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Guillem Anglada-Escude (1,2) Alan P. Boss(1) Alycia Weinberger (1) Ian Thompson (1)

The C arnegie A strometric P lanet S earch and the role of ground based astrometry in the pre-Gaia era. Guillem Anglada-Escude (1,2) Alan P. Boss(1) Alycia Weinberger (1) Ian Thompson (1) (1)Carnegie Institution for Science (2) Institute for Astrophysics - University of Goettingen.

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Guillem Anglada-Escude (1,2) Alan P. Boss(1) Alycia Weinberger (1) Ian Thompson (1)

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  1. The Carnegie Astrometric Planet Searchand the role of ground based astrometry in the pre-Gaia era. GuillemAnglada-Escude (1,2) Alan P. Boss(1) Alycia Weinberger (1) Ian Thompson (1) (1)Carnegie Institution for Science (2) Institute for Astrophysics - University of Goettingen

  2. Astrometry and radial velocity methods a K RV Time

  3. 1º 1/60 1’ 1/60 1’’ 1/1000 1 mas 1/100 10 mas 3474 km 120 km 2 km 2 m 2 cm 1 mas A closer look at astrometry…

  4. Astrometric recipes Exo-Jupiter formula G dwarf @ 10 pc M dwarf @ 10 pc 1.0 mas 0.1 mas Book on the moon Man on the moon Exo-Earth formula Gaia/ESA Ground based 0.3 mas 3 mas Paper width on the moon Euro width on the moon

  5. Ground based AstrometryWhy M dwarfs? Numerous Faint Low mass Poorly characterized Hosts to habitable planets(that can be detected)

  6. Carnegie Astrometric planet Search Alan Boss (PI, DTM/CIW) Alycia Weinberger (DTM/CIW) Ian Thompson (OCIW) ChistophBrik (OCIW) Greg Burley (OCIW) 2.5m duPont Telescope. Las Campanas Observatory, Chile Follow-up a sample of 120 M, L and T dwarfs

  7. Carnegie Astrometric planet Search CAPScam (I band), 2048x2048

  8. Classic local astrometry Extract, centroid and crossmatch the sources Input catalog Fit field distortions Shift (2 par) rotation, scale (4 par) Quadratic deformations (6 para) Iterate Obtain a new catalog

  9. CAPS pipeline : ATPa software • Fully coded in Java (run on your computer) • Graphic User Interface • One night processing and • Astrometric Iterative solution • Final Data products : catalog, maps of extracted sources, reference stars, motion of each star, etc. If you are interested in testing with your own images, please check http://www.dtm.ciw.edu/anglada/ It also has a Manual!

  10. Carnegie Astrometric Planet search : Lots of parallaxes of cool dwarfs 200+ new and updated parallaxes

  11. Carnegie Astrometric Planet Search program so far… • Astrometric detection needs long time baselines (5-10 yr) • Overall precision better than 1 mas/epoch. • Almost 4 years of baseline, Gas giants should be detected soon (if present) • About 120 M dwarfs

  12. Carnegie Astrometric Planet Search… candidates? brown dwarfs gas giant planets 0.25 milliarcsec accuracy, S/N = 4 0.1HZ 0.5 HZ

  13. Lessons learned from individual targets GJ 1214 GJ 317 VB 10 Transit + Doppler planet Charbonneau et al. 2009, Nat P=1.83 days M sin i ~ 6 Meartj D = 12.0 pc Radius 15% larger?? Doppler candidate Johnson et al 2007, ApJ P=690 days M sin i ~ 2 Mjup D = 9.6 pc [Fe/H] = -0.3?? Astrometric detection Pravdo & Shaklan 2010 ApJ P=270 days M ~ 6 Mjup D = 7 pc Galactic plane ? ? ?

  14. Lessons learned from individual targets : VB 10 GJ 317, Anglada-Escude et al. 2012 Astrometry 2 x offsets 2 x Proper motions 1 x Parallax Doppler 1xoffset Black & Scargle 1982 HD 125612 Fischer et al. 2007

  15. Lessons learned from individual targets : VB 10 Residual periodograms Pravdo & ShaklanApJ, 2009 K = 3000 m/s K = 1500 m/s Astrometric periodograms Anglada-Escude et al. ApJ, 2011

  16. Lessons learned from individual targets : VB 10 270 days 49.9 days Anglada-Escude et al. ApJ 2011, RV follow-up with MIKE/Magellan Bean et al. 2011, RV follow-up with CRIRES/VLT Lazorenko et al. 2011, Astrometric follow-up

  17. Lessons learned from individual targets GJ 1214 GJ 317 VB 10 Transit + Doppler planet Charbonneau et al. 2009, Nat P=1.83 days M sin i ~ 6 Meartj D = 12.0 pc Radius 15% larger?? Doppler candidate Johnson et al 2007, ApJ P=690 days M sin i ~ 2 Mjup D = 9.6 pc [Fe/H] = -0.3?? Astrometric detection Pravdo & Shaklan 2010 ApJ P=270 days M ~ 6 Mjup D = 7 pc Galactic plane Astrometric periodograms (need better understanding of sampling)

  18. Lessons learned from individual targets : GJ 317 d = 9.6 pc M* = 0.24 Msun M sin i = 1.85 Mjup P = 692 days, a = 0.95 AU Jonhson, Butler et al. ApJ 2007 Exo-Jupiter formula 0.78 mas

