esa is getting closer to determine where exactly philae is located:

Philae best fit search ellipse



Released 30/07/2015 8:00 pm
Copyright ESA/Rosetta/Philae/CONSERT

Based on the most recent calculations using CONSERT data and detailed comet shape models, Philae’s location has been revised to an area covering 34 x 21 m. The best fit area is marked in red, a good fit is marked in yellow, with areas on the white strip corresponding to previous estimates now discounted. One lander candidate proposed previously in the vicinity lies 62 m from the red marked area of the new CONSERT region, suggesting this is no longer a viable candidate.

still awaiting more info on philae, but they released how they modified the philae science sequence because it bounced:

Philae’s adapted first science sequence



Released 30/07/2015 8:00 pm
Copyright spacecraft: ESA/ATG medialab

A timeline of the science operations that Rosetta’s lander Philae performed between 12 and 15 November 2014, following touchdown on the surface of Comet 67P/Churyumov–Gerasimenko. This is an update on the graphic of the planned first science sequence.
Following Philae’s unexpected flight across the surface of the comet, the planned first science sequence had to be adapted according to the new situation. The graphic shows the approximate times (to the nearest 15 minutes) that each of Philae’s 10 instruments was activated; however, it does not indicate the success of data acquired.

Good pic of it.

:mellow:

just to remind everyone, that comet 67P/churyumov–gerasimenko nears perohelion:



Released 06/08/2015 11:00 am
Key moments in Rosetta’s first year at Comet 67P/Churyumov–Gerasimenko.

comet outburst ahead of perihelion:



Released 11/08/2015 10:00 am
Copyright ESA/Rosetta/MPS for OSIRIS Team MPS/UPD/LAM/IAA/SSO/INTA/UPM/DASP/IDA

A short-lived outburst from Comet 67P/Churyumov–Gerasimenko was captured by Rosetta’s OSIRIS narrow-angle camera on 29 July 2015. The image at left was taken at 13:06 GMT and does not show any visible signs of the jet. It is very strong in the middle image captured at 13:24 GMT. Residual traces of activity are only very faintly visible in the final image taken at 13:42 GMT.
The images were taken from a distance of 186 km from the centre of the comet. The jet is estimated to have a minimum speed of 10 m/s and originates from a location on the comet’s neck, in the rugged Anuket region.

29 July outburst context



Released 11/08/2015 10:00 am
Copyright ESA/Rosetta/MPS for OSIRIS Team MPS/UPD/LAM/IAA/SSO/INTA/UPM/DASP/IDA

This image, taken on 12 April 2015 by the OSIRIS narrow-angle camera, identifies the source region of the outburst from Comet 67P/Churyumov–Gerasimenko observed by Rosetta’s instruments on 29 July.

and some science done during/following the outburst:

Gas changes during 29 July outburst



Released 11/08/2015 10:00 am
Copyright ESA/Rosetta/ROSINA/UBern/ BIRA/LATMOS/LMM/IRAP/MPS/SwRI/TUB/UMich

During an outburst of gas and dust from Comet 67P/Churyumov–Gerasimenko on 29 July 2015, Rosetta’s ROSINA instrument detected a change in the composition of gases compared with previous days.
The graph shows the relative abundances of various gases after the outburst, compared with the measurements two days earlier.
For example, the amount of carbon dioxide (CO2) increased by a factor of two, methane (CH4) by four, and hydrogen sulphide (H2S) by seven, while the amount of water (indicated by the horizontal black line) stayed almost constant.

Discovery of diamagnetic cavity



Released 11/08/2015 10:00 am
Copyright ESA/Rosetta/RPC/IGEP/IC

The decrease in magnetic field strength measured by Rosetta’s RPC-MAG instrument during the outburst event on 29 July 2015. This is the first time a ‘diamagnetic cavity’ has been detected at Comet 67P/Churyumov–Gerasimenko and is thought to be caused by an outburst of gas temporarily increasing the gas flux in the comet’s coma, and pushing the pressure-balance boundary between it and incoming solar wind farther from the nucleus than expected under ‘normal’ levels of activity.

damn

here some recently released results from experiments done by philae:

MUPUS investigations at Abydos



Released 30/07/2015 8:00 pm
Copyright Spacecraft graphic: ESA/ATG medialab; data from Spohn et al (2015)

Summary of Philae’s MUPUS measurements at Abydos, its final landing site on Comet 67P/Churyumov–Gerasimenko. The graph at top shows the average surface temperature profile measured by the MUPUS thermal mapper, situated on the lander’s ‘balcony’. Gaps correspond to times when the instrument was not recording data. The profile shows a clear rise and fall in temperature, corresponding to lows of about –180ºC and ‘highs’ of about –145ºC in sync with the comet’s 12.4 hour day. The peaks are interpreted as infrared radiation from the directly insolated surface, with the more gentle variations outside of the peaks attributed to indirect lighting. The thermal inertia implied by the measured rapid rise and fall in the temperature suggest that the surface consists of a thin layer of dust atop a compacted dust-ice crust.
The graph at the bottom shows the hammering profile of the MUPUS penetrator. The displacement is expressed as the position of the depth sensor with respect to its starting position above the surface. An initial displacement of about 27 mm, perhaps through a thin layer of dust, is observed, followed by oscillations of 10–15 mm and smaller displacements. The reason for the lower amplitude after 80 minutes is unclear, but could indicate that the tip of the penetrator had locked to the ground. The data suggest that the instrument was hammering more or less on the spot, although not necessarily at exactly the same spot each time, with indentations of a few millimetres and recoils of up to 10 mm. The red lines indicate the power levels of MUPUS, which correspond to 0.49, 1.59, 2.17 and 4.23 joules, respectively. Discussion is ongoing as to whether the data reflect the full use of energy level 4. In any case, the results provide an estimate of the strength of the surface beneath the thin dust layer as at least 2 MPa.