Multiple supermassive black hole systems: SKA’s future leading role

Deane, Roger; Paragi, Zsolt; Jarvis, M.; Coriat, M.; Bernardi, G.; Frey, Sándor; Heywood, Ian; Kloeckner, H. R.

doi:10.22323/1.215.0151

Cited by 8 publications

(9 citation statements)

References 40 publications

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“…The Square Kilometre Array (SKA), when fully deployed, should have the powerful survey efficiency and sufficient sensitivity necessary to detect dual AGNs with separations less than 1 kpc, in principle, at all redshifts (Deane et al 2015). The SKA as an element of a VLBI array could be necessary to identify close pairs at parsecscale separations.…”

Section: Discussionmentioning

confidence: 99%

Four Dual Agn Candidates Observed With the Vlba

Gabányi¹,

Frey³

et al. 2016

ApJ

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According to hierarchical structure formation models, merging galaxies are expected to be seen in different stages of coalescence. However, there are currently no straightforward observational methods to either select or to confirm a large number of dual active galactic nucleus (AGN) candidates. Most attempts involve obtaining a better understanding of double-peaked narrow emission line sources, in order to distinguish the objects for which the emission lines originate from narrow-line kinematics or jet-driven outflows, from those which might harbor dual AGNs. We observed four such candidate sources with the Very Long Baseline Array (VLBA), at 1.5 GHz with a ∼10 mas angular resolution, for which the spectral profiles of AGN optical emission suggested the existence of dual AGNs. In SDSS J210449.13-000919.1 and SDSS J23044.82-093345.3 the radio structures are aligned with the optical emission features, thus the double-peaked emission lines might be the results of jet-driven outflows. In the third detected source SDSS J115523.74+150756.9, the radio structure is less extended and is oriented nearly perpendicular to the position angle derived from optical spectroscopy. The fourth source remained undetected with the VLBA, but it was imaged with the Very Large Array at arcsec resolution a few months before our observations, suggesting the existence of an extended radio structure. We did not detect two radio-emitting cores in any of the four sources, a convincing signature of duality.

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Section: Discussionmentioning

confidence: 99%

Four Dual Agn Candidates Observed With the Vlba

Gabányi¹,

Frey³

et al. 2016

ApJ

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“…Such precise distance information will: I) make the PTA signal to single GW sources coherent, allowing perform GW interferometric imaging of the whole sky with angular resolutions of arcminutes (Lee et al 2011). This will enable the search for electromagnetic counterparts to the GW sources, possibly enabling the follow-ups of GW sources with the traditional astronomical tools which can lead to the study of galaxy mergers (Burke-Spolaor 2013; Rosado & Sesana 2014;Deane et al 2015). II) allow us to measure the mass and spin of a SMBHB and map the non-linear dynamics of the gravitational field (Mingarelli et al 2012); when the pulsar term can be distinguished from the Earth term, each pulsar term sees a slightly different piece of the evolutionary history of the binary since its orbital period evolves over the light travel time between the Earth and the pulsar.…”

Section: Time To Detectionmentioning

confidence: 99%

Gravitational Wave Astronomy with the SKA

Janssen¹,

Hobbs

McLaughlin

et al. 2015

Proceedings of Advancing Astrophysics With the Square Kilometre Array — PoS(AASKA14)

372

302

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On a time scale of years to decades, gravitational wave (GW) astronomy will become a reality. Low frequency (∼10 −9 Hz) GWs are detectable through long-term timing observations of the most stable pulsars. Radio observatories worldwide are currently carrying out observing programmes to detect GWs, with data sets being shared through the International Pulsar Timing Array project. One of the most likely sources of low frequency GWs are supermassive black hole binaries (SMBHBs), detectable as a background due to a large number of binaries, or as continuous or burst emission from individual sources. No GW signal has yet been detected, but stringent constraints are already being placed on galaxy evolution models. The SKA will bring this research to fruition. In this chapter, we describe how timing observations using SKA1 will contribute to detecting GWs, or can confirm a detection if a first signal already has been identified when SKA1 commences observations. We describe how SKA observations will identify the source(s) of a GW signal, search for anisotropies in the background, improve models of galaxy evolution, test theories of gravity, and characterise the early inspiral phase of a SMBHB system. We describe the impact of the large number of millisecond pulsars to be discovered by the SKA; and the observing cadence, observation durations, and instrumentation required to reach the necessary sensitivity. We describe the noise processes that will influence the achievable precision with the SKA. We assume a long-term timing programme using the SKA1-MID array and consider the implications of modifications to the current design. We describe the possible benefits from observations using SKA1-LOW. Finally, we describe GW detection prospects with SKA1 and SKA2, and end with a description of the expectations of GW astronomy.Advancing Astrophysics with the Square Kilometre Array

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“…A number of ongoing and future missions and surveys will be sensitive to SMBBHs in all stages of evolution. For instance, space VLBI and mm VLBI at the shortest wavelengths feasible will provide us with the highest spatial resolution (e.g., Fish et al 2013, Tilanus et al 2014, while the Square Kilometer Array (SKA) will provide high sensitivity (e.g., Deane et al 2015). SKA and other current and upcoming PTA (pulsar timing array) experiments will detect the gravitational wave signatures of the most massive coalescing SMBBHs using pulsar timing (e.g., Lazio 2013, Hobbs 2013, Kramer & Champion 2013, Sesana 2015.…”

Section: Future Missions and Searchesmentioning

confidence: 99%

Compact object mergers: observations of supermassive binary black holes and stellar tidal disruption events

Komossa

Zensus

2014

Proc. IAU

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Abstract. The capture and disruption of stars by supermassive black holes (SMBHs), and the formation and coalescence of binaries, are inevitable consequences of the presence of SMBHs at the cores of galaxies. Pairs of active galactic nuclei (AGN) and binary SMBHs are important stages in the evolution of galaxy mergers, and an intense search for these systems is currently ongoing. In the early and advanced stages of galaxy merging, observations of the triggering of accretion onto one or both BHs inform us about feedback processes and BH growth. Identification of the compact binary SMBHs at parsec and sub-parsec scales provides us with important constraints on the interaction processes that govern the shrinkage of the binary beyond the "final parsec". Coalescing binary SMBHs are among the most powerful sources of gravitational waves (GWs) in the universe. Stellar tidal disruption events (TDEs) appear as luminous, transient, accretion flares when part of the stellar material is accreted by the SMBH. About 30 events have been identified by multi-wavelength observations by now, and they will be detected in the thousands in future ground-based or space-based transient surveys. The study of TDEs provides us with a variety of new astrophysical tools and applications, related to fundamental physics or astrophysics. Here, we provide a review of the current status of observations of SMBH pairs and binaries, and TDEs, and discuss astrophysical implications.

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Multiple supermassive black hole systems: SKA’s future leading role

Cited by 8 publications

References 40 publications

Four Dual Agn Candidates Observed With the Vlba

Four Dual Agn Candidates Observed With the Vlba

Gravitational Wave Astronomy with the SKA

Compact object mergers: observations of supermassive binary black holes and stellar tidal disruption events

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