Systematic KMTNet Planetary Anomaly Search. II. Six New q &lt; 2 × 10<sup>−4</sup> Mass-ratio Planets

Hwang, Kyu-Ha; Zang, Weicheng; Gould, Andrew; Udalski, A.; Bond, I. A.; Yang, Hongjing; Mao, Shude; Albrow, M. D.; Chung, Sun-Ju; Han, Cheongho; Jung, Youn Kil; Ryu, Yoon-Hyun; Shin, In-Gu; Shvartzvald, Yossi; Yee, Jennifer C.; Cha, Sang-Mok; Kim, Dong-Jin; Kim, Hyoun-Woo; Kim, S.-L.; Lee, Chung-Uk; Lee, Dong-Joo; Lee, Yongseok; Park, Byeong-Gon; Pogge, Richard W.; Mróz, P.; Poleski, R.; Skowron, J.; Szymański, M. K.; Soszyński, I.; Pietrukowicz, P.; Kozłowski, S.; Ulaczyk, K.; Rybicki, K.; Iwanek, P.; Wrona, Marcin; Gromadzki, M.; Abe, F.; Barry, Richard; Bennett, D. P.; Bhattacharya, Aparna; Hirosame, Fujii,; Fukui, A.; Hirao, Yuki; Itow, Y.; Kirikawa, Rintaro; Kondo, Iona; Koshimoto, Naoki; Munford, Brandon; Matsubara, Y.; Miyazaki, Shota; Muraki, Y.; Olmschenk, Greg; Ranc, Clément; Rattenbury, N. J.; Satoh, Yuki; Shoji, Hikaru; Silva, Stela Ishitani; Sumi, T.; Suzuki, D.; Tristram, P. J.; Yonehara, A.; Zhang, Xiangyu; Zhu, Wei; Penny, Matthew T.; Fouqué, P.

doi:10.3847/1538-3881/ac38ad

Cited by 37 publications

(52 citation statements)

References 68 publications

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“…We find that the light curve of OGLE-2016-BLG-1093 is qualitatively similar to that of KMT-2019-BLG-0842Lb (Jung et al 2020) or OGLE-2019-BLG-0960Lb (Yee et al 2021), both of which have much smaller mass ratios (q < 10 −4 ) than our best-fit solution. Following the formalism of Hwang et al (2022)…”

Section: Ground-based Light-curve Analysismentioning

confidence: 99%

Scaling K2. V. Statistical Validation of 60 New Exoplanets From K2 Campaigns 2–18

Christiansen¹,

Bhure²,

Zink³

et al. 2022

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The NASA K2 mission, salvaged from the hardware failures of the Kepler telescope, has continued Kepler’s planet-hunting success. It has revealed nearly 500 transiting planets around the ecliptic plane, many of which are the subject of further study, and over 1000 additional candidates. Here we present the results of an ongoing project to follow-up and statistically validate new K2 planets, in particular to identify promising new targets for further characterization. By analyzing the reconnaissance spectra, high-resolution imaging, centroid variations, and statistical likelihood of the signals of 91 candidates, we validate 60 new planets in 46 systems. These include a number of planets amenable to transmission spectroscopy (K2-384 f, K2-387 b, K2-390 b, K2-403 b, and K2-398 c), emission spectroscopy (K2-371 b, K2-370 b, and K2-399 b), and both (K2-405 b and K2-406 b); several systems with planets in or close to mean motion resonances (K2-381 and K2-398) including a compact, TRAPPIST-1-like system of five small planets orbiting a mid-M dwarf (K2-384); an ultra-short-period sub-Saturn in the hot Saturn desert (K2-399 b); and a super-Earth orbiting a moderately bright (V = 11.93), metal-poor ([Fe/H] = −0.579 ± 0.080) host star (K2-408 b). In total we validate planets around four F stars, 26 G stars, 13 K stars, and three M dwarfs. In addition, we provide a list of 37 vetted planet candidates that should be prioritized for future follow-up observation in order to be confirmed or validated.

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Section: Ground-based Light-curve Analysismentioning

confidence: 99%

Scaling K2. V. Statistical Validation of 60 New Exoplanets From K2 Campaigns 2–18

Christiansen¹,

Bhure²,

Zink³

et al. 2022

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“…In Figure 7, we plot the cumulative distributions of log q for this sample and the 23-planet sample from the MOA-II survey (Suzuki et al 2016). Hwang et al (2022) found a roughly uniform log q distribution over the range −5.0 < log q < −3.7 using the 11 planets from 2018-2019 KMTNet prime fields, and our sample extends the uniform feature to log q ∼ −1.5. Compared with the MOA-II sample, our sample has a higher rate of detections (4/14) below the apparent break in the mass-ratio function of the MOA-II sample, q break = 1.7 × 10 −4 (Suzuki et al 2016).…”

Section: Blended Light and Future High-resolution Observationsmentioning

confidence: 81%

“…The operator identified 9 "planet", 8 "planet/binary", 15 "binary/planet", 83 "binary", and 7 "finite source". Among them, six are known planets (four were previously published, one is in preparation, and KMT-2019-BLG-1552 is analyzed in this paper), seven are planets found by the AnomalyFinder (four were already published by Zang et al (2021); Hwang et al (2022), and three are in preparation). For the remaining events, the operator checked whether the OGLE and/or MOA data points are inconsistent with the KMTNet-based anomalies, cross-checked with C. Han's modeling, and fitted the candidate planetary events to binary-lens single-source (2L1S) model using the online data.…”

