First Assessment of the Binary Lens OGLE-2015-BLG-0232

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
Referencia bibliográfica

The Astrophysical Journal, Volume 870, Issue 1, article id. 11, 10 pp. (2019).

Fecha de publicación:
1
2019
Número de autores
57
Número de autores del IAC
1
Número de citas
9
Número de citas referidas
8
Descripción
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.