Ryu, Y-H and Yee, JC and Udalski, A and Bond, IA and Shvartzvald, Y and Zang, W and Jaimes, RF and Jørgensen, UG and Zhu, W and Huang, CX and Jung, YK and Albrow, MD and Chung, S-J and Gould, A and Han, C and Hwang, K-H and Shin, I-G and Cha, S-M and Kim, D-J and Kim, H-W and Kim, S-L and Lee, C-U and Lee, D-J and Lee, Y and Park, B-G and Pogge, RW and Collaboration, K and Novati, SC and Carey, S and Henderson, CB and Beichman, C and Gaudi, BS and team, S and Mróz, P and Poleski, R and Skowron, J and Szymański, MK and Soszyński, I and Kozłowski, S and Pietrukowicz, P and Ulaczyk, K and Pawlak, M and Collaboration, OGLE and Abe, F and Asakura, Y and Barry, R and Bennett, DP and Bhattacharya, A and Donachie, M and Evans, P and Fukui, A and Hirao, Y and Itow, Y and Kawasaki, K and Koshimoto, N and Li, MCA and Ling, CH and Masuda, K and Matsubara, Y and Miyazaki, S and Muraki, Y and Nagakane, M and Ohnishi, K and Ranc, C and Rattenbury, NJ and Saito, T and Sharan, A and Sullivan, DJ and Sumi, T and Suzuki, D and Tristram, PJ and Yamada, T and Yamada, T and Yonehara, A and Collaboration, MOA and Bryden, G and Howell, SB and Jacklin, S and Team, UKIRTM and Penny, MT and Mao, S and Fouqué, P and Wang, T and group, C-KMS and Street, RA and Tsapras, Y and Hundertmark, M and Bachelet, E and Dominik, M and Li, Z and Cross, S and Cassan, A and Horne, K and Schmidt, R and Wambsganss, J and Ment, SK and Maoz, D and Snodgrass, C and Steele, IA and Team, R and Bozza, V and Burgdorf, MJ and Ciceri, S and Ago, GD and Evans, DF and Hinse, TC and Kerins, E and Kokotanekova, R and Longa, P and MacKenzie, J and Popovas, A and Rabus, M and Rahvar, S and Sajadian, S and Skottfelt, J and Southworth, J and Essen, CV and Team, M (2018) OGLE-2016-BLG-1190Lb: The First Spitzer Bulge Planet Lies Near the Planet/Brown-dwarf Boundary. Astronomical Journal, 155. 40 - 40. ISSN 1538-3881

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We report the discovery of OGLE-2016-BLG-1190Lb, which is likely to be the first Spitzer microlensing planet in the Galactic bulge/bar, an assignation that can be confirmed by two epochs of high-resolution imaging of the combined source–lens baseline object. The planet’s mass, M p = 13.4 ± 0.9 M J , places it right at the deuterium-burning limit, i.e., the conventional boundary between “planets” and “brown dwarfs.” Its existence raises the question of whether such objects are really “planets” (formed within the disks of their hosts) or “failed stars” (low-mass objects formed by gas fragmentation). This question may ultimately be addressed by comparing disk and bulge/bar planets, which is a goal of the Spitzer microlens program. The host is a G dwarf, M host = 0.89 ± 0.07 M ⊙ , and the planet has a semimajor axis a ∼ 2.0 au. We use Kepler K2 Campaign 9 microlensing data to break the lens-mass degeneracy that generically impacts parallax solutions from Earth– Spitzer observations alone, which is the first successful application of this approach. The microlensing data, derived primarily from near-continuous, ultradense survey observations from OGLE, MOA, and three KMTNet telescopes, contain more orbital information than for any previous microlensing planet, but not quite enough to accurately specify the full orbit. However, these data do permit the first rigorous test of microlensing orbital-motion measurements, which are typically derived from data taken over <1% of an orbital period.

Item Type: Article
Additional Information: This is the final published version of the article (version of record). It first appeared online via IOP Publishing at http://doi.org/10.3847/1538-3881/aa9be4 - please refer to any applicable terms of use of the publisher.
Uncontrolled Keywords: gravitational lensing, micro
Subjects: Q Science > QB Astronomy > QB460 Astrophysics
Divisions: Faculty of Natural Sciences > School of Chemical and Physical Sciences
Depositing User: Symplectic
Date Deposited: 17 Jan 2018 16:55
Last Modified: 17 Jan 2018 16:55
URI: http://eprints.keele.ac.uk/id/eprint/4380

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