FIRST SPECTROSCOPIC INVESTIGATION OF A MICROLENSING EVENT: 
 NO EVIDENCE FOR THE BINARY I. BOISSE (LAM), A. SANTERNE (IA), J.-P. BEAULIEU (IAP), B. ROYA-AYALA (IA), C. RANC, N.C. SANTOS, V. BATISTA, D. BENNETT, E. SCHLAWIN, J.B. MARQUETTE, S. SOUSA, R. DIAZ, J.-M. ALMENARA, D. JAMES, T. HERTER

Introduction

V

J

E

U

S

N

30 cm/s

3 m/s

1 m/s

RV

Imaging

Transit

μ-lensing

from exoplanet.eu and exoplanet.org June 2014

http://exoplanet.eu http://exoplanet.org

OGLE-2011-BLG-0417

Shin et al. 2012Binary system

OGLE-2011-BLG-0417 Characteristics

Lens Source

K3 red giant 8 kpc

binary M dwarfs 0.95 kpc I = 16.3

I = 16.74V = 18.23 V = 19.42

OGLE-2011-BLG-0417 Characteristics

Lens Source

K3 red giant 8 kpc

binary M dwarfs 0.95 kpc I = 16.3

I = 16.74V = 18.23 V = 19.42

OGLE-2011-BLG-0417 Gould et al. 2013Predicted RV curve

OGLE-2011-BLG-0417 Gould et al. 2013Predicted RV curve

Several km/s

OGLE-2011-BLG-0417 Gould et al. 2013Predicted RV curve

Several km/s

P = 1.42 yr

OGLE-2011-BLG-0417 Gould et al. 2013Predicted RV curve

Several km/s

P = 1.42 yr

Phase is lost

Observations UVES @ VLT, ESO

Observations UVES @ VLT, ESO

Crowded field

Observations UVES @ VLT, ESO

Crowded field

10 spectra of ~1h

SNR ~ 20 (550nm)

Observations UVES @ VLT, ESO

Crowded field

10 spectra of ~1h

SNR ~ 20 (550nm)

1” slit: R~40 000

Observations UVES @ VLT, ESO

Crowded field

10 spectra of ~1h

SNR ~ 20 (550nm)

1” slit: R~40 000

Th-Ar calib before and after exposures

Data reduction Reduced with Reflex (ESO)

Data reduction CCF with K5 maskReduced with Reflex (ESO)

�80 �60 �40 �20 0 20 40 60 80 Radial velocity [km.s�1]

0.75

0.80

0.85

0.90

0.95

1.00

1.05

C C

F co

nt ra

st

source lens

3300 – 4500 Å 4800 – 5800 Å 5800 – 6800 Å

Data reduction CCF with K5 maskReduced with Reflex (ESO)

�80 �60 �40 �20 0 20 40 60 80 Radial velocity [km.s�1]

0.75

0.80

0.85

0.90

0.95

1.00

1.05

C C

F co

nt ra

st

source lens

3300 – 4500 Å 4800 – 5800 Å 5800 – 6800 Å

Data reduction CCF with K5 mask

(V-I) = 1.93 ; (V-I) = 2.68sourcelens

Reduced with Reflex (ESO)

�80 �60 �40 �20 0 20 40 60 80 Radial velocity [km.s�1]

0.75

0.80

0.85

0.90

0.95

1.00

1.05

C C

F co

nt ra

st

source lens

3300 – 4500 Å 4800 – 5800 Å 5800 – 6800 Å

Data reduction CCF with K5 mask

(V-I) = 1.93 ; (V-I) = 2.68sourcelens

Reduced with Reflex (ESO)

Bluer lens

�80 �60 �40 �20 0 20 40 60 80 Radial velocity [km.s�1]

0.75

0.80

0.85

0.90

0.95

1.00

1.05

C C

F co

nt ra

st

source lens

3300 – 4500 Å 4800 – 5800 Å 5800 – 6800 Å

Data reduction CCF with K5 mask

(V-I) = 1.93 ; (V-I) = 2.68sourcelens

Reduced with Reflex (ESO)

Bluer lens

lens source

Data reduction Corrected from BERV

Data reduction Corrected from BERV

Corrected from spectrograph drift (15 to 400 m/s in 1 h)

Data reduction Corrected from BERV

Corrected from spectrograph drift (15 to 400 m/s in 1 h)

But Variation of the illumination of the slit

Data reduction Corrected from BERV

Corrected from spectrograph drift (15 to 400 m/s in 1 h)

