1. Geometric information for VIRTIS-M data
F. Tosi and the VIRTIS Team

2. Available tools for irregular shapes
VER2DSK: a Unix script allowing to transform a raw shape model file (text file, properly formatted, *.ver) into a SPICE-compliant shape model file (binary, *.dsk).
TSTSHAPE.c: a procedure in the “C” language, allowing to show the aspect of a shape model (already converted into DSK format) with a given perspective and illumination. The user can set up the sub-spacecraft point, sub-solar point, distance and pixel scale to be applied, as well as the photometric function to be used in computing reflected sunlight.
RVGSS.c: a procedure in the “C” language, able to compute geometries for the central ray and 4 corners of each VIRTIS-M pixel (an input file with UTC times at mid-exposure for each line is needed). This code provides no computation for VIRTIS-H at the moment.
VIRTIS Science Team Meeting

3. Testing different shape models
Steins_shape_ver2a.ver – small craters included
Lambert
Lommel-Seeliger
Roe-Minnaert
SteinsFinal.ver – without small craters
Lambert
Lommel-Seeliger
Roe-Minnaert
VIRTIS Science Team Meeting

4. Cube I1_00179260351.QUB Triaxial Ellipsoid (updated pole location)
VIRTIS Science Team Meeting

5. VIRTIS Science Team Meeting
Cube I1_ QUB
Steins_shape_ver2a.ver
VIRTIS Science Team Meeting

6. VIRTIS Science Team Meeting
Cube I1_ QUB
SteinsFinal.ver
VIRTIS Science Team Meeting

7. Comparison with acquired data
VIRTIS Science Team Meeting

8. VIRTIS Science Team Meeting

9. VIRTIS Science Team Meeting

10. Cube I1_00179260351.QUB - Global coverage (1)
Steins_shape_ver2a.ver
(with small craters)
VIRTIS Science Team Meeting

11. (without small craters)
Cube I1_ QUB - Global coverage (2)
SteinsFinal.ver
(without small craters)
VIRTIS Science Team Meeting

12. VIRTIS Science Team Meeting
Steins_shape_ver2a.ver
Phase angle
Solar angle
Emission angle
30 March 2009
VIRTIS Science Team Meeting

13. Comparing different shape models (1)
Steins_shape_ver2a.ver
(with small craters)
SteinsFinal.ver
(without small craters)
VIRTIS Science Team Meeting

14. Comparing different shape models (2)
Steins_shape_ver2a.ver
(with small craters)
SteinsFinal.ver
(without small craters)
VIRTIS Science Team Meeting

15. Comparing different shape models (3)
Steins_shape_ver2a.ver
(with small craters)
SteinsFinal.ver
(without small craters)
VIRTIS Science Team Meeting

16. VIRTIS Science Team Meeting
Available tools
The tools develoved in collaboration with Lucas Kamp (VER2DSK, TSTSHAPE.c, RVGSS.c) are available on the VIRTIS ftp data (Rome), at the path:
ftp:// /ROSETTA_GEOMETRY/SPICE/kernels/plate/Steins/software_LWK/
VIRTIS Co-Is can download and use this software.
To use the RVGSS.c procedure, one has to first download and install the latest CSPICE distribution. Furthermore, an input file with UTC times at mid-exposure for each acquired data is needed to run the procedure.
These tools will be very useful also for the Lutetia flyby, coming in July 2010.
VIRTIS Science Team Meeting

17. VIRTIS Science Team Meeting
SPICE Concept
SPK (trajectory) and CK (attitude) files are time varying products. As such, they can be produced many times during a mission. In general, 3 kinds of SPK kernels may exist:
SPK
PcK
PLANNED → contain spacecraft pointing information to be used only for planning purposes
PREDICTED → contain pointing information to be uplinked to the spacecraft. Accuracy is adequate also for cameras (e.g., better than ~40 arcsec) and time sampling is usually dense
RECONSTRUCTED → contain spacecraft pointing information derived a posteriori from telemetry data. Accuracy is very high but the time sampling can be sparse (worse) wrt predicted kernels IK CK EK
ESP ESQ ENB
VIRTIS Science Team Meeting 7

18. SPICE policy for Rosetta
SPK (trajectory) and CK (attitude) files are produced by an automated system located at ESAC, operated by the ROSETTA Science Operations Center (RSOC).
The ESOC naming convention is used both for SPK and CK files, which are converted from ESOC’s DDID Orbit and Attitude files, respectively.
For the trajectory, several SPK files are produced, describing different phases of the mission (cruise, 1st Earth swingby, Mars Swingby, 2nd Earth swingby, 3rd Earth swingby, Steins asteroid flyby, Lutetia asteroid flyby, comet orbit). These products are updated periodically, until a reconstructed version is available.
There is NO reconstructed CK file since the uncertainty of the S/C positioning is worse than the uncertainty on the predicted attitude compared to the real one. As a consequence, no reconstructed file is provided by Flight Dynamics and the one used for the scenario is the latest predicted one.
VIRTIS Science Team Meeting

19. VIRTIS-M(is)alignment
The center image of VIRTIS is not coincident to the +Z axis of the spacecraft: unavoidable misalignments exist, which have been characterized in December 2006 after the PC4 observations:
Offset from Zs/c along Xs/c (deg)
Offset from Zs/c along Ys/c (deg)
VIRTIS-M
-0.075
VIRTIS-H
0.0027
VIRTIS Science Team Meeting

20. SPICE policy for VIRTIS
Since VIRTIS is an imaging spectrometer using an internal scanning mirror, with the SPICE system two ways can be followed to reconstruct an observational geometry:
We can use the ‘standard’ available kernels and try to reconstruct the geometry by recalculating the pointing direction of each pixel;
Or, we can first build a CK kernel accounting for the VIRTIS-M scanning mirror orientation, and load it along with the other kernels in order to reconstruct the pointing direction of the mirror at a given time.
As it was already done for VEx, also for Rosetta the second approach was chosen.
So we generate ‘type 2’ CK kernels, reconstructing the orientation of the scanning mirror for a given time interval, through the MSOPCK routine provided by NAIF, on the basis of telemetry data produced by the EGSE software:
Telemetry (*.PTM) files
Input file
MSOPCK
CK file
VIRTIS Science Team Meeting