Mass Astronomical Data at Dome A and VO Qiang LIU (NAOC/CCAA)
Outline Kunlun Station CSTAR AST3 Database and VO
Why Dome A? Kunlun Station at Dome A Position: 80.25 S, 77.06 E Temperature: Mean: -50 C Lowest: -80 C Altitude: 4093m Will Saunders et al, 2009
Kunlun Station at Dome A Why Dome A? Credit: Zhaohui SHANG Position: 80.25 S, 77.06 E Temperature: Mean: -50 C Lowest: -80 C Altitude: 4093m Will Saunders et al, 2009
Kunlun Station at Dome A Why Dome A? Credit: Zhaohui SHANG Position: 80.25 S, 77.06 E Temperature: Mean: -50 C Lowest: -80 C Altitude: 4093m Will Saunders et al, 2009
Kunlun Station at Dome A Why Dome A? Credit: Zhaohui SHANG Credit: Zhaohui SHANG Position: 80.25 S, 77.06 E Temperature: Mean: -50 C Lowest: -80 C Altitude: 4093m Will Saunders et al, 2009
Chinese Small Telescope Array (CSTAR) 4 telescopes with diameter 14.5cm, 1Kx1K CCD FOV: 4.5 O x4.5 O, all point to the south pole Filters: g, r, i and none filters, without any mechanical moveable instrument Installed at Dome A in Jan. 2008 by Xu ZHOU and Zhenxi ZHU
Chinese Small Telescope Array (CSTAR) 4 telescopes with diameter 14.5cm, 1Kx1K CCD FOV: 4.5 O x4.5 O, all point to the south pole Filters: g, r, i and none filters, without any mechanical moveable instrument Installed at Dome A in Jan. 2008 by Xu ZHOU and Zhenxi ZHU
Scientific Goal and Data Scientific Goal: atmosphere extinction, sky brightness, variable stars Hu ZOU et al., 2010, AJ Lingzhi WANG et al., 2010, prepared Data: 2008: ~360G 2009: ~1.15T 2010: ~1.0T
Scientific Goal and Data Dome A Cloud Coverage (Zou et al. 2010) Scientific Goal: atmosphere extinction, sky brightness, variable stars Hu ZOU et al., 2010, AJ Lingzhi WANG et al., 2010, prepared Data: 2008: ~360G 2009: ~1.15T 2010: ~1.0T
Scientific Goal and Data Dome A sky Cloud backgroud Coverage (Zou et et al. al. 2010) Scientific Goal: atmosphere extinction, sky brightness, variable stars Hu ZOU et al., 2010, AJ Lingzhi WANG et al., 2010, prepared Data: 2008: ~360G 2009: ~1.15T 2010: ~1.0T Median Sky Brightness (i-band) Dome A 20.5 La Palm (Spain) 20.10 Cerro Tololo (Chile) 20.07 Paranal (Chile) 19.93 Calar Alto (Spain) 19.57
Antarctic Schmidt Telescopes (AST3) Clear aperture500mm, Primary mirror: 680mm Wave band: 400nm 900nm (g, r, i filter for 3 telescopes ) Field of view: 4.14 Scale1 arcsec/pixel Image quality: 80% light energy encircled in 1 pixel Total oprcal length: 2.4m CCD: STA1600, 9micron /pixel, 10K 10K: 5KX10K
Schedule: Installation in 2011-2012 Survey Operation: 2012 2017
Credit: Xuefei GONG Schedule: Installation in 2011-2012 Survey Operation: 2012 2017
Scientific Goal of Data Scientific goal: Studies of Type Ia supernovae and the dark energy of the universe Microlensing and searching for extrasolar planets Variable stars Astroseismology Site testing such as measurement of atmosphere extinction and sky brightness Data: 2minX120d: ~16T for 1 AST3
Database and VO-CSTAR CSTAR in 2008: only SDSS i band Sources: more than 10000, limit mag. ~16 mag (Zhou et al. 2010, PASP), published at NAOC Science Data Center Visit: several GB 162 variables (Wang et al. 2010, prepared) CSTAR in 2009: will be published soon Credit: Lifan WANG
Database and VO-CSTAR CSTAR in 2008: only SDSS i band Sources: more than 10000, limit mag. ~16 mag (Zhou et al. 2010, PASP), published at NAOC Science Data Center Visit: several GB 162 variables (Wang et al. 2010, prepared) CSTAR in 2009: will be published soon Credit: Lifan WANG
Database and VO-AST3 2000 deg 2 Cosmological Survey Continuous observation for > 120 days Data reduction on-line
Database and VO-AST3 Supernovae - >2000 SNIa to z ~ 0.15 LMC continuous monitoring - Variable stars - Microlensing - Dark matter Galactic center continuous monitoring - Variable stars/microlensing/transients Galactic structure - RR Lyrae/Cepheids
Summary: We will get mass astronomical data from the telescopes at Dome A: 1.0T (CSTAR) + 48T (AST3) + more (2.5m ) We will publish the data under the collaboration with NAOC Science Data Center VO data is necessary for us: survey plancalibration
Thanks