Astrophys. J., 783, L26 (2014/March-2)
Probing the gaseous disk of T Tau N with CN 5-4 lines.
PODIO L., KAMP I., CODELLA C., NISINI B., ARESU G., BRITTAIN S., CABRIT S., DOUGADOS C., GRADY C., MEIJERINK R., SANDELL G., SPAANS M., THI W.-F., WHITE G.J. and WOITKE P.
Abstract (from CDS):
We present spectrally resolved observations of the young multiple system T Tau in atomic and molecular lines obtained with the Heterodyne Instrument for the Far Infrared on board Herschel. While CO, H2O, [C II], and SO lines trace the envelope and the outflowing gas up to velocities of 33 km/s with respect to systemic, the CN 5-4 hyperfine structure lines at 566.7, 566.9 GHz show a narrow double-peaked profile centered at systemic velocity, consistent with an origin in the outer region of the compact disk of T Tau N. Disk modeling of the T Tau N disk with the thermo-chemical code ProDiMo produces CN line fluxes and profiles consistent with the observed ones and constrain the size of the gaseous disk (Rout = 110_-20+10 AU) and its inclination (i = 25°± 5°). The model indicates that the CN lines originate in a disk upper layer at 40-110 AU from the star, which is irradiated by the stellar UV field and heated up to temperatures of 50-700 K. With respect to previously observed CN 2-1 millimeter lines, the CN 5-4 lines appear to be less affected by envelope emission, due to their larger critical density and excitation temperature. Hence, high-J CN lines are a unique confusion-free tracer of embedded disks, such as the disk of T Tau N.
astrochemistry - ISM: molecules - protoplanetary disks - stars: individual: T Tau
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