Lava Flows of Daedalia Planum – This image will be used to observe the previous flow of new material over old material, filling in craters and creating "flow lines."

NASA/JPL/University of Arizona (255 km above the surface. Scene is 5 km across.) www.uahirise.org/ESP_050274_1580

Terrain West of the Clay-Bearing Units of Mawrth Vallis

NASA/JPL/University of Arizona (5 km across, www.uahirise.org/ESP_013849_2030)

Southern Wall of a Canyon-Like Structure

NASA/JPL/University of Arizona (Apr 2011, 255 km above the surface, 5 km across; www.uahirise.org/ESP_022080_1690)

Possible Olivine-Rich Terrain on Etched, Intercrater Plains

NASA/JPL/University of Arizona (Dec 2009, 264 km above the surface, 5 km across; www.uahirise.org/ESP_015969_1775)

LIght-Toned Bedrock along the Floor of Coprates Catena

NASA/JPL/University of Arizona (5 km across; www.uahirise.org/ESP_019903_1645)

The rain in Spain

Károly Keresi

An Inverted Crater – There is a circular feature in this observation that appears to stand above the surrounding terrain. How did it form? (www.uahirise.org/ESP_043651_1590)

Yardangs: Nature’s Weathervanes

Though often beautiful to look at, yardangs are not permanent and will be eroded away by the persistence of the Martian winds.

NASA/JPL/University of Arizona (uahirise.org/ESP_050420_1910)

Terrain between South and Main Craters (Almost sounds like an address.)

NASA/JPL/University of Arizona (Nov 2016, 250 km above the surface, 5 km across; www.uahirise.org/ESP_048172_1025)

Slope Monitoring

NASA/JPL/University of Arizona (Acquired: Nov 2016, 279 km above the surface. Scene is 5 km across. www.uahirise.org/ESP_048490_1695)

Charlis Ortíz en el compromiso que enfrentó a Real Esppor Club y Trujillanos Fútbol Club, en el estadio nacional Brígido Iriarte (Nelson Pulido)

The Plains are Not Plain – This image covers some of the plains south of Capri Chasma in eastern Valles Marineris. (www.uahirise.org/ESP_045300_1630)

Cryptic Terrain – We call it “cryptic” only because of the lack of easily identifiable features.

NASA/JPL/University of Arizona (Nov 2016, 249 km above the surface, 5 km across; www.uahirise.org/ESP_048169_0985)

Southern Intercrater Plains

NASA/JPL/University of Arizona (Nov 2016, 250 km above the surface, 5 km across; www.uahirise.org/ESP_048167_1165)

Lava Channels in Daedalia Planum

Channelized lava flows with lots of topography. These flows could tell us something about the flow dynamics that emplaced them.

NASA/JPL/University of Arizona. (274 km above the surface. www.uahirise.org/ESP_049997_1595)

Mattress and toilet paper not included.

Martian Meanders and Scroll-Bars – Channels become inverted when the sediments filling them become more resistant to erosion than the surrounding material. Here, the most likely process leading to hardening of the channel material is chemical cementation by precipitation of minerals.

NASA/JPL/University of Arizona (www.uahirise.org/ESP_020673_1750)

Light-Toned Rock Outcrops and Aeolian Dunes in Trouvelot Crater

Image: NASA/JPL/University of Arizona (5 km. www.uahirise.org/ESP_016275_1960)

Marc Burgener - Switzerland

Old Features and New – Both recent and ancient features can often appear in the same observation. (www.uahirise.org/ESP_021699_1405)

NASA/JPL/University of Arizona

Tilted Layers East of Copernicus Crater – This is an interesting feature that appears to be a large monocline.

NASA/JPL/University of Arizona (257 km above the surface. Scene is 5 km across. uahirise.org/ESP_049893_1265)

Exposure of South Polar Layered Deposits — Topographic data is sparse in this area.

NASA/JPL/University of Arizona (Acquired: Feb 2017, approximately 254 kilometers above the surface. www.uahirise.org/ESP_049408_0920)

Slope Survey in Juventae Chasma –Juventae Chama is an enormous box canyon that opens to the north and forms the outflow channel Maja Valles.

