The 5-micron spectrum of Uranus: A search for CO and PH3

Details The 5-micron spectrum of Uranus: A search for CO and PH3 The 5-micron spectrum of Uranus: A search for CO and PH3

Apr 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003eaeja.....2132e&link_type=abstract

EGS - AGU - EUG Joint Assembly, Abstracts from the meeting held in Nice, France, 6 - 11 April 2003, abstract #2132

Computer Science

Scientific paper

As in the case of Jupiter and Saturn, the flux of Uranus at 5 microns is expected to come from deep atmospheric layers, at pressures above 1 bar. This spectral range thus looks appropriate for searching minor tropospheric species such as CO and PH3 which, in addition to CH3D, have spectral signatures at these wavelengths. Due to the relatively low tropospheric temperatures of Uranus, the flux at these wavelengths is probably due to reflected sunlight, rather than thermal emission. The 5-mu spectrum of Uranus was first detected at low spectral resolution (R=50) by Orton and Kaminski (Icarus 77, 109, 1989). The spectrum was again measured between 4.6 and 5.1 microns using the SpeX instrument at the NASA Infrared Telescope Facility (IRTF), in September 2000 and September 2001. The slit width was 0.8 arcsec, corresponding to a resolving power of 1000. H3+ emission lines were also detected in this spectral range, but the signal-to-noise ratio was low in the continuum. In October and November 2002, the spectrum of Uranus was again recorded in the 4.6-5.0 microns range, using the ISAAC imaging spectrometer at the UT1 (ANTU) of the Very Large Telescope (European Southern Observatory, Chile). The slit width was 2 arcsec, corresponding to a resolving power of 1500. The data will be compared with synthetic models in an attempt to derive constraints on the tropospheric abundances of CO and PH3.

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