scholarly journals Promise of Persistent Multi-Messenger Astronomy with the Blazar OJ 287

Galaxies ◽  
2021 ◽  
Vol 10 (1) ◽  
pp. 1
Author(s):  
Mauri J. Valtonen ◽  
Lankeswar Dey ◽  
Achamveedu Gopakumar ◽  
Staszek Zola ◽  
S. Komossa ◽  
...  
Keyword(s):  
Black Hole ◽  
Spectral Lines ◽  
Host Galaxy ◽  
Central Engine ◽  
Multi Wavelength ◽  
Hole Model ◽  
Electromagnetic Signals ◽  
The Times ◽  
Spectral Survey ◽  
Blazar Oj 287

Successful observations of the seven predicted bremsstrahlung flares from the unique bright blazar OJ 287 firmly point to the presence of a nanohertz gravitational wave (GW) emitting supermassive black hole (SMBH) binary central engine. We present arguments for the continued monitoring of the source in several electromagnetic windows to firmly establish various details of the SMBH binary central engine description for OJ 287. In this article, we explore what more can be known about this system, particularly with regard to accretion and outflows from its two accretion disks. We mainly concentrate on the expected impact of the secondary black hole on the disk of the primary on 3 December 2021 and the resulting electromagnetic signals in the following years. We also predict the times of exceptional fades, and outline their usefulness in the study of the host galaxy. A spectral survey has been carried out, and spectral lines from the secondary were searched for but were not found. The jet of the secondary has been studied and proposals to discover it in future VLBI observations are mentioned. In conclusion, the binary black hole model explains a large number of observations of different kinds in OJ 287. Carefully timed future observations will be able to provide further details of its central engine. Such multi-wavelength and multidisciplinary efforts will be required to pursue multi-messenger nanohertz GW astronomy with OJ 287 in the coming decades.

scholarly journals Linking the central engine to the jet properties in radio loud AGN

2014 ◽  
Vol 10 (S313) ◽  
pp. 329-330
Author(s):  
A. Olguín-Iglesias ◽  
J. León-Tavares ◽  
V. Chavushyan ◽  
E. Valtaoja ◽  
C. Añorve ◽  
...  
Keyword(s):  
Black Hole ◽  
Host Galaxy ◽  
Base Line ◽  
Black Hole Mass ◽  
Host Galaxies ◽  
Optical Telescope ◽  
Central Engine ◽  
Early Results ◽  
Relativistic Jet ◽  
Line Array

AbstractWe explore the connection between the black hole mass and its relativistic jet for a sample of radio-loud AGN (z < 1), in which the relativistic jet parameters are well estimated by means of long term monitoring with the 14m Metsähovi millimeter wave telescope and the Very Long Base-line Array (VLBA). NIR host galaxy images taken with the NOTCam on the Nordic Optical Telescope (NOT) and retrieved from the 2MASS all-sky survey allowed us to perform a detailed surface brightness decomposition of the host galaxies in our sample and to estimate reliable black hole masses via their bulge luminosities. We present early results on the correlations between black hole mass and the relativistic jet parameters. Our preliminary results suggest that the more massive the black hole is, the faster and the more luminous jet it produces.

scholarly journals Explaining temporal variations in the jet position angle of the blazar OJ 287 using its binary black hole central engine model

2021 ◽  
Author(s):  
Lankeswar Dey ◽  
Mauri J Valtonen ◽  
A Gopakumar ◽  
Rocco Lico ◽  
José L Gómez ◽  
...  
Keyword(s):  
Black Hole ◽  
Position Angle ◽  
Temporal Variations ◽  
Optical Observations ◽  
High Angular Resolution ◽  
Orbital Parameters ◽  
Engine Model ◽  
Binary Black Hole ◽  
Central Engine ◽  
Blazar Oj 287

Abstract The bright blazar OJ 287 is the best-known candidate for hosting a supermassive black hole binary system. It inspirals due to the emission of nanohertz gravitational waves (GWs). Observations of historical and predicted quasi-periodic high-brightness flares in its century-long optical lightcurve, allow us to determine the orbital parameters associated with the binary black hole (BBH) central engine. In contrast, the radio jet of OJ 287 has been covered with Very Long Baseline Interferometry (VLBI) observations for only about 30 years and these observations reveal that the position angle (PA) of the jet exhibits temporal variations at both millimetre and centimetre wavelengths. Here we associate the observed PA variations in OJ 287 with the precession of its radio jet. In our model, the evolution of the jet direction can be associated either with the primary black hole (BH) spin evolution or with the precession of the angular momentum direction of the inner region of the accretion disc. Our Bayesian analysis shows that the BBH central engine model, primarily developed from optical observations, can also broadly explain the observed temporal variations in the radio jet of OJ 287 at frequencies of 86, 43, and 15 GHz. Ongoing Global mm-VLBI Array (GMVA) observations of OJ 287 have the potential to verify our predictions for the evolution of its 86 GHz PA values. Additionally, thanks to the extremely high angular resolution that the Event Horizon Telescope (EHT) can provide, we explore the possibility to test our BBH model through the detection of the jet in the secondary black hole .

