Near-IR Spectroscopy and Imaging Polarimetry of RNO 91: Detection of Frozen H_2O, CO, and X(Cequiv N) In A Circumstellar Disk

Details Near-IR Spectroscopy and Imaging Polarimetry of RNO 91: Detection of Frozen H_2O, CO, and X(Cequiv N) In A Circumstellar Disk Near-IR Spectroscopy and Imaging Polarimetry of RNO 91: Detection of Frozen H_2O, CO, and X(Cequiv N) In A Circumstellar Disk

Dec 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992aas...18111403t&link_type=abstract

American Astronomical Society, 181st AAS Meeting, #114.03; Bulletin of the American Astronomical Society, Vol. 24, p.1301

Astronomy and Astrophysics

Astronomy

Scientific paper

We describe the results of a 3.0 to 5.0 microns spectroscopic study of the circumstellar disk around the T Tauri star RNO 91. The spectra were obtained with the CGAS spectrometer and the 3.0-m NASA Infrared Telescope Facility on Mauna Kea. The spectra show broad absorption bands centered at 3.05 microns (3275 cm(-1) ) and 4.62 microns (2167 cm(-1) ). A narrower absorption band is also present at 4.67 microns (2140 cm(-1) ). Imaging polarimetry at 2.2 microns demonstrates that RNO 91 has a large (2000 AU) flared disk that is optically thick out to lambda >= 2 microns and that most of the line-of-sight extinction toward RNO 91 is local, within the circumstellar disk. Thus, we conclude that the solid phase absorption bands likely result from absorption by material in the disk around RNO 91. By comparing the spectra of RNO 91 with spectra of laboratory ice analogs, we find the broad 3.05 and 4.62 microns bands are consistent with frozen H_2O and an unidentified -Cequiv N containing material X(Cequiv N), respectively. The X(Cequiv N) band has been seen previously only in the circumstellar shells around the protostars W33A and NGC7538 IRS9 (Lacy et al. 1984, ApJ. 276, 533) and the FU Orionis star L1551 IRS 5 (Tegler et al. 1992, ApJ., submitted). Laboratory experiments show that X(Cequiv N) is a somewhat refractory component produced by ultraviolet irradiation or ion bombardment of simple C and N bearing ices. The narrower absorption band at 4.67 microns is apparently due to absorption by frozen CO. We present the abundance of frozen CO and X(Cequiv N) relative to frozen H_2O in the disk around RNO 91 and discuss the implications of these abundances on comet formation.

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