Red noise versus planetary interpretations in the microlensing event ogle-2013-BLG-446

Bachelet, E.; Bramich, D. M.; Han, C.; Greenhill, J.; Street, R. A.; Gould, A.; D'Ago, G.; Alsubai, K.; Dominik, M.; Jaimes, R. Figuera; Horne, K.; Hundertmark, M.; Kains, N.; Snodgrass, C.; Steele, I. A.; Tsapras, Y.; Albrow, M. D.; Batista, V.; Beaulieu, J. P.; Bennett, D. P.; Brillant, S.; Caldwell, J. A. R.; Cassan, A.; Cole, A.; Coutures, C.; Dieters, S.; Prester, D. Dominis; Donatowicz, J.; Fouqué, P.; Hill, K.; Marquette, J. B.; Menzies, J.; Pere, C.; Ranc, C.; Wambsganss, J.; Warren, D.; Almeida, L. Andrade De; Choi, J. Y.; Depoy, D. L.; Dong, S.; Hung, L. W.; Hwang, K. H.; Jablonski, F.; Jung, Y. K.; Kaspi, S.; Klein, N.; Lee, C. U.; Maoz, D.; Muñoz, J. A.; Nataf, D.; Park, H.; Pogge, R. W.; Polishook, D.; Shin, I. G.; Shporer, A.; Yee, J. C.; Abe, F.; Bhattacharya, A.; Bond, I. A.; Botzler, C. S.; Freeman, M.; Fukui, A.; Itow, Y.; Koshimoto, N.; Ling, C. H.; Masuda, K.; Matsubara, Y.; Muraki, Y.; Ohnishi, K.; Philpott, L. C.; Rattenbury, N.; Saito, T. o.; Sullivan, D. J.; Sumi, T.; Suzuki, D.; Tristram, P. J.; Yonehara, A.; Bozza, Valerio; CALCHI NOVATI, Sebastiano; Ciceri, S.; Galianni, P.; S. H., Gu; Harpsøe, K.; Hinse, T. C.; Jørgensen, U. G.; Juncher, D.; Korhonen, H.; Mancini, L.; Melchiorre, Chiara; Popovas, A.; Postiglione, A.; Rabus, M.; Rahvar, S.; Schmidt, R. W.; Scarpetta, Gaetano; Skottfelt, J.; Southworth, John; Stabile, Antonio; Surdej, J.; Wang, X. B.; Wertz, O.

doi:10.1088/0004-637X/812/2/136

For all exoplanet candidates, the reliability of a claimed detection needs to be assessed through a careful study of systematic errors in the data to minimize the false positives rate. We present a method to investigate such systematics in microlensing data sets using the microlensing event OGLE-2013-BLG-0446 as a case study. The event was observed from multiple sites around the world and its high magnification (Amax ∼ 3000) allowed us to investigate the effects of terrestrial and annual parallax. Real-time modeling of the event while it was still ongoing suggested the presence of an extremely low-mass companion (∼3M) to the lensing star, leading to substantial follow-up coverage of the light curve. We test and compare different models for the light curve and conclude that the data do not favor the planetary interpretation when systematic errors are taken into account.