Astrometric Search For Extrasolar Planets In Stellar Multiple Systems

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We search for extrasolar planets with high precision relative astrometry (using AO assisted ground based imaging) in nearby stellar multiple systems, especially in binaries with low-mass stars. Using a narrow band-filter located at the near infrared to suppress differential chromatic refraction effects as well as an old globular cluster to monitor the astrometric long-term stability we achieve a final multi-epoch precision down to about 0.1 mas which enables us to find Jovian exoplanets around solar like stars and even less mass exoplanets around nearby low-mass stars. Because of a spatial resolution of about 0.1 arcsec, we are able to observe nearby binaries with apparent separations down to a few AU, which is less than the expected minimum separation allowing planet formation (about 20 AU), thus to study the conditions for planet formation in binaries. Such close binaries are difficult or even impossible to observe by other techniques like typical radial velocity observations or with PRIMA/VLTI due to the high spatial resolution needed to resolve them.
As a first result of our ongoing astrometric search program, we found a further stellar component in the exoplanet host binary HD19994 A & B. While searching the astrometric signal of the RV exoplanet around the A component (minimum signal about 0.15 mas), we detected the astrometric signal of a low mass star around HD19994B with a mass of about 0.34 solar masses. Looking at the residuals, an additional astrometric signal of more than 1 mas can be excluded and thus an upper mass limit of about 12 Jupiter masses can be given for the RV exoplanet around the primary.
T.R. and R.N thank the German Science Foundation for financial support (NE 515/23-1, NE 515/30-1, NE 515/33-1). A.S. acknowledge support from the National Science Foundation (NSF AST-0708074).

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