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\@writefile{toc}{\contentsline {section}{\numberline {1}Introduction}{1}}
\@writefile{toc}{\contentsline {section}{\numberline {2}Observations and data reduction}{2}}
\@writefile{toc}{\contentsline {subsection}{\numberline {2.1}Radio continuum}{2}}
\@writefile{lot}{\contentsline {table}{\numberline {1}{\ignorespaces NGC\nobreakspace  {}6764 global parameters.}}{3}}
\newlabel{tab_glob_param}{{1}{3}}
\@writefile{toc}{\contentsline {subsection}{\numberline {2.2}CO data}{3}}
\@writefile{lof}{\contentsline {figure}{\numberline {1}{\ignorespaces Radiocontinuum at 20 cm (VLA) with a synthesized beam of $1.39\hbox {$^{\prime \prime }$}\times 1.26\hbox {$^{\prime \prime }$}$. The contour levels are 0.1,0.35,..,3.85 and 4,5,..,14 mJy.beam$^{-1}$ for a rms noise of 70 $\mu $Jy.beam$^{-1}$.}}{3}}
\newlabel{fig_vla20}{{1}{3}}
\@writefile{lof}{\contentsline {figure}{\numberline {2}{\ignorespaces Radiocontinuum at 3.5 cm (VLA) with a synthesized beam of $2.50\hbox {$^{\prime \prime }$}\times 2.0\hbox {$^{\prime \prime }$}$. The contour levels are 0.1,0.2,..,1.5 and 2.,2.5,..,10 mJy.beam$^{-1}$ for a rms noise of 56 $\mu $Jy.beam$^{-1}$.}}{3}}
\newlabel{fig_vla35}{{2}{3}}
\@writefile{lof}{\contentsline {figure}{\numberline {3}{\ignorespaces Integrated intensity for the \unhbox \voidb@x \hbox {$^{12}$CO(1--0) }transition (a) and for the \unhbox \voidb@x \hbox {$^{12}$CO(2--1) }transition (b). The contours for (a) are 1,3,..,27 \unhbox \voidb@x \hbox {Jy.beam$^{-1}$}.\unhbox \voidb@x \hbox {km.s$^{-1}$}and for (b) 3,6,..,54 \unhbox \voidb@x \hbox {Jy.beam$^{-1}$}.\unhbox \voidb@x \hbox {km.s$^{-1}$}. a) VLA 20cm emission overlaid by the integrated intensity for the \unhbox \voidb@x \hbox {$^{12}$CO(1--0) }transition. The contours are 1,3,..,27 \unhbox \voidb@x \hbox {Jy.beam$^{-1}$}.\unhbox \voidb@x \hbox {km.s$^{-1}$}. The position of the major axis and the bar are shown respectively by the solid and dashed lines. b) Integrated intensity for the \unhbox \voidb@x \hbox {$^{12}$CO(2--1) }transition. The contours are 1,3,..,27 \unhbox \voidb@x \hbox {Jy.beam$^{-1}$}.\unhbox \voidb@x \hbox {km.s$^{-1}$}}}{4}}
\newlabel{fig_ico_pdbi}{{3}{4}}
\@writefile{lot}{\contentsline {table}{\numberline {2}{\ignorespaces PdBI observations}}{4}}
\@writefile{toc}{\contentsline {section}{\numberline {3}Synchrotron and thermal emission}{4}}
\@writefile{toc}{\contentsline {subsection}{\numberline {3.1}Radio distribution}{4}}
\@writefile{toc}{\contentsline {subsection}{\numberline {3.2}The H$\alpha $ emission}{4}}
\@writefile{lof}{\contentsline {figure}{\numberline {4}{\ignorespaces Radiocontinuum flux at different wavelength from single-dish or low spatial resolution measurements, except for the 8.4 GHz data (this work).}}{4}}
\newlabel{fig_radioSED}{{4}{4}}
\@writefile{lof}{\contentsline {figure}{\numberline {5}{\ignorespaces B image (DSS2) of NGC\nobreakspace  {}6764 overlaid by the H$\alpha $ flux in the center of NGC\nobreakspace  {}6764, the contours are spaced by 0.15 dex step starting at 0.5 $\sigma $ level.}}{5}}
