HST emission-line images of nearby 3CR radio galaxies: two photoionization, accretion and feedback modes. (arXiv:1811.04946v1 [astro-ph.GA])
<a href="http://arxiv.org/find/astro-ph/1/au:+Baldi_R/0/1/0/all/0/1">Ranieri D. Baldi</a> (1,2), <a href="http://arxiv.org/find/astro-ph/1/au:+Zaurin_J/0/1/0/all/0/1">Javier Rodríguez Zaurín</a> (2,3), <a href="http://arxiv.org/find/astro-ph/1/au:+Chiaberge_M/0/1/0/all/0/1">Marco Chiaberge</a> (2,4), <a href="http://arxiv.org/find/astro-ph/1/au:+Capetti_A/0/1/0/all/0/1">Alessandro Capetti</a> (5), <a href="http://arxiv.org/find/astro-ph/1/au:+Sparks_W/0/1/0/all/0/1">William B. Sparks</a> (2), <a href="http://arxiv.org/find/astro-ph/1/au:+McHardy_I/0/1/0/all/0/1">Ian M. McHardy</a> (1) ((1), University of Southampton, UK, (2) Space Telescope Science Institute, Baltimore, USA, (3) University of Sheffield, UK, (4) Johns Hopkins University, Baltimore, USA, (5) INAF-Observatory of Turin, Italy)
We present HST/ACS narrow-band images of a low-z sample of 19 3C radio
galaxies to study the H$alpha$ and [OIII] emissions from the narrow-line
region (NLR). Based on nuclear emission line ratios, we divide the sample into
High and Low Excitation Galaxies (HEGs and LEGs). We observe different line
morphologies, extended line emission on kpc scale, large [OIII]/H$alpha$
scatter across the galaxies, and a radio-line alignment. In general, HEGs show
more prominent emission line properties than LEGs: larger, more disturbed, more
luminous, and more massive regions of ionized gas with slightly larger covering
factors. We find evidence of correlations between line luminosities and (radio
and X-ray) nuclear luminosities. All these results point to a main common
origin, the active nucleus, which ionize the surrounding gas. However, the
contribution of additional photoionization mechanism (jet shocks and star
formation) are needed to account for the different line properties of the two
classes. A relationship between the accretion, photoionization and feedback
modes emerges from this study. For LEGs (hot-gas accretors), the synchrotron
emission from the jet represents the main source of ionizing photons. The lack
of cold gas and star formation in their hosts accounts for the moderate
ionized-gas masses and sizes. For HEGs (cold-gas accretors), an ionizing
continuum from a standard disk and shocks from the powerful jets are the main
sources of photoionization, with the contribution from star formation. These
components, combined with the large reservoir of cold/dust gas brought from a
recent merger, account for the properties of their extended emission-line
regions.
We present HST/ACS narrow-band images of a low-z sample of 19 3C radio
galaxies to study the H$alpha$ and [OIII] emissions from the narrow-line
region (NLR). Based on nuclear emission line ratios, we divide the sample into
High and Low Excitation Galaxies (HEGs and LEGs). We observe different line
morphologies, extended line emission on kpc scale, large [OIII]/H$alpha$
scatter across the galaxies, and a radio-line alignment. In general, HEGs show
more prominent emission line properties than LEGs: larger, more disturbed, more
luminous, and more massive regions of ionized gas with slightly larger covering
factors. We find evidence of correlations between line luminosities and (radio
and X-ray) nuclear luminosities. All these results point to a main common
origin, the active nucleus, which ionize the surrounding gas. However, the
contribution of additional photoionization mechanism (jet shocks and star
formation) are needed to account for the different line properties of the two
classes. A relationship between the accretion, photoionization and feedback
modes emerges from this study. For LEGs (hot-gas accretors), the synchrotron
emission from the jet represents the main source of ionizing photons. The lack
of cold gas and star formation in their hosts accounts for the moderate
ionized-gas masses and sizes. For HEGs (cold-gas accretors), an ionizing
continuum from a standard disk and shocks from the powerful jets are the main
sources of photoionization, with the contribution from star formation. These
components, combined with the large reservoir of cold/dust gas brought from a
recent merger, account for the properties of their extended emission-line
regions.
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