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 understandingof galaxy formation/evolution

-------------

-----------------

---------------Z = 2 - 3

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 ~ 105 – 1010 M⊙

• Where are they ?

- Centers of massive spheroids/bulges or quasars

Elliptical galaxy Bulges of Spirals Quasars/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/tEdd)]=M(0) exp(t/τ), with τ ~ 4.5 x 107 (ε/0.1) yrs

• Not enough time (only ~0.64 Gyr between z= 6 and 15), Seed mass?

• MBH with UV-lines uncertain (CIV: 0.1549 μm, MgII: 0.2798 μm)

• MBH 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 Spectroscopyof Quasars at z > 4.5

2.5-5.0 μm

spectroscopy

from space

(R ~ 130)

GMT2010 Workshop

BR 0006-6224 (z=4.51)

NP

NG

GMT2010 Workshop

QSONG : Hα 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 114816+525150 at z=6.42

Hα

GMT2010 Workshop

Massive Black Holes out to z ~ 6

• Black Hole Mass ~ 109.3 – 1010.1 M⊙

• No M > 1010 M ⊙ SMBHs at z ~ 6 + L/LE ~ 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 deg2 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 deg2 covered

GMT2010 Workshop

Quasars at z ~ 7?

GMT2010 Workshop

Quasars at z > 6.5?

GMT Project Handbook

Prominent Targetsfor New Generation

Facilities(~2014 and

beyond)

Giant Magellan Telescope

James 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 (tuniv = 1.7 billion years)

• Mass – 1014 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 (0.1-0.2”, also in Im & Stockman 1998)

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 – Eiso ~ 1054 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 days dT=8.5 days

First GRB afterglow (GRB071010B at z=0.947) observed by Korean Facility (Urata, Im, Lee, et al. 2009)

GMT2010 Workshop

GRB090423 at z ~ 8.2(Tanvir et al; Salvaterra et al. 2009)

• Y-band calibration data from LOAO (Im et al. 2009)

30-1.5hrsafter the burst

GMT2010 Workshop

GRB 100205A• Dark Burst with K ~ 21.9 AB

mag, H ~ 23.54 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 100905A

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

GMT2010 Workshop

GRB 100905A 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 080613-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