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M.F. Campbell (Colby C.), T.K. Sridharan, J.L. Hora (SAO), M. Kassis (Keck O.), L.C. Johnson, S.H. Fung (Colby C.), H. Beuther (MPIA Heidelberg), J.D. Adams (Cornell)
We have detected emission at 10.4 \mum (N band) and at 24.8 \mum from the high mass protostar candidate IRAS 18089-1732 with the MIRSI camera on the IRTF. Emission was detected within an arcsecond of a mm and sub-mm dust continuum peak at which there are an H2O maser and a hypercompact HII region (HC HII). This source was also detected by IRAC on Spitzer in the GLIMPSE survey.
Two sources, A & B, were detected in both MIRSI filters, and all IRAC bands. The brighter N band source, A, was registered to the IRAC 8 \mum position for astrometry. It is at the position of an MSX source, 10\arcsec NW of the H2O/HC HII/smm position. The fainter N band source, B, is within an arcsec of the H2O/HC HII/smm position. It is brighter than A at 24.8 \mum.
The 24.8 \mum emission of source B is offset E of the N band emission, and is extended about 2\farcs5 N-S (marginally resolved on the IRTF). The extension is roughly parallel to the SiO outflow axis. The CH3OH maser located 1\farcs5 to the SW is apparently outside the mid-ir peak. The SED of source B rises from 3.4 mJy at 3.6 \mum to 6.1 (+/- 3) Jy at 24.8 \mum, with an apparent silicate absorption in N band, suggesting that the source is deeply embedded.
The IRTF is operated by the University of Hawaii supported by NASA under Cooperative Agreement NCC5-538 issued through the OSS Planetary Astronomy Program.
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Bulletin of the American Astronomical Society, 37 #4
© 2005. The American Astronomical Soceity.