Based on observations carried out with the IRAM Plateau de Bure Interferometer. IRAM is supported by the INSU/CNRS (France), MPG (Germany), and IGN (Spain).

.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.

Available from http://tdc-www.harvard.edu/software/wcstools

.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.

... $^{\prime \prime }$

These values have been derived by fitting elliptical isophotes to the image with the task ellipse in the IRAF/STSDAS package.

.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.

... ellipses

With the task ellipse in the IRAF/STSDAS package.

.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.

... 200 pc

As in García-Burillo et al. (2005), we attempted to use the HST WFPC2 F814W image corrected for extinction. However, in NGC 2782, the extinction correction proved to be unreliable, and we were forced to rely only on the Spitzer/IRAC image.

.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.

... $M_\odot$

As derived from the short-spacing single-dish observations of Young et al. (1995), see Sect. 3.1.

.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.

... $V_{\rm circ}$

As noted in Sect. 3.3, the unfortunate coincidence of the PA of the bar and the disk line-of-nodes makes streaming signatures difficult to diagnose in PV and isovelocity diagrams.

.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.

... 300 pc

Indeed, the high maximum of the $\Omega -\kappa /2$ curve is certainly overestimated by the epicyclic approximation, since the orbits are very elongated. Hence, although in our simulations, $\Omega_{\rm p}$ of the secondary bar would indicate two ILRs, it is more likely that there is only a single ILR, roughly in the middle at $\sim$ 200 pc.

.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.