Techniques d'observation spectroscopique d'astéroïdes

List of Figures
1.1 A field obtained with INT-WFC on February 28, 2012. Ten asteroids were identified
(marked with pink), from which only three were known at the moment of
the observation. The size of the field is (15 arcmin x 15 arcmin) . . . . . . . . 34
1.2 a) The position of asteroids in the inner part of the Solar System (Source:
http://en.wikipedia.org/). b)The distribution of asteroids in a representation
(a,e)- bottom and (a,sini) - top, a is the semi-major axis and i the
inclination [Nedelcu, 2010]. . . . . . . . . . . . . . . . . . . . . . . . . . . . 36
1.3 The flowchart of Mega-Precovery [Vaduvescu et al., 2012]. . . . . . . . . . . . 39
1.4 The first part of the Minor Planet Electronic Circular issued for the orbit recovery
of the asteroid 2007 ES. . . . . . . . . . . . . . . . . . . . . . . . . . . . . 41
tel-00785991, version 1 - 7 Feb 2013
2.1 The diffraction pattern produced by a diffraction grating having b=d = 5µm
and N=1000. Different wavelengths are considered. . . . . . . . . . . . . . . . 45
2.2 The atmospheric transmission above Mauna Kea for the wavelength ranges 0.9
- 2.7 µm with a water vapor column of 1.6 mm and an air mass of 1 (Source:
http://www.gemini.edu/?q=node/10789). . . . . . . . . . . . . . . 46
2.3 The field of quasar PG1634+706 (north is at bottom of the figure). The object
and its spectrum are surrounded by a rectangle. In this image it can be distinguish
the zero order (objects are dots) and the first order (light is dispersed) -
Popescu et al. [2012a]. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 48
2.4 a) PG1634 + 706 spectrum obtained after data reduction and continuum subtraction;
b) the correlation coefficient between quasar spectrum and the template
spectrum shifted with different z [Popescu et al., 2012a]. . . . . . . . . . 49
2.5 The components of the radiation received from 1km square lunar mare area
(dark basaltic plain on Moon formed by ancient volcanic eruptions) having an
albedo of 006, considering the average Earth-Moon distance, phase angle 0, T
= 395K. The flux is measured in Watts per square meter per micron. Source
McCord & Adams [1977] . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 51
2.6 Reflectance spectra of several meteoritic important minerals: a) Spinel, b) Pyroxene,
c) Olivine, d) Iron-Nickel alloy. . . . . . . . . . . . . . . . . . . . . . 52
3.1 a) The 3m NASA InfraRed Telescope Facility at the Mauna Kea Observatory
on Hawaii. b) SpeX instrument mounted to IRTF telescope. As scale, SpeX is
1.4m tall and weighs 478kg. . . . . . . . . . . . . . . . . . . . . . . . . . . . 58
3.2 The data reduction procedure for NIR spectra obtained with IRTF/SpeX [Nedelcu,
2010]. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 60