\newlabel{fig_halpha_dss}{{5}{5}}
\@writefile{lof}{\contentsline {figure}{\numberline {6}{\ignorespaces H$\alpha $ emission overlaid by the \unhbox \voidb@x \hbox {$^{12}$CO(2--1) }emission.}}{5}}
\newlabel{fig_halpha_co21}{{6}{5}}
\@writefile{lof}{\contentsline {figure}{\numberline {7}{\ignorespaces Spectral index $\alpha $ between the 20cm and 3.5cm radiocontinuum emission overlaid with the H$\alpha $ emission.}}{5}}
\newlabel{fig_halpha_vlaspectralindex}{{7}{5}}
\@writefile{toc}{\contentsline {subsection}{\numberline {3.3}Nuclear Star Formation}{5}}
\@writefile{toc}{\contentsline {section}{\numberline {4}The molecular gas}{6}}
\@writefile{toc}{\contentsline {subsection}{\numberline {4.1}Distribution}{6}}
\@writefile{lof}{\contentsline {figure}{\numberline {8}{\ignorespaces Non-thermal flux, in mJy, at 3 different frequencies for a range of non-thermal spectral index between -1 and 0. The flux is computed for a supernov\ae production rate of $1.2\times 10^{-2}$ per year (Eckart et al. 1991) in the center of NGC\nobreakspace  {}6764.}}{6}}
\newlabel{fig_nonthermalflux}{{8}{6}}
\newlabel{tab_radio_th-noth}{{3.3}{6}}
\@writefile{lot}{\contentsline {table}{\numberline {3}{\ignorespaces Thermal (free-free) and non-thermal (synchrotron) contribution to the radio continuum emission in the center of NGC\nobreakspace  {}6764. The thermal contribution is estimated from the H$\alpha $ flux (see text).}}{6}}
\@writefile{lof}{\contentsline {figure}{\numberline {10}{\ignorespaces Channel maps for the \unhbox \voidb@x \hbox {$^{12}$CO(1--0) }emission. The rms noise corresponds to 2 mJy.beam$^{-1}$. The contours are 5,15,25,..,95 mJy.beam$^{-1}$. The synthesized beam is $2\hbox {$^{\prime \prime }$}\times 1.6\hbox {$^{\prime \prime }$}$. The rest velocity is 2400 \unhbox \voidb@x \hbox {km.s$^{-1}$}. The cross is located at the phase center, i.e. $\alpha _{2000}=$19:08:16.370 and $\delta _{2000}$=50:55:59.58.}}{7}}
\newlabel{fig_co10_chanmap}{{10}{7}}
\@writefile{lof}{\contentsline {figure}{\numberline {9}{\ignorespaces Ratio of the thermal radio continuum emission (mJy) and H$\alpha $ luminosity ($10^{40}$ erg/s) at the distance of NGC\nobreakspace  {}6764, assuming an electron temperature of 10,000 K and an optical extinction $A_V= 4$.}}{8}}
\newlabel{fig_ratio_radio_halpha}{{9}{8}}
\@writefile{lof}{\contentsline {figure}{\numberline {11}{\ignorespaces H$\alpha $ emission in NGC6764 (Log scale) overlaid by the integrated intensity of the CO(1-0) emission (contour levels 1,3,..,30 \unhbox \voidb@x \hbox {Jy.beam$^{-1}$}).}}{8}}
\newlabel{fig_halpha_co10}{{11}{8}}
\@writefile{lof}{\contentsline {figure}{\numberline {12}{\ignorespaces Cumulative distribution of the molecular gas on the position centered on the \unhbox \voidb@x \hbox {$^{12}$CO(1--0) }peak.}}{8}}
\newlabel{fig_h2cumu}{{12}{8}}
