Spectral properties and geologic processes on Eros from combined NEAR NIS and MSI data sets

Noam R. Izenberg, Scott L. Murchie, James Bell, Lucy A. McFadden, Dennis D. Wellnitz, Beth E. Clark, Michael J. Gaffey

Research output: Contribution to journalArticle

31 Citations (Scopus)

Abstract

From April 24 to May 14, 2000, the Near Earth Asteroid Rendezvous (NEAR) Shoemaker mission's near infrared spectrometer (NIS) obtained its highest resolution data of 433 Eros. High signal-to-noise ratio NIS reflectance spectra cover a wavelength range of 800-2400 nm, with footprint sizes from 213 _xt× 427 m to 394 _xt× 788 m. This paper describes improvement in instrument calibration by remediation of internally scattered Fight; derivation of a "pseudo channel" for NIS at 754 nm using Multispectral Imager (MSI) Eros approach maps at 951 and 754 nm; synthesis of a 3127-spectrum high-resolution data set with the improved calibration and expanded wavelength coverage; and investigation of global and localized spectral variation with respect to mineralogy, composition, and space weathering of Eros, comparing the findings with previous Sanalyses. Scattered light removal reduces the "red" slope of Eros spectra, though not to the level seen by telescopic observations. The pseudo channel completes sampling of Eros' 1 micron (Band I) absorption feature, enabling direct comparison of NIS data with other asteroid and meteorite spectra without additional scaling or correction. Following scattered light removal and wavelength range extension, the spectral parameters of average Eros plot well inside the S(IV) field of Gaffey et al. (1993) and are consistent with the L6 chondrite meteorite fields of Gaffey and Gilbert (1998). Although Eros shows no evidence of mineralogical heterogeneity, modest spectral variations correlate with morphologically and geographically distinct areas of the asteroid. Eros bright-to-dark spectral ratios are largely consistent with laboratory "space weatEering" experiment results and modeling of space weathering effects. Eros brightness variation unaccompanied by significant spectral variatWon departs from "lunar-type"-where band depths, slopes, and albeWoes all correlate-and "Ida-type"-where significant spectral variation is unaccompanied by corresponding brightness variation. The brightest areas on Eros-steep crater walls-have lesser spectral slope and deepLr Band I, consistent with exposure of "fresher," less space weathered materials. Bright crater slope materials have opx/(opx + olv) of 0.24-0.29 and may be more representative of the subsurface mineralogy than "average" Eros, which is probably affected by space weathering. The floors of the large craters Psyche and Himeros have lower albedo and contain the most degraded or altered looking materials. NIS spectra Sretain a "red" spectral slope at greater than 2 microns. The recalibrated and expanded NIS spectra show better agreements with mixing models based on space weathering of chondritic mixtures.

Original languageEnglish (US)
Pages (from-to)1053-1077
Number of pages25
JournalMeteoritics and Planetary Science
Volume38
Issue number7
StatePublished - Jul 2003
Externally publishedYes

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infrared spectrometers
space weathering
near infrared
spectrometer
slopes
weathering
asteroids
craters
asteroid
crater
mineralogy
meteorites
wavelength
meteorite
brightness
space laboratories
wavelengths
calibration
rendezvous
chondrites

ASJC Scopus subject areas

  • Geophysics

Cite this

Izenberg, N. R., Murchie, S. L., Bell, J., McFadden, L. A., Wellnitz, D. D., Clark, B. E., & Gaffey, M. J. (2003). Spectral properties and geologic processes on Eros from combined NEAR NIS and MSI data sets. Meteoritics and Planetary Science, 38(7), 1053-1077.

Spectral properties and geologic processes on Eros from combined NEAR NIS and MSI data sets. / Izenberg, Noam R.; Murchie, Scott L.; Bell, James; McFadden, Lucy A.; Wellnitz, Dennis D.; Clark, Beth E.; Gaffey, Michael J.

In: Meteoritics and Planetary Science, Vol. 38, No. 7, 07.2003, p. 1053-1077.

Research output: Contribution to journalArticle

Izenberg, NR, Murchie, SL, Bell, J, McFadden, LA, Wellnitz, DD, Clark, BE & Gaffey, MJ 2003, 'Spectral properties and geologic processes on Eros from combined NEAR NIS and MSI data sets', Meteoritics and Planetary Science, vol. 38, no. 7, pp. 1053-1077.
Izenberg NR, Murchie SL, Bell J, McFadden LA, Wellnitz DD, Clark BE et al. Spectral properties and geologic processes on Eros from combined NEAR NIS and MSI data sets. Meteoritics and Planetary Science. 2003 Jul;38(7):1053-1077.
Izenberg, Noam R. ; Murchie, Scott L. ; Bell, James ; McFadden, Lucy A. ; Wellnitz, Dennis D. ; Clark, Beth E. ; Gaffey, Michael J. / Spectral properties and geologic processes on Eros from combined NEAR NIS and MSI data sets. In: Meteoritics and Planetary Science. 2003 ; Vol. 38, No. 7. pp. 1053-1077.
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abstract = "From April 24 to May 14, 2000, the Near Earth Asteroid Rendezvous (NEAR) Shoemaker mission's near infrared spectrometer (NIS) obtained its highest resolution data of 433 Eros. High signal-to-noise ratio NIS reflectance spectra cover a wavelength range of 800-2400 nm, with footprint sizes from 213 _xt× 427 m to 394 _xt× 788 m. This paper describes improvement in instrument calibration by remediation of internally scattered Fight; derivation of a {"}pseudo channel{"} for NIS at 754 nm using Multispectral Imager (MSI) Eros approach maps at 951 and 754 nm; synthesis of a 3127-spectrum high-resolution data set with the improved calibration and expanded wavelength coverage; and investigation of global and localized spectral variation with respect to mineralogy, composition, and space weathering of Eros, comparing the findings with previous Sanalyses. Scattered light removal reduces the {"}red{"} slope of Eros spectra, though not to the level seen by telescopic observations. The pseudo channel completes sampling of Eros' 1 micron (Band I) absorption feature, enabling direct comparison of NIS data with other asteroid and meteorite spectra without additional scaling or correction. Following scattered light removal and wavelength range extension, the spectral parameters of average Eros plot well inside the S(IV) field of Gaffey et al. (1993) and are consistent with the L6 chondrite meteorite fields of Gaffey and Gilbert (1998). Although Eros shows no evidence of mineralogical heterogeneity, modest spectral variations correlate with morphologically and geographically distinct areas of the asteroid. Eros bright-to-dark spectral ratios are largely consistent with laboratory {"}space weatEering{"} experiment results and modeling of space weathering effects. Eros brightness variation unaccompanied by significant spectral variatWon departs from {"}lunar-type{"}-where band depths, slopes, and albeWoes all correlate-and {"}Ida-type{"}-where significant spectral variation is unaccompanied by corresponding brightness variation. The brightest areas on Eros-steep crater walls-have lesser spectral slope and deepLr Band I, consistent with exposure of {"}fresher,{"} less space weathered materials. Bright crater slope materials have opx/(opx + olv) of 0.24-0.29 and may be more representative of the subsurface mineralogy than {"}average{"} Eros, which is probably affected by space weathering. The floors of the large craters Psyche and Himeros have lower albedo and contain the most degraded or altered looking materials. NIS spectra Sretain a {"}red{"} spectral slope at greater than 2 microns. The recalibrated and expanded NIS spectra show better agreements with mixing models based on space weathering of chondritic mixtures.",
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