An infrared-submillimeter study of star-forming regions selected by the ISOSS 170um survey

TL;DR

This study investigates cold, massive star-forming regions using infrared and submillimeter observations, identifying multiple protostars and clumps with potential for high-mass star formation, highlighting ongoing star formation processes.

Contribution

First detailed multi-wavelength analysis of ISOSS-selected cold, massive star-forming regions revealing their substructure and potential for high-mass star formation.

Findings

Identified 1-4 submillimeter clumps per region with sizes 0.1-0.4 pc.

Dust temperatures range from 11.6 to 21.3 K.

Detected embedded protostars, some possibly forming high-mass stars.

Abstract

Using the ISOPHOT Serendipity Survey (ISOSS) at 170um a sample of galactic star-forming regions exhibiting very cold dust temperatures (< 20 K) and high masses (> 100 M_sun) has been established. We characterise the star-forming content of five regions that were selected as potential sites for early stage high-mass star formation using SCUBA (JCMT) and Spitzer observations. In every region we identify one to four submillimeter clumps with projected sizes between 0.1 and 0.4 pc. The dust temperatures range from 11.6 to 21.3 K and the estimated clump masses are 2 to 166 M_sun. Towards the majority of submillimeter peaks we find point sources in the near- to mid-infrared. Most are interpreted as low-mass young stellar objects but we also detect very red sources. They probably represent very young and deeply embedded protostars that continue to accrete clump material and may reach higher masses. Several candidate intermediate-mass proto- or pre-main-sequence stars embedded in the clumps are identified. A subset of four clumps may be massive enough (> 100 M_sun) to form high-mass stars and accompanying clusters. The absence of stellar precursors with current masses in the high-mass regime leave the type of star formation occuring in the clumps unsettled. We confirm the presence of large fractions of cold material as derived from large-scale far-infrared measurements which dominates the emission of most clumps and suggests that the star-forming process will continue.