Searching for low mass extra solar planets via microlensing. Jean-Philippe Beaulieu, Virginie Batista, Arnaud Cassan, Christian Coutures, Jadzia Donatowicz,

Searching for low mass extra Searching for low mass extra solar planets via microlensing.solar planets via microlensing.

Jean-Philippe Beaulieu, Virginie Batista, Arnaud Cassan, Christian Coutures, Jadzia Donatowicz,

Pascal Fouqué, Daniel Kubas, Jean-Baptiste Marquette, Olivier Mousis,

et al. (PLANET/RoboNET, HOLMES)

Europlanet, Potsdam

1-7 kpc from Sun

Galactic center Sun8 kpc

Light curve

Source starand images

Lens starand planet Observer

Target Field in the Central Galactic BulgeTarget Field in the Central Galactic Bulge

A planetary companionA planetary companion

Ep tqt

: 0.3 d, 20 sunE MMt

h 5.110 :Terre

d 110 3 :Jupiter

p5

p-3

tq

tq

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, microFUNAccurate photometry (Image subtraction since 2006)Real time analysis and modeling

All data, models, are shared immediately among the microlensing community.Cooperation is the way to go !

OGLE-III has an online anomaly detector (EWS)MOA-II

Detecting anomalies real time :

PLANET collaboration : PLANET collaboration : Probing Lensing Anomaly Probing Lensing Anomaly

NETwork (current NETwork (current members)members)

http://planet.iap.fr http://planet.iap.frM. D. Albrow, J.P. Beaulieu, D. Bennett, D. Bramich, S. Brillant, J. A. R. Caldwell, H. Calitz, A Cassan, K. Cook, C. Coutures, M. Dominik, J. Donatowicz, D. Dominis, P. Fouqué, J. Greenhill, K. Hill, M. Hoffman, K. Horne, U. Jorgensen, S. Kane, D. Kubas, R. Martin, J. Menzies, P. Meintjes, K. R. Pollard, K. C. Sahu, Y. Tsapras,J. Wambsganss, A. Williams, M. Zub Institut d'Astrophysique de Paris, INSU CNRS, Paris, FranceUniv. of Canterbury, Dept. of Physics & Astronomy, Christchurch, New ZealandSouth African Astronomical Observatory, South AfricaBoyden Observatory, Bloemfountein, South AfricaCanopus observatory, Univ. of Tasmania, Hobart, AustraliaNiels Bohr Institute, Copenhagen, DenmarkUniv. of Potsdam, Potsdam, GermanySpace Telescope Science Institute, Baltimore, U.S.A.Perth Observatory, Perth, Australia

Boyden 1.5m

PLANET/RoboNet PLANET/RoboNet

SITESSITESESO 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

OBSERVING STRATEGY, DECISION TAKINGOBSERVING STRATEGY, DECISION TAKING

Homebase checks :- OGLE, MOA alert pages- results from Bayesian PSPL fits to OGLE data (Albrow)- results from K.Horne priority pages- data collected by PLANET/RoboNet and current fits

He can ask for data to be re-reduced to double check anomalies.

Then he decides an observing strategy, sampling rates for different eventsHe issues anomaly alerts to the community.

Homebase should be on the deck 24 hours a day for 2-3 weeks

Real time analysis Real time analysis systemsystem

Data from all site uploaded to Paris every 5 min

http://planet.iap.frRoboNet

SAAOBoyden

Chile

Hobart

Perth

Brasil

Data stored in ParisModels updatedPrediction of future behaviorAlert if anomalies

In Out

OGLE-2005-BLG-390

OGLE-2005-BLG-390OGLE-2005-BLG-390

Coopération : PLANET/RoboNET, OGLE-III, MOA-II

AT LAST, A TEXT BOOK MICROLENSING EVENT

Data in the anomaly from : PLANET-Danish, OGLE, MOA-II, PLANET-PerthData outside the anomaly from : PLANET/Robonet, PLANET-Hobart

Gould Loeb 1992, Bennett & Rhie 1996, …

PROBABILITY DENSITIES OF THE PROBABILITY DENSITIES OF THE STAR AND ITS PLANETSTAR AND ITS PLANET

A companion to this frozen super Earth ?

Kubas et al., 2007 submittedExcluding at : 50 % Jupiter over 1.1-2.3 AU 70 % 3 Jupiter over 1.5-2.2 AU Core accretion models by Idal & Lin

Gould et al. 2006, MicroFUN, OGLE, RoboNet

OGLE-2005-BLG-169Lb : a weak Neptune planet signalOGLE-2005-BLG-169Lb : a weak Neptune planet signal

A new Jovian analogue in a resonnant caustic system

4455

5 microlensing planets, their time scale.

Do gas giants prefer host stars that cause longer events ?Ie more massive ones ?

KB-07-197

PLANET/Robonet/HOLMES (network of 9 telescopes). Now – 200?MicroFUN Now-200?OGLE III and MOA-2- Constraints on Jupiters and low mass planets (down to few Earth mass)- Monitoring of high mag events - Monitoring of any mag events (PLANET/RoboNet, OGLE) Las cumbres plans ?A 1m observing in J from Antartica ?Network of wide field imager Earth Hunter + OGLE-IV + MOA-2 2011+ ?

Statistics on Cool Earth mass planets, possibly habitable zone.NASA mission MPF ( PI Bennett) to be re-submitted ?ESA DUNE mission (cosmic shear + planet search )

Abundance of planets in habitable zone. MPF : 36 months, 200 million stars, 4 fields of 0.66 sq2, FWHM=0.25 arcsec ~100 q Earth, ~6000 q Jupiter (q fraction of stars with planets), Mars detectable

Current status of microlensing planet huntingCurrent status of microlensing planet hunting

CONCLUSION

Microlensing is probing “Frozen” planets.

5 microlensing planets for 3 scenarios : •2 Strong caustic•2 High mag central caustic• 1 Planetary caustic

3 ~Jupiters, 1 ~5.5 Earth, 1 ~13 Earth(Probability of detecting Jupiters is ~50 times larger)Giant planets are rare, suggests 1-15 MEARTH might be common

Giant planets in events with large tE (more massive stars)

Several planets in “stock”… modeling underway.

~Earth mass planets on ~AU orbits to be discovered soon…