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

Yang, Xiaolong; Ling, Xiang; Yang, Jun; Mi, L. G.; Cui, Lang; An, Tao; Hong, Xiaoyu; Ho, Luis C.

doi:10.1093/mnras/stx1743

Cited by 7 publications

(4 citation statements)

References 54 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…In PKS1155+251, the components appear to be moving inwards resulting in the source shrinking in size (Tremblay et al, 2008). Yang et al (2017) observed the source with the VLBA at 24 and 43 GHz and suggested that the southern component may harbour another black hole. Further observations are required to clarify the nature of this source.…”

Section: Proper Motionmentioning

confidence: 99%

Compact steep-spectrum and peaked-spectrum radio sources

O'Dea,

Saikia

2020

Preprint

View full text Add to dashboard Cite

Compact steep-spectrum (CSS) and peaked spectrum (PS) radio sources are compact, powerful radio sources. The multi-frequency observational properties and current theories are reviewed with emphasis on developments since the earlier review of O'Dea (1998). There are three main hypotheses for the nature of PS and CSS sources. (1) The PS sources might be very young radio galaxies which will evolve into CSS sources on their way to becoming large radio galaxies. (2) The PS and CSS sources might be compact because they are confined (and enhanced in radio power) by interaction with dense gas in their environments. (3) Alternately, the PS sources might be transient or intermittent sources. Each of these hypotheses may apply to individual objects. The relative number in each population will have significant implications for the radio galaxy paradigm. Proper motion studies over long time baselines have helped determine hotspot speeds for over three dozen sources and establish that these are young objects. Multifrequency polarization observations have demonstrated that many CSS/PS sources are embedded in a dense interstellar medium and vigorously interacting with it. The detection of emission line gas aligned with the radio source, and blue-shifted HI absorption and [OIII] emission lines indicates that AGN feedback is present in these objects -possibly driven by the radio source. CSS/PS sources with evidence of episodic AGN over a large range of time-scales have been discussed. The review closes with a discussion of open questions and prospects for the future.

show abstract

Section: Proper Motionmentioning

confidence: 99%

Compact steep-spectrum and peaked-spectrum radio sources

O'Dea,

Saikia

2020

Preprint

View full text Add to dashboard Cite

show abstract

“…Such an extension is unusual but not unprecedented among CSOs. For example, the quasar PKS 1155+251 (Yang et al 2017) shows a similar feature, where the steep-spectrum trail emission extends to a distance of ∼ 90 pc. A possible explanation is the brightening of the hot spot in a transverse direction within the lobe due to pressure differences at the location of the jet-ISM interaction.…”

Section: Eastern Extensionmentioning

confidence: 96%

J1110+4817 -- a compact symmetric object candidate revisited

Krezinger,

Frey,

et al. 2020

Preprint

View full text Add to dashboard Cite

Compact symmetric objects (CSOs) are radio-emitting active galactic nuclei (AGNs) typically with a double-lobed radio structure confined to within 1 kpc. CSOs represent the earliest evolutionary phase of jetted AGNs. Some of them may eventually evolve into large-scale extended double sources, while others stall within the host galaxy and die out, depending on the longevity of nuclear activity, the jet power, and parameters of the surrounding galactic environment. Studying CSOs is a useful tool for understanding the evolution of the galaxies and the interactions between the jets and the medium of the host galaxy. Based on milliarcsecresolution imaging observations using very long baseline interferometry (VLBI), it is not always straightforward to distinguish between a compact double-lobed or a core-jet structure. The quasar J1110+4817 was considered a CSO candidate in the literature earlier, but because of the lack of clear evidence, it could not be securely classified as a CSO. Here we present a comprehensive analysis of archival multi-frequency VLBI observations combined with accurate Gaia optical astrometric information. Lower-frequency VLBI images reveal an extended radio feature nearly perpendicular to the main structural axis of the source, apparently emanating from the brighter northern feature, that is rare among the known CSOs. While the presence of a binary AGN system cannot be fully excluded, the most plausible explanation is that J1110+4817 is a CSO.

show abstract

“…Temporal variability, double-peaked emission lines, and helical jet structures have all been used to identify BBH candidates. Direct imaging of parsec-or subparsec-scale separated BBHs has been carried out by Very Long Baseline Interferometry (VLBI) techniques (e.g., Rodriguez et al 2006;Deane et al 2014;Kharb et al 2017;Yang et al 2017;Kharb et al 2020). Multiple direct and indirect observational techniques throughout the whole electromagnetic spectrum have been used to confirm two supermassive black holes (SMBHs) in any given binary system (see De Rosa et al 2019 for a review).…”

Section: Introductionmentioning

confidence: 99%

A Relook at the Black Hole Binary Candidate J1328+2752 with VLBI

Nandi,

Kharb,

Caproni

et al. 2024

ApJ

View full text Add to dashboard Cite

We present multiband follow-up observations of the supermassive binary black hole (BBH) candidate and misaligned double–double radio galaxy, J1328+2752. To investigate its parsec-scale structure, we have carried out observations with the Very Long Baseline Array (VLBA) and the European Very Long Baseline Interferometry (VLBI) Network. Additionally, we have obtained optical spectroscopic observations with the 3.6 m Devasthal Optical Telescope. Within 3.5 yr of our previous VLBI observations, the central parsec-scale radio structure of J1328+2752 has changed from a double component to a single central component and its flux density has increased by a factor of 3 in the 5 GHz VLBA observations. The new radio component is largely unresolved at 3, 5, and 8 GHz. The multifrequency radio data shows a convex-shaped spectrum for this unresolved component. The turnover frequency is at ∼3 GHz. While the total intensity image does not reveal any details, a super-resolved VLBA 5 and 8 GHz spectral index image does indicate the presence of two components at a separation of ∼4.2 pc with spectral indices −0.5 ± 0.3 and −0.9 ± 0.3. We have not observed a simultaneous change in the optical line profiles or intensities over the past few years. The radio structure, the variation of the flux density, and spectral shape can potentially be consistent both with the signature of a young radio source or a BBH at the center of J1328+2752.

show abstract

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

Cited by 7 publications

References 54 publications

Compact steep-spectrum and peaked-spectrum radio sources

Compact steep-spectrum and peaked-spectrum radio sources

J1110+4817 -- a compact symmetric object candidate revisited

A Relook at the Black Hole Binary Candidate J1328+2752 with VLBI

Contact Info

Product

Resources

About