Techniques d'observation spectroscopique d'astéroïdes

128 CHAPTER 7. SPECTRAL PROPERTIES OF MAIN BELT ASTEROIDS
rock brought by Apollo 14 mission. A meteorite spectrum that seems to match this asteroid
spectrum is that of an Achondrite - Ureilite type, PCA82506,80.
Applying de-reddening model, it can be found that it is characterized by a low spaceweathering
effect ( Cs = -0.157 µm). This small value of Cs can be explained by the fact
that (3623) Chaplin resides in the outer part of the Main Belt, being less affected by the solar
wind ion radiation. After removing the exponential continuum, the laboratory spectra that
match this spectrum are those of a sample from Fayetteville meteorite - an ordinary chondrite
meteorite and a Igneous Plutonic rock.
(1333) Cevenola and (3623) Chaplin were observed over two consecutive nights in order
to detect spectral variations in their spectra. Their correspondent spectra has the same profile,
which is interpreted as a homogeneity of the surfaces of each object.
tel-00785991, version 1 - 7 Feb 2013
Relative Reflectance
2.4
2.2
2
1.8
1.6
1.4
1.2
1
0.8
0.6
0.4
(a)
(10484) Hecht
0.8 1 1.2 1.4 1.6 1.8 2 2.2 2.4
Wavelength [um]
Relative Reflectance
1.3
1.2
1.1
1
0.9
0.8
0.7
0.6
0.5
(b)
(31569) 1999FL18
0.8 1 1.2 1.4 1.6 1.8 2 2.2 2.4
Wavelength [um]
1.4
1.1
1.3
1.2
1
Relative Reflectance
1.1
1
0.9
0.8
0.7
0.6
0.5
Hecht
V
Sv
Sr
Relative Reflectance
0.9
0.8
0.7
0.6
0.5
1999 FL18
V
Sv
Sr
0.8 1 1.2 1.4 1.6 1.8 2 2.2 2.4
Wavelength [um]
0.8 1 1.2 1.4 1.6 1.8 2 2.2 2.4
Wavelength [um]
(c)
(d)
Figure 7.7: The NIR spectra of a) (10484) Hecht and b) (31569) 1999 FL18. Both spectra are normalized to 1.25
µm.Taxonomic classification of c) (10484) Hecht and d) (31569) 1999 FL18.