GMT2010 Workshop 12 Years Ago, JWST (NGST) Deep Field Simulation (2’ x 2’) Im & Stockman (1998)

GMT2010 Workshop High Redshift Universe

GMT2010 Workshop The Quest for First Something Myungshin Im (CEOU, Astronomy Program, Dept. of Physics & Astronomy, Seoul National University)

GMT2010 Workshop The very beginning of Astronomical Objects First stars, galaxies, quasars, black holes, …. ?

GMT2010 Workshop Critical for our understanding of galaxy formation/evolution Z = Z = 0 Z > 6

GMT2010 Workshop GMT Advantages High angular resolution Moderate to high spectral resolution spectroscopy (R > 1000) Quick response possible

GMT2010 Workshop Supermassive Black Holes (SMBH) What are they? - Black Holes with masses ~ 10 5 – M ⊙ Where are they ? - Centers of massive spheroids/bulges or quasars Elliptical galaxyBulges of SpiralsQuasars/AGNs

GMT2010 Workshop First SMBHs in Early Universe Quasars are powered by matters accreted to SMBHs. Quasars have been discovered out to z ~ 6.43 (Fan et al; Willott et al. 2007). QSO at z=6.43 (Willott et al. 2007) Luminous quasars exist out to z ~ 6.4.

GMT2010 Workshop Growth of SMBHs ? M(t)=M(0) exp[(1-ε)/ε (t/t Edd )]=M(0) exp(t/τ), with τ ~ 4.5 x 10 7 (ε/0.1) yrs Not enough time (only ~0.64 Gyr between z= 6 and 15), Seed mass? M BH with UV-lines uncertain (CIV: μm, MgII: μm) M BH from Balmer lines (most reliable)  Growth History of SMBHs Volonteri & Rees (2006) Sijacki, Springel, & Haehnelt (2009) ε=0.1 ε=0.2 ε=0.4 Super-critical

GMT2010 Workshop AKARI Spectroscopy of Quasars at z > μm spectroscopy from space (R ~ 130)

GMT2010 Workshop BR (z=4.51) NP NG

GMT2010 Workshop QSONG : H α lines of 14 QSOs at 4.5 < z < 6.22 z = 4.69 z = 5.80 z = 5.59 z = 4.97 Im et al. 2010, in prep

GMT2010 Workshop SDSS J at z=6.42 HαHα

GMT2010 Workshop Massive Black Holes out to z ~ 6 Black Hole Mass ~ – M ⊙ No M > M ⊙ SMBHs at z ~ 6 + L/L E ~ 1 (vs ~ 0.1 at lower redshift)  Formation of the most massive BHs Quasar Cliff? Shen et al. (2007) ? Im et al. (2010) More points here (H. Jun) AKARISDSS

GMT2010 Workshop Infrared Medium-Deep Survey (IMS) J-band Imaging over 200 deg 2 to ~23 AB mag (+I,z,Y,…) to identify and study z > 6.5 quasars Observation started at late May, 2009 using UKIRT (9 nights) Currently, ~30 deg 2 covered

GMT2010 Workshop Quasars at z ~ 7?

GMT2010 Workshop Quasars at z > 6.5? GMT Project Handbook Prominent Targets for New Generation Facilities (~2014 and beyond) Giant Magellan TelescopeJames Webb Space Telescope

GMT2010 Workshop GMT and High-z Quasars Probe of the reionization epoch (Talks by X. Fan, S. Wyithe) Growth of the first SMBHs With moderate resolution spectroscopy, - Mass tracers CIV (z < 13), MgII (z < 6.8) - Narrow velocity widths (~1000 km/sec) - Resolving outflow signatures

GMT2010 Workshop First Clusters Emerging late in hierarchical galaxy formation (strong function of redshift, and cosmology, such as the power-law spectrum, non-Guassianity) Comparing theory vesus observation (how do we determine halo mass?) How do we identify them? (Reed et al. 2008)

GMT2010 Workshop Kang & Im (2009) – Analysis of Spitzer GOODS + VLT data Proto-cluster at z=3.7 (t univ = 1.7 billion years) Mass – M ⊙ Also, at z ~ 0.7, 1.8, 2.55, and 4.0 (all associated with AGNs or submm galaxies)  Member galaxies are too faint for spectroscopy: Larger telescopes are needed. Number density contour showing an overdensity of galaxies at A area. Proto-Clusters at High Redshift

GMT2010 Workshop Frist Galaxies Some claim detection of galaxies out to z ~ 10  very small ( ”, also in Im & Stockman 1998) 3”3” Galaxies at z ~ 6 (12.5 Gyrs ago). Bouwens et al. (2007)

GMT2010 Workshop First Star (Explosion) GRB? The most energetic phonomenon in the Universe – E iso ~ erg/sec Possible origins: Hypernovae explosion or merging of neutron stars GRB afterglow lasts a few days – weeks dT=0.5 days dT=5.5 daysdT=8.5 days First GRB afterglow (GRB071010B at z=0.947) observed by Korean Facility (Urata, Im, Lee, et al. 2009)

GMT2010 Workshop GRB at z ~ 8.2 (Tanvir et al; Salvaterra et al. 2009) Y-band calibration data from LOAO (Im et al. 2009) hrs after the burst

GMT2010 Workshop GRB A Dark Burst with K ~ 21.9 AB mag, H ~ AB mag, 2.6 hrs after the burst (no optical detection) GRB at 11 < z < 13.5, or dusty GRB at a lower redshift BOAO JK observation (with H.-I. Sung), LOAO zY observation (Im et al. GCN Circulars 10398)  confirm afterglow nature KASINICS K-band

GMT2010 Workshop GRB A UKIRT zJHK imaging from 15 min after the burst (Im et al. 2010, GCN Circular 11222)

GMT2010 Workshop GRB A at 6. 7 < z < 8.5 Easy imaging/spectroscopy target for GMT

GMT2010 Workshop H Neutral Fraction and HII Bubble Size McQuinn et al. Decadal Survey White paper (2010)

GMT2010 Workshop Metals in ISM/IGM McQuinn et al. Decadal Survey White paper (2010) Kawai et al. (2006), Totani et al. (2006) 4hr integration with Subaru GRB like GRB with R=3000 z=6.3

GMT2010 Workshop GMT and First something First QSOs: re-ionization state, BH growth history, host galaxy First proto-clusters: halo mass, galaxy properties in overdensity (z > 2) First GRBs: re-ionization state of the early universe