Formation Scenario of SMBHs and Gravitational Wave
Hisaaki Shinkai (Osaka Institute of Technology) Nobuyuki Kanda (Osaka City Univ.)
Toshikazu Ebisuzaki (RIKEN)
1
First International Meeting on KAGRA,
@Daejeon, Korea. 2016 June25
https://www.ligo.caltech.edu/system/avm̲image̲sqls/binaries/57/page/Black̲Hole̲Mass̲Chart.jpg?1465864737
BHs!
29M+36M=62M 7M+14M=20M
why not more?
Slide copy from Hiroyuki Nakano
3GW150914
4.7% of mass emitted
in total 2.8% of mass
emitted by ISCO
1% of mass
emitted
in ringdown?
4
1601.07217
Kinugawa, Nakano, Nakamura 1505.06962
Kinugawa, Miyamoto, Kanda, Nakamura
BH-BH from Pop III
Rees, M.J. 1978. Observatory 98: 210
5Gas Cloud
BHs
IMBHs
SMBHs
Halo
Galaxy Globular
Cluster Massive
Stars
6
Yagi, CQG 29 075005 (2012) [arXiv:1202.3512]
HLX-1 has 20,000M BH!
http://hubblesite.org/newscenter/archive/releases/2012/2012/11/full/
Starburst galaxy M82 has 1000M BH
BHs
IMBHs
SMBHs
Matsushita+, ApJ, 545, L107 (2000)
Matsumoto+, ApJ, 547, L25 (2001)
7
BHs
IMBHs
SMBHs
'Missing link' founded
Ebisuzaki +, ApJ, 562, L19 (2001)
(1)formation of IMBHs by runaway mergers of massive stars in dense star clusters,
(2) accumulations of IMBHs at the center region of a galaxy due to sinkages of clusters by dynamical friction
(3) mergings of IMBHs by multi-body interactions and gravitational radiation.
Marchant & Shapiro 1980; Portegies Zwart et al. 1999;
Portegies Zwart & McMillan 2002;
Portegies Zwart et al. 2004;
Holger & Makino 2003
Matsubayashi et al. 2007
Iwasawa et. al. 2010
Matsubayashi, HS, Ebisuzaki, ApJ 614 (2004) 864
Matsubayashi, HS, Ebisuzaki, ApJ 614 (2004) 864
10-24 10-23 10-22 10-21 10-20
Strain Equivalent Noise spectrum [1/√Hz]
6 7 8 9
10 2 3 4 5 6 7 8 9100 2 3 4 5 6 7 8 91000
frequency [Hz]
LCGT
LCGT (varRSED, BWstudy2009) LCGT (varRSEB, Bwstudy2009) advanced Virgo
advanced LIGO(ZERO DET, High P) advanced LIGO(NS-NS)
Einstein Telescope ET_B ET_C
Kagra(LCGT) designed strain (2013/3)
BH quasi-normal ringing frequency (spin=0)
Mtotal f̲QNM
1 78200 Hz
10 7820 Hz
100 782 Hz
1000 78.2 Hz
10000 7.82 Hz
M/M f QNM
a = 0
a = 0.98 a = 0.49
f
QNM= c
32 GM 1 0.63(1 a)
0.3⇥ Black-Hole Ringdown frequency
1000
100 10
10
314
Mass Function of Giant Molecular Clouds
1 100 104 106
10-4 1 104 108 1012
M 10
12M
10
9M
galaxy mass
GMC mass
A&A 580, A49 (2015) [arXiv:1505.04696]
How many BHs in a Galaxy?
15
10 100 1000 104
10-7 0.001 10.000 105
1309.1223v3
10
12M
10
9M
Galaxy Mass n(M)
BH mass
Molecular Clouds
Maximum Core
Building Block BH
How many BHs in a Galaxy?
16
Count BHs to form a SMBH
10 1000 105 107 109 1011
10-7 10-4 0.1 100 105
10 100 1000 104
10-7 0.001 10.000 105
10
12M
10
9M
Galaxy Mass n(M)
BH mass
Building Block BH
BH mass n(M)
How many BHs in a Galaxy?
17
(sub-)Galaxy
from Halo model
Star Formation Rate
peak z=3.16
Count BHs to form a SMBH
How many Galaxies in the Universe?
18
1011 1012 1013 1014 1015
10-23 10-21 10-19 10-17 10-15 10-13
z = 0 z = 5
1012 1013 1014 1015
5 10 50 100 500 1000
(1) Halo number density
(2) N of seeds of Galaxy (subHalo)
(3) N of Galaxy
within z=1 within z=5
M
11×1011 5×1011 1×1012 5×1012
0.01 1 100
M
1.95How many Galaxies in the Universe?
19
図F
BH mass
z z
BH mass
in Standard Cosmology
How many BH mergers in the Universe?
20
Detectable Distances at bKAGRA
M/M fQNM
a= 0 a= 0.98 a= 0.49
fQNM= c3
2 GM 1 0.63(1 a)0.3⇥ Black-Hole Ringdown frequency
1000
100
10
103
Hierarchical Growth
(1) mass distribution
(2)
(3) Ringdown only : 1% of total mass emission
Strainnoiseamplitude[1/√ Hz]
frequency[Hz]
Kagra
TOBA
aLIGO aVIRGO
ET
BH Mass (final BH) [M⊙]
SNR at d=1000 Mpc
(a) Kagra
a = 0.9
a = 0.5 a = 0.0
BH Mass (final BH) [M⊙]
(a) SNR=10
Detectable Distance [Mpc]
a = 0.0 a = 0.5
a = 0.9
Kagra
21
Event Rates at bKAGRA
Preliminary
1-10 events/yr
BH spin=0.9,0.5,0.0
BH Mass Frequency
Summary
By accumulating data, we can discuss astrophysics:
formation scenario of SMBH, number counts of galaxies,
…(and later) cosmological models/gravitational theories.
1 10 100 1000 104
0.05 0.10 0.50 1 5 10
1 10 100 1000
0.05 0.10 0.50 1 5 10
peak at 100-200M
different from PopIII model
22