scholarly journals The Unique Blazar OJ 287 and Its Massive Binary Black Hole Central Engine

Universe ◽  
2019 ◽  
Vol 5 (5) ◽  
pp. 108 ◽  
Author(s):  
Lankeswar Dey ◽  
Achamveedu Gopakumar ◽  
Mauri Valtonen ◽  
Stanislaw Zola ◽  
Abhimanyu Susobhanan ◽  
...  
Keyword(s):  
Black Hole ◽  
Strong Field ◽  
Observable Universe ◽  
Engine Model ◽  
Binary Black Hole ◽  
Central Engine ◽  
Optical Light Curve ◽  
General Relativistic ◽  
Improved Model ◽  
Blazar Oj 287

The bright blazar OJ 287 is the best-known candidate for hosting a nanohertz gravitational wave (GW) emitting supermassive binary black hole (SMBBH) in the present observable universe. The binary black hole (BBH) central engine model, proposed by Lehto and Valtonen in 1996, was influenced by the two distinct periodicities inferred from the optical light curve of OJ 287. The current improved model employs an accurate general relativistic description to track the trajectory of the secondary black hole (BH) which is crucial to predict the inherent impact flares of OJ 287. The successful observations of three predicted impact flares open up the possibility of using this BBH system to test general relativity in a hitherto unexplored strong field regime. Additionally, we briefly describe an ongoing effort to interpret observations of OJ 287 in a Bayesian framework.

scholarly journals HOST GALAXY PROPERTIES AND BLACK HOLE MASS OF SWIFT J164449.3+573451 FROM MULTI-WAVELENGTH LONG-TERM MONITORING ANDHSTDATA

2015 ◽  
Vol 808 (1) ◽  
pp. 96 ◽  
Author(s):  
Yongmin Yoon ◽  
Myungshin Im ◽  
Yiseul Jeon ◽  
Seong-Kook Lee ◽  
Philip Choi ◽  
...  
Keyword(s):  
Black Hole ◽  
Host Galaxy ◽  
Black Hole Mass ◽  
Multi Wavelength ◽  
Long Term Monitoring ◽  
Term Monitoring

scholarly journals Understanding the environment around the intermediate mass black hole candidate ESO 243-49 HLX-1

2017 ◽  
Vol 602 ◽  
pp. A103 ◽  
Author(s):  
N. A. Webb ◽  
A. Guérou ◽  
B. Ciambur ◽  
A. Detoeuf ◽  
M. Coriat ◽  
...  
Keyword(s):  
Black Hole ◽  
Host Galaxy ◽  
Intermediate Mass ◽  
Rotating Disc ◽  
Large Variability ◽  
Black Hole Candidate ◽  
Supermassive Black Hole ◽  
Flux Variability ◽  
The Galaxy ◽  
Multi Wavelength

Aims. ESO 243-49 HLX-1, otherwise known as HLX-1, is an intermediate mass black hole (IMBH) candidate located 8′′ (3.7 Kpc) from the centre of the edge-on S0 galaxy ESO 243-49. How the black hole came to be associated with this galaxy, and the nature of the environment in which it resides, remain unclear. Using multi-wavelength observations we aim to investigate the nature of the medium surrounding HLX-1, search for evidence of past mergers with ESO 243-49 and constrain parameters of the galaxy, including the mass of the expected central supermassive black hole, essential for future modelling of the interaction of the IMBH and ESO 243-49. Methods. We have reduced and analysed integral field unit observations of ESO 243-49 that were taken with the MUSE instrument on the VLT. Using complementary multi-wavelength data, including X-shooter, HST, Swift, Chandra and ATCA data, we have further examined the vicinity of HLX-1. We additionally examined the nature of the host galaxy and estimate the mass of the central supermassive black hole in ESO 243-49 using (black hole mass)–(host spheroid) scaling relations and the fundamental plane of black hole activity. Results. No evidence for a recent minor-merger that could result in the presence of the IMBH is discerned, but the data are compatible with a scenario in which minor mergers may have occurred in the history of ESO 243-49. The MUSE data reveal a rapidly rotating disc in the centre of the galaxy, around the supermassive black hole. The mass of the supermassive black hole at the centre of ESO 243-49 is estimated to be 0.5−23 × 107M⊙. Studying the spectra of HLX-1, that were taken in the low and hard state, we determine Hα flux variability to be at least a factor 6, compared to observations taken during the high and soft state. This Hα flux variability over one year indicates that the line originates close to the intermediate mass black hole, excluding the possibility that the line emanates from a surrounding nebula or a star cluster. The large variability associated with the X-ray states of HLX-1 confirms that the Hα line is associated with the object and therefore validates the distance to HLX-1.

