2. Microlensing, « blue dot team » Jean-Philippe Beaulieu Collaborators/interested by a microlensing program on EUCLID IAP : Batista, Marquette Observatoire Toulouse : Fouqué Manchester : Kerins, Mao, Rattenbury Heidelberg : Cassan, Grebel ESO : Kubas USA : Bennett, Gaudi, Gould BLUE DOT LOGO ????

3. Action item list for microlensers in 2008 Useful action already done : White paper to exoplanet task force (Bennett et al. astroph) JDEM RFI answer (Bennett, et al., ) Participation to exoplanet forum (Gaudi et al.) Exoplanet task force report EPRAT white paper (Beaulieu et al.) Another EPRAT white paper (Dominik et al.) Being done now : Celebrating a 3 earth mass planet Discovering more planets in 2008 Next generation of ground based survey Discussing a microlensing program on board EUCLID To be done shortly : Organisation of a microlensing workshop in Paris (January 2009)

4. “Recommendation B. II. 2 Without impacting the launch schedule of the astrometric mission cited above *, launch a Discovery-class space-based microlensing mission to determine the statistics of planetary mass and the separation of planets from their host stars as a function of stellar type and location in the galaxy, and to derive   over a very large sample. * “Recommendation B. I. a. 1 Launch and operate a space based astrometric mission capable of detecting planets down to the mass of the Earth around 60-100 nearby stars…” Reading the Scriptures (aka exoplanet task force) :

5. Technology Ground-based 1-2m, Wide FOV Telescope –Several very similar telescopes already operating MOA-II Pan-STARRS-1 - $20M Space-based microlensing mission –Requires almost no technology development. –Can extensively leverage other missions (Spitzer, NextView, Ikonos, JWST) –Can use many components that are demonstrated on orbit or flight qualified.

6. MPF Mission Design 1.1-m aperture consisting of a three- mirror anastigmat telescope feeding a 147 Mpixel HgCdTe focal plane (35 2048 2 arrays) The spacecraft bus is a near-identical copy of that used for Spitzer. The telescope system very similar to NextView commercial Earth- observing telescope designs. Detectors developed for JWST meet MPFs requirements. All elements are at TRL 6 or better. Total Cost $300M (without launch vehicle) MPF Mission Requirements

7. Dark Energy Synergy Space-based microlensing mission telescope requirements are very similar to the requirements for many proposed dark energy missions. Combined dark energy/planet finding mission probably could be accomplished at a substantial savings. ADEPT, Destiny, SNAP, DUNE/SPACE/Euclid –Wide FOV, >1.1m aperture, technical specifications appear to satisfy space- based microlensing survey specifications –DUNE/SPACE/Euclid can meet all the science goals without modification to hardware. Trade study: –Observing time –Pass bands –FOV and Detectors –Orbit –Telemetry –Aperture –Optics –Pointing

8. Dark Energy Synergy Everything that is good for COSMIC SHEAR measurements, is good for microlensing. We have the same requirements, just slightly less stringent. Everything that is good for COSMIC SHEAR measurements, is good for microlensing. Everything that is good for COSMIC SHEAR measurements, is good for microlensing. Everything that is good for COSMIC SHEAR measurements, is good for microlensing. Everything that is good for COSMIC SHEAR measurements, is good for microlensing.

9. Summary Ground-based Next-Generation Survey: +$10M—$20M –Complete network with a single wide FOV 1-2m telescope in SA. –Frequency of planets >M  beyond the snow line. –Test planet formation theories. Either: Space-based Microlensing Mission: +$300M + launch –Complete census of planets with mass greater than Mars and a > 0.5 AU. –Sensitivity to all Solar System planet analogs except Mercury. –Demographics of planetary systems - tests planet formation theories. –Detect “outer” habitable zone (Mars-like orbits) where detection by imaging is easiest. –Can find moons and free floating planets. Or: Joint  lensing/Dark Energy Mission +$100M—$200M? Total cost to “Exoplanet Community”: $120M—$420M

10. The near-term: automated follow-up The near-term: automated follow-up 1-5 yr Milestones: A.An optimised planetary microlens follow-up network, including feedback from fully-automated real-time modelling. B.The first census of the cold planet population, involving planets of Neptune to super-Earth (few M ⊕ to 20 M ⊕ ) with host star separations around 2 AU. C.Under highly favourable conditions, sensitivity to planets close to Earth mass with host separations around 2 AU. Running existing facilities with existing operations

11. The medium-term: wide-field telescope networks The medium-term: wide-field telescope networks 5-10 yr Milestones: A.Complete census of the cold planet population down to ~10 M ⊕ with host separations above 1.5 AU. B.The first census of the free-floating planet population. C.Sensitivity to planets close to Earth mass with host separations around 2 AU. Several existing nodes already. Adding one node in South Africa, + operation : 10-20 M$

