WFPC2 observations of the Ursa Minor dwarf spheroidal galaxy

被引:53
作者
Mighell, KJ [1 ]
Burke, CJ [1 ]
机构
[1] Kitt Peak Natl Observ, Natl Opt Astron Observ, Tucson, AZ 85726 USA
关键词
galaxies : abundances; galaxies : evolution; galaxies : individual (Ursa Minor); Local Group;
D O I
10.1086/300923
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
We present our analysis of archival Hubble Space Telescope (HST) Wide Field Planetary Camera 2 (WFPC2) observations in F555W (similar to V and F814W (similar to I) of the central region of the Ursa Minor dwarf spheroidal (dSph) galaxy. The V versus V-I color-magnitude diagram features a sparsely populated blue horizontal branch, a steep thin red giant branch, and a narrow subgiant branch. The main sequence reaches approximately 2 mag below the main-sequence turnoff (V-TO(UMi) approximate to 23.27 +/- 0.11 mag) of the median stellar population. We compare the fiducial sequence of Ursa Minor with the fiducial sequence of the Galactic globular cluster M92 (NGC 6341). The excellent match between Ursa Minor and M92 confirms that the median stellar population of the UMi dSph galaxy is metal-poor ([Fe/H](UMi) approximate to [Fe/H](M92) approximate to -2.2 dex) and ancient (age(UMi) approximate to age(M92) approximate to 14 Gyr). The B-V reddening and the absorption in V are estimated to be E(B-V) = 0.03 +/- 0.01 mag and A(V)(UMi) = 0.09 +/- 0.03 mag. A new estimate of the distance modulus of Ursa Minor, (m - M)(o)(UMi) = 19.18 +/- 0.12 mag, has been derived based on fiducial-sequence fitting with M92 [Delta VUMi-M92 = 4.60 +/- 0.03 mag and Delta(V-I)(UMi-M92) = 0.010 +/- 0.005 mag] and the adoption of the apparent V distance modulus for M92 of (m-M)(V)(M92) = 14.67 +/- 0.08 mag. The Ursa Minor dSph galaxy is then at a distance of 69 +/- 4 kpc from the Sun. These HST observations indicate that Ursa Minor has had a very simple star formation history, consisting mainly of a single major burst of star formation about 14 Gyr ago that lasted less than or similar to 2 Gyr. While we may have missed minor younger stellar populations because of the small held of view of the WFPC2 instrument, these observations clearly show that most of the stars in the central region of the Ursa Minor dSph galaxy are ancient. If the ancient Galactic globular clusters such as M92 formed concurrently with the early formation of the Milky Way galaxy itself, then the Ursa Minor dwarf spheroidal is probably as old as the Milky Way.
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页码:366 / 380
页数:15
相关论文
共 36 条
[1]   THE UNIVERSE AT FAINT MAGNITUDES .1. MODELS FOR THE GALAXY AND THE PREDICTED STAR COUNTS [J].
BAHCALL, JN ;
SONEIRA, RM .
ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES, 1980, 44 (01) :73-110
[2]   AN ANALYSIS OF THE BASEL STAR CATALOG [J].
BAHCALL, JN ;
RATNATUNGA, KU ;
BUSER, R ;
FENKART, RP ;
SPAENHAUER, A .
ASTROPHYSICAL JOURNAL, 1985, 299 (02) :616-632
[3]   COMPARISONS OF A STANDARD GALAXY MODEL WITH STELLAR OBSERVATIONS IN 5 FIELDS [J].
BAHCALL, JN ;
SONEIRA, RM .
ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES, 1984, 55 (01) :67-99
[4]  
BIRETTA J, 1995, 9506 WFPC2
[5]  
BIRETTA JA, 1996, WFPC2 INSTRUMENT HDB
[6]   CONFLICT OVER THE AGE OF THE UNIVERSE [J].
BOLTE, M ;
HOGAN, CJ .
NATURE, 1995, 376 (6539) :399-402
[7]   REDDENINGS DERIVED FROM H-1 AND GALAXY COUNTS - ACCURACY AND MAPS [J].
BURSTEIN, D ;
HEILES, C .
ASTRONOMICAL JOURNAL, 1982, 87 (08) :1165-&
[8]  
CARETTA E, 1997, A AS, V121, P95
[9]   PROPER MOTIONS AND BRIGHT-STAR PHOTOMETRY IN THE URSA MINOR DWARF GALAXY [J].
CUDWORTH, KM ;
OLSZEWSKI, EW ;
SCHOMMER, RA .
ASTRONOMICAL JOURNAL, 1986, 92 (04) :766-776
[10]   REDDENINGS OF CEPHEIDS USING BVI PHOTOMETRY [J].
DEAN, JF ;
WARREN, PR ;
COUSINS, AWJ .
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, 1978, 183 (03) :569-583