A companion on the planet/brown dwarf mass boundary on a wide orbit discovered by gravitational microlensing

Poleski, R.; Udalski, A.; Bond, I. A.; Beaulieu, J. P.; Clanton, Christian; Gaudi, Scott; Szymański, M. K.; Soszyński, I.; Skowron, J.; Wyrzykowski, Ł.; Ulaczyk, K.; Bennett, D. P.; Sumi, T.; Suzuki, D.; Rattenbury, N. J.; Koshimoto, Naoki; Abe, F.; Asakura, Y.; Barry, Richard; Bhattacharya, Aparna; Donachie, M.; Evans, P.; Fukui, A.; Hirao, Yuki; Itow, Y.; Li, M. C. A.; Ling, C. H.; Masuda, K.; Matsubara, Y.; Muraki, Y.; Nagakane, M.; Ohnishi, Kouhei; Ranc, Clément; Saito, To.; Sharan, A.; Sullivan, D. J.; Tristram, P. J.; Yamada, Tōru; Yonehara, A.; Batista, V.; Marquette, J. B.

doi:10.1051/0004-6361/201730928

Cited by 15 publications

(14 citation statements)

References 61 publications

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“…Measurements of planet occurrence rates from microlensing also superficially appear to contradict previous radial velocity results, although a more careful analysis indicates that the microlensing and radial velocity results are consistent (Montet et al 2014;Clanton & Gaudi 2014a,b). Other notable microlensing discoveries include circumbinary planets (Bennett et al 2016), planets on orbits of ∼1-10 AU around components of moderately wide binary stars (e.g., Gould et al 2014b;Poleski et al 2014), planets on wide orbits comparable to Uranus and Neptune (e.g., Poleski et al 2017), and planets orbiting ultracool dwarfs (e.g. Shvartzvald et al 2017).…”

Section: Introductionmentioning

confidence: 99%

Predictions of the WFIRST Microlensing Survey. I. Bound Planet Detection Rates

Penny

Gaudi

Kerins

et al. 2019

ApJS

198

265

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The Wide Field InfraRed Survey Telescope (WFIRST) is the next NASA astrophysics flagship mission, to follow the James Webb Space Telescope (JWST). The WFIRST mission was chosen as the top-priority large space mission of the 2010 astronomy and astrophysics decadal survey in order to achieve three primary goals: to study dark energy via a wide-field imaging survey, to study exoplanets via a microlensing survey, and to enable a guest observer program. Here we assess the ability of the several WFIRST designs to achieve the goal of the microlensing survey to discover a large sample of cold, low-mass exoplanets with semimajor axes beyond roughly one AU, which are largely impossible to detect with any other technique. We present the results of a suite of simulations that span the full range of the proposed WFIRST architectures, from the original design envisioned by the decadal survey, to the current design, which utilizes a 2.4-m telescope donated to NASA. By studying such a broad range of architectures, we are able to determine the impact of design trades on the expected yields of detected exoplanets. In estimating the yields we take particular care to ensure that our assumed Galactic model predicts microlensing event rates that match observations, consider the impact that inaccuracies in the Galactic model might have on the yields, and ensure that numerical errors in lightcurve computations do not bias the yields for the smallest mass exoplanets. For the nominal baseline WFIRST design and a fiducial planet mass function, we predict that a total of ∼1400 bound exoplanets with mass greater than ∼0.1 M ⊕ should be detected, including ∼200 with mass 3 M ⊕ . WFIRST should have sensitivity to planets with mass down to ∼0.02 M ⊕ , or roughly the mass of Ganymede.

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Section: Introductionmentioning

confidence: 99%

Predictions of the WFIRST Microlensing Survey. I. Bound Planet Detection Rates

Penny

Gaudi

Kerins

et al. 2019

ApJS

198

265

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“…These are OGLE-2008-BLG-355 (Koshimoto et al 2014), MOA-2009-BLG-387 (Batista et al 2011) and MOA-2011-BLG-322Lb (Shvartzvald et al 2014. Another candidate super-Jupiter mass planet in the sample orbiting a low mass star is MOA-2012-BLG-006 (Poleski et al 2017), but a mass measurement for this event would be quite difficult, because of its bright giant source star. In addition to these events in the sample, the following events are candidates for super-Jupiter planets orbiting low-mass stars: MOA-2010-BLG-73, OGLE-2013-BLG-0102, OGLE-2013-BLG-1761, OGLE-2015-BLG-0954, MOA-2016-BLG-227, OGLE-2016-BLG-0263, KMT-2016-BLG-1397, and KMT-2017-BLG-1038(Street et al 2013Jung et al 2015;Hirao et al 2017;Shin et al 2016;Bennett et al 2017;Koshimoto et al 2017b;Zang et al 2018;Shin et al 2019).…”

Section: Introductionmentioning

confidence: 99%

Keck Observations Confirm a Super-Jupiter Planet Orbiting M Dwarf OGLE-2005-BLG-071L

