Presentation is loading. Please wait.

Presentation is loading. Please wait.

Kepler + Keck: Planet Masses and Densities Kepler + Keck: Planet Masses and Densities Geoff Marcy UC Berkeley + Preliminary Results.

Published byClemence Chase Modified over 8 years ago

Similar presentations

Presentation on theme: "Kepler + Keck: Planet Masses and Densities Kepler + Keck: Planet Masses and Densities Geoff Marcy UC Berkeley + Preliminary Results."— Presentation transcript:

1 Kepler + Keck: Planet Masses and Densities Kepler + Keck: Planet Masses and Densities Geoff Marcy UC Berkeley + Preliminary Results

2 Howard Isaacson, Jason Rowe, Andrew Howard, John Johnson Acknowledgements Acknowledgements William Borucki David Koch Stephen Bryson Jason Rowe David Charbonneau Guillermo Torres Francois Fressin Jean-Michel Désert Lars Buchhave Sam Quinn Dan Fabrycky Debra Fischer Natalie Batalha Thomas Gautier Steve Howell Charlie Sobeck David Latham Ron Gilliland Eric Ford Elliott Horsch Tom Barclay Jessie Christiansen Jack Lissauer Dimitar Sasselov Sara Seager Jon Jenkins Mike Haas Doug Caldwell Jeff Van Cleve David Ciardi Jeff Smith Martin Still Martin Stumpe Peter Tenebaum Lucianne Walkowicz Bill Cochran Mike Endl Leslie Rogers Special Thanks to:

3 Howard Isaacson, Jason Rowe, Andrew Howard, John Johnson Special Thanks to: Acknowledgements Acknowledgements William Borucki David Koch Stephen Bryson Jason Rowe David Charbonneau Guillermo Torres Francois Fressin Jean-Michel Désert Lars Buchhave Sam Quinn Dan Fabrycky Debra Fischer Natalie Batalha Thomas Gautier Steve Howell Charlie Sobeck David Latham Ron Gilliland Eric Ford Elliott Horsch Tom Barclay Jessie Christiansen Jack Lissauer Dimitar Sasselov Sara Seager Jon Jenkins Mike Haas Doug Caldwell Jeff Van Cleve David Ciardi Jeff Smith Martin Still Martin Stumpe Peter Tenebaum Lucianne Walkowicz Bill Cochran Mike Endl Leslie Rogers Kepler’s Heavy Lifters

4 4 Mass-Radius Diagram

5 5 Value of planet masses: - Fraction Rocky vs. R PL - Interior Structure - Formation Physics

6 10-meter Keck Telescope HiRES Spectrometer

7 Doppler Work at Vmag = 13.9 Challenges: Moonlight, Sky lines, Cosmic rays Kepler-8: (45 min, Full moon)

8 Red CCD Middle CCD Blue CCD 8000 A 3600 A Kepler-8 V = 13.5 mag Keck- HiRES Spectrometer

9 Doppler Precision: <2.0 m/s RMS = 2.0 m/s RMS includes Stellar jitter RV “Standard”: HD 182488 (G8V)

10 KOIs with Keck Multi-Epoch RVs 7 17 18 20 22 70 72 84 87 97 137 157 377 157 377 975 1611 104 108 111 112 116 122 123 148 153 180 244 245 246 261 263 274 281 283 284 285 292 295 299 305 306 309 314 316 321 323 365 719 1442 Published RV Work In Progress This List Available from David Ciardi (NExSci) 5 6 8 41 42 82 85 94 103

11 KOIs with Keck Multi-Epoch RVs 7 17 18 20 22 70 72 84 87 97 137 157 377 157 377 975 1611 104 108 111 112 116 122 123 148 153 180 244 245 246 261 263 274 281 283 284 285 292 295 299 305 306 309 314 316 321 323 365 719 1442 Published RV Work In Progress This List Available from David Ciardi (NExSci) 5 6 8 41 42 82 85 94 103

12 KOIs with Keck Multi-Epoch RVs 7 17 18 20 22 70 72 84 87 97 137 157 377 157 377 975 1611 104 108 111 112 116 122 123 148 153 180 244 245 246 261 263 274 281 283 284 285 292 295 299 305 306 309 314 316 321 323 365 719 1442 Published RV Work In Progress This List Available from David Ciardi (NExSci) 5 6 8 41 42 82 85 94 103 WARNING: UNPUBLISHED, PRELIMINARY RESULTS AHEAD

13 Phased Light Curve: KOI-246 R = 2.57 R E P = 5.40 d R STAR from SME analysis of Spectrum, Asteroseismology & Evol. Model

14 Phased Light Curve: KOI-246 R = 2.57 R E P = 5.40 d R STAR from SME analysis of Spectrum, Asteroseismology & Evol. Model Density = ?

