Single CO peak in the double bar galaxy NGC 5850

NGC 5850 is a prototype of double-barred galaxy (Friedli et al. 1996) classified as SBb(sr) I-II (Higdon et al. 1998; Prieto et al. 1997). This kind of system is primordial to understand the physical mechanism responsible for feeding galaxy nuclei and boost the star formation rate. The CO(1-0) emission has been mapped in NGC 5850, i) in the very center, using the IRAM Plateau de Bure interferometer, to reach a 2.4\arcsec$\times$1.5\arcsec
(PA$=$$-{165}^{\circ }$) spatial resolution, and ii) in the primary bar with the IRAM-30m telescope, with a 22\arcsec beam. We have found CO emission in the center of NGC 5850, located in a single peak on the northern part of the nuclear ring. The high velocity dispersion of the molecular gas may prevent star formation in that region. Gas simulations performed with a single bar pattern and without the tidal influence of the companion NGC 5846 are unable to reproduce the features observed in NGC 5850 (Combes, Leon, Friedli, 1999, in preparation). The decoupling of a second bar appears necessary. The presence of the single molecular peak could be due to an $m=1$ mode excited by the massive companion.