The selene project and the following lunar mission

The Pisgah Automated Survey: A Photometric Search for Low‐Mass Detached Eclipsing Binaries and Other Variable Stars

“…In actuality, the OGLE experiment detected two foreground eclipsing M dwarfs in a 2.4 deg 2 field centered at the Small Magellanic Cloud (Udalski et al 1998), while ASAS found two new binaries with estimated masses of about 0.8 in its first M , phase covering 300 deg 2 (Pojmanski 2000). The triangles in Figure 2 show the estimated locations of these four systems.…”

“…The simulation then distributes the binaries in space with random inclinations and with a space density that drops above and below the Galactic disk, following a two-component exponential to account for the thin and thick disk components (see Gilmore, King, & van der Kruit 1990). The binary magnitudes are assigned by look-up from the massmagnitude relations of Henry & McCarthy (1993), and the radii (Pojmanski 1997), the Pisgah Survey, and OGLE (Udalski et al 1998), respectively. From these histograms we conclude that a survey like ASAS will not be successful in detecting M dwarf eclipsing binaries, which have colors VϪ…”

“…Superimposed in this diagram we show two horizontal dotted lines at and 19.5, which represent the effective de-I p 12.0 tection limits of two published photometric surveys we have used to calibrate our simulation. 4 Those surveys, both conducted by the Warsaw University Observatory in Poland, are the Optical Gravitational Lensing Experiment (OGLE; Udalski et al 1992) and the All Sky Automated Survey (ASAS; Pojmanski 1997). Figure 3 shows the number distributions of binaries predicted by our simulations for those two surveys after applying the corresponding survey-dependent completion functions.…”

“…Once the magnitudes are adjusted in this way, the script assembles a separate light curve for each star, including now all the data collected up to this time. It is possible to identify variables from their light curves at this time using the strategy employed by Pojmanski (1997), who selected stars with standard deviations larger than expected for their magnitude. j I I Figure 10 shows graphically how this strategy would work for one of the fields monitored by the survey (stars above the dashed line in the figure are variable candidates).…”

Simulation of the Lunar Gravity Field Recovery Based on Lunar Solo and Bi‐Orbiters

“…In view that lunar satellite of China and Japan may fly around the moon simultaneously, there will be close cooperation between these two countries on VLBI measurement, and the observation data will be shared. The main orbiter of "SELENE" will be in a circular and polar orbit, and its height will be 100km [12] , the satellite will be more sensible to high degree coefficients of lunar gravity field. In simulation, the combination of simultaneous Doppler and VLBI tracking data of two satellites at heights of 200km and 100km is considered, and the D-VLBI (Differential-VLBI ) between these two satellites is not investigated here.…”