This map of Mars shows relative locations of three types of findings related to salt or frozen water, plus a new type of finding that may be related to both salt and water.
Shallow subsurface water ice found by the Gamma Ray Spectrometer and Neutron Spectrometer on NASA's Mars Odyssey orbiter is depicted in colors signifying concentrations.
The presence of hydrogen, shown in blue, signifies higher concentrations of water ice.
The white squares mark locations of impact craters in the northern hemisphere which exposed water ice close to the surface. Red squares mark locations where the Thermal Emission Imaging System on Mars Odyssey has found deposits of chlorite may have resulted from evaporation of salty water.
On Earth, chilled but unfrozen brine in rocky permafrost environments provides habitats for the growth of organisms and could provide habitats in similar conditions on Mars.
Cryopegs are isolated pockets of highly saline, liquid water that is permanently subzero (Celsius) in temperature due to chilling by the surrounding permafrost.
In this graphic, mm-cm refers to depths below the ground surface of millimeters to centimeters in vertical scale (fractions of an inch); cm-m refers to depths of centimeters to meters scale (half an inch to several yards); m-km refers to depths of meters to kilometers scale (a yard to a few miles); and 10's km refers to depth of tens of kilometers (several miles or more).
From Mars' Newton crater, at 41.6 degrees south latitude, 202.3 degrees east longitude, the HiRise Camera captured this series of images from early spring of one Mars year to mid-summer of the following year.
During warm seasons, small dark features, called recurring slope lineae, appear and incrementally grow during warm seasons and fade in cold seasons, extend downslope possibly signifying the presence of liquid water.
However, "The flows are not dark because of being wet," said Alfred McEwen of the University of Arizona. "They are dark for some other reason."
These five images were taken from early spring of one Mars year to mid-summer of the following year, during the warm season when surface temperatures range from about 10 degrees below zero Fahrenheit to 80 degrees above zero Fahrenheit.
Dark flows in Mars' Newton Crater extend downslope, right to left, from bedrock outcrops. More than 1,000 individual flows have been discovered from 0.5 to 5 yards wide with lengths hundreds of yards long.
Published:Caption:James MartinPhoto:NASA/JPL-Caltech/Univ. of Arizona
Warm-season flows in Horowitz Crater
Even in the warm season Mars is too cold for pure water. This suggests the presence of salt water, which has lower freezing points.
Salt deposits over much of Mars indicate brines were abundant in Mars' past. These recent observations suggest brines still may form near the surface today in limited times and places.
When these slopes were checked with the orbiter's Compact Reconnaissance Imaging Spectrometer for Mars (CRISM), no sign of water appeared, which means the features may either quickly dry on the surface or could be shallow subsurface flows.