super-massive black holes of quasars at world’s end myungshin im (seoul national university)...
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Super-massive Black Holes of Quasars at
World’s End
Myungshin Im
(Seoul National University)
Youichi Ohyama (ISAS & ASIAA)Minjin Kim, Induk Lee, H. M. Lee, M. G. Lee (SNU),T. Wada, T. Nakagawa (ISAS/JAXA), Xiaohui Fan (U. Arizona)
[Rest-frame Optical Spectra of Quasars at 4.5 < z < 6.5]
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10 Years Ago
JWST Simulation from Im & Stockman (1998)
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Quasars
• Quasars = QUASi-stellAR radio sources. Extremely bright, compact active galactic nuclei, powered by accretion of matters around supermassive blackholes.
• Peculiar radio stars, 3C48, 3C273, spectroscopically identified to be at cosmological distance (1960, 1962, Bolton, Schmidt) discovery of quasars.
• QSO (Quasi-Stellar Object) radio-quiet populations are included.
• Active Galactic Nuclei (AGN): Blazar, BL-Lac, Seyferts-I,II, etc.
3C273
AGN Unification Picture
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Super-massive Black Holes in Nearby Galaxies• Supermassive black holes (SMBHs) at the centers of massive galaxi
es (bulges): 106 – 1010 M⊙
• SMBH mass tightly correlates with, mass, velocity dispersion, and K-band luminosity of the host galaxy (e.g., Gebhardt et al. 2000; Ferrarese & Merritt 2000; Marconi & Hunt 2003)
Marconi & Hunt (2003)
But why?
Which was born first?
When did the massive SMBHs appear?
Is it consistent with the hierarchical galaxy formation?
: Important questions for the galaxy formation and evolution.
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Supermassive Black Holes 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 existed out to z ~ 6.4.
But, how massive were they, and can you grow such SMBHs in short time scale?
Undertanding the nature of SMBHs in QSOs in the early universe is very important!
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Measuring (or estimating) SMBH mass
• Direct measurement from stellar motion.• Reverberation mapping: BLR size correlation with L(51
00) L(5100) and Hβ width can be used for MBH measurement (Kaspi et al. 2000)!
• Single epoch measurement using optical or UV spectra (e.g., Vestergaard et al. 2005; Greene & Ho 2005).
[M = f*R*v2/G ; Vestergaard (2008)]
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Quasar spectrum
(Im, Lee, et al. 2007)
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Single Epoch Measurement
Wavelength
Flu
x
[M = f*R*v2/G ; Vestergaard (2008)]
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Masses of SMBHs at high redshift• MBH measurements for high redshift QSOs rely on the UV-line
s (CIV: 0.1549 micron, MgII: 0.2798 micon)
• SMBHs (M ~ 109 – 1010 M⊙ or more) at 2 < z < 5
Shen et al. (2007), Also see Vestergaard et al. (2008)
A few more points here from ground-basedNIR spectroscopy(Jiang et al.; Kurk et al. 2007)
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Growth of SMBH
• The mass growth rate: ~ exp(t/τ), where τ ~ 4.5 x 107 (ε/0.1) yrs at the Eddingto
n limited accretion [ε = radiative efficiency]
• At z=5.5, t ~ 1 Gyr, at z=6, t ~ 0.9 Gyr, and at z=15, t ~ 0.26 Gyr
• Growing 109 -1010 M⊙ BHs is very challenging even from 1000 M⊙ at z > 5.5
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Need for Better Mass Measurement
Netzer et al. (2007)
But the reliability of CIV measurement has been in question (or even MgII – outflow contribution, asymmetric profile, etc)
At higher z, metallicity abundance may decrease
Need for a well-calibrated, independent measure of MBH using optical spectra such as Hα or Hβ (e.g., Greene & Ho 2005).
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AKARI Spectroscopy
Japanese 68cm IR telescope optimized for FIR all-sky survey. Participation from ESA and Korea (mainly Seoul National Univ. group). Launched in Feb., 2006. Cold mission ended in late August, 2007.
NIR Grism and Prism Spectroscopy
- NP (Prism): Slit-less spectroscopy at 2 - 5 micron. R=19 at 3.5 micron, FWHM=15000 km/sec.
- NG (Grism): Slit-less or with slit-aperture at 2.5 – 5 micron. R=120 at 3.6 micron, FWHM=2500 km/sec. The only facility in the world capable of studying Balmer lines at 4 < z < 6.5 !
Detection of Hα (Prism data) of QSO at z=4.3 (Oyabu et al. 2007)
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AKARI Open Time Program HZQSO (PI: Im)
Program Summary
Observation of rest-frame optical lines of QSOs at z > 4.5 (mainly Hα) using AKARI NG & NP.
Masses of super-massive black holes in the early universe. Test the empirical relations of line luminosity/continuum. Study the metallicity evolution (Fe abundance, OIII lines, etc).
Targets
14 Known QSOs at z > 4.5. Good visibility (stringent orbital constraint of AKARI).
3.6 micron flux > ~ 100 uJy (for detection of H-alpha).