NASA/JPL/University of Arizona (Acquired: Feb 2017, approximately 268 kilometers above the surface. Scene is 5 km top to bottom and Norh is to the right. www.uahirise.org/ESP_049467_1755)

My first Floriade shot, amazingly in black and white.

Tyrrhena Terra

NASA/JPL/University of Arizona (Acquired: December 2016, approximately 271 kilometers above the surface. Scene is 5 km across; www.uahirise.org/ESP_048525_1790)

Clays along a Scarp in Northwest Argyre Planitia

NASA/JPL/University of Arizona (5 km across, www.uahirise.org/ESP_013653_1405)

A Ridged Surface in South Hellas Planitia — An odd surface of ridges and troughs. Doesn’t look like dunes or scallops. It also seems we caught a dust devil in action!

(NASA/JPL/University of Arizona. Acquired: Feb 2017, approximately 259 kilometers above the surface. www.uahirise.org/ESP_049568_1290)

Potential Dike Associated with Aromatum Chaos

NASA/JPL/University of Arizona (Acquired: November 2016, approximately 268 kilometers above the surface. Scene is 5 km across; www.uahirise.org/ESP_048451_1785)

Hard Knocks in Tyrrhena Terra – This is largely ancient hard bedrock that has been cratered by numerous impacts over the eons.

NASA/JPL/University of Arizona (www.uahirise.org/ESP_021716_1685)

Southern Middle-Latitude Craters

NASA/JPL/University of Arizona (Acquired: November 2016, approximately 249 kilometers above the surface. Scene is 5 km across. www.uahirise.org/ESP_048466_1340)

Isidis Basin Ejecta – This scene is a jumbled mess! There are blocks and smears of many different rocks types that appear to have been dumped into a pile. (www.uahirise.org/ESP_011261_1960)

NASA/JPL/University of Arizona

Dunes of the Southern Highlands — Sand dunes are scattered across Mars and one of the larger populations exists in the Southern hemisphere, just west of the Hellas impact basin.

NASA/JPL/University of Arizona (www.uahirise.org/ESP_049371_1380)

A Gullied Crater

NASA/JPL/University of Arizona (Acquired: November 2016, approximately 252 kilometers above the surface. Scene is less than 5 km across and North is to the right. www.uahirise.org/ESP_048317_1260)

Fans and Crater Floor Deposits Southeast of Vinogradov Crater – The origin of the deposits remains speculative, and their physical character and association with alluvial fans suggests they may be the result of deposition into a shallow lake.

NASA/JPL/University of Arizona (www.uahirise.org/ESP_016843_1590)

Cefalu Crater

NASA/JPL/University of Arizona (Acquired: December 2016, approximately 287 kilometers above the surface. Scene is less than 5 km across; www.uahirise.org/ESP_048543_2040)

The Floor of Tithonium Chasma

NASA/JPL/University of Arizona (Acquired: December 2016, approximately 262 kilometers above the surface. Scene is 5 km across. www.uahirise.org/ESP_048545_1750)

Stratigraphy of Alluvial Fans in Saheki Crater: Some of the best-preserved alluvial fans on Mars are in this area, which we've images many times previously. (www.uahirise.org/ESP_044491_1585)

Eastern State Penitentiary in PA. My gf made this a MUST on our recent trip. She finds some damn good photo ops.

To Great Depths — This image from eastern Hellas Planitia shows some of the unusual features on the basin floor.

NASA/JPL/University of Arizona (www.uahirise.org/ESP_049330_1425)

TWE Block Party, Bobigny (93)

Patch of Light-Toned Terrain

NASA/JPL/University of Arizona (Mar 2011, 251 km above the surface, 5 km top to bottom and North is to the left; www.uahirise.org/ESP_021592_1355)

Terra Cimmeria

NASA/JPL/University of Arizona (Dec 2012, 259 km above the surface, 5 km top to bottom and North is to the right; www.uahirise.org/ESP_029773_1665)

A Steep Scarp in Chasma Boreale on the Opposite Side of an Original Avalanche Site

NASA/JPL/University of Arizona (320 km above the surface, less than 5 km across).

www.uahirise.org/ESP_051362_2650

​

Inspired by the song of The Mars Volta.

Listen to the song that inspired the artwork:

The Mars Volta - Inertiatic Esp

Signed limited editions of 8 on sale from today.

www.robertogrosso.com/