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  • 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