15min:

JUN-ICHI NAKASHIMA, Department of Astronomy, University of Illinois at Urbana-Champaign, 1002 W. Green St., Urbana, IL 61801 / The Graduate University for Advanced Studies, Nobeyama Radio Observatory, Minamimaki, Minamisaku, Nagano 384-1305, Japan; SHUJI DEGUCHI AND NARIO KUNO, Nobeyama Radio Observatory, National Astronomical Observatory, Minamimaki, Minamisaku, Nagano 384-1305, Japan.

IRAS 19312+1950 is an SiO maser source that exhibits a prominent nebulosity and rich-molecular species. Though SiO maser sources are mostly identified as a late-type star with active mass-loss, the kind of this object is unclear. To reveal the true character of IRAS 19312+1950, mapping observations of this object were made in the CO J=1-0, ¹³CO J=1-0, C¹⁸O J=1-0, CS J=2-1, and HCN J=1-0 lines and in the 150 GHz continuum band using the Nobeyama 45m telescope. The line profiles of the ¹²CO and HCN spectra consists of a weak component with the width of 50 km s^-1 and a strong component of the width of 3 km s^-1. The profile of the ¹³CO, C¹⁸O, and CS lines have only the narrow component. Both of the components have an intensity peak at the IRAS position. The narrow component was clearly resolved with a 15'' telescope beam. The spectral energy distribution of this object exhibits a doubly peaked profile between 1 and 25 µm. The 150 GHz continuum flux density was found to be 0.07 Jy, which is consistent with the flux density predicted by the expanding envelope model with a mass loss rate of 10^-4 M_ødot yr^-1 at a distance of 2.5 kpc. Though the present observations do not preclude the possibility of a young stellar object, we suggest that IRAS 19312+1950 is an AGB/post-AGB star. In addition to the results of single dish observations, we report a preliminary result of recent mapping observations in the HCO⁺ J=1-0 line with the Berkeley-Illinois-Maryland-Association (BIMA) Millimeter Array. In the HCO⁺ spectrum, both of the strong-narrow and weak-broad components were confirmed. And then, in the integrated intensity map of HCO⁺, we clearly found a bipolar flow, which corresponds the red- and blue-shift wings of the broad component.