Confirmation of the Planetary Microlensing Signal and Star and Planet Mass Determinations for Event Ogle-2005-BLG-169

Bennett, D. P.; Bhattacharya, Aparna; Anderson, Jay; Bond, I. A.; Anderson, N.; Barry, Richard; Batista, V.; Beaulieu, J. P.; Depoy, D. L.; Dong, Subo; Gaudi, B. Scott; Gilbert, Emily A.; Gould, Andrew; Pfeifle, Ryan W.; Pogge, R. W.; Suzuki, D.; Terry, Sean K.; Udalski, A.

doi:10.1088/0004-637x/808/2/169

Cited by 169 publications

(199 citation statements)

References 53 publications

Supporting

Mentioning

194

Contrasting

Order By: Relevance

“…Close-ups of summed images centered on the OGLE-2007-BLG-349 target from each visit are shown in Figure 8, and the change in magnification of the target is clearly visible. Because these images were taken within a year of peak magnification, the separation between the lens and source stars (Bennett et al 2006(Bennett et al , 2007(Bennett et al , 2015 is not detectable.…”

Section: Hst Imagesmentioning

confidence: 99%

See 1 more Smart Citation

THE FIRST CIRCUMBINARY PLANET FOUND BY MICROLENSING: OGLE-2007-BLG-349L(AB)c

Bennett¹,

Rhie²,

Udalski³

et al. 2016

Self Cite

106

View full text Add to dashboard Cite

We present the analysis of the first circumbinary planet microlensing event, OGLE-2007-BLG-349. This event has a strong planetary signal that is best fit with a mass ratio of q≈3.4×10 −4 , but there is an additional signal due to an additional lens mass, either another planet or another star. We find acceptable light-curve fits with two classes of models: two-planet models (with a single host star) and circumbinary planet models. The light curve also reveals a significant microlensing parallax effect, which constrains the mass of the lens system to be M L ≈0.7  M . Hubble Space Telescope (HST) images resolve the lens and source stars from their neighbors and indicate excess flux due to the star(s) in the lens system. This is consistent with the predicted flux from the circumbinary models, where the lens mass is shared between two stars, but there is not enough flux to be consistent with the two-planet, one-star models. So, only the circumbinary models are consistent with the HST data. They indicate a planet of mass m c =80±13 Å M , orbiting a pair of M dwarfs with masses of M A =0.41±0.07 and M B =0.30±0.07, which makes this the lowest-mass circumbinary planet system known. The ratio of the separation between the planet and the center of mass to the separation of the two stars is ∼40, so unlike most of the circumbinary planets found by Kepler, the planet does not orbit near the stability limit.

show abstract

Section: Hst Imagesmentioning

confidence: 99%

“…For possibilities 1 and 3, we require a mass-luminosity relation, and we use the same empirical mass-luminosity relation that was used in Bennett et al (2015). We use the mass-luminosity relations of Henry & McCarthy (1993), Henry et al (1999), and Delfosse et al (2000) …”

Section: Light-curve Models With Hst Constraintmentioning

confidence: 99%

THE FIRST CIRCUMBINARY PLANET FOUND BY MICROLENSING: OGLE-2007-BLG-349L(AB)c

Bennett¹,

Rhie²,

Udalski³

et al. 2016

Self Cite

106

View full text Add to dashboard Cite

show abstract

“…2017). The lens detection can be confirmed by measuring the lens-source relative proper motion (Batista et al 2015;Bennett et al 2015). Figure 7 shows the probability distribution of I-, V-, H-, and K-band magnitudeof the lens star with extinction.…”

