The Phoenicis Lacus quadrangle is one of a series of 30 quadrangle maps of Mars used by the United States Geological Survey (USGS) Astrogeology Research Program. The Phoenicis Lacus quadrangle is also referred to as MC-17 (Mars Chart-17). Parts of Daedalia Planum, Sinai Planum, and Solis Planum are found in this quadrangle. Phoenicis Lacus is named after the phoenix which according to myth burns itself up every 500 years and then is reborn.

The Phoenicis Lacus quadrangle covers the area from 90° to 135° west longitude and 0° to 30° south latitude on Mars. The Tharsus rise, which was formed from lava flows, occupies part of area. The volcanoes Pavonis Mons and Arsia Mons are believed to have once had glaciers on them. Glaciers may still exist under a thin layer of rocks. The ice can be a source of water for the possible future colonization of the planet. One of the most prominent features of this quadrangle is a large intersecting set of canyons called Noctis Labyrinthus. Other interesting features are lava channels, Dark slope streaks, pit crater chains, and large troughs (called fossae). Research published in the journal Icarus has found pits in Zumba Crater are caused by hot ejecta falling on ground containing ice. The pits are formed by heat forming steam that rushes out from groups of pits simultaneously, thereby blowing away from the pit ejecta.

Noctis Labyrinthus is a large canyon system found in the Phoenicis Lacus quadrangle. Its walls contain many layers of rocks. Research, described in December 2009, found a variety of minerals—including clays, sulfates, and hydrated silicas in some of the layers.

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  Moasic of Viking 1 Orbiter pictures showing location of Noctus Labyrinthus
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  Noctis Labyrinthus, as seen by Viking 1
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  Part of Noctus Labyrinthus, as seen by Themis in the day Arrow points to area that will be enlarged. Red box shows the region covered by a CTX image which follows.
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  Part of Noctis Labrynthus as seen by CTX Box shows the area covered by the following HiRISE image
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  North and south walls of part of Noctis Labyrinthus, as seen by HiRISE under HiWish program
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  Wide view of north wall of part of Noctis Labyrinthus, as seen by HiRISE under HiWish program
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  Close view of north wall of part of Noctis Labyrinthus, as seen by HiRISE under HiWish program
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  Close view of south wall of part of Noctis Labyrinthus, as seen by HiRISE under HiWish program

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  Mariner 9 view of the Noctis Labyrinthus "labyrinth" at the western end of Valles Marineris on Mars. Linear graben, grooves, and crater chains dominate this region, along with a number of flat-topped mesas. The image is roughly 400 km across, centered at 6 S, 105 W, at the edge of the Tharsis bulge. North is
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  Part of Noctis Labyrinthus taken with Mars Global Surveyor. Courtesy NASA/Malin Space Science Systems.
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  Layers in the wall of Noctis Labyrinthus taken with Mars Global Surveyor, under the MOC Public Targeting Program. Courtesy NASA/Malin Space Science Systems.
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  Layers in the lower portion of two neighbouring buttes within the Noctis Labyrinthus formation on Mars are visible in this image.
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  Section of layers near top of Noctis Labyrinthus, as seen by HiRISE under HiWish program
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  Group of layers near the bottom of Noctis Labyrinthus, as seen by HiRISE under HiWish program
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  Wide view of cliff with layers in Noctis Labyrinthus
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  Close-up of part of previous image of layers in Noctis Labyrinthus, as seen by HiRISE under HiWish program
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  Wide view of floor of Noctis Labyrinthus, as seen by HiRISE under HiWish program
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  Close-up of complex, dark dunes in the previous image of the floor of Noctis Labyrinthus, as seen by HiRISE under HiWish program
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  Close-up of some layers in wall of Noctis Labyrinthus, as seen by HiRISE under HiWish program
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  Layers on floor of Noctus Labyrinthus, as seen by HiRISE under HiWish program. Layers probably contain a variety of minerals that were formed with groundwater.
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  Close-up of layers on floor of Noctis Labyrinthus, as seen by HiRISE under HiWish program. This is an enlargement from the center of the previous picture.
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  Layers in a section near the top of wall in Noctis Labyrinthus, as seen by HiRISE under HiWish program
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  Floor of Noctis Labyrinthus showing layered structures, as seen by HiRISE under HiWish program
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  Layered mesa on floor of Noctis Labyrinthus, as seen by HiRISE under HiWish program Note: this is an enlargement of a previous image.
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  Enlargement of edge of mesa on floor of Noctis Labyrinthus showing layers, as seen by HiRISE under HiWish program. Note: this is an enlargement of a previous image.
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  Enlargement of a light-toned structure on floor of Noctis Labyrinthus, as seen by HiRISE under HiWish program. Note: this is an enlargement of a previous image.
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  Light-toned butte on floor of Noctis Labyrinthus, as seen by HiRISE under HiWish program. Note: this is an enlargement of a previous image.
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  Thin dark layers on floor of Noctis Labyrinthus, as seen by HiRISE under HiWish program. Note: this is an enlargement of a previous image.
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  Context image for following image of Noctis Labyrinthus, as seen by CTX
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  Layers inside Noctis Labyrinthus, as seen by HiRISE under HiWish program
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  Layers in Noctis Labyrinthus, as seen by HiRISE under HiWish program

