gmt2010 workshop 12 years ago, jwst (ngst) deep field simulation (2’ x 2’) im & stockman...
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GMT2010 Workshop
12 Years Ago,
JWST (NGST) Deep
Field Simulation
(2’ x 2’)
Im & Stockman
(1998)
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GMT2010 Workshop
High Redshift Universe
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GMT2010 Workshop
The Quest for First Something
Myungshin Im
(CEOU, Astronomy Program, Dept. of Physics & Astronomy,
Seoul National University)
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GMT2010 Workshop
The very beginning of Astronomical Objects
• First stars, galaxies, quasars, black holes, ….
?
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GMT2010 Workshop
Critical for our understandingof galaxy formation/evolution
-------------
-----------------
---------------Z = 2 - 3
Z = 0
Z > 6
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GMT2010 Workshop
GMT Advantages
• High angular resolution
• Moderate to high spectral resolution spectroscopy (R > 1000)
• Quick response possible
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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
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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.
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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
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GMT2010 Workshop
AKARI Spectroscopyof Quasars at z > 4.5
2.5-5.0 μm
spectroscopy
from space
(R ~ 130)
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GMT2010 Workshop
BR 0006-6224 (z=4.51)
NP
NG
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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
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GMT2010 Workshop
SDSS J 114816+525150 at z=6.42
Hα
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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
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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
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GMT2010 Workshop
Quasars at z ~ 7?
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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
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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
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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)
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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
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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)
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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)
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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
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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
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GMT2010 Workshop
GRB 100905A
• UKIRT zJHK imaging from 15 min after the burst (Im et al. 2010, GCN Circular 11222)
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GMT2010 Workshop
GRB 100905A at 6. 7 < z < 8.5
Easy imaging/spectroscopy target for GMT
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GMT2010 Workshop
H Neutral Fraction and HII Bubble Size
McQuinn et al.
Decadal Survey
White paper (2010)
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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
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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