Spectroscopic Signatures of Terrestrial Exoplanets Adam Kraus.

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Presentation transcript:

Spectroscopic Signatures of Terrestrial Exoplanets Adam Kraus

What are the expected spectral features of terrestrial exoplanets? What can we learn from them about local conditions and chemistry? What does this imply about design options for future planet-search missions?

Signature: Vibrational Transitions Not all molecules (N 2, O 2 ) are IR active Those of interest: H 2 O (Asymmetric Top) CH 4 (Symmetric Top) N 2 O (Asymmetric Linear) CO 2 (Symmetric Linear) Absorption strength => Abundances Resolution of lines => P, T Presence => Nonequilibrium chemistry

Infrared Spectra

Signature: Photodissociation O 3 is produced in the upper atmosphere: O + O 2 => O 3 thus it is a tracer gas. O 3 photodissociates in two bands: –Chappuis band: nm –Huggins-Hartley band: Shortward of 300 nm, photodissociation of other molecules absorbs all light

Optical Absorption Spectrum

Signature: Broadband Colors Terrain types like ocean, vegetation, and soil have distinctive albedos and colors: –Ocean: Albedo 5%, blue color –Soil:Albedo 20%, red color –Vegetation:Albedo 20%, green color On a planet with differentiated terrain, rotation will lead to variability in both color and reflected luminosity

Optical Reflection Spectra

TPF: Terrestrial Planet Finder Goal: Directly observe terrestrial exoplanets Scheduled to launch in mid-2010s Two technology choices: –Optical coronagraph –Infrared interferometer

Technology Choice: Coronagraph coronagraph.html tpf_sample.cfm

Technology Choice: Interferometer about.html

Comparative Benefits Coronagraph: –Broadband colors (Geography, vegetation) –Optical/NIR spectra (O 3, H 2 O) Interferometer –NIR/MIR spectra (H 2 O, CO 2, N 2 O, CH 4 ) Decision pending the outcome of precursor projects like Kepler and SIM.