dIrrs

• LMC (Smecker-Hane et al 2001, Dolphin 2000, Holtzman et al 1999, Olsen 1999). No strong bursts obvious. Bar has different population from disk. Oldest clusters as old as oldest MW clusters. CMD, Smecker-Hane et al 2001, Fig 1 SFH, Smecker-Hane et al 2001, Fig 5

• SMC (Dolphin et al 2001, but also see Harris, this conference): no strong bursts evident. Oldest stars as old as oldest MW stars CMD, Dolphin et al 2001, Fig 8 SFH, Dolphin et al 2001, Fig 13

• IC10 (Hunter 2001): Stars down to  6 $M_\odot$. IMF in ``starburst'' consistent with normal, depending on SFH. IMF in field steeper than normal under assumption of constant SFR. Few small clusters, no super star clusters. CMD, Hunter 2001, Fig 6

• IC1613 (Skillman 2003): dominant intermediate age population, some old stars, no strong evidence for bursts CMD, Skillman et al 2003, Fig 2 SFH, Skillman et al 2003, Fig 14

• NGC 6822 (Wyder 2003, 2001, Gallart 1997): roughly constant SFR, with likely contribution from a very old population required CMD, Wyder 2003, Fig 2 SFH, Wyder 2003, Fig 2

• Sex A (Dolphin et al 2003) suggest relatively constant recent rate, but strong increase about 2.5 Gyr ago; data strongly inconsistent with constant SFR. Depends on accurate modelling of completeness for faintest stars. CMD, Dolphin et al 2003, Fig 1 SFH, Dolphin et al 2003, Fig 9

• WLM (Dolphin 2000): some old stars required (HB detected by Rejkuba et al 2000) , but then a lull in SF until more recent activity (but CMD is not particularly deep) CMD, Dolphin 2000, Fig 2 SFH, Dolphin 2000, Fig 3

• Pegasus: Gallagher 1998: SF probed only over last Gyr or so, roughly constant rate but with apparent significant recent increase. Aparicio et al 1997 suggest evidence for old population with recent bursting mode CMD, Gallagher et al 1997, Fig 4 SFH, Gallagher et al 2000, Fig 13

• GR8: Dohm-Palmer et al 1998: recent SF history relatively constant

• Leo A. Dolphin et al 2002 detect RR Lyraes, indicating ancient population. Schulte-Ladbeck also find RHB stars. Tolstoy et al suggested predominantly young galaxy, but apparently this is not the case. Population gradient exists.

• Sag DIG.

• LGS 3. Miller et al detect HB stars. Suggest strong component of very old stars, followed by much lower, but roughly constant SFH, with population gradient such that outer regions have more declining SFH. CMD, Miller et al 2001, Fig 3 SFH, Miller et al 2001, Fig 5

• Phoenix. Held et al and Holtzman et al find HB stars, and in fact, stars at wide range of ages CMD, Holtzman et al 2000, Fig 2 SFH, Holtzman et al 2000, Fig 6

• Aquarius.