16. February 2021

An in-depth look at the ge­o­log­i­cal con­text of the Mars 2020 land­ing site through the eyes of DLR's HRSC in­stru­ment

Image of the region around Jezero Crater
Im­age of the re­gion around Jeze­ro Crater
Image 1/2, Credit: ESA/DLR/FU Berlin, CC BY-SA 3.0 IGO

Image of the region around Jezero Crater

Jeze­ro Crater lies ex­act­ly on the bound­ary be­tween the an­cient high­land re­gion of Ter­ra Sabaea and the sim­i­lar­ly aged Isidis im­pact basin, whose present-day Isidis Plani­tia plain was formed pri­mar­i­ly by sig­nif­i­cant­ly younger de­posits. The near­by Nili Fos­sae graben sys­tem, which rough­ly traces the shape of the Isidis basin rim through its cur­va­ture, was formed pre­cise­ly by this im­pact as a re­sult of tec­ton­ic frac­tures. Ad­join­ing Jeze­ro Crater to the south­west is the vol­canic re­gion of Syr­tis Ma­jor. This im­age was cre­at­ed from the red, green and blue chan­nels of HRSC and com­bined with high-res­o­lu­tion da­ta from its nadir chan­nel, which is di­rect­ed per­pen­dic­u­lar to the sur­face of Mars. The dark, bluish-black ar­eas are cov­ered by a lay­er of an­cient vol­canic ash that is wide­ly dis­persed by the wind and of­ten piles up in­to im­pres­sive dune fields. The high res­o­lu­tion of the da­ta pro­cessed for this im­age al­lows for greater en­large­ment, en­abling a clos­er look at in­di­vid­u­al de­tails of the land­scape. For this im­age, small gaps in the im­age mo­sa­ic were in­ter­po­lat­ed.
Topographic map of the surroundings of Jezero Crater
To­po­graph­ic map of the sur­round­ings of Jeze­ro Crater
Image 2/2, Credit: ESA/DLR/FU Berlin, CC BY-SA 3.0 IGO

Topographic map of the surroundings of Jezero Crater

DLR's High Res­o­lu­tion Stereo Cam­era (HRSC) or­bits Mars on board ESA's Mars Ex­press space­craft. Its nine sen­sors, ar­ranged at right an­gles to the north-south flight di­rec­tion, record the sur­face of Mars from dif­fer­ent an­gles and in four colour chan­nels. From the four in­clined stereo chan­nels and the nadir chan­nel, which is di­rect­ed per­pen­dic­u­lar to the sur­face of Mars, sci­en­tists at the DLR In­sti­tute of Plan­e­tary Re­search and the Freie Uni­ver­sität Berlin com­pute dig­i­tal ter­rain mod­els, which as­sign el­e­va­tion in­for­ma­tion to each pix­el. The height dif­fer­ence in this area of 1.5 mil­lion square kilo­me­tres (see key at bot­tom right), from the low­est point in Isidis Plani­tia to the high­est crater rim in Ter­ra Sabaea, is over 6800 me­tres – the floor of Jeze­ro Crater lies at an el­e­va­tion of ap­prox­i­mate­ly mi­nus 2600 me­tres. The el­e­va­tion da­ta in this im­age is ref­er­enced to the Mars Areoid, a no­tion­al line of equal grav­i­ta­tion­al at­trac­tion, anal­o­gous to sea lev­el on Earth. The high res­o­lu­tion of the da­ta pro­cessed for this im­age al­lows for greater en­large­ment of the im­ages for a clos­er look at in­di­vid­u­al de­tails of the land­scape.
  • These images show the topography of the Jezero Crater and its surroundings. They were created using data from the High Resolution Stereo Camera (HRSC) operated by DLR; these data make it possible to create views of large areas of the Martian surface as digital terrain models.
  • HRSC's high-resolution digital terrain models have made important contributions to the selection of numerous landing sites on Mars – including for NASA's Mars 2020 mission.
  • The HRSC stereo camera has been mapping the Red Planet in unprecedented resolution, in three dimensions and in colour since 2004 as part of ESA's Mars Express mission.
  • Focus: Space, planetary research

On Thursday, 18 February 2021, at approximately 21:55 CET, NASA's control centre in Pasadena should receive the radio signal indicating that the Perseverance rover has been gently lowered onto the surface of Mars by a 'sky crane' as part of NASA's Mars 2020 mission. Perseverance's new home will be the floor of a former lake in the Jezero impact crater. There, the mobile laboratory, which is the size of a small car, will begin its search for traces of past life and collect samples for later return to Earth.

