Breaking All the Rules: The Compact Symmetric Object 0402+379

Maness, H.; Taylor, G. B.; Zavala, R. T.; Peck, A. B.; Pollack, L. K.

doi:10.1086/380919

Cited by 67 publications

(98 citation statements)

References 23 publications

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“…In some other cases H I is located in front of the lobe brighter and closer to the nucleus, as in 3C49, 3C268.3 (Labiano et al 2006), and possibly 0402+379 (Maness et al 2004). This supports the idea that radio lobe asymmetries may be indeed due to jet-cloud interactions (Sect.…”

Section: Wwwan-journalorgmentioning

confidence: 93%

Radio properties of CSSs and GPSs

Fanti¹

2009

Astron Nachr

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Section: Wwwan-journalorgmentioning

confidence: 93%

Radio properties of CSSs and GPSs

Fanti¹

2009

Astron Nachr

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“…However, evidence for such systems is elusive and confirmed cases are rare despite circumstantial evidence. Examples can be found in Kochanek et al (1999), Junkkarinen et al (2001), Ballo et al (2004), Maness et al (2004), Guainazzi et al (2005), Rodriguez et al (2006), Hudson et al (2006), Barth et al (2008). The best-known examples of dual AGNs are found in NGC 6240 (Komossa et al 2003), EGSD2 J142033+525917 (Gerke et al 2007), EGSD2 J141550+520929 (Comerford et al 2009a), the z = 0.36 galaxy COSMOS J100043+020637 (Comerford et al 2009b).…”

Section: Introductionmentioning

confidence: 99%

ERRATUM: “ACTIVE GALACTIC NUCLEI WITH DOUBLE-PEAKED NARROW LINES: ARE THEY DUAL ACTIVE GALACTIC NUCLEI?” (2009, ApJ, 705, L76)

Wang

Chen

et al. 2009

ApJ

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Double-peaked [O III] profiles in active galactic nuclei (AGNs) may provide evidence for the existence of dual AGNs, but a good diagnostic for selecting them is currently lacking. Starting from ∼ 7000 active galaxies in SDSS DR7, we assemble a sample of 87 type 2 AGNs with double-peaked [O III] profiles. The nuclear obscuration in the type 2 AGNs allows us to determine redshifts of host galaxies through stellar absorption lines. We typically find that one peak is redshifted and another is blueshifted relative to the host galaxy. We find a strong correlation between the ratios of the shifts and the double peak fluxes. The correlation can be naturally explained by the Keplerian relation predicted by models of co-rotating dual AGNs. The current sample statistically favors that most of the [O III] double-peaked sources are dual AGNs and disfavors other explanations, such as rotating disk and outflows. These dual AGNs have a separation distance at ∼ 1 kpc scale, showing an intermediate phase of merging systems. The appearance of dual AGNs is about ∼ 10 −2 , impacting on the current observational deficit of binary supermassive black holes with a probability of ∼ 10 −4 (Boroson & Lauer).

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“…Maness et al (2004) performed spectral line observations of 0402+379 at 1.348 GHz. H i absorption at a redshift of 560 km s −1 from the systemic velocity of the source (16,489 ± 300 km s −1 ; Xu et al 1994) was observed and attributed to a high velocity gas system, possibly due to a merger.…”

Section: Introductionmentioning

confidence: 99%

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

Rodriguez

Taylor

Zavala

et al. 2009

ApJ

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We have recently discovered a supermassive binary black hole system with a projected separation between the two black holes of 7.3 pc in the radio galaxy 0402+379 (Rodriguez et al. 2006). This is the most compact supermassive binary black hole pair yet imaged by more than two orders of magnitude. We present Global VLBI observations at 1.3464 GHz of this radio galaxy, taken to improve the quality of the H i data. Two absorption lines are found toward the southern jet of the source, one redshifted by 370 ± 10 km s −1 and the other blueshifted by 700 ± 10 km s −1 with respect to the systemic velocity of the source, which, along with the results obtained for the opacity distribution over the source, suggests the presence of two mass clumps rotating around the central region of the source. We propose a model consisting of a geometrically thick disk, of which we only see a couple of clumps, that reproduces the velocities measured from the H i absorption profiles. These clumps rotate in circular Keplerian orbits around an axis that crosses one of the supermassive black holes of the binary system in 0402+379. We find an upper limit for the inclination angle of the twin jets of the source to the line of sight of θ = 66 • , which, according to the proposed model, implies a lower limit on the central mass of ∼ 7 × 10 8 M and a lower limit for the scale height of the thick disk of ∼ 12 pc.

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Breaking All the Rules: The Compact Symmetric Object 0402+379

Cited by 67 publications

References 23 publications

Radio properties of CSSs and GPSs

Radio properties of CSSs and GPSs

ERRATUM: “ACTIVE GALACTIC NUCLEI WITH DOUBLE-PEAKED NARROW LINES: ARE THEY DUAL ACTIVE GALACTIC NUCLEI?” (2009, ApJ, 705, L76)

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

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