DISCOVERY OF A GAS GIANT PLANET IN MICROLENSING EVENT OGLE-2014-BLG-1760

Journal Article · Tue Nov 01 04:00:00 EDT 2016 · The Astronomical Journal (Online)

DOI:https://doi.org/10.3847/0004-6256/152/5/140· OSTI ID:22862846

Bhattacharya, A.; Bennett, D. P. ^[1]; Bond, I. A.; Ling, C. H. ^[2]; Sumi, T.; Hirao, Y.; Koshimoto, N.; Nagakane, M. ^[3]; Udalski, A. ^[4]; Street, R.; Tsapras, Y. ^[5]; Abe, F.; Itow, Y.; Masuda, K.; Matsubara, Y.; Muraki, Y. ^[6]; Freeman, M.; Li, M. C. A. ^[7]; Fukui, A. ^[8]; others, and

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1. Department of Physics, University of Notre Dame, 225 Nieuwland Science Hall, Notre Dame, IN 46556 (United States)
2. Institute of Natural and Mathematical Sciences, Massey University, Auckland 0745 (New Zealand)
3. Osaka University, 1-1 Yamadaoka, Suita, Osaka Prefecture 565-0871 (Japan)
4. Warsaw University Observatory, Al. Ujazdowskie 4, 00-478 Warszawa (Poland)
5. Las Cumbres Observatory Global Telescope Network, 6740 Cortona Drive, Suite 102, Goleta, CA 93117 (United States)
6. Institute for Space-Earth Environmental Research, Nagoya University, 464-8601 Nagoya (Japan)
7. Department of Physics, University of Auckland, Private Bag 92019, Auckland (New Zealand)
8. Okayama Astrophysical Observatory, National Astronomical Observatory of Japan, Asakuchi, 719-0232 Okayama (Japan)

We present the analysis of the planetary microlensing event OGLE-2014-BLG-1760, which shows a strong light-curve signal due to the presence of a Jupiter mass ratio planet. One unusual feature of this event is that the source star is quite blue, with V-I=1.48±0.08. This is marginally consistent with a source star in the Galactic bulge, but it could possibly indicate a young source star on the far side of the disk. Assuming a bulge source, we perform a Bayesian analysis assuming a standard Galactic model, and this indicates that the planetary system resides in or near the Galactic bulge at D{sub L}=6.9±1.1 kpc. It also indicates a host-star mass of M{sub ·}=0.51{sub -0.28}{sup +0.44}M{sub ⊙}, a planet mass of m{sub p}=0.56{sub -0.26}{sup +0.34}M{sub J}, and a projected star–planet separation of a{sub ⊥}=1.75{sub -0.33}{sup +0.34} au. The lens–source relative proper motion is μ{sub rel}=6.5±1.1 mas yr{sup -1}. The lens (and stellar host star) is estimated to be very faint compared to the source star, so it is most likely that it can be detected only when the lens and source stars start to separate. Due to the relatively high relative proper motion, the lens and source will be resolved to about ~46 mas in 6–8 yr after the peak magnification. So, by 2020–2022, we can hope to detect the lens star with deep, high-resolution images.

• OSTI ID: 22862846
• Journal Information: The Astronomical Journal (Online), Journal Name: The Astronomical Journal (Online) Journal Issue: 5 Vol. 152; ISSN 1538-3881
• Country of Publication: United States
• Language: English

Related Subjects

79 ASTRONOMY AND ASTROPHYSICS
GALAXIES
GRAVITATIONAL LENSES
PLANETS
PROPER MOTION
RESOLUTION
STARS
VISIBLE RADIATION