ;
MARLEAU, F .
PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC, 1989, 101 (646) :1088-1104
[5]   MAIN-SEQUENCE CCD PHOTOMETRY OF THE GLOBULAR-CLUSTER NGC-362 [J].
BOLTE, M .
ASTROPHYSICAL JOURNAL, 1987, 315 (02) :469-479
[6]  
Buonanno R, 1998, ASTRON ASTROPHYS, V333, P505
[7]  
BUONANNO R, 1999, UNPUB
[8]   Abundances for globular cluster giants .1. Homogeneous metallicities for 24 clusters [J].
Carretta, E ;
Gratton, RG .
ASTRONOMY & ASTROPHYSICS SUPPLEMENT SERIES, 1997, 121 (01) :95-112
[9]  
CARRETTA E, 1999, UNPUB APJ
[10]   An updated theoretical scenario for globular cluster stars [J].
Cassisi, S ;
Castellani, V ;
Degl'Innocenti, S ;
Weiss, A .
ASTRONOMY & ASTROPHYSICS SUPPLEMENT SERIES, 1998, 129 (02) :267-279