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\@writefile{toc}{\contentsline {title}{AGN Beyond the 100pc Scale}{1}}
\@writefile{toc}{\contentsline {author}{R A E Fosbury}{1}}
\@writefile{toc}{\contentsline {section}{\numberline {1}Introduction}{1}}
\newlabel{int}{{1}{1}}
\@writefile{toc}{\contentsline {section}{\numberline {2}AGN--host Interactions}{2}}
\newlabel{agn-hi}{{2}{2}}
\@writefile{toc}{\contentsline {subsection}{\numberline {2.1}The AGN Radiation Field}{2}}
\newlabel{agn-rad}{{2.1}{2}}
\@writefile{lof}{\contentsline {figure}{\numberline {1}{\ignorespaces A sketch of the optically thick nuclear torus whose shadow produces a sharply defined `ionization cone' of the type that is commonly seen in Seyfert 2 galaxies.}}{3}}
\newlabel{tor-per}{{1}{3}}
\@writefile{lof}{\contentsline {figure}{\numberline {2}{\ignorespaces A schematic representation of the apparent anisotropy of the AGN radiation field in different wavebands. The torus is essentially opaque from the MIR through to the soft X-ray but can become transparent outside this range. This pattern is useful for identifying type 2 AGN in multiband surveys. The spin axis has been left clear to indicate the possible presence of a particle jet and its associated, beamed radiation field.}}{4}}
\newlabel{agn-ani}{{2}{4}}
\@writefile{toc}{\contentsline {subsection}{\numberline {2.2}Winds and Jets}{5}}
\newlabel{agn-win}{{2.2}{5}}
\@writefile{lof}{\contentsline {figure}{\numberline {3}{\ignorespaces A sketch showing the relation of the particle jet and associated photon beam to the nuclear torus in a radio-loud AGN. The jet and the beam are both, of course, bi-directional and have only been separated in the diagram for clarity.}}{6}}
\newlabel{jet-bea}{{3}{6}}
\@writefile{toc}{\contentsline {section}{\numberline {3}Observational Techniques and Examples}{6}}
\newlabel{agn-ote}{{3}{6}}
\@writefile{lof}{\contentsline {figure}{\numberline {4}{\ignorespaces An X-ray image of {\it  Cygnus\nobreakspace  {}A} with the CHANDRA ACIS instrument. (Courtesy A.Wilson et al. NASA/UMD)}}{8}}
\newlabel{cha-ima}{{4}{8}}
\@writefile{lof}{\contentsline {figure}{\numberline {5}{\ignorespaces An X-ray cartoon of {\it  Cygnus\nobreakspace  {}A} that illustrates the interactions between the jets and the surrounding intracluster medium. (Courtesy CHANDRA X-ray Observatory, NASA/CXC/SAO)}}{9}}
\newlabel{cyg-xra}{{5}{9}}
\@writefile{toc}{\contentsline {subsection}{\numberline {3.1}Local AGN}{9}}
\newlabel{agn-loc}{{3.1}{9}}
\@writefile{lof}{\contentsline {figure}{\numberline {6}{\ignorespaces An early (WFPC) image taken with HST of the ionization cone in the Seyfert galaxy NGC\nobreakspace  {}5728 (Courtesy A.S. Wilson, STScI/NASA). This was taken with the PC before correction of Hubble's spherical aberration. It is in the light of H${\alpha }$\ and [O\nobreakspace  {}III] and the structure has an overall extent of some 1.8kpc. The apex of each cone indicates, presumably, the site of the obscured AGN.}}{10}}
\newlabel{ion-con}{{6}{10}}
\@writefile{lof}{\contentsline {figure}{\numberline {7}{\ignorespaces An HST WFPC\nobreakspace  {}2 image of the Circinus galaxy in two narrow (H${\alpha }$\ and [O\nobreakspace  {}III]) and two broad (NIR and green) filters. The nearside ionization cone can be seen projected against the disk by virtue of its strong hydrogen and oxygen line emission. (Courtesy A.S. Wilson et al., NASA)}}{10}}
\newlabel{dis-con}{{7}{10}}
\@writefile{lof}{\contentsline {figure}{\numberline {8}{\ignorespaces The powerful radio galaxy {\it  Cygnus\nobreakspace  {}A}. The colour image on the right is a combination of B, V, R and I broad band and [O\nobreakspace  {}III] and H${\alpha }$\ narrow band exposures from the HST WFPC\nobreakspace  {}2 archive with the addition of a B-band exposure with Keck. The B-band contour map on the left is from the Keck LRISp polarimeter showing the measured $\ensuremath  {\mathchoice {\unhbox \voidb@x \hbox {\relax \mathversion  {bold}$\displaystyle E$}} {\unhbox \voidb@x \hbox {\relax \mathversion  {bold}$\textstyle E$}} {\unhbox \voidb@x \hbox {\relax \mathversion  {bold}$\scriptstyle E$}} {\unhbox \voidb@x \hbox {\relax \mathversion  {bold}$\scriptscriptstyle E$}}}$-vectors and the location of the apertures used for spectropolarimetry (a negative version of the colour image is shown as an underlay). The position of the radio axis (R) and the outline of the ionization cone (IC) are shown. The blue, equatorial ring on the southeast side consists of starlight and is unpolarized.}}{11}}
\newlabel{cyg-ima}{{8}{11}}
\@writefile{lof}{\contentsline {figure}{\numberline {9}{\ignorespaces A cartoon of {\it  Cygnus\nobreakspace  {}A} which illustrates the various components, their positions and orientations. The letters `FC' followd by a number represent various so-called `featureless continua' that had been seen in the spectropolarimetry as polarized or unpolarized sources.}}{12}}
\newlabel{cyg-car}{{9}{12}}
