Extended soft X-ray emission in 3CR radio galaxies at<i>z</i>&lt; 0.3: high excitation and broad line galaxies

Balmaverde, B.; Capetti, A.; Grandi, P.; Torresi, E.; Chiaberge, M.; Zaurín, J. Rodríguez; Tremblay, G. R.; Axon, D. J.; Baum, Stefi A.; Giovannini, G.; Kharb, P.; Macchetto, F.; O’Dea, C. P.; Sparks, W. B.

doi:10.1051/0004-6361/201219561

Cited by 36 publications

(32 citation statements)

References 76 publications

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“…Several subsets of the 3CR sample have been also observed by other groups (e.g. Balmaverde et al 2012;Wilkes et al 2013). Here we present an update of the summary also including the 16 targets analysed in the present work (Cycle 17).…”

Section: B X-ray Observations Of the 3cr Samplesupporting

confidence: 64%

The 3CR Chandra Snapshot Survey: Extragalactic Radio Sources with Redshifts between 1 and 1.5

Stuardi

Missaglia

Massaro

et al. 2018

ApJS

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The aim of this paper is to present an analysis of newly acquired X-ray observations of 16 extragalactic radio sources, listed in the Third Cambridge Revised (3CR) catalog, and not previously observed by Chandra. Observations were performed during Chandra Cycle 17, extending X-ray coverage for the 3CR extragalactic catalog up to z=1.5. Among the 16 targets, two lie at z <0.5 (i.e., 3CR 27, at z=0.184 and 3CR 69, at z=0.458), all the remaining 14 have redshifts between 1.0 and 1.5. In the current sample there are three compact steep spectrum (CSS) sources, three quasars and an FR I radio galaxy, while the other nine are FR II radio galaxies. All radio sources have an X-ray counterpart. We measured nuclear X-ray fluxes as well as X-ray emission associated with radio jet knots, hotspots or lobes in three energy bands: soft (0.5-1 keV), medium (1-2 keV) and hard (2-7 keV). We also performed standard X-ray spectral analysis for the four brightest nuclei. We discovered X-ray emission associated with: the radio lobe of 3CR 124; a hotspot of the quasar 3CR 220.2; another hotspot of the radio galaxy 3CR 238; and the jet knot of 3CR 297. We also detected extended X-ray emission around the nuclear region of 3CR 124 and 3CR 297 on scales of several tens of kpc. Finally, we present an update on the X-ray observations performed with Chandra and XMM-Newton on the entire 3CR extragalactic catalog.

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Section: B X-ray Observations Of the 3cr Samplesupporting

confidence: 64%

The 3CR Chandra Snapshot Survey: Extragalactic Radio Sources with Redshifts between 1 and 1.5

Stuardi

Missaglia

Massaro

et al. 2018

ApJS

Self Cite

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“…The mean unabsorbed normalization at 1 keV is 8% of the absorbed one. In addition to the second power-law, a MEKAL model is required in a few objects: in some cases, this component is directly related to collisional gas emission (cluster or shocked gas), in the other ones it could mimic photoionized features (Balmaverde et al 2012). Indeed, in two radio galaxies, i.e.…”

Section: Resultsmentioning

confidence: 99%

Radio morphology–accretion mode link in Fanaroff–Riley type II low-excitation radio galaxies

Macconi

Torresi²,

Grandi³

et al. 2020

Monthly Notices of the Royal Astronomical Society

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Fanaroff-Riley II low-excitation radio galaxies (FRII-LERGs) are characterized by weak nuclear excitation on pc-scales and by properties typical of powerful FRIIs (defined as high-excitation, hereafter HERGs/BLRGs) on kp-scales. Since a link between the accretion properties and the power of the produced jets is expected both from theory and observations, their nature is still debated. In this work we investigate the X-ray properties of a complete sample of 19 FRII-LERGs belonging to the 3CR catalog, exploiting Chandra and XMM-Newton archival data. We also analyze 32 FRII-HERGs/BLRGs with Chandra data as a control sample. We compared FRII-LERG and FRII-HERG/BLRG X-ray properties and optical data available in literature to obtain a wide outlook of their behavior. The low accretion rate estimates for FRII-LERGs, from both X-ray and optical bands, allow us to firmly reject the hypothesis for that they are the highly obscured counterpart of powerful FRII-HERGs/BLRGs. Therefore, at least two hypothesis can be invoked to explain the FRII-LERGs nature: (i) they are evolving from classical FRIIs because of the depletion of accreting cold gas in the nuclear region, while the extended radio emission is the heritage of a past efficiently accreting activity; (ii) they are an intrinsically distinct class of objects with respect to classical FRIs/FRIIs. Surprisingly, in this direction a correlation between accretion rates and environmental richness is found in our sample. The richer the environment, the more inefficient is the accretion. In this framework, the FRII-LERGs are intermediate between FRIs and FRII-HERGs/BLRGs both in terms of accretion rate and environment.

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“…In some objects, for example, a spatial correspondence between the extended soft X-ray emission and the [O iii]λ5007 emission was observed (e.g. Young et al 2001, Bianchi et al 2006, Wang et al 2011and Balmaverde et al 2012. The most probable scenario for cases like these establishes that the extended X-ray emission comes from gas in the NLR photoionized by the central AGN.…”

Section: The Double Stellar Nucleus and The Agnmentioning

confidence: 99%

The nuclear region of NGC 613 – I. Multiwavelength analysis

Silva

Menezes

Steiner

2020

Monthly Notices of the Royal Astronomical Society

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In this paper, we report a detailed study with a variety of data from optical, nearinfrared, X-ray, and radio telescopes of the nuclear region of the galaxy NGC 613 with the aim of understanding its complexity. We detected an extended stellar emission in the nucleus that, at first, appears to be, in the optical band, two stellar nuclei separated by a stream of dust. The active galactic nucleus (AGN) is identified as a variable point-like source between these two stellar components. There is a central hard X-ray emission and an extended soft X-ray emission that closely coincides with the ionization cone, as seen in the [O iii]λ5007 emission. The centroid of the [O i]λ6300 emission does not coincide with the AGN, being shifted by 0.24 arcsec towards the ionization cone; this shift is probably caused by a combination of differential dust extinction together with emission and reflection in the ionization cone. The optical spectra extracted from the central region are typical of low-ionization nuclear emission-line regions. We also identify 10 H ii regions, eight of them in a star forming ring that is visible in Brγ, [Fe ii]λ16436 and molecular CO(3-2) images observed in previous studies. Such a ring also presents weak hard X-ray emission, probably associated with supernova remnants, not detected in other studies. The position of the AGN coincides with the centre of a nuclear spiral (detected in previous works) that brings gas and dust from the bar to the nucleus, causing the high extinction in this area.

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Extended soft X-ray emission in 3CR radio galaxies atz< 0.3: high excitation and broad line galaxies

Cited by 36 publications

References 76 publications

The 3CR Chandra Snapshot Survey: Extragalactic Radio Sources with Redshifts between 1 and 1.5

The 3CR Chandra Snapshot Survey: Extragalactic Radio Sources with Redshifts between 1 and 1.5

Radio morphology–accretion mode link in Fanaroff–Riley type II low-excitation radio galaxies

The nuclear region of NGC 613 – I. Multiwavelength analysis

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