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

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

Mar 18, 2023 135 likes •577 views

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 -

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OHP2015: Twenty Years of Giant Exoplanets

Exoplanet Reflections: the light from 51 Peg b

OHP - France, Oct. 7th 2015

Jorge H. C. Martins

(ESO - Chile, IA/U. Porto)

Supervisors:

  • N. C. Santos & P. Figueira (IA/U. Porto), C. Melo (ESO - Chile)

Colaborators:

  • J. P. Faria & M. Montalto & S. G. Sousa & D. Cunha (IA/U. Porto)
  • D. Ehrenreich & C. Lovis & M. Mayor & F. Pepe & S. Udry (Uni. Geneve)
  • I. Boisse (LAM)
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Introduction Method Results Future

Why detect reflected light in the visible?

I 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 Collier Cameron et al. (1999); Charbonneau et al. (1999) I More recently: Leigh et al. (2003); Rodler et al. (2010)

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Introduction Method Results Future

Why detect reflected light in the visible?

Permits a direct characterisation of the planet I 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 (H2O, CH4, e.g. Swain et al. 2008) I albedo (e.g. Demory 2014)

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Introduction Method Results Future

Why detect reflected light in the visible?

Permits a direct characterisation of the planet I 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 (H2O, CH4, e.g. Swain et al. 2008) I albedo (e.g. Demory 2014)

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Introduction Method Results Future

Why the albedo?

It is highly dependent of the composition of the planet’s atmosphere

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Introduction Method Results Future

Why the albedo?

It is highly dependent of the composition of the planet’s atmosphere I High albedos are typically associated with high-altitude condensates

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Introduction Method Results Future

Why the albedo?

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

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Introduction Method Results Future

Problem

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Introduction Method Results Future

Problem

FPlanet FStar = Ag

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Introduction Method Results Future

Problem

FPlanet FStar = Ag g(α)

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Introduction Method Results Future

Problem

FPlanet FStar = Ag g(α)

! RP

a

"2

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Introduction Method Results Future

Problem

FPlanet FStar = Ag g(α)

! RP

a

"2

R = RJup, P = 2days, Ag = 0.3:

FPlanet FStar

≈ 6.8 × 10≠5

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The Method

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Introduction Method Results Future

The Cross Correlation Function

(e.g. Baranne et al. 1996) Wavelenght Radial Velocity

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Introduction Method Results Future

The Cross Correlation Function

(e.g. Baranne et al. 1996) Wavelenght Radial Velocity

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Introduction Method Results Future

The Cross Correlation Function

(e.g. Baranne et al. 1996) Wavelenght Radial Velocity

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Introduction Method Results Future

The Cross Correlation Function

(e.g. Baranne et al. 1996) Wavelenght Radial Velocity

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Introduction Method Results Future

The Cross Correlation Function

(e.g. Baranne et al. 1996) Wavelenght Radial Velocity

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Introduction Method Results Future

The Cross Correlation Function

(e.g. Baranne et al. 1996) Wavelenght Radial Velocity S/NCCF = √n S/Nspectrum

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Introduction Method Results Future

The Cross Correlation Function

(e.g. Baranne et al. 1996) Wavelenght Radial Velocity S/NCCF = √n S/Nspectrum for a binary mask with 3600 lines, the S/N increases 60 times!!!

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Introduction Method Results Future

The Cross Correlation Function

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Introduction Method Results Future

The Cross Correlation Function

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Introduction Method Results Future

The Cross Correlation Function

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Introduction Method Results Future

Detecting the planetary signal

Planet+Star Observations Martins et al, 2013 MNRAS, 436(2), 1215-1224

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Introduction Method Results Future

Detecting the planetary signal

Planet+Star Observations Martins et al, 2013 MNRAS, 436(2), 1215-1224 Planet+Star CCFs CCF

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Introduction Method Results Future

Detecting the planetary signal

Planet+Star Observations Martins et al, 2013 MNRAS, 436(2), 1215-1224 Planet+Star CCFs Individual Planet CCFs CCF Star removal

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SLIDE 27

Introduction Method Results Future

Detecting the planetary signal

Planet+Star Observations Martins et al, 2013 MNRAS, 436(2), 1215-1224 Planet+Star CCFs Individual Planet CCFs Planet Signal CCF Star removal RV Correction and CCF stack

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SLIDE 28

What can be done with this?

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Introduction Method Results Future

The Data

I 51 Peg b;

(Mayor & Queloz 1995)

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Introduction Method Results Future

The Data

I 51 Peg b; I HARPS@ESO’s 3.6m;

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Introduction Method Results Future

The Data

I 51 Peg b; I HARPS@ESO’s 3.6m; I 90 spectra / ∼12.5h ;

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Introduction Method Results Future

The Data

I 51 Peg b; I HARPS@ESO’s 3.6m; I 90 spectra / ∼12.5h ; I ∼ 20 spectra

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Introduction Method Results Future

What we found:

Amplitude 6.0±0.4×10≠5 Significance 3.7±0.2σnoise FWHM 22.6±3.6km s≠1

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Introduction Method Results Future

What we found:

Amplitude 6.0±0.4×10≠5 Significance 3.7±0.2σnoise FWHM 22.6±3.6km s≠1

⇓

Inflated hot Jupiter with high albedo!

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Introduction Method Results Future

What we found:

kplanet 132+19

≠15 km s≠1

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SLIDE 36

Introduction Method Results Future

What we found:

kplanet 132+19

≠15 km s≠1

⇓

Real mass 0.46+0.06

≠0.01 MJup

Inclination 80+10

≠19 ¶

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The Future

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Introduction Method Results Future

Next generation of Observing Facilities

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Introduction Method Results Future

2 Day Jupiter with EELT

(from Martins et al. 2013)

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Introduction Method Results Future

Ultimate goal

Variation of Earth’s geometric albedo over 24h (from Garcìa Muñoz 2014)

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Introduction Method Results Future

Summary

I The detection of reflected light at optical wavelengths from other planets is already possible I We were able to recover the reflected visible light spectrum of 51Peg on its orbiting planet I 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 better characterise the planets.

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Introduction Method Results Future

Summary

I The detection of reflected light at optical wavelengths from other planets is already possible I We were able to recover the reflected visible light spectrum of 51Peg on its orbiting planet I 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 better characterise the planets.

Thank you!