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The Earths transmission spectrum from lunar eclipse observations: The pale red dot. E. Palle, M.R. Zapatero-Osorio, R. Barrena, P. Montañes-Rodriguez,

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Presentation on theme: "The Earths transmission spectrum from lunar eclipse observations: The pale red dot. E. Palle, M.R. Zapatero-Osorio, R. Barrena, P. Montañes-Rodriguez,"— Presentation transcript:

1 The Earths transmission spectrum from lunar eclipse observations: The pale red dot. E. Palle, M.R. Zapatero-Osorio, R. Barrena, P. Montañes-Rodriguez, E. Martin, A. Garcia-Muñoz

2 But isolating the light from the planet is VERY challenging, what if direct detection is not possible? What about transiting Earths? Atmospheric characterization of Hot Jupiters has already been achieved trough transit spectroscopy

3 Poster 36: Montañes-Rodriguez et al.

4 We can observe it during a lunar eclipse NOT, Visible, μm WHT, Near-IR, μm La Palma, Canaries

5 Lunar eclipse August 16th 2008

6 Umbra Penumbra Brigth Moon

7 Umbra Umbra/Bright Bright HαHα

8 Earths Transmission Spectrum The pale red dot μmμm

9 O2O2 O3O3 Ca II H2OH2O Earths Transmission Spectrum Visible μmμm

10 O4O4 Ca II HαHα NO 2 ? Fraunhofer lines structure

11 CO 2 H2OH2O O 2O O 2 O 2O 2 O 2N 2 Earths Transmission Spectrum Near-IR ZJ μmμm

12 Atmospheric Dimers: Van de Waals molecules: Weakly bound complexes They are present as minor rather than trace species. One likely origin of continuum absorption. Observed on Earth (gas) and Jupiter (gas; (H 2 ) 2 ), Ganymede, Europa and Callisto (condensed), and in the laboratory (gas/condensed). Never on Venus/Mars, where there must be CO 2 – X NOT contained in the common spectral libraries Calo and Narcisi (1980)

13 CH 4 CO 2 H2OH2O Earths Transmission Spectrum Near-IR HK μmμm

14 How deep we see in the planet atmosphere? h T(h, ) Traub, 2009 h min ? Are antropogenic signatures visible in the lower layers? Is there a surface signal?

15 Evolution of the Earths Transmission Spectrum during the eclipse

16 Reflection vs Transmission

17 Earths Reflectance Spectrum: Earthshine Same instrumentation only two months apart μmμm

18 Reflected spectrumTransmission Spectrum CO 2 CH 4 O2O2 CO 2 Blue planet? O 2 O 2O 2 O 2N 2 O 2O 2 Palle et al, 2009 μmμm

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20 Thus, the transmission spectrum of telluric planets contains more information for the atmospheric characterization than the reflected spectrum. And it is also less technically challenging But, how far are we from making the measurements ?

21 F* F* - F* ( ) + F* ( ) T A a ____ A * A p*a ______ A * + Ruido

22 Wavelength (μm) Differential transit spectroscopy M star + Earth : 1 (2) measurement S s+p / S p

23 M8 star + 1 Earth... with the E-ELT ~5 h ~ 150 h ~ 50 h ~ 25 h Wavelength (μm) Work in progress...

24 Still, we must pursue the characterization with direct observations Exploration of surface features Presence of continents Rotational period Localized surface biomarkers (vegetation) Orbital light curve Ocean glints and polarization effects

25 Conclusions We have obtained the Earths transmission spectra μm First order detection and characterization of the main constituents of the Earth's atmosphere Detection of the Ionosphere : Ca II, ( Mg, Fe, ??) Detection of O 2 O 2 and O 2 N 2 interactions Offers more information than the reflectance spectra Using the measured Earth transmission spectrum and several stellar spectra, we compute the probability of characterizing a transiting earth with E-ELT For a Earth in the habitability zone of an M-star, it is possible to detect H 2 O, O 2, CH 4,CO 2 (= Life) within a few tens of hours of observations.

26 Thank you

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29 The Ring effect Rotational Raman Scattering (RRS) Early evidence: Sky-scattered Fraunhofer lines were less deep but broader than solar lines λ ex λ ex -Δλ, λ ex, λ ex +Δλ frequency redistribution Incident λ + Stokes + Anti-Stokes branches incident photon Incident exiting difference/ ratio

30 The Ring effect: Rotational Raman scattering Transmission spectrum Solar spectrum Vountas et al. (1998)

31 How deep we see in the planet atmosphere? Evidences? Ref.: Kaltenegger & Traub 2009

32 Nowadays we can monitor night lights, atmospheric changes, plankton blooms, forest health, etc...

33 But, how does our planet look like to ET?

34 We will need a detailed understanding of the micro-scale processes to interpret the observed macro-scale properties When observing an exoplanet, all the light will come from a single point.

35 Observing the Earth as a planet (no spatial resolution) Earth–as-a-point observations with a very remote sensor A compilation of high spatial resolution data into a global spectra or photometry, and modeling Earthshine Observations: The Earthshine is the ghostly glow on the dark side of the Moon

36 The Earthshine on the moon ES/MS = albedo (+ geometry and moon properties)

37 Leonardo da Vinci, Codex Leicester, 1510

38 Chappuis Ozone band B-O 2 A-O 2 Atmospheric Water vapor Rayleigh Scattering Spectral Albedo of the Earth: 2003/11/19 Montañés-Rodriguez et al., ApJ, 2006

39 Kaltenegger & Traub Palle et al, 2009

40 Calo and Narcisi (1980)

41 Terrestrial inner-orbit planets based on their transits: - About 50 planets if most have R ~ 1.0 Re - About 185 planets if most have R ~ 1.3 Re - About 640 planets if most have R ~ 2.2 Re (Or possibly some combination of the above) About 12% of the cases with two or more planets per system CoRoT & KEPLER can provide this input Many other surveys: Plato, TESS, Ground-based searches,...


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