OGLE-2016-BLG-1190Lb: The First Spitzer Bulge Planet Lies Near the Planet/Brown-dwarf Boundary

Ryu, Yoon-Hyun; Yee, Jennifer C.; Udalski, A.; Bond, I. A.; Shvartzvald, Yossi; Zang, Weicheng; Jaimes, R. Figuera; Jørgensen, U. G.; Zhu, Wei; Huang, Chelsea X.; Jung, Youn Kil; Albrow, M. D.; Chung, Sun-Ju; Gould, Andrew; Han, Cheongho; Hwang, Kyu-Ha; Shin, In-Gu; Cha, Sang-Mok; Kim, Dong-Jin; Kim, H.-W.; Kim, S.-L.; Lee, C.-U.; Lee, D.-J.; Lee, Y.; Park, B.-G.; Pogge, Richard W.; Novati, S. Calchi; Carey, Sean; Henderson, Calen B.; Beichman, C.; Gaudi, B. Scott; Mróz, P.; Poleski, R.; Skowron, J.; Szymański, M. K.; Soszyński, I.; Kozłowski, S.; Ulaczyk, K.; Pawlak, M.; Abe, F.; Asakura, Y.; Barry, Richard; Bennett, D. P.; Bhattacharya, Aparna; Donachie, M.; Evans, P.; Fukui, A.; Hirao, Yuki; Itow, Y.; Kawasaki, Kohei; Koshimoto, Naoki; Li, M. C. A.; Ling, C. H.; Masuda, K.; Matsubara, Y.; Miyazaki, Shota; Muraki, Y.; Nagakane, M.; Ohnishi, Koji; Ranc, Clément; Rattenbury, N. J.; Saito, To.; Sharan, A.; Sullivan, D. J.; Sumi, T.; Suzuki, D.; Tristram, P. J.; Yamada, Tōru; Yonehara, A.; Bryden, G.; Howell, Stephen B.; Jacklin, Savannah; Penny, Matthew T.; Mao, Shude; Fouqué, P.; Wang, T.; Street, R. A.; Tsapras, Y.; Hundertmark, M.; Bachelet, E.; Dominik, M.; Li, Zhexing; Cross, Stephen; Cassan, A.; Horne, K.; Schmidt, R. W.; Wambsganß, J.; Ment, S. K.; Maoz, Dan; Snodgrass, C.; Steele, I. A.; Bozza, V.; Burgdorf, M.; Ciceri, S.; D’Ago, G.; Evans, D. F.; Hinse, T. C.; Kerins, E.; Kokotanekova, Rosita; Longã, P.; MacKenzie, Jasmine; Popovas, A.; Rabus, M.; Rahvar, S.; Sajadian, Sedighe; Skottfelt, J.; Southworth, J.; Essen, C. von

doi:10.3847/1538-3881/aa9be4

Cited by 61 publications

(27 citation statements)

References 77 publications

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“…The wide-field optical and infra-red telescopes on Mauna Kea (CFHT-MegaCam, CFHT-WIRCAM, Subaru-HyperSuprimeCam, and UKIRT-WFCAM) can therefore add significant value to the existing microlensing survey networks. This has been demonstrated by our data set's contribution to several planet discoveries in 2016 (Koshimoto et al 2017;Ryu et al 2018;Han et al 2017).…”

Section: Discussionsupporting

confidence: 62%

Measurement of Source Star Colors with the K2C9-CFHT Multi-color Microlensing Survey

Zang

Penny

Zhu

et al. 2018

PASP

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K2 Campaign 9 (K2C9) was the first space-based microlensing parallax survey capable of measuring microlensing parallaxes of free-floating planet candidate microlensing events. Simultaneous to K2C9 observations we conducted the K2C9 Canada-France-Hawaii Telescope Multi-Color Microlensing Survey (K2C9-CFHT MCMS) in order to measure the colors of microlensing source stars to improve the accuracy of K2C9's parallax measurements. We describe the difference imaging photometry analysis of the K2C9-CFHT MCMS observations, and present the project's first data release. This includes instrumental difference flux lightcurves of 217 microlensing events identified by other microlensing surveys, reference image photometry calibrated to PanSTARRS data release 1 photometry, and tools to convert between instrumental and calibrated flux scales. We derive accurate analytic transformations between the PanSTARRS bandpasses and the Kepler bandpass, as well as angular diametercolor relations in the PanSTARRS bandpasses. To demonstrate the use of our data set, we analyze ground-based and K2 data of a short timescale microlensing event, OGLE-2016-BLG-0795. We find the event has a timescale t E = 4.5 ± 0.1 days and microlens parallax π E = 0.12 ± 0.03 or 0.97 ± 0.04, subject to the standard satellite parallax degeneracy. We argue that the smaller value of the parallax is more likely, which implies that the lens is likely a stellar-mass object in the Galactic bulge as opposed to a super-Jupiter mass object in the Galactic disk.

