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For refcode 1996A&A...314..738B:
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Copyright by European Southern Observatory (ESO). Reproduced by permission
1996A&A...314..738B The molecular gas content of spiral galaxies in compact groups. Boselli, A., Mendes de Oliveira, C., Balkowski, C., Cayatte, V., Casoli, F. Max-Planck-Institut fur Kernphysik, Postfach 103980, D-69117 Heidelberg, Germany European Southern Observatory (La Silla), Casilla 19001, Santiago 19, Chile Instituto Astronomico e Geofisico, USP, C.P. 9638, Sao Paulo, 01065-970, Brazil Observatoire de Paris, DAEC, Unite associee au CNRS D0173 et a l'Universite Paris 7, F-92195 Meudon Cedex, France DEMIRM and URA 336 du CNRS, Observatoire de Paris, 61 Av. de l'Observatoire, F-75014 Paris, France Received 19 December 1995/Accepted 2 May 1996 Abstract. We present ^12^CO(J=1-0) line observations of 15 late-type optically selected galaxies in compact groups. In order to study the effects of environment on the molecular content of compact group galaxies we use the CO(1-0) emission to estimate an indicative molecular hydrogen content of the target galaxies adopting a standard conversion factor X = N(H_2_)/I(CO). We compare the frequency distribution of the normalized hybrid molecular gas surface density to the one obtained for an optically selected reference sample of isolated galaxies. Despite their high-density environment, compact group galaxies have, on average, similar CO emission compared to isolated galaxies of same sizes and luminosities. However there are some compact group galaxies with perturbed morphologies and high far-infrared fluxes which have an enhanced CO emissivity. Keywords: galaxies: evolution - galaxies: interaction - galaxies: spiral -galaxies: ISM - radio lines: galaxies
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