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First assessment of the binary lens OGLE-2015-BLG-0232

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 brightne...

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Detalles Bibliográficos
Autores principales: Bachelet, Etienne (Autor) , Hundertmark, Markus (Autor) , Schmidt, Robert W. (Autor) , Tsapras, Yiannis (Autor) , Wambsganß, Joachim (Autor)
Formato: Article (Journal)
Lenguaje:inglés
Publicado: 2019
In: The astrophysical journal
Year: 2019, Volumen: 870, Número: 1
ISSN:1538-4357
DOI:10.3847/1538-4357/aaedb9
Acceso en línea:Verlag, Volltext: http://dx.doi.org/10.3847/1538-4357/aaedb9
Verlag, Volltext: http://stacks.iop.org/0004-637X/870/i=1/a=11
Enlace del recurso
Notas de Autor:E. Bachelet, V. Bozza, C. Han, A. Udalski, I.A. Bond, J.-P. Beaulieu, R.A. Street, H.-I. Kim, D.M. Bramich, A. Cassan, M. Dominik, R. Figuera Jaimes, K. Horne, M. Hundertmark, S. Mao, J. Menzies, C. Ranc, R. Schmidt, C. Snodgrass, I.A. Steele, Y. Tsapras, J. Wambsganss (The RoboNet collaboration), P. Mróz, I. Soszyński, M.K. Szymański, J. Skowron, P. Pietrukowicz, S. Kozłowski, R. Poleski, K. Ulaczyk, M. Pawlak (The OGLE collaboration), and F. Abe, R. Barry, D.P. Bennett, A. Bhattacharya, M. Donachie, A. Fukui, Y. Hirao, Y. Itow, K. Kawasaki, I. Kondo, N. Koshimoto, M. Cheung Alex Li, Y. Matsubara, Y. Muraki, S. Miyazaki, M. Nagakane, N.J. Rattenbury, H. Suematsu, D.J. Sullivan, T. Sumi, D. Suzuki, P.J. Tristram, and A. Yonehara (The MOA collaboration)
Descripción
Sumario: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.
Notas:Gesehen am 22.01.2019
Published 2018 December 27
Descripción Física:Online Resource
ISSN:1538-4357
DOI:10.3847/1538-4357/aaedb9

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