Physical Property Of The Gemini Molecular Cloud

We present observations of a 4 squared degree area toward the Gemini cloud obtained using J = 1-0 transitions of 12 CO, 13 CO and C18 O. No C18 O emission was detected. The reason may be that the emission of C18 O is too faint to be detected, or no emission of C18 O. Several methods are used to estimate the distance, and the result is about 400 pc. We used the C UPID(part of the STARLINK project software) clump- finding algorithm CLUMPFIND to composed of 36 core candidates of 13 CO. These core candidates have a mea n Vlsr 0.32 km s-1, diameter of 0.25 pc, excitation temperatures of 7.9 K, optical depth of 0.33, line width of 0.54 km s-1, column density of 0.7 1021 cm-2 and a mean mass of 1.4 M⊙ and virial mass of 6.7 M⊙. Non-thermal broadening mechanism plays a dominant role in most of those core candidates. The great difference of Vlsr among those 36 core candidates may be triggered by stochastic processes between clouds such as collisions and chaotic magnetic fields. Two kinds of CMF are present in this paper, namely the CMF of LTE masses, and the virial masses derived from 13 CO. Their power indices are 1.83 and 1.63, respectively. They are likely to be starless core candidates for no infrared counterpart found in the line of sight of the 36 core candidates, or transient structures, which probably disperse after ～106 yr. The magnetic field in Gemini molecular cloud may range from 14-53 μG, and prefer the lower value.