Facial reconstruction

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Bhattacharya, A and Bennett, DP and Bond, IA and Sumi, T and Udalski, A and Street, R and Tsapras, Y and Abe, F and Freeman, M and Fukui, A and Hirao, Y and Itow, Y and Koshimoto, N and Li, MCA and Ling, CH and Masuda, K and Matsubara, Y and Muraki, Y and Nagakane, M and Ohnishi, K and Rattenbury, N and Saito, T and Sharan, A and Sullivan, DJ and Suzuki, D and Tristram, PJ and Skowron, J and Szymanski, MK and Soszynski, I and Poleski, R and Mroz, P and Kozlowski, S and Pietrukowicz, P and Ulaczyk, K and Wyrzykowski, L and Bachelet, E and Bramich, DM and D'Ago, G and Dominik, M and Jaimes, RF and Horne, K and Hundertmark, M and Kains, N and Menzies, J and Schmidt, R and Snodgrass, C and Steele, IA and Wambsganss, J (2016) DISCOVERY OF A GAS GIANT PLANET IN MICROLENSING EVENT OGLE-2014-BLG-1760. ASTRONOMICAL JOURNAL, 152 (5). ISSN 0004-6256

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Open Access URL: https://arxiv.org/pdf/1603.05677.pdf (Accepted version)


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\pm 0.08. This is marginally consistent with source star in the Galactic bulge, but it could possibly indicate a young source star in 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_L = 6.9 \pm 1.1 kpc. It also indicates a host star mass of M_* = 0.51 \pm 0.44 M_\odot, a planet mass of m_p = 180 \pm 110 M_\oplus, and a projected star-planet separation of a_\perp = 1.7\pm 0.3\,AU. The lens-source relative proper motion is \mu_{\rm rel} = 6.5\pm 1.1 mas/yr. The lens (and stellar host star) is predicted to be very faint, so it is most likely that it can detected only when the lens and source stars are partially resolved. Due to the relatively high relative proper motion, the lens and source will be resolved to about \sim46\,mas in 6-8 years after the peak magnification. So, by 2020 - 2022, we can hope to detect the lens star with deep, high resolution images.

Item Type: Article
Uncontrolled Keywords: 0201 Astronomical And Space Sciences
Subjects: Q Science > QB Astronomy
Divisions: Astrophysics Research Institute
Related URLs:
Date Deposited: 13 Apr 2017 10:53
Last Modified: 13 Apr 2017 10:53
DOI or Identification number: 10.3847/0004-6256/152/5/140
URI: http://researchonline.ljmu.ac.uk/id/eprint/6253

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