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We have mapped with the IRAM interferometer at Plateau de Bure (PdBI) the12CO emission towards intergalactic star forming regions located in the tidaltail stemming from NGC7319, in the Stephan's Quintet compact group of galaxies.The 13CO emission of the same region was observed with the IRAM 30m telescopeand optical spectroscopy of several HII regions in the area were obtained withthe Calar Alto 3.5m telescope. We recovered with the interferometer about 50%of the CO(1-0) total emission that had been earlier measured with single dishobservations. We find two main areas of CO emission: (i) an elongated regiontowards the area known as SQ B where a Tidal Dwarf Galaxy could currently beforming (ii) a barely resolved area at the tip of the optical tidal arm. Bothregions follow dust lanes visible on HST images and their CO peak coincidesspatially exactly with the maximum of the Halpha line emission. In SQ B, thereis furthermore very good kinematical agreement between the CO, Halpha and HIcomponents. We conclude from these coincidences that the gaseous matter foundin quantities in the area is physically associated to the optical tidal tailand thus that the intergalactic atomic hydrogen there was expelled fromNGC7319. Furthermore, the relatively high oxygen abundances (about solar)estimated from the optical spectra of the HII regions imply that the gasfeeding the star formation originated from the inner regions of the parentgalaxy. In SQ B, we derive from different tracers a star formation rate of 0.5\msun/yr. The inferred molecular gas consumption time of 0.5 Gyr lies in therange of values found for spiral and starburst galaxies. On the other hand, theratio of 12CO/13CO>25 is much higher than the values found in disks of spiralgalaxies. A relatively low opacity for the 12CO gas is the most likely reason.

Molecular and ionized gas in the tidal tail in Stephan's Quintet