Kepler - STScI

Discovery and characteriza1on of planets around binary stars Veselin Kostov (Advisor P. R. McCullough) STScI, Apr, 02, 2013 th
Back in the 17 century… “De raris mirisque Anni”, Johannes Kepler, 1629, Leipzig th
Back in the 17 century… “Jeremiah Horrocks Watching the Transit of Venus in 1639”, Eyre Crowe, 1891 “De raris mirisque Anni”, Johannes Kepler, 1629, Leipzig April 13, 1769, Tahi1 April 13, 1769, Tahi1 James Cook poin1ng at map April 13, 1769, Tahi1 James Cook poin1ng at map Image credit: Carleton Bailie, United Launch Alliance. Image credit: NASA/JPL-­‐
Caltech/Ball Outline Image credit: Carleton Bailie, United Launch Alliance. 1.  Kepler Mission 2.  Eclipsing Binary (EB) Stars 3.  Planets in EB systems Image credit: NASA/JPL-­‐
Caltech/Ball 4.  How to find and characterize 3. 5.  Summary Kepler Mission Image credit: Carleton Bailie, United Launch Alliance. Image credit: NASA/JPL-­‐
Caltech/Ball • 
Detect Earth analogs in the habitable zone of stars similar to the Sun and determine their occurrence frequency Kepler Mission Image credit: Carleton Bailie, United Launch Alliance. Image credit: NASA/JPL-­‐
Caltech/Ball • 
Detect Earth analogs in the habitable zone of stars similar to the Sun and determine their occurrence frequency • 
Uninterrupted, simultaneous monitoring of many stars and searching for periodic dips in the stellar light, caused by a planet moving across the disk of the star Kepler Mission Image credit: Carleton Bailie, United Launch Alliance. Image credit: NASA/JPL-­‐
Caltech/Ball • 
Detect Earth analogs in the habitable zone of stars similar to the Sun and determine their occurrence frequency • 
Uninterrupted, simultaneous monitoring of many stars and searching for periodic dips in the stellar light, caused by a planet moving across the disk of the star à Rpl/Rstar à Period à Orb. Inclina1on • 
• 
Image credit: SETI Ins1tute Kepler Mission Image credit: Carter Roberts / Eastbay Astronomical Society • 
Targets: ~150,000 stars over a 105 sq. degrees field of view in the Cygnus Region Kepler Mission Image credit: Carter Roberts / Eastbay Astronomical Society Image credit: NASA/JPL • 
Targets: ~150,000 stars over a 105 sq. degrees field of view in the Cygnus Region • 
Telescope: 0.95m in an Earth-­‐trailing heliocentric orbit with P~370days; no moving parts like shuders/filters/etc except reac1on wheels Kepler Mission Image credit: Carter Roberts / Eastbay Astronomical Society Image credit: NASA/JPL • 
Targets: ~150,000 stars over a 105 sq. degrees field of view in the Cygnus Region • 
Telescope: 0.95m in an Earth-­‐trailing heliocentric orbit with P~370days; no moving parts like shuders/filters/etc except reac1on wheels • 
Precision (required): noise (instrument
+shot+stellar) ~ 20 ppm (4-­‐sigma detec1on of Earth-­‐like transit (depth ~ 80ppm) in 6.5hours) • 
Bandpass: Kp = 423 to 897 nm • 
Duty Cycle: 30 min (long cadence) and 1 min (short cadence) Kepler Mission • 
2740 planet candidates (115 confirmed as planets) as of Apr, 02, 2012
Kepler Mission • 
2740 planet candidates (115 confirmed as planets) as of Apr, 02, 2012
• 
Data: freely available to the public, updated every 3 months
Kepler Mission • 
2740 planet candidates (115 confirmed as planets) as of Apr, 02, 2012
• 
Data: freely available to the public, updated every 3 months
• 
First 2.4 R_Earth planet in the habitable zone of a Solar-type star Kepler 22
(statistical confirmation, RV 1-sigma upper limit of 36 MEarth; Borucki et al., 2011):
Kepler 22b Kepler Mission: Eclipsing Binaries •  Detached EB
(Movie Credit:
R. Pogge, OSU)
Kepler Mission: Eclipsing Binaries •  Detached EB
(Movie Credit:
R. Pogge, OSU)
•  Semidetached EB
(Image Credit:
Cronodon)
Kepler Mission: Eclipsing Binaries •  Detached EB
(Movie Credit:
R. Pogge, OSU)
•  Semidetached EB
(Image Credit:
Cronodon)
•  Contact EB
(Movie Credit:
Software Systems
Consulting)
Kepler Mission: Kepler 16, First direct evidence of a planet orbiGng around a binary star! (Doyle et al., 2011) (Movie Credit: NASA/JPL-­‐Caltech/Tim Pyle) Kepler Mission: Kepler 16 (top), Doyle et al., 2011; Kepler 34 (lower leh) and Kepler 35 (lower right), Welsh et al., 2012; found by eye Kep 16 à ß  Kep 34 Kep 35 à Kepler Mission •  Eclipsing Binaries (EB): close to edge-­‐on, pre-­‐selected by Nature for search for transi1ng planets Kepler Mission •  Eclipsing Binaries (EB): close to edge-­‐on, pre-­‐selected by Nature for search for transi1ng planets •  EB from Kepler: 4+ years con1nuous, 30-­‐min data on 2165 EB (Slawson et al.,