12. The longer-term: a space-based microlensing survey 10+ yr Milestones: A.A complete census of planets down to Earth mass with separations exceeding 1 AU B.Complementary coverage to Kepler of the planet discovery space. C.Potential sensitivity to planets down to 0.1 M ⊕, including all Solar System analogues except for Mercury. D.Complete lens solutions for most planet events, allowing direct measurements of the planet and host masses, projected separation and distance from the observer. Dedicated ~400 M$, or participation to Dark energy probes Excellent synergy Dark Energy/Microlensing

13. Searching for low mass extra solar planets via microlensing. Jean-Philippe Beaulieu, (PLANET/RoboNET, HOLMES)

14. 1-7 kpc from Sun Galactic centerSun 8 kpc Light curve Source star and images Lens star and planet Observer Target Field in the Central Galactic Bulge Probability ~10 -6

15. A planetary companion

16. If planetary Einstein Ring < source star disk: planetary microlensing effect is washed out (Bennett & Rhie 1996) For a typical bulge giant source star, the limiting mass is ~10 M  For a bulge, solar type main sequence star, the limiting mass is ~ 0.1 M  Earth mass planet signal is washed out for giant source stars Need to monitor small stars to get low mass planets. Sensitivity to Earths depends on source size

17. Hunting for planets via microlensing Detecting real time microlensing event : OGLE-III and MOA 2 Selecting microlensing event with good planet detection efficiency Two schools : - Mainly high magnification events and alerted anomalies (microFUN) - Monitoring a larger number of events (PLANET/ROBONET). Networks of telescopes to do 24 hours monitoring : PLANET/RoboNET, microFUN Accurate photometry (Image subtraction since 2006) Real time analysis and modeling All data, models, are shared immediately among the community. Cooperation is the way to go ! OGLE-III has an online anomaly detector (EWS) MOA-II Detecting anomalies real time :

18. PLANET/RoboNet SITES ESO Danish 1.54m 2003-2008 Sutherland, SAAO 1m 2002+ Boyden, 1.5m, CCD 2006, 2007 Perth 0.6m 2002-2007+ Hobart 1m, 2002-2007+ Brazil 0.6m, 2007+ Robonet : Liverpool 2m, Canary 2005+ Faulkes North 2m, Hawaii 2006+ Faulkes South 2m, Australia 2007+ Goals at each site : - 1 % photometry, - Adapted Sampling rate - Online analysis. Boyden 1.5m

19. 2 Jupiter mass planets detected microlensing (2004, 2005) : Strong caustic Central caustic Small fraction of M dwarfs orbited by a Jovian companion

20. OGLE-2005-BLG-390 Coopération : PLANET/RoboNET, OGLE-III, MOA-II

21. PROBABILITY DENSITIES OF THE STAR AND ITS PLANET

22. Gould et al. 2006, MicroFUN, OGLE, RoboNet OGLE-2005-BLG-169Lb : a weak Neptune planet signal

23. Gaudi et al., 2008, Science

25. 3 bodies, 0.5 Mo, ~0.7 Mjup, ~0.3 Mjup Triple lens, with finite source effects, parallaxe, & taking into account rotation of planets Ultimate nightmare for normal microlensing planet hunters. Two other multiple systems « in stock », modeling underway. One has been giving headaches to Bennett since late 2004. The other one is much further down the road… (Dong et al. 2008)

26. Earth mass planet signal is washed out for giant source stars DUNE-ML photometry Earth at 1 AU ?

27. Monitor 2 10 8 stars down to J,Y,H ~22 Color information ~ once a week ~4 deg 2 observed every ~20 min Sensitivity to planets with a 3 months dedicated observing program : –16 frocky rocky planets (Earth, Venus, Mars) –580 fjupiter Jupiter planets –120 fsat Saturne –16 fnep Neptune planets Earth in habitable zone is feasible, but requires statistics (telescope time). The bulk of host system is M and K dwarfs DUNE MICROLENSING PLANET SEARCH

28. CURRENT RESULTS Microlensing is probing “Frozen” planets. 7 microlensing planets for 3 scenarios : 3 Strong caustic 2 High mag central caustic 1 Planetary caustic 3 ~Jupiters, 1 ~5.5 Earth, 1 ~13 Earth (Probability of detecting Jupiters is ~30 times larger) Giant planets are rare, suggests 1-15 M EARTH might be common 1 system with ~0.7 Jup (2.3 AU), and ~0.3 Jup (4.6 AU) Several planets in “stock”… modeling underway. ~Earth mass planets on ~AU orbits to be discovered soon… Total cooperation between teams Total cooperation between teams Indication : systems with multiple planets more common ?

29. CONTRIBUTION WITHIN BDT Frozen super Earth - Earth mass planets are already accessible Multiple planet systems with frozen ~Earth and Giant planet are accessible Statistics about such systems in a few years Down to frozen mars mass planet : Monitoring very high mag events with small telescopes Network of wide field imagers Wide field imager in space Habitable earth : Wide field imager in space (recomm from exo planet task force)