\@writefile{lof}{\contentsline {figure}{\numberline {13}{\ignorespaces \unhbox \voidb@x \hbox {$^{12}$CO(1--0) }spectra within a box $5 \hbox {$^{\prime \prime }$}\times 3\hbox {$^{\prime \prime }$}$ located 3 \hbox {$^{\prime \prime }$}northern than the \unhbox \voidb@x \hbox {$^{12}$CO(1--0) }peak, at the (putative) position of the outflow}}{8}}
\newlabel{fig_spec_co_outflow}{{13}{8}}
\@writefile{toc}{\contentsline {subsection}{\numberline {4.2}Kinematics}{8}}
\@writefile{toc}{\contentsline {subsubsection}{\numberline {4.2.1}First and second velocity moments}{8}}
\@writefile{lot}{\contentsline {table}{\numberline {4}{\ignorespaces Position (J2000.0) of the peak emission in radiocontinuum (20cm), CO emission and H$\alpha $ emission (off-filter and emission line). The distance to the radiocontinuum peak is given in arcsec.}}{9}}
\newlabel{tab_astrom_peak}{{4}{9}}
\@writefile{lof}{\contentsline {figure}{\numberline {14}{\ignorespaces Isovelocity field contours of the \unhbox \voidb@x \hbox {$^{12}$CO(2--1) }overlaying the 20cm radiocontinuum emission. Thick lines are negative velocities by 10 \unhbox \voidb@x \hbox {km.s$^{-1}$}step. The reference velocity is 2400 \unhbox \voidb@x \hbox {km.s$^{-1}$}. The 20cm peak is indicated by a white star.}}{9}}
\newlabel{fig_co_mom1}{{14}{9}}
\@writefile{lof}{\contentsline {figure}{\numberline {15}{\ignorespaces Velocity dispersion from the \unhbox \voidb@x \hbox {$^{12}$CO(1--0) }observations overlaid by the velocity field. The thick lines are negative velocities by 10 \unhbox \voidb@x \hbox {km.s$^{-1}$}\ step.}}{9}}
\newlabel{fig_co_mom2}{{15}{9}}
\@writefile{toc}{\contentsline {subsubsection}{\numberline {4.2.2}Effects of the outflow}{9}}
\@writefile{toc}{\contentsline {subsubsection}{\numberline {4.2.3}Lindblad resonances}{10}}
\@writefile{lof}{\contentsline {figure}{\numberline {16}{\ignorespaces The asymmetry of the \unhbox \voidb@x \hbox {$^{12}$CO(1--0) }velocity dispersion $\sigma _V(+)$ is computed along the major axis (see text for explanation). The two bumps are connected to the starburst (84 \unhbox \voidb@x \hbox {km.s$^{-1}$}) and to the bar reconnection zone (78 \unhbox \voidb@x \hbox {km.s$^{-1}$}). These values are given without beam-smearing deconvolution.}}{10}}
\newlabel{fig_co_disp_excess}{{16}{10}}
\@writefile{lof}{\contentsline {figure}{\numberline {17}{\ignorespaces Integra \unhbox \voidb@x \hbox {$^{12}$CO(1--0) }(Jy.\unhbox \voidb@x \hbox {km.s$^{-1}$}) in the velocity range 20--100\unhbox \voidb@x \hbox {km.s$^{-1}$}. The contours are from 0.05 to 1 Jy.\unhbox \voidb@x \hbox {km.s$^{-1}$}by step of 0.05 ($\sigma \sim 0.02$ Jy.\unhbox \voidb@x \hbox {km.s$^{-1}$}).}}{10}}
\newlabel{fig_Ico10_20_100}{{17}{10}}
\newlabel{tab_resonances}{{4.2.3}{11}}
\@writefile{lot}{\contentsline {table}{\numberline {5}{\ignorespaces Resonances in NGC\nobreakspace  {}6764 between the disk and the wave-based bar feature ($\Omega _{\unhbox \voidb@x \hbox {bar}}$=22 \unhbox \voidb@x \hbox {km.s$^{-1}$.kpc$^{-1}$}). (see text for description)}}{11}}
