EDP Sciences
Free access
Volume 392, Number 3, September IV 2002
Page(s) 945 - 954
Section Formation, structure and evolution of stars
DOI http://dx.doi.org/10.1051/0004-6361:20021191

A&A 392, 945-954 (2002)
DOI: 10.1051/0004-6361:20021191

High-resolution study of the young stellar objects in Mon R2 IRS 3

T. Preibisch1, Y. Y. Balega2, D. Schertl1 and G. Weigelt1

1  Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany
2  Special Astrophysical Observatory, Nizhnij Arkhyz, Zelenchuk region, Karachai-Cherkesia, 357147, Russia

(Received 22 May 2002 / Accepted 21 June 2002)

We present a bispectrum speckle interferometry study of the embedded young stellar objects in Mon R2 IRS 3 in the near-infrared H and K bands. Our images with a resolution of 75 mas ( $\cor 62$ AU) show a close triple system surrounded by strong diffuse nebulosity and three additional infrared sources ( K magnitudes ~11.8-13.7) within 3'' of the brightest object IRS 3 A ( $K\sim 7.9$). We use HST/NICMOS archive images to derive near-infrared photometry for the sources and estimate the stellar masses of the three brightest objects IRS 3 A, B, and C to be in the range ~ 5- $15\,M_\odot$. IRS 3 A is surrounded by a bipolar nebula (position angle ~ $30\degr$), suggesting it to be embedded in a thick circumstellar disk or a torus with polar cavities. IRS 3 B shows a remarkable jet-like emission feature pointing towards the north-east (position angle $50\degr$). This feature consists of at least three individual knots with projected separations of 130, 230, and 290 mas (110, 190, and 240 AU) from IRS 3 B, which are much brighter in the K band than in the H band. This strongly indicates outflow activity from IRS 3 B, which is therefore probably the source of the compact high velocity molecular outflow reported from Mon R2 IRS 3. We also analyze Chandra X-ray archive data for the Mon R2 region and find IRS 3 A and IRS 3 C to be sources of hard ( $3\!-\!10$ keV) and variable X-ray emission, suggesting plasma temperatures of at least $50 \times 10^6$ K. The similarity of the X-ray properties to those of Class I protostars suggests magnetic interaction between the protostars and their circumstellar disks to be the origin of the X-ray emission; this provides indirect evidence for the presence of circumstellar disks in the intermediate- to high-mass young stellar objects IRS 3 A and IRS 3 C.

Key words: techniques: interferometric -- stars: individual: Mon R2 IRS 3 -- stars: formation -- stars: X-rays -- stars: winds, outflows

Offprint request: T. Preibisch, preib@mpifr-bonn.mpg.de

SIMBAD Objects in preparation

© ESO 2002

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