Exoplanet Reflections: the light from 51 Peg b OHP - France, Oct. 7 - PowerPoint PPT Presentation

OHP2015: Twenty Years of Giant Exoplanets Exoplanet Reflections: the light from 51 Peg b OHP - France, Oct. 7 th 2015 Jorge H. C. Martins (ESO - Chile, IA/U. Porto) Supervisors: N. C. Santos & P. Figueira (IA/U. Porto), C. Melo (ESO - Chile) J. P. Faria & M. Montalto & S. G. Sousa & D. Cunha (IA/U. Porto) Colaborators: D. Ehrenreich & C. Lovis & M. Mayor & F. Pepe & S. Udry (Uni. Geneve) I. Boisse (LAM)

Introduction Method Results Future Why detect reflected light in the visible? In the optical, an exoplanet’s signal is essentially reflected light I It is essentially a copy of the star’s spectrum I It represents a direct detection of an exoplanet I Some pioneering reflected light studies I Collier Cameron et al. (1999); Charbonneau et al. (1999) More recently: I Leigh et al. (2003); Rodler et al. (2010)

Introduction Method Results Future Why detect reflected light in the visible? Permits a direct characterisation of the planet Dynamics I inclination and real mass (e.g. Rodler et al. 2012) I rotation (e.g. Kawahara 2012) I atmosphere physics (winds, e.g. Snellen et al. 2010) I Interiors I composition ( H 2 O , CH 4 , e.g. Swain et al. 2008) I albedo (e.g. Demory 2014) I

Introduction Method Results Future Why detect reflected light in the visible? Permits a direct characterisation of the planet Dynamics I inclination and real mass (e.g. Rodler et al. 2012) I rotation (e.g. Kawahara 2012) I atmosphere physics (winds, e.g. Snellen et al. 2010) I Interiors I composition ( H 2 O , CH 4 , e.g. Swain et al. 2008) I albedo (e.g. Demory 2014) I

Introduction Method Results Future Why the albedo? It is highly dependent of the composition of the planet’s atmosphere

Introduction Method Results Future Why the albedo? It is highly dependent of the composition of the planet’s atmosphere High albedos are typically associated with high-altitude condensates I

Introduction Method Results Future Why the albedo? It is highly dependent of the composition of the planet’s atmosphere High albedos are typically associated with high-altitude condensates I Low albedos are caused by strong atomic/molecular gas absorption in I cloud-poor atmospheres.

Introduction Method Results Future Problem

Introduction Method Results Future Problem F Planet F Star = A g

Introduction Method Results Future Problem F Planet F Star = A g g ( α )

Introduction Method Results Future Problem ! R P " 2 F Planet F Star = A g g ( α ) a

Introduction Method Results Future Problem ! R P " 2 F Planet F Star = A g g ( α ) a F Planet ≈ 6 . 8 × 10 ≠ 5 R = R Jup , P = 2 days , A g = 0 . 3: F Star

The Method

Introduction Method Results Future The Cross Correlation Function (e.g. Baranne et al. 1996) Wavelenght Radial Velocity

Introduction Method Results Future The Cross Correlation Function (e.g. Baranne et al. 1996) Wavelenght Radial Velocity

Introduction Method Results Future The Cross Correlation Function (e.g. Baranne et al. 1996) Wavelenght Radial Velocity

Introduction Method Results Future The Cross Correlation Function (e.g. Baranne et al. 1996) Wavelenght Radial Velocity

Introduction Method Results Future The Cross Correlation Function (e.g. Baranne et al. 1996) Wavelenght Radial Velocity

Introduction Method Results Future The Cross Correlation Function (e.g. Baranne et al. 1996) Wavelenght Radial Velocity S / N CCF = √ n S / N spectrum

Introduction Method Results Future The Cross Correlation Function (e.g. Baranne et al. 1996) Wavelenght Radial Velocity S / N CCF = √ n S / N spectrum for a binary mask with 3600 lines, the S/N increases 60 times!!!

Introduction Method Results Future The Cross Correlation Function

Introduction Method Results Future The Cross Correlation Function

Introduction Method Results Future The Cross Correlation Function

Introduction Method Results Future Detecting the planetary signal Planet+Star Martins et al, 2013 Observations MNRAS, 436(2), 1215-1224

Introduction Method Results Future Detecting the planetary signal Planet+Star Martins et al, 2013 Observations MNRAS, 436(2), 1215-1224 CCF Planet+Star CCFs

Introduction Method Results Future Detecting the planetary signal Planet+Star Martins et al, 2013 Observations MNRAS, 436(2), 1215-1224 CCF Planet+Star CCFs Star removal Individual Planet CCFs

Introduction Method Results Future Detecting the planetary signal Planet+Star Martins et al, 2013 Observations MNRAS, 436(2), 1215-1224 CCF Planet+Star CCFs Star removal Individual Planet CCFs RV Correction and CCF stack Planet Signal

What can be done with this?

Introduction Method Results Future The Data 51 Peg b; I (Mayor & Queloz 1995)

Introduction Method Results Future The Data 51 Peg b; I HARPS@ESO’s 3.6m; I

Introduction Method Results Future The Data 51 Peg b; I HARPS@ESO’s 3.6m; I 90 spectra / ∼ 12.5h ; I

Introduction Method Results Future The Data 51 Peg b; I HARPS@ESO’s 3.6m; I 90 spectra / ∼ 12.5h ; I ∼ 20 spectra I

Introduction Method Results Future What we found: 6.0 ± 0.4 × 10 ≠ 5 Amplitude Significance 3.7 ± 0.2 σ noise 22.6 ± 3.6 km s ≠ 1 FWHM

Introduction Method Results Future What we found: 6.0 ± 0.4 × 10 ≠ 5 Amplitude Significance 3.7 ± 0.2 σ noise 22.6 ± 3.6 km s ≠ 1 FWHM ⇓ Inflated hot Jupiter with high albedo!

Introduction Method Results Future What we found: 132 + 19 ≠ 15 km s ≠ 1 k planet

Introduction Method Results Future What we found: 132 + 19 ≠ 15 km s ≠ 1 k planet ⇓ 0.46 + 0 . 06 Real mass ≠ 0 . 01 M Jup 80 + 10 Inclination ¶ ≠ 19

The Future

Introduction Method Results Future Next generation of Observing Facilities

Introduction Method Results Future 2 Day Jupiter with EELT (from Martins et al. 2013)

Introduction Method Results Future Ultimate goal Variation of Earth’s geometric albedo over 24h (from Garcìa Muñoz 2014)

Introduction Method Results Future Summary The detection of reflected light at optical wavelengths from other I planets is already possible We were able to recover the reflected visible light spectrum of 51Peg on I its orbiting planet 51 Peg b is most likely an inflated hot Jupiter with a high albedo I Future generation of instruments and observing facilities will allow us to I better characterise the planets.

Introduction Method Results Future Summary The detection of reflected light at optical wavelengths from other I planets is already possible We were able to recover the reflected visible light spectrum of 51Peg on I its orbiting planet 51 Peg b is most likely an inflated hot Jupiter with a high albedo I Future generation of instruments and observing facilities will allow us to I better characterise the planets. Thank you!