\@writefile{toc}{\contentsline {subsubsection}{\numberline {4.2.4}Non-circular motions}{11}}
\@writefile{lof}{\contentsline {figure}{\numberline {18}{\ignorespaces Azimutal frequency $\Omega $ (stars) estimated from the rotation curve (HI+CO data). The third first data point are from CO(1-0) observations and the outer point from the HI observations (Wilcots et al. 2001). The UHR (diamond) and ILRs (cross) have estimated by setting the bar corotation at the semi major axis of the bar ($\sim $ 40\hbox {$^{\prime \prime }$}). The bar pattern speed is estimated to be 22\unhbox \voidb@x \hbox {km.s$^{-1}$.kpc$^{-1}$}.}}{11}}
\newlabel{fig_resonances}{{18}{11}}
\@writefile{toc}{\contentsline {subsection}{\numberline {4.3}CO line ratio}{11}}
\@writefile{lof}{\contentsline {figure}{\numberline {19}{\ignorespaces Position-velocity diagram of the \unhbox \voidb@x \hbox {$^{12}$CO(1--0) }(left) and \unhbox \voidb@x \hbox {$^{12}$CO(2--1) }(right) emission in the center of NGC\nobreakspace  {}6764. The offset 0 is taken at the CO peak. The major axis PA is 62\unhbox \voidb@x \hbox {$^\circ $}, and the PA of 90\unhbox \voidb@x \hbox {$^\circ $}has been added to compare with Fig. 1 of Eckart et al. (1996). The units are in \unhbox \voidb@x \hbox {Jy.beam$^{-1}$}}}{12}}
\newlabel{fig_co_pvdiag}{{19}{12}}
\@writefile{lof}{\contentsline {figure}{\numberline {20}{\ignorespaces Integrated intensity \unhbox \voidb@x \hbox {$^{12}$CO(1--0) }line overlaid by the \unhbox \voidb@x \hbox {$^{12}$CO(2--1) }to \unhbox \voidb@x \hbox {$^{12}$CO(1--0) }line ratio integrated over all the channels. The contours are from 0.2 up to 0.95 by step of 0.05}}{13}}
\newlabel{fig_co_line_ratio}{{20}{13}}
\@writefile{lof}{\contentsline {figure}{\numberline {21}{\ignorespaces \unhbox \voidb@x \hbox {$^{12}$CO(2--1) }to \unhbox \voidb@x \hbox {$^{12}$CO(1--0) }maximum line ratio $\Re _{max}$ computed in the center of NGC\nobreakspace  {}6764 for each \unhbox \voidb@x \hbox {$^{12}$CO(1--0) }channel (10 \unhbox \voidb@x \hbox {km.s$^{-1}$}width).}}{13}}
\newlabel{fig_coratiomax_vel}{{21}{13}}
\@writefile{lof}{\contentsline {figure}{\numberline {22}{\ignorespaces \unhbox \voidb@x \hbox {$^{12}$CO(2--1) }to \unhbox \voidb@x \hbox {$^{12}$CO(1--0) }line ratio for different velocities, indicated on each panel, with a channel width of 10 \unhbox \voidb@x \hbox {km.s$^{-1}$}. The first contour is for 0.4 and by step of 0.1. The radio continuum peak is shown by a cross.}}{14}}
\newlabel{fig_co_line_ratio_chan}{{22}{14}}
\@writefile{lof}{\contentsline {figure}{\numberline {23}{\ignorespaces \unhbox \voidb@x \hbox {$^{12}$CO(2--1) }/\unhbox \voidb@x \hbox {$^{12}$CO(1--0) }line ratio at the channel 120 \unhbox \voidb@x \hbox {km.s$^{-1}$}(10 \unhbox \voidb@x \hbox {km.s$^{-1}$}width) overlaid by the H$alpha$ isocontours.}}{15}}
\newlabel{fig_coratio_halpha_120}{{23}{15}}
\@writefile{toc}{\contentsline {subsection}{\numberline {4.4}\unhbox \voidb@x \hbox {H$_2$}mass}{15}}
