High-resolution spectroscopy of the extended narrow-line region of IC 5063 and NGC 7212

Congiu, Enrico; Contini, M.; Ciroi, S.; Cracco, V.; Berton, M.; Mille, F. Di; Frezzato, Michele; Mura, G. La; Rafanelli, P.

doi:10.1093/mnras/stx1628

Cited by 30 publications

(44 citation statements)

References 58 publications

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“…Breaking the observed emission into discrete energy bands and cone/cross-cone regions, we find significant, up to 3.6 kpc, extended emission at 1% of the surface brightness. This extended emission is strongly associated with soft X-rays in the south−north cone direction (accounting for more than 14% of the total counts), and is consistent with the observed ENLR region (e.g., Cracco et al 2011;Congiu et al 2017) and compact double radio source (e.g., Tran 1995a,b;Falcke et al 1998).…”

Section: Discussionsupporting

confidence: 82%

“…Optical ground-based observations and emission line diagnostics (e.g., BPT diagrams; Baldwin et al 1981), from Congiu et al (2017) (see also Contini et al 2012) suggest that the ionization mechanism for NGC 7212 is a combination of photoionization and shocks, which is qualitatively consistent with our results. Recently, Terao et al (2016) suggests that NGC 7212 is not likely affected by fast shocks based on near-IR observations.…”

Section: Physical Modelssupporting

confidence: 90%

“…We find a thermal component in the 1.5 − 8.0 annular region with kT ∼ 7.0 keV (∼10 8 K) that is not found in the 1.5 nuclear region which may indicate the presence of one of these hot cocoons. Further evidence supporting jet-ISM interactions in NGC 7212 is reported by Congiu et al (2017). However, we cannot rule out supernova heating in the 1.5 nuclear region or the 1.5 − 8.0 annular region.…”

Section: Radial Profiles and Fwhmmentioning

confidence: 52%

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Chandra Observations of NGC 7212: Large-scale Extended Hard X-Ray Emission

Jones

Fabbiano

Elvis

et al. 2020

ApJ

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Recent observations of nearby Compton thick (CT) active galactic nuclei (AGNs) with Chandra have resolved hard (> 3 keV) X-ray emission extending out from the central supermassive black hole to kiloparsec scales, challenging the long-held belief that the characteristic hard X-ray continuum and fluorescent Fe K lines originate in the inner ∼parsec due to the excitation of obscuring material. In this paper we present the results of the most recent Chandra ACIS-S observations of NGC 7212, a CT AGN in a compact group of interacting galaxies, with a total effective exposure of ∼150 ks. We find ∼20% of the observed emission is found outside of the central kiloparsec, with ∼17% associated with the soft X-rays, and ∼3% with hard X-ray continuum and Fe K line. This emission is extended both along the ionization cone and in the cross-cone direction up to ∼3.8 kpc scales. The spectrum of NGC 7212 is best represented by a mixture of thermal and photoionization models that indicate the presence of complex gas interactions. These observations are consistent with what is observed in other CT AGN (e.g., ESO 428−G014, NGC 1068), providing further evidence that this may be a common phenomenon. High-resolution observations of extended CT AGN provide an especially valuable environment for understanding how AGN feedback impacts host galaxies on galactic scales.

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Section: Discussionsupporting

confidence: 82%

Section: Physical Modelssupporting

confidence: 90%

Section: Radial Profiles and Fwhmmentioning

confidence: 52%

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Chandra Observations of NGC 7212: Large-scale Extended Hard X-Ray Emission

Jones

Fabbiano

Elvis

et al. 2020

ApJ

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“…In the future our aim is to increase the size of the sample, in order to have a better statistic. Furthermore, we will investigate the relation between the X-ray complexity and other potential inclination indicators, such as the [O III] line position ( [15], [3]) and ionization cones (e.g., [17], [6] and references therein), and other physical parameters of AGN such as Eddington ratio and large scale environment [11].…”

Section: Discussion and Future Workmentioning

confidence: 99%

The link between X-ray complexity and optical lines in NLS1s

Vietri¹,

Berton²,

Ciroi³

et al. 2018

Proceedings of Revisiting Narrow-Line Seyfert 1 Galaxies and Their Place in the Universe — PoS(NLS1-2018)

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Narrow-line Seyfert 1 galaxies (NLS1s) are a subclass of active galactic nuclei (AGN). It is often believed that these AGN have small black hole mass, which is responsible for the narrowness of the permitted lines. They are also characterised by a high accretion rate, typically closer to the Eddington limit. Nevertheless, narrow permitted lines might also be caused by a disk-like broadline region (BLR) viewed pole-on. This class of objects presents strong X-ray emission, which is characterised by a very steep spectral index described by a single power law. In particular, some of them exhibit particular features around the iron K-shell energy at 6-8 keV. Recently, this different spectral behaviour was attributed to inclination. In this work we are going to analyse optical spectra to measure in different ways the width of Hβ , which is another potential inclination indicator. Our aim is to search for a correlation between the high-energy spectral complexity and FWHM of Hβ , in order to verify whether or not the broad-line region could be flattened.

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“…However, the main focus of these studies were to investigate AGN activity in at the core of this galaxy and its impact on the galaxy environemnt in general and ISM in particular. Further, a large attempt were made to explore the AGN jets and outflows [12] [13] [14]. The origin of dust in ETGs is one of the long debated issue.…”

Section: Introductionmentioning

confidence: 99%

Multiphase ISM in Nearby Early Type Galaxy IC 5063

Tate¹,

Kyadampure²,

Pandey³

et al. 2018

IJAA

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A multiwavelength study of a nearby dust lane early-type galaxy IC 5063 is presented. The objectives are to investigate dust extinction properties and the association of interstellar dust with other phases of ISM. The color-index maps as well as the extinction maps derived from the analysis of deep CCD observations in optical passbands revealed a prominent dust lane along its optical major axis in the inner region. In addition, two more fainter and extended dust patterns are apparent in the color index map as well as extinction maps. These features are also evident in the smooth model subtracted residual maps. The extinction curve derived for this galaxy revealed that dust grains in it are identical to the canonical grains in the Milky Way with the dust grains little larger than the canonical grains. The total extinction measured in the V band extinction map enabled us to quantify the dust content of this galaxy to be equal to 4 4.9 10 M ×  , an order of magnitude shorter than that estimated using the IRAS flux densities at 60 and 100 μm. A Multiphase ISM study revealed a surprising similarity in the morphologies of the H α emitting ionized gas distribution and X-ray emitting gas. Systematic analysis of high resolution X-ray observations using Chandra telescope enabled us to detect 18 discrete X-ray sources within optical D 25 region of IC 5063, out of which 17 sources were separated out as the low mass X-ray binaries and one as the high mass X-ray binary source in the X-ray color-color plot.

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High-resolution spectroscopy of the extended narrow-line region of IC 5063 and NGC 7212

Cited by 30 publications

References 58 publications

Chandra Observations of NGC 7212: Large-scale Extended Hard X-Ray Emission

Chandra Observations of NGC 7212: Large-scale Extended Hard X-Ray Emission

The link between X-ray complexity and optical lines in NLS1s

Multiphase ISM in Nearby Early Type Galaxy IC 5063

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