Abstract
The observed scaling relations imply that supermassive black holes (SMBH) and their host galaxies evolve together. Near-Eddington winds from the SMBH accretion discs explain many aspects of this connection. The wind Eddington factor \(\dot{m}\) should be in the range ∼1–30. A factor \(\dot{m}\sim 1\) give black hole winds with velocities v∼0.1c, observable in X-rays, just as seen in the most extreme ultrafast outflows (UFOs). Higher Eddington factors predict slower and less ionized winds, observable in the UV, as in BAL QSOs.
In all cases the wind must shock against the host interstellar gas and it is plausible that these shocks should cool efficiently. There is detailed observational evidence for this in some UFOs. The wind sweeps up the interstellar gas into a thin shell and propels it outwards. For SMBH masses below a certain critical (M–σ) value, all these outflows eventually stall and fall back, as the Eddington thrust of the wind is too weak to drive the gas to large radii. But once the SMBH mass reaches the critical M–σ value the global character of the outflow changes completely. The wind shock is no longer efficiently cooled, and the resulting thermal expansion drives the interstellar gas far from the black hole, which is unlikely to grow significantly further. Simple estimates of the maximum stellar bulge mass M b allowed by self-limited star formation show that the SMBH mass is typically about 10−3 M b at this point, in line with observation.
The expansion-driven outflow reaches speeds v out≃1200 km s−1 and drives rates \(\dot{M}_{\mathrm{out}}\sim 4000~\mathrm {M}_{\odot }\,\mathrm{yr}^{-1}\) in cool (molecular) gas, giving a typical outflow mechanical energy L mech≃0.05L Edd, where L Edd is the Eddington luminosity of the central SMBH. This is again in line with observation. These massive outflows may be what makes galaxies become red and dead, and can have several other potentially observable effects. In particular they have the right properties to enrich the intergalactic gas with metals.
Our current picture of SMBH-galaxy coevolution is still incomplete, as there is no predictive theory of how the hole accretes gas from its surroundings. Recent progress in understanding how large-scale discs of gas can partially cancel angular momentum and promote dynamical infall offers a possible way forward.
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References
D. Batcheldor, Astrophys. J. 711, L108 (2010)
C.M. Booth, J. Schaye, Mon. Not. R. Astron. Soc. 398, 53 (2009)
L. Ciotti, J.P. Ostriker, Astrophys. J. 487, L105 (1997)
S. Collin-Souffrin, A.M. Dumont, Astron. Astrophys. 229, 292 (1990)
J. Debuhr, E. Quataert, C.-P. Ma, Mon. Not. R. Astron. Soc. 412, 1341 (2011)
W. Dehnen, D.E. McLaughlin, J. Sachania, Mon. Not. R. Astron. Soc. 369, 1688 (2006)
K.D. Denney et al., Astrophys. J. 702, 1353 (2009)
T. Di Matteo, V. Springel, L. Hernquist, Nature 433, 604 (2005)
T. Di Matteo, J. Colberg, V. Springel, L. Hernquist, D. Sijacki, Astrophys. J. 676, 33 (2008)
A.C. Fabian, Mon. Not. R. Astron. Soc. 308, L39 (1999)
C.-A. Faucher-Giguère, E. Quataert, Mon. Not. R. Astron. Soc. 425, 605 (2012)
L. Ferrarese, D. Merritt, Astrophys. J. 539, L9 (2000)
C. Feruglio, R. Maiolino, E. Piconcelli et al., Astron. Astrophys. 518, L155 (2010)
S. Garrison-Kimmel, M. Rocha, M. Boylan-Kolchin, J. Bullock, J. Lally, arXiv:1301.3137 (2013)
K. Gebhardt et al., Astrophys. J. 539, L13 (2000)
M.G. Haehnelt, P. Natarajan, M.J. Rees, Mon. Not. R. Astron. Soc. 300, 817 (1998)
N. Häring, H.-W. Rix, Astrophys. J. 604, L89 (2004)
L. Hernquist, Astrophys. J. 356, 359 (1990)
P.F. Hopkins, L. Hernquist, Astrophys. J. Suppl. Ser. 166, 1 (2006)
W. Ishibashi, A.C. Fabian, Mon. Not. R. Astron. Soc. 427, 2998 (2012)
