Rosetta-- Geomorphology
Read MoreBase Map for Agilkia Landing Site Geomorph Information
This is the same base map used for the Geomorphologic / Terrain study but not annotated.
The base image is an OSIRIS image montage taken on 14 September 2014 from a distance of about 30 km with an image scale is 0.5 m/pixel.
Image Source: ESA/Rosetta/OSIRIS CC: BY-SA IGO 3.0
http://creativecommons.org/licenses/by-sa/3.0/igo/Preliminary Geologic Map of the Agilkia landing site for Philae
This is a Geomorphologic / Terrain study map of the area surrounding the ladning site for the Philse Lander of the Rosetta Mission.
The base image is an OSIRIS image montage taken on 14 September 2014 from a distance of about 30 km with an image scale is 0.5 m/pixel.
The Geologic and Terrain interpretations are by Bill Harris
Image Source: ESA/Rosetta/OSIRIS CC: BY-SA IGO 3.0
http://creativecommons.org/licenses/by-sa/3.0/igo/Navcam View of Agilkia area
ESA-generated montage of 6 November 14 Navcam images. Enhanced and annotated by Bill Harris.
SOURCE: ESA/ROSETTA/
"ESA_Rosetta_NAVCAM_141106_Mosaic"
CC: BY-SA IGO 3.0
http://creativecommons.org/licenses/by-sa/3.0/igo/
Enhancements and annotation (c) Bill HarrisGeomorphology of the Agilkia landing site
A discussion of the geology and morphology of the (nominal) Philae landing site on the Smaller Lobe of Comet 67P/C-G. From the examination of Rosetta's Navcam and OSIRIS imagery an interpretation of the nature and causes of the surface features can be made.
The following features will be discussed in separate image poster-presentations:
Landing site
"Effusive" deposits
Residual scree
Plumed deposits
Pitted terrain
Image source: ESA/Rosetta mission
Data interpretation: Bill HarrisProcessed Color Image of 67P/C-G
This is a processed version of an image--
Paper_22395_abstract_18425_0.png
contained in the abstract of a paper given at the AGU 2014 Fall Meeeting:
P41C-3942
Color Variegation on 67P/Churyumov-Gerasimenko
Stubbe Hviid, et al
It has been processed to eliminate the masking color of the overlying dust and emphasize the variations of the underlying features. In this way, the spectral signature of the surface materials of the comet can be evaluated.
Image Source: ESA/Rosetta/OSIRIS/DLR