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We present a 350 micron APEX/SABOCA map of IRAS 05399-0121/SMM 1, which is adense double-core system in Orion B9. We combined these data with our previousLABOCA 870-micron data. The spatial resolution of the new SABOCA image, ~3400AU, is about 2.6 times better than provided by LABOCA. We also make use ofSpitzer infrared observations to characterise the star-formation activity inthe source. The source is filamentary and remains a double-core system on the3400 AU scale probed here, where the projected separation between IRAS 05399and SMM 1 is 0.14 pc. The broadband spectral energy distribution of IRAS 05399suggests that it is near the Stage 0/I borderline. A visual inspection of theSpitzer/IRAC images provides hints of a quadrupolar-like jet morphology aroundIRAS 05399, supporting the possibility that it is a binary system. Thetemperature map reveals warm spots towards IRAS 05399 and the southeastern tipof the source. These features are likely to be imprints of protostellar orshock heating, while external heating could be provided by the nearby high-massstar-forming region NGC 2024. A simple analysis suggests that the densityprofile at the position of SMM 1 has the form ~r^-(2.3_{-0.9}^{+2.2}). Thesource splitting into two subcores along the long axis can be explained bycylindrical Jeans-type fragmentation but the steepness of the density profileis shallower than what is expected for an isothermal cylinder. The differencebetween the evolutionary stages of IRAS 05399 (protostellar) and SMM 1(starless) suggests that the former has experienced a phase of rapid massaccretion, supported by the very long outflow it drives. The protostellar jetfrom IRAS 05399 might have influenced the nearby core SMM 1.

astronomy and astrophysics

SABOCA 350-micron and LABOCA 870-micron dust continuum imaging of IRAS  05399-0121: mapping the dust properties of a pre- and protostellar core  system