The masers of E-type methanol in Orion KL and SGR B2

Details The masers of E-type methanol in Orion KL and SGR B2 The masers of E-type methanol in Orion KL and SGR B2

Apr 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987ap%26ss.132..263z&link_type=abstract

Astrophysics and Space Science (ISSN 0004-640X), vol. 132, no. 2, April 1987, p. 263-268.

Astronomy and Astrophysics

Astrophysics

8

Interstellar Masers, Methyl Alcohol, Orion Constellation, Sagittarius Constellation, Abundance, Interstellar Gas, Population Inversion, Velocity Distribution

Scientific paper

Using a simplified model, the statistical equilibrium and radiative transfer equations of E-type-CH3OH are solved for Orion KL and Sgr B2. According to the authors' calculation results and the observation data taken by Matsakis et al. (1980) and Morimoto et al. (1985), the physical conditions of both sources are estimated. In the J2 - J1 E methanol maser region of Orion KL, the density, kinetic temperature, dust temperature, and the fractional abundance are 0.8 - 2×106cm-3, ⪉150, 30 - 90K, 0.8 - 8×10-6, respectively. In the 4-1 - 30 E and 5-1 - 40 E methanol maser region of Sgr B2 the corresponding physical conditions are 104cm3, 45, 23K, and 7×10-7, respectively.

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