Anthony Boccaletti Paris Observatory -France - Science in Santiago

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PERFORMANCE: MATURE PLANETSintensive simulations to assess the characterization capabilities (not just detection !!!) led by A.-L.Maire (Paris Obs.)use the Cahoy et al. (2010) models for gas/ice Giants and Stam (2008) models for telluricgiants: extrapolation of spectra to other spectral type than G (Flux conservation). no extrapolationin separation. We consider R = 1 R Jupitertelluric: the extrapolation is approximative because many features can change with Sp (red-edgeA.-L. Maire et al.: Exoplanet characterization using space high-contrast imagingfor instance). We consider R = 2.5 R Earthterization usingSNR-basedspace high-contrastcriterionimagingTable 6. Values of SNR r derived from Eq. (7).to distinguish between modelsTable 5. Star-planet separations for giant planets extrapolated toother stellar types assuming Eq. (3). The values for the solar-typestar are those modeled by Cahoy et al. (2010).Spectral type Luminosity (L⊙) Separations (AU)A0 28 4.2 10.6 26.5 53.0F0 4.8 1.8 4.4 11.0 21.9G2 1 0.8 2 5 10K0 0.45 0.5 1.3 3.4 6.7M0 0.09 0.24 0.6 1.5 3Planet Parameter SNR r NoteJupiter 0.8/2 AU 15Jupiter 0.8 AU metallicity 1/3x 30Jupiter 2 AU metallicity 1/3x 30 CH 4 bandsJupiter 5 AU metallicity 1/3x 30 CH 4 bandsNeptune 0.8/2 AU 15Neptune 0.8 AU metallicity 10/30x 30Neptune 2 AU metallicity 10/30x 25 CH 4 bandsForest Earth 0/50/100% clouds 25 blue channelsOcean Earth 0/50/100% clouds 25 blue channelsClear Earth 0/50/100% forests 12 red channels50% cloudy Earth 0/50/100% forests 30 red channelsCloudy Earth 0/50/100% forests 220 red channelsance of the “red edge” in the planet spectra depends stronglyon the cloud thickness and coverage, but it still alters the spec-Observing Planetary Systems II - Santiago, ChileNeptune analogs and super-Earths can be detected in the range2–4 AU for stars closer than 10 pc. There are no A stars within5pc(exceptfortheSiriusbinarysystem)sowedonotplotthe
PERFORMANCE - SPECTRAL TYPEM stars G stars A starslimit in separa,on [AU]Jupiter Neptune Super EarthA0 < 20 pc 1 -‐ 10 2 -‐ 3 2 -‐ 3G2 < 10pc 1 -‐ 7 1 -‐ 3 1 -‐ 2M0 < 5pc 0.5 -‐ 4 0.5 -‐ 1.5 0.5 -‐ 1Observing Planetary Systems II - Santiago, Chile
Page 1 and 2: Anthony BoccalettiParis Observatory
Page 3 and 4: TIMELINE OF EXOPLANETS DIRECTDETECT
Page 11 and 12: Observing Planetary Systems II - Sa
Page 13 and 14: PROPOSALformer proposal SEE COAST (
Page 15 and 16: TOP-LEVEL SCIENCEcharacterization o
Page 17 and 18: SCIENCE - GIANTSKarkoschka (1994)10
Page 19 and 20: SCIENCE - TELLURICSThe Earthsome Ea
Page 21 and 22: MISSION PARAMETERSThe recipe :Our c
Page 23 and 24: OPTO-MECHANICAL DESIGNOptical imple
Page 25 and 26: RAW CONTRASTInstrumental simulation
Page 27: PERFORMANCE: DISKSdisk science :- p
Page 31 and 32: SPECTROSCOPY - TELLURICNo cloudsSur
Page 33 and 34: WHAT’S NEXT ?SPICES not selected
Page 35: TECH. READINESS LEVELSPICES 21Table

Anthony Boccaletti Paris Observatory -France - Science in Santiago

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