But Variation of the illumination of the slit

Corrected from RV telluric reference (O2 lines)

Data reduction

6550 6600 6650 6700 6750 6800 6850 6900 6950 Time [BJD - 2 450 000]

�0.6

�0.4

�0.2

0.0

0.2

0.4

0.6

0.8

R el

at iv

e R

V [k

m .s

� 1 ]

lens source

Data reduction

6550 6600 6650 6700 6750 6800 6850 6900 6950 Time [BJD - 2 450 000]

�0.6

�0.4

�0.2

0.0

0.2

0.4

0.6

0.8

R el

at iv

e R

V [k

m .s

� 1 ]

lens source

Stars RV share same systematics !

Data reduction

6550 6600 6650 6700 6750 6800 6850 6900 6950 Time [BJD - 2 450 000]

�0.6

�0.4

�0.2

0.0

0.2

0.4

0.6

0.8

R el

at iv

e R

V [k

m .s

� 1 ]

lens source

Stars RV share same systematics !

Used RV source as a reference for RV lens

Results

RMS = 94 m/s

6500 6600 6700 6800 6900 7000 Time [BJD - 2 450 000]

40

42

44

46

48

50

52

54

D iff

er en

tia lR

V (R

V le

n s

-R V

so u rc

e) [k

m .s

� 1 ]

OGLE-2011-BLG-0417

predicted best model observed

6500 6600 6700 6800 6900 7000

42.2

42.4

42.6

42.8

43.0

Results

RMS = 94 m/s

6500 6600 6700 6800 6900 7000 Time [BJD - 2 450 000]

40

42

44

46

48

50

52

54

D iff

er en

tia lR

V (R

V le

n s

-R V

so u rc

e) [k

m .s

� 1 ]

OGLE-2011-BLG-0417

predicted best model observed

6500 6600 6700 6800 6900 7000

42.2

42.4

42.6

42.8

43.0

Results

RMS = 94 m/s PASTIS validation tool

Diaz et al. 2014

6500 6600 6700 6800 6900 7000 Time [BJD - 2 450 000]

40

42

44

46

48

50

52

54

D iff

er en

tia lR

V (R

V le

n s

-R V

so u rc

e) [k

m .s

� 1 ]

OGLE-2011-BLG-0417

predicted best model observed

6500 6600 6700 6800 6900 7000

42.2

42.4

42.6

42.8

43.0

Results

RMS = 94 m/s PASTIS validation tool

Diaz et al. 2014 Probability < 2 10 -7

Conclusion

Spectroscopic follow-up observations of microlensing event is possible

We don’t confirm the Gould et al. prediction

Boisse et al. 2015

Conclusion

Spectroscopic follow-up observations of microlensing event is possible

We don’t confirm the Gould et al. prediction

Boisse et al. 2015

Yee et al. 2015Recently same method on a different target

Conclusion

Bright component is most probably not the light from the lens

Spectroscopic follow-up observations of microlensing event is possible

We don’t confirm the Gould et al. prediction

Boisse et al. 2015

Yee et al. 2015Recently same method on a different target

Conclusion

Bright component is most probably not the light from the lens

Spectroscopic follow-up observations of microlensing event is possible

The lens is not detectable

We don’t confirm the Gould et al. prediction

Boisse et al. 2015

Yee et al. 2015Recently same method on a different target

Conclusion

Bright component is most probably not the light from the lens

Spectroscopic follow-up observations of microlensing event is possible

The lens is not detectable

We don’t confirm the Gould et al. prediction

High angular resolution observations planned

Boisse et al. 2015

Yee et al. 2015Recently same method on a different target

Keck AO imaging

No blend within 130mas

Probability to have another star within 130mas ~ 50ppm

Santerne et al. (submitted)

Spectral Energy Distribution

0.3 0.4 0.5 0.6 0.7 0.8 1.0 1.3 1.5 1.8 2.0 2.5 Wavelength [µm]

10�18

10�17

10�16

10�15

C al

ib ra

te d

flu x

[e rg

.s �

1 .c

m �

2 .Å

� 1 ]

J H K

Santerne et al. (submitted)

Spectral Energy Distribution

0.3 0.4 0.5 0.6 0.7 0.8 1.0 1.3 1.5 1.8 2.0 2.5 Wavelength [µm]

10�18

10�17

10�16

10�15

C al

ib ra

te d

flu x

[e rg

.s �

1 .c

m