Asteroid Spectroscopy

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Correction Process - I The pattern identifies presence of an offset. Channel offset determined for each set of observations relative to some reference set. Offsets are derived by using the steep edge of the 1.4 µm atmospheric water vapor feature.
Correction Process - II Offsets should be established to ~0.1-0.2 pixels. Pixel offset corrections are applied to the raw standard star spectra prior to calculation of the extinction coefficients (or their use in ratios). Pixel offset corrections are applied to the raw object spectra prior to extinction corrections.
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Lecture #2 Asteroid Spectroscopy Pr
Page 3 and 4: HAYABUSA Sample Return Mission A la
Page 5 and 6: Remote Sensing Techniques for Chara
Page 7 and 8: Why Mineralogy rather than Composit
Page 9 and 10: Mineralogical Characterizations Min
Page 11 and 12: VNIR Spectra Detection and composit
Page 13 and 14: Transition metal elements commonly
Page 15 and 16: Shell #3 Shell #2 Shell #1 Nucleus
Page 17 and 18: First Series Transition metals Peri
Page 19 and 20: In minerals, the metal cations (e.g
Page 21 and 22: Consider Fe 2+ in an octahedral sit
Page 23 and 24: ∆ O is the energy difference betw
Page 25 and 26: Most cation sites in transition met
Page 27 and 28: The result is multiple absorption f
Page 29 and 30: Spectra of different HED meteorite
Page 31 and 32: The broad 1 µm olivine feature is
Page 33 and 34: Olivine-Pyroxene Mixture Spectra Wi
Page 35 and 36: In Olivine-Pyroxene mixtures, the r
Page 37 and 38: Molecular Vibrations Also Produce S
Page 39 and 40: Some potentially important asteroid
Page 41 and 42: Mineralogical Analysis of Vesta Gaf
Page 43 and 44: Is a Thin Surface Layer Representat
Page 45 and 46: Observational Methodologies Standar
Page 47 and 48: Typical instrumental flux measureme
Page 49 and 50: Correction for extinction using a S
Page 51 and 52: Extinction correction with channel
Page 53: Implications for Analysis Irrespect
Page 57: The Upside -- Asteroid spectra obta
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Asteroid Spectroscopy

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