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

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

星系的并合

大质量黑洞的并合

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

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

超大质量黑洞双黑洞的观测 NGC3393 Fabbiano 2011

超大质量黑洞双黑洞的观测 0402+379 (z=0.055) Rodriguez 2006

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

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

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

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

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

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

超大质量黑洞双黑洞的观测

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)

High-z Supermassive BHs Example: SDSS 1114-5251 (Fan et al. 2003, Wu et al 2014) z=6.43 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 

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

Hierarchical Models of Galaxy Formation

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

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

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

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

Mass fluctuation Zeldovich Spectrum： Transfer Function:

Mass fluctuation

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

Extended PS Theory（Lacey & Cole 1993）

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)

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

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

Comic Evolution of SMBHs

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

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

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

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-

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≳10-3.5 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)

Remnants of Massive Stars Heger et al. 2003 (for single, non-rotating stars) Z=Z metalicity Z=0 10M 25M 40M 140M 260M

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)

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

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

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)

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

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

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

Volonteri, M. et al. 2005

Distribution of BH spins (Yuan et al. 2007)

Distribution of accretion efficiencies (Yuan et al. 2007)

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

Xu, Yuan et al, 2015, RAA

BHB coalescence and Gravitational Waves

Gravitational radiation：

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

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

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

recoil Z=16 Koushiappas &  Zentner 2006

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

S/N>5, LISA 3-year mission

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

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

Thanks!