  19. Lessons learned from individual targets : GJ 317 d = 9.6 pc a =0.78 mas d = 14.9 pc 0.32 mas M* = 0.42 Msun M sin i = 1.8 Mjup P = 692 days a = 0.95 AU

  20. Lessons learned from individual targets : GJ 317

  21. Lessons learned from individual targets : GJ 317 Likelihood function Mass Period

  22. Lessons learned from individual targets : GJ 317 Provides optimal sampling in highly dimensional spaces N = 13 Likelihood function Run a few million steps and you are done! Mass Period

  23. Lessons learned from individual targets : GJ 317

  24. Lessons learned from individual targets : GJ 317 First exoplanet “confirmed” with Ground based astrometry!

  25. Lessons learned from individual targets GJ 1214 GJ 317 VB 10 Transit + Doppler planet Charbonneau et al. 2009, Nat P=1.83 days M sin i ~ 6 Meartj D = 12.0 pc Radius 15% larger?? Doppler candidate Johnson et al 2007, ApJ P=690 days M sin i ~ 2 Mjup D = 9.6 pc [Fe/H] = -0.3?? Astrometric detection Pravdo & Shaklan 2010 ApJ P=270 days M ~ 6 Mjup D = 7 pc Galactic plane Astrometric periodograms (need better understanding of sampling)

  26. Lessons learned from individual targets GJ 1214 GJ 317 VB 10 Transit + Doppler planet Charbonneau et al. 2009, Nat P=1.83 days M sin i ~ 6 Meartj D = 12.0 pc Radius 15% larger?? Doppler candidate Johnson et al 2007, ApJ P=690 days M sin i ~ 2 Mjup D = 9.6 pc [Fe/H] = -0.3?? Astrometric detection Pravdo & Shaklan 2010 ApJ P=270 days M ~ 6 Mjup D = 7 pc Galactic plane Astrometric periodograms (need better understanding of sampling) Combine RV+Astrometry

  27. Lessons learned from individual targets : GJ 1214 HARPS-TERRA RVs (updated) CAPS Astrometry (new) RMS < 1.0 mas 30 transit times and updated Transit observables Sada et al, 2010, Carter et al. 2011, Kundurthy et al., 2011 • K band, low res(new) • 4 Optical bands • 3x2MASS bands • 4xWISE bands (new)

  28. Lessons learned from individual targets : GJ 1214 Previous NEW! +12% 14.47 (0.14) pc 0.175 (0.009) Ms 3.9 10-3Ls 3200 K d M* L* Teff 12.9 (1.0) pc 0.155 Ms 3.3 10-3Ls 2900 K +13% +19% +10%

  29. Lessons learned from individual targets : GJ 1214

  30. Lessons learned from individual targets : GJ 1214

  31. Lessons learned from individual targets GJ 1214 GJ 317 VB 10 Transit + Doppler planet Charbonneau et al. 2009, Nat P=1.83 days M sin i ~ 6 Meartj D = 12.0 pc Radius 15% larger?? Doppler candidate Johnson et al 2007, ApJ P=690 days M sin i ~ 2 Mjup D = 9.6 pc [Fe/H] = -0.3?? Astrometric detection Pravdo & Shaklan 2010 ApJ P=270 days M ~ 6 Mjup D = 7 pc Galactic plane Astrometric periodograms (need better understanding of sampling) Combine RV+Astrometry

  32. Lessons learned from individual targets GJ 1214 GJ 317 VB 10 Transit + Doppler planet Charbonneau et al. 2009, Nat P=1.85 days M sin i ~ 6 Meartj D = 14.5 pc Everything is good! Doppler candidate Johnson et al 2007, ApJ P=690 days M sin i ~ 2 Mjup D = 9.6 pc [Fe/H] = -0.3?? Astrometric detection Pravdo & Shaklan 2010 ApJ P=270 days M ~ 6 Mjup D = 7 pc Galactic plane Astrometric periodograms (need better understanding of sampling) Combine RV+Astrometry Transits+RV, astrometry Simultaneous FIT!

  33. ‘Other’ exoplanet related programs… 10 years before Gaia Young field M dwarfs (UV and X ray sources) from Shkolnik et al. 2009 ApJ 61 new parallaxes! 12 New members to nearby young moving groups (Beta Pictoris 10 Myr, AB Dor 40 Myr) Based on astrometry obtained with ATPa (just accepted for publication, ApJ) J. O’Faherty PhD. Thesis Shkonlik, Anglada-Escude, Weinberger, Boss et al. 2011 (to be submitted!)

  34. Early L brown dwarf at 12 pc

  35. Early L brown dwarf at 12 pc

  36. Synergies? • The obvious… • Combine with ground based observations • Targeted follow-up of peculiar systems • Extend time baselines

  37. How you do that??? Doppler CAPS Gaia v MCMC

  38. How you do that??? Doppler CAPS Gaia v MCMC

  39. Astrometric model is LINEAR in the relevant quantities Only becomes (a bit) more complicate when combined with RVs, or for highly eccentric orbits (e>0.6)

  40. Conclusions Experience : As ground based transit surveys did for COROT & Kepler… prepares the tools, identifies pitfalls Cool parallaxes NOW : Ground based astrometry, gives your parallaxes NOW at sufficient accuracy (nearby cool stars) First population statistics of ‘long period’ Gas giantsaround M dwarfs available before Gaia When Gaia data is released (residuals, not solutions!) … • Combine astrometric solutions • Time to pack (at least CAPS, RECONS and a few others) • … work continues on L, T and Y dwarfs! (nIR astrometry)

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