H I Observations of the Supermassive Binary Black Hole System in 0402+379

Rodriguez, Carl L.; Taylor, G. B.; Zavala, R. T.; Pihlström, Y. M.; Peck, A. B.

doi:10.1088/0004-637x/697/1/37

Cited by 66 publications

(50 citation statements)

References 17 publications

(26 reference statements)

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“…Bianchi et al identify a binary AGN in Mrk 463 with projected separation ∼ 3.8 kpc [580]. Finally, using multifrequency observations with the Very Long Baseline Array (VLBA), Rodriguez et al [581,582] report the discovery of a SMBH binary in the radio galaxy 0402+379 with a total estimated mass of 1.5×10 8 M ⊙ and a projected orbital separation of just 7.3 pc. This is the smallest orbital separation by more than two orders of magnitude, but even for this relatively close binary the emitted gravitational waves have frequency ∼ 2 × 10 −13 Hz, way too low to be observed by LISA, and a merger time ∼ 10 18 yr (much longer than the age of the Universe) if gravitational radiation is the only dissipative mechanism.…”

Section: Spins: Theoretical Expectationsmentioning

confidence: 99%

Quasinormal modes of black holes and black branes

Berti

Cardoso

Starinets

2009

Class. Quantum Grav.

1,740

2,169

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Abstract. Quasinormal modes are eigenmodes of dissipative systems. Perturbations of classical gravitational backgrounds involving black holes or branes naturally lead to quasinormal modes. The analysis and classification of the quasinormal spectra requires solving non-Hermitian eigenvalue problems for the associated linear differential equations. Within the recently developed gauge-gravity duality, these modes serve as an important tool for determining the near-equilibrium properties of strongly coupled quantum field theories, in particular their transport coefficients, such as viscosity, conductivity and diffusion constants. In astrophysics, the detection of quasinormal modes in gravitational wave experiments would allow precise measurements of the mass and spin of black holes as well as new tests of general relativity. This review is meant as an introduction to the subject, with a focus on the recent developments in the field.

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Section: Spins: Theoretical Expectationsmentioning

confidence: 99%

Quasinormal modes of black holes and black branes

Berti

Cardoso

Starinets

2009

Class. Quantum Grav.

1,740

2,169

View full text Add to dashboard Cite

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“…The rapid gas concentration may fuel intensive black hole accretion. Although AGN pairs with >10 kpc transverse separations comprise ∼0.1% of the AGN population (e.g., Hennawi et al 2006Hennawi et al , 2010Myers et al 2007Myers et al , 2008Green et al 2010), there are surprisingly few known kpc-to pc-scale binaries (e.g., Komossa et al 2003;Valtonen et al 2008;Rodriguez et al 2009), owing in large to the observational difficulty of spatially resolving such binaries.…”

Section: Introductionmentioning

confidence: 99%

Mergers in Double-Peaked [O Iii] Active Galactic Nuclei

Myers

Djorgovski

et al. 2011

ApJ

109

115

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As a natural consequence of galaxy mergers, binary active galactic nuclei (AGNs) should be commonplace. Nevertheless, observational confirmations are rare, especially for binaries with separations less than 10 kpc. Such a system may show two sets of narrow emission lines in a single spectrum owing to the orbital motion of the binary. We have obtained high-resolution near-infrared images of 50 double-peaked [O iii]λ5007 AGNs with the Keck II laser guide star adaptive optics system. The Sloan Digital Sky Survey sample is compiled from the literature and consists of 17 type-1 AGNs between 0.18 < z < 0.56 and 33 type-2 AGNs between 0.03 < z < 0.24. The new images reveal eight type-1 and eight type-2 sources that are apparently undergoing mergers. These are strong candidates of kpc-scale binary AGNs because they show multiple components separated between 0.6 and 12 kpc and often disturbed morphologies. Because most of the type-1s are at higher redshifts than the type-2s, the higher merger fraction of type-1s (47% ± 20%) compared to that of type-2s (24% ± 10%) can be attributed to the general evolution of galaxy merger fraction with redshift. Furthermore, we show that AGN mergers are outliers of the M BH -σ relation because of overestimated stellar velocity dispersions, illustrating the importance of removing mergers from the samples defining the M BH -σ relations. Finally, we find that the emission-line properties are indistinguishable for spatially resolved and unresolved sources, emphasizing that scenarios involving a single AGN can produce the same double-peaked line profiles and they account for at least 70% of the double-peaked [O iii] AGNs.

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“…The caveat is that it will resolve out much more smooth emission so it can be difficult to discern an overall source structure. In addition, the motion of matter around the putative BBH system could be probed with VLBI or synthesis radio telescope observations of the velocity distribution of H I absorption line profiles, as done for the known BBH in B0402+379 (Rodriguez et al 2009;Morganti, Emonts & Oosterloo 2009). …”

Section: Discussionmentioning

confidence: 99%

VLBA 24 and 43 GHz observations of massive binary black hole candidate PKS 1155 + 251

Yang

Ling

Yang

et al. 2017

Monthly Notices of the Royal Astronomical Society

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PKS 1155+251 is a radio-loud quasar source at z = 0.203. Observations using very long baseline interferometry (VLBI) at ∼2, 5, 8 and 15 GHz show that the structure of the radio source is quite complicated on parsec scales and that the outer hot spots are apparently undergoing a significant contraction. Because these results cannot be fully explained based on the compact symmetric object (CSO) scenario with a radio core located between the northern and southern complexes, we made observations with the Very Long Baseline Array (VLBA) at 24 and 43 GHz to search for compact substructures and alternative interpretations. The results show that the radio core revealed in the previous VLBI observations remains compact with a flat spectrum in our sub-milli-arcsecond-resolution images; the northern lobe emission becomes faint at 24 GHz and is mostly resolving out at 43 GHz; the southern complex is more bright but has been resolved into the brightest southern-end (S1) and jet or tail alike components westwards. Explaining the southern components aligned westward with a standard CSO scenario alone remains a challenge. As for the flatter spectral index of the southern-end component S1 between 24 and 43 GHz in our observations and the significant 15 GHz VLBA flux variability of S1, an alternative scenario is that the southern complex may be powered by a secondary black hole residing at S1. But more sensitive and high-resolution VLBI monitoring is required to discriminate the CSO and the binary black hole scenarios.

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H I Observations of the Supermassive Binary Black Hole System in 0402+379

Cited by 66 publications

References 17 publications

Quasinormal modes of black holes and black branes

Quasinormal modes of black holes and black branes

Mergers in Double-Peaked [O Iii] Active Galactic Nuclei

VLBA 24 and 43 GHz observations of massive binary black hole candidate PKS 1155 + 251

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