Getting Precise Stellar Parameters in PLATOs first field PLATO science conference 24/25 th Feb 2011 T. Granzer, K.G. Strassmeier, & M. Weber Dedicated photometric characterization survey in Strmgren uvby n w and H Deliverables: (b-y), c1, m1, Teff, [M/H], log g; Flux F(H ) down to 13mag. Constraints: bright limit 9.5, faint 16mag First field (fixed) in southern hemisphere Challenge: 2000 2 A dedicated input catalog? Challenge: 2000 sq-deg Super Wasp-South (SAAO), 8x11.1cm lens optics, FoV 7.8x7.8,~35 pointings, filters on demand (?) (Paranal): 2.6m Ritchey- Crtien, FoV 1x1,~2000 pointings, ugriz&H RoboTel (C. Armazones): 80cm, Cassegrain, 33.5 arcmin, ~7500 pts., full Strmgren and H set (plus UBVRI, ugriz). Robotel NGC 891 LBT Mt.Graham 5min, seeing 0.8 B-band RoboTel in Potsdam 20min, seeing 3.3 V-band Identical Instrument on STELLA-1, 1.2m, Izaa 40 sec, on seeing 10 1 Bochum-University/Antofagasta Observatory at base of Cerro Armazones ~350 clear nights ~50% seeing < 1 Image: R. Chini Strmgren indices (b-y)for eff. Temperature m1=(v-b)-(b-y)for line blanketing c1=(u-v)-(v-b)for Balmer discontinuity For late-type (FGKM) stars (dwarfs), m1 is a good proxy for metallicity, c1 for log(g) Holmberg et al., A&A 475, 519 Ramirez & Melendez, ApJ 626, 446 rnadttir et al., A&A 521, A40 The calibrations used for error analysis are from: 3-year survey? 1300h/year h>30 85% clear nights Moon: 3-5 days around full moon Downtime