Extreme Magnification Microlensing Event Ogle-2008-BLG-279: Strong Limits on Planetary Companions to the Lens Star

Yee, Jennifer C.; Udalski, A.; Sumi, T.; Dong, Subo; Kozłowski, S.; Bird, Jonathan C.; Cole, A. A.; Higgins, David; McCormick, J.; Monard, L. A. G.; Polishook, David; Shporer, Avi; Spector, O.; Szymański, M. K.; Kubiak, M.; Pietrzyński, G.; Soszyński, I.; Szewczyk, O.; Ulaczyk, K.; Wyrzykowski, Ł.; Poleski, R.; Allen, William H.; Bos, M.; Christie, Grant; DePoy, D. L.; Eastman, Jason D.; Gaudi, B. Scott; Gould, Andrew; Han, Cheongho; Kaspi, S.; Lee, Chung-Uk; Mallia, F.; Maury, A.; Maoz, Dan; Natusch, T.; Park, B. G.; Pogge, Richard W.; Santallo, R.; Abe, F.; Bond, I. A.; Fukui, A.; Furusawa, K.; Hearnshaw, John; Hosaka, S.; Itow, Y.; Kamiya, K.; Korpela, A.; Kilmartin, P. M.; Lin, Wei; Ling, C. H.; Makita, S.; Masuda, K.; Matsubara, Y.; Miyake, N.; Muraki, Y.; Nagaya, M.; Nishimoto, K.; Ohnishi, Kouhei; Perrott, Y. C.; Rattenbury, N. J.; Sako, T.; Saito, To.; Skuljan, L.; Sullivan, D. J.; Sweatman, W. L.; Tristram, P. J.; Yock, P. C. M.; Albrow, M. D.; Batista, V.; Fouqué, P.; Beaulieu, J. P.; Bennett, D. P.; Cassan, A.; Comparat, Johan; Coutures, C.; Dieters, S.; Greenhill, J.; Horne, K.; Kains, N.; Kubas, D.; Martín, Roland; Menzies, John; Wambsganß, J.; Williams, A.; Zub, M.

doi:10.1088/0004-637x/703/2/2082

Cited by 75 publications

(42 citation statements)

References 30 publications

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“…The determined angular radius of the source star is θ = 6.11 ± 0.53 μas, implying that the source star is a Galactic bulge clump giant star. The uncertainty of θ is estimated from the combination of those of the colors and magnitudes of the source and the clump centroid and an additional 7% intrinsic error in the conversion process from the color to the source radius (Yee et al 2009). Then, the Einstein radius is measured as…”

Section: Resultsmentioning

confidence: 99%

Ogle-2009-BLG-092/Moa-2009-BLG-137: A Dramatic Repeating Event With the Second Perturbation Predicted by Real-Time Analysis

Ryu¹,

Han²,

Hwang³

et al. 2010

ApJ

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We report the result of the analysis of a dramatic repeating gravitational microlensing event OGLE-2009-BLG-092/MOA-2009, for which the light curve is characterized by two distinct peaks with perturbations near both peaks. We find that the event is produced by the passage of the source trajectory over the central perturbation regions associated with the individual components of a wide-separation binary. The event is special in the sense that the second perturbation, occurring ∼100 days after the first, was predicted by the real-time analysis conducted after the first peak, demonstrating that real-time modeling can be routinely done for binary and planetary events. With the data obtained from follow-up observations covering the second peak, we are able to uniquely determine the physical parameters of the lens system. We find that the event occurred on a bulge clump giant and it was produced by a binary lens composed of a K-and M-type main-sequence stars. The estimated masses of the binary components are M 1 = 0.69±0.11 M and M 2 = 0.36±0.06 M , respectively, and they are separated in projection by r ⊥ = 10.9±1.3 AU. The measured distance to the lens is D L = 5.6 ± 0.7 kpc. We also detect the orbital motion of the lens system.

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Section: Resultsmentioning

confidence: 99%

Ogle-2009-BLG-092/Moa-2009-BLG-137: A Dramatic Repeating Event With the Second Perturbation Predicted by Real-Time Analysis

Ryu¹,

Han²,

Hwang³

et al. 2010

ApJ

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“…For observations towards the Galactic bulge, the sensitivity of gravitational microlensing to planets with masses much below that of Earth has already been demonstrated [74,103,157], and it has been pointed out that, already without deploying a space mission, one could reach down to objects similar to the moon [158,159].…”

Section: Future Directionsmentioning

confidence: 99%

Studying planet populations by gravitational microlensing

Dominik

2010

Gen Relativ Gravit

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The 'most curious' effect of the bending of light by the gravity of stars has evolved into a successful technique unlike any other for studying planets within the Milky Way and even other galaxies. With a sensitivity to cool planets around low-mass stars even below the mass of Earth, gravitational microlensing fits in between other planet search techniques to form a complete picture of planet parameter space, which is required to understand their origin in general, that of habitable planets more particularly, and that of planet Earth especially. Current campaigns need to evolve from first detections to obtaining a sample with well-understood selection bias that allows to draw firm conclusions about the planet populations. With planetary signals being a transient phenomenon, gravitational microlensing is a driver for new technologies in scheduling and management of non-proprietary heterogeneous telescope networks, and can serve to demonstrate forefront science live to the general public.

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“…From the observational side, the surveys Microlensing Planet Search (MPS) (Rhie 1999) and Microlensing Observations in Astrophysics (MOA) (Rhie et al 2000;Sumi et al 2003) demonstrated for the first time that microlensing technique is sensitive enough to detect earth-mass exoplanets. Shvartzvald et al (2017) show the possibility to detect Earth-mass Planet in a 1 AU Orbit around an Ultracool Dwarf and Yee et al (2009) present an extreme magnification microlensing event and its sensitivity to planets with masses as small as 0.2M ⊕ 2M M ars with projected separations near the Einstein ring ( 3 AU). Gould et al (2014) even showed the capability of microlensing technique to discover Earth-mass planets around 1 AU in binary systems.…”

Section: Introductionmentioning

confidence: 99%

Microlensing Path Parameterization for Earth-like Exoplanet Detection around Solar-mass Stars

Almeida¹,

Nascimento²

2018

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We propose a new parametrization of the impact parameter u 0 and impact angle α for microlensing systems composed by an Earth-like Exoplanet around a Solar mass Star at 1 AU. We present the caustic topology of such system, as well as the related light curves generated by using such a new parametrization. Based on the same density of points and accuracy of regular methods, we obtain results 5 times faster for discovering Earth-like exoplanet. In this big data revolution of photometric astronomy, our method will impact future missions like WFIRST (NASA) and Euclid (ESA) and they data pipelines, providing a rapid and deep detection of exoplanets for this specific class of microlensing event that might otherwise be lost.

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Extreme Magnification Microlensing Event Ogle-2008-BLG-279: Strong Limits on Planetary Companions to the Lens Star

Cited by 75 publications

References 30 publications

Ogle-2009-BLG-092/Moa-2009-BLG-137: A Dramatic Repeating Event With the Second Perturbation Predicted by Real-Time Analysis

Ogle-2009-BLG-092/Moa-2009-BLG-137: A Dramatic Repeating Event With the Second Perturbation Predicted by Real-Time Analysis

Studying planet populations by gravitational microlensing

Microlensing Path Parameterization for Earth-like Exoplanet Detection around Solar-mass Stars

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