Abstract
The Clementine UVVIS camera returned over half a million images while in orbit around the Moon in 1994. Since the Clementine mission, our knowledge of lunar topography, gravity, and the location of features on the surface has vastly improved with the success of the Gravity Recovery and Interior Laboratory (GRAIL) mission and ongoing Lunar Reconnaissance Orbiter (LRO) mission. In particular, the Lunar Reconnaissance Orbiter Camera (LROC) has returned over a million images of the Moon since entering orbit in 2009. With the aid of improved ephemeris and on-orbit calibration, the LROC team created a series of precise and accurate global maps. With the updated reference frame, older lunar maps, such as those generated from Clementine UVVIS images, are misaligned making cross-mission analysis difficult. In this study, we use feature-based matching routines to refine and recalibrate the interior and exterior orientation parameters of the Clementine UVVIS camera. After applying these updates and rigorous orthorectification, we are able generate precise and accurate maps from UVVIS images to help support lunar science and future cross-mission investigations.
Highlights
1.1 BackgroundIn 1994, the Clementine mission launched as part of a joint program between the Strategic Defense Initiative Organization and NASA (Nozette et al, 1994)
In the late 1990’s the United States Geologic Survey (USGS) and the RAND Corporation used over 500,000 match points to systematically control 43,871 images used in the 750 nm global basemap (Davies et al, 1996; Edwards et al, 1996; McEwen and Robinson, 1997) to create the Clementine Lunar Control Network (CLCN)
In order to improve the observational geometry of each Clementine UVVIS image, we have developed a processing pipeline that provides statistics needed to refine the interior and exterior orientation parameters
Summary
In 1994, the Clementine mission launched as part of a joint program between the Strategic Defense Initiative Organization and NASA (Nozette et al, 1994). In the late 1990’s the United States Geologic Survey (USGS) and the RAND Corporation used over 500,000 match points to systematically control 43,871 images used in the 750 nm global basemap (Davies et al, 1996; Edwards et al, 1996; McEwen and Robinson, 1997) to create the Clementine Lunar Control Network (CLCN) This analysis ignored topographic effects during the triangulation (i.e. assumed a spherical Moon with a radius of 1737.4 km) and later investigations showed the existence of large horizontal offsets (8-10 km) in the resulting maps due to extreme changes in the camera orientation parameters (Cook et al, 2002). We are using images acquired by the Lunar Reconnaissance Orbiter (LRO) to update the Clementine UVVIS internal and external orientation parameters in order to create precise and accurate map products
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