Fossil shell emission in dying radio loud AGNs

Kino, Motoki; Ito, Hirotaka; Kawakatu, Nozomu; Orienti, M.; Nagai, Hiroshi; Wajima, Kiyoaki; Itoh, R.

doi:10.1002/asna.201512263

Cited by 5 publications

(4 citation statements)

References 28 publications

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“…Similar trends are seen in the gamma-ray band [216]. For gamma rays, inverse-Compton emission in the TeV band is predicted to be detectable for shocked shells surrounding the remnant lobes of 3C 84 [217]. If such a detection comes into fruition, this will enable study of high energy physics in remnants for the first time.…”

Section: Multi-wavelength Observationssupporting

confidence: 52%

The Dynamics and Energetics of Remnant and Restarting RLAGN

Mahatma

2023

Galaxies

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In this article, I review past, current, and future advances on the study of radio-loud AGN (RLAGN; radio-loud quasars and radio galaxies) lifecycles exclusively in the remnant and restarting phases. I focus on their dynamics and energetics as inferred from radio observations while discussing their radiative lifetimes, population statistics, and trends in their physical characteristics. I briefly summarise multi-wavelength observations, particularly X-rays, that have enabled studies of the large-scale environments of RLAGN in order to understand their role in feedback. Furthermore, I discuss analytic and numerical simulations that predict key properties of remnant and restarting sources as found in wide-area surveys, and discuss the prospects of future surveys that may shed further light on these elusive subpopulations of RLAGN.

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Section: Multi-wavelength Observationssupporting

confidence: 52%

The Dynamics and Energetics of Remnant and Restarting RLAGN

Mahatma

2023

Galaxies

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“…First, let us begin with an estimate the size of NLR (R NLR ) for NGC 1275. The L Hβ luminosity is estimated by the luminosity of the Hα and Hβ emission line luminosities has the empirical relation of 3L Hβ ≈ L Hα ( Figure 5 in Greene and Ho 2005) and we have L Hα ∼ 1 × 10 42 erg s −1 in NGC 1275 by KANATA observation (Yamazaki et al 2013;Kino et al 2016). Therefore, the size of NRL in NGC 1275 can be estimated as R NLR ≈ 0.6 × 10 2 pc L where the filling factor of the NRL, and the number density of electrons are ǫ fill , and n, respectively.…”

Section: A Cloud In Narrow Line Region?mentioning

confidence: 60%

Evidence of Jet–Clump Interaction: A Flip of the Radio Jet Head of 3C 84

Kino

Wajima

Kawakatu

et al. 2018

ApJ

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Radio jets in active galaxies have been expected to interact with circumnuclear environments in their early phase evolutions. By performing the multi-epoch monitoring observation with the KVN and VERA Array (KaVA) at 43 GHz, we investigate the kinematics of the notable newborn bright component C3 located at the tip of the recurrent jet of 3C 84. During 2015 August-September, we discover the flip of C3 and the amount of the flip is about 0.4 milli-arcsecond in angular scale, which corresponds to 0.14 parsec in physical scale. After the flip of C3, it wobbled at the same location for a few months and then it restarted to propagate towards the southern direction. The flux density of C3 coherently showed the monotonic increase during the observation period. The flip is in good agreement with hydrodynamical simulations of jets in clumpy ambient medium. We estimate the number density of the putative clump based on the momentum balance between the jet thrust and the ram pressure from the clump and it is about 10 3−5 cm −3 . We briefly discuss possible origins of the clump.

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“…Such an origin has been suggested to ex-plain the diffuse 6.4 keV line at the Galactic center (Nobukawa et al 2015). At the central region of NGC 1275, cosmic-ray protons could be enhanced by jet-induced shock acceleration (Kino et al 2016). By assuming a proton energy spectrum with an index of −2.5 and an energy density of 20 eV cm −3 in 0.1-1000 MeV, Nobukawa et al (2015) estimated the intensity of proton-induced Fe-Kα line to be I 6.4keV = 6.6 × 10 35 NH/10 24 cm −2 Up/20 eV cm −3 S/1 pc 2 erg s −1 .…”

Section: Consideration Of Multi-wavelength Resultsmentioning

confidence: 93%

Hitomi Observation of Radio Galaxy NGC 1275: The First X-ray Microcalorimeter Spectroscopy of Fe-Kα Line Emission from an Active Galactic Nucleus

Aharonian,

Akamatsu,

Akimoto

et al. 2017

Preprint

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The origin of the narrow Fe-Kα fluorescence line at 6.4 keV from active galactic nuclei has long been under debate; some of the possible sites are the outer accretion disk, the broad line region, a molecular torus, or interstellar/intracluster media. In February-March 2016, we performed the first X-ray microcalorimeter spectroscopy with the Soft X-ray Spectrometer (SXS) onboard the Hitomi satellite of the Fanaroff-Riley type I radio galaxy NGC 1275 at the center of the Perseus cluster of galaxies. With the high energy resolution of ∼ 5 eV at 6 keV achieved by Hitomi/SXS, we detected the Fe-Kα line with ∼ 5.4 σ significance. The velocity width is constrained to be 500-1600 km s −1 (FWHM for Gaussian models) at 90% confidence. The SXS also constrains the continuum level from the NGC 1275 nucleus up to ∼ 20 keV, giving an equivalent width ∼ 20 eV of the 6.4 keV line. Because the velocity width is narrower than that of broad Hα line of ∼ 2750 km s −1 , we can exclude a large contribution to the line flux from the accretion disk and the broad line region. Furthermore, we performed pixel map analyses on the Hitomi/SXS data and image analyses on the Chandra archival data, and revealed that the Fe-Kα line comes from a region within ∼ 1.6 kpc from the NGC 1275 core, where an active galactic nucleus emission dominates, rather than that from intracluster media. Therefore, we suggest that the source of the Fe-Kα line from NGC 1275 is likely a low-covering fraction molecular torus or a rotating molecular disk which probably extends from a pc to hundreds pc scale in the active galactic nucleus system.

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Fossil shell emission in dying radio loud AGNs

Cited by 5 publications

References 28 publications

The Dynamics and Energetics of Remnant and Restarting RLAGN

The Dynamics and Energetics of Remnant and Restarting RLAGN

Evidence of Jet–Clump Interaction: A Flip of the Radio Jet Head of 3C 84

Hitomi Observation of Radio Galaxy NGC 1275: The First X-ray Microcalorimeter Spectroscopy of Fe-Kα Line Emission from an Active Galactic Nucleus

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