1. Exoplanet Transits and SONG Angelle Tanner

2. Venus Transiting the Sun

3. Transit Frequency gives us ORBIT SIZE Orbit Size with Star Temperature tells us if planet is in habitable zone. Transit duration, depth, gives us PLANET SIZE Size and Mass (with a doppler measurement of the “wobble”) gives DENSITY Density is clue to COMPOSITION.

4. Primary Transmission spectrum Terminator Secondary Emission spectrum Dayside Primary Eclipse Secondary Eclipse See thermal radiation from planet disappear and reappear See radiation from star transmitted Through the planet’s atmosphere

5. Because we can study their atmospheres!

6. SONG could: Make RV measurements during transit to determine the angle between stellar rotation and planet orbital plane

7. Left: Charbonneau, D., Brown, T., Latham, D. et al, 2000, ApJ 529, L45 Right: Brown, T., Charbonneau, D., Gilliland, R. et al, 2001, ApJ 552, 699 Currently 166 confirmed transiting systems

8. Goal: To find transiting habitable Earths

9. Mar 7, 2009 – launch! Aug 6, 2009 – confirmed HAT-P-7b 2010 – six confirmed systems June 15, 2010 – 706 planet candidates 2011 – 4 confirmed systems thus far Feb 2, 2011 – 1235 planet candidates, 54 in HZ Kepler-11 system with 7 planets Two days ago – Kepler 16b – Tatooine planet!!

10. ~1200 Kepler candidate planets 54 are in The HZ!

11. Currently monitoring 3000 M dwarfs 8 40 cm telescopes, with 26’ CCD FOV At Mt Hopkins, AZ with plans to go South M4.5, V=14.6, K=12.2 m/sCharbonneau et al. 2009 No features seen in ground based transmission spectrum – Bean et al. 2010 GJ 1214 – the lightest star w/ a planet

12. They are abundant and close We are sensitive to lighter planets RV surveys reach the habitable zone Once found, they make ideal planet transit targets K m/s 0.10 0.32 0.60 2.23 5.73 M V M K 4.8 3.3 9.0 5.3 11.7 6.8 16.6 9.4 19.4 10.5

13. Stars within 25 pc Red = V < 8 SONG could: 1) Follow-up the brightest Mearth candidates, 2) Follow-up Kepler candidates, or 3) do its own survey of K/M stars

14. Sunspots/Plage Pulsations Granulation Flares

15. Barnard’s star shows and anti-correlation between Hα and RV jitter - Zechmeister et al 2009 S-index indicator not necessarily correlated with RV jitter (Wright et al. 2009) Other indicators such as S HK and log R’ HK also don’t always correlate with RV jitter (Fischer & Issacson 2010)

16. P-modes for α Cen A (Butler et al., Fischer et al. )

17. T * = 2800 K & T spot = 2600 K Vsini=2 km/s Vsini=10 km/s σ RV ~ 10 m/s 14 m/s @ 0.5 mic σ RV ~ 2 m/s 10 m/s @ 1.0 mic σ RV ~ 2 m/s 10 m/s @ 1.6 mic NO detections < 20 Me for < 500 observations fo vsini > 20 m/s – Barnes et al 2010 SONG could: Perform intense studies of RV jitter noise as a function of spectral type

18. 1)Follow-up for Rossiter-McLaughlin effect 2)Follow-up for Mearth, Kepler and other transit detections 3)RV jitter studies with simultaneous photometric monitoring 4)????