1. 2015 Xinjiang Pulsar and Gravitational-Wave School
星系并合与超大质量双黑洞
袁业飞（Ye-Fei Yuan）
中国科学技术大学天文学系
2015/10/25

2. Outline Basic Observations(SMBMB)
Hierarchical Models of Galaxy Formation
Comic Evolution of MBHs
BHB coalescence and Gravitational Waves

3. 星系的并合

4. 大质量黑洞的并合

5. 超大质量黑洞双黑洞的观测
Komossa, et al., 2003, ApJL

6. 超大质量黑洞双黑洞的观测
Fu, H et al., 2013, Nature

7. 超大质量黑洞双黑洞的观测
NGC3393
Fabbiano 2011

8. 超大质量黑洞双黑洞的观测
(z=0.055)
Rodriguez 2006

9. 超大质量黑洞双黑洞的观测
4C12.50
Begelman et al , 1980, Nature

10. 超大质量黑洞双黑洞的观测
Komossa, et al., 2003, ApJL

11. 超大质量黑洞双黑洞的观测
3C326
Merritt& Ekers, 2002; Liu 2004

12. 超大质量黑洞双黑洞的观测
HE0450–2958
Magain et al. 2005, nature

13. 超大质量黑洞双黑洞的观测
BL Lac object OJ287: p=11.86 yr (Sillapaa et al. 1988)

14. 超大质量黑洞双黑洞的观测
Hayasaki 2009
Yan et al. 2015, ApJ

15. 超大质量黑洞双黑洞的观测

16. Basic Observations Most local galaxies host MBHs (106-109Msun)
M-б(L) Relation
(Ferrarese and Merritt 2000, Gebhardt et al 2000, Tremaine et al 2002)
Co-evolution between galaxies, MBHs and QSOs
Accretion history and Spins of MBHs (Soltan’s argument)
(Yu and Tremanie 2002, Wang et al. 2006)
Existence of SMBH (~109Msun) at z>6
(Fan et al. 2001; Barth et al. 2003; Willott et al. 2005)

17. High-z Supermassive BHs
Example: SDSS (Fan et al. 2003, Wu et al 2014)
z= Mbh 4 x 109 M
How did this SMBH grow so massive?
e-folding (Edd) time:
4 x (/0.1) -1 107yr
Mseed ~100 M
Age of universe (z=6.43)
8 x 108 yr 

18. Questions 1)Existence of SMBH at t<1Gyr, while
2)Much smaller BHs exist in 13Gyr old galaxies

19. Hierarchical Models of Galaxy Formation

20. History of the Universe
Barkana & Loeb, 2001, Phys. Rep.

21. Linear gravitational Growth
Density contrast：
Basic equations：
Linearizaton for small perturbation：
Einstein-de Sitter Universe：

22. z=0:
Small scale structure: nonlinear
Large scale structure: linear

23. Statistical description of the density perturbation：Probability Functional
Gaussian Spectrum：
Power Spectrum：

24. Mass fluctuation
Zeldovich Spectrum：
Transfer Function:

25. Mass fluctuation

26. Press-Schechter Theory（1974）
Problem：
BCEK Theory (Bond et al. 1991)

27. Extended PS Theory（Lacey & Cole 1993）

28. Condensations in Hierarchical Cosmology
Consider linear
growth of DM
perturbations
in concordance
cosmology 30 20
collapse redshift
Smallest scales
condense first
Jeans mass:
~104-5 M 10 2 3 4 5 6 7
log (Mass/ M)

29. Merging tree of dark matter halo and evolution of massive black holes
time

30. Dark matter Halo Merging Tree—A Self Adaptive Code
Time
(Yuan et al. 2007)

31. Comic Evolution of SMBHs

32. Modeling the Gas in the First Halos: Cooling and Chemistry
Collapsed Dark Matter halos virialize,
gas shock heated to virial temperature
Efficient cooling is a necessary condition for
continued contraction following virialization
Primordial gas chemically simple: H, He, H2

33. Radiative Cooling Function (H+He gas)
COSMIC TIME
MASS SCALE
cf. Halo virial temperature:
log( cooling rate / erg s-1 cm3 )
log( Temperature / K )

34. Cooling and Chemistry Molecular cooling to T~102 K (M~105 M ; z~20)
End of “Dark Age” controlled by
abundance of H2 : (Saslaw & Zipoy 1967
Haiman, Thoul & Loeb 1996)
Molecular cooling to T~102 K (M~105 M ; z~20)
Atomic cooling to T~104 K (M~108 M ; z~12)
What is the molecular abundance?
nH2/nH ~10-6 after recombination
~10-3 in collapsed objects

