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Moon tracking in Grasse MeO station (7845)

This article discusses the theory and model for the new generation of Lunar Laser Ranging (LLR) data from the MeO station in Grasse, including telescope specifications, detection methods, and results from 1987 to 2005. It also explores the distribution of normal points with the age of the moon and the use of adaptive optics for improved accuracy and observations. The article concludes with details on data formats and how to receive the data.

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Moon tracking in Grasse MeO station (7845)

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  1. Moon tracking in GrasseMeO station (7845) J.M. Torre, E. Samain, F. Pierron, M. Aimar, D. Albanese, D. Féraudy, H. Mariey, G. Martinot-Lagarde, J. Paris, M. Pierron, H Viot Theory and Model for the New Generation of the Lunar Laser Ranging Data, ISSI, Bern, Switzerland, February 2010

  2. MeO LLR station • Telescope diameter : 1.54 m • Altitude : 1270 m • Laser : Nd-YAG frequency-doubled 532nm 20ps pulse width50mJ in green10Hz pulse rate • Detection : APD in Single photon mode Theory and Model for the New Generation of the Lunar Laser Ranging Data, ISSI, Bern, Switzerland, February 2010

  3. Results from 1987 to 2005 The difference in the number of normal points between A-XV and the other reflectors is due to the observation strategy: We range on A-XV until we obtain echoes and only after that we attempt to range on another reflector. Sometimes we only have echoes on A-XV (efficiency 3 times better than for the other reflectors). Theory and Model for the New Generation of the Lunar Laser Ranging Data, ISSI, Bern, Switzerland, February 2010

  4. Distribution of Normal Points with the age of the Moon Only 3 observations at the full Moon in 1990, 1996 and 2000 during an eclipse Theory and Model for the New Generation of the Lunar Laser Ranging Data, ISSI, Bern, Switzerland, February 2010

  5. 2005 : Results Theory and Model for the New Generation of the Lunar Laser Ranging Data, ISSI, Bern, Switzerland, February 2010

  6. First results with the new station Theory and Model for the New Generation of the Lunar Laser Ranging Data, ISSI, Bern, Switzerland, February 2010

  7. December 2009, 8th to 9th Is it possible to have a set of reflectors coordinates to obtain the same residuals on all the reflectors ? Theory and Model for the New Generation of the Lunar Laser Ranging Data, ISSI, Bern, Switzerland, February 2010

  8. View of the monitoring screen Theory and Model for the New Generation of the Lunar Laser Ranging Data, ISSI, Bern, Switzerland, February 2010

  9. January 2010, 21th to 22th Theory and Model for the New Generation of the Lunar Laser Ranging Data, ISSI, Bern, Switzerland, February 2010

  10. Lunar Laser Ranging Adaptive Optic (AO) • The diffraction limit of a 1.54 m telescope could permit to have a spot in the range of 200 m. • An AO system used for the up link could improve the link budget by a factor 100 • The same AO system used for the down link could permit to reduce the detection field of view by a factor 10 : the noise to signal ratio would be improved by 10 • Depending on the atmospheric conditions, the size of the laser beacon on the lunar surface is between 2 to 10 km. Theory and Model for the New Generation of the Lunar Laser Ranging Data, ISSI, Bern, Switzerland, February 2010

  11. Adaptive optic • Downlink • The analysis of the wave front has to be done on the details of the lunar surface (when the surface is lighted by the Sun) • Uplink • Injection of the laser through the classical optical path • High energy deformable mirror • Diffusion of the laser pulses onto the wave front sensor • The speed aberration introduces an angular shift between the uplink and the downlink • As soon this angle is greater than the isoplanetism area, the correction between the 2 paths has to be different • The lunar surface used to analyze the wave front is shifted of few km from the actual position of the target Theory and Model for the New Generation of the Lunar Laser Ranging Data, ISSI, Bern, Switzerland, February 2010

  12. What do the scientists need ? • More accuracy • To increase the number of observations • To increase the arc per night • More echoes at the : • Full Moon • New Moon Theory and Model for the New Generation of the Lunar Laser Ranging Data, ISSI, Bern, Switzerland, February 2010

  13. Which Data Format ? • MNC • CSTG • CRD (new ILRS data format) 5120091210035843116817924883858265921301910028002928040 087865+05426 5320a1638 99999 0000103093447845780153200007147900003000442764102891001 143231168178488385826592000028908786278502600280224000 Theory and Model for the New Generation of the Lunar Laser Ranging Data, ISSI, Bern, Switzerland, February 2010

  14. How do you want to receive the data ? dale.boggs@jpl.nasa.govedc@dgfi.badw-muenchen.defrancou@danof.obspm.frjgw@logos.jpl.nasa.govjwj@center.shao.ac.cnmueller@ife.uni-hannover.demoon@ASTRO.AS.UTEXAS.EDUnoll@cddisa.gsfc.nasa.govwtni@phys.nthu.edu.twEkaterina Alesnkina <aek@gao.spb.ru>jchapron@danof.obspm.fr turysher@jpl.nasa.gov • Personalized e-mail (mnc or/and cstg) To be added or removed to this list or to modify your address please send an e-mail to : torre@oca.eu • CRD on ILRS server Theory and Model for the New Generation of the Lunar Laser Ranging Data, ISSI, Bern, Switzerland, February 2010

  15. Thanks !!! For publications using LLR data from Grasse the MeO team asks for acknowledgement of input. Without this support we may not be able to survive. Theory and Model for the New Generation of the Lunar Laser Ranging Data, ISSI, Bern, Switzerland, February 2010

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