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

Bhattacharya, Aparna; Bennett, D. P.; Bond, I. A.; Sumi, T.; Udalski, A.; Street, R. A.; Tsapras, Y.; Abe, F.; Freeman, Matthew; Fukui, A.; Hirao, Yuki; Itow, Y.; Koshimoto, Naoki; Li, M. C. A.; Ling, C. H.; Masuda, K.; Matsubara, Y.; Muraki, Y.; Nagakane, M.; Ohnishi, Kouhei; Rattenbury, N. J.; Saito, To.; Sharan, A.; Sullivan, D. J.; Suzuki, D.; Tristram, P. J.; Skowron, J.; Szymański, M. K.; Soszyński, I.; Poleski, R.; Mróz, P.; Kozłowski, S.; Pietrukowicz, P.; Ulaczyk, K.; Wyrzykowski, Ł.; Bachelet, E.; Bramich, D. M.; D’Ago, G.; Dominik, M.; Jaimes, R. Figuera; Horne, K.; Hundertmark, M.; Kains, N.; Menzies, John; Schmidt, R. W.; Snodgrass, C.; Steele, I. A.; Wambsganß, J.

doi:10.3847/0004-6256/152/5/140

Cited by 30 publications

(7 citation statements)

References 61 publications

(85 reference statements)

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“…Penny et al (2016) suggested thepossibility of alack of planets in the Galactic bulge. OGLE-2013-BLG-1761Lb can be added to the growing list of planets discovered by microlensing, such as OGLE-2015-BLG-0051Lb (Han et al 2016a), OGLE-2014-BLG-1760Lb (Bhattacharya et al 2016), and OGLE-2012-BLG-0724Lb (Hirao et al 2016b), which counters this suggestion. This work contributes to thesample of planets found by microlensing, which is useful for testing planetary formation theories and the planet distribution in the Galaxy.…”

Section: Discussionmentioning

confidence: 94%

OGLE-2013-BLG-1761Lb: A Massive Planet around an M/K Dwarf

Hirao

Udalski

Sumi

et al. 2017

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We report the discovery and the analysis of the planetary microlensing event, OGLE-2013-BLG-1761. There are some degenerate solutions in this event because the planetary anomaly is only sparsely sampled. However,the detailed lightcurve analysis ruled out all stellar binary models and shows the lens to be a planetary system. There is the so-called close/wide degeneracy in the solutions with the planet/host mass ratio of q∼(7.0±2.0)×10 −3 and q∼(8.1±2.6)×10−3 with the projected separation in Einstein radius units of s=0.95 (close) and s=1.18 (wide), respectively. The microlens parallax effect is not detected, but the finite source effect is detected. Our Bayesian analysis indicates that the lens system is located = . The preference of the large lens distance in the Bayesian analysis is due to the relatively large observed source star radius. The distance and other physical parameters may be constrained by the future high-resolution imaging by large groundtelescopes orHST. If the estimated lens distance is correct, thenthis planet provides another sample for testing the claimed deficit of planets in the Galactic bulge.-

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Section: Discussionmentioning

confidence: 94%

OGLE-2013-BLG-1761Lb: A Massive Planet around an M/K Dwarf

Hirao

Udalski

Sumi

et al. 2017

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“…However, the value of the lens-source proper motion, 6.0±1.2 mas yr −1 , does not rule out a scenario with a lens and source lying in the Galactic bulge (Koz lowski et al 2006). If it is confirmed that the new exoplanetary system OGLE-2015-BLG-1670L lies in the Galactic bulge, then it will be one more object in the growing list of planets orbiting stars in the bulge, similar to MOA-2011-BLG-293Lb (Yee et al 2012;Batista et al 2014), OGLE-2015-BLG-0051Lb (Han et al 2016), OGLE-2014-BLG-1760Lb (Bhattacharya et al 2016), OGLE-2012-BLG-0724Lb (Hirao et al 2016), and OGLE-2013-BLG-1761Lb (Hirao et al 2017). In the future, it will be possible to use this sample to assess the planet demography close to the Galactic center and test whether or not there is a lack of planets in the Galactic bulge (Penny et al 2016).…”

Section: Summary and Discussionmentioning

confidence: 99%

OGLE-2015-BLG-1670Lb: A Cold Neptune beyond the Snow Line in the Provisional WFIRST Microlensing Survey Field

