The Mean Spectral Energy Distribution and Stellar Mass Density of ...

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Sept 2006 Finding high redshift galaxies •Historically selected in the optical => redshifted rest-frame UV (e.g. Steidel et al. 1996, Madau et al. 1996) •UV selected galaxies are relatively unobscured and vigorously starforming Berkeley – Gregory Rudnick steidel et al. (2003)
Observing the buildup of stellar mass •One method is to measure the SFR(z) •Select galaxies in UV and convert UV light to SFR •assume IMF + dust •Dust extinction is important, but uncertain •Misses contribution from heavily obscured galaxies, e.g. Sub-mm galaxies Sept 2006 Berkeley – Gregory Rudnick Giavalisco et al. 2004
Page 1 and 2: Massive Galaxies, the Mean SED, and
Page 3 and 4: Sept 2006 How do Galaxies Grow? Ber
Page 5: Sept 2006 How do Galaxies Grow? Ber
Page 9 and 10: Sept 2006 What have deep NIR survey
Page 11 and 12: The most common massive galaxy at 2
Page 13 and 14: Queiscent Massive Galaxies Sept 200
Page 15 and 16: Sept 2006 Field-to-field Variance H
Page 17 and 18: How to address Science Questions
Page 19 and 20: Sept 2006 Volume Averaged rest-fram
Page 21: Sept 2006 The benefits of averaging
Page 24 and 25: Sept 2006 Observed ρ * Evolution B
Page 26: Sept 2006 Conclusions • Volume av

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