1 CO2 is inferred on the surface of Ganymede by the presence of
an absorption band at -4.26 mum in reflectance spectra returned by
the Near Infrared Mapping Spectrometer (NIMS) aboard the Galileo
spacecraft. Detailed studies of NIMS observations of Ganymede show
that the CO2 absorption band on Ganymede is symmetric about 4.257
mum +/- 0.004 mm and is negligibly different from the CO2 absorption
band on Callisto. In general, bright terrains (sulci) contain less
CO2 than dark terrains (regiones), little or no CO2 is detected at
the poles, and, unlike for Callisto, there does not appear to be
any leading/trailing hemisphere asymmetry in the distribution of
CO2 nor do impact craters tend to be CO2 rich. High spatial resolution
observations show that CO2 is occasionally enriched in terrain containing
larger-grained ice in comparison with adjacent terrain of similar
morphology and ice abundance, that the dark ejecta of Kittu is depleted
in CO2 with respect to adjacent terrain, and that only one observed
impact crater (Mir) is enriched in CO2. The CO2 that is detected
by NIMS is in the nonice material(s) present, not in the fraction
that is ice. The ice in all terrain types where CO2 is detected is
always sufficiently large-grained that its low reflectance in the
region of the CO2 band prevents discrimination of the CO2 absorption
band from the continuum. Areas with relatively fine-grained ice that
are sufficiently bright at 4 mm for CO2 to be observed, such as the
polar regions, do not contain detectable CO2.
%0 Journal Article
%1 Hibbitts2003
%A Hibbitts, C. A.
%A Pappalardo, R. T.
%A Hansen, G. B.
%A McCord, T. B.
%D 2003
%J Journal of Geophysical Research-Planets
%K EVOLUTION EXTENSIONAL FROST; GALILEAN GROOVED HIGH-RESOLUTION; ICY INSTABILITY; JUPITER; SATELLITES; SPECTROMETER; SURFACE; TERRAIN; WATER-ICE;
%N E5
%P 5036
%T Carbon dioxide on Ganymede
%V 108
%X 1 CO2 is inferred on the surface of Ganymede by the presence of
an absorption band at -4.26 mum in reflectance spectra returned by
the Near Infrared Mapping Spectrometer (NIMS) aboard the Galileo
spacecraft. Detailed studies of NIMS observations of Ganymede show
that the CO2 absorption band on Ganymede is symmetric about 4.257
mum +/- 0.004 mm and is negligibly different from the CO2 absorption
band on Callisto. In general, bright terrains (sulci) contain less
CO2 than dark terrains (regiones), little or no CO2 is detected at
the poles, and, unlike for Callisto, there does not appear to be
any leading/trailing hemisphere asymmetry in the distribution of
CO2 nor do impact craters tend to be CO2 rich. High spatial resolution
observations show that CO2 is occasionally enriched in terrain containing
larger-grained ice in comparison with adjacent terrain of similar
morphology and ice abundance, that the dark ejecta of Kittu is depleted
in CO2 with respect to adjacent terrain, and that only one observed
impact crater (Mir) is enriched in CO2. The CO2 that is detected
by NIMS is in the nonice material(s) present, not in the fraction
that is ice. The ice in all terrain types where CO2 is detected is
always sufficiently large-grained that its low reflectance in the
region of the CO2 band prevents discrimination of the CO2 absorption
band from the continuum. Areas with relatively fine-grained ice that
are sufficiently bright at 4 mm for CO2 to be observed, such as the
polar regions, do not contain detectable CO2.
@article{Hibbitts2003,
abstract = {[1] CO2 is inferred on the surface of Ganymede by the presence of
an absorption band at -4.26 mum in reflectance spectra returned by
the Near Infrared Mapping Spectrometer (NIMS) aboard the Galileo
spacecraft. Detailed studies of NIMS observations of Ganymede show
that the CO2 absorption band on Ganymede is symmetric about 4.257
mum +/- 0.004 mm and is negligibly different from the CO2 absorption
band on Callisto. In general, bright terrains (sulci) contain less
CO2 than dark terrains (regiones), little or no CO2 is detected at
the poles, and, unlike for Callisto, there does not appear to be
any leading/trailing hemisphere asymmetry in the distribution of
CO2 nor do impact craters tend to be CO2 rich. High spatial resolution
observations show that CO2 is occasionally enriched in terrain containing
larger-grained ice in comparison with adjacent terrain of similar
morphology and ice abundance, that the dark ejecta of Kittu is depleted
in CO2 with respect to adjacent terrain, and that only one observed
impact crater (Mir) is enriched in CO2. The CO2 that is detected
by NIMS is in the nonice material(s) present, not in the fraction
that is ice. The ice in all terrain types where CO2 is detected is
always sufficiently large-grained that its low reflectance in the
region of the CO2 band prevents discrimination of the CO2 absorption
band from the continuum. Areas with relatively fine-grained ice that
are sufficiently bright at 4 mm for CO2 to be observed, such as the
polar regions, do not contain detectable CO2.},
added-at = {2009-11-03T20:21:25.000+0100},
author = {Hibbitts, C. A. and Pappalardo, R. T. and Hansen, G. B. and McCord, T. B.},
biburl = {https://www.bibsonomy.org/bibtex/214bf0616427472f2502eb2512dbf6d43/svance},
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interhash = {089f6230a0d278c7186bb50d8c751c40},
intrahash = {14bf0616427472f2502eb2512dbf6d43},
journal = {Journal of Geophysical Research-Planets},
keywords = {EVOLUTION EXTENSIONAL FROST; GALILEAN GROOVED HIGH-RESOLUTION; ICY INSTABILITY; JUPITER; SATELLITES; SPECTROMETER; SURFACE; TERRAIN; WATER-ICE;},
number = {E5},
owner = {svance},
pages = 5036,
timestamp = {2009-11-03T20:21:51.000+0100},
title = {Carbon dioxide on Ganymede},
volume = 108,
year = 2003
}