Techniques d'observation spectroscopique d'astÃ©roÃ¯des

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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
tel-00785991, version 1 - 7 Feb 2013 7.3 The NIR spectra with the error-bars for (1333) Cevenola; a) obtained in March 12, 2007; b) obtained in March 13, 2007. The spectra are normalized to 1.25 µm.124 7.4 a) The visible and the averaged NIR spectrum of(1333) Cevenola; b) A polynomial fit for the V+NIR spectrum of (1333) Cevenola compared with the theoretical spectra of Sq, Q and K taxonomic types; c) the comparison between the spectrum of (1333) Cevenola and the spectrum of a sample from Saratov meteorite; d) the comparison between the spectrum of (1333) Cevenola and the spectrum of a sample from Hamlet#1 meteorite. . . . . . . . . . . . . . . . . . 125 7.5 The NIR spectra of (3623) Chaplin; a) obtained in March 12, 2007; b) obtained in March 13, 2007. The spectra are normalized to 1.25 µm. . . . . . . . . . . . 126 7.6 a) The NIR averaged spectrum of (3623) Chaplin; b) A polynomial fit for (3623) Chaplin compared with the theoretical spectra of S, Sv and Sq taxonomic types;; c) the comparison between the spectrum of (3623) Chaplin and the spectrum of a sample from igneous plutonic rock; d) the comparison between the spectrum of spectrum of (3623) Chaplin and the spectrum of a sample from low-calcium impact melt breccia rock. . . . . . . . . . . . . . . . . . 127 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. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 128 A.1 The GuideDog interface is used to control the guider system of the telescope. Source: Rayner et al. [2004]. . . . . . . . . . . . . . . . . . . . . . . . . . . . 135 A.2 The BigDog interface is used to control the spectrograph set-up and spectra acquisition. Source: Rayner et al. [2004]. . . . . . . . . . . . . . . . . . . . . 136
Page 1 and 2: OBSERVATOIRE DE PARIS ÉCOLE DOCTOR
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Page 9 and 10: Résumé: L’objectif fondamental
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5 M4AST - Modeling of Asteroids Spe
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CHAPTER 5. M4AST - MODELING OF ASTE
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6 Spectral properties of near-Earth
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7 Spectral properties of Main Belt
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CHAPTER 7. SPECTRAL PROPERTIES OF M
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A The GuideDog and the BigDog inter
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B List of publications B.1 First Au
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APPENDIX B. LIST OF PUBLICATIONS 13
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Bibliography Adams, J. B. 1974. Vis
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BIBLIOGRAPHY 143 Brunetto, R., Vern
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BIBLIOGRAPHY 145 Donnison, J. R. 19
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BIBLIOGRAPHY 149 Popescu, M., Birla
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A&A 535, A15 (2011) Table 1. Log of
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A&A 535, A15 (2011) Table 3. Summar
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Band I center [um] 1.04 1.02 1 0.98
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A&A 544, A130 (2012) DOI: 10.1051/0
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M. Popescu et al.: M4AST - Modeling
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U.P.B. Sci. Bull., Series A, Vol. 7
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Applications of optical and infrare
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Mon. Not. R. Astron. Soc. 000, 000-
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Spectral properties of (854), (1333
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Vernazza P., Mothé-Diniz T., Baruc
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Techniques d'observation spectroscopique d'astÃ©roÃ¯des

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