Chinese-international collaboration solved the central question : ” How common are planets

1. Chinese-international collaborationsolved the central question: ”Howcommonare planets like the Earth”

2. Exoplanet research with SONG: Jupiter-Saturn like exoplanets are uncommon – Are Earth-like exoplanets common? Is our solar system ”normal” or is something unusual the cause for ourexistence? SONG is particular sensitive to planets as in our solar system -- are they common or rare? . Design driver: 5 years of observation will tell number of Earths in the Galaxy

3. Doppler and transit planets dominate the number of known exoplanets –-- This will change in the future 420/ 70 of 440 known Primarily oxygen-rich stars are orbited by giant exoplanets 16 stars of 250,000 toward the galactic centre showed transiting exoplanets 110 expected from solar neighbourhood

4. Since 2004 we have searched for exoplanets using the Danish 1.54m telescope at ESO La Silla dedicated 4 months/year for microlensingsearch. SONG can do Doppler and microlensing, but will do microlensing 200 times more efficient thattraditionaltelescopes.

6. Habitable exoplanets: orbits: 0.4 AU – 4 AU around stars A5 - M0 (0.5-2.5M_sun) ¼ of all stars ¾ of all stars SONG: firsttelescope withmainsensitivity to exoplanets as all the planets in our solar system

7. lens star

8. Observed 5.5 Earth-mass planet OB05390 is on the limit of what existing telescopes can observe Hypothetical 1 Earth-mass planet

9. microlensning = observations in dense stellar fields 10 microlensing exoplanets are now known; incl a 3 and a 5 Earth-mass,terrestrial planet in an Earth-like orbit. SONG will be able to detect Mars mass planets in terrestrial orbits

10. ”Lucky Imaging” cameras at the SONG telescopes will reach almost as sharp images as a space-telescope. Normal camera Lucky imaging camera

11. MOA finding chart (1.8m NewZeeland) Lucky Imaging 1.54m Danish, Chile VLT/NACO 8m

12. mikrolinser --jordlignende exo-planeter SONG is a follow-up survey able to find small planets To observe smaller mass planets, requires to be able to resolve smaller source stars (i.e Lucky Imaging if fields are crowded), and observe more events (i.e. faster telescopes, observing a larger fraction of the year and night).

13. Pan-STARRS at Haleakala, Maui, Hawaii: next step in NEOsearch Aim: to identify ”all” NEOs > 1km, and 99% > 300m. It goes 5 mag (i.e. a factor 100) deeper than previous surveys, and is expected to identify 10 mill new main belt asteroids, and >10.000 new NEOs and TNOs First of 4 planned telescopes has started The camera has 1.4 billion pixels and a field of 7 sqr deg pr exposure. Two exposures pr minute of 2Gb size 0.3” resolution. Vlim=24 (intg 29.4) 6000 sqr.deg. pr night = the full sky scanned every week.

14. Large Synoptic Survey Telescope LSST will detect NEOs to 100 m diam. One 8.4 m mirror, 3 Gpixel CCD, Vlim = 27 full sky cover every 3 nights from 2014; 30 TB/night 10 sqr.deg. in each 15 sec exposure at 0.2”resolution in 5 bands, 4000Å-1.06mu 2.7km Cerro Pachon in North Chile

15. Tests with microlensing alerts in the whole Galactic plane are now being performed at VYSOS-5” (right) and Mauna Loa Observatory in Hawaii and VYSOS-6” (below) at Cerro Armazones Observatory in Atacama, Chile.

16. The SONG telescopes have: Smaller PSF (factor 9) Better throughput (factor 1.5) Faster slew and pointing (factor 2) Broader filters (factor 4) Better use of the year (factor 2) mikrolinser --jordlignende exo-planeter Roughly speaking, SONG can reach 3 mag fainter stars (=see smaller planets) with a 10 times higher efficiency => statistics on Earth-Mars like planets in 5 years Will we have microlenses enough to observe?

17. Difraction limit: The best seeing at La Silla, DK1.54m is 0.8”; typical seeing is 1” to 1.5” Lucky Imaging tests: 0.35” For a 1m mirror, the diffraction limit is 0.15” at 5000 Å 0.25” at 8000 Å

19. To understand whetherwecanbenefit from surveys in the general Galactic plane, I have made a simple Galactic model: Disk: cylinder of r = 15 kpc, h = 2 kpc Bulge: Extinction: 0.63mag per kpc

20. We now integrate the total Einstein areas out through a cone of 1 square degree of the sky The Einstein-area is the probability of a source star at distance ds being linsed. When multiplied by the number of source stars at ds, it gives the total number of lensing events at any given time of some baseline magnitude. The number per year is then approx. 52/3 times this number. This integration with the simple Galactic model gives good agreement with the number and distribution of OGLE events, and predict that the number of events could be doubled by looking out of center with a modest sized telescope.

21. A global network of 1m telescopes for long time series observations • High resolution imaging for microlensing at summer time • High resolution spectrograph for low mass RV observations in winter

22. First astrometric detection of an exoplanet from ground: VB10b May 2009. GAIA expects to identify 10,000 giant exoplanets within 200 pc

23. First 9 direct imaging detected exoplanets indicate a huge future potential for this method

24. WASP-2 Transit accuracy of 0.5 milli-mag from the ground (DK1.54m); timing accuracy of 10 s The Kepler satellite has 5 times better photometric accuracy (0.1 milli-mag) Many more transiting exoplanets will be announced in coming years. WASP-6