Ranc¹,

Bennett²,

Hirao³

et al. 2019

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We present the analysis of the microlensing event OGLE-2015-BLG-1670, detected in a high-extinction field, very close to the Galactic plane. Due to the dust extinction along the line of sight, this event was too faint to be detected before it reached the peak of magnification. The microlensing light-curve models indicate a high-magnification event with a maximum of A max 200, very sensitive to planetary deviations. An anomaly in the light curve has been densely observed by the microlensing surveys MOA, KMTNet, and OGLE. From the light-curve modeling, we find a planetary anomaly characterized by a planet-to-host mass ratio, q = 1.00 +0.18 −0.16 × 10 −4 , at the peak recently identified in the mass-ratio function of microlensing planets. Thus, this event is interesting to include in future statistical studies about planet demography. We have explored the possible degeneracies and find two competing planetary models resulting from the s ↔ 1/s degeneracy. However, because the projected separation is very close to s = 1, the physical implications for the planet for the two solutions are quite similar, except for the value of s. By combining the light-curve parameters with a Galactic model, we have estimated the planet mass M 2 = 17.9 +9.6 −8.8 M ⊕ and the lens distance D L = 6.7 +1.0 −1.3 kpc, corresponding to a Neptune-mass planet close to the Galactic bulge. Such events with a low absolute latitude (|b| ≈ 1.1 deg) are subject to both high extinction and more uncertain source distances, two factors that may affect the mass measurements in the provisional Wide Field Infrared Survey Telescope fields. More events are needed to investigate the potential trade-off between the higher lensing rate and the difficulty in measuring masses in these low-latitude fields.

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“…There are several ingredients to this improvement. The improved MOA and CTIO photometry provides more accurate t E and color values, and the analysis of Boyajian et al (2014), as optimized for microlensing targets (Bhattacharya et al 2016), provides a more accurate source radius. Finally, Nataf et al (2013) has provided a more accurate determination of the properties of the red clump giants that are used to determine the dust extinction in the foreground of the source.…”

Section: Revisiting Photometry and Light-curve Modelingmentioning

confidence: 99%

“…which comes from the Boyajian et al (2014) analysis, but with the color range optimized for the needs of microlensing surveys (Bhattacharya et al 2016).…”

Section: Lens Propertiesmentioning

confidence: 99%

MOA-2007-BLG-400 A Super-Jupiter-mass Planet Orbiting a Galactic Bulge K-dwarf Revealed by Keck Adaptive Optics Imaging

Bhattacharya

Bennett

Beaulieu

et al. 2021

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We present Keck/NIRC2 adaptive optics imaging of planetary microlensing event MOA-2007-BLG-400 that resolves the lens star system from the source. We find that the MOA-2007-BLG-400L planetary system consists of a 1.71 ± 0.27M Jup planet orbiting a 0.69 ± 0.04M e K-dwarf host star at a distance of 6.89 ± 0.77 kpc from the Sun. So, this planetary system probably resides in the Galactic bulge. The planet-host star projected separation is only weakly constrained due to the close-wide light-curve degeneracy; the 2σ projected separation ranges are 0.6-1.0 au and 4.7-7.7 au for close and wide solutions, respectively. This host mass is at the top end of the range of masses predicted by a standard Bayesian analysis. Our Keck follow-up program has now measured lens-source separations for six planetary microlensing events, and five of these six events have host star masses above the median prediction under the assumption that assumes that all stars have an equal chance of hosting planets detectable by microlensing. This suggests that more massive stars may be more likely to host planets of a fixed mass ratio that orbit near or beyond the snow line. These results also indicate the importance of host star mass measurements for exoplanets found by microlensing. The microlensing survey imaging data from NASA's Nancy Grace Roman Space Telescope (formerly WFIRST) mission will be doing mass measurements like this for a huge number of planetary events.

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

Cited by 30 publications

References 61 publications

OGLE-2013-BLG-1761Lb: A Massive Planet around an M/K Dwarf

OGLE-2013-BLG-1761Lb: A Massive Planet around an M/K Dwarf

OGLE-2015-BLG-1670Lb: A Cold Neptune beyond the Snow Line in the Provisional WFIRST Microlensing Survey Field

MOA-2007-BLG-400 A Super-Jupiter-mass Planet Orbiting a Galactic Bulge K-dwarf Revealed by Keck Adaptive Optics Imaging

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