Lava sometimes forms a tube as it moves away from the vent (opening from which lava flows from a volcano). The top of a stream of lava cools down, thereby forming a solid roof. Meanwhile, the lava continues moving in the tube. Often, when all the lava leaves the tube, the roof collapses, making a channel. These features are found on Mars. Some can be seen around Pavonis Mons, in the picture below. Some people have suggested that future colonists on Mars could use lava tunnels as shelters. They would offer great protection from radiation, especially ultraviolet radiation. Lava Channels on the flank of the volcano Pavonis Mons are pictured below in a picture from Mars Odyssey THEMIS. Sometimes the lava tube remains intact for a time. Lava will break out along the tube to accumulate or flow away. Lava flows often have a lobate appearance at the edges. A good view of such a lava tube is shown below.

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  Lava tubes were once covered over with lava flowing in them, but the roofs have now collapsed and the lava has left. Also, some straight troughs (grabens) crosscut the lava channels. Picture taken by THEMIS.

Many of the volcanoes on Mars show strong evidence of past and possible present glacial activity. When glaciers melt and retreat, they leave behind material that was carried in and on the ice. Often the material is dropped in a ridge, called a moraine. An example of moraines is shown in the picture below from the flank of Arsia Mons, a picture taken with the Mars Odyssey THEMIS.

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  Ridges on side of Arsia Mons, a large volcano, may be moraines dropped by glacial activity.

A picture below shows dark streaks on the slopes of Aganippe Fossa. Such streaks are common on Mars. They occur on steep slopes of craters, troughs, and valleys. The streaks are dark at first. They get lighter with age. Sometimes they start in a tiny spot, then spread out and go for hundreds of meters. They have been seen to travel around obstacles, like boulders. It is believed that they are avalanches of bright dust that expose a darker underlying layer. However, several ideas have been advanced to explain them. Some involve water or even the growth of organisms. The streaks appear in areas covered with dust. Much of the Martian surface is covered with dust. Fine dust settles out of the atmosphere covering everything. We know a lot about this dust because the solar panels of the Mars Rovers get covered with dust, thus reducing the electrical energy. The power of the Rovers has been restored many times by the wind, in the form of dust devils, cleaning the panels and boosting the power. So, we know that dust settles from the atmosphere then returns over and over. Dust storms are frequent, especially when the spring season begins in the southern hemisphere. At that time, Mars is 40% closer to the Sun. The orbit of Mars is much more elliptical then the Earth's. That is the difference between the farthest point from the Sun and the closest point to the Sun is very great for Mars, but only a slight amount for the Earth. Also, every few years, the entire planet is engulfed in global dust storms. When NASA's Mariner 9 craft arrived there, nothing could be seen through the dust storm. Other global dust storms have also been observed, since that time.

