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

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

2004-11-05

arxiv.org/abs/astro-ph/0411142v1

Astronomy and Astrophysics

Astrophysics

Accepted by A&A; 14 pages, 7 b/w figures

Scientific paper

10.1051/0004-6361:20041595

Observations at mid-infrared (4.8-17.65 um) and radio (0.7-1.3 cm) wavelengths are used to constrain the structure of the high-mass star-forming region W3 IRS5 on 0.1'' (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 M0/yr 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, 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.

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