2:15 PM - 2:30 PM
[PPS04-03] Reflectance spectra of carbonaceous chondrites and their dependence on incidence angle
Keywords:Martian Moons, Reflection spectral, carbonaceous chondrites
Martian Moons eXploration (MMX) aims to elucidate the origin of the two Martian satellites, Phobos and Deimos, and provide new insights into the planetary formation process. We will conduct one sample return for the red region and one for the blue area of Phobos, and remote sensing observations for Deimos.
This spacecraft will be equipped with a wide-angle spectroscopic camera (OROCHI). This camera consists of eight wide-angle cameras, seven of which are equipped with bandpass filters to observe the surface of Phobos and Deimos at seven wavelengths: 390nm, 480nm, 550nm, 650nm, 730nm, 860nm, and 950nm, and adjusted to focus on the satellite surface at 20 km from the satellite. And the remaining one has a 550nm bandpass filter on it, adjusted to be in focus when it lands.
To determine the sampling site by OROCHI, we have to obtain the reflection spectrum of the site and know whether it is red or blue in advance. On the other hand, even if the surface material is the same, the reflection spectrum may change depending on the surface condition of the observation area. One possible reason for this is the spectral dependence of the reflection properties of minerals. If this phenomenon occurs, there will be no significant difference when observing the spectra of red and blue regions. Therefore, it is essential to clarify the relationship between the surface condition of minerals and the way the observed spectrum changes.
In this study, we checked whether the spectra obtained from spectroscopic observations of meteorite samples changed or not by changing the incidence and reflection angles while keeping the phase angle (light source - observation sample - camera) fixed. In this presentation, we will report on the changes in the reflection spectra of carbonaceous chondrites and their causes.
This spacecraft will be equipped with a wide-angle spectroscopic camera (OROCHI). This camera consists of eight wide-angle cameras, seven of which are equipped with bandpass filters to observe the surface of Phobos and Deimos at seven wavelengths: 390nm, 480nm, 550nm, 650nm, 730nm, 860nm, and 950nm, and adjusted to focus on the satellite surface at 20 km from the satellite. And the remaining one has a 550nm bandpass filter on it, adjusted to be in focus when it lands.
To determine the sampling site by OROCHI, we have to obtain the reflection spectrum of the site and know whether it is red or blue in advance. On the other hand, even if the surface material is the same, the reflection spectrum may change depending on the surface condition of the observation area. One possible reason for this is the spectral dependence of the reflection properties of minerals. If this phenomenon occurs, there will be no significant difference when observing the spectra of red and blue regions. Therefore, it is essential to clarify the relationship between the surface condition of minerals and the way the observed spectrum changes.
In this study, we checked whether the spectra obtained from spectroscopic observations of meteorite samples changed or not by changing the incidence and reflection angles while keeping the phase angle (light source - observation sample - camera) fixed. In this presentation, we will report on the changes in the reflection spectra of carbonaceous chondrites and their causes.