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We present sub-arcsecond images of the mm dust emission and 13 CO J=2–1 line emission in the young quadruple system GG Tau. These observations unambiguously resolve the circumbinary disk of the close (∼ 0.3) binary system into two distinct components: an extremely dense, sharp-edged ring, surrounded by an extended disk. Continuum emission is also detected(More)
We report new high resolution (0.6 − 1.7) images of GM Aur in the 12 CO J = 2→ 1 line and the 1.3 and 2.7 mm continuum. The dust disk, located at the center of the CO disk, is resolved by the 0.6 beam of the interferometer. We derive a minimum radius of ∼ 200 AU, and a total mass (dust+gas) of about ∼ 0.025 M. Our CO observations also resolve the Keplerian(More)
We present the results of a search for dust and gas emission around T Tauri stars in the Taurus-Auriga region, conducted with the IRAM interferometer in CO, HCO + and the adjacent continua at 1.3 and 3.4 mm. We studied a sample of young stars with and without the near-infrared spectral signature of disks, to learn whether young stars with little or no(More)
We report interferometric images of the UY Aur binary in 13 CO J = 1→ 0 and J = 2→ 1 which reveal evidence for a large (≥ 20) circumbinary disk around the two pre-main-sequence stars. This is the second detection of a circumbinary disk around T Tauri stars. A Keplerian rotation curve around a central mass of ∼1.2 M provides a good fit to the velocity data.(More)
The formation of planets around binary stars may be more difficult than around single stars. In a close binary star (with a separation of less than a hundred astronomical units), theory predicts the presence of circumstellar disks around each star, and an outer circumbinary disk surrounding a gravitationally cleared inner cavity around the stars. Given that(More)
We investigate the use of the gravity sensitive neutral sodium (Na i) doublet at 8183 Å and 8195 Å (Na 8200 Å doublet) as an age indicator for M dwarfs. We measured the Na doublet equivalent width (EW) in giants, old dwarfs, young dwarfs, and candidate members of the β Pic moving group using medium-resolution spectra. Our Na 8200 Å doublet EW analysis shows(More)
The young system RX J0529.3+1210 was initially identified as a single−lined spectroscopic binary. Using high−resolution infrared spectra, acquired with NIR-SPEC on Keck II, we measured radial velocities for the secondary. The method of using the infrared regime to convert single−lined spectra into double−lined spectra, and derive the mass ratio for the(More)
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