Visible near-infrared (Vis–NIR) reflectance spectroscopy is a powerful nondestructive technique allowing the parent bodies identification of cosmomaterials such as meteorites, micrometeorites, and interplanetary dust particles (IDPs) studied in the laboratory. Previous studies showed that meteorites do not represent the full diversity of the solar system small bodies. We present here an experimental setup we developed for measuring Vis–NIR microspectroscopy of individual IDPs. We acquired diffuse Vis–NIR reflectance spectra of 15 particles ranging 7–31 μm in size. We discuss the requirements, the abilities, as well as the limitations of the technique. For sizes smaller than 17 μm, the slopes increase with decreasing particles sizes, while for sizes larger than 17 μm, the slopes are randomly distributed. The visible reflectance levels do not appear to be affected by the size of the IDPs, and show a bimodal distribution. Among the studied particles, we identified an IDP (L2079C18) exhibiting a feature at 0.66 μm, which is similar to the one observed by remote sensing on the surface of hydrated asteroids. This is the first detection of a hydration band in the reflectance spectrum of an IDP that could indicate a possible link between hydrated IDPs with hydrated asteroid surfaces.

可见近红外（Vis–NIR）反射光谱法是一种强大的无损检测技术，可让母体识别实验室中研究的宇宙材料，如陨石，微陨石和行星际尘埃粒子（IDP）。先前的研究表明，陨石并不代表太阳系小天体的全部多样性。我们在这里介绍了我们开发的用于测量单个IDP的Vis-NIR显微光谱的实验装置。我们获得的颗粒15 7-31范围内的漫反射可见-近红外反射光谱μ在大小为m。我们讨论了该技术的要求，能力和局限性。对于尺寸小于17小μ m，则斜率随颗粒尺寸的增加，而对于尺寸大于17 μm，坡度是随机分布的。可见反射率水平似乎不受IDP大小的影响，并显示双峰分布。在所研究的颗粒，我们确定了在0.66表现出特征的IDP（L2079C18）μ米，这类似于由遥感水合小行星的表面上观察到的。这是在IDP反射光谱中首次检测到水合带，这可能表明水合IDP与水合小行星表面之间可能存在联系。