Mathematics – Probability
Scientific paper
May 2009
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009aas...21431504r&link_type=abstract
American Astronomical Society, AAS Meeting #214, #315.04; Bulletin of the American Astronomical Society, Vol. 41, p.760
Mathematics
Probability
Scientific paper
V4046 Sgr is a 12 Myr-old spectroscopic binary with a period of 2.4 days. At a distance of 73 pc (Torres et al. 2008), it is the second closest classical T Tauri star to the Earth after TW Hydra. Previously, rotational transitions of CO, HCO+, CN, and HCN were detected with the 30m IRAM telescope (Kastner et al. 2008). The double peaked CO profiles can be fit by a model invoking a Keplerian disk with outer radius of 250 AU that is viewed at an inclination of 35 degrees. The CO line profile was asymmetric, with the redshifted emission peak in both C-12 and C-13 brighter than the blueshifted peak. We have used the SMA to spatially resolve the J=2-1 CO emission line and the 230 GHz continuum. The CO channel maps show a disk consistent with Keplerian rotation. At the velocity of the redshifted emission peak, these observations reveal enhanced CO emission a few arcseconds to the southwest of the binary. A question arises as to whether this enhanced CO emission is associated with a third star in the system. According to the analysis of Tokovinin et al. (2006), the probability that a binary with a 2.4 day period has an associated tertiary star is essentially 100%. We searched archival Chandra and HST (ACS and NICMOS) images in the vicinity of V4046 Sgr to look for a star at the position of the enhanced CO emission. While there is a star in the HST ACS images approximately coincident with the enhanced CO emission, our preliminary analysis suggests that this star is not physically associated with V4046 Sgr. We will present a detailed discussion of the SMA results. This work has been partially supported by a NASA ADA grant to RIT and UCLA.
Kastner Joel H.
Rodriguez David R.
Wilner David J.
Zuckerman Ben
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