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We present the detection of molecular gas from galaxies located in nearbyvoids using the CO line emission as a tracer. The observations were done usingthe 45m Nobeyama Radio Telescope. Void galaxies lie in the most under denseparts of our universe and a significant fraction of them are gas rich, latetype spiral galaxies. Although isolated, they have ongoing star formation butappear to be slowly evolving compared to galaxies in denser environments. Notmuch is known about their star formation properties or cold gas content. Inthis study we searched for molecular gas in five void galaxies. The galaxieswere selected based on their relatively high IRAS fluxes or Ha lineluminosities, both of which signify ongoing star formation. All five galaxiesappear to be isolated and two lie within the Bootes void. We detected CO lineemission from four of the five galaxies in our sample and the molecular gasmasses lie between 10^8 to 10^9 Msolar. We did follow-up Ha imagingobservations of three detected galaxies using the Himalayan Chandra Telescopeand determined their star formation rates (SFRs). The SFR varies from 0.2 to 1Msolar/yr, which is similar to that observed in local galaxies. Our studyindicates that although void galaxies reside in under dense regions, theirdisks contain molecular gas and have star formation rates similar to galaxiesin denser environments.

Detection of Molecular Gas in Void Galaxies : Implications for Star Formation in Isolated Environments