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Dissecting a site of massive star formation: IRAS 23033+5951

Published online by Cambridge University Press:  01 August 2006

Michael A. Reid
Affiliation:
Harvard-Smithsonian Center for Astrophysics, Submillimeter Array, 645 North A'ohoku Pl., Hilo, HI, 96720, USA email: mareid@sma.hawaii.edu
Brenda C. Matthews
Affiliation:
Herzberg Institute of Astrophysics, 5071 West Saanich Road, Victoria, British Columbia, V9E 2E7, Canada email: brenda.matthews@nrc-cnrc.gc.ca
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Abstract

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We present new BIMA observations of the massive star-forming region IRAS 23033+5951 in Cepheus. 3 mm continuum observations reveal that the source decomposes into at least three dusty clumps, each of which has sufficient mass to form a massive star. The most massive clump has a mass of about 225 M and appears to house the massive protostar which drives the prominent CO outflow seen in the region. Our H13CN, 1-0, N2H+ 1-0, and H13CO+ 1-0 maps show that the three continuum sources are all embedded in an elongated structure whose long axis is perpendicular to the outflow. Both H13CO+ and H13CN peak at the geometric center of this structure, which lies between the two prominent continuum peaks. All three lines – H13CN, H13CO+, and N2H+ –show the same velocity gradient along the long axis of their integrated intensity maps. Although the approximately 90,000 AU length of the elongated structure prohibits a disk interpretation, the fact that the dynamical and gas masses of the structure differ by only a factor of a few suggests that the structure may be partially rotationally supported. We also detect a signature of infall toward the center of the structure, seen as an asymmetrically blue HCO+ line where its optically thin isotope, H13CO+, is symmetric and single-peaked.

Type
Contributed Papers
Copyright
Copyright © International Astronomical Union 2007

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