The frequency of snowline planets from a 2 nd generation microlensing survey
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1 The frequency of snowline planets from a 2 nd generation microlensing survey Yossi Shvartzvald Tel-Aviv University with Dan Maoz, Matan Friedmann (TAU) in collaboration with OGLE, MOA, µfun
2 Microlensing basics Amplification ~milliarcsec
3 Microlensing basics S. Gaudi
4 Microlensing basics S. Gaudi
5 Microlensing Surveys - 1 st Generation Survey challenge: Galactic bulge event probability ~10-6 Monitor many stars, low cadence OGLE, Chile, 1.3m MOA, NZ, 1.8m
6 Microlensing Surveys - 1 st Generation ~ 650 events/year
7 Microlensing Surveys - 1 st Generation Follow-Up Network on bright, high-magnification events: higher sensitivity to planets high S/N light curves OGLE, Chile, 1.3m MOA, NZ, 1.8m
8 Microlensing Surveys - 1 st Generation Bond et al. 2004
9 Microlensing Surveys - 1 st Generation Gould et al Udalski et al Gaudi et al. 2008
10 Microlensing statistics Microlensing probes a unique region of planetary parameter-space Gould et al. 2006,2009
11 Microlensing statistics near the Einstein radii of stars ~ their snow lines. Snowline scaling with mass: R M Lens S Gould et al. 2006,2009
12 Microlensing statistics snowline planet frequency Gould et al (6 planets): ~1/3 of stars have snowline-region giant planets ~1/6 of stars have solar-like planetary systems Sumi et al (10 planets): Neptunes are at least 3 times more common than Jupiters Cassan et al (3 planets+gould10+sumi10): ~1/6 host Jupiters ~1/2 host Neptunes ~2/3 host super-earths
13 Microlensing Surveys - 1 st Generation But only 16 planets detected ( ) Why?
14 Microlensing Surveys - 1 st Generation But only 16 planets detected ( ) Why? High magnification events are rare events (~1%) ~7 events/year ~2 planets/year
15 Microlensing Surveys - 1 st Generation But only 16 planets detected ( ) Why? High magnification events are rare events (~1%) ~7 events/year ~2 planets/year Solution: Generation II microlensing survey
16 Second generation microlensing survey Wise Obs., Israel, 1m OGLE, Chile, 1.3m MOA, NZ, 1.8m
17 The generation-ii network
18 The generation-ii network Group OGLE
19 The generation-ii network Group OGLE MOA
20 The generation-ii network Group OGLE MOA WISE
21 Second generation microlensing survey 8 deg 2 of bulge with highest lensing rate covered quasi-continuously by all 3 telescopes cadences min
22 Gen-II planets First ML planet in the habitable zone MOA M P L M a AU M M J I-band (mag) I-band (mag) OGLE MOA Wise Survey data only All data Batista et al HJD Yee, Shvartzvald et al. 2012
23 Earth at ~1 AU from one member of a 15 AU binary Gen-II planets OGLE Gould et al., Science 2014
24 Super-Jupiter around M dwarf Gen-II planets M MOA P L a 4.3 AU M M M J Shvartzvald et al. 2014
25 Gen-II planets Jupiter around M dwarf OGLE M P M a AU M L M J Poleski et al. 2014, Tsapras et al. 2014
26 Gen-II planets Saturn/Jupiter around M dwarf OGLE M M M P a AU L M J Udalski et al. in prep
27 Gen-II planets Cold Jupiters around low-mass stars are common?
28 What to expect from Generation II? a simulation: Simulating the experiment Monte-Carlo of many Solar-System-like planetary systems, host star properties matching those of bulge microlensing population, random inclinations. Shvartzvald & Maoz 2012
29 Simulation results: can detect ~15-20% of planets around microlensed stars; Simulating the experiment S Shvartzvald & Maoz 2012
30 sample Sample Events 167
31 Anomalous events Sample Anomalous Planetary Events (16.3%) 8 (4.8%) Mass ratio
32 Anomalous events Sample Anomalous Planetary Events (16.3%) 8 (4.8%) Mass ratio Accounting for detection efficiency, >24% snowline planet frequency
33 Conclusions 2 nd generation microlening survey: A controlled experiment for the abundance of planets at a few AU Cold Jupiters around low-mass stars are common (?) Preliminary results suggest a lower limit of 24% snowline planet frequency
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