35. 3D Simulations of a Primordial Gas Cloud
Abel, Bryan & Norman (AMR)
Bromm, Coppi & Larson (SPH)
Mtot  106 M
z  20
T200 K
n 104 cm-3
M = few 100 M 
f* < 1 %
Temperature Density
Gas Phase Chemistry:
H + e-  H- + 
H-+ H  H2+ e-

36. What forms in these early halos?
STARS: FIRST GENERATION METAL FREE
- massive stars with harder spectra
- boost in ionizing photon rate by a factor of ~ 20
- return to “normal” stellar pops at Z≳ Z⊙
(Tumlinson & Shull 2001 ; Bromm, Kudritzki & Loeb 2001; Schaerer 2002)
SEED BLACK HOLES: (~102-6 M⊙ )
- boost by ~10 in number of ionizing photons/baryon
- harder spectra up to hard X-rays
- must eventually evolve to quasars and remnant holes
[to z~6 super-massive BHs; probed by gravity waves]
(Oh; Venkatesan & Shull; Haiman, Abel & Rees; Haiman & Menou)

37. Remnants of Massive Stars
Heger et al (for single, non-rotating stars)
Z=Z
metalicity
Z=0
10M M 40M M M

38. Formation of seed BH Direct formation from a collapsing gas cloud?
The loss of angular momentum
Turbulent viscosity
Global dynamical instabilities
Formation of the seed BH
Supermassive star  BH
Quasi-star (a small BH + envelope)
(Begelman et al. 2007)

39. z=10, T=300K
z=20
z=10, T=4000
z=20
Lodato & Natarajan 2007

40. Remnant of Pop. III stars
First star (z>10) forms at high –бpeaks of the primordial density field
Top heavy stellar IMF: inefficient cooling of zero metallicity gas
Little mass loss: zero metallicity star

41. First generation of stars are simpler in principle to model:
Metal Free Gas Cooling
Pop III Star Formation
First generation of stars are simpler in principle to model:
Chemistry of unenriched gas is simpler
Gas has not yet been ionized or disturbed by winds from other stars
Model Results
Massive & short lived
Early objects zcoll~ 20-30
H2 controls cooling
Yoshida, Omukai, Hernquist, & Abel (2006)

42. Observational tests of seed formation
Gravitational waves from seeds merging (LISA)
Integrated BH mass density
Volonteri et al. 2007

43. Cosmic evolution of SMBHs
Seed black hole：
Total accreted Mass：
Spin change by accretion：
SSD Model
MHD Model
(McKinney & Gammie 2004;
Shapiro 2005)

44. Volonteri, Haardt, Madau, 2003
Dynamical Evolution of BH Binaries
Gravitational slingshot (BHB interaction with background stars)
Gravitational radiation
Spin change by coalescences
Test particle approximation
The spin of the newly formed black hole after merging is the summation of the spin of the heavier BH in the binary and the angular momentum of the lighter one at ISCO.
Triple BH interactions
Volonteri, Haardt, Madau, 2003

45. Volonteri, M. et al. 2005

46. Distribution of BH spins
(Yuan et al. 2007)

47. Distribution of accretion efficiencies
(Yuan et al. 2007)

48. LF of QSOs
Xu, Yuan et al, 2015, RAA

49. Xu, Yuan et al, 2015, RAA

50. BHB coalescence and Gravitational Waves

51. Gravitational radiation：

52. The mean comoving number density of potential BH pairs
M1+M2<105,106
M1/M2=10-1,-2,-3
M1<105,106

53. M1=M2=1.1x105Msun
z=13
Koushiappas &  Zentner 2006

54. S/N>1
Z=12
recoil
z=16
S/N>5
Koushiappas &  Zentner 2006

55. recoil
Z=16
Koushiappas &  Zentner 2006

56. Model dependent results
(e.g. Sesana, Volonteri, Haardt 2007)
Pop III
KBD
BVRlf,hf

57. S/N>5, LISA 3-year mission

58. Gong X. F & Xu S. N. & Shan B. et al. , 2012 Class. Quantum Grav

59. Gong X. F & Xu S. N. & Shan B. et al. , 2012 Class. Quantum Grav

60. Thanks!