scholarly journals Localization of binary black hole mergers with known inclination

2019 ◽  
Vol 488 (3) ◽  
pp. 4459-4463 ◽  
Author(s):  
K Rainer Corley ◽  
Imre Bartos ◽  
Leo P Singer ◽  
Andrew R Williamson ◽  
Zoltán Haiman ◽  
...  
Keyword(s):  
Black Hole ◽  
Binary System ◽  
Active Galactic Nuclei ◽  
Prior Information ◽  
Galactic Nuclei ◽  
Electromagnetic Emission ◽  
Accretion Discs ◽  
Host Galaxies ◽  
Binary Black Hole

ABSTRACT The localization of stellar-mass binary black hole mergers using gravitational waves is critical in understanding the properties of the binaries’ host galaxies, observing possible electromagnetic emission from the mergers, or using them as a cosmological distance ladder. The precision of this localization can be substantially increased with prior astrophysical information about the binary system. In particular, constraining the inclination of the binary can reduce the distance uncertainty of the source. Here, we present the first realistic set of localizations for binary black hole mergers, including different prior constraints on the binaries’ inclinations. We find that prior information on the inclination can reduce the localization volume by a factor of 3. We discuss two astrophysical scenarios of interest: (i) follow-up searches for beamed electromagnetic/neutrino counterparts and (ii) mergers in the accretion discs of active galactic nuclei.

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.

SDSS J154751.94+025550 with double-peaked broad H β but single-peaked broad H α: a candidate for central binary black hole system?

2021 ◽  
Vol 507 (4) ◽  
pp. 5205-5213
Author(s):  
XueGuang Zhang
Keyword(s):  
Black Hole ◽  
Active Galactic Nuclei ◽  
Galactic Nuclei ◽  
Emission Lines ◽  
Broad Line ◽  
Line Profiles ◽  
Physical Conditions ◽  
Binary Black Hole ◽  
Sinusoidal Function

ABSTRACT In this manuscript, an interesting blue active galactic nuclei (AGNs) SDSS J154751.94+025550 (=SDSS J1547) is reported with very different line profiles of broad Balmer emission lines: double-peaked broad H β but single-peaked broad H α. SDSS J1547 is the first AGN with detailed discussions on very different line profiles of the broad Balmer emission lines, besides the simply mentioned different broad lines in the candidate for a binary black hole (BBH) system in SDSS J0159+0105. The very different line profiles of the broad Balmer emission lines can be well explained by different physical conditions to two central BLRs in a central BBH system in SDSS J1547. Furthermore, the long-term light curve from CSS can be well described by a sinusoidal function with a periodicity about 2159 d, providing further evidence to support the expected central BBH system in SDSS J1547. Therefore, it is interesting to treat different line profiles of broad Balmer emission lines as intrinsic indicators of central BBH systems in broad line AGN. Under assumptions of BBH systems, 0.125 per cent of broad-line AGN can be expected to have very different line profiles of broad Balmer emission lines. Future study on more broad line AGN with very different line profiles of broad Balmer emission lines could provide further clues on the different line profiles of broad Balmer emission lines as indicator of BBH systems.

Density diagnostics of photoionized outflows in active galactic nuclei

2019 ◽  
Vol 15 (S350) ◽  
pp. 274-277
Author(s):  
Junjie Mao
Keyword(s):  
Black Hole ◽  
Active Galactic Nuclei ◽  
State Of The Art ◽  
Density Measurement ◽  
Galactic Nuclei ◽  
Next Generation ◽  
Host Galaxies ◽  
Current Generation ◽  
X Ray ◽  
The Impact

AbstractPhotoionized outflows in active galactic nuclei (AGNs) are thought to influence their circumnuclear and host galactic environment. However, the distance of the outflow with respect to the black hole is poorly constrained, which limits our understanding of the kinetic power by the outflow. Therefore, the impact of AGN outflows on their host galaxies is uncertain. If the density of the outflow is known, its distance can be derived. Density measurement via variability studies and density sensitive lines have been used, albeit not very effective in the X-ray band. Good measurements are rather demanding or challenging for the current generation of (grating) spectrometers. The next generation of spectrometers will certainly provide data with better quality and large quantity, leading to tight constraints on the location and the kinetic power of AGN outflows. This contribution summarizes the state-of-the-art in this field.

