MOA-2011-BLG-293Lb: A TEST OF PURE SURVEY MICROLENSING PLANET DETECTIONS

Yee, Jennifer C.; Shvartzvald, Yossi; Gal‐Yam, A.; Bond, I. A.; Udalski, A.; Kozłowski, S.; Han, Cheongho; Gould, Andrew; Skowron, J.; Suzuki, D.; Abe, F.; Bennett, D. P.; Botzler, C. S.; Chote, P.; Freeman, Matthew; Fukui, A.; Furusawa, K.; Itow, Y.; Kobara, S.; Ling, C. H.; Masuda, K.; Matsubara, Y.; Miyake, N.; Muraki, Y.; Ohmori, K.; Ohnishi, Kouhei; Rattenbury, N. J.; Saito, To.; Sullivan, D. J.; Sumi, T.; Suzuki, Kunio; Sweatman, W. L.; Takino, S.; Tristram, P. J.; Wada, K.; Szymański, M. K.; Kubiak, M.; Pietrzyński, G.; Poleski, R.; Ulaczyk, K.; Wyrzykowski, Ł.; Allen, William H.; Almeida, L. A.; Batista, V.; Bos, M.; Christie, Grant; Depoy, D. L.; Dong, Subo; Drummond, J.; Finkelman, Ido; Gaudi, B. Scott; Gorbikov, E.; Henderson, Calen B.; Higgins, David; Jablonski, F.; Kaspi, S.; Manulis, I.; Maoz, Dan; McCormick, J.; McGregor, D.; Monard, L. A. G.; Moorhouse, D.; Muñoz, J. A.; Natusch, T.; Ngan, H.; Ofek, E. O.; Pogge, Richard W.; Santallo, R.; Tan, T. G.; Thornley, G.; Shin, In-Gu; Choi, J.-Y.; Park, S.-Y.; Lee, Chung-Uk; Koo, Jae‐Rim

doi:10.1088/0004-637x/755/2/102

Cited by 211 publications

(178 citation statements)

References 43 publications

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“…This implies that the lens system is very likely to be in the Galactic bulge. Penny et al (2016) (Rattenbury et al 2015), and MOA-2011-BLG-293L (Yee et al 2012;Batista et al 2014). Actually, the problem with the Penny et al (2016) analysis is pretty easy to understand.…”

Section: Lens Properties and Discussionmentioning

confidence: 99%

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

Bhattacharya

Bennett

Bond

et al. 2016

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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.

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Section: Lens Properties and Discussionmentioning

confidence: 99%

“…These error-bar estimates are good measures of the relative uncertainties for measurements with the same telescope, but they are often wrong by a factor of ∼2 (Yee et al 2012). To determine the uncertainties for the model parameters, it is necessary to have accurate error bars that will give c » dof 1 2 for each data set.…”

Section: Data Reductionmentioning

confidence: 99%

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

Bhattacharya

Bennett

Bond

et al. 2016

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“…For this readjustment, we follow the standard procedure of Yee et al (2012), where the error bars are renormalized by…”

Section: Observation and Datamentioning

confidence: 99%

OGLE-2014-BLG-0289: Precise Characterization of a Quintuple-peak Gravitational Microlensing Event

Udalski¹,

Han²,

Bozza³

et al. 2018

ApJ

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We present the analysis of the binary-microlensing event OGLE-2014-BLG-0289. The event light curve exhibits five very unusual peaks, four of which were produced by caustic crossings and the other by a cusp approach. It is found that the quintuple-peak features of the light curve provide tight constraints on the source trajectory, enabling us to precisely and accurately measure the microlensing parallax E p . Furthermore, the three resolved caustics allow us to measure the angular Einstein radius E q . From the combination of E p and E q , the physical lens parameters are uniquely determined. It is found that the lens is a binary composed of two M dwarfs with masses M M 0.52 0.04 1 =   and M M 0.42 0.03 2 =   separated in projection by a 6.4 0.5 au =  . The lens is located in the disk with a distance of D 3.3 0.3 kpc L =  . The reason for the absence of a lensing signal in the Spitzer data is that the time of observation corresponds to the flat region of the light curve.

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“…Photometry of the data were conducted using the pipelines developed by the individual groups based on the difference imaging analysis method (Alard & Lupton 1998;Bramich et al 2013). Since the data sets were taken using different instruments and reduced based on different software, we normalize the error bars of the individual data sets using the method described in Yee et al (2012). According to this method, error bars are rescaled by the relation k 0 2 min…”

Section: Observations and Datamentioning

confidence: 99%

OGLE-2017-BLG-0329L: A Microlensing Binary Characterized with Dramatically Enhanced Precision Using Data from Space-based Observations

Han¹,

Novati²,

Udalski³

et al. 2018

ApJ

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Mass measurements of gravitational microlenses require one to determine the microlens parallax π E , but precise π E measurement, in many cases, is hampered due to the subtlety of the microlens-parallax signal combined with the difficulty of distinguishing the signal from those induced by other higher-order effects. In this work, we present the 1 analysis of the binary-lens event OGLE-2017-BLG-0329, for which π E is measured with a dramatically improved precision using additional data from space-based Spitzer observations. We find that while the parallax model based on the ground-based data cannot be distinguished from a zero-π E model at the 2σ level, the addition of the Spitzer data enables us to identify two classes of solutions, each composed of a pair of solutions according to the wellknown ecliptic degeneracy. It is found that the space-based data reduce the measurement uncertainties of the north and east components of the microlens-parallax vector E p by factors ∼18 and ∼4, respectively. With the measured microlens parallax combined with the angular Einstein radius measured from the resolved caustic crossings, we find that the lens is composed of a binary with component masses of either (M 1 , M 2 )∼(1.1, 0.8) M e or ∼(0.4, 0.3) M e according to the two solution classes. The first solution is significantly favored but the second cannot be securely ruled out based on the microlensing data alone. However, the degeneracy can be resolved from adaptive optics observations taken ∼10 years after the event.

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MOA-2011-BLG-293Lb: A TEST OF PURE SURVEY MICROLENSING PLANET DETECTIONS

Cited by 211 publications

References 43 publications

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

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

OGLE-2014-BLG-0289: Precise Characterization of a Quintuple-peak Gravitational Microlensing Event

OGLE-2017-BLG-0329L: A Microlensing Binary Characterized with Dramatically Enhanced Precision Using Data from Space-based Observations

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