Techniques d'observation spectroscopique d'astéroïdes
Techniques d'observation spectroscopique d'astéroïdes
Techniques d'observation spectroscopique d'astéroïdes
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CHAPTER 7. SPECTRAL PROPERTIES OF MAIN BELT ASTEROIDS 125<br />
Relative Reflectance<br />
(a)<br />
1.2<br />
1.15<br />
1.1<br />
1.05<br />
1<br />
0.95<br />
0.9<br />
0.85<br />
0.8<br />
0.75<br />
0.7<br />
(1333) Cevenola :V<br />
(1333) Cevenola :NIR<br />
0.5 1 1.5 2 2.5<br />
Wavelength [um]<br />
Relative Reflectance<br />
(b)<br />
1.2<br />
1.15<br />
1.1<br />
1.05<br />
1<br />
0.95<br />
0.9<br />
0.85<br />
0.8<br />
Cevenola<br />
0.75<br />
Sq<br />
Q<br />
0.7<br />
K<br />
0.5 1 1.5 2 2.5<br />
Wavelength [um]<br />
0.23<br />
0.22<br />
0.25<br />
0.24<br />
tel-00785991, version 1 - 7 Feb 2013<br />
Relative Reflectance<br />
(c)<br />
0.21<br />
0.2<br />
0.19<br />
0.18<br />
0.17<br />
0.16<br />
Cevenola<br />
Saratov met.<br />
0.5 1 1.5 2 2.5<br />
Wavelength [um]<br />
Relative Reflectance<br />
(d)<br />
0.23<br />
0.22<br />
0.21<br />
0.2<br />
0.19<br />
0.18<br />
Cevenola<br />
Hamlet #1 met.<br />
0.5 1 1.5 2 2.5<br />
Wavelength [um]<br />
Figure 7.4: a) The visible and the averaged NIR spectrum of(1333) Cevenola; b) A polynomial fit for the V+NIR<br />
spectrum of (1333) Cevenola compared with the theoretical spectra of Sq, Q and K taxonomic types; c) the<br />
comparison between the spectrum of (1333) Cevenola and the spectrum of a sample from Saratov meteorite; d)<br />
the comparison between the spectrum of (1333) Cevenola and the spectrum of a sample from Hamlet#1 meteorite.<br />
ering model proposed by Brunetto et al. [2006]. Thus, fitting the spectrum with an exponential<br />
continuum I found C s = -0.133 µm, corresponding to a relatively fresh surface. The C s value<br />
gives the number of displacements per cm 2 , d = 0.45×10 19 displacements/cm 2 .<br />
Comparing the original spectrum of (1333) Cevenola with all laboratory spectra from Relab,<br />
M4AST found matches with ordinary chondrite meteorites (L and LL subtypes, and petrologic<br />
classes 4 and 5). In terms of standard deviation and correlation coefficient, the best matches<br />
where those of samples from Saratov, Hamlet #1 (Fig. 7.4) and Paranaiba. These meteorites<br />
are ordinary chondrites with low iron content.<br />
I compared also the de-reddened spectrum of (1333) Cevenola to laboratory spectra from<br />
Relab. In this case, the four methods used give relatively different solutions. The spectral<br />
solutions that can be selected are the spectrum of a sample from Denver meteorite and the<br />
spectrum of a sample from Hamlet #1 meteorite. Both meteorites are ordinary chondrites with<br />
low iron content.
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