Techniques d'observation spectroscopique d'astéroïdes

CHAPTER 5. M4AST - MODELING OF ASTEROIDS SPECTRA 87
Relative Reflectance
0.21
0.2
0.19
0.18
0.17
Relative Reflectance
0.23
0.22
0.21
0.2
0.19
0.18
tel-00785991, version 1 - 7 Feb 2013
(a)
Relative Reflectance
(c)
Relative Reflectance
0.16
0.15
0.34
0.33
0.32
0.31
0.29
0.28
0.27
0.26
Apophis
Lunar soil
0.5 1 1.5 2 2.5
Wavelength [um]
0.3
0.095
0.09
0.085
0.08
Apophis de−red.
Cherokee Springs met.
1 1.5 2 2.5
Wavelength [um]
(b)
Relative Reflectance
(d)
Relative Reflectance
0.17
Apophis
0.16
Hamlet met.
0.5 1 1.5 2 2.5
Wavelength [um]
0.185
0.18
0.175
0.17
0.165
0.16
0.155
0.15
0.145
0.14
0.074
0.072
0.07
0.068
0.066
0.064
0.062
0.06
Apophis de−red.
Cat Mountain met.
1 1.5 2 2.5
Wavelength [um]
(e)
0.075
1996 FG3
Sete Lagoas met.
0.5 1 1.5 2 2.5
Wavelength [um]
(f)
0.058
0.056
0.054
1996 FG3
Murchison met.
0.5 1 1.5 2 2.5
Wavelength [um]
Figure 5.8: Asteroid spectra and the best two matches derived from a comparison with laboratory spectra:(a)
spectrum of Apophis and the spectrum of a simulant Lunar soil, (b) spectrum of Apophis and the spectrum of
a particulate sample from the Hamlet meteorite, (c) de-reddened spectrum of Apophis and the spectrum of a
particulate sample from the Cherokee Springs meteorite, (d) de-reddened spectrum of Apophis and the spectrum
of a particulate sample from the Cat Mountain meteorite, (e) spectrum of 1996 FG3 and the spectrum of a sample
from the meteorite Sete Lagoas, and (f) spectrum of 1996 FG3 and the spectrum of a sample from the Murchison
meteorite heated to 1000 ◦ C.