Radiative shock-wave theory. II - High-velocity shocks and thermal instabilities

Binette, L.; Dopita, Michael A.; Tuohy, I. R.

doi:10.1086/163544

Cited by 189 publications

(191 citation statements)

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“…These radiation fields form the input for the shock and photoionization code MAPPINGS (Binette et al 1985;Sutherland & Dopita 1993;Allen et al 2008;Dopita et al 2013), which models the interstellar medium (ISM) and produces a simulated emission-line spectrum from the nebular gas surrounding the ionizing radiation field.…”

Section: Starburst-agn Mixing Modelsmentioning

confidence: 99%

Starburst–AGN mixing – II. Optically selected active galaxies

Davies

Kewley

et al. 2014

Monthly Notices of the Royal Astronomical Society

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We use 4 galaxies from the Calar Alto Legacy Integral Field Area (CALIFA) survey with clear signs of accretion onto supermassive black holes to investigate the relative contribution of star-formation and active galactic nucleus (AGN) activity to the lineemission of each galaxy as a function of radius. The combination of star-formation and AGN activity produces curved "mixing sequences" on standard optical diagnostic diagrams, and the fraction of emission due to AGN activity decreases smoothly with distance from the centre of the galaxy. We use the AGN activity profiles to calculate the size of the AGN narrow line regions, which have radii of ∼ 6.3 kpc. We calculate the fractional contribution of the star-formation and the AGN activity to the global Hα, [O II] λλ 3727,3729 and [O III] λ 5007 luminosities of each galaxy, and show that both ionization sources contribute significantly to the emission in all three lines. We use weighted combinations of stellar and AGN photoionization models to produce mixing models, which are consistent with observations for 85 percent of spaxels across the galaxies in our sample. We also present a new diagnostic for starburst-AGN mixing which requires only the [O II], [O III] and Hβ emission lines, and can therefore be used to calculate AGN fractions up to z ∼ 0.85 in the optical and z ∼ 3.5 in the nearinfrared. We anticipate that this diagnostic will facilitate studies of the properties of AGN ionizing radiation fields and the relative optical contribution of star-formation and AGN activity over cosmic time.

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Section: Starburst-agn Mixing Modelsmentioning

confidence: 99%

Starburst–AGN mixing – II. Optically selected active galaxies

Davies

Kewley

et al. 2014

Monthly Notices of the Royal Astronomical Society

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“…For the region between the two nuclei (squares) and between the central regions and the southern emission knot (triangles) the data points follow the shock-wave model of Binette et al (1985) very well. Shock-heating in this region might be due to interaction of the radio-jet (18" S) with the ambient gas.…”

Section: S P E C T R O S C O P Ymentioning

confidence: 69%

Integral Field Spectrography of the double AGN merging system Markarian 463

Chatzichristou

1995

International Astronomical Union Colloquium

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A b s t r a c t . Markarian 463, a system of 2 interacting/merging galaxies (E and W) has been observed with SILFID at C F H T in sub-arcsec resolution conditions. We found that both nuclei are AGNs, with the W component being a Sy 2 or LINER and the E component, hitherto known to be a "hidden" Seyfert 1, having essentially Sy 2 characteristics. The bipolar collimated emission originating from the E nucleus is a conspicuous feature in the [OIII]SOOT and Ha reconstructed images, as well as in the V -R color map. In velocity maps some previously undetected kinematical features are detected, most notably a sharp velocity gradient (more than 300 km « _ 1 ) within 2" NE of the E nucleus. In addition, in the direct imaging mode a bright optical jet extending ~ 1.2" S from the E nucleus and a fuzzy blue component 0.8" W of the W nucleus were seen. Both were also discovered on HST images. Detailed ionization maps reveal individual regions with distinct physical conditions, which constrain the mechanism(s) responsible for the ionization of the gas. I n t r o d u c t i o n : T h e M r k 4 6 3 s y s t e mAlthough the origin of nuclear activity in galaxies is still not fully understood, most observational data can be reproduced by the black hole -accretion disk model. In this model of AGN, galaxy interaction and merging is a n efficient mechanism for fuelling the central black hole, with gas supplied by the host galaxy, the interacting companion, or both (Roos 1981, Norman andSilk 1983). In order to further investigate how interaction and merging of galaxies can trigger their nuclear activity, we selected a sample of active galaxies with disturbed morphologies and/or multiple nuclei. Mrk 463 was one of the systems we observed in bidimensional spectroscopy as well as in direct imaging mode.Optically, Mrk 463 is a complex system containing two central condensations, the E and W nuclei, separated by ~ 4" (~ 4 Kpc for z~ 0.05), embedded in a common diffuse body with prominent tidal tails. The E nucleus shows a typical Seyfert 2 spectrum (strong, blue-asymmetric, broad-based lines) but polarization studies have shown clear signatures of a "hidden" Seyfert 1 nucleus Goodrich, 1987 and1990;Mazzarella et al. 1991). Hutchings and Neff (1989) discovered a linear [OHI] 5 oo7 feature centered on this nucleus, extending ~ 20" in the N-S direction. It is associated with a similar radio structure Ulvestad 1988, Mazzarella et al. 1991). Recently, a one-sided linear 229 terms of use, available at https://www.cambridge.org/core/terms. https://doi

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“…In reality, EELR spectra are likely to be emissivity-weighted averages of several (perhaps very many) clouds with a range of density and size. Better agreement with the [0 III] temperature diagnostic and other line ratios can be achieved (with some fine tuning) by models incorporating a mixture of low-density matter-bounded and higher-density radiation-bounded clouds, with the former partially shielding the latter from the ionizing continuum (Binette et al 1996).…”

Section: The Agn Radiation Fieldmentioning

confidence: 99%

“…In particular, strong shocks driven into the cool gas cause local heating, ionization, and compression. For shock velocities v s > 200kms _ 1 , the gas is heated to temperatures in excess of 2 x 10 5 K and becomes a significant local source of ionizing radiation (Binette et al 1985). Such photoionizing shocks have recently been discussed in detail as an ionization mechanism for EELR by Sutherland, Bicknell, & Dopita (1993), Dopita & Sutherland (1995) and Morse, Raymond, & Wilson (1996).…”

Section: Fast Shocksmentioning

confidence: 99%