Ogle 2003 blg 235 moa 2003 blg 53 a definitive planetary microlensing event
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OGLE-2003-BLG-235/MOA-2003-BLG-53: A Definitive Planetary Microlensing Event. David Bennett University of Notre Dame. Author List:. I.A. Bond, A. Udalski, M. Jaroszynski, N.J. Rattenbury, B. Paczynski, I. Soszynski, L. Wyrzykowski, M.K. Szymanski, M. Kubiak,

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Ogle 2003 blg 235 moa 2003 blg 53 a definitive planetary microlensing event
OGLE-2003-BLG-235/MOA-2003-BLG-53: A Definitive Planetary Microlensing Event

David Bennett

University of Notre Dame


Author list
Author List:

I.A. Bond, A. Udalski, M. Jaroszynski,

N.J. Rattenbury, B. Paczynski, I. Soszynski,

L. Wyrzykowski, M.K. Szymanski, M. Kubiak,

O. Szewczyk, K. Zebrun, G. Pietrzynski, F.Abe, D.P. Bennett, S. Eguchi, Y. Furuta, J.B. Hearnshaw, K. Kamiya, P.M. Kilmartin, Y. Kurata, K. Masuda, Y. Matsubara, Y. Muraki, S. Noda, K. Okajima,

T. Sako, T. Sekiguchi, D.J. Sullivan, T. Sumi,

P.J. Tristram, T. Yanagisawa, and P.C.M. Yock

(the MOA and OGLE collaborations)


Real time lightcurve monitoring is critical
Real-Time Lightcurve Monitoring is Critical!

  • Ian Bond (IFA, Edinburgh) noticed a caustic crossing for this event on July 23, 2003.

  • He contacted the telescope and requested additional images

  • The requested images caught the caustic crossing endpoint.

  • This caustic endpoint data is critical to the conclusion that a planet is required.


Lightcurve
Lightcurve

OGLE

alert


Definition of a planet
Definition of a Planet

  • Formed by core accretion? (with a rocky core)

    • But we don’t know that this is how planets form!

    • We aren’t even sure about Jupiter’s rocky core!

  • Secondary Mass < 13 Mjupiter?

    • This is the Deuterium burning threshold for solar metalicity, but why is that important?

    • What if binary is a 0.08 M?

      • Mass ratio may only be 0.16!

    • In the brown dwarf desert

  • Planetary mass fraction  < 0.03

    • In the brown dwarf desert

    • Easily measured in a microlensing lightcurve!!


Lightcurve close up fit
Lightcurve close-up & fit

  • Cyan curve is the best fit single lens model

    • 2 = 651

  • Magenta curve is the best fit model w/ mass fraction   0.03

    • 2 = 323

  • 7 days inside caustic = 0.12 tE

    • Long for a planet,

    • but mag = only 20-25%

    • as expected for a planet near the Einstein Ring


Caustic structure magnification pattern
Caustic Structure & Magnification Pattern

Blue and red dots indicate times of observations

Parameters:

tE = 61.6  1.8 days

t0= 2848.06  0.13 MJD

umin = 0.133  0.003

ap = 1.120  0.007

 = 0.0039  0.007 q = /(1+ )

 = 223.8  1.4

t*= 0.059  0.007 days or */E = 0.00096  0.00011


Alternative models a p 1
Alternative Models: ap < 1

2 = 110.4

tE = 75.3 days

t0= 2850.64 MJD

umin = 0.098

ap = 0.926

 = 0.0117

 = -6.1

t*= 0.036 days

Also planetary!


Alternative models a p 11
Alternative Models: ap < 1

2 = 110.4

tE = 75.3 days

t0= 2850.64 MJD

umin = 0.098

ap = 0.926

 = 0.0117

 = -6.1

t*= 0.036 days

Also planetary!


Alternative models 180
Alternative Models:  ~180

2 = 40.15

tE = 76.0 days

t0= 2847.09 MJD

umin = 0.100

ap = 1.064

 = 0.0127

 = 185.6

t*= 0.034 days

Also planetary!


Alternative models 1801
Alternative Models:  ~180

2 = 40.15

tE = 76.0 days

t0= 2847.09 MJD

umin = 0.100

ap = 1.064

 = 0.0127

 = 185.6

t*= 0.034 days

Also planetary!


Alternative models early 1 st caustic crossing
Alternative Models: Early 1st Caustic Crossing

2 = 7.37

tE = 58.5 days

t0= 2847.90 MJD

umin = 0.140

ap = 1.121

 = 0.0069

 = 218.9

t*= 0.061 days

Excluded by 2.7

Adjust

 = 0.0039  0.007 to

 = 0.0039  0.011


Lens star constraints
Lens Star Constraints

Using Isource = 19.7

and V-I = 1.58,we conclude that the source is a bulge G dwarf of radius:

* = 520  80 as

Iblend= 20.7  0.4

Gives likelihood curve


Planetary parameters in physical units
Planetary Parameters in Physical Units

  • Best fit lens distance = 5.2 kpc

    • 90% c.l. range is 2.3-5.4 kpc

  • Best fit separation = 3.0 AU

    • 90% c.l. range is 1.3-3.1 AU

  • Best fit stellar mass = 0.36 M

    • 90% c.l. range is 0.08-0.39 M

  • Best fit planet mass = 1.5 Mjup

    • 90% c.l. range is 0.3-1.6 Mjup

  • If lens star is a 0.6 M white dwarf

    • Dlens = 6.1 kpc

    • ap = 1.8 AU

    • Mp = 2.5 Mjup


Conclusions
Conclusions

1st definitive lensing planetary discovery

- complete coverage not required for characterization

Real-time data monitoring was critical!

S. Gaudi video


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