ivo://CDS/P/Moon/LROC-WAC-100mCDSFernique P.2018-02-06T16:26:00Z2019-05-21T07:21:00ZCDS Helpdeskcds-question@unistra.frThe MoonThe WAC global mosaic is comprised of over 15,000 images acquired between November 2009 and February 2011. The WAC maps the whole Moon in one month, however the solar incidence angle at the equator changes about 28deg from the beginning to the end of the month. To even out the incidence angle variations, the mosaic is comprised of data collected over three periods (1/20/2010 to 1/28/2010, 5/30/2010 to 6/6/2010, 7/24/2010 to 7/31/2010) (Table 1). Some gores were filled with data taken at other times. The non-polar images were map projected onto the GLD100 (WAC derived 100m/pixel DTM) while polar images were map projected on the LOLA shape model (80deg to 90deg N/S) and the GLD100 (60deg to 80deg N/S). Accurate positioning of each WAC image was ensured using ephemeris provided by the LOLA and GRAIL team and an improved camera geometry model (Speyerer, E.J. et al, 2014, Pre-flight and On-orbit Geometric Calibration of the Lunar Reconnaissance Orbiter Camera). To reduce brightness discrepancies across image boundaries, all images were corrected to a common photometric geometry using a Hapke model (Sato, H. et al, 2014, Resolved Hapke parameter maps of the Moon). This mosaic uses only the 643 nm band of the WAC. This HiPS has been created based on 100m resolution WAC Global Morphologic map byhttps://alasky.cds.unistra.fr/Planets/CDS_P_Moon_LROC-WAC-100mSurveyResearchIsDerivedFromArizona State University http://wms.lroc.asu.edu/lroc/view_rdr/WAC_GLOBALThis HiPS is distributed under ODbL license by Unistra/CNRShttps://alasky.cds.unistra.fr/Planets/CDS_P_Moon_LROC-WAC-100mhttps://alaskybis.cds.unistra.fr/Planets/CDS_P_Moon_LROC-WAC-100m55136 55620https://alasky.cds.unistra.fr/Planets/CDS_P_Moon_LROC-WAC-100m/Moc.fits