Relics of Nuclear Activity: Do All Galaxies Have Massive Black Holes?

Marel, van der; Roeland, P

doi:10.1017/s0074180900112926

Cited by 3 publications

(4 citation statements)

References 43 publications

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“…As it is widely believed that the activity of quasars is powered by accretion onto a supermassive black hole [BH] (see Rees 1984 and references therein), the detections of supermassive BHs in a number of nearby galaxies and the discovery of a correlation between the mass of the central BH and the luminosity of the host bulge provide substantial support for the hypothesis that most galaxies contain a supermassive BH (see e.g. Ford et al 1998;Ho 1998;Magorrian et al 1998;Richstone et al 1998;and van der Marel 1998). A recent study by Salucci et al (1999a) shows that the mass function of supermassive BHs inferred from the relation of BH mass to bulge luminosity is consistent with the luminosity function of quasars.…”

Section: Introductionmentioning

confidence: 99%

Quasars and galaxy formation

Cattaneo

2001

Monthly Notices of the Royal Astronomical Society

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Quasars are widely believed to be powered by accretion onto supermassive black holes and there is now considerable evidence for a link between mergers, quasars and the formation of spheroids. Cattaneo, Haehnelt & Rees (1999) have demonstrated that a very simple model in which supermassive black holes form and accrete most of their mass in mergers of galaxies of comparable masses can reproduce the observed relation of black hole mass to bulge luminosity. Here we show that this simple model can account for the luminosity function of quasars and for the redshift evolution of the quasar population provided a few additional assumptions are made. We use the extended Press-Schechter formalism to simulate the formation of galaxies in hierarchical models of the formation of structures and we assume that, when two galaxies of comparable masses merge, their central black holes coalesce and a fraction of the gas in the merger remnant is accreted by the supermassive black hole over a time-scale of about 10^7 yr. We find that the decrease in the merging rate with cosmic time and the depletion in the amount of cold gas available due to the formation of stars are not sufficient to explain the strong decline in the space density of bright quasars between z=2 and z=0, since larger and larger structures form, which can potentially host brighter and brighter quasars. To explain the redshift evolution of the space density of bright quasars between z=2 and z=0 we need to assume that there is a dependence on redshift either in the fraction of available gas accreted or in the time-scale for accretion.Comment: 8 pages, 8 figures, submitted to MNRA

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Section: Introductionmentioning

confidence: 99%

Quasars and galaxy formation

Cattaneo

2001

Monthly Notices of the Royal Astronomical Society

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“…A correlation between the mass of a supermassive black hole and the luminosity of the bulge of the host galaxy was already apparent in the first small sample of detections. The larger samples meanwhile available have backed up the existence of such a correlation (Kormendy 1993; Kormendy & Richstone 1995; MacLeod 1997; Magorrian et al 1998; Ford et al 1998; van der Marel 1998; Ho 1998).…”

Section: Introductionmentioning

confidence: 99%

The distribution of supermassive black holes in the nuclei of nearby galaxies

Cattaneo

Haehnelt

Rees

1999

Monthly Notices of the Royal Astronomical Society

108

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A B S T R A C TThe growth of supermassive black holes by merging and accretion in hierarchical models of galaxy formation is studied by means of Monte Carlo simulations. A tight linear relation between masses of black holes and masses of bulges arises if the mass accreted by supermassive black holes scales linearly with the mass-forming stars and if the redshift evolution of mass accretion tracks closely that of star formation. Differences in redshift evolution between black hole accretion and star formation introduce a considerable scatter in this relation. A non-linear relation between black hole accretion and star formation results in a non-linear relation between masses of remnant black holes and masses of bulges. The relation of black hole mass to bulge luminosity observed in nearby galaxies and its scatter are reproduced reasonably well by models in which black hole accretion and star formation are linearly related but do not track each other in redshift. This suggests that a common mechanism determines the efficiency for black hole accretion and the efficiency for star formation, especially for bright bulges.

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“…In this section, we briefly review the current observational implications for the existence of IMBHs and the formation mechanisms of IMBHs [41,34,54] and IMBH binaries [43].…”

Section: Intermediate-mass Black Holesmentioning

confidence: 99%

“…Other possible evidence includes the radial massto-light ratio [35] and the surface brightness profiles [36,37] of globular clusters, stellar proper motions near their centers [38,39] and observations of several millisecond pulsars in the galactic globular cluster [40]. IMBH detection is important since it will give us clues for the formation mechanism of SMBHs [41]. Since the observable range of DPF for these sources are within 50kpc, DPF targets are IMBH binaries in our Galaxy.…”

Section: Introductionmentioning

confidence: 98%

Gravitational wave observations of galactic intermediate-mass black hole binaries with DECIGO path finder

Yagi

2012

Class. Quantum Grav.

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Abstract.DECIGO Path Finder (DPF) is a space-borne gravitational wave (GW) detector with sensitivity in the frequency band 0.1-100Hz. As a first step mission to DECIGO, it is aiming for launching in 2016-2017. Although its main objective is to demonstrate technology for GW observation in space, DPF still has a chance of detecting GW signals and performing astrophysical observations. With an observable range up to 50 kpc, its main targets are GW signals from galactic intermediate mass black hole (IMBH) binaries. By using inspiral-merger-ringdown phenomenological waveforms, we perform both pattern-averaged analysis and Monte Carlo simulations including the effect of detector motion to find that the masses and (effective) spins of the IMBHs could be determined with errors of a few percent, should the signals be detected. Since GW signals from IMBH binaries with masses above 10 4 M ⊙ cannot be detected by ground-based detectors, these objects can be unique sources for DPF. If the inspiral signal of a 10 3 M ⊙ IMBH binary is detected with DPF, it can give alert to the ringdown signal for the ground-based detectors 10 2 -10 3 s before coalescence. We also estimate the possible bound on the graviton Compton wavelength from a possible IMBH binary in ω Centauri. We obtain a slightly weaker constraint than the solar system experiment and an about 2 orders of magnitude stronger constraint than the one from binary pulsar tests. Unfortunately, the detection rate of IMBH binaries is rather small. GW observations of galactic IMBH binaries with DPF2

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Relics of Nuclear Activity: Do All Galaxies Have Massive Black Holes?

Cited by 3 publications

References 43 publications

Quasars and galaxy formation

Quasars and galaxy formation

The distribution of supermassive black holes in the nuclei of nearby galaxies

Gravitational wave observations of galactic intermediate-mass black hole binaries with DECIGO path finder

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