15 KOI-246 A Second Transiting Planet Cand. R = 1.13 R Earth R = 1.13 R E P=9.60 d

16 KOI-246 A Second Transiting Planet Cand. R = 1.13 R Earth R = 1.13 R E P=9.60 d Density = ?

17 RVs for KOI-246

18 Outer, Non-Transiting Planet

19 Phased RVs for KOI-246 RVs in phase w/ Transits. Mass = 8.49 M Earth Density: 2.75 g/cc Rock + volatiles? (see L.Rogers)

20 Phased RVs for KOI-246.02 R = 1.13 R E Nondetection: Too low mass.

21 RVs for Third Planet: Non-Transiting

22 MCMC Planet Mass Determination

23 R = 2.57 R E Rho = 2.76 g/cc Rock + Volatiles?

24 KOI-104 P = 2.51 d R = 3.39 R E

25 RVs for KOI-104

26 Phased RVs for KOI-104

27 RVs for 2 nd Planet Non-Transiting

28 MCMC Mass Determination

29 R = 3.39 R E Rho = 1.91 g/cc

30 KOI-321 R=1.70 R E P = 2.43 d

31 RVs for KOI-321

32 Phased RVs for KOI-321

33 MCMC Mass Analysis: KOI-321

34 R = 1.70 RE Rho = 7.43 g/cc Mostly Rock?

35 Future of Precise RVs of KOIs RV + TTV  Planet masses

36 Future of Precise RVs of KOIs RV + TTV  Planet masses Photometry  RV Correction (Aigrain, Pont, et al.)

37 Future of Precise RVs of KOIs RV + TTV  Planet masses Photometry  RV Correction (Aigrain, Pont, et al.) Priors for PSF of Keck spectrometer

38 Future of Precise RVs of KOIs RV + TTV  Planet masses Photometry  RV Correction (Aigrain, Pont, et al.) Priors for PSF of Keck spectrometer HARPS-North & New, Improved SOPHIE

39 Preliminary Results Transition from Neptune-like to Rocky: < 2.5 R E

40 Preliminary Results Transition from Neptune-like to Rocky: < 2.5 R E Fraction of Planets that are Rocky vs. R PL : Key Goal of Extended Kepler Mission

41 Preliminary Results Transition from Neptune-like to Rocky: < 2.5 R E Fraction of Planets that are Rocky vs. R PL : Key Goal of Extended Kepler Mission RV Spectrometers on Big Telescopes (and TTV work) in Northern Hemisphere are needed.

42 42 Preliminary and Not Shown Mass-Radius Diagram 246 104 321

Download ppt "Kepler + Keck: Planet Masses and Densities Kepler + Keck: Planet Masses and Densities Geoff Marcy UC Berkeley + Preliminary Results."

Similar presentations

Astrobiology in the Context of a Research University Dimitar D. Sasselov Center for Planetary Astrophysics & Department of Astronomy Harvard University.

Astrobiology in the Context of a Research University Dimitar D. Sasselov Center for Planetary Astrophysics & Department of Astronomy Harvard University.
A Search for Earth-size Planets Borucki – Page 1 KEPLER; Data Validation and Follow Up Observations CoRoT Symposium W.J. Borucki & the Kepler Team 5 February.

A Search for Earth-size Planets Borucki – Page 1 KEPLER; Data Validation and Follow Up Observations CoRoT Symposium W.J. Borucki & the Kepler Team 5 February.
K2 Kepler’s Second Mission 1 K2 - a 2-wheel Kepler mission; The second highest peak in the world, a worthy ascent Steve B. Howell NASA Ames Research Center.

K2 Kepler’s Second Mission 1 K2 - a 2-wheel Kepler mission; The second highest peak in the world, a worthy ascent Steve B. Howell NASA Ames Research Center.
Exoplanet Atmospheres: Insights via the Hubble Space Telescope Nicolas Crouzet 1, Drake Deming 2, Peter R. McCullough 1 1 Space Telescope Science Institute.

