Advanced

Age and metallicity gradients in the Galactic Bulge - A differential study using HST/WFPC2

Feltzing, Sofia LU and Gilmore, G. (2000) In Astronomy & Astrophysics 355. p.949-965
Abstract
The Galactic Bulge has long been assumed to be a largely old stellar population. However, some recent studies based on observations with the HST WF/PC-1 and WFPC2 of stars in the Galactic Bulge have concluded that the old population may not make up more then 30% of the total. Other studies using HST/WFPC2 differential studies of `Bulge' globular clusters and field stars have found the bulge to be comparable in age to the Galactic Halo. A complication in all these studies is the presence of a substantial population of stars which mimic a young bulge population, but which may be, and are often assumed to be, foreground disk stars whose reddening and distance distributions happen to mimic a young bulge turnoff. We show, using number counts in... (More)
The Galactic Bulge has long been assumed to be a largely old stellar population. However, some recent studies based on observations with the HST WF/PC-1 and WFPC2 of stars in the Galactic Bulge have concluded that the old population may not make up more then 30% of the total. Other studies using HST/WFPC2 differential studies of `Bulge' globular clusters and field stars have found the bulge to be comparable in age to the Galactic Halo. A complication in all these studies is the presence of a substantial population of stars which mimic a young bulge population, but which may be, and are often assumed to be, foreground disk stars whose reddening and distance distributions happen to mimic a young bulge turnoff. We show, using number counts in HST/WFPC2 colour-magnitude diagrams of both field stars in the Bulge and of two `bulge' and one `disk' globular cluster (NGC6528, NGC6553, and NGC5927) that the stars interpreted as young in fact are foreground disk stars. Thus, we confirm that the bulk of the bulge field stars in Baade's Window are old. The existence of a young metal-rich population cannot, however, be ruled out from our data. We also test for age and metallicity gradients in the Galactic Bulge between the two low extinction windows Baade's window (l=1fdg1 , b=-4fdg8 ) and Sagittarius-I (l=1fdg3 , b=-2fdg7 ). We use the colour-magnitude diagram of a metal-rich globular cluster as an empirical isochrone to derive a metallicity difference of <~ 0.2 dex between Baade's window and SGR-I window. This corresponds to a metallicity gradient of <~ 1.3 dex/kpc, in agreement with recent near-IR CMD studies. Such a steep gradient, if detected, would require the existence of a short scale length inner component to the Bulge, most likely that prominent in the near infra red, which perhaps forms a separate entity superimposed on the larger, optical Bulge as observed in Baade's window. Based on observations with the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc. under NASA contract No. NAS5-26555 (Less)
Please use this url to cite or link to this publication:
author
organization
publishing date
type
Contribution to journal
publication status
published
subject
keywords
NGC6553 Galaxy: stellar content, Galaxy: abundances Galaxy: center Galaxy: general Galaxy: globular clusters: individual: NGC5927, NGC6528
in
Astronomy & Astrophysics
volume
355
pages
949 - 965
publisher
EDP Sciences
external identifiers
  • scopus:0000724604
ISSN
0004-6361
language
English
LU publication?
yes
id
f6dce675-9af1-4411-a6ef-42c77ac2c794 (old id 113711)
alternative location
http://aa.springer.de/bibs/0355003/2300949/small.htm
date added to LUP
2007-07-13 09:39:48
date last changed
2017-10-01 04:34:33
@article{f6dce675-9af1-4411-a6ef-42c77ac2c794,
  abstract     = {The Galactic Bulge has long been assumed to be a largely old stellar population. However, some recent studies based on observations with the HST WF/PC-1 and WFPC2 of stars in the Galactic Bulge have concluded that the old population may not make up more then 30% of the total. Other studies using HST/WFPC2 differential studies of `Bulge' globular clusters and field stars have found the bulge to be comparable in age to the Galactic Halo. A complication in all these studies is the presence of a substantial population of stars which mimic a young bulge population, but which may be, and are often assumed to be, foreground disk stars whose reddening and distance distributions happen to mimic a young bulge turnoff. We show, using number counts in HST/WFPC2 colour-magnitude diagrams of both field stars in the Bulge and of two `bulge' and one `disk' globular cluster (NGC6528, NGC6553, and NGC5927) that the stars interpreted as young in fact are foreground disk stars. Thus, we confirm that the bulk of the bulge field stars in Baade's Window are old. The existence of a young metal-rich population cannot, however, be ruled out from our data. We also test for age and metallicity gradients in the Galactic Bulge between the two low extinction windows Baade's window (l=1fdg1 , b=-4fdg8 ) and Sagittarius-I (l=1fdg3 , b=-2fdg7 ). We use the colour-magnitude diagram of a metal-rich globular cluster as an empirical isochrone to derive a metallicity difference of &lt;~ 0.2 dex between Baade's window and SGR-I window. This corresponds to a metallicity gradient of &lt;~ 1.3 dex/kpc, in agreement with recent near-IR CMD studies. Such a steep gradient, if detected, would require the existence of a short scale length inner component to the Bulge, most likely that prominent in the near infra red, which perhaps forms a separate entity superimposed on the larger, optical Bulge as observed in Baade's window. Based on observations with the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc. under NASA contract No. NAS5-26555},
  author       = {Feltzing, Sofia and Gilmore, G.},
  issn         = {0004-6361},
  keyword      = {NGC6553  Galaxy: stellar content,Galaxy: abundances  Galaxy: center  Galaxy: general  Galaxy: globular clusters: individual: NGC5927,NGC6528},
  language     = {eng},
  pages        = {949--965},
  publisher    = {EDP Sciences},
  series       = {Astronomy & Astrophysics},
  title        = {Age and metallicity gradients in the Galactic Bulge - A differential study using HST/WFPC2},
  volume       = {355},
  year         = {2000},
}