2011) Kepler Mission •  Eclipsing Binaries (EB): close to edge-­‐on, pre-­‐selected by Nature for search for transi1ng planets •  EB from Kepler: 4+ years con1nuous, 30-­‐min data on 2165 EB (Slawson et al.,
2011)
•  Theory: circumbinary (CB) planets can form and survive even close to their parent stars and are likely to be co-­‐planar (Quintana and Lissauer, 2006; Pierens and Nelson 2007a, 2007b, 2008; Doolin and Blundell, 2011, Haghighipour et al., 2010; Schwarz et al., 2011; Artymowicz and Lubow, 1994; Holman and Weigert, 1999; Dvorak, 1984; Scholl et al., 2007) ==> should be able to observe their transits Kepler Mission •  Eclipsing Binaries (EB): close to edge-­‐on, pre-­‐selected by Nature for search for transi1ng planets •  EB from Kepler: 4+ years con1nuous, 30-­‐min data on 2165 EB (Slawson et al.,
2011)
•  Theory: circumbinary (CB) planets can form and survive even close to their parent stars and are likely to be co-­‐planar (Quintana and Lissauer, 2006; Pierens and Nelson 2007a, 2007b, 2008; Doolin and Blundell, 2011, Haghighipour et al., 2010; Schwarz et al., 2011; Artymowicz and Lubow, 1994; Holman and Weigert, 1999; Dvorak, 1984; Scholl et al., 2007) ==> should be able to observe their transits •  Total number as of Apr, 02, 2013: •  planetary candidates à 3000 •  confirmed transi1ng CB planets à 7! Kepler Mission •  Eclipsing Binaries (EB): close to edge-­‐on, pre-­‐selected by Nature for search for transi1ng planets •  EB from Kepler: 4+ years con1nuous, 30-­‐min data on 2165 EB (Slawson et al.,
2011)
•  Theory: circumbinary (CB) planets can form and survive even close to their parent stars and are likely to be co-­‐planar (Quintana and Lissauer, 2006; Pierens and Nelson 2007a, 2007b, 2008; Doolin and Blundell, 2011, Haghighipour et al., 2010; Schwarz et al., 2011; Artymowicz and Lubow, 1994; Holman and Weigert, 1999; Dvorak, 1984; Scholl et al., 2007) ==> should be able to observe their transits •  Total number as of Apr, 02, 2013: •  planetary candidates à 3000 •  confirmed transi1ng CB planets à 7! Planets in binaries: overview • 
Classification (Dvorak, 1984):
–  S-type [CircumStellar]
–  P-type [CircumBinary]
–  L-type [at Trojan points]
–  Image Credit: Schwarz et al.,
2011
Planets in binaries: overview • 
Classification (Dvorak, 1984):
–  S-type [CircumStellar]
–  P-type [CircumBinary]
–  L-type [at Trojan points]
–  Image Credit: Schwarz et al.,
2011
• 
Census (Pre-Kepler):
–  S-type: ~ 20% (Haghighipour,
2009; Mugrauer and
Neuhauser, 2009, Schwarz et
al., 2011)
–  P-type: 0%
–  L-type: 0%
Planets in binaries: overview • 
Classification (Dvorak, 1984):
–  S-type [CircumStellar]
–  P-type [CircumBinary]
–  L-type [at Trojan points]
–  Image Credit: Schwarz et al.,
2011
• 
Census (Pre-Kepler):
–  S-type: ~ 20% (Haghighipour,
2009; Mugrauer and
Neuhauser, 2009, Schwarz et
al., 2011)
–  P-type: 0%
Yet nearly half of all Solar-­‐type stars are –  L-type: 0%
members of mul1ple (2+) systems! Planets in binaries: Stability Cri1cal semimajor axis as a func1on of binary eccentricity and mass frac1on (Holman and Weigert, 1999) Discovery and characteriza1on 1. Examine all Kepler EB Discovery and characteriza1on 1. Examine all Kepler EB Discovery and characteriza1on 1. Examine all Kepler EB 2. Note extra transits! Discovery and characteriza1on 3. Calculate Radial Velocity of EB Discovery and characteriza1on 3. Calculate Radial Velocity of EB a) Stellar Spectrum b) Doppler Boos1ng Discovery and characteriza1on 4. Study the EB system Discovery and characteriza1on 5. Use the unique behavior of CB transits to constrain the parameters of the system Discovery and characteriza1on 5. Use the unique behavior of CB transits to constrain the parameters of the system Discovery and characteriza1on 6. Simulate, simulate, simulate… Discovery and characteriza1on 6. Simulate, simulate, simulate… Discovery and characteriza1on 6. Simulate, simulate, simulate… 7. Announce it to the rest of the world! Summary •  Extensive theore1cal work on forma1on, evolu1on and stability suggests CB planet may be common; predic1ons lack observa1onal support •  “…there is a deep-­‐set skepGcism about the idea of the formaGon of planets around binary star systems…” (Hessman et al., 2011) •  First confirmed, transi1ng CB planet announced 2011; 6 more as of Apr, 02, 2013 •  Treasure throve of unmatched-­‐quality EB data publicly available, released con1nuously References !"#"$%&''()*+)",)&-+()./00()121()3.4()35)
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