Section: Anomalyfinder Results For the 2019-prime Fields And Protocolsmentioning

confidence: 99%

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Systematic KMTNet Planetary Anomaly Search. IV. Complete Statistical Sample of 2019 Prime-Field Microlensing Planets

Zang¹,

Yang²,

Han³

et al. 2022

Preprint

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We report the complete statistical planetary sample from the prime fields (Γ ≥ 2 hr −1 ) of the 2019 Korea Microlensing Telescope Network (KMTNet) microlensing survey. We develop the optimized KMTNet Anoma-lyFinder algorithm and apply it to the 2019 KMTNet prime fields. We find a total of 14 homogeneously selected planets and report the analysis of three planetary events, KMT-2019-BLG-(1042,1552,2974. The planet-host mass ratios, q, for the three planetary events are 6.34 × 10 −4 , 4.89 × 10 −3 and 6.18 × 10 −4 , respectively. A Bayesian analysis indicates the three planets are all cold giant planets beyond the snow line of their host stars. The 14 planets are basically uniform in log q over the range −5.0 < log q < −1.5. This result suggests that the planets below q break = 1.7 × 10 −4 proposed by the MOA-II survey may be more common than previously believed. This work is an early component of a large project to determine the KMTNet mass-ratio function, and the whole sample of 2016-2019 KMTNet events should contain about 120 planets.

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“…Microlensing remains the principal method for detecting cool, lowmass exoplanets, including planets beyond the snow-line (Hwang et al 2022;Gaudi 2012); a demographic of particular importance for verifying theories of planetary formation.…”

Section: Introductionmentioning

confidence: 99%

Kepler K2 Campaign 9: II. First space-based discovery of an exoplanet using microlensing

Specht¹,

Poleski²,

Penny³

et al. 2022

Preprint

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We report on the discovery of a bound exoplanetary microlensing event from a blind search of data gathered from Campaign 9 of the Kepler K2 mission (K2C9). K2-2016-BLG-0005Lb is a densely sampled, binary caustic-crossing microlensing event with caustic entry and exit points that are resolved in the K2C9 data, enabling the lens-source relative proper motion to be measured. We have fitted a binary microlens model to the K2 dataset, and to simultaneous observations from the Optical Gravitational Lensing Experiment (OGLE-IV), Canada-France-Hawaii Telescope (CFHT), Microlensing Observations in Astrophysics (MOA-2), the Korean Microlensing Telescope Network (KMTNet), and the United Kingdom InfraRed Telescope (UKIRT). Whilst the groundbased data only sparsely sample the binary caustic, they provide a clear detection of parallax that allows us to break completely the microlensing mass-position-velocity degeneracy and measure the planet's mass directly. We find a host mass of 0.58 ± 0.03 M and a planetary mass of 1.1 ± 0.1 M J . The system lies at a distance of 5.2 ± 0.2 kpc from Earth towards the Galactic bulge. The projected physical separation of the planet from its host is found to be 4.2 ± 0.3 au which, for circular orbits, corresponds to 𝑎 = 4.4 +1.9 −0.4 au and period 𝑃 = 13 +9 −2 yr, making K2-2016-BLG-0005Lb a close Jupiter analogue. Though previous exoplanet microlensing events have included space-based data, this event is the first bound microlensing exoplanet to be discovered from space-based data. Even through a space telescope not designed for microlensing studies, this result highlights the advantages for exoplanet microlensing discovery that come from continuous, high-cadence temporal sampling that is possible from space. The precision mass and distance measurements of cool low-mass exoplanets from microlensing that will be obtainable from the NASA Nancy Grace Roman Space Telescope and, potentially, the ESA Euclid space telescope, will unlock a key regime for testing planet formation theories.

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Systematic KMTNet Planetary Anomaly Search. II. Six New q < 2 × 10⁻⁴ Mass-ratio Planets

Cited by 37 publications

References 68 publications

Scaling K2. V. Statistical Validation of 60 New Exoplanets From K2 Campaigns 2–18

Scaling K2. V. Statistical Validation of 60 New Exoplanets From K2 Campaigns 2–18

Systematic KMTNet Planetary Anomaly Search. IV. Complete Statistical Sample of 2019 Prime-Field Microlensing Planets

Kepler K2 Campaign 9: II. First space-based discovery of an exoplanet using microlensing

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Systematic KMTNet Planetary Anomaly Search. II. Six New q < 2 × 10−4 Mass-ratio Planets

Cited by 37 publications

References 68 publications

Scaling K2. V. Statistical Validation of 60 New Exoplanets From K2 Campaigns 2–18

Scaling K2. V. Statistical Validation of 60 New Exoplanets From K2 Campaigns 2–18

Systematic KMTNet Planetary Anomaly Search. IV. Complete Statistical Sample of 2019 Prime-Field Microlensing Planets

Kepler K2 Campaign 9: II. First space-based discovery of an exoplanet using microlensing

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Systematic KMTNet Planetary Anomaly Search. II. Six New q < 2 × 10⁻⁴ Mass-ratio Planets