Development of software for high-precision LLR data analysis etc.

[Speaker 1]
Ryosuke Nagasawa, M1, SOKENDAI, Mitaka(supervisor : Hideo Hanada)
Development of software for high-precision LLR data analysis
We are developing new analysis software for precise determination of lunar orbital/rotational motion and tidal deformation using lunar laser ranging (LLR) observation data.
As the first step of the study, we construct an LLR observation model. This model consists of the lunar orbit and libration obtained from lunar-planetary ephemeris DE430 (provided by NASA JPL), and the other newest physical models compatible with IERS Conventions (2010) such as Earth orientation, solid Earth/Moon tides, and some factors affecting propagation delay. For the purpose of calculating these components precisely, we use the modules of the geodetic data analysis software “c5++” (Otsubo et al., Japan Geoscience Union Meeting 2011). LLR observation data are provided as normal points. In this calculation, there are 3577 points distributed from June 1996 to July 2013, obtained at 4 observatories: Apache Point, Grasse, Matera and McDonald. Comparing the observed and calculated one-way ranges, the mean and the standard deviation of the residuals are about 5.7 cm and 4.8 cm respectively.
The first step has almost finished. Currently we are working on the next step, the integration of lunar motion. This presentation contains the outline of LLR and the current status of the software development, including the details of above-mentioned modeling.

[Speaker 2]
Sumire Tatehora, D1, SOKENDAI, Mitaka(supervisor : Nobuo Arimoto)
Morphological studies of high-z massive galaxies
Thanks to the Cosmic Assembly Near-IR Deep Extragalactic Legacy Survey (CANDLES) HST/WFC3 imaging with high spatial resolution, we investigate the morphology of galaxies in the distant universe. We select 20 passively evolving galaxies and 586 star-forming galaxies at 1.4<phot-z<2.5 in the COSMOS-CANDELS 210 square arcmin field and measure effective radius and Se ́rsic index by using the GALFIT package (Peng et al. 2002). We present the results of size-mass, Se ́rsic index-mass relation and discuss whether it has correlation between galaxy morphology and BzK color.