Observational consequencies of baryonic gaseous dark matter

Possible observational consequencies of dark matter in the Galaxy in the form of dense molecular gas clouds -- clumpuscules of masses $M_c\sim 10^{-3}~\msun$ and radii $R_c\sim 3\times 10^{13}$ cm -- are considered. Recent models of the extreme scattering events -- refraction of radio-waves from quasars in dense plasma clumps in the Galactic halo -- definitely show on such clouds as possible dark matter candidate. We arugue that collisions of such clumpuscules are quite frequent: around $1-10~\msun$ a year can be ejected in the intestellar medium due to collisions. Optical continuum and 21 cm emissions from post-collisional gas are found to be observable. We show that clumpuscules can form around O stars HII regions of sizes $R\sim 30$ pc and emission measure $EM\simeq 20$ cm$^{-6}$ pc, and can also be observable in $H_\alpha$ emission. Evaporation of clumpuscules by external ionising radiation can be a substantial mass source. From requirement that the total mass input on the Hubble time cannot exceed the luminous mass in the Galaxy, typical radius of clouds is constrained as $R_c