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Extragalactic Background Fluctuation from the Numerical Galaxies. Hideki Yahagi DTAP, NAOJ Masahiro Nagashima Univ. of Durham Yuzuru Yoshii IoA, Univ. of Tokyo. Cosmic Background Radiation. Hauser & Dwek (2002). WMAP. Cosmic Microwave Background. Benett et al. (2003). ISO.

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extragalactic background fluctuation from the numerical galaxies

Extragalactic Background Fluctuationfromthe Numerical Galaxies

Hideki Yahagi DTAP, NAOJ

Masahiro Nagashima Univ. of Durham

Yuzuru Yoshii IoA, Univ. of Tokyo

cosmic background radiation
Cosmic Background Radiation

Hauser & Dwek (2002)

cosmic far ir background
ISOCosmic far-IR Background

Matsuhara et al. (2000)

gc n body sam
νGC = N-body + SAM
  • Dark matter carries most of mass in the Universe
    • Galaxies are baryonic components accumulated at the bottom of the potential well generated by dark matter
    • We can treat the evolution of dark matter distribution (by N-body method) and evolution of galaxies (by Semi-analytic model; SAM) separately
  • Spatial distribution →N-body
  • Other observable quantities →SAM
  • Kauffmann et al. (1999)
parameters of n body simulation
Parameters of N-body simulation
  • Computer:VPP-5000 (@ ADAC/NAOJ)
  • Number of particles:5123
  • Cosmological parameters:

W=0.3, l=0.7, s8=1.0

  • Box size:70h-1 Mpc
  • Movie
mass function of dark halos
Effective mass resolution is several 1010M8

(L = 70h-1Mpc)

Well-fitted by Sheth-Tormen type mass function

Mass Function of Dark Halos

Yahagi, Nagashima, and Yoshii (2003)

applications of gc
Angular correlation function of galaxies

Yahagi, Nagashima, Miyazaki, Gouda, & Yoshii

Extragalactic background fluctuation

Nagashima, Yahagi, & Yoshii

Cosmic string search

Japanese Virtual Observatory groups

Applications of νGC
angular correlation function
Wedge diagramAngular Correlation Function

40x40 arcmin2

RC<22

22<RC<24

24<RC<26

26<RC

angular correlation function1
Field-to-field variationAngular Correlation Function

(DD-2DR+RR)/RR(Landy & Szalay 1993)

angular correlation function2
Integral ConstraintsAngular Correlation Function

1+wtrue=<1+wtrue> =<1+wobs><(n/<n>)2 >

~1+<wobs>+σ2

angular correlation function4
Angular Correlation Function
  • Subaru Suprime-Cam
    • GTO 2.2 deg2 field
      • S. Miyazaki (Subaru telescope, NAOJ)et al.

Subaru Telescope

(National Astronomical Observatory of Japan)

Suprime-Cam

(National Astronomical Observatory)

extragalactic background fluctuation
Two-body correlation function of galaxies

Correlation function of galaxies brighter than the limiting magnitude

Edxtra-galactic background fluctuation

Correlation function of galaxies dimmer than the limiting magnitude

Extragalactic Background Fluctuation
extragalactic background fluctuation1
Diffuse extra-galactic background light (EBL)

Superposition of unresolved galaxies ?(NIR)

Expected outcome from EBL anisotropy

Source of EBL

Number of unresolved galaxies

IR Satellite projects

SIRTF

Astro-F, SPICA

Extragalactic Background Fluctuation
summary
Summary
  • N-body + SAM = νGC
    • High mass resolution
      • Parallelized AMR N-body simulation code
  • Comparison with observation
    • Angular correlation function
      • Our catalog realizes the observational data
    • Extragalactic background light
      • Our catalog fits the 2MASS results quite well
      • What is the origin of the excess at 10mins<?