Observational and modeling techniques in microlensing planet searches

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1 Observational and modeling techniques in microlensing planet searches Dijana Dominis Prester , Belgrade

2 Simulating synthetic data Fitting Optimizing

3 q = 0.3 i = d R * ( x ( x = 1R 1 2 = 10R, 45, y 1 y o ) = (460,65) 2 E Sun ) = (285,853)

4

5 Modeling a Synthetic Light Curve Standard deviation (errorbars): 1 σ m = σ 0 1+ Δm σ [ σ, σ ] 0 min Gaussian scatter Noisy data Picking random data points (i.e. 30 out of 100) Irregular data coverage Fitting the light curve by using an inverse 2 χ optimization method)

6

7

8 Chi square test Chi squared per degrees of freedom: χ 2 / d. o. f. ( x( t) x( t) ) 2 = obs theor n n + 1 data parameters (close to 1 for a good fit)

9

10 q=0.3 i=45 d=0.6 Phase: 0.25

11 Phase: 0.47

12 Phase: 0.75

13 Phase: 1.00

14 Orbiting binary (P=100 days) with separation of 0.6 RE

15 Orbiting binary (P=100 days) with separation of 0.6 RE Misinterpretation even with High quality data is possible!

16 Static approximation q=0.1 d=1

17

18

19 Periods of Binary Systems A large fraction of the Galactic stars are in binary systems Gaussian-like distribution in log P with 4 maximum around 10 days 10 (between 1 day and 10 days) Long period binaries (P > 100 days): more binaries with high mass ratios

20 Distribution of binary periods Duquenney & Mayor (1991)

21 Time scales Orbiting binary Separation ~ A.U. Period P ~months/years Event duration ~ P Long lasting events Static approximation Short Einstein crossing times (~ days/weeks) Much more common

22 Statistic 2 χ Percentage of fits with small 100 magnification patterns for each binary system n dp data points (out of 100) light curves per realization

23 Binary mass ratio q Static approximation (black line: single lens) Easier to detect stellar binary lenses than planetary binaries!

24 Separation of the binary components d (static approximation)

25 Separation of the binary components d Microlensing is the most sensitive to separations around 1 Einstein radius! (orbiting binary)

26 Size of errorbars Number of data points (data sampling) Better data quality increases the detection!

27 Summary of part I Statistical analysis Significant chance for misinterpretation of a binary lens by a single lens Higher probability for misinterpretation for short lasting events Separation and mass ratio play an important role: Minimum around 1 Einstein radius Probability for planet detection

28 Binary source - single lens model (BS-SL) Superposition of two light curves: i i i i F ( t) = FA AA( t) + FB AB ( t) + Fblend observing site i Optimizing code BISCO (Binary Source Code for Optimization, Dominis 2005) uses the genetic algorithm PIKAIA (Charbonneau 1995) to find the best solution: { t, u ( A), u ( B), t ( A), t ( B), F / F } j E par 0 = (2n os 0 + 1) n 0 pb A B

29 Binary source light curve (in magnitudes)

30 Genetic algorithm Numeric optimization of an inverse problem (one light curve => set of physical parameters) Uses natural selection (selection of parents, mutation, crossing, evolution) Useful for complicated parameter spaces with many local minima

31 - GENETIC ALGORITHM (numeric optimization) - evolution of a random initial population

32 ??? FITNESS selection criterion (probability for crossing and survival) χ 2 / d. o. f. (goodness of fit, sum of squared residuals)

33 A simulated binary source single lens microlensing event BISCO is capable of reconstructing the event parameters from simulated data

34 OGLE-2003-BLG-222 OGLE-2004-BLG-347 (I=19.9) (I=17.5) 1 x1

35 OGLE-2003-BLG-222 Binary source fit, GA (Dominis) Binary lens fit, Powell (Cassan) F F A B =0.96 q d = 0.10 = 0.26 R E A Time (days) Degeneracy!

36 OB Binary source model

37 OB Binary lens model

38 OGLE-2004-BLG-347 Binary source fit (Dominis) Binary lens fit (Cassan) Magnification F F A B =0.47 q d = 0.75 = 3.07 R E Time (days) Degeneracy!

39 OB Binary source model

40 OB Binary lens model

41 Flux ratio method applied on OB fr(i)=0.50

42 fr(r)=0.46

43

44 Ambiguity in the light curve solution

45 Is there a limit on chi-squared-perdegree-of-freedom difference to decide about the model to be accepted? Δχ Δχ Δχ / d. o. f / d. o. f / d. o. f.( OB.( OB.( OB ) ) 390) = 14% = 1.7% 7.3% Or do we need a merit of fit adjusted to the relative sizes of the two peaks? =

46 Synthetic realistic light curve (black) (Gaussian noise, irregular data sampling)

47 Best fit (red line) to the synthetic data (black) σ σ 0 = 0.03mag min = 0.018mag 30/100 data points χ 2 A u max 0 = = t 0. 18P 0 = / d. o. f = 1. 32

48 B R

49 Single Point Mass Lens Einstein radius: 4GM c D RE = 2 tot L D D S LS Microlensing: the source and the images cannot be resolved

50 ) ( ' ' 4 ' 2 2 θ α θ β α α α β θ α φ = = + = = = S LS LS S S D D D D D u u c GM r GM Gravitational potential u angular distance of the light ray from the mass Lens equation

51 = = = = Ε Ε n i i i i n i i i i x x x x m x y y x x x x x m c G x 2 2 2, 4 ) ( θ β θ θ α for n point masses:

52 Critical curves Caustics

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