Phobos flyby images

The first image from 7 March
15 March 2010

Images from the recent flyby of Phobos, on 7 March 2010, are released today. The images show Mars’ rocky moon in exquisite detail, with a resolution of just 4.4 metres per pixel. They show the proposed landing sites for the forthcoming Phobos-Grunt mission.

ESA's Mars Express spacecraft orbits the Red Planet in a highly elliptical, polar orbit that brings it close to Phobos every five months. It is the only spacecraft currently in orbit around Mars whose orbit reaches far enough from the planet to provide a close-up view of Phobos.

Like our Moon, Phobos always shows the same side to the planet, so it is only by flying outside the orbit that it becomes possible to observe the far side. Mars Express did just this on 7, 10 and 13 March 2010. Mars Express also collected data with other instruments.

Phobos in 3D

Phobos is an irregular body measuring some 27 × 22 × 19 km. Its origin is debated. It appears to share many surface characteristics with the class of ‘carbonaceous C-type’ asteroids, which suggests it might have been captured from this population. However, it is difficult to explain either the capture mechanism or the subsequent evolution of the orbit into the equatorial plane of Mars. An alternative hypothesis is that it formed around Mars, and is therefore a remnant from the planetary formation period.

In 2011 Russia will send a mission called Phobos–Grunt (meaning Phobos Soil) to land on the martian moon, collect a soil sample and return it to Earth for analysis.

The Phobos-Grunt landing site

For operational and landing safety reasons, the proposed landing sites were selected on the far side of Phobos within the area 5°S-5°N, 230-235°E. This region was imaged by the HRSC high-resolution camera of Mars Express during the July-August 2008 flybys of Phobos. But new HRSC images showing the vicinity of the landing area under different conditions, such as better illumination from the Sun, remain highly valuable for mission planners.

Mars Express HRSC views of Phobos 10 March 2010
Mars moon Phobos

It is expected that Earth-based ESA stations will take part in controlling Phobos-Grunt, receiving telemetry and making trajectory measurements, including implementation of very long-baseline interferometry (VLBI). This cooperation is realized on the basis of the agreement on collaboration of the Russian Federal Space Agency and ESA in the framework of the Phobos-Grunt and ExoMars projects.

Mars Express HRSC views of Phobos 10 March 2010
Phobos in 3D

Mars Express will continue to encounter Phobos until the end of March, when the moon will pass out of range. During the remaining flybys, HRSC and other instruments will continue to collect data.

More information

Mars Express Phobos flyby 7 March 2010

Univ.-Prof. Dr. Gerhard Neukum
Freie Universitaet Berlin
Mobile: +49 171-7647177
Tel: +49 30 838 70579; +49 30 838 70575
Email: gneukum @ zedat.fu-berlin.de

Prof. Dr. Ralf Jaumann
German Aerospace Center
Phone: +49 30 67055-400
Fax: +49 30 67055-402
Email: ralf.jaumann @ dlr.de
Olivier Witasse
ESA Mars Express project scientist
ESTEC, The Netherlands
Email: owitasse @ rssd.esa.int

Updates as the flybys take place will be posted on the Mars Express blog.

Note to editors

The High Resolution Stereo Camera (HRSC) experiment on the ESA Mars Express mission is led by the Principal Investigator (PI) Prof. Dr. Gerhard Neukum, who also designed the camera. The science team of the experiment consists of 45 Co-Investigators from 32 institutions and 10 nations. The camera was developed at the German Aerospace Center (DLR) under the leadership of the PI and built in cooperation with industrial partners (EADS Astrium, Lewicki Microelectronic GmbH and Jena-Optronik GmbH). HRSC is operated by the DLR Institute of Planetary Research, through ESA/ESOC. The science planning coordination between all instruments is performed at ESA/ESAC. The systematic processing of the HRSC image data is carried out at DLR. The scenes shown here were processed by the PI group at the Institute for Geosciences of the Freie Universitaet Berlin in cooperation with DLR, Institute of Planetary Research, Berlin.

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