Not in the crowded region to avoid the confusion of spectra.
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Observations & Targets
Name z NG
NP Hα?
BR 0006-6208 4.51 3 2 Yes
BR 1202-0727 4.694 1 0 Yes
SDSS J 165354+405402
4.97 2 0 Yes
SDSS J 161705+443522
5.50 2 0 No
SDSS J 162100+515548
5.59(5.71)
4 0 Yes
SDSS J 172100+601721
5.799 4 0 No
SDSS J 000239+255034
5.80 3 2 Yes
SDSS J 000552-006555
5.85 0 1 No
SDSS J 113717+354956
6.01 0 1 No
SDSS J 160253+422824
6.07 0 1 Yes
FLX J 1427386+331241
6.10 0 2 No
SDSS J 125051+313021
6.13 0 1 Yes?
SDSS J 162331+311200
6.22 0 3 Yes?
SDSS J 114816+525150
6.42 7 2 No?
Observations were carried out in 2006 - 2007.
3 QSOs have both NG/NP data.
8 QSOs out of 14 show Hα detection.
1 pointing ~ 10 min.
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NIR Prism Observation
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BR 0006-6224 (z=4.51)
NP
NG
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Hα Detections (NG) z = 4.69
z = 5.80
z = 5.59
z = 4.97
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Hα Detections (NP) z = 6.13 z = 6.07
z = 6.22
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Line Luminosity/Width, Black Hole Mass
Log(L(Hα) erg/sec) ~ 45.5 erg/sec FWHM ~ 2500 - 5000 km/sec. Log(MBH M⊙) ~ 9.2 – 10.1 (Hα method from McGill, Woo, Treu & Ma
lkan 2007). When no FWHM available (NP data), FWHM=4000 km/sec was ass
umed to calculate MBH.
z = 4.51
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Redshifts of Quasars
• BR0004-6224: z=4.51 vs 4.49 in the literature (e.g., Storrie-Lombardi et al. 2004) our measurement shows z=4.51 +-0.01
• SDSS J1621+5155: Tentative redshift of 5.71 from the ground-based observation (not published) our measurement shows z=5.59 +-0.01
• In all other cases, the literature values and our measurements agree well
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Comparison with other MBH estimators
Two targets have independent CIV and/or MgII based measurements
1. SDSS J000552-000655 (z=5.85)
No detection in Hα M < 1.5 x 109 M⊙ vs.
0.7 x 109 M⊙ (CIV) or 0.3 x 109 M ⊙ (MgII) (Both from Kurk et al. 2007)
2. SDSS J162331+311200 (z=6.22)
3.5 x 109 M⊙ (our measurement)vs.
1.5 x 109 M⊙ (MgII; Jiang et al. 2007)
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SMBH Mass
• BH Mass ~ 109.3 – 1010.1 M⊙
A few x 109 M⊙ SMBHs existed at z ~ 6 (0.95 Gyr)
• 1010 M⊙ SMBHs existed at z ~ 5 (1.2 Gyr)
• No M ~ 1010 M⊙ SMBHs at z > 5.5 (tuniv ~ 1 Gyr) ???
6 6.5
Shen et al. (2007) :Jiang et al. (2007) Kurk et al. (2007)
: Our work
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Discussion
• MBH = Mseed x exp[t(z)/τ ], τ ~ 4.5 x 107 yrs
• Δt (z=15 – 6.0) = 0.64 Gyr, e-holding time ~ 14.4 or growth factor of exp(14.4)=1.8x106
• To get 109.5 M⊙, we need Mseed ~ 1800 M⊙
- Upper envelope of SMBH mass: 1010 M⊙ at z=5 (1.15 Gyr) 109.5 M⊙ at z=6 (0.91 Gyr)
1010 M⊙ / 109.5 M⊙ ≈ exp{[t(z=5)-t(z=6)]/τ }
τ ≈ 1.5 x 108 yrs (3x 4.5 x 107 yrs) To get 109.5 M⊙, we need Mseed ~ 107 M⊙
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QSONG (QSO Study with NIR Grism)
• AKARI NIR grism observation of high-z and low-z AGNs
• High-z study (HQSONG): 129 QSOs at 3.4 < z < 6.5 with z_AB < 19 – 19.5 mag Establish mass evolution of SMBHs at high redshift
• Low-z study (LQSONG): 119 AGNs with reverberation mass, bright QSOs (PG quasars and SNUQSO quasars) + red AGNs (NIR Hydrogen lines and PAHs) Understand the NIR Hydrogen Line characteristics, diagnostics for studying SMBHs
• Observation started in June, 2008 (duration ~1.5 years)
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Summary• The first detection of Hα from QSOs at z >
4.5 out to z=6.22 using AKARI’s unique capability
• Supermassive black holes with109.2 – 1010 M⊙ existed in the early universe. (confirmed with a well-calibrated method using Hα)
• Lack of 1010 M⊙ SMBHs at z > 5.5: They are emerging at z ~ 5.5 ?
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