In data from three clear nights of a WHT/UES run in 2000 Oct/Nov , and using improved Doppler tomographic signal-analysis techniques , we have carried out a deep search for starlight reflected from the innermost of \upsilon ( upsilon ) And ’ s three planets .
We place upper limits on the planet ’ s radius R _ { p } as functions of its projected orbital velocity K _ { p } \approx 139 \sin { i } km s ^ { -1 } for various assumptions about the wavelength-dependent geometric albedo spectrum p ( \lambda ) of its atmosphere .
For a grey albedo p we find R _ { p } \sqrt { p } < 0.98 ~ { } R _ { J } with 0.1 % false-alarm probability ( 4- \sigma ) .
For a ? Class V model atmosphere , the mean albedo in our 380-676 nm bandpass is \left < p \right > \sim 0.42 , requiring R _ { p } < 1.51 ~ { } R _ { J } , while an ( isolated ) Class IV model with \left < p \right > \sim 0.19 requires R _ { p } < 2.23 ~ { } R _ { J } .
The star ’ s v _ { rot } \sin { i } \sim 10  km s ^ { -1 } and estimated rotation period P _ { rot } \sim 10 d suggest a high orbital inclination i \sim 70 - 80 ^ { \circ } .
We also develop methods for assessing the false-alarm probabilities of faint candidate detections , and for extracting information about the albedo spectrum and other planetary parameters from faint reflected-light signals .