%0 Journal Article
%4 dpi.inpe.br/plutao/2012/11.28.18.48.47
%2 dpi.inpe.br/plutao/2012/11.28.18.48.48
%@doi 10.1088/0004-637X/756/1/48
%@issn 0004-637X
%@issn 1538-4357
%F lattes: 7812463045514059 86 ChoiSHUSGBDFHSKSPPUPKSWABBBCFFFIKLMMMMOORSSSSSTTWYBSSSTABBCDDFGGHHHHHJJKKLLLMMPRRSSSSTWWABCDDGHJLMMMNNPTTYABBBCCCCDDDGKMMSZ:2012:NETYAM
%T A new type of ambiguity in the planet and binary interpretations of central perturbations of high-magnification gravitational microlensing events
%D 2012
%8 Sep.
%A Choi, J. -Y.,
%A Shin, I. -G.,
%A Han, C.,
%A Udalski, A.,
%A Sumi, T.,
%A Gould, A.,
%A Bozza, V.,
%A Dominik, M.,
%A Fouqué, P.,
%A Horne, K.,
%A Szyma ski, M. K.,
%A Kubiak, M.,
%A Soszy ski, I.,
%A Pietrzy ski, G.,
%A Poleski, R.,
%A Ulaczyk, K.,
%A Pietrukowicz, P.,
%A Koz owski, S.,
%A Skowron, J.,
%A Wyrzykowski, .,
%A Abe, F.,
%A Bennett, D. P.,
%A Bond, I. A.,
%A Botzler, C. S.,
%A Chote, P.,
%A Freeman, M.,
%A Fukui, A.,
%A Furusawa, K.,
%A Itow, Y.,
%A Kobara, S.,
%A Ling, C. H.,
%A Masuda, K.,
%A Matsubara, Y.,
%A Miyake, N.,
%A Muraki, Y.,
%A Ohmori, K.,
%A Ohnishi, K.,
%A Rattenbury, N. J.,
%A Saito, To.,
%A Sullivan, D. J.,
%A Suzuki, D.,
%A Suzuki, K.,
%A Sweatman, W. L.,
%A Takino, S.,
%A Tristram, P. J.,
%A Wada, K.,
%A Yock, P. C. M.,
%A Bramich, D. M.,
%A Snodgrass, C.,
%A Steele, I. A.,
%A Street, R. A.,
%A Tsapras, Y.,
%A Alsubai, K. A.,
%A Browne, P.,
%A Burgdorf, M. J.,
%A Calchi Novati, S.,
%A Dodds, P.,
%A Dreizler, S.,
%A Fang, X. -S.,
%A Grundahl, F.,
%A Gu, C. -H.,
%A Hardis, S.,
%A Harps e, K.,
%A Hinse, T. C.,
%A Hornstrup, A.,
%A Hundertmark, M.,
%A Jessen-Hansen, J.,
%A J rgensen, U. G.,
%A Kains, N.,
%A Kerins, E.,
%A Liebig, C.,
%A Lund, M.,
%A Lunkkvist, M.,
%A Mancini, L.,
%A Mathiasen, M.,
%A Penny, M. T.,
%A Rahvar, S.,
%A Ricci, D.,
%A Scarpetta, G.,
%A Skottfelt, J.,
%A Southworth, J.,
%A Surdej, J.,
%A Tregloan-Reed, J.,
%A Wambsganss, J.,
%A Wertz, O.,
%A Almeida, Leonardo Andrade de,
%A Batista, V.,
%A Christie, G.,
%A Depoy, D. L.,
%A Dong, Subo,
%A Gaudi, B. S.,
%A Henderson, C.,
%A Jablonski, Francisco,
%A Lee, C. -U.,
%A McCormick, J.,
%A McGregor, D.,
%A Moorhouse, D.,
%A Natusch, T.,
%A Ngan, H.,
%A Pogge, R. W.,
%A Tan, T. -G.,
%A Thornley, G.,
%A Yee, J. C.,
%A Albrow, M. D.,
%A Bachelet, E.,
%A Beaulieu, J. -P.,
%A Brillant, S.,
%A Cassan, A.,
%A Cole, A. A.,
%A Corrales, E.,
%A Coutures, C.,
%A Dieters, S.,
%A Dominis Prester, D.,
%A Donatowicz, J.,
%A Greenhill, J.,
%A Kubas, D.,
%A Marquette, J. -B.,
%A Menzies, J. W.,
%A Sahu, K. C.,
%A Zub, M.,
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%@affiliation Instituto Nacional de Pesquisas Espaciais (INPE)
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%@electronicmailaddress leonardo@das.inpe.br
%B Astrophysical Journal
%V 756
%N 1
%P 48 (9pp)
%K galactic bulge, gravitational microlensing.
%X High-magnification microlensing events provide an important channel to detect planets. Perturbations near the peak of a high-magnification event can be produced either by a planet or a binary companion. It is known that central perturbations induced by both types of companions can be generally distinguished due to the essentially different magnification pattern around caustics. In this paper, we present a case of central perturbations for which it is difficult to distinguish the planetary and binary interpretations. The peak of a lensing light curve affected by this perturbation appears to be blunt and flat. For a planetary case, this perturbation occurs when the source trajectory passes the negative perturbation region behind the back end of an arrowhead-shaped central caustic. For a binary case, a similar perturbation occurs for a source trajectory passing through the negative perturbation region between two cusps of an astroid-shaped caustic. We demonstrate the degeneracy for two high-magnification events of OGLE-2011-BLG-0526 and OGLE-2011-BLG-0950/MOA-2011-BLG-336. For OGLE-2011-BLG-0526, the χ2 difference between the planetary and binary model is ∼3, implying that the degeneracy is very severe. For OGLE- 2011-BLG-0950/MOA-2011-BLG-336, the stellar binary model is formally excluded with Δχ2 ∼ 105 and the planetary model is preferred. However, it is difficult to claim a planet discovery because systematic residuals of data from the planetary model are larger than the difference between the planetary and binary models. Considering that two events observed during a single season suffer from such a degeneracy, it is expected that central perturbations experiencing this type of degeneracy is common.
%@language pt