Techniques d'observation spectroscopique d'astéroïdes

6.5 a) The NIR spectrum of 2010 TD54; b) a polynomial fit for the spectrum of
2010 TD54 compared with the theoretical spectra of Sv, Sr and S types; c)
the reflectance spectrum of 2010 TD54 and the closest match resulting from
meteorite comparison - the L4 ordinary chondrite Saratov; d) the de-reddened
spectrum of 2010 TD54 and the closest match resulting from meteorite comparison
- the H4 ordinary chondrite Gruneberg. . . . . . . . . . . . . . . . . . 103
6.6 NIR spectrum of (164400) 2005 GN59 and its taxonomic classification. . . . . 105
tel-00785991, version 1 - 7 Feb 2013
6.7 The NIR spectrum of (5620) Jasonwheeler; b) a polynomial fit for the spectrum
of (5620) Jasonwheeler compared with the theoretical spectra of D and T
types; c) estimation of thermal flux in the spectrum of (5620) Jasonwheeler - the
dashed line indicates where a linearly extrapolated continuum would fall, the
solid line shows the presence of thermal flux; d), e), f) the reflectance spectrum
of (5620) Jasonwheeler and the closest three matches resulting from meteorite
comparison: the CM2 carbonaceous chondrite Mighei/Meghei, the CM2 carbonaceous
chondrite Cold Bokkeveld, and the CM2 carbonaceous chondrite
ALH84029 [Popescu et al., 2011]. . . . . . . . . . . . . . . . . . . . . . . . . 107
6.8 Visible [Binzel et al., 2004a] and NIR spectrum of 2001 SG286. A linear fit
and the D-type theoretical spectrum are plotted for comparison. . . . . . . . . . 108
6.9 a) Wavelength position of the centers of the two absorption bands computed
using Cloutis et al. [1986a]. The regions enclosed correspond to the band centers
computed for the H, L, and LL chondrites, respectively [de León et al.,
2010]; b) BAR versus band I centers. The regions enclosed by continuous lines
correspond to the values computed for basaltic achondrites, ordinary chondrites(OC),
and olivine-rich meteorites(Ol) [Gaffey et al., 1993b]. . . . . . . . 109
7.1 a) Spectrum of (9147) Kourakuen normalized to 1.25 µm; b) a polynomial fit of
the spectrum of (9147) Kourakuen compared with the theoretical spectra of V,
Sv, and Sr types; c) the comparison between the spectrum of (9147) Kourakuen
and the spectrum of a sample from Pavlovka, d) the comparison between the
spectrum of (9147) Kourakuen and the spectrum of a mixture of Pyroxene-
Hypersthene-Plagioclase-Bytownite-Ilmenite. . . . . . . . . . . . . . . . . . . 116
7.2 a) The visible and NIR spectrum of (854) Frostia; b) A polynomial fit for the
spectrum of (854) Frostia compared with the theoretical spectra of V, Sv and
Sr types; c) the comparison between the spectrum of (854) Frostia and the
spectrum of a sample from ”ALHA76005,85” meteorite; d) the comparison
between the spectrum of (854) Frostia and the spectrum of a sample from Y −
793591,90 meteorite. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 120