A Curved 150 pc Long Jet in the Double-peaked Emission-line AGN KISSR 434

Kharb, P.; Vaddi, Sravani; Sebastian, Biny; Subramanian, Smitha; Das, Mousumi; Paragi, Z.

doi:10.3847/1538-4357/aafad7

Cited by 31 publications

(33 citation statements)

References 78 publications

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“…Radio jets associated with AGN tend to have a radio spectral index of α ∼ 0.7, so lower-frequency imaging (such as C-band, which is roughly twice as sensitive as X-band for the VLBA) may help in detecting their emission. It is also possible jet precession due to a binary SMBH may result in a curved pc-scale jet morphology, as was seen in the AGN KISSR 434 (Kharb et al 2019). Multi-epoch imaging with the VLBA may be able to monitor the periodic core shifts induced by such a jet precession, or a periodic increase in luminosity as the jet swings into our line-ofsight and relativistic beaming effects become significant (as is modeled in the famous AGN OJ 287,BL Lacertae, and 3C 66B, Valtonen & Pihajoki 2013;Stirling et al 2003;Sudou et al 2003).…”

Section: The Binary Smbh Scenariomentioning

confidence: 94%

The Search for Binary Supermassive Black Holes Amongst Quasars with Offset Broad Lines Using the Very Long Baseline Array

Breiding,

Burke-Spolaor,

Eracleous

et al. 2021

Preprint

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In several previous studies, quasars exhibiting broad emission lines with 1000 km s −1 velocity offsets with respect to the host galaxy rest frame have been discovered. One leading hypothesis for the origin of these velocity-offset broad lines is the dynamics of a binary supermassive black hole (SMBH). We present high-resolution radio imaging of 34 quasars showing these velocity-offset broad lines with the Very Long Baseline Array (VLBA), aimed at finding evidence for the putative binary SMBHs (such as dual radio cores), and testing the competing physical models. We detect exactly half of the target sample from our VLBA imaging, after implementing a 5σ detection limit. While we do not resolve double radio sources in any of the targets, we obtain limits on the instantaneous projected separations of a radio-emitting binary for all of the detected sources under the assumption that a binary still exists within our VLBA angular resolution limits. We also assess the likelihood that a radio-emitting companion SMBH exists outside of our angular resolution limits, but its radio luminosity is too weak to produce a detectable signal in the VLBA data. Additionally, we compare the precise sky positions afforded by these data to optical positions from both the SDSS and Gaia DR2 source catalogs. We find projected radio/optical separations on the order of ∼10 pc for three quasars. Finally, we explore how future multi-wavelength campaigns with optical, radio, and X-ray observatories can help discriminate further between the competing physical models.

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Section: The Binary Smbh Scenariomentioning

confidence: 94%

The Search for Binary Supermassive Black Holes Amongst Quasars with Offset Broad Lines Using the Very Long Baseline Array

Breiding,

Burke-Spolaor,

Eracleous

et al. 2021

Preprint

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“…We estimated the pc-scale jet speed using the jet-to-counterjet surface brightness ratio (𝑅 J ; Ghisellini et al (1993); Kharb et al (2019)) at 2.3 GHz. In the absence of a visible counterjet, we used the 3𝜎 noise level along the counterjet (southern) direction as the limiting counterjet brightness, and subsequently obtained a lower limit to the ratio, 𝑅 J > 13.58.…”

Section: Sub-kpc and Pc-scale Jetmentioning

confidence: 99%

The peculiar WAT NGC 2329 with Seyfert/FR I-like radio lobes

Das,

Kharb,

Morganti

et al. 2021

Preprint

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We report the complex radio properties of the radio galaxy NGC 2329 that resides in the centre of the galaxy cluster Abell 569. For this study, we have used archival data from the Very Large Array (VLA) at various resolutions and frequencies, as well as the Very Long Baseline Array (VLBA). While the wide-angle tailed (WAT) Fanaroff-Riley type I (FR I) radio morphology of the source has been discussed widely in the literature, the nature of the inner lobes has not been as widely discussed. In particular, we note that the inner lobes resemble the bubble-like radio structures observed in Seyfert galaxies. Polarization-sensitive data from the VLA clearly show magnetic field structures consistent with FR Is for the outer lobes and Seyferts for the inner lobes in NGC 2329. FR Is are classified as radio-loud (RL) active galactic nuclei (AGN) and Seyferts as radio-quiet (RQ) AGN, making this source unique. The VLBA shows a onesided radio jet suggesting a relativistic pc-scale outflow, leading into the inner lobes. Electron lifetime estimates suggest that the outer FR I-like lobes are nearly twice as old (∼45 Myr) as the inner Seyfert-like lobes (∼25 Myr). Gas inflow in this merging cluster seems to have rejuvenated the AGN about ∼25 Myr ago, and may have caused a change in the accretion disc state. The complex composite radio morphology of NGC 2329 suggests that the RL/RQ dichotomy is a function of time in the lifecycle of an AGN.

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“…So the methods of the search are needed to be developed, including classification, clustering, and other mathematical methods. The previous works of double-peaked profiles dedicated to the specific objects, such as the reference [9]- [11], etc. The machine learning based on parallelized hadoop is used to identify the double-peaked profiles on H α line in the LAMOST [12].…”

Section: Related Workmentioning

confidence: 99%

SVM-Lattice: A Recognition and Evaluation Frame for Double-Peaked Profiles

Yang

Cai

et al. 2020

IEEE Access

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In big data era, the special data with rare characteristics may be of great significations. However, it is very difficult to automatically search these samples from the massive and high-dimensional datasets and systematically evaluate them. The DoPS, our previous work [1], provided a search method of rare spectra with double-peaked profiles from massive and high-dimensional data of LAMOST survey. The identification of the results is mainly depended on visually inspection by astronomers. In this paper, as a follow-up study, a new lattice structure named SVM-Lattice is designed based on SVM(Support Vector Machine) and FCL(Formal Concept Lattice) and particularly applied in the recognition and evaluation of rare spectra with double-peaked profiles. First, each node in the SVM-Lattice structure contains two components: the intents are defined by the support vectors trained by the spectral samples with the specific characteristics, and the relevant extents are all the positive samples classified by the support vectors. The hyperplanes can be extracted from every lattice node and used as classifiers to search targets by categories. A generalization and specialization relationship is expressed between the layers, and higher layers indicate higher confidence of targets. Then, including a SVM-Lattice building algorithm, a pruning algorithm based on association rules, and an evaluation algorithm, the supporting algorithms are provided and analysed. Finally, for the recognition and evaluation of spectra with double-peaked profiles, several data sets from LAMOST survey are used as experimental dataset. The results exhibit good consistency with traditional methods, more detailed and accurate evaluations of classification results, and higher searching efficiency than other similar methods. INDEX TERMS SVM-Lattice, double-peaked profiles, support vector machine, formal concept lattice.

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A Curved 150 pc Long Jet in the Double-peaked Emission-line AGN KISSR 434

Cited by 31 publications

References 78 publications

The Search for Binary Supermassive Black Holes Amongst Quasars with Offset Broad Lines Using the Very Long Baseline Array

The Search for Binary Supermassive Black Holes Amongst Quasars with Offset Broad Lines Using the Very Long Baseline Array

The peculiar WAT NGC 2329 with Seyfert/FR I-like radio lobes

SVM-Lattice: A Recognition and Evaluation Frame for Double-Peaked Profiles

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