The High Resolution Stereo Camera (HRSC) operated by the German Aerospace Center (Deutsches Zentrum für Luft-und Raumfahrt; DLR) has been imaging the Red Planet, in three dimensions and in colour, since 2004 as part of ESA's Mars Express mission. The data it collects make it possible to create images of large areas of the Martian surface – not only as colour mosaic images, but also as digital terrain models. These provide researchers with important information about the terrain and elevation of the land, also known as the topography of the region.

HRSC's high-resolution digital terrain models have made important contributions to the selection of numerous landing sites on Mars, including that of the Mars 2020 mission. Accurate topographical information is critical for ensuring a safe landing.

The latest map sheets, each covering an area of over three million square kilometres, can be downloaded from the website of the HRSC team at DLR and from the map server of the Freie Universität Berlin. One of these map sheets (MC-13 East) was used for the image products shown here. This section depicts the wider geographical context around the landing site, located at approximately 18 degrees north and 77 degrees east. The area shown is more than 1.5 million square kilometres (1330 by 1195 kilometres – over twice the size of the Iberian Peninsula) and gives a good overview of the location of the impact crater and the geological context. However, the maps shown here not only provide a large-scale overview of the geographic location, they also provide an outstanding view of detail that is exceptional for such large-scale images. The high resolution of these image here allows them to be greatly enlarged for a closer look at individual detail of the landscape.

The extraordinary geological diversity of this region helped Jezero Crater finally come out on top after the intensive, meticulous selection of the landing site, which took five years. The crater lies exactly on the border between the ancient highland region of Terra Sabaea, where rocks from the Martian Palaeozoic (the Noachian: 4.1–3.7 billion years ago) can still be found, and the similarly ancient Isidis impact basin, which was formed 3.9 billion years ago. However, its present-day Isidis Planitia plain was formed primarily by much younger deposits formed in the Martian Middle Ages, the Hesperian (3.7–3.0 billion years ago) and the Martian Modern (the Amazonian 3.0 billion years to present day). The nearby Nili Fossae graben system, which roughly traces the shape of the rim of the Isidis basin through its curvature, was formed precisely by this impact as a result of tectonic fractures. To the southwest of Jezero Crater is the volcanic region of Syrtis Major, whose most recent lava flows are also assigned to the Hesperian. Thus, the rocks and deposits in and around the crater originate from all three geological epochs of Mars.

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Flight over Jezero Crater – landing site of the Mars 2020 mission
A simulated flight over Jezero Crater on Mars. Home to a standing body of water more than 3.5 billion years ago, this crater is where NASA’s Mars 2020 mission Perseverance rover will land to search for signs of past microbial life. The video is based on data from the High Resolution Stereo Camera...
Credit: ESA/DLR/FU Berlin/HRSC Science Team

A crater lake left behind a diverse mineralogy

In addition to the different ages of the rocks in the vicinity of Jezero Crater, their diverse mineralogical composition is particularly interesting, as researchers can use the minerals to infer the environmental conditions at the time of their formation. The Perseverance rover will be able to study them directly in the crater. The detailed map of Jezero Crater (top right) shows that the crater rim is breached by three valleys which were former rivers. Neretva Vallis and Sava Vallis were inflow channels that have created two deltas on the western and northwestern rim of the crater, which are also considered evidence for the existence of a former lake. Perseverance will examine the larger of the two in the west in more detail.

Pliva Vallis in the east of Jezero Crater was an outflow channel through which water was discharged from the crater. This is why this former crater lake is referred to as an 'open basin lake'. These lakes were once numerous on Mars. Compared to closed basins (with inflow but no outflow), they are interesting because they were freshwater lakes with a stable water level. Lakes in closed basins, on the other hand, were subjected to more frequent periods of drying out, which turned them into salt lakes, thus making them less promising in the search for conditions that are conducive to life.

The large map shows the water catchment area of the two inflow channels, from which material from the surrounding area was transported by the rivers into the crater and deposited in the two deltas. Spacecraft orbiting Mars have used spectrometers to detect a variety of minerals in this catchment area. These are mainly silicates from the olivine and pyroxene groups, both mineral classes that originate from magma within the Martian mantle and indicate basaltic volcanic deposits that were not subject to long-term weathering by water. Even more exciting, however, are the carbonates identified on the inner rim of Jezero Crater, which have rarely been found on Mars thus far, and which, together with the clay minerals more frequently found on Mars, testify to the weathering by water of rock with a volcanic source.