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  Aganippe Fossa as seen by HiRISE. Full size image shows layers and streaks.

Research, published in January 2012 in Icarus, found that dark streaks were initiated by airblasts from meteorites traveling at supersonic speeds. The team of scientists was led by Kaylan Burleigh, an undergraduate at the University of Arizona. After counting some 65,000 dark streaks around the impact site of a group of five new craters, patterns emerged. The number of streaks was greatest closer to the impact site, so the impact somehow probably caused the streaks. Also, the distribution of the streaks formed a pattern with two wings extending from the impact site. The curved wings resembled scimitars, curved knives. This pattern suggests that an interaction of airblasts from the group of meteorites shook dust loose enough to start dust avalanches that formed the many dark streaks. At first it was thought that the shaking of the ground from the impact caused the dust avalanches, but if that was the case the dark streaks would have been arranged symmetrically around the impacts, rather than being concentrated into curved shapes.

The crater cluster lies near the equator 510 miles south of Olympus Mons, on a type of terrain called the Medusae Fossae formation. The formation is coated with dust and contains wind-carved ridges called yardangs. These yardangs have steep slopes thickly covered with dust, so when the sonic boom of the airblast arrived from the impacts dust started to move down the slope. Using photos from Mars Global Surveyor and HiRISE camera on NASA's Mars Reconnaissance Orbiter, scientists have found about 20 new impacts each year on Mars. Because the spacecraft have been imaging Mars almost continuously for a span of 14 years, newer images with suspected recent craters can be compared to older images to determine when the craters were formed. Since the craters were spotted in a HiRISE image from February 2006, but were not present in a Mars Global Surveyor image taken in May 2004, the impact occurred in that time frame.

The largest crater in the cluster is about 22 meters (72 feet) in diameter with close to the area of a basketball court. As the meteorite traveled through the Martian atmosphere it probably broke up; hence a tight group of impact craters resulted. Dark slope streaks have been seen for some time, and many ideas have been advanced to explain them. This research may have finally solved this mystery.

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  Image indicates crater cluster and curved lines formed by airblast from meteorites. Meteorites caused airblast which caused dust avalanches on steep slopes. Image is from HiRISE.
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  Close up of previous image along light/dark boundary. Dark line in middle of image shows border between light and dark area of curved lines. Green arrows show high areas of ridges. Loose dust moved down steep slopes when it felt the airblast from meteorite strikes. Image is from HiRISE.

Pit craters are common near volcanoes in the Tharsis and Elysium system of volcanoes. Pit craters form when a void is produced by a cracking of the surface caused by stretching. Also, lava may drain out of an underground chamber, thus leaving an empty space. When material slides into a void, a pit crater or a pit crater chain forms. Pit craters do not have rims or ejecta around them, like impact craters do. On Mars, individual pit craters can join to form chains or even to form troughs that are sometimes scalloped. Pit craters are not common on Earth. Sinkholes, where the ground falls into a hole (sometimes in the middle of a town) resemble pit craters on Mars. However, on the Earth these holes are caused by limestone being dissolved thereby causing a void. The image below of Arsia Chasmata contains a pit crater chain.

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  Arsia Chasmata, as seen by HiRISE. A pit crater chain is visible in the lower right.

Certain areas on Mars possess large troughs (long narrow depressions) called fossae in the geographical language used for Mars. This term is derived from Latin; therefore fossa is singular and fossae is plural. Troughs form when the crust is stretched until it breaks. The stretching can be due to the large weight of a nearby volcano. Fossae/pit craters are common near volcanoes in the Tharsis and Elysium system of volcanoes. A trough often has two breaks with a middle section moving down, leaving steep cliffs along the sides; such a trough is called a graben. Lake George, in northern New York State, is a lake that sits in a graben.

