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- W1641963952 abstract "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 μm. 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 |$sim4-9enspace text M_odot$| under the single-temperature assumption, and |$sim4-8enspace text M_odot$| under the radiative transfer model assumptions, consistent with virial mass estimates from C18O 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 |$20enspacetext L_odot$| from the IRAS upper limits. The single-temperature assumption yields a best estimate of the total luminosity of |$5.3enspacetext L_odot$|. 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 $2.5enspacetext L_odot$. 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 <40, 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." @default.
- W1641963952 created "2016-06-24" @default.
- W1641963952 date "1995-06-15" @default.
- W1641963952 modified "2023-09-26" @default.
- W1641963952 title "A submillimetre study of the Class 0 protostar HH24MMS" @default.
- W1641963952 doi "https://doi.org/10.1093/mnras/274.4.1219" @default.
- W1641963952 hasPublicationYear "1995" @default.
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