Global MOLA Map of Mars for ITW by Constantine Thomas
NOTE: This map was constructed using the MOLA 1/32nd degree global topography map (with reference to higher resolution 1/64th degree maps), rendered using POVRay 3.02 by Constantine Thomas. The sea levels and features shown on this map and the Marineris Map are based on accurate topographic data, and are provided as an optional replacement for the maps in ITW. However, they are NOT official, and are not canonical - they're just an option for you to use!
(left-click on image to view larger version.)
Click here for MOLA Marineris Map
(Green Numbered Dots)
(White Lettered Dots)
(White Numbered Dots)
- Acheron Fossae
- Olympus Mons
- Alba Patera
- Arsia Mons
- Pavonis Mons
- Ascraeus Mons
- Kasei Vallis
- Elysium Mons
- Hecates Tholus
- Albor Tholus*
- Tartarus Montes*
- Orcus Patera
- Apollinaris Patera*
- Nix Olympica
- Zeus Tourist Resort
- As Sulyami
- Dao City
- Stygis Ciudad
- Ica Nova
- Liu Hsin
*: This feature is spelt incorrectly on the ITW Map.
**: Agassiz Crater is not shown on the ITW map - I've added it here since it's more obvious than nearby Heaviside crater.
bold type: These settlements have been moved since they would otherwise be underwater on this map.
EXPLANATION AND NOTES
The sea level for the Borealis and Hellas Seas was set on this map (and the Marineris Map) at 4.6 km above the lowest point on Mars. This is the lowest sea level at which it is still possible to flood the Chryse, Amazonis and Adamas Bays all at the same time - note however that the shorelines on this map (which follow the topographic contours) are significantly different to the shorelines shown on the ITW map (ITW18-19, shown as a Green Outline here) that are based on older, incorrect data. This level is assumed to be the level of the Water Table over the whole planet - the Marineris sea levels are higher than this but are assumed to be contained within Marineris, presumably by faulting or impermeable rock layers.
There are a number of important differences between this map and the ITW map:
The Borealis Sea is continuous around the planet. It is impossible for the Borealis to have the gap in it shown in ITW while still being able to flood any of the bays.
The Borealis Sea shorelines extend further south across the planet. The settlement of Dayville (G) had to be moved to avoid being submerged.
All three bays (Chryse, Amazonis and Adamas) are much larger. The settlements of Clarke (H) and Moyobamba (J) had to be moved to the shoreline to avoid being submerged.
I've assumed that the water level in Hellas is the same as in the Borealis. This doesn't necessarily have to be the case, if there is enough faulting, impermeable rocks, etc to prevent the northern hemisphere water table from reaching as far south as Hellas. However, the Hellas water level would have to be about 3 km lower than the Borealis level for Hellas Sea to have the shape shown on the ITW19. The settlement of Dao City (I) was moved to avoid being flooded.
Isidis Planitia is now flooded, to form the Isidis Sea. This is formed by water rising from the water table below it. It is very unlikely that this basin could be isolated from the rest of the nearby Borealis Sea and its water table.
Railways are shown as a thin black line on the map. Since the polar regions are now surrounded by water several hundred metres deep, I've re-routed the northern spur of the railway to connect directly to the settlement of Clarke (H), rather than go to the pole. Anyone wishing to go to the pole can take a ship or plane from there. The southern spur still goes to the South Pole though.
Several of the craters are in the wrong place in the ITW map - the correct locations are shown on the map presented here.
Seasonal sea ice is not shown. In addition, the water here is coloured blue to make it more visible against the martian background terrain. In reality, it is coffee-coloured.
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