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  Oti Fossae, as seen by HiRISE. Go to Fossa (geology) for more information.
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  Oti Fossae, as seen by THEMIS. These parallel graben are found on the northeastern side of Arsia Mons; they are in line with the NE/SW trend of the three volcanoes in Tharsis.
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  Oti Fossae, as seen by THEMIS. These parallel graben are found on the northeastern side of Arsia Mons; they are in line with the NE/SW trend of the three volcanoes in Tharsis.
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  Claritas Fossae as seen by HiRISE. Note the steep scarp.

The most common form of volcanism on the Earth is basaltic. Basalts formed from molten rocks that cooled on the surface. They originated from the partial melting of the upper mantle. They are rich in iron and magnesium (mafic) minerals and commonly dark gray in color. The principal type of volcanism on Mars is probably also basaltic. Although Mars displays many volcanoes here and other places, there has been no evidence of recent volcanic activity, even at a very low level. Research, published in 2017, found no active release of volcanic gases during two successive Martian years. They looked for the outgassing of sulfur-bearing chemicals with spectrometers.

The dsovery of a new volcano at the east side of Noctis Labrinthus was announced at a conference in March 2024. It was seen since the early 1970s, but erosion had concealed it from view. There are hints that an adjacent glacier buried underneath the volcanic slopes. The new volcano has a diameter of about 280 miles (450 kilometers and measures roughly 29,600 feet (9,022 meters) in elevation. Note: this mountain is higher than any peak in the United States. Lava flows, pyroclastic deposits (made of volcanic materials such as ash, cinders, pumice and tephra) and hydrothermal mineral deposits occur in several areas nearby. Some of the minerals found in the region are mafic (high Ca pyroxenes, e.g., augite)—these suggest volcanic material. The volcano is located at 7.40°S, 94.60°W. The authors of the paper consider the volcano to be an eroded shield volcano. Sub-circular depressions near the top are interpreted as caldera remnants.

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  Map of Phoenicis Lacus quadrangle with major features labeled. This area contains two large volcanoes, Pavonis Mons and Arsia Mons, as well as the famous Noctis Labyrinthus canyon system.
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  Arsia Mons showing its position among other volcanoes as seen by THEMIS
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  Topography around Arsia Mons
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  Arsia Mons, as seen by Mars Global Surveyor
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  Small Volcano in Phoenicis Lacus quadrangle. Image is 1.9 miles wide.
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  Volcanic crater (upper) and impact crater (lower). Image about 5 km across.
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  Several lava flows, as seen by HiRISE under HiWish program
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  Lava flows moving around higher ground, as seen by HiRISE under HiWish program
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  Lava flow, as seen by HiRISE under HiWish program
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  Edge of lava flow, as seen by HiRISE under HiWish program

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  Crater showing layers and depression on floor, as seen by HiRISE under HiWish program
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  Close view of layers in crater, as seen by HiRISE under HiWish program
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  Zumba Crater, as seen by HiRISE. Zumba Crater is a very young crater.
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  Small crater, as seen by HiRISE under HiWish program. Much of the ejecta consists of boulders.
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  Young crater with bright ejecta in the Phoenicis Lacus quadrangle as seen by HiRISE under HiWish program The impact reached down to a layer that is light-toned. That light-toned material was then deposited on a dark surface.

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  Claritas Rupes, as seen by HiRISE. Click on image to see layers. Scale bar is 1000 meters long.
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  New Impact that formed between March 2000 and July 2003. Scale bar is 500 meters long. Image taken with HiRISE.
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  Channel, as seen by HiRISE under HiWish program. Arrows indicate position of channel in this rather dark photo.

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  Wide view of mounds and lines, as seen by HiRISE under HiWish program. The lines may be petrified dunes.
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  Close, color view of lines from previous image, as seen by HiRISE under HiWish program. Here they look like old dunes. Colors show different minerals.