The Nature of Jets in Double-peaked Emission-line AGN in the KISSR Sample

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

doi:10.3847/1538-4357/ac0c82

Cited by 15 publications

(19 citation statements)

References 87 publications

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“…Based on 6 GHz VLA observations of SDSS quasi-stellar objects, Kellermann et al (2016) have ★ E-mail: vaishnavrao@iitb.ac.in suggested RQAGN to be those having 21 ≤ log[L 6 (W Hz −1 )] ≤ 23. Radio observations have revealed that most Seyferts possess subparsec or parsec-scale radio emission (e.g, de Bruyn & Wilson 1976;Ulvestad & Wilson 1984;Roy et al 1994;Thean et al 2001;Kharb et al 2021) and 40% display kpc-scale radio structures (KSRs; Gallimore et al 2006;Singh et al 2015).…”

Section: Introductionmentioning

confidence: 99%

AGN Feedback Through Multiple Jet Cycles in the Seyfert Galaxy NGC 2639

V.¹,

Kharb²,

Rubinur³

et al. 2023

Preprint

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The Seyfert galaxy NGC 2639 is known to exhibit three episodes of AGN jet/lobe activity. We present here the upgraded Giant Metrewave Radio Telescope (uGMRT) 735 MHz image of NGC 2639 showing a fourth episode as witnessed by the discovery of ∼ 9 kpc radio lobes misaligned with the previously known ∼ 1.5 kpc, ∼ 360 parsec, and ∼ 3 parsec jet features detected through the Karl G. Jansky Very Large Array (VLA) and the Very Long Baseline Array (VLBA), respectively. Using the spectral ageing software BRATS, we derive the ages of the ∼ 9 kpc, ∼ 1.5 kpc, and ∼ 360 parsec episodes to be, respectively, 34 +4 −6 Myr, 11.8 +1.7 −1.4 Myr, and 2.8 +0.7 −0.5 Myr, and conclude that minor mergers occurred 9-22 Myr apart. NGC 2639 shows a deficit of CO(1-0) molecular gas in its central ∼ 6 kpc region. The GALEX NUV image also shows a clear deficiency of recent star-formation in the same region, while the star formation rate (SFR) surface density in NGC 2639 is lower by a factor of 5 − 18 compared to the global Schmidt law of star-forming galaxies. This makes NGC 2639 a rare case of a radio-quiet AGN showing episodic jet activity and possible signatures of negative AGN feedback.

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Section: Introductionmentioning

confidence: 99%

AGN Feedback Through Multiple Jet Cycles in the Seyfert Galaxy NGC 2639

V.¹,

Kharb²,

Rubinur³

et al. 2023

Preprint

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“…3). Such double-peaks have been attributed to several different sources, such as the presence of dual AGN (Rubinur et al 2019;Maschmann et al 2020), AGN-driven outflows (Nevin et al 2018;Rakshit & Woo 2018;Kharb et al 2021) or rotating discs (Eracleous et al 2009). In our analysis, we find such double-peaks in the non-rotating spherical system, which are caused solely due to the presence of lateral outflows caused by the jet (see Fig.…”

Section: Nature Of Jet-ism Interactions and Their Spatial Extentmentioning

confidence: 49%

Modelling observable signatures of jet-ISM interaction: thermal emission and gas kinematics

Meenakshi,

Mukherjee,

Wagner

et al. 2022

Preprint

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Relativistic jets are believed to have a substantial impact on the gas dynamics and evolution of the interstellar medium (ISM) of their host galaxies. In this paper, we aim to draw a link between the simulations and the observable signatures of jet-ISM interactions by analyzing the emission morphology and gas kinematics resulting from jet-induced shocks in simulated disc and spherical systems. We find that the jet-induced laterally expanding forward shock of the energy bubble sweeping through the ISM causes large-scale outflows, creating shocked emission and high-velocity dispersion in the entire nuclear regions (∼ 2 kpcs) of their hosts. The jetted systems exhibit larger velocity widths (> 800 km s −1 ), broader Position-Velocity maps and distorted symmetry in the disc's projected velocities than systems without a jet. We also investigate the above quantities at different inclination angles of the observer with respect to the galaxy. Jets inclined to the gas disc of its host are found to be confined for longer times, and consequently couple more strongly with the disc gas. This results in prominent shocked emission and high-velocity widths, not only along the jet's path, but also in the regions perpendicular to them. Strong interaction of the jet with a gas disc can also distort its morphology. However, after the jets escape their initial confinement, the jet-disc coupling is weakened, thereby lowering the shocked emission and velocity widths.

