Imaging ‘footprints’ of Rosetta’s OSIRIS camera during the descent to the comet’s surface. A primary focus was the pit named Deir el-Medina, as indicated by the number of footprints indicated in blue. The trail of orange and red squares reflect the change in pointing of the camera towards the impact site, subsequently named Sais. The final image was acquired at about 20 m above the surface, and the touchdown point was only 33 m from the centre of the predicted landing ellipse. Credit: ESA/Rosetta/MPS for OSIRIS Team MPS/UPD/LAM/IAA/SSO/INTA/UPM/DASP/IDA ESA’s Rosetta completed its incredible mission on 30 September, collecting unprecedented images and data right until the moment of contact with the comet’s surface. Rosetta’s signal disappeared from screens at ESA’s mission control at 11:19:37 GMT, confirming that the spacecraft had arrived on the surface of Comet 67P/Churyumov–Gerasimenko and switched off some 40 minutes earlier and 720 million kilometres from Earth.
One of the final pieces of information received from Rosetta was sent by its navigation startrackers: a report of a ’large object’ in the field of view – the comet horizon.
Reconstruction of the final descent showed that the spacecraft gently struck the surface only 33 m from the target point.
The accuracy once again highlighted the excellent work of the flight dynamics specialists who supported the entire mission.
The spot, just inside an ancient pit in the Ma’at region on the comet’s ’head’, was named Sais, after a town where the Rosetta Stone was originally located.
Numerous images were taken of the neighbouring pit, capturing incredible details of its layered walls that will be used to help decipher the comet’s geological history.
The final image was acquired about 20 m above the impact point. In addition, a number of Rosetta’s dust, gas and plasma analysis instruments collected data. Rosetta’s last image of Comet 67P/Churyumov-Gerasimenko, taken with the OSIRIS wide-angle camera shortly before impact, at an estimated altitude of about 20 m above the surface. The initially reported 51 m was based on the predicted impact time. Now that this has been confirmed, and following additional information and timeline reconstruction, the estimated distance is now thought to be around 20 metres, and analysis is ongoing. The image scale is about 2 mm/pixel and the image measures about 96 cm across. Credit: ESA/Rosetta/MPS for OSIRIS Team MPS/UPD/LAM/IAA/SSO/INTA/UPM/DASP/IDA The pressure of the gas outflow from the comet was seen to rise as the surface neared. Scans revealed temperatures between about –190ºC and –110ºC down to a few centimetres below the surface. The variation was most likely due to shadows and local topography as Rosetta flew across the surface.
A last measurement of water vapour emission was made on 27 September, estimating the comet was emitting the equivalent of two tablespoons of water per second. During its most active period in August 2015, estimates were in the region of two bathtubs’ worth of water every second.
The first indications from spectral readings show there to be no significant differences in surface composition at the high resolutions obtained all the way down, and there was no obvious indication of small icy patches near the landing site.
The measurements also suggest an increase in very small dust grains – possibly around a millionth of a millimetre – close to the surface.
The last observation of the gas coma surrounding the comet was made the day before the final descent. Carbon dioxide was still being outgassed, at a greater distance from the Sun than when the comet was approaching it. Comet landing sites in context. Credit: CIVA: ESA/Rosetta/Philae/CIVA; NAVCAM: ESA/Rosetta/NAVCAM – CC BY-SA IGO 3.0; OSIRIS: ESA/Rosetta/MPS for OSIRIS Team MPS/UPD/LAM/IAA/SSO/INTA/UPM/DASP/IDA; ROLIS: ESA/Rosetta/Philae/ROLIS/DLR Stable solar wind conditions reigned during the final measurements of the solar wind and interplanetary magnetic field, providing ’quiet’ background values that will be important for calibration.
Decreasing comet plasma densities were observed from about 2 km above the surface, with no obvious detection of local outgassing from the Ma’at pits.
Magnetic field measurements down to an estimated 11 m above the surface confirmed the previous observations of the comet as a non-magnetic body.
No large dust particles were collected during the descent, in itself an interesting result. First impressions are that the observed water vapour production was too low to lift dust grains above a detectable size from the surface.
”It’s great to have these first insights from Rosetta’s last set of data,” says Matt Taylor, ESA’s Rosetta Project Scientist. ”Operations have been completed for over two months now, and the instrument teams are very much focused on analysing their huge datasets collected during Rosetta’s two-plus years at the comet.
”Data from this period will eventually be made available in our archives in the same way as all Rosetta data.” Artist’s impression of Rosetta shortly before hitting Comet 67P/Churyumov–Gerasimenko on 30 September 2016. Credit: ESA/ATG medialab Explore further:Far away, so close
Provided by:European Space Agency