scholarly journals Hot Gas and AGN Feedback in Galaxies and Nearby Groups

2012 ◽  
Vol 8 (S295) ◽  
pp. 257-260
Author(s):  
Christine Jones ◽  
William Forman ◽  
Akos Bogdan ◽  
Scott Randall ◽  
Ralph Kraft ◽  
...  
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Dark Matter Halos ◽  
Early Type ◽  
X Ray ◽  
Massive Galaxies ◽  
Hot Gas ◽  
Supermassive Black Hole ◽  
The Galaxy ◽  
Galaxy Cores

AbstractMassive galaxies harbor a supermassive black hole at their centers. At high redshifts, these galaxies experienced a very active quasar phase, when, as their black holes grew by accretion, they produced enormous amounts of energy. At the present epoch, these black holes still undergo occasional outbursts, although the mode of their energy release is primarily mechanical rather than radiative. The energy from these outbursts can reheat the cooling gas in the galaxy cores and maintain the red and dead nature of the early-type galaxies. These outbursts also can have dramatic effects on the galaxy-scale hot coronae found in the more massive galaxies. We describe research in three areas related to the hot gas around galaxies and their supermassive black holes. First we present examples of galaxies with AGN outbursts that have been studied in detail. Second, we show that X-ray emitting low-luminosity AGN are present in 80% of the galaxies studied. Third, we discuss the first examples of extensive hot gas and dark matter halos in optically faint galaxies.

The effects of outbursts from Supermassive Black Holes: A close look at M87

2019 ◽  
Vol 15 (S359) ◽  
pp. 99-107
Author(s):  
C. Jones ◽  
W. Forman
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Fossil Record ◽  
Virgo Cluster ◽  
Supermassive Black Holes ◽  
Article Title ◽  
X Ray ◽  
Hot Gas ◽  
Supermassive Black Hole ◽  
Evolution Of Galaxies

AbstractSupermassive black holes (SMBHs) play[-105pt]Kindly check and confirm the Article Title. fundamental roles in the evolution of galaxies, groups, and clusters. The fossil record of supermassive black hole outbursts is seen through the cavities and shocks that are imprinted on these gas-rich systems. For M87, the central galaxy in the Virgo cluster, deep Chandra observations illustrate the physics of AGN feedback in hot, gas-rich atmospheres and allow measurements of the age, duration, and power of the outburst from the supermassive black hole in M87 that produced the observed cavities and shocks in the hot X-ray atmosphere.

scholarly journals Be/X-Ray Binaries with Black Holes in the Galaxy and in the Magellanic Clouds

2014 ◽  
Vol 1 (1) ◽  
pp. 175-180 ◽  
Author(s):  
Janusz Ziolkowski
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Neutron Star ◽  
Magellanic Clouds ◽  
X Ray ◽  
The Galaxy ◽  
X Ray Binaries ◽  
Successful Candidate

I will start with the statistics indicating that the objects named in the title of my talk are either non-existing or very elusive to detect (not a single such object is known against 119 known Be/neutron star X-ray binaries). After brief reviewing of the properties of Be/X-ray binaries I discuss several objects that were proposed as the long sought for candidates for Be/black hole X-ray binaries. After three unsuccessful candidates (LS I +61° 303, LS 5039 and MAXI J1836-194), a successful candidate (AGL J2241+4454/MWC 656) was finally, very recently, announced.

scholarly journals On the apparent lack of Be X-ray binaries with black holes in the galaxy and in the Magellanic Clouds

2010 ◽  
Vol 6 (S275) ◽  
pp. 329-330
Author(s):  
Janusz Ziółkowski ◽  
Krzysztof Belczyński
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Neutron Star ◽  
Stellar Population ◽  
Magellanic Clouds ◽  
Population Synthesis ◽  
X Ray ◽  
Stellar Population Synthesis ◽  
The Galaxy ◽  
X Ray Binaries

AbstractIn the Galaxy there are 67 Be X-ray binaries known to-date. Out of those, 45 host a neutron star, and for the reminder the nature of a companion is not known. None, so far, is known to host a black hole. This disparity is referred to as a missing Be – black hole X-ray binary problem. The stellar population synthesis calculations following the formation of Be X-ray binaries (Belczyński & Ziółkowski 2009) predict that the ratio of the binaries with neutron stars to the ones with black holes is rather high FNS/BH ~ 30–50. A comparison of this ratio with the number of confirmed Be – neutron star X-ray binaries (45) indicates that the expected number of Be – black hole X-ray binaries is of the order of only ~0–2. This is entirely consistent with the observed Galactic sample. Therefore, there is no problem of the missing Be+BH X-Ray Binaries for the GalaxyIn the Magellanic Clouds there are 94 Be X-ray binaries known to-date. Out of those, 60 host a neutron star. Again, none hosts a black hole. The stellar population synthesis calculations carried out specifically for the Magellanic Clouds (Ziółkowski & Belczyński 2010) predict that the ratio of the Be X-ray binaries with neutron stars to the ones with black holes is only FNS/BH ~ 10. This value is rather too low, as it implies the expected number of Be+BH X-ray binaries of the order of ~6, while none is observed. We found, that to remove the discrepancy, one has to take into account a different history of the star formation rate in the Magellanic Clouds, with the respect to the Galaxy. New stellar population synthesis calculations are currently being carried out.

scholarly journals 11.1. Black holes and galaxy centers

1998 ◽  
Vol 184 ◽  
pp. 451-458 ◽  
Author(s):  
Douglas Richstone
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Central Black Hole ◽  
The Core ◽  
Supermassive Black Hole ◽  
Normal Galaxy ◽  
The Galaxy ◽  
Major Review

