OGLE-2016-BLG-1266: A Probable Brown Dwarf/Planet Binary at the Deuterium Fusion Limit

Albrow, M. D.; Yee, Jennifer C.; Udalski, A.; Novati, S. Calchi; Carey, Sean; Henderson, Calen B.; Beichman, Charles; Bryden, G.; Gaudi, B. Scott; Shvartzvald, Yossi; Team, Spitzer; Szymański, M. K.; Mróz, P.; Skowron, J.; Poleski, R.; Soszyński, I.; Kozłowski, S.; Pietrukowicz, P.; Ulaczyk, K.; Pawlak, M.; Chung, Sun-Ju; Gould, Andrew; Han, Cheongho; Hwang, Kyu-Ha; Jung, Y. K.; Ryu, Yoon-Hyun; Shin, In-Gu; Zhu, Wei; M., S.; Kim, D. J.; Kim, H. W.; Kim, S. L.; Lee, C. U.; Lee, D. J.; Lee, Y.; Park, B. G.; Pogge, Richard W.

doi:10.3847/1538-4357/aabf3f

Cited by 12 publications

(9 citation statements)

References 70 publications

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“…PID 10036, 11006, 12013, 12015, 13005, 14012, PI: S. Dong; PID: 13250, PI: S. Carey; PID 14121). Following the successful 2014 pilot program, Spitzer took on a new role as a 'microlens parallax satellite' with the primary objective of measuring the Galactic distribution of exoplanets towards the bulge (Calchi Novati et al 2015a,b, 2018Shvartzvald et al 2015Shvartzvald et al , 2016Shvartzvald et al , 2017Shvartzvald et al , 2019Udalski et al 2015bUdalski et al , 2018Yee et al 2015a,b;Zhu et al 2015aZhu et al ,b, 2016Zhu et al , 2017bBozza et al 2016;Han et al 2016Han et al , 2017Han et al , 2018Poleski et al 2016;Street et al 2016;Chung et al 2017Chung et al , 2019Shin et al 2017Shin et al , 2018Albrow et al 2018;Ryu et al 2018;Wang et al 2018;Jung et al 2019;Li et al 2019;Shan et al 2019;Zang et al 2019Zang et al , 2020Gould et al 2020;Hirao et al 2020).…”

Section: Introductionmentioning

confidence: 99%

Pixel level decorrelation in service of the Spitzer microlens parallax survey

Dang

Novati

Carey

et al. 2020

Monthly Notices of the Royal Astronomical Society

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Microlens parallax measurements combining space-based and ground-based observatories can be used to study planetary demographics. In recent years, the Spitzer Space Telescope was used as a microlens parallax satellite. Meanwhile, Spitzer IRAC has been employed to study short-period exoplanets and their atmospheres. As these investigations require exquisite photometry, they motivated the development of numerous self-calibration techniques now widely used in the exoplanet atmosphere community. Specifically, Pixel Level Decorrelation (PLD) was developed for starring-mode observations in uncrowded fields. We adapt and extend PLD to make it suitable for observations obtained as part of the Spitzer Microlens Parallax Campaign. We apply our method to two previously published microlensing events, OGLE-2017-BLG-1140 and OGLE-2015-BLG-0448, and compare its performance to the state-of-the-art pipeline used to analyses Spitzer microlensing observation. We find that our method yields photometry 1.5–6 times as precise as previously published. In addition to being useful for Spitzer, a similar approach could improve microlensing photometry with the Nancy Grace Roman Space Telescope.

