2016AJ....152..140B

Query : 2016AJ....152..140B

2016AJ....152..140B - Astron. J., 152, 140-140 (2016/November-0)

Discovery of a gas giant planet in microlensing event OGLE-2014-BLG-1760.

BHATTACHARYA A., BENNETT D.P., BOND I.A., SUMI T., UDALSKI A., STREET R., TSAPRAS Y., ABE F., FREEMAN M., FUKUI A., HIRAO Y., ITOW Y., KOSHIMOTO N., LI M.C.A., LING C.H., MASUDA K., MATSUBARA Y., MURAKI Y., NAGAKANE M., OHNISHI K., RATTENBURY N., SAITO T., SHARAN A., SULLIVAN D.J., SUZUKI D., TRISTRAM P.J. (The MOA Collaboration), SKOWRON J., SZYMANSKI M.K., SOSZYNSKI I., POLESKI R., MROZ P., KOZLOWSKI S., PIETRUKOWICZ P., ULACZYK K., WYRZYKOWSKI L. (The OGLE Collaboration), BACHELET E., BRAMICH D.M., D'AGO G., DOMINIK M., FIGUERA JAIMES R., HORNE K., HUNDERTMARK M., KAINS N., MENZIES J., SCHMIDT R., SNODGRASS C., STEELE I.A., WAMBSGANSS J. (The RoboNet Collaboration)

Abstract (from CDS):

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 DL=6.9±1.1 kpc. It also indicates a host-star mass of M*=0.51–0.28+0.44M☉, a planet mass of mp=0.56–0.26+0.34MJ, and a projected star-planet separation of a⊥=1.75–0.33+0.34 au. The lens-source relative proper motion is µrel=6.5±1.1 mas yr–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.

Abstract Copyright: © 2016. The American Astronomical Society. All rights reserved.

Journal keyword(s): gravitational lensing: micro - planetary systems - planetary systems

CDS comments: Mispirnts: MOA 2011-BLG-353 = MOA 2010-BLG-353; EWS 2005-BLG-380 = EWS 2005-BLG-390.

Simbad objects: 10

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Number of rows : 10
N Identifier Otype ICRS (J2000)
RA 		ICRS (J2000)
DEC 		Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2026 		#notes
1 OGLE-2008-BLG-092 ** 17 47 29.4593818584 -34 43 35.461182180       15.48   ~ 43 0
2 MOA 2008-BLG-310 * 17 54 14.53 -34 46 41.0           GV 51 1
3 OGLE-2005-BLG-390 * 17 54 19.2 -30 22 38           KIII 54 1
4 MOA 2011-BLG-293 * 17 55 39.350 -28 28 36.65           ~ 30 1
5 MOA 2014-BLG-547b Pl 17 57 38.160 -28 57 47.37           ~ 5 0
6 MOA 2014-BLG-547 * 17 57 38.160 -28 57 47.37           ~ 6 0
7 MOA 2008-BLG-288 * 17 59 08.81 -30 45 34.1           ~ 14 0
8 NAME Baade Window reg 18 03.5 -30 01           ~ 643 3
9 MOA 2010-BLG-353 * 18 05 12.940 -27 17 35.64           ~ 12 0
10 NAME Galactic Bulge reg ~ ~           ~ 4794 0

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