The IRAS point source 22343+7501 is embedded in the L1251 molecular cloud. Initial observations of this object were made at near-infrared wavelengths, whereupon we discovered several discrete sources embedded in the cloud. This prompted us to obtain observations at several wavelengths, to try to understand as much about the nature of the source as possible.

We note present mm continuum service observations (CANSERV) of IRAS 22343+7501, obtained in August 1993 with the JCMT and UKT14 bolometer (more details may be found in Rosvick & Davidge 1994). The source was detected at 1.3, 1.1 and 0.85 mm only; shorter wavelengths were not possible at the time of the observations, due to poor sky conditions. Table 1 lists the results.

Wavelength (mm)	Flux (Jy)

1.3		0.232 (0.024)

1.1		0.383 (0.030)

0.8		0.710 (0.114)

Our near-infrared observations and the IRAS far-infrared observations indicated that the source is just past the protostellar phase of its evolution. The mm observations confirm this; Cabrit & Andre (1991) obtained 1.3 mm continuum observations of 25 embedded sources and found that their sources with molecular outflows have much higher 1.3 mm fluxes. The 1.3 mm flux for IRAS 22343+7501 falls within the outflow values of Cabrit & Andre, thus supporting the existence of an outflow as discovered by Sato & Fukui (1989) and the young age of this object.

Part of our analysis involved the construction of a spectral energy distribution from mm to near-infrared wavelengths. Figure 1 contains the mm portion of the spectral energy distribution, plus one IRAS observation at 100 microns, as well as a blackbody model distribution, shown as a dashed line. We calculated the model by estimating values for the dust temperature (37 K), source size (1.5 x 10-10 sr) and dust optical depth (which is given by the frequency of the observation divided by the frequency (3.0 x 1012 Hz) at which the dust becomes optically thin, raised to the power of 1.4). The match between the model and the observations is quite good, implying a single dust temperature in this wavelength region.

We estimated the mass of the circumstellar material using the 1.3 mm flux, the opacity per unit mass column density (0.02 cm2/g), the Planck function at 1.3 mm for a dust temperature of 37 K, and the distance to the source (200 pc). The above assumes the dust emission is optically thin and isothermal at 1.3 mm, which results in an approximate value of 0.04 solar mass.

References:

Cabrit, S., and Andre, P. 1991, ApJ, 379, L25

Rosvick, J.M., and Davidge, T.J. 1994, subm to PASP

Sato, F., and Fukui, Y. 1989, ApJ, 343, 773

J. M. Rosvick,

Department of Physics and Astronomy, University of Victoria, Box 3055, Victoria, BC, Canada V8W 3P6

T. J. Davidge,

Department of Geophysics and Astronomy, University of British Columbia, Vancouver, BC, Canada

&

Gemini Canada Project Office, Dominion Astrophysical Observatory, 5071 West Saanich Road, Victoria, BC, Canada