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“…We now turn our attention to much smaller spatial scales than probed by the GMRT and VLA observations. We focus on the KPNO Internal Spectroscopic Survey Red (KISSR; [115]) sample of Seyfert and LINER galaxies [116]. This sample was chosen based on the presence of doublepeaked emission lines in their SDSS spectra as well as a radio detection in the VLA FIRST survey [117].…”

Section: Signatures Of Jet + Wind Feedback On Parsec-scalesmentioning

confidence: 99%

Looking for Signatures of AGN Feedback in Radio-Quiet AGN

Kharb

Silpa

2023

Galaxies

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In this article, we discuss the state of “AGN feedback” in radio-quiet (RQ) AGN. This study involves heterogeneous samples of nearby Seyfert and LINER galaxies as well as quasi-stellar objects (QSOs) that have been observed at low radio frequencies (few ∼100 MHz) with the upgraded Giant Meterwave Radio Telescope (GMRT) and ∼GHz frequencies with the Karl G. Jansky Very Large Array (VLA) and Very Long Baseline Array (VLBA). These multi-frequency, multi-resolution observations detect a range of arcsecond-scale radio spectral indices that are consistent with the presence of multiple contributors including starburst winds and AGN jets or winds; steep spectrum “relic” emission is observed as well. Polarization-sensitive data from the VLA and GMRT suggest that the radio outflows are stratified (e.g., in IIIZw2, Mrk231); distinct polarization signatures suggest that there could either be a “spine + sheath” structure in the radio outflow, or there could be a “jet + wind” structure. Similar nested biconical outflows can also explain the VLBA and SDSS emission-line data in the KISSR sample of double-peaked emission-line Seyfert and LINER galaxies. Furthermore, the modeling of the emission-lines with plasma modeling codes such as MAPPINGS indicates that parsec-scale jets and winds in these sources can disturb or move the narrow-line region (NLR) gas clouds via the “shock + precursor” mechanism. Apart from the presence of “relic” emission, several Seyfert and LINER galaxies show clear morphological signatures of episodic jet activity. In one such source, NGC2639, at least four distinct episodes of jets are observed, the largest one of which was only detectable at 735 MHz with the GMRT. Additionally, a ∼6 kpc hole in the CO molecular gas along with a dearth of young stars in the center of its host galaxy is observed. Multiple jet episodes on the 10–100 parsec scales and a ∼10 parsec hole in the molecular gas is also observed in the Seyfert galaxy NGC4051. This suggests a link between episodic jet activity in RQ AGN and “AGN feedback” influencing the evolution of their host galaxies. However, a similar simple relationship between radio outflows and molecular gas mass is not observed in the Palomar–Green (PG) QSO sample, indicating that “AGN feedback” is a complex phenomenon in RQ AGN. “AGN feedback” must occur through the local impact of recurring multi-component outflows in RQ AGN. However, global feedback signatures on their host galaxy properties are not always readily evident.

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The Nature of Jets in Double-peaked Emission-line AGN in the KISSR Sample

Cited by 15 publications

References 87 publications

AGN Feedback Through Multiple Jet Cycles in the Seyfert Galaxy NGC 2639

AGN Feedback Through Multiple Jet Cycles in the Seyfert Galaxy NGC 2639

Modelling observable signatures of jet-ISM interaction: thermal emission and gas kinematics

Looking for Signatures of AGN Feedback in Radio-Quiet AGN

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