The study of supermassive galactic black holes (BH) has moved beyond discovery to maturity. The are now ∼ 15 reliable detections. The mass of a central black hole apparently correlates with the mass of the hot component of its galactic host. It may be that every normal galaxy has a supermassive black hole carrying about 10−3 of its bulge mass, with important consequences for the structure and evolution of the core of the galaxy. The most recent major review is by Kormendy & Richstone (1995, KR).

scholarly journals A fast and long-lived outflow from the supermassive black hole in NGC 5548

Science ◽  
2014 ◽  
Vol 345 (6192) ◽  
pp. 64-68 ◽  
Author(s):  
J. S. Kaastra ◽  
G. A. Kriss ◽  
M. Cappi ◽  
M. Mehdipour ◽  
P.-O. Petrucci ◽  
...  
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
High Resolution ◽  
Accretion Disk ◽  
Active Galaxies ◽  
Ionized Gas ◽  
X Ray ◽  
Supermassive Black Hole ◽  
Space Observatories ◽  
Ngc 5548

Supermassive black holes in the nuclei of active galaxies expel large amounts of matter through powerful winds of ionized gas. The archetypal active galaxy NGC 5548 has been studied for decades, and high-resolution x-ray and ultraviolet (UV) observations have previously shown a persistent ionized outflow. An observing campaign in 2013 with six space observatories shows the nucleus to be obscured by a long-lasting, clumpy stream of ionized gas not seen before. It blocks 90% of the soft x-ray emission and causes simultaneous deep, broad UV absorption troughs. The outflow velocities of this gas are up to five times faster than those in the persistent outflow, and, at a distance of only a few light days from the nucleus, it may likely originate from the accretion disk.

scholarly journals Black hole feedback and the evolution of massive early-type galaxies

2019 ◽  
Author(s):  
Ignacio Martín-Navarro ◽  
Joseph N Burchett ◽  
Mar Mezcua
Keyword(s):  
Black Hole ◽  
Galaxy Formation ◽  
Theoretical Understanding ◽  
Massive Black Holes ◽  
Massive Galaxies ◽  
Hot Gas ◽  
The Galaxy ◽  
Stellar Velocity ◽  
Mass Size ◽  
Galaxy Halo

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.

scholarly journals Cool circumgalactic gas of passive galaxies from cosmological inflow

2019 ◽  
Vol 625 ◽  
pp. A11 ◽  
Author(s):  
Andrea Afruni ◽  
Filippo Fraternali ◽  
Gabriele Pezzulli
Keyword(s):  
Parametric Models ◽  
Hydrodynamic Interactions ◽  
Dark Matter Halos ◽  
Early Type ◽  
Hot Gas ◽  
The Galaxy ◽  
Central Regions ◽  
Different Temperatures ◽  
Cool Gas ◽  
Multi Phase

The circumgalactic medium (CGM) of galaxies consists of a multi-phase gas with components at very different temperatures, from 104 K to 107 K. One of the greatest puzzles about this medium is the presence of a large amount of low-temperature (T ∼ 104 K) gas around quiescent early-type galaxies (ETGs). Using semi-analytical parametric models, we describe the cool CGM around massive, low-redshift ETGs as the cosmological accretion of gas into their dark matter halos, resulting in an inflow of clouds from the external parts of the halos to the central galaxies. We compare our predictions with the observations of the COS-LRG collaboration. We find that inflow models can successfully reproduce the observed kinematics, the number of absorbers and the column densities of the cool gas. Our MCMC fit returns masses of the cool clouds of about 105 M⊙ and shows that they must evaporate during their journey due to hydrodynamic interactions with the hot gas. We conclude that the cool gas present in the halos of ETGs likely cannot reach the central regions and feed the galaxy star formation, thus explaining why these passive objects are no longer forming stars.

scholarly journals Mergers of Luminous Early-Type Galaxies

2009 ◽  
Vol 5 (S267) ◽  
pp. 270-270
Author(s):  
Z. L. Wen ◽  
J. L. Han ◽  
F. S. Liu
Keyword(s):  
Black Hole ◽  
Gravitational Wave ◽  
Galaxy Mergers ◽  
Early Type ◽  
Redshift Range ◽  
Large Sample ◽  
Massive Galaxies ◽  
Supermassive Black Hole ◽  
Merger Rate ◽  
Close Pairs

Galaxy mergers play an important role in many astrophysical processes, such as growth of massive galaxies, triggering AGN, formation of supermassive black hole (SMBH) binaries, and gravitational wave (GW) radiation. Merger rate is one of key quantities for these studies. Previous studies show that the pair fraction varies in a range of 1%–10% in the redshift range of z = 0.2–1.2. These merger rates are usually calculated from projected close pairs, and very few previous authors have carefully checked the merging fraction of a large sample of pairs.

scholarly journals Chandra and VLA Observations of Supermassive Black Hole Outbursts in M87

2012 ◽  
Vol 8 (S295) ◽  
pp. 261-264
Author(s):  
William Forman ◽  
C. Jones ◽  
Eugene Churazov
Keyword(s):  
Black Hole ◽  
Energy Input ◽  
Virgo Cluster ◽  
Relativistic Plasma ◽  
Radio Observations ◽  
X Ray ◽  
Massive Galaxies ◽  
Supermassive Black Hole

AbstractWe discuss the effects of supermassive black hole (SMBH) outbursts on the hot atmospheres surrounding the central massive galaxies in groups and clusters, as observed with X-ray and radio observations. We focus on a detailed study of the supermassive black hole in M87 at the center of the Virgo cluster using Chandra and VLA observations. We summarize the outburst history and describe the clearly observed energy input from buoyant bubbles of relativistic plasma produced by the central SMBH, uplifted filaments of X-ray emitting gas, and the Mach 1.2 shock together balance the energy lost as gas radiatively cools.

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