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

TL;DR

This study uses high-resolution dust continuum imaging at 350 and 870 microns, combined with infrared data, to analyze the structure, temperature, and star formation activity of a double-core system in Orion B9, revealing insights into core fragmentation and protostellar evolution.

Contribution

It provides the first high-resolution SABOCA 350-micron map of IRAS 05399-0121, combined with LABOCA data, to study dust properties and core fragmentation in a binary protostellar system.

Findings

The system remains a double-core at 3400 AU resolution.

IRAS 05399 is near the Stage 0/I boundary with signs of binary formation.

The density profile suggests cylindrical Jeans fragmentation, but is shallower than isothermal expectations.

Abstract

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