Download - Near & Long Term Planet Searches (not a review) S. R. Kulkarni California Institute of Technology
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Near & Long Term Planet Near & Long Term Planet Searches (not a review)Searches (not a review)
S. R. KulkarniS. R. Kulkarni
California Institute of TechnologyCalifornia Institute of Technology
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Programs at CaltechPrograms at Caltech
Searches for planets in binary stars using Searches for planets in binary stars using precision RV (Keck HIRES)precision RV (Keck HIRES)
Searches for planets in binary stars using Searches for planets in binary stars using astrometry (Palomar Interferometer)astrometry (Palomar Interferometer)
EPIcS (on SIM)EPIcS (on SIM)
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Planets via RV Planets via RV
Geared towards single stars or >2 arcsec Geared towards single stars or >2 arcsec binariesbinaries
Precise Point Spread Function (PSF) modelingPrecise Point Spread Function (PSF) modeling Accurate velocity calibrationAccurate velocity calibration
Two approachesTwo approaches• Iodine cell for both (e.g. California-Carnegie searches)Iodine cell for both (e.g. California-Carnegie searches)• Stable spectrograph & synthetic spectra (e.g. Swiss)Stable spectrograph & synthetic spectra (e.g. Swiss)
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Bias of Current RV surveysBias of Current RV surveys
Speckle Binaries
Visual Binaries
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Difficulty observing speckle binariesDifficulty observing speckle binaries
Problem: Observed (without the iodine cell) stellar spectra cannot be used as templates since the composite spectrum of a spectroscopic binary is time variable
Solution: Use synthetic stellar spectra as templates
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Results: HD 209458 & HD179949Results: HD 209458 & HD179949
Precision RVs (filled circles) with synthetic spectra as templates
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Results: SB2 HD 4676Results: SB2 HD 4676F6V+F6V, orbital period of ~13 days, Keck/HIRES
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RV study of Speckle Binaries RV study of Speckle Binaries (Konacki)(Konacki)
100 speckle binaries with angular separation 0.3 arcsec or less
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Status and Near FutureStatus and Near Future
Current approach demonstrably works but Current approach demonstrably works but achieved precision is 20 m/sachieved precision is 20 m/s
Next step: Combine best of both worldsNext step: Combine best of both worlds Observe with and without Iodine cellObserve with and without Iodine cell Use Iodine observations to model PSF and Use Iodine observations to model PSF and
wavelength calibrationwavelength calibration Cross-correlate with synthetic spectra and derive Cross-correlate with synthetic spectra and derive
both stellar velocitiesboth stellar velocities Expected precision is 10 m/s (increased photon Expected precision is 10 m/s (increased photon
noise at the very least)noise at the very least)
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Ground Based AstrometryGround Based Astrometry
Phase difference between two points increases Phase difference between two points increases with length of baseline with length of baseline
RMS phase ~ (d/rRMS phase ~ (d/r00))5/65/6
As a result bigger telescopes (larger d) does not As a result bigger telescopes (larger d) does not increase astrometric precision (though result in increase astrometric precision (though result in better photon SNR)better photon SNR)
Adaptive Optics and Interferometery (very narow Adaptive Optics and Interferometery (very narow angle astrometry) open up new regimes of angle astrometry) open up new regimes of ground based astrometryground based astrometry
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Shao & Colavita
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Very Narrow Angle Astrometry
Shao & Colavita
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STEPS (Traditional but with CCDSTEPS (Traditional but with CCD))
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GJ 569Bb (Keck AO): An ExampleGJ 569Bb (Keck AO): An Example
Lane et al.
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PHASES:PHASES:
Palomar High-precision Palomar High-precision AStrometric Exoplanet SearchAStrometric Exoplanet Search
Caltech, MSC, JPL, MIT Caltech, MSC, JPL, MIT
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Scanning the FringeScanning the Fringe
Lane & Mutterspaugh
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Shao & Colavita
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Planets in Binary StarsPlanets in Binary Stars
Starting an astrometric search for planets in Starting an astrometric search for planets in binary starsbinary stars
Demonstrated precision is 20 microarcsecond Demonstrated precision is 20 microarcsecond and goal is 10 microarcsecand goal is 10 microarcsec
The survey, if successful, will be a big boost to The survey, if successful, will be a big boost to SIM and astrometry in generalSIM and astrometry in general
Planets thus found will motivate novel direct Planets thus found will motivate novel direct detection approachesdetection approaches
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Planets exist in binary stars
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Phases Sample (I)Phases Sample (I)
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Phases Sample (II)Phases Sample (II)
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Keck Outrigger ArrayKeck Outrigger Array
Very Narrow Angle is the basis of Keck Very Narrow Angle is the basis of Keck Outrigger ArrayOutrigger Array
Main concern: need to find multiple reference Main concern: need to find multiple reference stars.stars.
