Comparison of OVRO Millimeter Array and/HST/NICMOS Images of the IRAS04302+2247 Circumstellar Disk

Details Comparison of OVRO Millimeter Array and/HST/NICMOS Images of the IRAS04302+2247 Circumstellar Disk Comparison of OVRO Millimeter Array and/HST/NICMOS Images of the IRAS04302+2247 Circumstellar Disk

Oct 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999alma.confe..47p&link_type=abstract

Science with the Atacama Large Millimeter Array (ALMA), Associated Universities, Inc., held October 6-8, 1999 at Carnegie Instit

Computer Science

Ovro, Circumstellar, Disk, Near Infrared, Hst, Molecular Gas, Morphology

Scientific paper

We present a comparison of Owens Valley Radio Observatory millimeter interferometry of the IRAS 04302+2247 circumstellar disk to near-infrared images obtained by the Hubble Space Telescope. IRAS 04302+2247 is a low-luminosity Class I young stellar object in the Taurus star-forming clouds at a distance of 140 pc. The HST/NICMOS image shows a sharp central absorption lane 7" (1000 AU) in length running directly between a bright scattered light background from bipolar reflection nebulae of roughly equivalent brightnesses. This dark lane has been interpreted as an optically thick disk seen precisely edge-on, occulting the star (Padgett et al. 1999 AJ 117, 1490). OVRO maps of the 13CO(1-0) emission indicates that dense gas is resolved along the position angle of the dust lane observed by HST. In addition, channel maps show a velocity gradient primarily along the major axis of this molecular bar, indicating rotation around a central source and supporting the disk interpretation of the scattered light structure. The resolution in the 3 mm OVRO image prevents us from making definitive statements about the relationship between the molecular gas and the detailed morphology seen by NICMOS. However, the 0".1 resolution of the ALMA array will rival that of the Hubble Space Telescope, providing complementary long wavelength molecular gas morphology and kinematics. Padgett, D. L., Brandner, W., Stapelfeldt, K. R.,Strom, S. E., Terebey, S.,Koerner 1999,

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