Bibcode
Bachelet, E.; Bozza, V.; Han, C.; Udalski, A.; Bond, I. A.; Beaulieu, J.-P.; Street, R. A.; Kim, H.-I.; Bramich, D. M.; Cassan, A.; Dominik, M.; Figuera Jaimes, R.; Horne, K.; Hundertmark, M.; Mao, S.; Menzies, J.; Ranc, C.; Schmidt, R.; Snodgrass, C.; Steele, I. A.; Tsapras, Y.; Wambsganss, J.; The RoboNet collaboration; Mróz, P.; Soszyński, I.; Szymański, M. K.; Skowron, J.; Pietrukowicz, P.; Kozłowski, S.; Poleski, R.; Ulaczyk, K.; Pawlak, M.; The OGLE collaboration; Abe, F.; Barry, R.; Bennett, D. P.; Bhattacharya, A.; Donachie, M.; Fukui, A.; Hirao, Y.; Itow, Y.; Kawasaki, K.; Kondo, I.; Koshimoto, N.; Li, M. Cheung Alex; Matsubara, Y.; Muraki, Y.; Miyazaki, S.; Nagakane, M.; Rattenbury, N. J.; Suematsu, H.; Sullivan, D. J.; Sumi, T.; Suzuki, D.; Tristram, P. J.; Yonehara, A.; The MOA collaboration
Bibliographical reference
The Astrophysical Journal, Volume 870, Issue 1, article id. 11, 10 pp. (2019).
Advertised on:
1
2019
Journal
Citations
9
Refereed citations
8
Description
We present an analysis of the microlensing event OGLE-2015-BLG-0232.
This event is challenging to characterize for two reasons. First, the
light curve is not well sampled during the caustic crossing due to the
proximity of the full Moon impacting the photometry quality. Moreover,
the source brightness is difficult to estimate because this event is
blended with a nearby K dwarf star. We found that the light-curve
deviations are likely due to a close brown dwarf companion (i.e., s =
0.55 and q = 0.06), but the exact nature of the lens is still unknown.
We finally discuss the potential of follow-up observations to estimate
the lens mass and distance in the future.