Re-evaluating the Very Hot Gas Giant WASP-12b

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Step 4: Keck1/MOSFIRE Multi-Object Eclipse Spectroscopy of WASP-12b: scheduled for Oct. 2012 28
Conclusions: ● An M0 dwarf is located only 1” from WASP-12: observers must correct for this object! Also: is it physically associated with WASP-12? ● WASP-12b has a nearly isothermal NIR photosphere, so its C/O ratio cannot be uesfully constrained with the present data. ● Controversies remain: ● How prolate is WASP-12b? ● What is the correct 4.5 µm flux? ● Additional Spitzer measurements can resolve both these issues! Crossfield et al., submitted 29
Page 1 and 2: Re-evaluating the Very Hot Gas Gian
Page 3 and 4: E Transiting Planets with Measured
Page 5 and 6: The Extreme Planet WASP-12b: Period
Page 7 and 8: Modeling of initial eclipse photome
Page 9 and 10: Step 1: Subaru/MOIRCS narrowband 2.
Page 11 and 12: Planet/star Flux Ratio (10 -3 ) Cro
Page 13 and 14: Campo+2011 Cowan+2012 4.5µm Eclips
Page 15 and 16: A fainter star very close to WASP-1
Page 17 and 18: IRTF/SpeX K-band imaging shows that
Page 19 and 20: Transit/Eclipse contamination Keck/
Page 21 and 22: Dilution-corrected planetary spectr
Page 23 and 24: The similarly hot (~3200 K) planet
Page 25 and 26: A high C/O ratio cannot be defended
Page 27: Followup observations will confirm
Page 32 and 33: de Mooij poster; Preliminary! Swain
Page 34: Planet/Star Flux Density (10 -3 ) F

Re-evaluating the Very Hot Gas Giant WASP-12b

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