Calibrating the Galaxy Halo – Black Hole Relation Based on the Clustering of Quasars

Abstract Observationally, constraining the baryonic cycle within massive galaxies has proven to be quite difficult. In particular, the role of black hole feedback in regulating star formation, a key process in our theoretical understanding of galaxy formation, remains highly debated. We present here observational evidence showing that, at fixed stellar velocity dispersion, the temperature of the hot gas is higher for those galaxies hosting more massive black holes in their centers. Analyzed in the context of well-established scaling relations, particularly the mass–size plane, the relation between the mass of the black hole and the temperature of the hot gas around massive galaxies provides further observational support to the idea that baryonic processes within massive galaxies are regulated by the combined effects of the galaxy halo virial temperature and black hole feedback, in agreement with the expectations from the EAGLE cosmological numerical simulation.

Download Full-text

Calibrating the Galaxy Halo–Black Hole Relation Based on the Clustering of Quasars

The Astrophysical Journal ◽

10.1086/425263 ◽

2005 ◽

Vol 621 (1) ◽

pp. 95-103 ◽

Cited By ~ 28

Author(s):

J. Stuart B. Wyithe ◽

Abraham Loeb

Keyword(s):

Black Hole ◽

The Galaxy ◽

Galaxy Halo

Download Full-text

Effects of supernovae feedback and black hole outflows in the evolution of Dwarf Spheroidal Galaxies

Proceedings of the International Astronomical Union ◽

10.1017/s174392132000215x ◽

2020 ◽

Vol 15 (S359) ◽

pp. 280-282

Author(s):

Gustavo Amaral Lanfranchi ◽

Anderson Caproni ◽

Jennifer F. Soares ◽

Larissa S. de Oliveira

Keyword(s):

Black Hole ◽

Homogeneous Medium ◽

Massive Black Hole ◽

Dwarf Spheroidal Galaxies ◽

Stellar Feedback ◽

Gas Removal ◽

The Galaxy ◽

Main Driver ◽

Ia Supernovae ◽

Jet Structure

AbstractThe gas evolution of a typical Dwarf Spheroidal Galaxy is investigated by means of 3D hydrodynamic simulations, taking into account the feedback of type II and Ia supernovae, the outflow of an Intermediate Massive Black Hole (IMBH) and a static cored dark matter potential. When the IMBH’s outflow is simulated in an homogeneous medium a jet structure is created and a small fraction of the gas is pushed away from the galaxy. No jet structure can be seen, however, when the medium is disturbed by supernovae, but gas is still pushed away. In this case, the main driver of the gas removal are the supernovae. The interplay between the stellar feedback and the IMBH’s outflow should be taken into account.

Download Full-text

On the formation and stability of fermionic dark matter halos in a cosmological framework

Monthly Notices of the Royal Astronomical Society ◽

10.1093/mnras/staa3986 ◽

2020 ◽

Author(s):

Carlos R Argüelles ◽

Manuel I Díaz ◽

Andreas Krut ◽

Rafael Yunis

Keyword(s):

Black Hole ◽

Dark Matter ◽

Space Distribution ◽

Coarse Grained ◽

Dark Matter Halos ◽

The Core ◽

The Galaxy ◽

Gravitating Systems ◽

The Given ◽

First Time

Abstract The formation and stability of collisionless self-gravitating systems is a long standing problem, which dates back to the work of D. Lynden-Bell on violent relaxation, and extends to the issue of virialization of dark matter (DM) halos. An important prediction of such a relaxation process is that spherical equilibrium states can be described by a Fermi-Dirac phase-space distribution, when the extremization of a coarse-grained entropy is reached. In the case of DM fermions, the most general solution develops a degenerate compact core surrounded by a diluted halo. As shown recently, the latter is able to explain the galaxy rotation curves while the DM core can mimic the central black hole. A yet open problem is whether this kind of astrophysical core-halo configurations can form at all, and if they remain stable within cosmological timescales. We assess these issues by performing a thermodynamic stability analysis in the microcanonical ensemble for solutions with given particle number at halo virialization in a cosmological framework. For the first time we demonstrate that the above core-halo DM profiles are stable (i.e. maxima of entropy) and extremely long lived. We find the existence of a critical point at the onset of instability of the core-halo solutions, where the fermion-core collapses towards a supermassive black hole. For particle masses in the keV range, the core-collapse can only occur for Mvir ≳ E9M⊙ starting at zvir ≈ 10 in the given cosmological framework. Our results prove that DM halos with a core-halo morphology are a very plausible outcome within nonlinear stages of structure formation.

