Rest-frame Luminosity Functions Based on The K’-Selected Galaxy Sample on The Subaru Deep Field
Download
1 / 8

Nobunari Kashikawa ( National Astronomical Observatory of Japan ) - PowerPoint PPT Presentation


  • 85 Views
  • Uploaded on

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

loader
I am the owner, or an agent authorized to act on behalf of the owner, of the copyrighted work described.
capcha
Download Presentation

PowerPoint Slideshow about ' Nobunari Kashikawa ( National Astronomical Observatory of Japan )' - druce


An Image/Link below is provided (as is) to download presentation

Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author.While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server.


- - - - - - - - - - - - - - - - - - - - - - - - - - E N D - - - - - - - - - - - - - - - - - - - - - - - - - -
Presentation Transcript

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 Galaxy Sample on The Subaru Deep Field

  • 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 Galaxy Sample on The Subaru Deep Field

  • 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 Galaxy Sample on The Subaru Deep Field

  • 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 Galaxy Sample on The Subaru Deep Field

  • bluing [email protected]<1 at any abs. mags.

  • [email protected]>1

  • →subsequent SF

  • by merging @1<z<3

  • more massivegalaxies (luminous in K’) are redder at every epoch


Star formation rate density
Star Formation Rate Density Galaxy Sample on The Subaru Deep Field

  • 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 Galaxy Sample on The Subaru Deep Field

  • 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 Galaxy Sample on The Subaru Deep Field

  • 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)


  • ad