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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}CO data}{2}}
\@writefile{lot}{\contentsline {table}{\numberline {1}{\ignorespaces NGC\nobreakspace  {}6764 global parameters.}}{3}}
\newlabel{tab_glob_param}{{1}{3}}
\@writefile{lot}{\contentsline {table}{\numberline {2}{\ignorespaces PdBI observations}}{3}}
\@writefile{lof}{\contentsline {figure}{\numberline {2}{\ignorespaces Radiocontinuum at 20 cm (VLA) with a synthesized beam of $2.50\hbox {$^{\prime \prime }$}\times 2.0\hbox {$^{\prime \prime }$}$. The contour levels are 0.1,0.35,..,3.85,4,5,..,14 mJy.beam$^{-1}$ for a rms noise of 70 $\mu $Jy.beam$^{-1}$.}}{3}}
\newlabel{fig_vla20}{{2}{3}}
\@writefile{toc}{\contentsline {subsection}{\numberline {2.2}Radio continuum}{3}}
\@writefile{lof}{\contentsline {figure}{\numberline {1}{\ignorespaces Integrated intensity for the \unhbox \voidb@x \hbox {$^{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}$}}}{4}}
\newlabel{fig_ico_pdbi}{{1}{4}}
\@writefile{lof}{\contentsline {figure}{\numberline {3}{\ignorespaces Radiocontinuum flux at different wavelength from single-dish or low spatial resolution measurements, except for the 8.4 GHz data (this work).}}{4}}
\newlabel{fig_radioSED}{{3}{4}}
\@writefile{toc}{\contentsline {section}{\numberline {3}The molecular gas}{4}}
\@writefile{toc}{\contentsline {subsection}{\numberline {3.1}Distribution}{4}}
\@writefile{lof}{\contentsline {figure}{\numberline {4}{\ignorespaces VLA 20cm emission overlaid by CO(1-0) emission with contour levels from 1 to 27 \unhbox \voidb@x \hbox {Jy.beam$^{-1}$}\unhbox \voidb@x \hbox {km.s$^{-1}$}by step of 1 \unhbox \voidb@x \hbox {Jy.beam$^{-1}$}\unhbox \voidb@x \hbox {km.s$^{-1}$}. The position of the major axis and the bar are shown respectively by the solid and dashed lines.}}{5}}
\newlabel{fig_vla_ico_bar}{{4}{5}}
\@writefile{lof}{\contentsline {figure}{\numberline {5}{\ignorespaces H$\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$^{-1}$}).}}{5}}
\newlabel{fig_halpha_co10}{{5}{5}}
\@writefile{lof}{\contentsline {figure}{\numberline {6}{\ignorespaces Cumulative distribution of the molecular gas mass on the position centered on the \unhbox \voidb@x \hbox {$^{12}$CO(1--0) }peak.}}{5}}
\newlabel{fig_h2cumu}{{6}{5}}
\@writefile{toc}{\contentsline {subsection}{\numberline {3.2}$^{12}$CO as molecular gas mass tracer ?}{6}}
\@writefile{toc}{\contentsline {subsection}{\numberline {3.3}Kinematics}{6}}
\@writefile{lof}{\contentsline {figure}{\numberline {7}{\ignorespaces Isovelocity field contours 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$^{-1}$}.}}{7}}
\newlabel{fig_co_mom1}{{7}{7}}
\@writefile{lof}{\contentsline {figure}{\numberline {8}{\ignorespaces Velocity dispersion from the \unhbox \voidb@x \hbox {$^{12}$CO(1--0) }observations overlaid by the \unhbox \voidb@x \hbox {$^{12}$CO(1--0) }integrated intensity with contours levels 2,4,..30 \unhbox \voidb@x \hbox {Jy.beam$^{-1}$}\unhbox \voidb@x \hbox {km.s$^{-1}$}}}{7}}
\newlabel{fig_co_mom2}{{8}{7}}
\@writefile{lof}{\contentsline {figure}{\numberline {9}{\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.}}{8}}
\newlabel{fig_co_disp_excess}{{9}{8}}
\@writefile{lof}{\contentsline {figure}{\numberline {10}{\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$^{-1}$}).}}{8}}
\newlabel{fig_Ico10_20_100}{{10}{8}}
\@writefile{lof}{\contentsline {figure}{\numberline {11}{\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.}}{9}}
\newlabel{fig_co10_chanmap}{{11}{9}}
\@writefile{lof}{\contentsline {figure}{\numberline {12}{\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}$}}}{10}}
\newlabel{fig_co_pvdiag}{{12}{10}}
\newlabel{tab_resonances}{{3.3}{10}}
\@writefile{lot}{\contentsline {table}{\numberline {3}{\ignorespaces Resonances in NGC\nobreakspace  {}6764 between the disk and the wave-based bar feature ($\Omega _{\unhbox \voidb@x \hbox {bar}}$=22 \unhbox \voidb@x \hbox {km.s$^{-1}$.kpc$^{-1}$}). (see text for description)}}{10}}
\@writefile{toc}{\contentsline {subsection}{\numberline {3.4}CO line ratio}{10}}
\@writefile{lof}{\contentsline {figure}{\numberline {13}{\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}{{13}{11}}
