1. Response to Comment on “Athabasca Valles, Mars: A Lava-Draped Channel System”
by W. L. Jaeger, L. P. Keszthelyi, A. S. McEwen, T. N. Titus, C. M. Dundas, and P. S. Russell
Science
Volume 320(5883):1588c-1588c
June 20, 2008
Published by AAAS

2. Fig. 1. Viking Mars Digital Image Model mosaic of Elysium and Amazonis planitiae, Mars.
Viking Mars Digital Image Model mosaic of Elysium and Amazonis planitiae, Mars. The giant shield volcanoes Elysium Mons and Olympus Mons are labeled, as is the Athabasca Valles channel system. The study area depicted in figure 1 of Jaeger et al. (1) is outlined by a black box. The locations of MOC images R , R , and S [and, therefore, of figure 1, F to I, of Page (5)] are indicated by a black star.
W. L. Jaeger et al. Science 2008;320:1588c
Published by AAAS

3. Fig. 2. Subsection of HiRISE image PSP_002292_1875 showing two impact craters (A and B) and several RMLs. The gray box indicates the location of figure 1A of Page (5).
Subsection of HiRISE image PSP_002292_1875 showing two impact craters (A and B) and several RMLs. The gray box indicates the location of figure 1A of Page (5). The irregular shape of these craters is not indicative of postimpact modification. Rather, it is a characteristic of secondaries formed by the relatively low-velocity, low-energy impact of ejecta from a nearby larger crater, probably Zunil (9).
W. L. Jaeger et al. Science 2008;320:1588c
Published by AAAS