A submillimetre study of the Class 0 protostar HH24MMS

Details A submillimetre study of the Class 0 protostar HH24MMS A submillimetre study of the Class 0 protostar HH24MMS

Jun 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995mnras.274.1219w&link_type=abstract

Monthly Notices of the Royal Astronomical Society, Volume 274, Issue 4, pp. 1219-1224.

Astronomy and Astrophysics

Astronomy

29

Radiative Transfer, Stars: Formation, Dust, Extinction, Ism: Individual: Hh24Mms, Radio Continuum: Stars

Scientific paper

Results are presented of a JCMT submillimetre continuum study of the recently discovered candidate protostellar source HH24MMS. New submillimetre flux densities are listed, which were obtained under good weather conditions on Mauna Kea, and the shortest wavelength detection of this source is now 350 mum. The spectrum of HH24MMS is discussed and its implications for the mass, luminosity and evolutionary stage of the source are derived under two different sets of assumptions: (i) a grey-body single-temperature fit to the submillimetre spectral energy distribution, and (ii) a radiative transfer calculation with a dust model of icy and fluffy grains and a radial temperature dependence. A VLA continuum source coincident with the submillimetre source indicates an embedded young stellar object, and hence a protostellar source which has passed the ambipolar diffusion phase; the radio spectral index shows the emission to be partly free-free and partly thermal dust. A 450-μm map of HH24MMS shows the source to be unresolved E-W, and partially resolved N-S, with a deconvolved FWHM of 21 arcsec. The total mass of HH24MMS under this Gaussian is found to be ~4-9 M_solar under the single-temperature assumption, and ~4-8 M_solar under the radiative transfer model assumptions, consistent with virial mass estimates from C^18O linewidths. If the higher values are correct, they may be indicating partial gas freezing on to dust grains. Because of the absence of far-IR data the total luminosity is still uncertain. We can place an upper limit of 20 L_solar from the IRAS upper limits. The single-temperature assumption yields a best estimate of the total luminosity of 5.3 L_solar. The radiative transfer model attempts to separate the two contributions to this luminosity of external heating and internal heating, and suggests an upper limit to the luminosity of the central protostellar source of 2.5 L_solar. We use the ratio of total to submillimetre luminosity to determine the appropriate classification of a young stellar object, finding a value of this ratio for this source of <400, well below the Class 0 upper limit of 200. Hence we confirm that HH24MMS is a Class 0 protostar, which is at the beginning of the protostellar accretion phase.

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