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Rest-frame Luminosity Functions Based on The K’-Selected Galaxy Sample on The Subaru Deep Field. Nobunari Kashikawa ( National Astronomical Observatory of Japan ) appeared in Kashikawa et al., AJ, 125, 53, 2003. Introduction. Approach to explore the rest luminosity functions photo-z

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Rest-frame Luminosity Functions Based on The K’-Selected Galaxy Sample on The Subaru Deep Field

Nobunari Kashikawa

(National Astronomical Observatory of Japan)

appeared in Kashikawa et al., AJ, 125, 53, 2003

introduction
Introduction
  • Approach to explore the rest luminosity functions
    • photo-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 sample
    • K’-band → less sensitive to extinction, k-correction, current star-formation & tracing the rest-λ longer than age-sensitive spectral break at 4000Å
  • Subaru Deep Field (SDF)
    • 2’×2’ very deep (K’<25.5) K’-band imaged area
    • B<28.08, V<26.28, R<27.88, I<25.93, z’<24.27, J<25.5 (Vega, 5σ)
    • In this study, 439 galaxy sample with K’<24
    • we are now conducting a deep (R<28) and wide (34’×27’) follow-up optical imaging
rest k lf
Rest-K’ LF
  • no evolution up to z=2.5
  • old stellar population was already in place by z=2-3

⇔Papovich et al. (2002)

from stellar-mass estimate

“massive present-day galaxies were

not fully assembled by z=2.5”

  • save the hierarchical model if

“M/LK decreases with z” (Drory et al. 2002 for z<1.2)

No number evolution for

LK selected galaxies

Decreases with z for

M selected galaxies

  • Bolzonella et al. (2003)

no evolution of rest-Ks LF up to z=2

→consistent with our study

rest uv 2000a lf
Rest-UV(2000A) LF
  • consistent with
  • Cowie et al. (1999) @z<1.5 and
  • Steidel et al. (1999) @z=3
  • strong evolution (1.0mag brighter)
  • up to z=3.5
  • shallow faint end slope @z=3
  • The rest-B LF shows mild brightening with epoch up to z=2.5
evolution of rest uv k color
Evolution of Rest UV-K’ color
star formation rate density
Star Formation Rate Density
  • rest UV-LF → SFRD
  • broadly consistent with previous results @z<1.5
  • show slight deficiencies @z>1.5
  • ← due to the shallower faint-
  • end slope of our UV-LF
  • If the slope of the rest UV-LF @ z=3 is really as steep as α=-1.6, our K’-selected sample contributes only 42% of the total UV luminosity density @ z=3
  • 58%…
  • →faint blue galaxies @z>3?
  • but uncertainty is large
n z on sdf
N(z) on SDF
  • Kauffman&Charlot(1988) test for PLE vs. hierarchical model
  • consistent with previous obs. on K<21
  • first time to derive N(z) down to K=24
  • models - taking account of selection function of SDF & dust extinction
  • consistent with PLE on reliable mag. range 22<K<23
  • hierarchical model shows an apparent deficiency at z>2
  • KS-test also supports that PLE agree with obs.
  • The N(z) of FIRES (Daddi et al. in this proceedings) down to K=24 is consistent with our study.
subaru deep field project
Subaru Deep Field Project
  • On-going Subaru Observatory Project to search high-z (4<z<7) populations.
  • Survey: 34’x27’ wide FOV of Suprime-Cam
          • z’<26.5 (9.3hr exp.) NB921(14.0hr exp.)
          • i’<27.1 (11.0hr exp.) NB816(12.0hr exp.)
          • R<27.5 (10.2hr exp.)
          • B<27.8 (11.25 exp.)
          • Follow-up spectroscopy & NIR imaging
  • Discovery of two z=6.6 Lyman-alpha emitters (Kodaira et al. 2003)
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