Astron. Astrophys. 364, 625-632 (2000)

The protostellar system HH108MMS ^*

R. Siebenmorgen ¹ and E. Krügel <sup>2

1</sup> European Southern Observatory, Karl-Schwarzschild-Strasse 2, 85748 Garching b. München, Germany
² MPIfR, Auf dem Hügel 69, 53121 Bonn, Germany

Received 12 May 2000 / Accepted 20 October 2000

Abstract

We probe the region around the protostar HH108MMS by deep mid infrared photometric and polarimetric imaging. The protostar is detected at 14µm in absorption against the diffuse background. Next to HH108MMS, we find a second absorbing core, named Q1, and the young stellar object IRAS18331-0035 which is more advanced in its evolution and already seen in emission at 12µm and 14µm. HH108MMS, Q1 and IRAS18331-0035 form a triplet along an extended filamentary absorption feature. From the variation of the surface brightness across the source, we derive for HH108MMS and Q1 the optical depth and density profile. Along the axes which are parallel to the filament, the density distributions follow a power law. We estimate that the intensity of the background radiation at 14µm is about two times stronger than the intensity of the interstellar radiation field in the solar neighborhood. The present photometric data of IRAS18331-0035 between 12µm and 1.3mm can be explained by a central source with a luminosity of 2.5  that is surrounded by a spherical cloud of 1.1  with a density distribution. As HH108MMS is also seen in the millimeter dust emission, we can derive the ratio of the dust extinction coefficients at 14µm and 1.3mm and obtain . Because models for the dust in the diffuse interstellar medium predict a ratio of around 2000, our value points to fluffy composite grains which are expected to prevail in dense and cold environments.

First mid infrared polarisation images of pre-stellar absorbing cores are presented. At 12 and 14 the polarisation of the region around HH108MMS is strong () and tightly correlated with the source triplet. We demonstrate that the high degree of polarisation can be explained by extinction of rotationally aligned dust particles of moderate elongation.

Key words: ISM: dust, extinction stars: pre-main sequence stars: individual: HH108MMS techniques: polarimetric infrared: ISM: continuum

* Based on observations with ISO, an ESA project with instruments funded by ESA Member States (especially the PI countries: France, Germany, the Netherlands and the United Kingdom) with the participation of ISAS and NASA.

Send offprint requests to: rsiebenm@eso.org

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Contents

• 1. Introduction
• 2. Observations
  • 2.1. Photometric imaging
  • 2.2. Polarimetric imaging
• 3. Results
  • 3.1. The optical depth profiles of the protostars
  • 3.2. The density structure of the protostars
  • 3.3. The spectral energy distribution of IRAS18331-0035
  • 3.4. Mid-infrared polarisation images
  • 3.5. The degree of polarisation in the mid-infrared
• 4. Discussion: pre-stellar evolution
• 5. Conclusion
• Acknowledgements
• References

© European Southern Observatory (ESO) 2000

Online publication: January 29, 2001
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