Download Full-text

The Center of the Galaxy: Evidence for a Massive Black Hole

Black Holes in Binaries and Galactic Nuclei: Diagnostics, Demography and Formation - ESO ASTROPHYSICS SYMPOSIA ◽

10.1007/10720995_10 ◽

2006 ◽

pp. 63-71

Author(s):

Andreas Eckart ◽

Thomas Ott ◽

Reinhard Genzel

Keyword(s):

Black Hole ◽

Massive Black Hole ◽

The Galaxy

Download Full-text

The Galaxy Zoo survey for giant AGN-ionized clouds: past and present black hole accretion events

Monthly Notices of the Royal Astronomical Society ◽

10.1111/j.1365-2966.2011.20101.x ◽

2011 ◽

Vol 420 (1) ◽

pp. 878-900 ◽

Cited By ~ 78

Author(s):

William C. Keel ◽

S. Drew Chojnowski ◽

Vardha N. Bennert ◽

Kevin Schawinski ◽

Chris J. Lintott ◽

...

Keyword(s):

Black Hole ◽

Black Hole Accretion ◽

The Galaxy ◽

Hole Accretion

Download Full-text

Maturing satellite kinematics into a competitive probe of the galaxy–halo connection

Monthly Notices of the Royal Astronomical Society ◽

10.1093/mnras/sty2950 ◽

2018 ◽

Vol 482 (4) ◽

pp. 4824-4845 ◽

Cited By ~ 7

Author(s):

Johannes U Lange ◽

Frank C van den Bosch ◽

Andrew R Zentner ◽

Kuan Wang ◽

Antonio S Villarreal

Keyword(s):

The Galaxy ◽

Galaxy Halo

Download Full-text

Accretion and Outflow in Active Galaxies

Proceedings of the International Astronomical Union ◽

10.1017/s1743921310006484 ◽

2009 ◽

Vol 5 (S267) ◽

pp. 273-282

Author(s):

Andrew King

Keyword(s):

Black Hole ◽

Large Scale ◽

Host Galaxy ◽

Small Scale ◽

Gas Flows ◽

Inverse Compton ◽

The Galaxy ◽

Black Hole Growth ◽

Lower Excitation ◽

Hole Growth

AbstractI review accretion and outflow in active galactic nuclei. Accreti4on appears to occur in a series of very small-scale, chaotic events, whose gas flows have no correlation with the large-scale structure of the galaxy or with each other. The accreting gas has extremely low specific angular momentum and probably represents only a small fraction of the gas involved in a galaxy merger, which may be the underlying driver.Eddington accretion episodes in AGN must be common in order for the supermassive black holes to grow. I show that they produce winds with velocities v ~ 0.1c and ionization parameters implying the presence of resonance lines of helium-like and hydrogen-like iron. The wind creates a strong cooling shock as it interacts with the interstellar medium of the host galaxy, and this cooling region may be observable in an inverse Compton continuum and lower-excitation emission lines associated with lower velocities. The shell of matter swept up by the shocked wind stalls unless the black hole mass has reached the value Mσ implied by the M–σ relation. Once this mass is reached, further black hole growth is prevented. If the shocked gas did not cool as asserted above, the resulting (“energy-driven”) outflow would imply a far smaller SMBH mass than actually observed. Minor accretion events with small gas fractions can produce galaxy-wide outflows, including fossil outflows in galaxies where there is little current AGN activity.

Download Full-text