VIS-NIR lightcurve of 2867 Steins during the Rosetta fly-by

Details VIS-NIR lightcurve of 2867 Steins during the Rosetta fly-by VIS-NIR lightcurve of 2867 Steins during the Rosetta fly-by

Dec 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008agufm.p54b..02d&link_type=abstract

American Geophysical Union, Fall Meeting 2008, abstract #P54B-02

Computer Science

Performance

6008 Composition (1060), 6055 Surfaces, 6094 Instruments And Techniques, 6099 General Or Miscellaneous

Scientific paper

During the Rosetta cruise phase, on the September 5th 2008, VIRTIS obtained the first VIS-NIR hyperspectral images of the surface of the E-type asteroid 2867 Steins. VIRTIS is an imaging spectrometer that combines into a single instrument 3 spectral channels: two of them are also devoted to imaging. The third one is solely devoted to high resolution spectroscopy in the IR range (2-5 micrometers). VIRTIS-M (Visible InfraRed Thermal Imaging Spectrometer) is a high performance hyperspectral mapper operating in the VIS (0.25-1.05 micron) and IR ( 0.95-5 micron) ranges, with spatial resolution of 250 microrad (IFOV) and Field of View (FOV) of 3.6° x 3.6°. VIRTIS observations were done in two phases: the first one, when the distance from the asteroid was between 223000 km and 20700 km , and the second one, from 2800 km to 1100 km, passing through the closest approach. The first phase was dedicated to acquire spectrophotometric lightcurve; the second was devoted to high resolution spectral imaging. At its closest approach, corresponding to a distance of 800 km, Rosetta flew by Steins at a relative speed of 8.6 km/s . The spectrophometric lightcurve was measured during the approach to the asteroid, when the its apparent size was less than a VIRTIS-M pixel. These observations were scheduled to span over a period of time of 6.5 h, which was enough to follow an entire Steins rotation. About 100 spectral images were collected during this phase at spectral resolution of 6 nm/band in the VIS range and 30 nm/band in the IR. Few points were collected at higher resolutions ( 2 nm and 10 nm respectively). During the observations, the solar phase angle was quite constant corresponding to 38°. These are the first observations in 288 spectral bands, between 0.25-5 micron, of an asteroid covering the whole rotational period. Thanks to this data set we will investigate the spectral behavior of the asteroid's surface through a whole rotation.

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