Section: Discussionmentioning

confidence: 82%

OGLE-2013-BLG-1761Lb: A Massive Planet around an M/K Dwarf

Hirao

Udalski

Sumi

et al. 2017

Self Cite

View full text Add to dashboard Cite

We report the discovery and the analysis of the planetary microlensing event, OGLE-2013-BLG-1761. There are some degenerate solutions in this event because the planetary anomaly is only sparsely sampled. However,the detailed lightcurve analysis ruled out all stellar binary models and shows the lens to be a planetary system. There is the so-called close/wide degeneracy in the solutions with the planet/host mass ratio of q∼(7.0±2.0)×10 −3 and q∼(8.1±2.6)×10−3 with the projected separation in Einstein radius units of s=0.95 (close) and s=1.18 (wide), respectively. The microlens parallax effect is not detected, but the finite source effect is detected. Our Bayesian analysis indicates that the lens system is located = . The preference of the large lens distance in the Bayesian analysis is due to the relatively large observed source star radius. The distance and other physical parameters may be constrained by the future high-resolution imaging by large groundtelescopes orHST. If the estimated lens distance is correct, thenthis planet provides another sample for testing the claimed deficit of planets in the Galactic bulge.-

show abstract

“…For each MCMC fit, the source distance is picked randomly from this distribution. From emperical mass-luminosity relations (Henry & McCarthy 1993;Henry et al 1999;Delfosse et al 2000) and massdistance relations, we estimated the lens distance, host-star and planet mass, host-star brightness, and host-star and planet projected separation using a method similar to that used by Batista et al (2015) and Bennett et al (2015). Then, we calculated mean, median, and posterior distributions for each parameter from all of these MCMC fits, as seen in Table 3 , spans the range from the mass of Saturn to that of Jupiter.…”

Section: Lens Properties and Discussionmentioning

confidence: 99%

“…This is close to the Jupiter/Sun mass ratio, but the host star probably has a mass of *   M M , so this planet is probably a low-mass gas giant, like Saturn. Follow-up observations with JWST, HST, or adaptive optics in 2020-2022 should be able to measure the lens brightness and determine the planetary mass and distance using the methods of Bennett et al (2006Bennett et al ( , 2007Bennett et al ( , 2015, and Batista et al (2015). Later with WFIRST (Spergel et al 2015), a similar kind of study will provide the statistics needed to determine the planetary mass function as a function of the host-star mass and distance.…”

Section: Lens Properties and Discussionmentioning

confidence: 99%

Discovery of a Gas Giant Planet in Microlensing Event Ogle-2014-BLG-1760

Bhattacharya

Bennett

Bond

et al. 2016

Self Cite

View full text Add to dashboard Cite

We present the analysis of the planetary microlensing event OGLE-2014-BLG-1760, which shows a strong lightcurve signal due to the presence of a Jupiter mass ratio planet. One unusual feature of this event is that the source star is quite blue, with -=  V I 1.48 0.08. This is marginally consistent with a source star in the Galactic bulge, but it could possibly indicate a young source star on the far side of the disk. Assuming a bulge source, we perform a Bayesian analysis assuming a standard Galactic model, and this indicates that the planetary system resides in or near the Galactic bulge at =  D 6.9 1.1 kpc , and a projected star-planet separation of = -+ a 1.75 0.33 0.34 au. The lens-source relative proper motion is m =  6.5 1.1 rel mas yr −1 . The lens (and stellar host star) is estimated to be very faint compared to the source star, so it is most likely that it can be detected only when the lens and source stars start to separate. Due to the relatively high relative proper motion, the lens and source will be resolved to about ∼46 mas in 6-8 yr after the peak magnification. So, by 2020-2022, we can hope to detect the lens star with deep, high-resolution images.

show abstract

Confirmation of the Planetary Microlensing Signal and Star and Planet Mass Determinations for Event Ogle-2005-BLG-169

Cited by 169 publications

References 53 publications

THE FIRST CIRCUMBINARY PLANET FOUND BY MICROLENSING: OGLE-2007-BLG-349L(AB)c

THE FIRST CIRCUMBINARY PLANET FOUND BY MICROLENSING: OGLE-2007-BLG-349L(AB)c

OGLE-2013-BLG-1761Lb: A Massive Planet around an M/K Dwarf

Discovery of a Gas Giant Planet in Microlensing Event Ogle-2014-BLG-1760

Contact Info

Product

Resources

About