Wise J233237.05–505643.5: A Double-Peaked, Broad-Lined Active Galactic Nucleus With a Spiral-Shaped Radio Morphology

Abstract

We present radio continuum mapping, optical imaging, and spectroscopy of the newly discovered double-peaked, broad-lined active galactic nucleus (AGN) WISE J233237.05−505643.5 at redshift z = 0.3447. This source exhibits an FR-I and FR-II hybrid morphology, characterized by a bright core, jet, and Doppler-boosted lobe structures in Australian Telescope Compact Array continuum maps at 1.5, 5.6, and 9 GHz. Unlike most FR-II objects, W2332−5056 is hosted by a disk-like galaxy. The core has a projected 5 linear radio feature that is perpendicular to the curved primary jet, hinting at unusual and complex activity within the inner 25 kpc. The multiepoch, optical-near-IR photometric measurements indicate significant variability over a 3-20 yr baseline from the AGN component. Gemini South optical data show unusual double-peaked emission-line features: the centroids of the broad-lined components of Hα and Hβ are blueshifted with respect to the narrow lines and host galaxy by ∼3800 km s −1 . We examine possible cases that involve single or double supermassive black holes in the system and discuss the required future investigations to disentangle the mysterious nature of this system.

Finding counterparts for all-sky X-ray surveys with Nway: a Bayesian algorithm for cross-matching multiple catalogues

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A systematic search for close supermassive black hole binaries in the Catalina Real-time Transient Survey

“…It should be noted, though, that there is no unique spectral characteristic signature of a SMBH binary, despite several theoretical efforts to identify one, e.g., Shen & Loeb (2010); Montuori et al (2011). Initial searches (Bogdanović et al 2008;Dotti et al 2009;Boroson & Lauer 2009) looked for double broad-line emission systems -thought to originate in gas associated with the two SMBHs, where the velocity separation between the two emission line systems traces the projected orbital velocity of the binary -or single line systems with a systematic velocity offset of the broad component from the narrow component (e.g., Tsalmantza 2011;Tsai et al 2013), under the assumption that only one SMBH is active and Keplerian rotation about this produces the shift. However, it is possible to explain such phenomena via a disk emitter model with a single SMBH rather than requiring a binary system.…”

Dual AGN Candidates with Double-peaked [O iii] Lines Matching that of Confirmed Dual AGNs

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