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Section: Discussionsupporting

confidence: 62%

Measurement of Source Star Colors with the K2C9-CFHT Multi-color Microlensing Survey

Zang

Penny

Zhu

et al. 2018

PASP

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“…The 13 submitted papers based on these data are Hwang et al (2018), Shin et al (2017Shin et al ( , 2018, Mróz et al (2017), Han et al (2017b,a), Ryu et al (2017Ryu et al ( , 2018, Jung et al (2017a,b), Calchi Novati et al (2016), Shvartzvald et al (2017), and Albrow et al (2018).…”

Section: Data Policymentioning

confidence: 99%

The KMTNet/K2-C9 (Kepler) Data Release

Hwang

Kim

Albrow

et al. 2018

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-We present Korea Microlensing Telescope Network (KMTNet) light curves for microlensing-event candidates for the 2016 season, which covers an area of 97 deg 2 observed at cadences ranging from Γ = 0.2 hr −1 to Γ = 8 hr −1 from three southern sites in Chile, South Africa, and Australia. These 2163 light curves are comprised of 1856 "clear microlensing" and 307 "possible microlensing" events (including 265 previously released from the K2 C9 field). The data policy is very similar to the one governing the 2015 release. The changes relative to 2015 in the algorithms to find and vet microlensing events are comprehensively described.

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“…However, this requires the host star to be relatively bright and the planet to be fairly massive. If the planetary perturbation in the microlensing light curve persists for a significant fraction ( 10%) of the orbital period, then it becomes possible to constrain the full orbit (Ryu et al 2018). If the planet imposes prominent features (i.e., caustic crossing) in the light curve, from which its locations at certain epochs can be precisely determined, then a much shorter perturbation can still provide meaningful constraints on the full orbit (Gaudi et al 2008;Bennett et al 2010).…”

Section: Introductionmentioning

confidence: 99%

A Pair of Planets Likely in Mean-motion Resonance From Gravitational Microlensing

Madsen

Zhu

2019

ApJL

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We combine statistical arguments and dynamical analysis to study the orbital configuration of the microlensing planetary system OGLE-2012-BLG-0026L. This system is known to host two massive planets, with both projected close to the Einstein ring at the time of the detection. Assuming an isotropic distribution for the orbital orientation, we find that the two planets should also be closely spaced in three-dimensional space and that the ratio of their orbital periods is almost certainly less than two. With N-body numerical integrations, we then identify two types of stable configurations: the two planets can be in first-order mean-motion resonances (MMRs) and have significant ( 0.1) eccentricities, or they stay out of MMRs and have nearly circular orbits. The latter is disfavored, given the absence of similar planet pairs in radial velocity (RV) observations as well as the theoretical difficulties in forming such a configuration. Therefore, the two massive planets in OGLE-2012-BLG-0026L are likely in a resonance configuration. Our work shows that the microlensing technique, which usually only measures the projected configurations, can also probe the detailed dynamical state of multi-planet systems. We also discuss theoretical implications of measuring the multiplicity and the orbital architecture of cold planets.

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OGLE-2016-BLG-1190Lb: The First Spitzer Bulge Planet Lies Near the Planet/Brown-dwarf Boundary

Cited by 61 publications

References 77 publications

Measurement of Source Star Colors with the K2C9-CFHT Multi-color Microlensing Survey

Measurement of Source Star Colors with the K2C9-CFHT Multi-color Microlensing Survey

The KMTNet/K2-C9 (Kepler) Data Release

A Pair of Planets Likely in Mean-motion Resonance From Gravitational Microlensing

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