The Host Galaxies of Radio‐loud Active Galactic Nuclei: The Black Hole–Galaxy Connection

2002 ◽  
Vol 580 (1) ◽  
pp. 96-103 ◽  
Author(s):  
Matthew O’Dowd ◽  
C. Megan Urry ◽  
Riccardo Scarpa
Keyword(s):  
Black Hole ◽  
Active Galactic Nuclei ◽  
Galactic Nuclei ◽  
Host Galaxies

MASSIVE BINARY BLACK HOLE IN ACTIVE GALACTIC NUCLEI AS COSMIC RAYS GENERATOR

1995 ◽  
Vol 04 (02) ◽  
pp. 215-218
Author(s):  
V.I. DOKUCHAEV
Keyword(s):  
Black Hole ◽  
Cosmic Rays ◽  
Active Galactic Nuclei ◽  
Orbital Motion ◽  
Galactic Nuclei ◽  
Frictional Drag ◽  
High Energies ◽  
Binary Black Hole ◽  
Bow Shocks ◽  
Binary Orbit

A model of bow shocks generated by a supersonic orbital motion of a gravitationally bound massive binary black hole in the dense environment of active galactic nuclei (AGN) is proposed. The binary orbit is evolutionary contracting due to gravitational radiation and frictional drag in the ambient gas. The model provides the suitable conditions for the acceleration of cosmic rays up to the ultra-high energies.

scholarly journals OBSCURED GOODS ACTIVE GALACTIC NUCLEI AND THEIR HOST GALAXIES ATz< 1.25: THE SLOW BLACK HOLE GROWTH PHASE

2011 ◽  
Vol 734 (2) ◽  
pp. 121 ◽  
Author(s):  
B. D. Simmons ◽  
J. Van Duyne ◽  
C. M. Urry ◽  
E. Treister ◽  
A. M. Koekemoer ◽  
...  
Keyword(s):  
Black Hole ◽  
Active Galactic Nuclei ◽  
Growth Phase ◽  
Galactic Nuclei ◽  
Host Galaxies ◽  
Black Hole Growth ◽  
Hole Growth

scholarly journals THE BLACK HOLE-BULGE RELATIONSHIP IN LUMINOUS BROAD-LINE ACTIVE GALACTIC NUCLEI AND HOST GALAXIES

2008 ◽  
Vol 135 (3) ◽  
pp. 928-946 ◽  
Author(s):  
Jiajian Shen ◽  
Daniel E. Vanden Berk ◽  
Donald P. Schneider ◽  
Patrick B. Hall
Keyword(s):  
Black Hole ◽  
Active Galactic Nuclei ◽  
Galactic Nuclei ◽  
Broad Line ◽  
Host Galaxies

scholarly journals Slow and massive: low-spin SMBHs can grow more

2019 ◽  
Vol 489 (1) ◽  
pp. 1373-1378 ◽  
Author(s):  
Kastytis Zubovas ◽  
Andrew King
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Active Galactic Nuclei ◽  
Large Scale ◽  
Size Dependence ◽  
Galactic Nuclei ◽  
Host Galaxy ◽  
Host Galaxies ◽  
The Galaxy ◽  
Mass Increment

Abstract Active galactic nuclei (AGNs) probably control the growth of their host galaxies via feedback in the form of wide-angle wind-driven outflows. These establish the observed correlations between supermassive black hole (SMBH) masses and host galaxy properties, e.g. the spheroid velocity dispersion σ. In this paper we consider the growth of the SMBH once it starts driving a large-scale outflow through the galaxy. To clear the gas and ultimately terminate further growth of both the SMBH and the host galaxy, the black hole must continue to grow its mass significantly, by up to a factor of a few, after reaching this point. The mass increment ΔMBH depends sensitively on both galaxy size and SMBH spin. The galaxy size dependence leads to ΔMBH ∝ σ5 and a steepening of the M–σ relation beyond the analytically calculated M ∝ σ4, in agreement with observation. Slowly spinning black holes are much less efficient in producing feedback, so at any given σ the slowest spinning black holes should be the most massive. Current observational constraints are consistent with this picture, but insufficient to test it properly; however, this should change with upcoming surveys.

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