Why not focus Outrigger on binary star?Why not focus Outrigger on binary star? Achieves SIM like precision ahead of SIMAchieves SIM like precision ahead of SIM No reference star problem!No reference star problem!
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Some Obvious Points that are Some Obvious Points that are worth rememberingworth remembering
RV + Astrometry is better than eitherRV + Astrometry is better than either RV + Astrometry is sensitive to all RV + Astrometry is sensitive to all
inclination anglesinclination angles Full orbit determinationsFull orbit determinations
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SIM: A Michelson InterferometerSIM: A Michelson Interferometer
Three Colinear Fixed Baseline InterferometersThree Colinear Fixed Baseline Interferometers
Baseline: 10 mBaseline: 10 mWavelength: 0.4-1 micron (CCD)Wavelength: 0.4-1 micron (CCD)Aperture: 0.3 mAperture: 0.3 mField of View: 0.3 arcsecondField of View: 0.3 arcsecondResolution: 10 milliarcsecondResolution: 10 milliarcsecond
Orbit: Earth Trailing (SIRTF)Orbit: Earth Trailing (SIRTF)Launch: 2009 Launch: 2009 Lifetime: 5 yr (10 yr?)Lifetime: 5 yr (10 yr?)
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How does SIM work?How does SIM work?
Principal Observable is Delay:Principal Observable is Delay: Delay = B . s + CDelay = B . s + C B = baselineB = baseline
s = source directions = source direction C = instrumental constantC = instrumental constant
Stabilize with 2 grid stars observed with “guide” interferometers Stabilize with 2 grid stars observed with “guide” interferometers Derive B from observations of the grid stars (known s)Derive B from observations of the grid stars (known s)Keep track of C from internal metrologyKeep track of C from internal metrologyMeasure Delay with “science” interferometerMeasure Delay with “science” interferometer
http://http://planetquestplanetquest..jpljpl..nasanasa..govgov//simcraftsimcraft//simsim_frames.html_frames.html
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Planet Detection: Comparison
Detection LimitsSIM: 1 as over 5 years (mission lifetime)Keck Interferometer: 20 as over 10 years
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Reference Stars: RequirementsReference Stars: Requirements
Reference stars should not have planets!Reference stars should not have planets!
Moderate distance K giants (mini-grid)Moderate distance K giants (mini-grid)
or or Eccentric Binaries Eccentric Binaries
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Reference Star: K giantsReference Star: K giants
Considerable Preparatory Work: Identification & Stability
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Reference Stars: Eccentric G star Reference Stars: Eccentric G star binariesbinaries
Eccentric binaries do not possess planets Eccentric binaries do not possess planets over a range of orbital separation.over a range of orbital separation.
Risk: Uneasy Feeling
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Extrasolar Planets InterferometriC Survey: Extrasolar Planets InterferometriC Survey: EPIcs, a two-pronged searchEPIcs, a two-pronged search
Known extra-solar system planets (7%) are differentKnown extra-solar system planets (7%) are different (orbital period and eccentricity distribution)(orbital period and eccentricity distribution)
Two possibilities:Two possibilities: Solar System is unique.Solar System is unique. Planetary Systems are ubiquitous BUT diversePlanetary Systems are ubiquitous BUT diverse
Tier 1-Tier 2 ProgramTier 1-Tier 2 Program
100 nearby stars at 1.5 microarcsec100 nearby stars at 1.5 microarcsec 1000 nearby stars at 4 microarcsec1000 nearby stars at 4 microarcsec
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Extra-solar Planet Interferometric SurveyExtra-solar Planet Interferometric Survey(EPIcS)(EPIcS)
M. Shao & S. R. Kulkarni (Co-PI)M. Shao & S. R. Kulkarni (Co-PI)
S. Baliunas C. BeichmanS. Baliunas C. BeichmanA. Boden D. Kirkpatrick A. Boden D. Kirkpatrick D. Lin D. StevensonD. Lin D. StevensonT. Loredo S. UnwinT. Loredo S. UnwinD. Queloz D. Queloz S. Shaklan C. Gelino S. Shaklan C. Gelino S. TremaineS. TremaineA. WolszczanA. Wolszczan
http://www.astro.caltech.edu/~srkhttp://www.astro.caltech.edu/~srk