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Section: Introductionmentioning

confidence: 99%

Pixel level decorrelation in service of the Spitzer microlens parallax survey

Dang

Novati

Carey

et al. 2020

Monthly Notices of the Royal Astronomical Society

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“…Therefore more and more accurate mass measurements of such systems are required. The microlensing method is a powerful way to detect these systems and some of such events have been discovered by the microlensing method (Han et al 2013;Jung et al 2018a,b;Albrow et al 2018). Figure 13 shows the mass distribution of discovered systems with a brown dwarf/a late M-dwarf hosting a gas giant (0.01 M ⊙ < M h < 0.3 M ⊙ , 0.01 M Jup < M p < 13.6 M Jup ).…”

Section: Discussion and Summarymentioning

confidence: 99%

“…The mass probability distribution of low-mass host stars (M h < 0.1 M ⊙ ) depends strongly on the shape of the mass function which has large uncertainty. In Albrow et al (2018), the lens parameters are directly derived by combining measurements from Earth and from the Spitzer telescope . The increase in number of the mass measurements by the space parallax effect and high resolution images are greatly anticipated by W F IRST satellite in the near future, and would contribute significantly to clarification of the formation theory of a gas giant around a low-mass star.…”

Section: Discussion and Summarymentioning

confidence: 99%

MOA-bin-29b: A Microlensing Gas-giant Planet Orbiting a Low-mass Host Star

Kondo

Sumi

Bennett

et al. 2019

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We report the discovery of a gas giant planet orbiting a low-mass host star in the microlensing event MOA-bin-29 that occurred in 2006. We find five degenerate solutions with the planet/host-star mass ratio of q ∼ 10 −2 . The Einstein radius crossing time of all models are relatively short (∼ 4 − 7 days), which indicates that the mass of host star is likely low. The measured lens-source proper motion is 5 − 9 mas yr −1 depending on the models. Since only finite source effects are detected, we conduct a Bayesian analysis in order to obtain the posterior probability distribution of the lens physical properties. As a result, we find the lens system is likely to be a gas giant orbiting a brown dwarf

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“…40 The CFHT Mircolensing Collaboration. populations, including binary brown dwarfs (Albrow et al 2018), single-mass objects (Zhu et al 2016;Chung et al 2017;Shin et al 2018;Shvartzvald et al 2019), and planetary systems Street et al 2016;Shvartzvald et al 2017b;Calchi Novati et al 2018Ryu et al 2018).…”

Section: Introductionmentioning

confidence: 99%

Spitzer Parallax of OGLE-2018-BLG-0596: A Low-mass-ratio Planet around an M Dwarf

Jung

Gould

Udalski

et al. 2019

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We report the discovery of a Spitzer microlensing planet OGLE-2018-BLG-0596Lb, with preferred planet-host mass ratio q∼2×10 −4 . The planetary signal, which is characterized by a short (∼1 day) "bump" on the rising side of the lensing light curve, was densely covered by ground-based surveys. We find that the signal can be explained by a bright source that fully envelops the planetary caustic, i.e., a "Hollywood" geometry. Combined with the source proper motion measured from Gaia, the Spitzer satellite parallax measurement makes it possible to precisely constrain the lens physical parameters. The preferred solution, in which the planet perturbs the minor image due to lensing by the host, yields a Uranus-mass planet with a mass of M p =13.9±1.6M ⊕ orbiting a mid M-dwarf with a mass of M h =0.23±0.03M e . There is also a second possible solution that is substantially disfavored but cannot be ruled out, for which the planet perturbs the major image. The latter solution yields M p =1.2±0.2M ⊕ and M h =0.15±0.02M e . By combining the microlensing and Gaia data together with a Galactic model, we find in either case that the lens lies on the near side of the Galactic bulge at a distance D L ∼6±1 kpc. Future adaptive optics observations may decisively resolve the major image/minor image degeneracy.

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OGLE-2016-BLG-1266: A Probable Brown Dwarf/Planet Binary at the Deuterium Fusion Limit

Cited by 12 publications

References 70 publications

Pixel level decorrelation in service of the Spitzer microlens parallax survey

Pixel level decorrelation in service of the Spitzer microlens parallax survey

MOA-bin-29b: A Microlensing Gas-giant Planet Orbiting a Low-mass Host Star

Spitzer Parallax of OGLE-2018-BLG-0596: A Low-mass-ratio Planet around an M Dwarf

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