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Evolution of Galaxies from Modeling DEEP2 and SDSS Galaxy Clustering

Evolution of Galaxies from Modeling DEEP2 and SDSS Galaxy Clustering. Zheng Zheng I N S T I T U T E for ADVANCED STUDY with Alison Coil (University of Arizona) Idit Zehavi (Case Western Reserve University).

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Evolution of Galaxies from Modeling DEEP2 and SDSS Galaxy Clustering

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  1. Evolution of Galaxies from Modeling DEEP2 and SDSS Galaxy Clustering Zheng Zheng I N S T I T U T E for ADVANCED STUDY with Alison Coil (University of Arizona) Idit Zehavi (Case Western Reserve University) The 7th Sino-German Workshop on “Galaxies, Super-massive Black Holes, and the Cosmic Web” Shanghai, Sep. 25th 2006

  2. Outline • Halo Occupation Distribution (HOD) • HOD Modeling of DEEP2 and SDSS Galaxy Clustering Comparison of HODs at z~1 and z~0 • Evolution of Galaxies from z~1 to z~0 • Summary and Future Work

  3. Cosmological Model initial conditions energy & matter contents Galaxy Formation Physics gas dynamics, cooling star formation, feedback m 8ns  Dark Halo Population n(M) (r|M) v(r|M) Halo Occupation Distribution P(N|M) spatial bias within halos velocity bias within halos Galaxy Clustering Galaxy-Mass Correlations

  4. Galaxy Samples DEEP2, z~1 Coil et al 2006 SDSS, z~0 Zehavi et al 2005 Measurements of two-point correlation functions as a function of luminosity

  5. Two-point correlation function of galaxies Excess probability w.r.t. random distribution of finding galaxy pairs at a given separation 1-halo term Central 2-halo term Satellite

  6. Scatter between galaxy luminosity and host halo mass M1 - mass of a halo on average hosting one satellite galaxy above Lmin Mmin - characteristic minimum mass of halos hosting Lmin galaxies Halo Occupation Distribution Motivated by predictions of galaxy formation models. For a sample of galaxies more luminous than Lmin * Mean occupation function of central galaxies: step-like function * Mean occupation function of satellite galaxies: powerlaw-like function scatter following Poisson distribution

  7. Modeling results DEEP2 galaxies L

  8. Distribution of central galaxy luminosity Mean Scatter Lc: steep increase and large scatter in low mass halos

  9. Mass scales of host halos The scaling relation between Mmin and M1 does not seem to evolve much, M1~16Mmin at z~1 M1~18Mmin at z~0

  10. Satellite fraction Decreasing with luminosity Above the same L/L*, more satellites in z~0 SDSS galaxies than in z~1 DEEP2 galaxies

  11. Establishing an evolution link between DEEP2 and SDSS galaxies z~1 z~0 Growth of DM halos

  12. z~1 z~1 Star Formation Merging Merging z~0 z~0 Stellar mass evolution

  13. Star formation efficiency vs Halo mass

  14. Stellar mass evolution (z~1 to z~0) as a function of halo mass

  15. z~1 Star Formation Merging z~0

  16. Fardal et al. 2006 Tentative conclusion: For central galaxies in z~0 M<1012 h-1Msun halos, ~80% of their stars form after z~1 For central galaxies in z~0 M>1012 h-1Msun halos, ~25% of their stars form after z~1

  17. Summary & Future Work • HODs at z~1 and z~0 from modeling two-point correlation functions of DEEP2 and SDSS galaxies Evolution link through halo evolution Stellar mass evolution from z~1 to z~0 for central galaxies as a function of halo mass (pure merger vs star formation) Useful constraints to galaxy formation models Clustering measurements for galaxy samples based on stellar mass Galaxy samples at different redshifts Luminous end of galaxies Evolution of satellite galaxies

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