\@writefile{lof}{\contentsline {figure}{\numberline {10}{\ignorespaces An optical image (greyscale, HST WFPC\nobreakspace  {}2) and a radio map (contours, ATCA) of the radio galaxy PKS\nobreakspace  {}B2152-699 showing the bright jet-cloud interaction (HIC) to the NE and a fainter counter feature to the SW. The associated cartoon illustrates the location and the orientation of the various observed components with `RC' marking the offset position of the 6cm radio source associated with the HIC. }}{13}}
\newlabel{p21-ima}{{10}{13}}
\@writefile{toc}{\contentsline {subsection}{\numberline {3.2}Distant AGN}{13}}
\newlabel{agn-dis}{{3.2}{13}}
\@writefile{lof}{\contentsline {figure}{\numberline {11}{\ignorespaces The ultraviolet--optical SED of the radio galaxy TXS\nobreakspace  {}0211-122, $z=2.340$\ measured with the Keck (optical) and VLT (NIR) telescopes. The red line shows a template radio-loud quasar spectrum scattered by a clumpy dust distribution within the illuminated `ionization cones' in the host galaxy. In this powerful source, the entire UV-optical continuum can be ascribed to the scattered AGN light which completely dominates the host galaxy starlight. The narrow emission lines---which are relatively much stronger than in the scattered quasar light---originate from the photoionized ISM of the host. The shortest wavelength emission line is Lyman-$\alpha $\ and the redmost line is H$\alpha $. (Courtesy J. Vernet et al.)}}{15}}
\newlabel{txs-sed}{{11}{15}}
\@writefile{lof}{\contentsline {figure}{\numberline {12}{\ignorespaces Optical spectropolarimetry of TXS\nobreakspace  {}0211-122 obtained with the Keck LRISp instrument. The top two panels show differently scaled versions of the total flux. The third panel shows the fractional polarization in both line and continuum wavelength bins. The final (bottom) panel shows the position angle of the $\ensuremath  {\mathchoice {\unhbox \voidb@x \hbox {\relax \mathversion  {bold}$\displaystyle E$}} {\unhbox \voidb@x \hbox {\relax \mathversion  {bold}$\textstyle E$}} {\unhbox \voidb@x \hbox {\relax \mathversion  {bold}$\scriptstyle E$}} {\unhbox \voidb@x \hbox {\relax \mathversion  {bold}$\scriptscriptstyle E$}}}$-vector in the same wavelength bins: for comparison, the PA of the major axis of the restframe UV image of this source is 122$^{\circ }$\ which is geometrically consistent with the scattering origin of the alignment effect. The degree of polarization is also consistent with dust (single-)scattering models within ionization cones where the integration over scattering angle dilutes the net polarization. Note the low fractional polarization in the narrow bands centred on the strong, narrow emission lines. (Courtesy J. Vernet et al.)}}{16}}
\newlabel{txs-pol}{{12}{16}}
\@writefile{lof}{\contentsline {figure}{\numberline {13}{\ignorespaces A diagram representing the scattering, absorption and thermal emission balance for the dust content of the ionization cones ({\em  only}) in an type\nobreakspace  {}2 active galaxy. Starting with the naked quasar SED in the upper left corner, the lower green line represents the escaping flux after some modest dust extinction when seen close to the AGN axis (as a type\nobreakspace  {}1 object). The lower left black line represents the quasar light scattered out of the ionization cone, by the same dust that produces the extinction for a type\nobreakspace  {}1 observer, towards an observer who would see this as a type\nobreakspace  {}2 object. The red spectrum is an observation of one of the redshift 2.5 radio galaxies. The FIR SED (black curve on the right) is the thermal emission from the dust that is causing the extinction and scattering within the cones. The red sub-mm points are observations of the source represented by the red spectrum and the blue observations represent other high-z radio galaxies. This analysis suggests that the bulk of the cool dust thermal emission from AGN like this is coming from dust heated by star formation rather than being reprocessed quasar power. (Courtesy J. Vernet et al.)}}{17}}
\newlabel{ene-bal}{{13}{17}}
\@writefile{lof}{\contentsline {figure}{\numberline {14}{\ignorespaces The emission line halo of TXS\nobreakspace  {}0211-122 from Keck long-slit spectroscopy. The halo can be seen in all the strong UV emission lines but is most extended in Lyman-$\alpha $. the spectra are plotted aligned and on the same spatial scale as the restframe UV and radio images. Some of these halos can be detected even beyond the extent of the radio lobes. (Courtesy M. Villar-Mart\'{\i }n et al.)}}{18}}
\newlabel{lya-hal}{{14}{18}}
\@writefile{toc}{\contentsline {section}{\numberline {4}What next?}{19}}
\newlabel{wha-nex}{{4}{19}}
\@writefile{lof}{\contentsline {figure}{\numberline {15}{\ignorespaces An ultraviolet line ratio diagram plotted for the NLR radio galaxies at $2\leq z\leq 3$. The red line shows a sequence of photoionization models as a function of metallicity in Solar units. The black and blue points are (similar) sources from different observed samples. The dashed green line shows the locus of points established for quasar BLR---which of course have a much higher particle density---again labelled with metallicity in Solar units. (Courtesy J. Vernet et al.)}}{20}}
\newlabel{cnh-lrd}{{15}{20}}
\@writefile{toc}{\contentsline {section}{\numberline {5}Further Reading}{20}}
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