We present the detection of molecular gas using CO ( 1–0 ) line emission and followup H \alpha imaging observations of galaxies located in nearby voids .
The CO ( 1–0 ) observations were done using the 45m telescope of the Nobeyama Radio Observatory ( NRO ) and the optical observations were done using the Himalayan Chandra Telescope ( HCT ) .
Although void galaxies lie in the most underdense parts of our universe , a significant fraction of them are gas rich , spiral galaxies that show signatures of ongoing star formation .
Not much is known about their cold gas content or star formation properties .
In this study we searched for molecular gas in five void galaxies using the NRO .
The galaxies were selected based on their relatively higher IRAS fluxes or H \alpha line luminosities .
CO ( 1–0 ) emission was detected in four galaxies and the derived molecular gas masses lie between ( 1 - 8 ) \times 10 ^ { 9 } ~ { } M _ { \odot } .
The H \alpha imaging observations of three galaxies detected in CO emission indicates ongoing star formation and the derived star formation rates vary between from 0.2 - 1.0 M _ { \odot } ~ { } yr ^ { -1 } , which is similar to that observed in local galaxies .
Our study shows that although void galaxies reside in underdense regions , their disks may contain molecular gas and have star formation rates similar to galaxies in denser environments .