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Simulation of High- z Dust Enrichment

Simulation of High- z Dust Enrichment. H. Hirashita (University of Tsukuba) T. Suwa (Univ. of Tsukuba). Contents. Sub-mm Galaxies at High- z Models ( N -body + Dust) Results Strategy for Survey Observation. 1. Sub-mm Galaxies at High- z.

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Simulation of High- z Dust Enrichment

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  1. Simulation of High-z Dust Enrichment H. Hirashita (University of Tsukuba) T. Suwa (Univ. of Tsukuba)

  2. Contents • Sub-mm Galaxies at High-z • Models (N-body + Dust) • Results • Strategy for Survey Observation

  3. 1. Sub-mm Galaxies at High-z Luminosity function at 850 mm (Chapman et al. 2005) A lot of sub-mm luminous galaxies are found up to z ~ 3. z ~ 2.5 z ~ 1

  4. Relation with Optical Samples Number：Lya blobs Thick ○：with sub-mm ~ 5×1012 Lsun Geach et al. (2005) z = 3.1

  5. Galaxy Evolution Scenario in Optical Mori & Umemura (2006) Optical spectra evolve from Lya-emitter-like properties Lyman-break-galaxy-like ones. stars gas How about sub-mm galaxies? ⇒Necessary to include dust evolution.

  6. 150Mpc/h 2. Models (N-body + Dust) • N-body Simulation • LCDM model Cosmological Simulation • Box Size: (150Mpc/h)3 ⇔ 104 arcmin2 • Dust Evolution Model • Increase of Dust Content by SNe II • Evolution of Dust Optical Depth • Evolution of UV and FIR Luminosities • Dust evolution model is applied to dark halos in the simulation to estimate LIRand LUV

  7. Star Formation Rate SFR • SFR(t) = t/M0 exp(–t /) • t: Age of the dark halo • t: Star formation timescale (= R/vcir) • M0: available gas mass for star formation (eMgas) e = 0.1 (t > t) e = 0.5 (t < t) • The above SFR is applied to each halo. t t/t

  8. UV radiation IR radiation Dust grains (~0.1mm) Absorb UV Radiate IR Observer Massive stars 3～100MO LUV and LIR Estimation • LUV ∝ SFR(t) • LIR= (1-[1-exp(-dust)]/dust) LUV - dust: Optical depth of dust, ∝ Mdust/R2 -Mdust is increased by SNe II (0.4MO per SN) - Supernova rate ∝ SFR(t)

  9. 3. Results Data from Chapman et al. (2005) Our prediction at z ~ 3 z ~ 2.5 z ~ 1

  10. Lya Emitters with Sub-mm z = 3: sub-mm luminous Lya emitters (LIR > 5×1012Lsun) Lya emitters are selected by t < 2×108 yr.

  11. Results (LIR>1011LO) at z = 6 497 galaxies (LIR>1011LO) are found in (150Mpc/h)3

  12. Results (LIR>1011LO) at z = 10 30 galaxies (LIR>1011LO) are found in (50Mpc/h)3 ~1000arcmin2

  13. 4. Strategy for Survey Observation • Although the dust opacity is lower at z ~ 6, we can detect ~ 30 galaxies in a 100 arcmin2 survey.← Cosmic variance is large, so we should observe known clustering regions already observed in optical. • We could expect detection of a few z ~ 10 galaxies. (A survey at 220 GHz is favorable.)

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