The Quasar SDSS J105041.35+345631.3: Black Hole Recoil or Extreme Double-Peaked Emitter?

Shields, G. A.; Rosario, D. J.; Smith, Krista Lynne; Bonning, E. W.; Salviander, S.; Kalirai, J.; Strickler, R.; Ramírez-Ruiz, E.; Dutton, Aaron A.; Treu, Tommaso; Marshall, Phil

doi:10.1088/0004-637x/707/2/936

Cited by 75 publications

(72 citation statements)

References 27 publications

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“…For example, the sources SDSS J153636.22+044127.0 (J1536+0441, Boroson & Lauer 2009) and SDSS J105041.35+ 345631.3 (J1050+3456, Shields et al 2009b) show doublepeaked, broad Balmer emission lines (Hα, Hβ, and Hγ ), which resemble two broad-line regions (BLRs) with significant velocity differences (>2000 km s −1 ). However, these objects might instead be members of the sub-class of AGNs/quasars called "double-peaked emitters" (also known as "disk emitters") where the double peaks of the Balmer lines are attributed to emission from a single accretion disk.…”

Section: Introductionmentioning

confidence: 99%

A CANDIDATE DUAL ACTIVE GALACTIC NUCLEUS ATz= 1.175

Barrows

Stern

Madsen

et al. 2011

ApJ

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The X-ray source CXOXBJ142607.6+353351 (CXOJ1426+35), which was identified in a 172 ks Chandra image in the Boötes field, shows double-peaked rest-frame optical/UV emission lines, separated by 0. 69 (5.5 kpc) in the spatial dimension and by 690 km s −1 in the velocity dimension. The high excitation lines and emission line ratios indicate both systems are ionized by an active galactic nucleus (AGN) continuum, and the double-peaked profile resembles that of candidate dual AGNs. At a redshift of z = 1.175, this source is the highest redshift candidate dual AGN yet identified. However, many sources have similar emission line profiles for which other interpretations are favored. We have analyzed the substantial archival data available in this field as well as acquired near-infrared (NIR) adaptive optics (AO) imaging and NIR slit spectroscopy. The X-ray spectrum is hard, implying a column density of several 10 23 cm −2 . Though heavily obscured, the source is also one of the brightest in the field, with an absorption-corrected 2-10 keV luminosity of ∼10 45 erg s −1 . Outflows driven by an accretion disk may produce the double-peaked lines if the central engine accretes near the Eddington limit. However, we may be seeing the narrow line regions of two AGNs following a galactic merger. While the AO image reveals only a single source, a second AGN would easily be obscured by the significant extinction inferred from the X-ray data. Understanding the physical processes producing the complex emission line profiles seen in CXOJ1426+35 and related sources is important for interpreting the growing population of dual AGN candidates.

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Section: Introductionmentioning

confidence: 99%

A CANDIDATE DUAL ACTIVE GALACTIC NUCLEUS ATz= 1.175

Barrows

Stern

Madsen

et al. 2011

ApJ

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“…Significant additional support for this scenario comes from the growing evidence in favor of the presence of binary black hole systems within the nuclei of active galaxies. One line of evidence comes from recent discoveries of double-peaked broad low-ionization lines separated by > 2000 km s −1 (Komossa, Zhou & Lu 2008;Boroson & Lauer 2009;Shields, et al 2009); however, it must be noted that these systems could just be superpositions of two active galactic nuclei (AGN) within the same cluster of galaxies (e.g., Dotti & Ruszkowski 2009). X-ray imaging and spectroscopy indicate that both the optical nuclei (separated by a projected distance of ∼1.3 kpc) of the ultraluminous infrared galaxy NGC 6240 are active and thus house SMBHs (Komossa et al 2003).…”

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confidence: 99%

On the origin of X-shaped radio galaxies

Gopal-Krishna

Biermann

Gergely

et al. 2012

Res. Astron. Astrophys.

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After a brief, critical review of the leading explanations proposed for the small but important subset of radio galaxies showing an X-shaped morphology (XRGs) we propose a generalized model, based on the jet-shell interaction and spin-flip hypotheses. The most popular scenarios for this intriguing phenomenon invoke either hydrodynamical backflows and over-pressured cocoons or rapid jet reorientations, presumably from the spin-flips of central engines following the mergers of pairs of galaxies, each of which contains a supermassive black hole (SMBH). We confront these models with a number of key observations and thus argue that none of the models is capable of explaining the entire range of salient observational properties of XRGs, although some of the arguments raised in the literature against the spin-flip scenario are probably not tenable. We then propose here a new scenario which also involves galactic mergers but would allow the spin of the central engine to maintain its direction. Motivated by the detailed multi-band observations of the nearest radio galaxy, Centaurus A, this new model emphasizes the role of interactions between the jets and the shells of stars and gas that form and rotate around the merged galaxy and can cause temporary deflections of the jets, occasionally giving rise to an X-shaped radio structure. Although each of the models is likely to be relevant to a subset of XRGs, the bulk of the evidence indicates that most of them are best explained by the jet-shell interaction or spin-flip hypotheses.

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“…While in Ref. [62] (SDSS J105041+345631) and in Ref. [92] (SDSS J153636+044127) there is speculation that 3500 km/s recoiling black holes are responsible for these features in the spectra.…”

Section: Discussionmentioning

confidence: 95%

“…Several studies made predictions of specific observational features of recoiling supermassive black holes in the cores of galaxies in the electromagnetic spectrum [46][47][48][49][50][51][52] from infrared [53] to X-rays [54][55][56] and morphological aspects of the galaxy cores [57][58][59]. Notably, there began to appear observations indicating the possibility of detection of such effects [60][61][62], and although alternative explanations are possible [63][64][65][66], there is still the exciting possibility that these observations can lead to the first confirmation of a prediction of General Relativity in the highly-dynamical, strong-field regime.…”

Section: Introductionmentioning

confidence: 99%

Modeling maximum astrophysical gravitational recoil velocities

Lousto

Zlochower

2011

Phys. Rev. D

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We measure the recoil velocity as a function of spin for equal-mass, highly-spinning black-hole binaries, with spins in the orbital plane, equal in magnitude and opposite in direction. We confirm that the leading-order effect is linear in the spin and the cosine of angle between the spin direction and the infall direction at merger. We find higher-order corrections that are proportional to the odd powers in both the spin and cosine of this angle. Taking these corrections into account, we predict that the maximum recoil will be 3680 ± 130km s −1 .

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The Quasar SDSS J105041.35+345631.3: Black Hole Recoil or Extreme Double-Peaked Emitter?

Cited by 75 publications

References 27 publications

A CANDIDATE DUAL ACTIVE GALACTIC NUCLEUS ATz= 1.175

A CANDIDATE DUAL ACTIVE GALACTIC NUCLEUS ATz= 1.175

On the origin of X-shaped radio galaxies

Modeling maximum astrophysical gravitational recoil velocities

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