Techniques d'observation spectroscopique d'astéroïdes

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. . . . . . . . . . . 87
tel-00785991, version 1 - 7 Feb 2013
6.1 a) The visible [Binzel et al., 2004b] and the NIR spectrum of (1917) Cuyo; b)
a polynomial fit of the V+NIR spectrum of (1917) Cuyo compared with the
theoretical spectra of R and Sr types; c) reflectance spectrum of (1917) Cuyo
and the closest match resulting from meteorite comparison - H3-4 ordinary
chondrite Dhajala; d) De-reddened spectrum of (1917) Cuyo and the closest
match resulting from meteorite comparison, H6 ordinary chondrite Lancon. . . 96
6.2 a) The visible [Vernazza, 2006] and the NIR spectra of (8567) 1996 HW1; b) a
polynomial fit of the V+NIR spectrum of (8567) 1996 HW1 compared with the
theoretical spectra of S and Sq types; c) reflectance spectrum of (8567) 1996
and the closest match resulting from the meteorite comparison - the LL4 ordinary
chondrite Hamlet; d) de-reddened spectrum of (8567) 1996 HW1 and the
closest match resulting from meteorite comparison -the LL6 ordinary chondrite
Cherokee Springs. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 98
6.3 a) The visible [Binzel et al., 2004b] and the NIR spectra of (16960) 1998 QS52;
b) a polynomial fit of the V+NIR spectrum of (16960) 1998 QS52 compared
with the theoretical spectra of Sr, Sq and Q types; c) the reflectance spectrum
of (16960) 1998 QS52 and the closest fit resulting from spectral comparison
- the L4 ordinary chondrite Saratov; d) the de-reddened spectrum of (16960)
1998 QS52 and the closest fit resulting from meteorite comparison - the LL4
ordinary chondrite Hamlet. . . . . . . . . . . . . . . . . . . . . . . . . . . . . 100
6.4 a) The NIR spectrum of (188452) 2004 HE62 normalized to 1.25 µm; b) a
polynomial fit for the spectrum of (188452) 2004 HE62 compared with the
theoretical spectra of Sr and Sv types; c) the reflectance spectrum of (188452)
2004 HE62 and the closest fit resulting from meteorite spectra comparison -
the L6 ordinary chondrite La Criolla; d) the de-reddened spectrum of (188452)
2004 HE62 and the closest matches resulting from meteorite comparison - the
H6 ordinary chondrite Nanjemoy. . . . . . . . . . . . . . . . . . . . . . . . . 102