\@writefile{toc}{\contentsline {section}{\numberline {5}Outflow}{16}}
\newlabel{tab_shell}{{5}{16}}
\@writefile{lot}{\contentsline {table}{\numberline {6}{\ignorespaces Morphological parameters for the bubble derived from the 20cm radiocontiuum map. h is the projected height and R$_{base}$ is the base projected radius .}}{16}}
\@writefile{lot}{\contentsline {table}{\numberline {7}{\ignorespaces The 20cm radiocontinuum emission in the outflow frame (rotation of 17 \unhbox \voidb@x \hbox {$^\circ $}) after subtracting the central component associated with the AGN (63 mJy). The center is fixed to the central radiocontinuum and the flux is given in mJy.}}{17}}
\newlabel{tab_vla20_sub}{{7}{17}}
\@writefile{toc}{\contentsline {section}{\numberline {6}Discussion}{17}}
\@writefile{toc}{\contentsline {subsection}{\numberline {6.1}The relation between the nuclear starburst and the AGN}{17}}
\@writefile{lof}{\contentsline {figure}{\numberline {24}{\ignorespaces Spectra index $\alpha $ (S$_\nu \propto \nu ^\alpha $) derived from the 20 and 3.5cm radiocontinuum.}}{17}}
\newlabel{fig_indexspec}{{24}{17}}
\@writefile{lot}{\contentsline {table}{\numberline {8}{\ignorespaces Bubble/Nucleus contributions for H$\alpha $ and 20cm radiocontinuum by fitting a 2D gaussian on the central contribution. The molecular gas mass for the NSB is the mass emcompassed by one CO(1-0) beam at the maximum (310$\times $250 pc).}}{18}}
\newlabel{tab_fluxes}{{8}{18}}
\@writefile{toc}{\contentsline {subsection}{\numberline {6.2}GMC destruction}{18}}
\newlabel{equa_energy_tidal}{{12}{18}}
\newlabel{equa_energy_gmc}{{13}{18}}
\@writefile{lof}{\contentsline {figure}{\numberline {25}{\ignorespaces Isocurves of cutoff radius r$_t$ (pc) at the distance R (pc) from the nucleus of mass M (Log(\unhbox \voidb@x \hbox {$\@mathcal {M}_{\odot }$})) where the tidal energy of a GMC, is comparable to its internal energy (see text). The velocity dispersion is estimated from Sanders et al. (1985) to be $\sigma = 1.35 r_t^{0.62} \unhbox \voidb@x \hbox {km.s$^{-1}$}$.}}{19}}
\newlabel{fig_tidal_trunc}{{25}{19}}
\@writefile{toc}{\contentsline {subsection}{\numberline {6.3}Nuclear star formation scenario}{19}}
\@writefile{lof}{\contentsline {figure}{\numberline {26}{\ignorespaces Critical density of the molecular clouds through the differential tidal shearing of the galaxy rotation. The solid line shows the critical density from the inner fitted rotation curve. The dotted lines shows the critical density for different central mass (in \unhbox \voidb@x \hbox {$\@mathcal {M}_{\odot }$}). The dashed horizontal lines shows the means density of molecular clouds with differents diameter D from Sanders et al. (1985) with $<\rho > = 19.5 (D/\unhbox \voidb@x \hbox {20 pc})^{-0.75}$ \unhbox \voidb@x \hbox {$\@mathcal {M}_{\odot }$}.pc$^{-3}$}}{19}}
\newlabel{fig_tidal_shearing}{{26}{19}}
\@writefile{toc}{\contentsline {section}{\numberline {7}Conclusions}{19}}
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