Subarcsecond mid-infrared and radio observations of the W3 IRS5 protocluster

¹ Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany e-mail: vdtak@mpifr-bonn.mpg.de
² School of Physics, University of Sydney, NSW 2006, Australia
³ NASA Goddard Space Flight Center, Infrared Astrophysics, Code 685, Greenbelt MD 20771, USA

Received: 5 July 2004
Accepted: 27 October 2004

Abstract

Observations at mid-infrared (4.8–17.65 μm) and radio (0.7–1.3 cm) wavelengths are used to constrain the structure of the high-mass star-forming region W3 IRS5 on 01 (200 AU) scales. Two bright mid-infrared sources are detected, as well as diffuse emission. The bright sources have associated compact radio emission and probably are young high-mass stars. The measured sizes and estimated temperatures indicate that these sources together can supply the observed far-infrared luminosity. However, an optically thick radio source with a possible mid-infrared counterpart may also contribute significant luminosity; if so, it must be extremely deeply embedded. The infrared colour temperatures of 350–390 K and low radio brightness suggest gravitational confinement of the H ii regions and ongoing accretion at a rate of a few 10^-8  yr^-1 or more. Variations in the accretion rate would explain the observed radio variability. The low estimated foreground extinction suggests the existence of a cavity around the central stars, perhaps blown by stellar winds. At least three radio sources without mid-infrared counterparts appear to show proper motions of ~100 km s^-1, and may be deeply embedded young runaway OB stars, but more likely are clumps in the ambient material which are shock-ionized by the OB star winds.