MULTIPLICITY, DISKS, AND JETS IN THE NGC 2071 STAR-FORMING REGION

We present centimeter (cm) and millimeter (mm) observations of the NGC 2071 star-forming region performed with the Very Large Array (VLA) and Combined Array for Research in Millimeter-wave Astronomy (CARMA). We detected counterparts at 3.6 cm and 3 mm for the previously known sources IRS 1, IRS 2, I...

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Bibliographic Details
Published in:The Astrophysical journal 2012-02, Vol.746 (1), p.1-10
Main Authors: CARRASCO-GONZALEZ, Carlos, OSORIO, Mayra, ANGLADA, Gutllem, D'ALESSIO, Paola, RODRIGUEZ, Luis F, GOMEZ, José F, TORRELLES, José M
Format: Article
Language:English
Subjects:
ACCRETION DISKS
Arrays
ASTRONOMY
ASTROPHYSICS, COSMOLOGY AND ASTRONOMY
Disks
DUSTS
Earth, ocean, space
Emission
ENERGY SPECTRA
Exact sciences and technology
Jets
MASS
MORPHOLOGY
PROTOPLANETS
Spectral energy distribution
Star formation
STARS
Wavelengths
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Summary:We present centimeter (cm) and millimeter (mm) observations of the NGC 2071 star-forming region performed with the Very Large Array (VLA) and Combined Array for Research in Millimeter-wave Astronomy (CARMA). We detected counterparts at 3.6 cm and 3 mm for the previously known sources IRS 1, IRS 2, IRS 3, and VLA 1. All these sources show spectral energy distributions (SEDs) dominated by free-free thermal emission at cm wavelengths and thermal dust emission at mm wavelengths, suggesting that all of them are associated with young stellar objects (YSOs). IRS 1 shows a complex morphology at 3.6 cm, with changes in the direction of its elongation. We discuss two possible explanations to this morphology: the result of changes in the direction of a jet due to interactions with a dense ambient medium, or that we are actually observing the superposition of two jets arising from two components of a binary system. Higher angular resolution observations at 1.3 cm support the second possibility, since a double source is inferred at this wavelength. IRS 3 shows a clear jet-like morphology at 3.6 cm. Over a timespan of four years, we observed changes in the morphology of this source that we interpret as due to ejection of ionized material in a jet. The emission at 3 mm of IRS 3 is angularly resolved, with a deconvolved size (FWHM) of ~120 AU, and seems to be tracing a dusty circumstellar disk perpendicular to the radio jet. An irradiated accretion disk model around an intermediate-mass YSO can account for the observed SED and spatial intensity profile at 3 mm, supporting this interpretation.
ISSN:0004-637X
1538-4357
DOI:10.1088/0004-637X/746/1/71