Sedimentary Deposits within Ius Chasma
NASA/JPL-Caltech/UArizona
Sedimentary Deposits within Ius Chasma
ESP_040976_1725  Science Theme: Sedimentary/Layering Processes
Sedimentary deposits are common within Valles Marineris. Most of the larger chasmata contain kilometer-thick light-toned layered deposits composed of sulfates. However, some of the chasmata, like Ius Chasma shown in this HiRISE image, either lack these deposits or have much thinner deposits.

The light-toned deposits in Ius Chasma are observed both along the floor and inner wallrock materials. Some of the light-toned deposits appear to post-date formation of the chasma floor, whereas other deposits appear to lie beneath wallrock materials, indicating they are older. By examining the stratigraphy using digital terrain models and 3D images, it should be possible to decipher the relative ages of the different geologic units. CRISM data may also provide insight into the mineralogy, which will tell scientists about the aqueous conditions that emplaced the light-toned deposits.

Written by: Cathy Weitz (audio: Tre Gibbs)  (15 July 2015)
 
Acquisition date
24 April 2015

Local Mars time
14:19

Latitude (centered)
-7.245°

Longitude (East)
276.247°

Spacecraft altitude
261.8 km (162.7 miles)

Original image scale range
26.7 cm/pixel (with 1 x 1 binning) so objects ~80 cm across are resolved

Map projected scale
25 cm/pixel and North is up

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Equirectangular

Emission angle
9.0°

Phase angle
25.6°

Solar incidence angle
35°, with the Sun about 55° above the horizon

Solar longitude
331.2°, Northern Winter

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North azimuth:  97°
Sub-solar azimuth:  355.9°
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POSTSCRIPT
NASA’s Jet Propulsion Laboratory, a division of the California Institute of Technology in Pasadena, Calif., manages the Mars Reconnaissance Orbiter for NASA’s Science Mission Directorate, Washington. The HiRISE camera was built by Ball Aerospace and Technology Corporation and is operated by the University of Arizona.