scholarly journals SIZING UP PARTIALLY DEPLETED GALAXY CORES

2012 ◽  
Vol 755 (2) ◽  
pp. 163 ◽  
Author(s):  
Bililign T. Dullo ◽  
Alister W. Graham
Keyword(s):  
Galaxy Cores

scholarly journals Ultraluminous Infrared Galaxies

1999 ◽  
Vol 186 ◽  
pp. 289-294 ◽  
Author(s):  
D.B. Sanders ◽  
J.A. Surace ◽  
C.M. Ishida
Keyword(s):  
Globular Clusters ◽  
Elliptical Galaxy ◽  
Seyfert Galaxies ◽  
Infrared Galaxies ◽  
Primary Stage ◽  
Massive Black Holes ◽  
Bolometric Luminosity ◽  
Ultraluminous Infrared Galaxies ◽  
Supernova Explosions ◽  
Galaxy Cores

At luminosities above ~ 1011L⊙, infrared galaxies become the dominant population of extragalactic objects in the local Universe (z < 0.5), being more numerous than optically selected starburst and Seyfert galaxies, and QSOs at comparable bolometric luminosity. At the highest luminosities, ultraluminous infrared galaxies (ULIGs: Lir > 1012L⊙), outnumber optically selected QSOs by a factor of ~ 1.5–2. All of the nearest ULIGs (z <0.1) appear to be advanced mergers that are powered by both a circumnuclear starburst and AGN, both of which are fueled by an enormous concentration of molecular gas (~ 1010M⊙) that has been funneled into the merger nucleus. ULIGs may represent a primary stage in the formation of massive black holes and elliptical galaxy cores. The intense circumnuclear starburst that accompanies the ULIG phase may also represent a primary stage in the formation of globular clusters, and the metal enrichment of the intergalactic medium by gas and dust expelled from the nucleus due to the combined forces of supernova explosions and powerful stellar winds.

scholarly journals 3.3. Circumnuclear regions of active and non-active barred galaxies

1998 ◽  
Vol 184 ◽  
pp. 93-94
Author(s):  
J.H. Knapen
Keyword(s):  
High Resolution ◽  
Near Infrared ◽  
Infrared Imaging ◽  
Seyfert Galaxy ◽  
Active Galaxies ◽  
Necessary Condition ◽  
Nuclear Activity ◽  
Barred Galaxies ◽  
Galaxy Cores

I discuss the role of galactic bars in the fuelling of (circum)nuclear activity. Since the majority of all galaxies are barred, the presence of a bar in a Seyfert galaxy cannot be the sole reason for their activity, although it appears to be a necessary condition for activity. Two options for further work are being explored, high-resolution near-infrared imaging of samples of active and non-active galaxies, and detailed case studies of selected galaxy cores.

scholarly journals Ejection of Supermassive Black Holes from Galaxy Cores

2008 ◽  
Vol 678 (2) ◽  
pp. 780-797 ◽  
Author(s):  
Alessia Gualandris ◽  
David Merritt
Keyword(s):  
Black Holes ◽  
Supermassive Black Holes ◽  
Galaxy Cores

scholarly journals ON THE TRANSITION FROM NUCLEAR-CLUSTER- TO BLACK-HOLE-DOMINATED GALAXY CORES

2010 ◽  
Vol 714 (2) ◽  
pp. L313-L317 ◽  
Author(s):  
Kenji Bekki ◽  
Alister W. Graham
Keyword(s):  
Black Hole ◽  
Nuclear Cluster ◽  
Galaxy Cores

scholarly journals Recoiling Black Holes: Electromagnetic Signatures, Candidates, and Astrophysical Implications

2012 ◽  
Vol 2012 ◽  
pp. 1-8 ◽  
Author(s):  
S. Komossa
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Active Galactic Nuclei ◽  
Galactic Nuclei ◽  
Host Galaxies ◽  
Wide Range ◽  
Galaxy Cores ◽  
Galaxy Assembly ◽  
Anisotropic Emission

Supermassive black holes (SMBHs) may not always reside right at the centers of their host galaxies. This is a prediction of numerical relativity simulations, which imply that the newly formed single SMBH, after binary coalescence in a galaxy merger, can receive kick velocities up to several 1000 km/s due to anisotropic emission of gravitational waves. Long-lived oscillations of the SMBHs in galaxy cores, and in rare cases even SMBH ejections from their host galaxies, are the consequence. Observationally, accreting recoiling SMBHs would appear as quasars spatially and/or kinematically offset from their host galaxies. The presence of the “kicks” has a wide range of astrophysical implications which only now are beginning to be explored, including consequences for black hole and galaxy assembly at the epoch of structure formation, black hole feeding, and unified models of active galactic nuclei (AGN). Here, we review the observational signatures of recoiling SMBHs and the properties of the first candidates which have emerged, including follow-up studies of the candidate recoiling SMBH of SDSSJ092712.65+294344.0.

scholarly journals Evolutionary models of rotating dense stellar systems: challenges in software and hardware

2014 ◽  
Vol 10 (S312) ◽  
pp. 239-240
Author(s):  
Jose Fiestas
Keyword(s):  
Black Hole ◽  
Globular Clusters ◽  
High Performance ◽  
Stellar Systems ◽  
Evolutionary Models ◽  
The Galaxy ◽  
Black Hole Growth ◽  
Galaxy Cores ◽  
Hole Growth ◽  
Gravitating Systems

AbstractWe present evolutionary models of rotating self-gravitating systems (e.g. globular clusters, galaxy cores). These models are characterized by the presence of initial axisymmetry due to rotation. Central black hole seeds are alternatively included in our models, and black hole growth due to consumption of stellar matter is simulated until the central potential dominates the kinematics in the core. Goal is to study the long-term evolution (~ Gyr) of relaxed dense stellar systems, which deviate from spherical symmetry, their morphology and final kinematics. With this purpose, we developed a 2D Fokker-Planck analytical code, which results we confirm by detailed N-Body techniques, applying a high performance code, developed for GPU machines. We compare our models to available observations of galactic rotating globular clusters, and conclude that initial rotation modifies significantly the shape and lifetime of these systems, and can not be neglected in studying the evolution of globular clusters, and the galaxy itself.

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