Документ взят из кэша поисковой машины. Адрес оригинального документа : http://www.atnf.csiro.au/pub/people/atzioumi/kameno/GPSFFA.aux Дата изменения: Mon Feb 10 17:07:43 2003 Дата индексирования: Mon Dec 24 16:53:40 2007 Кодировка:

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\@writefile{toc}{\contentsline {section}{\numberline {1}Introduction}{1}}
\@writefile{toc}{\contentsline {section}{\numberline {2}The Sample}{2}}
\@writefile{toc}{\contentsline {section}{\numberline {3}Observations and Results}{3}}
\newlabel{eqn:ffaspectrum}{{1}{4}}
\newlabel{eqn:peakfreq}{{2}{4}}
\@writefile{toc}{\contentsline {section}{\numberline {4}Discussion}{4}}
\newlabel{eqn:ssaspectrum}{{4}{5}}
\newlabel{eqn:ssaasymmetry}{{5}{5}}
\@writefile{toc}{\contentsline {section}{\numberline {5}Conclusions}{8}}
\@writefile{lot}{\contentsline {table}{\numberline {1}{\ignorespaces Trichromatic VLBA observations and image performance.}}{9}}
\newlabel{tab:imageperform}{{1}{9}}
\@writefile{lot}{\contentsline {table}{\numberline {2}{\ignorespaces Flux densities and FFA parameters of each component.}}{10}}
\newlabel{tab:compflux}{{2}{10}}
\@writefile{lot}{\contentsline {table}{\numberline {3}{\ignorespaces Flux densities and FFA parameters of each component.}}{11}}
\newlabel{tab:ffafitparam}{{3}{11}}
\@writefile{lof}{\contentsline {figure}{\numberline {1}{\ignorespaces Trichromatic images and distributions of FFA opacity of nine GPS sources. Five type-1 sources and four type-2 sources are shown in upper and lower panels, respectively. Contours start at $\pm 3 \sigma $ level, increasing by factors of 2. The FFA opacity $\tau _{\rm f}$ is derived by spectral fitting with equation 1\relax . }}{12}}
\newlabel{fig:images}{{1}{12}}
\@writefile{lof}{\contentsline {figure}{\numberline {2}{\ignorespaces Spectra of type-1 sources. Flux densities at 2.3, 8.4, and 15.4 GHz are measured by Gaussian model fitting of CLEAN images using the task `IMFIT' in AIPS, as listed in table 2\relax . Errors are RSS (root sum squares) of fitting errors shown in IMFIT and flux calibration errors. The solid lines are results of the FFA spectral fitting with the model spectrum defined as equation 1\relax . Fitting parameters are listed in table 3\relax .}}{13}}
\newlabel{fig:SPECtype1}{{2}{13}}
\@writefile{lof}{\contentsline {figure}{\numberline {3}{\ignorespaces Spectra of type-2 GPS sources.}}{14}}
\newlabel{fig:SPECtype2}{{3}{14}}
\@writefile{lof}{\contentsline {figure}{\numberline {4}{\ignorespaces \relax \fontsize {10}{12}\normalfont \abovedisplayskip 10\p@ plus2\p@ minus5\p@ \abovedisplayshortskip \z@ plus3\p@ \belowdisplayshortskip 6\p@ plus3\p@ minus3\p@ \def \leftmargin \leftmargini \parsep 5\p@ plus2.5\p@ minus\p@ \topsep 10\p@ plus4\p@ minus6\p@ \itemsep 5\p@ plus2.5\p@ minus\p@ {\leftmargin \leftmargini \topsep 6\p@ plus2\p@ minus2\p@ \parsep 3\p@ plus2\p@ minus\p@ \itemsep \parsep }\belowdisplayskip \abovedisplayskip Histograms of the FFA opacities towards components A ($\tau _{\rm fA}$: {\it left}) and B ($\tau _{\rm fB}$: {\it right}). Open and filled areas indicate type 2 (radio and Seyfert galaxies) and 1 (quasars), respectively. Component B shows significant difference between type-1 and -2 sources, which component A does not. }}{14}}
\newlabel{fig:FFAhistogram}{{4}{14}}