\@writefile{lof}{\contentsline {figure}{\numberline {14}{\ignorespaces \unhbox \voidb@x \hbox {$^{12}$CO(2--1) }to \unhbox \voidb@x \hbox {$^{12}$CO(1--0) }line ratio integrated on the whole range of channels overlaid by the \unhbox \voidb@x \hbox {$^{12}$CO(1--0) }contour levels (1,3,5,..,30 \unhbox \voidb@x \hbox {Jy.beam$^{-1}$}\unhbox \voidb@x \hbox {km.s$^{-1}$}).}}{11}}
\newlabel{fig_co_line_ratio}{{14}{11}}
\@writefile{lof}{\contentsline {figure}{\numberline {15}{\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).}}{11}}
\newlabel{fig_coratiomax_vel}{{15}{11}}
\@writefile{lof}{\contentsline {figure}{\numberline {16}{\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.}}{12}}
\newlabel{fig_co_line_ratio_chan}{{16}{12}}
\@writefile{lof}{\contentsline {figure}{\numberline {17}{\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.}}{13}}
\newlabel{fig_coratio_halpha_120}{{17}{13}}
\@writefile{toc}{\contentsline {section}{\numberline {4}Star Formation}{13}}
\@writefile{lof}{\contentsline {figure}{\numberline {18}{\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.}}{14}}
\newlabel{fig_radioflux_snr}{{18}{14}}
\newlabel{tab_radio_th-noth}{{4}{14}}
\@writefile{lot}{\contentsline {table}{\numberline {4}{\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).}}{14}}
\@writefile{toc}{\contentsline {section}{\numberline {5}The outflow/shell}{14}}
\@writefile{lof}{\contentsline {figure}{\numberline {19}{\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 $A_V= 4$.}}{14}}
\newlabel{fig_ratio_radio_halpha}{{19}{14}}
\newlabel{tab_shell}{{5}{14}}
\@writefile{lot}{\contentsline {table}{\numberline {5}{\ignorespaces Morphological parameters for the bubble derived from the 20cm radiocontiuum map. h is the height and R$_{base}$ is the disk radius .}}{14}}
\@writefile{lot}{\contentsline {table}{\numberline {6}{\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.}}{15}}
\newlabel{tab_vla20_sub}{{6}{15}}
\@writefile{lof}{\contentsline {figure}{\numberline {20}{\ignorespaces Spectra index $\alpha $ (S$_\nu \propto \nu ^\alpha $) derived from the 20 and 3.5cm radiocontinuum.}}{15}}
\newlabel{fig_indexspec}{{20}{15}}
\@writefile{toc}{\contentsline {subsection}{\numberline {5.1}H$\alpha $ emission}{15}}
\@writefile{toc}{\contentsline {section}{\numberline {6}Discussion}{15}}
\@writefile{toc}{\contentsline {subsection}{\numberline {6.1}The nuclear starburst/AGN}{15}}
\@writefile{lof}{\contentsline {figure}{\numberline {21}{\ignorespaces B image (DSS2) of NGC\nobreakspace  {}6764 overlaid by the H$\alpha $ uncalibrated flux in the center of NGC\nobreakspace  {}6764, the contours are spaced by 0.15dex step starting at 0.5 $\sigma $ level.}}{16}}
\newlabel{fig_halpha_dss}{{21}{16}}
\@writefile{lof}{\contentsline {figure}{\numberline {22}{\ignorespaces H$\alpha $ emission overlaid by the \unhbox \voidb@x \hbox {$^{12}$CO(2--1) }emission.}}{16}}
\newlabel{fig_halpha_co21}{{22}{16}}
\@writefile{lof}{\contentsline {figure}{\numberline {23}{\ignorespaces Spectral index $\alpha $ between the 20cm and 3.5cm radiocontinuum emission overlaid with the H$\alpha $ emission.}}{16}}
\newlabel{fig_halpha_vla35}{{23}{16}}
\@writefile{lot}{\contentsline {table}{\numberline {7}{\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 $250 pc).}}{16}}
\newlabel{tab_fluxes}{{7}{16}}
\@writefile{toc}{\contentsline {subsection}{\numberline {6.2}GMC destruction in the center by a central mass}{16}}
\@writefile{lot}{\contentsline {table}{\numberline {8}{\ignorespaces Position (J2000.0) of the peak emission in radiocontinuum (20cm), CO emission and H$\alpha $ emission (off-filter and emission line). The distance to the radiocontinuum peak is given in arcsec.}}{17}}
\newlabel{tab_astrom_peak}{{8}{17}}
\newlabel{equa_energy_tidal}{{13}{17}}
\newlabel{equa_energy_gmc}{{14}{17}}
\@writefile{lof}{\contentsline {figure}{\numberline {24}{\ignorespaces Distance R (pc) to the nucleus of mass M (\unhbox \voidb@x \hbox {$\@mathcal {M}_{\odot }$}) where the tidal energy of a GMC, of cutoff radius r$_t$ (pc), 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}$}$.}}{17}}
\newlabel{fig_tidal_trunc}{{24}{17}}
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\@writefile{lof}{\contentsline {figure}{\numberline {25}{\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$^{-3}$}}{18}}
\newlabel{fig_tidal_shearing}{{25}{18}}
\@writefile{toc}{\contentsline {section}{\numberline {7}Conclusions}{18}}
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