2019AJ....158...28J

Query : 2019AJ....158...28J

2019AJ....158...28J - Astron. J., 158, 28-28 (2019/July-0)

Spitzer parallax of OGLE-2018-BLG-0596: a low-mass-ratio planet around an M dwarf.

JUNG Y.K., GOULD A., UDALSKI A., SUMI T., YEE J.C., SHVARTZVALD Y., ZANG W., HAN C., ALBROW M.D., CHUNG S.-J., HWANG K.-H., RYU Y.-H., SHIN I.-G., ZHU W., CHA S.-M., KIM D.-J., KIM H.-W., KIM S.-L., LEE C.-U., LEE D.-J., LEE Y., PARK B.-G., POGGE R.W. (The KMTNet Collaboration), MROZ P., SZYMANSKI M.K., SKOWRON J., POLESKI R., SOSZYNSKI I., PIETRUKOWICZ P., KOZLOWSKI S., ULACZYK K., RYBICKI K.A., IWANEK P., WRONA M. (The OGLE Collaboration), BEICHMAN C.A., BRYDEN G., CALCHI NOVATI S., CAREY S., GAUDI B.S., HENDERSON C.B. (The Spitzer Team), ABE F., BARRY R., BENNETT D.P., BOND I.A., BHATTACHARYA A., DONACHIE M., FUKUI A., HIRAO Y., ITOW Y., KONDO I., KOSHIMOTO N., LI M.C.A., MATSUBARA Y., MIYAZAKI S., MURAKI Y., NAGAKANE M., RANC C., RATTENBURY N.J., SUEMATSU H., SULLIVAN D.J., SUZUKI D., TRISTRAM P.J., YONEHARA A. (The MOA Collaboration), JACKLIN S., PENNY M.T., STASSUN K.G. (The UKIRT Microlensing Team), FOUQUE P., MAO S., WANG T. (The CFHT Microlensing Collaboration)

Abstract (from CDS):

We report the discovery of a Spitzer microlensing planet OGLE-2018-BLG-0596Lb, with preferred planet-host mass ratio q ∼ 2 x 10–4. The planetary signal, which is characterized by a short (∼1 day) "bump" on the rising side of the lensing light curve, was densely covered by ground-based surveys. We find that the signal can be explained by a bright source that fully envelops the planetary caustic, i.e., a "Hollywood" geometry. Combined with the source proper motion measured from Gaia, the Spitzer satellite parallax measurement makes it possible to precisely constrain the lens physical parameters. The preferred solution, in which the planet perturbs the minor image due to lensing by the host, yields a Uranus-mass planet with a mass of Mp = 13.9 ± 1.6 M⊕ orbiting a mid M-dwarf with a mass of Mh = 0.23 ± 0.03 M☉. There is also a second possible solution that is substantially disfavored but cannot be ruled out, for which the planet perturbs the major image. The latter solution yields Mp = 1.2 ± 0.2 M⊕ and Mh = 0.15 ± 0.02 M☉. By combining the microlensing and Gaia data together with a Galactic model, we find in either case that the lens lies on the near side of the Galactic bulge at a distance DL ∼ 6 ± 1 kpc. Future adaptive optics observations may decisively resolve the major image/minor image degeneracy.

Abstract Copyright: © 2019. The American Astronomical Society. All rights reserved.

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

Simbad objects: 5

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Number of rows : 5
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-2005-SMC-001 BD? 00 40 28.50 -73 44 46.1           ~ 21 0
2 MOA 2018-BLG-145 * 17 56 13.3348253400 -29 11 56.615704692           ~ 8 0
3 MOA 2018-BLG-145b Pl 17 56 13.3348253400 -29 11 56.615704692           ~ 7 0
4 MOA 2016-BLG-383 * 17 58 52.30 -27 36 48.8           ~ 14 0
5 NAME Galactic Bulge reg ~ ~           ~ 4794 0

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