\@writefile{lof}{\contentsline {figure}{\numberline {5}{\ignorespaces \relax \fontsize {10}{12}\normalfont \abovedisplayskip 10\p@ plus2\p@ minus5\p@ \abovedisplayshortskip \z@ plus3\p@ \belowdisplayshortskip 6\p@ plus3\p@ minus3\p@ \def \leftmargin \leftmargini \parsep 5\p@ plus2.5\p@ minus\p@ \topsep 10\p@ plus4\p@ minus6\p@ \itemsep 5\p@ plus2.5\p@ minus\p@ {\leftmargin \leftmargini \topsep 6\p@ plus2\p@ minus2\p@ \parsep 3\p@ plus2\p@ minus\p@ \itemsep \parsep }\belowdisplayskip \abovedisplayskip Histogram of the FFA opacity ratio $R$ defined as $R = {\begingroup \tau _{\rm fA}\endgroup \over \tau _{\rm fB}}$, where $\tau _{\rm fA}$ and $\tau _{\rm fB}$ are the FFA coefficients of double component. Since components are labeled in order of $\tau _{\rm f}$, $R$ is always larger than or equal to 1. Open and filled areas indicate type 2 (radio and Seyfert galaxies) and 1 (quasars), respectively. This histogram shows that type 1 sources are significantly asymmetric than type 2 sources are, in terms of FFA opacities. }}{15}}
\newlabel{fig:FFAasymmetry}{{5}{15}}
\@writefile{lof}{\contentsline {figure}{\numberline {6}{\ignorespaces \relax \fontsize {10}{12}\normalfont \abovedisplayskip 10\p@ plus2\p@ minus5\p@ \abovedisplayshortskip \z@ plus3\p@ \belowdisplayshortskip 6\p@ plus3\p@ minus3\p@ \def \leftmargin \leftmargini \parsep 5\p@ plus2.5\p@ minus\p@ \topsep 10\p@ plus4\p@ minus6\p@ \itemsep 5\p@ plus2.5\p@ minus\p@ {\leftmargin \leftmargini \topsep 6\p@ plus2\p@ minus2\p@ \parsep 3\p@ plus2\p@ minus\p@ \itemsep \parsep }\belowdisplayskip \abovedisplayskip {\it (left)}: Comparison between the FFA opacity ratio $R$ and intrinsic spectral index $\alpha _0$. Open circles and filled squares stand for the type 2 and 1 objects, respectively. Type-1 sources are likely to have a larger spectral index than that of type-2 objects. A small correlation is found between $R$ and $\alpha _0$ with the normalized correlation coefficient of $\rho = 0.54$, which yields confidence limits of 87\%. {\it (right)}: Comparison between the FFA asymmetry index $R$ and the flux density asymmetry index defined as $FR = {\begingroup S_{0 \rm A}\endgroup \over S_{0 \rm B}}$. There is No significant difference between the flux density asymmetry indices of type-1 and -2 objects. No significant correlation is found between $R$ and $FR$ with the normalized correlation coefficient of $\rho = 0.29$.}}{16}}
\newlabel{fig:FFAcorrelation}{{6}{16}}
\@writefile{lof}{\contentsline {figure}{\numberline {7}{\ignorespaces \relax \fontsize {10}{12}\normalfont \abovedisplayskip 10\p@ plus2\p@ minus5\p@ \abovedisplayshortskip \z@ plus3\p@ \belowdisplayshortskip 6\p@ plus3\p@ minus3\p@ \def \leftmargin \leftmargini \parsep 5\p@ plus2.5\p@ minus\p@ \topsep 10\p@ plus4\p@ minus6\p@ \itemsep 5\p@ plus2.5\p@ minus\p@ {\leftmargin \leftmargini \topsep 6\p@ plus2\p@ minus2\p@ \parsep 3\p@ plus2\p@ minus\p@ \itemsep \parsep }\belowdisplayskip \abovedisplayskip A schematic diagram of a GPS source. If the line of sight is close to the jet axis (type 1 sources), a large difference in the path length through the ambient plasma causes asymmetric FFA opacities. A type 2 source, on the contrary, has small difference in the path length, since the line of sight is nearly perpendicular to the jet axis. }}{17}}
\newlabel{fig:unifiedmodel}{{7}{17}}