Growth of massive black holes during radiatively inefficient accretion phases

Growth of massive black holes during radiatively inefficient accretion phases Xinwu Cao Shanghai Astronomical Observatory, CAS

Growth of massive black holes is mainly through accretion. The black hole mass density accreted in bright AGN phases is which can match to the measured local black hole mass density, if a suitable radiative efficiency is adopted. Observations show nuclear activities in many low-luminosity AGNs/normal galaxies. Motivation 1. How were the bright AGNs switched off? 2. How much local massive black hole mass was accreted in low-luminosity AGNs/normal galaxies?

Different accretion modes Slim disk: optically thick, disk-thickness: Standard thin disk: optically thick, disk-thickness: Radiatively inefficient accretion flow (RIAF): optically thin, hot, disk-thickness: faint due to low radiative efficiency Accretion mode transition occurs while

Spectra of slim disks(Wang et al. 1999) Spectra of thin disks(Laor & Netzer1989) Spectra of RIAFs(Manmoto 2000)

Slim/thin disks: bright AGNs RIAFs: low-luminosity AGNs/normal galaxies Difficulty: only local faint AGNs/normal galaxies can be well observed. Constraints from the X-ray background(XRB) Observed X-ray background(Comastri 2004)

How were the bright AGNs switched off? • (Cao, 2005, ApJ, 631, L101) • estimate number density of faint AGNs from the hard XLF(Ueda et al. 2003). • the duration of RIAFs in faint AGN accreting • at a critical rate, • calculate the spectra of RIAFs • calculate the contribution to the XRB from RIAFs in faint AGNs • comparison with the observed XRB provides a constraint on the timescale

Blue: 0.05 Red: 0.01 Green: 0.005 Conclusion: bright AGNs are switched off in less than ~1-5% of bright AGN lifetime. Most LLAGNs/normal galaxies are accreting at So, how low is the accretion rate for LLAGNs/normal galaxies? or ?

The contribution from the RIAFs in all inactive galaxies to the cosmological XRB can be calculated by where is the template spectrum of a RIAF surrounding a black hole ( solar masses) accreting at active galaxies: described by the Ueda’s X-ray LF, with inactive galaxies:

Black hole density in inactive galaxies The black hole mass density at redshift accreted during active galaxy phases from to is where given by Marconi et al. (2004). The black hole mass density at redshift accreted during inactive galaxy phases from to is

The total accreted black hole mass density is The total black hole mass density Thus, The black hole mass density in active galaxies is The initial condition:

If the number ratio of Compton-thick to Compton-thin AGNs is 0.6, the radiative efficiencies are ~0.1-0.17.

Black hole spin and radiative efficiency The evolution of black hole mass and spin through accretion is described by The evolution of black hole mass as a function of spin parameter is

Corresponding to the radiative efficiencies derived, the spin parameter is required. Black hole spin and radiative efficiency

XRB synthesis for inactive black hole mass density derived for local black hole mass density for

for XRB synthesis for inactive black hole mass density derived for local black hole mass density

The number of Compton-thick AGNs with is assumed to be half of those with for for

The constraints on accretion rates as functions of the number ratio of Compton-thick AGNs with to those with

3. Conclusions 1. Bright AGNs are switched off in less than ~1-5% of bright AGN lifetime, which may be the evidence that the gas near the black hole is blown away by AGN radiation. 2. Black hole growth is not important during inactive galaxy phases (<2-5% local black hole mass density was accreted in inactive galaxies). The average accretion rate of inactive galaxies should be

Template spectra for RIAFs a=0 a=0.9

The scenario for AGN formation and evolution 1. Birth of AGNs Mergers between galaxies trigger nuclear gas flows to feed the black hole, and trigger nuclear starbursts. The nucleus is obscured by dense gas. 2. Bright AGN phase accreting at around or slightly less than the Eddington rate. The gas becomes transparent and the nucleus can be seen. 3. Death of bright AGNs radiation of AGNs expels gases to quench both accretion and star formation. 4. Faint AGN phases accreting at very low rates

Growth of massive black holes during radiatively inefficient accretion phases