Bennett

Bhattacharya

Beaulieu

et al. 2020

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We present adaptive optics imaging from the NIRC2 instrument on the Keck-2 telescope that resolves the exoplanet host (and lens) star as it separates from the brighter source star. These observations yield the K-band brightness of the lens and planetary host star, as well as the lens-source relative proper motion, µ rel,H . in the heliocentric reference frame. The µ rel,H measurement allows determination of the microlensing parallax vector, π E , which had only a single component determined by the microlensing light curve. The combined measurements of µ rel,H and K L provide the masses of the host stat, M host = 0.426 ± 0.037M , and planet, m p = 3.27 ± 0.32M Jupiter with a projected separation of 3.4 ± 0.5 AU. This confirms the tentative conclusion of a previous paper (Dong et al. 2009b) that this super-Jupiter mass planet, OGLE-2005-BLG-071Lb, arXiv:1909.04740v1 [astro-ph.EP] 10 Sep 2019 -2orbits an M-dwarf. Such planets are predicted to be rare by the core accretion theory and have been difficult to find with other methods, but there are two such planets with firm mass measurements from microlensing, and an additional 11 planetary microlens events with host mass estimates < 0.5M and planet mass estimates > 2 Jupiter masses that could be confirmed by high angular follow-up observations. We also point out that OGLE-2005-BLG-071L has separated far enough from its host star that it should be possible to measure the host star metalicity with spectra from a high angular resolution telescope such as Keck, the VLT, the Hubble Space Telescope or the James Webb Space Telescope.

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“…Otherwise, the HR labels indicate the current best estimates for mass and distances for these host stars. (124) [49,50], (220) [59,75], (132) [58,76], (026) [23,77], (293) [17,78], (319) [14,59], (400) [59,79], (192) [7,9], (169) [55,56,63], (071) [80,81], (235) [52,59,82], (227) [57], (605) [12], (950) [83], (563) [84], (006) [85], (310) [16,18], (368) [11], (387) [60], (349) [24], (109) [20,21].…”

Section: Resultsmentioning

confidence: 99%

Accurate Mass Measurements for Planetary Microlensing Events Using High Angular Resolution Observations

Beaulieu

2018

Universe

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The microlensing technique is a unique method to hunt for cold planets over a range of mass and separation, orbiting all varieties of host stars in the disk of our galaxy. It provides precise mass-ratio and projected separations in units of the Einstein ring radius. In order to obtain the physical parameters (mass, distance, orbital separation) of the system, it is necessary to combine the result of light curve modeling with lens mass-distance relations and/or perform a Bayesian analysis with a galactic model. A first mass-distance relation could be obtained from a constraint on the Einstein ring radius if the crossing time of the source over the caustic is measured. It could then be supplemented by secondary constraints such as parallax measurements, ideally by using coinciding ground and space-born observations. These are still subject to degeneracies, like the orbital motion of the lens. A third mass-distance relation can be obtained thanks to constraints on the lens luminosity using high angular resolution observations with 8 m class telescopes or the Hubble Space Telescope. The latter route, although quite inexpensive in telescope time is very effective. If we have to rely heavily on Bayesian analysis and limited constraints on mass-distance relations, the physical parameters are determined to 30-40% typically. In a handful of cases, ground-space parallax is a powerful route to get stronger constraint on masses. High angular resolution observations will be able to constrain the luminosity of the lenses in the majority of the cases, and in favorable circumstances it is possible to derive physical parameters to 10% or better. Moreover, these constraints will be obtained in most of the planets to be discovered by the Euclid and WFIRST satellites. We describe here the state-of-the-art approaches to measure lens masses and distances with an emphasis on high angular resolution observations. We will discuss the challenges, recent results and perspectives. Universe 2018, 4, 61 2 of 17 host stars. Over ∼90 planets have been discovered by microlensing over the past 13 years 1 , including cold super Earths [6-10] cold Neptunes [11-13], Saturns in the disk [14,15], planets in the Bulge [16-19], multiple planet systems [20-23], a circumbinary planet [24], brown dwarf desert objects [25,26] brown dwarfs orbiting M dwarfs [27] and a first exomoon candidate [28]. Surprisingly a M dwarf orbited by a super Earth has been serendipitously found towards the anti-galactic center with a source star at 800 pc ([29]). Exoplanets could also be discovered in the M31 galaxy and a first candidate has been reported by [30].Although the number of detected planets is relatively low compared to that discovered by the radial velocity and transit methods, microlensing probes a part of the parameter space (host separation vs. planet mass), which is mostly not accessible in the medium term to any other technique (Figure 1). Microlensing complements these detections because it is most sensitive to planets beyond the distance where water ice form...

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A companion on the planet/brown dwarf mass boundary on a wide orbit discovered by gravitational microlensing

Cited by 15 publications

References 61 publications

Predictions of the WFIRST Microlensing Survey. I. Bound Planet Detection Rates

Predictions of the WFIRST Microlensing Survey. I. Bound Planet Detection Rates

Keck Observations Confirm a Super-Jupiter Planet Orbiting M Dwarf OGLE-2005-BLG-071L

Accurate Mass Measurements for Planetary Microlensing Events Using High Angular Resolution Observations

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