A.R. King, Astrophys. J. 596, L27 (2003)
A.R. King, Astrophys. J. 635, L121 (2005)
A.R. King, Mon. Not. R. Astron. Soc. 402, 1516 (2010)
A.R. King, K.A. Pounds, Mon. Not. R. Astron. Soc. 345, 657 (2003)
A.R. King, J.E. Pringle, Mon. Not. R. Astron. Soc. 373, L90 (2006)
A.R. King, J.E. Pringle, Mon. Not. R. Astron. Soc. 377, L25 (2007)
A.R. King, J.E. Pringle, J.A. Hofmann, Mon. Not. R. Astron. Soc. 385, 1621 (2008)
A.R. King, K. Zubovas, C. Power, Mon. Not. R. Astron. Soc. 415, L6 (2011)
C. Leitherer, C. Robert, L. Drissen, Astrophys. J. 401, 596 (1992)
G. Lodato, D.J. Price, Mon. Not. R. Astron. Soc. 405, 1212 (2010)
C.J. Lonsdale, C.J. Lonsdale, H.E. Smith, P.J. Diamond, Astrophys. J. 592, 804 (2003)
N.J. McConnell, C.-P. Ma, K. Gebhardt, S.A. Wright, J.D. Murphy, T.R. Lauer, J.R. Graham, D.O. Richstone, Nature 480, 215 (2011)
D.E. McLaughlin, A.R. King, S. Nayakshin, Astrophys. J. 650, L37 (2006)
R.C. McQuillin, D.E. McLaughlin, Mon. Not. R. Astron. Soc. 423, 2162 (2012)
N. Murray, E. Quataert, T.A. Thompson, Astrophys. J. 618, 569 (2005)
J.F. Navarro, C.S. Frenk, S.D.M. White, Astrophys. J. 462, 563 (1996)
J.F. Navarro, C.S. Frenk, S.D.M. White, Astrophys. J. 490, 493 (1997)
C. Nixon, A. King, D. Price, J. Frank, Astrophys. J. 757, L24 (2012)
C. Nixon, A. King, D. Price, Mon. Not. R. Astron. Soc. 434, 1946 (2013)
G.I. Ogilvie, Mon. Not. R. Astron. Soc. 304, 557 (1999)
K. Ohsuga, S. Mineshige, Outflow launching mechanisms. Space Sci. Rev. (2013). doi:10.1007/s11214-013-0017-3
A. Pontzen, F. Governato, Mon. Not. R. Astron. Soc. 421, 3464 (2012)
K.A. Pounds, A.R. King, Mon. Not. R. Astron. Soc. 433, 1369 (2013)
K.A. Pounds, S. Vaughan, Mon. Not. R. Astron. Soc. 413, 1251 (2011)
K.A. Pounds, J.N. Reeves, A.R. King, K.L. Page, P.T. O’Brien, M.J.L. Turner, Mon. Not. R. Astron. Soc. 345, 705 (2003)
C. Power, K. Zubovas, S. Nayakshin, A.R. King, Mon. Not. R. Astron. Soc. 413, L110 (2011)
J.N. Reeves, P.T. O’Brien, M.J. Ward, Astrophys. J. 593, L65 (2003)
R.A. Riffel, T. Storchi-Bergmann, Mon. Not. R. Astron. Soc. 411, 469 (2011a)
R.A. Riffel, T. Storchi-Bergmann, Mon. Not. R. Astron. Soc. 417, 2752 (2011b)
D.S.N. Rupke, S. Veilleux, Astrophys. J. 729, L27+ (2011)
N.I. Shakura, R.A. Sunyaev, Astron. Astrophys. 24, 337 (1973)
J. Silk, A. Nusser, Astrophys. J. 725, 556 (2010)
J. Silk, M.J. Rees, Astron. Astrophys. 331, L1 (1998)
A. Soltan, Mon. Not. R. Astron. Soc. 200, 115 (1982)
D.N. Spergel et al., Astrophys. J. Suppl. Ser. 148, 175 (2003)
E. Sturm, E. González-Alfonso, S. Veilleux et al., Astrophys. J. 733, L16+ (2011)
M. Su, T.R. Slatyer, D.P. Finkbeiner, Astrophys. J. 724, 1044 (2010)
L.J. Tacconi, R. Genzel, D. Lutz, D. Rigopoulou, A.J. Baker, C. Iserlohe, M. Tecza, Astrophys. J. 580, 73 (2002)
F. Tombesi, M. Cappi, J.N. Reeves, G.G.C. Palumbo, T. Yaqoob, V. Braito, M. Dadina, Astron. Astrophys. 521, A57+ (2010). arXiv:1006.2858
F. Tombesi, M. Cappi, J.N. Reeves, G.G.C. Palumbo, V. Braito, M. Dadina, Astrophys. J. 742, 44 (2011)
S. Veilleux, D.S.N. Rupke, D.-C. Kim et al., Astrophys. J. Suppl. Ser. 182, 628 (2009)
K. Zubovas, A.R. King, Astrophys. J. 745, L34 (2012a)
K. Zubovas, A.R. King, Mon. Not. R. Astron. Soc. 426, 2751 (2012b)
K. Zubovas, A.R. King, S. Nayakshin, Mon. Not. R. Astron. Soc. 415, L21 (2011)
Acknowledgements
I thank ISSI for its hospitality, and Ken Pounds, Jim Pringle, Kastytis Zubovas, Chris Nixon, Sergei Nayakshin, and Chris Power for comments on this chapter, and for many fruitful interactions on these subjects over the years.
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King, A. The Supermassive Black Hole—Galaxy Connection. Space Sci Rev 183, 427–451 (2014). https://doi.org/10.1007/s11214-013-0018-2
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DOI: https://doi.org/10.1007/s11214-013-0018-2