Coevolution of Black Holes and Galaxies

By F. Panessa, M. Cappi, L. Bassani, Mauro Dadina, R. D. Ceca, Silvia Pellegrini, G. Trinchieri, A. Wolter, G. Palumbo. 2004

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DWARF GALAXIES WITH OPTICAL SIGNATURES OF ACTIVE MASSIVE BLACK HOLES (2013, methodology): “The most secure method of discovering supermassive BHs uses stellar or gas dynamics to weigh the central BH (see review in Kormendy 2004). However, the gravitational sphere of influence cannot be resolved for low-mass BHs in small galaxies much beyond the Local Group. For example, rinfl = GMBH/σ 2 ∼”
The Cosmic Evolution of Hard X-Ray-selected Active Galactic Nuclei (2004, methodology): “Barger et al. (2001b) adopted a value of about 35, based on the radio and submillimeter properties of a Chandra X-ray sample, whereas Fabian (2004) suggested a lower value of about 15, based on the suppression of UV and optical light in the local Seyfert galaxies Mrk 335, NGC 3783, and NGC 5548.”
Molecular gas in NUclei of GAlaxies (NUGA) - IV. Gravitational torques and AGN feeding (2005, unknown): “The different values of AGN duty-cycles discussed in the literature range from 107 to 108 yr (Ho et al. 2003; Martini 2004; Wada 2004; Merloni 2004).”
Towards a physical model of dust tori in Active Galactic Nuclei (2005, background): “It is known that many spiral galaxies harbor young nuclear star clusters (e.g. Gallimore & Matthews 2003; Walcher et al. 2004; Böker et al. 2002, 2004).”