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lec03_05oct2009

lec03_05oct2009 - Extrasolar planet detection Methods and...

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Extrasolar planet detection: Methods and limits Ge/Ay133
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Spectral Energy Distributions (or, Blinded by the light!...)
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How do you find a planet? Look for it? Hard (as we’ve seen)! Only planets imaged are very young and far from their stars. Are such objects common or rare?
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How do you find a planet? Look for it? Hard! Where should you look? Few AU? Look for its affect on the star? (Indirect)
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Astrometric displacement of the Sun due to Jupiter as seen from a distance of 10 pc (Current state of the art w/Keck AO = 200  μ as, as of 2007) 200 μ as
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Discovery space for indirect methods: Radial velocity Astrometry ( r =distance to the star)
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Radial velocity signature is distance independent (S/N is not!) First (written) proposal by Otto Struve, The Observatory 72, p. 199-200 (1952) 51 Peg announced in 1995 (PSR 1257+12 in 1992). .
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Spectroscopy with Echelles: Photons have come a long way, don’t lose them! Echelle spectrometers in conjunction with large format arrays can provide R~30,000-100,000 spectra across the entire visible or near-IR range ( λ< 5 μ m, good for late type stars and brown dwarfs).
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