Volcanic minerals, carbonates, clay minerals – these three types of deposits have been found both in the delta and elsewhere in the crater. Some carbonates (limestones) are thought to have been formed directly in the lake. Such lake carbonates and especially the clay minerals indicate freshwater conditions that enable life and have the potential to preserve traces of life – biosignatures – particularly well in their interior. However, other types of minerals have also been discovered there, namely those that paint a different picture of the crater lake. These include sulphates that contain iron oxide, amorphous silicon oxides and hydroxides, which tend to form in acidic waters that gradually dried up. These minerals indicate that the environmental conditions in Jezero Crater became drier and less conducive to life at a later stage. However, even among these minerals there are some in which biosignatures can be very well preserved.

In addition, it will be particularly important to study materials of magmatic origin that are also found on the crater floor. If a sample of lava or other volcanic rock, as unaltered as possible, could be examined on site or even brought to Earth, this would provide insights into the inner development of the planet.

Jezero Crater's surroundings are also worth a visit

If everything goes well and the rover is still functioning after the nominal mission duration of one Martian year (two Earth years), it would be possible to start studying the closer surroundings outside the crater. This would allow Perseverance to be used to investigate some of the oldest rocks formed during the Isidis impact – known as megabreccias, these agglomerated debris could provide valuable information about the early history of Mars. To achieve this aim, a route west out of the crater would need to be planned to reach Noachian bedrock, igneous rocks and lava flows from Syrtis Major. This would allow researchers to gain, refine and substantiate comprehensive on-site knowledge of the lithology throughout Martian history. Not to mention that the rover could also collect samples of these rocks for transport back to Earth, which would provide extraordinary scientific added value.

Image of the region around Jezero Crater
Image of the region around Jezero Crater
Jezero Crater lies exactly on the boundary between the ancient highland region of Terra Sabaea and the similarly aged Isidis impact basin, whose presentday Isidis Planitia plain was formed primarily by significantly younger deposits. The nearby Nili Fossae graben system, which roughly traces the shape of the Isidis basin rim through its curvature, was formed precisely by this impact as a result of tectonic fractures. Adjoining Jezero Crater to the southwest is the volcanic region of Syrtis Major. This image was created from the red, green and blue channels of HRSC and combined with high-resolution data from its nadir channel, which is directed perpendicular to the surface of Mars. The dark, bluish-black areas are covered by a layer of ancient volcanic ash that is widely dispersed by the wind and often piles up into impressive dune fields. The high resolution of the data processed for this image allows for greater enlargement, enabling a closer look at individual details of the landscape. For this image, small gaps in the image mosaic were interpolated.
Credit: ESA/DLR/FU Berlin, CC BY-SA 3.0 IGO

The search for life

In addition to the search for molecular remains of possible former life forms, the main goal of the Mars 2020 mission is to collect samples for transport to Earth in the early 2030s. The aim is to obtain the most promising and diverse samples possible and deposit them on the surface of Mars for later return. The analysis of samples in laboratories on Earth can provide more accurate results than can be obtained with instruments on Mars rovers. Perseverance can only take samples from a relatively shallow depth of a few centimetres. However, it is thought that traces of former life are most likely to be found at greater depths, where they may have been protected from the degrading effects of UV radiation at the surface and the cosmic radiation that penetrates deeper into the soil. These deeper traces may have remained preserved over Martian history. Finally, it is assumed that the best environmental conditions for the existence of life (habitability) prevailed about 3.7 to 3.4 billion years ago. Incidentally, life on Earth also emerged during this period.

As part of the European Space Agency (ESA) ExoMars 2022 mission, the next Mars rover – Rosalind Franklin – is scheduled to land in Oxia Planum on 10 June 2023. This rover has been designed to reach deeper into the subsurface. It will be able to collect core samples from depths of up to two metres and examine them for biosignatures directly on site using highly specialised instruments inside the rover.

Contact
  • Elke Heinemann
    Ger­man Aerospace Cen­ter (DLR)
    Pub­lic Af­fairs and Com­mu­ni­ca­tions
    Telephone: +49 2203 601-2867
    Fax: +49 2203 601-3249

    Contact
  • Daniela Tirsch
    Ger­man Aerospace Cen­ter (DLR)

    In­sti­tute of Plan­e­tary Re­search
    Telephone: +49 30 67055-488
    Fax: +49 30 67055-402
    Linder Höhe
    51147 Köln
    Contact
  • Ulrich Köhler
    Ger­man Aerospace Cen­ter (DLR)
    In­sti­tute of Plan­e­tary Re­search
    Rutherfordstraße 2
    12489 Berlin
    Contact
  • Ernst Hauber
    Ger­man Aerospace Cen­ter (DLR)
    In­sti­tute of Plan­e­tary Re­search
    Plan­e­tary Ge­ol­o­gy
    Telephone: +49 30 67055-325
    Fax: +49 30 67055-402
    Rutherfordstraße 2
    12489 Berlin
    Contact

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