Nobunari KashikawaNational Astronomical Observatory of Japan

appeared in Kashikawa et al., AJ, 125, 53, 2003Rest-frame Luminosity Functions Based on The K-Selected Galaxy Sample on The Subaru Deep Field

IntroductionApproach to explore the rest luminosity functionsphoto-z the best-fit SED template for each sample galaxy the rest-frame luminosity at any z and at any rest-wavelength less precise but deeper than spectroscopic sample Deep K-selected sampleK-band less sensitive to extinction, k-correction, current star-formation & tracing the rest- longer than age-sensitive spectral break at 4000Subaru Deep Field (SDF) 22 very deep (K

Rest-K LFno evolution up to z=2.5old stellar population was already in place by z=2-3Papovich et al. (2002) from stellar-mass estimatemassive present-day galaxies were not fully assembled by z=2.5save the hierarchical model ifM/LK decreases with z (Drory et al. 2002 for z

Rest-UV(2000A) LFconsistent with Cowie et al. (1999) @z

Evolution of Rest UV-K colorbluing trend@z1subsequent SF by merging @1

Star Formation Rate Densityrest UV-LF SFRDbroadly consistent with previous results @z1.5 due to the shallower faint- end slope of our UV-LFIf the slope of the rest UV-LF @ z=3 is really as steep as =-1.6, our K-selected sample contributes only 42% of the total UV luminosity density @ z=358%faint blue galaxies @z>3but uncertainty is large

N(z) on SDF

consistent with previous obs. on K

Subaru Deep Field ProjectOn-going Subaru Observatory Project to search high-z (4