Published online by Cambridge University Press: 14 August 2015
The very low upper limits on distributed intergalactic (i.g.) HI (Gunn and Peterson 1965, Wampler 1967), and H2 (Field et al. 1966) have made it clear for some time now that if a smooth distributed i.g. gas exists in significant amounts (Ωig ≳ 10^−3), it must be ionized. X-Ray emission from rich clusters of galaxies such as Coma, indeed show that an intracluster gas can be seen (cf. Field 1974). Also persuasive in this connection are the head-tail radio galaxies in clusters, whose prototype is NGC 1265 (Miley et al. 1972, Jaffe and Perola 1973).