1. Stellar AGB evolution and its impact on galaxy spectrophotometric properties at low and high redshift: an updated view Alberto Buzzoni INAF – Oss. Astronomico di Bologna, Italy

2. UV evolutionary paths for (old) low-mass stars Dorman et al. (1993) Core mass Renzini & Buzzoni (1986)

3. EHB stars Brown et al. (1999) Castellani et al. (2006)Buson et al. (2006) Low Z High Z Vassiliadis & Wood ‘94 Dorman et al. ‘93 (high-mass) MS

4. Back-in-time HB evolution Buzzoni (1989) Brown et al. (2000) HB temperature distribution

5. Buzzoni, Arnaboldi & Corradi (2006) The puzzling problem of Planetary Nebulae Weidemann (2000)

6. PNe and galaxy environment UV enhancedUV poor

7. Probing AGB extension

8. Mass loss & SB magnitudes Reimers’s law 

9. “Unconventional” fates

10. AGB deployment and UV upturn (when infrared speaks to ultraviolet) No PNe Buzzoni & Gonzàlez-Lòpezlira (2007) data compilation from Cantiello et al. (2003)

11. Toward a unitary picture? O’Connell (1999) UV enhanced UV poor Metal richMetal poor Globular clusters AGB ~ RGB [Fe/H]  lowest (« -0.5 dex) η  highest (0.4-0.5) Core mass  low (~0.54 Mo) HB  blue PN  poor rate Metal-rich GCs & dE’s AGB >> RGB [Fe/H]  intermediate (< 0.0 dex) η  lowest (0.0-0.1 ?) Core mass  highest (~0.65 Mo) HB  red PN  yes “standard” rate Ellipticals AGB > RGB [Fe/H]  highest (> 0.0 dex) η  low (0.1-0.3 ?) Core mass  lowest (<0.52 Mo) HB  blue due to metal-rich PN  poor rate Spiral galaxies AGB >> RGB η  VERY high (»1.5 ?) Core mass  highest (0.7-0.8 Mo) HB  red PN  yes “standard” rate UV enhanced?  yes but due to young