The spatial extension of extended narrow line regions in MaNGA AGN

Chen, Jianhang; Shi, Yong; Dempsey, Ross; Law, David R.; Chen, Yanmei; Yan, Renbin; Bing, L.; Rembold, Sandro Barboza; Li, Songlin; Yu, Xiaoling; Riffel, Rogemar A.; Brownstein, Joe R.; Riffel, Rogério

doi:10.1093/mnras/stz2183

Cited by 34 publications

(31 citation statements)

References 102 publications

(185 reference statements)

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“…10 displays the r KDR,c against the r NLR,c . The average < r NLR,c > is 3.00 ± 0.33 kpc and individual values range between 0.4 and 10.1 kpc, which are in good agreement with previous values obtained for MaNGA AGN based on spatially resolved BPT diagrams (Chen et al 2019). The KDRs present extents of: < r KDR,c >= 0.96 ± 0.09 kpc, varying between 0.2 and 2.3 kpc.…”

Section: Comparison Between the Nlr And Kdr Extentssupporting

confidence: 90%

“…The extent of the NLR correlates with the AGN luminosity and ranges from a few hundred parsecs in low luminosity AGN (e.g. Fraquelli et al 2003;Schmitt et al 2003;do Nascimento et al 2019;Chen et al 2019) to tens of kpc in the most luminous objects (e.g. Bennert et al 2002;Greene et al 2011;Liu et al 2013bLiu et al , 2014Storchi-Bergmann et al 2018).…”

Section: Estimates Of the Nlr And Kdr Extentsmentioning

confidence: 99%

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Ionised Gas Kinematics in MaNGA AGN. Extents of the Narrow Line and Kinematically Disturbed regions

Deconto-Machado,

Riffel,

Ilha

et al. 2022

Preprint

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Context. Feedback from active galactic nuclei (AGN) in general seems to play an important role in the evolution of galaxies, although the impact of AGN winds on their host galaxies is still pending on detailed analysis. Aims. We analyse the kinematics of a sample of 170 AGN host galaxies as compared to those of a matched control sample of nonactive galaxies from the MaNGA survey in order to characterise and estimate the extents of the Narrow Line Region (NLR) and of the kinematically disturbed region (KDR) by the AGN. Methods. We define the observed NLR radius (r NLR,o ) as the farthest distance from the nucleus within which both [O iii]/Hβ and [N ii]/Hα ratios fall in the AGN region of the BPT diagram and the Hα equivalent width is required to be larger than 3.0 Å. The extent of the KDR (r KDR,o ) is defined as the distance from the nucleus within which the AGN hosts galaxies shows a more disturbed gas kinematics than the control galaxies. Results. The AGN [O iii]λ5007 luminosity ranges from 10 39 to 10 41 erg s −1 , and the kinematics derived from the [O iii] line profiles reveal that, on average, the most luminous AGN (L[O iii] > 3.8 × 10 40 erg s −1 ) possess higher residual difference between the gaseous and stellar velocities and velocities dispersion than their control galaxies in all the radial bins. Spatially resolved NLR's and KDR's were found in 55 and 46 AGN host galaxies, with corrected radii 0.2 < r KDR,c < 2.3 kpc and 0.4 < r NLR,c < 10.1 kpc, with a relation between the two given by log r KDR,c = (0.53 ± 0.12) log r NLR,c + (1.07 ± 0.22), respectively. On average, the extension of the KDR corresponds to about 30 per cent of that of the NLR. Assuming that the KDR is due to an AGN outflow, we have estimated ionised gas mass outflow rates that range between 10 −5 and ∼ 1 M yr −1 , and kinetic powers that range from 10 34 to 10 40 erg s −1 . Conclusions. Comparing the power of the AGN ionised outflows with the AGN luminosities, they are always below the 0.05 L AGN model threshold for having a an important feedback effect on their respective host galaxies. The mass outflow rates (and power) of our AGN sample correlate with their luminosities, populating the lowest AGN luminosity range of the correlations previously found for more powerful sources.