scholarly journals Gravitational and Electromagnetic Perturbations of a Charged Black Hole in a General Gauge Condition

Particles ◽  
2021 ◽  
Vol 4 (2) ◽  
pp. 106-128
Author(s):  
Claudia Moreno ◽  
Juan Carlos Degollado ◽  
Darío Núñez ◽  
Carlos Rodríguez-Leal
Keyword(s):  
Black Hole ◽  
Scalar Function ◽  
Gauge Condition ◽  
Fluid Distribution ◽  
Electromagnetic Signal ◽  
Charged Fluid ◽  
Coupled Equations ◽  
Electromagnetic Signals ◽  
Limiting Case ◽  
Weyl Scalar

We derive a set of coupled equations for the gravitational and electromagnetic perturbation in the Reissner–Nordström geometry using the Newman–Penrose formalism. We show that the information of the physical gravitational signal is contained in the Weyl scalar function Ψ4, as is well known, but for the electromagnetic signal, the information is encoded in the function χ, which relates the perturbations of the radiative Maxwell scalars φ2 and the Weyl scalar Ψ3. In deriving the perturbation equations, we do not impose any gauge condition and as a limiting case, our analysis contains previously obtained results, for instance, those from Chandrashekhar’s book. In our analysis, we also include the sources for the perturbations and focus on a dust-like charged fluid distribution falling radially into the black hole. Finally, by writing the functions on the basis of spin-weighted spherical harmonics and the Reissner–Nordström spacetime in Kerr–Schild type coordinates, a hyperbolic system of coupled partial differential equations is presented and numerically solved. In this way, we completely solve a system that generates a gravitational signal as well as an electromagnetic/gravitational one, which sets the basis to find correlations between them and thus facilitates gravitational wave detection via electromagnetic signals.

An accreting < 105M⊙ black hole at the center of dwarf galaxy IC750

2019 ◽  
Vol 15 (S356) ◽  
pp. 376-376
Author(s):  
Ingyin Zaw
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Dwarf Galaxies ◽  
Dwarf Galaxy ◽  
Host Galaxy ◽  
Scaling Relations ◽  
Host Galaxies ◽  
Seed Formation ◽  
Maser Emission ◽  
Water Masers

AbstractNuclear black holes in dwarf galaxies are important for understanding the low end of the supermassive black hole mass distribution and the black hole-host galaxy scaling relations. IC 750 is a rare system which hosts an AGN, found in ˜0.5% of dwarf galaxies, with circumnuclear 22 GHz water maser emission, found in ˜3–5% of Type 2 AGNs. Water masers, the only known tracer of warm, dense gas in the center parsec of AGNs resolvable in position and velocity, provide the most precise and accurate mass measurements of SMBHs outside the local group. We have mapped the maser emission in IC 750 and find that it traces a nearly edge-on warped disk, 0.2 pc in diameter. The central black hole has an upper limit mass of ˜1 × 105 M⊙ and a best fit mass of ˜8 × 104 M⊙, one to two orders of magnitude below what is expected from black hole-galaxy scaling relations. This has implications for models of black hole seed formation in the early universe, the growth of black holes, and their co-evolution with their host galaxies.

Substructure in black hole scaling diagrams and implications for the coevolution of black holes and galaxies

2019 ◽  
Vol 15 (S359) ◽  
pp. 37-39
Author(s):  
Benjamin L. Davis ◽  
Nandini Sahu ◽  
Alister W. Graham
Keyword(s):  
Black Hole ◽  
Stellar Mass ◽  
Host Galaxy ◽  
Scaling Relations ◽  
Black Hole Mass ◽  
Physical Processes ◽  
Stellar Velocity ◽  
Galaxy Sample ◽  
Evolutionary Paths ◽  
Black Hole Masses

AbstractOur multi-component photometric decomposition of the largest galaxy sample to date with dynamically-measured black hole masses nearly doubles the number of such galaxies. We have discovered substantially modified scaling relations between the black hole mass and the host galaxy properties, including the spheroid (bulge) stellar mass, the total galaxy stellar mass, and the central stellar velocity dispersion. These refinements partly arose because we were able to explore the scaling relations for various sub-populations of galaxies built by different physical processes, as traced by the presence of a disk, early-type versus late-type galaxies, or a Sérsic versus core-Sérsic spheroid light profile. The new relations appear fundamentally linked with the evolutionary paths followed by galaxies, and they have ramifications for simulations and formation theories involving both quenching and accretion.

scholarly journals Supermassive black hole mass regulated by host galaxy morphology

2009 ◽  
Vol 400 (4) ◽  
pp. 1803-1807 ◽  
Author(s):  
Y. Watabe ◽  
N. Kawakatu ◽  
M. Imanishi ◽  
T. T. Takeuchi
Keyword(s):  
Black Hole ◽  
Host Galaxy ◽  
Black Hole Mass ◽  
Supermassive Black Hole ◽  
Galaxy Morphology
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