Exoplanet Atmospheres: Insights via the Hubble Space Telescope Nicolas Crouzet 1, Drake Deming 2, Peter R. McCullough 1 1 Space Telescope Science Institute.
Adding a LASER Frequency Comb to NIRSPEC Peter Plavchan, NExScI Keck Science Meeting 2009.

Adding a LASER Frequency Comb to NIRSPEC Peter Plavchan, NExScI Keck Science Meeting 2009.
Investigating the structure of transiting planets, from hot Jupiters to Kepler super Earths Jonathan Fortney University of California, Santa Cruz Thanks.

Investigating the structure of transiting planets, from hot Jupiters to Kepler super Earths Jonathan Fortney University of California, Santa Cruz Thanks.
Lecture 1: Introduction & Methods 1.Introduction 2.Techniques for discovery & study 3.The NASA Kepler mission Planetary Systems Orbiting Diverse Stars.

Lecture 1: Introduction & Methods 1.Introduction 2.Techniques for discovery & study 3.The NASA Kepler mission Planetary Systems Orbiting Diverse Stars.
Prospects for measuring η-Earth from RV David W. Latham Harvard-Smithsonian Center for Astrophysics 5 Octoberber 2013.

Prospects for measuring η-Earth from RV David W. Latham Harvard-Smithsonian Center for Astrophysics 5 Octoberber 2013.
The Kepler Input Catalog and Follow-Up Observations Dave Latham for the Kepler Team 6 June 2006.

The Kepler Input Catalog and Follow-Up Observations Dave Latham for the Kepler Team 6 June 2006.
Reaching the 1% accuracy level on stellar mass and radius determinations from asteroseismology Valerie Van Grootel (University of Liege) S. Charpinet (IRAP.

Reaching the 1% accuracy level on stellar mass and radius determinations from asteroseismology Valerie Van Grootel (University of Liege) S. Charpinet (IRAP.
Exoplanet- Asteroseismology Synergies Bill Chaplin, School of Physics & Astronomy University of Birmingham, UK EAHS2012, Oxford, 2012 March 15.

Exoplanet- Asteroseismology Synergies Bill Chaplin, School of Physics & Astronomy University of Birmingham, UK EAHS2012, Oxford, 2012 March 15.
Science Opportunities for HARPS-NEF David W. Latham PDR - 6 December 2007.

Science Opportunities for HARPS-NEF David W. Latham PDR - 6 December 2007.
Stellar obliquities in exoplanetary systems

Stellar obliquities in exoplanetary systems
Exoplanet Transits and SONG Angelle Tanner. Venus Transiting the Sun.

Exoplanet Transits and SONG Angelle Tanner. Venus Transiting the Sun.
Terrestrial Planets. II. 1.Earth as a planet: interior & tectonics. 2.Dynamics of the mantle 3.Modeling terrestrial planets.

Terrestrial Planets. II. 1.Earth as a planet: interior & tectonics. 2.Dynamics of the mantle 3.Modeling terrestrial planets.
All About Exoplanets Dimitar D. Sasselov Harvard-Smithsonian Center for Astrophysics.

All About Exoplanets Dimitar D. Sasselov Harvard-Smithsonian Center for Astrophysics.
New Results from Kepler: Systems of Multiple Transiting Planets w/ Correlated TTVs Eric B. Ford Extreme Solar Systems II September 12, 2011 Based on a.

New Results from Kepler: Systems of Multiple Transiting Planets w/ Correlated TTVs Eric B. Ford Extreme Solar Systems II September 12, 2011 Based on a.
Lecture 11: The Discovery of the World of Exoplanets

Lecture 11: The Discovery of the World of Exoplanets
KOI-730 as a System of Four Planets in a Chain of Resonances Daniel Fabrycky UC Santa Cruz Matthew Holman, Joshua Carter, Jason Rowe, Darin Ragozzine,

KOI-730 as a System of Four Planets in a Chain of Resonances Daniel Fabrycky UC Santa Cruz Matthew Holman, Joshua Carter, Jason Rowe, Darin Ragozzine,
Lecture III: Gas Giant Planets 1.From Lecture II: Phase separation 2.Albedos and temperatures 3.Observed transmission spectra 4.Observed thermal spectra.

Lecture III: Gas Giant Planets 1.From Lecture II: Phase separation 2.Albedos and temperatures 3.Observed transmission spectra 4.Observed thermal spectra.

Similar presentations

Ads by Google