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Section: Comparison Between the Nlr And Kdr Extentssupporting

confidence: 90%

Section: Estimates Of the Nlr And Kdr Extentsmentioning

confidence: 99%

Ionised Gas Kinematics in MaNGA AGN. Extents of the Narrow Line and Kinematically Disturbed regions

Deconto-Machado,

Riffel,

Ilha

et al. 2022

Preprint

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“…The bottom panel shows a positive trend, albeit with a large spread, between the size and the luminosity of the ELRs. The distribution of the sources in this plane could be consistent with the behavior expected from photoionization of a central source (i.e., r ∝ L 0.5 Ext ), as already found in Seyfert galaxies and QSOs (e.g., Bennert et al 2002;Husemann et al 2014;Sun et al 2018;Chen et al 2019).…”

Section: Luminosities and Sizes Of The Elrsupporting

confidence: 85%

The MURALES survey

Balmaverde

Capetti

Marconi

et al. 2020

A&A

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We present the final observations of a complete sample of 37 radio galaxies from the Third Cambridge Catalogue (3C) with redshift < 0.3 and declination < 20° obtained with the VLT/MUSE optical integral field spectrograph. These data were obtained as part of the MUse RAdio Loud Emission line Snapshot (MURALES) survey with the main goal of exploring the AGN feedback process in the most powerful radio sources. We present the data analysis and, for each source, the resulting emission line images and the 2D gas velocity field. Thanks to the unprecedented depth these observations reveal emission line regions (ELRs) extending several tens of kiloparsec in most objects. The gas velocity shows ordered rotation in 25 galaxies, but in several sources it is highly complex. We find that the 3C sources show a connection between radio morphology and emission line properties. In the ten FR I sources the line emission region is generally compact, only a few kpc in size; only in one case does it exceed the size of the host. Conversely, all but two of the FR II galaxies show large-scale structures of ionized gas. The median extent is 16 kpc with the maximum reaching a size of ∼80 kpc. There are no apparent differences in extent or strength between the ELR properties of the FR II sources of high and low gas excitation. We confirm that the previous optical identification of 3C 258 is incorrect: this radio source is likely associated with a quasi-stellar object at z ∼ 1.54.

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“…2b and Methods section ‘The host galaxies of the QPEs’). This in turn suggests that the two galaxies reported here have not been active for approximately at least the last 10 3 –10 4 years, assuming narrow-line region light-travel timescales 19 . Although the number of known QPEs is too low to reach firm statistical conclusions, our blind search is inherently designed to sample the population of the QPEs’ host galaxies without bias, as opposed to serendipitous or archival discoveries, which rely on the source being previously active and known 1 , 2 .…”

Section: Mainmentioning

confidence: 61%

X-ray quasi-periodic eruptions from two previously quiescent galaxies

Arcodia

Merloni

Nandra

et al. 2021

Nature

116

171

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Quasi-periodic eruptions (QPEs) are very-high-amplitude bursts of X-ray radiation recurring every few hours and originating near the central supermassive black holes of galactic nuclei1,2. It is currently unknown what triggers these events, how long they last and how they are connected to the physical properties of the inner accretion flows. Previously, only two such sources were known, found either serendipitously or in archival data1,2, with emission lines in their optical spectra classifying their nuclei as hosting an actively accreting supermassive black hole3,4. Here we report observations of QPEs in two further galaxies, obtained with a blind and systematic search of half of the X-ray sky. The optical spectra of these galaxies show no signature of black hole activity, indicating that a pre-existing accretion flow that is typical of active galactic nuclei is not required to trigger these events. Indeed, the periods, amplitudes and profiles of the QPEs reported here are inconsistent with current models that invoke radiation-pressure-driven instabilities in the accretion disk5–9. Instead, QPEs might be driven by an orbiting compact object. Furthermore, their observed properties require the mass of the secondary object to be much smaller than that of the main body10, and future X-ray observations may constrain possible changes in their period owing to orbital evolution. This model could make QPEs a viable candidate for the electromagnetic counterparts of so-called extreme-mass-ratio inspirals11–13, with considerable implications for multi-messenger astrophysics and cosmology14,15.

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The spatial extension of extended narrow line regions in MaNGA AGN

Cited by 34 publications

References 102 publications

Ionised Gas Kinematics in MaNGA AGN. Extents of the Narrow Line and Kinematically Disturbed regions

Ionised Gas Kinematics in MaNGA AGN. Extents of the Narrow Line and Kinematically Disturbed regions

The MURALES survey

X-ray quasi-periodic eruptions from two previously quiescent galaxies

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