dSphs

• NGC 205. Lee: Has young central population. Outer regions appear mostly old. Central region may have had continuous star formation until recently.

• NGC 147. Han et al: no younger stars, but apparent intermediate age population that is centrally concentrated.

• NGC 185. Martinez-Delgado et al: mostly old, but low level of continuous star formation up to present.

• Sagittarius: Bellazzini et al, Layden & Sarajedini: old stars present, likely as as as old MW globulars. LS suggest episodic star formation with 3 episodes, although don't quantify how discrete different populations are. CMD, Layden et al 2000, Fig 6

• Fornax: Saviane et al, Stetson et al, Buonanno et al: range of ages present, all the way up to a few hundred Myr. Possible gap between an older population and the intermediate-young population suggested by Saviane et al on basis of bimodal metallicity distribution. Buonanno et al suggest intermediate-young population is episodic (but clearly less so than Carina). CMD, Buonanno et al 2000, Fig 4

• Leo I. Dolphin suggests mostly intermediate (few Gyr) age stars, but some ancient stars. Held et al find RR Lyraes. No obvious strong bursts CMD, Dolphin 2001, Fig 14 SFH, Dolphin 2001, Fig 15

• Sculptor. Predominantly old, some intermediate age possible. Hurley-Keller et al find peculiar spur population that is centrally concentrated, find radial gradient in HB but no apparent age or metallicity gradient, and suggest gradient in binary star properties. Majewski et al suggest two distinct populations and radial metallicity gradient. CMD, Hurley-Keller et al 1999, Fig 1

• Leo II. Dolphin 2001: predominantly old and older-intermediate age, with extended star formation. Possible very few younger stars but relatively sharp termination of SF at a few Gyr. CMD, Dolphin 2001, Fig 8 SFH, Dolphin 2001, Fig 9

• Sextans. Likely significantly old, but some intermediate possible (Harbeck unpublished). Bellazzini et al find a mismatch in luminosity between the BHB and RHB and suggest two distinct populations in metallicity. CMD, Bellazzini et al 2001, Fig 1

• Carina. Clearly distinct episodes of star formation.

• Ursa Minor. Predominantly old. Ikuta and Arimoto suggest extended SF based on chemical evidence. CMD, Carrerra et al 2001, Fig 4

• Draco. Predominantly old.

• Antlia. Has old population but also likely younger population. CMD, Carrerra et al 2001, Fig 4

• Tucana. Predominantly old-intermediate age, no evidence for young popuation in this isolated galaxy. CMD, archival, Fig 4

• And companions