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A brown dwarf orbiting an M-dwarf: MOA 2009-BLG-411L
, Article Astronomy and Astrophysics ; Volume 547 , 2012 ; 00046361 (ISSN) ; Fouqué, P ; Han, C ; Gould, A ; Albrow, M. D ; Beaulieu, J. P ; Bertin, E ; Bond, I. A ; Christie, G. W ; Heyrovský, D ; Horne, K ; Jørgensen, U. G ; Maoz, D ; Mathiasen, M ; Matsunaga, N ; McCormick, J ; Menzies, J ; Nataf, D ; Natusch, T ; Oi, N ; Renon, N ; Tsapras, Y ; Udalski, A ; Yee, J. C ; Batista, V ; Bennett, D. P ; Brillant, S ; Caldwell, J. A. R ; Cassan, A ; Cole, A ; Cook, K. H ; Coutures, C ; Dieters, S ; Dominik, M ; Dominis Prester, D ; Donatowicz, J ; Greenhill, J ; Kains, N ; Kane, S. R ; Marquette, J. B ; Martin, R ; Pollard, K. R ; Sahu, K. C ; Street, R. A ; Wambsganss, J ; Williams, A ; Zub, M ; Bos, M ; Dong, S ; Drummond, J ; Gaudi, B. S ; Graff, D ; Janczak, J ; Kaspi, S ; Kozłowski, S ; Lee, C. U ; Monard, L. A. G ; Muñoz, J. A ; Park, B. G ; Pogge, R. W ; Polishook, D ; Shporer, A ; Abe, F ; Botzler, C. S ; Fukui, A ; Furusawa, K ; Hearnshaw, J. B ; Itow, Y ; Korpela, A. V ; Ling, C.H ; Masuda, K ; Matsubara, Y ; Miyake, N ; Muraki, Y ; Ohnishi, K ; Rattenbury, N. J ; Saito, T ; Sullivan, D ; Sumi, T ; Suzuki, D ; Sweatman, W. L ; Tristram, P. J ; Wada, K ; Allan, A ; Bode, M. F ; Bramich, D. M ; Clay, N ; Fraser, S. N ; Hawkins, E ; Kerins, E ; Lister, T. A ; Mottram, C. J ; Saunders, E. S ; Snodgrass, C ; Steele, I. A ; Wheatley, P. J ; Bozza, V ; Browne, P ; Burgdorf, M. J ; Calchi Novati, S ; Dreizler, S ; Finet, F ; Glitrup, M ; Grundahl, F ; Harpsøe, K ; Hessman, F. V ; Hinse, T. C ; Hundertmark, M ; Liebig, C ; Maier, G ; Mancini, L ; Rahvar, S ; Ricci, D ; Scarpetta, G ; Skottfelt, J ; Southworth, J ; Surdej, J ; Zimmer, F ; Sharif University ot Technology
2012
Abstract
Context. Caustic crossing is the clearest signature of binary lenses in microlensing. In the present context, this signature is diluted by the large source star but a detailed analysis has allowed the companion signal to be extracted. Aims. MOA 2009-BLG-411 was detected on August 5, 2009 by the MOA-Collaboration. Alerted as a high-magnification event, it was sensitive to planets. Suspected anomalies in the light curve were not confirmed by a real-time model, but further analysis revealed small deviations from a single lens extended source fit. Methods. Thanks to observations by all the collaborations, this event was well monitored. We first decided to characterize the source star properties...
MOA-2010-BLG-311: A planetary candidate below the threshold of reliable detection
, Article Astrophysical Journal ; Volume 769, Issue 1 , 2013 ; 0004637X (ISSN) ; Hung, L. W ; Bond, I. A ; Allen, W ; Monard, L. A. G ; Albrow, M. D ; Fouqué, P ; Dominik, M ; Tsapras, Y ; Udalski, A ; Gould, A ; Zellem, R ; Bos, M ; Christie, G. W ; Depoy, D. L ; Dong, S ; Drummond, J ; Gaudi, B. S ; Gorbikov, E ; Han, C ; Kaspi, S ; Klein, N ; Lee, C.U ; Maoz, D ; McCormick, J ; Moorhouse, D ; Natusch, T ; Nola, M ; Park, B. G ; Pogge, R. W ; Polishook, D ; Shporer, A ; Shvartzvald, Y ; Skowron, J ; Thornley, G ; Abe, F ; Bennett, D. P ; Botzler, C. S ; Chote, P ; Freeman, M ; Fukui, A ; Furusawa, K ; Harris, P ; Itow, Y ; Ling, C. H ; Masuda, K ; Matsubara, Y ; Miyake, N ; Ohnishi, K ; Rattenbury, N. J ; Saito, T ; Sullivan, D. J ; Sumi, T ; Suzuki, D ; Sweatman, W. L ; Tristram, P. J ; Wada, K ; Yock, P. C. M ; Szymański, M. K ; Soszyński, I ; Kubiak, M ; Poleski, R ; Ulaczyk, K ; Pietrzyński, G ; Wyrzykowski, Ł ; Bachelet, E ; Batista, V ; Beatty, T. G ; Beaulieu, J. P ; Bennett, C. S ; Bowens-Rubin, R ; Brillant, S ; Caldwell, J. A. R ; Cassan, A ; Cole, A. A ; Corrales, E ; Coutures, C ; Dieters, S ; Dominis Prester, D ; Donatowicz, J ; Greenhill, J ; Henderson, C. B ; Kubas, D ; Marquette, J. B ; Martin, R ; Menzies, J. W ; Shappee, B ; Williams, A ; Wouters, D ; Van Saders, J ; Zub, M ; Street, R. A ; Horne, K ; Bramich, D. M ; Steele, I. A ; Alsubai, K. A ; Bozza, V ; Browne, P ; Burgdorf, M. J ; Calchi Novati, S ; Dodds, P ; Finet, F ; Gerner, T ; Hardis, S ; Harpsøe, K ; Hessman, F. V ; Hinse, T. C ; Hundertmark, M ; Jørgensen, U. G ; Kains, N ; Kerins, E ; Liebig, C ; Mancini, L ; Mathiasen, M ; Penny, M. T ; Proft, S ; Rahvar, S ; Ricci, D ; Sahu, K. C ; Scarpetta, G ; Schäfer, S ; Schönebeck, F ; Snodgrass, C ; Southworth, J ; Surdej, J ; Wambsganss, J ; Sharif University of Technology
Institute of Physics Publishing
2013
Abstract
We analyze MOA-2010-BLG-311, a high magnification (A max > 600) microlensing event with complete data coverage over the peak, making it very sensitive to planetary signals. We fit this event with both a point lens and a two-body lens model and find that the two-body lens model is a better fit but with only Δχ2 ∼ 80. The preferred mass ratio between the lens star and its companion is q = 10-3.7 ± 0.1, placing the candidate companion in the planetary regime. Despite the formal significance of the planet, we show that because of systematics in the data the evidence for a planetary companion to the lens is too tenuous to claim a secure detection. When combined with analyses of other...
MOA-2009-BLG-387Lb: A massive planet orbiting an M dwarf
, Article Astronomy and Astrophysics ; Volume 529 , 2011 ; 00046361 (ISSN) ; Gould, A ; Dieters, S ; Dong, S ; Bond, I ; Beaulieu, J. P ; Maoz, D ; Monard, B ; Christie, G. W ; McCormick, J ; Albrow, M. D ; Horne, K ; Tsapras, Y ; Burgdorf, M. J ; Calchi Novati, S ; Skottfelt, J ; Caldwell, J ; Kozłowski, S ; Kubas, D ; Gaudi, B. S ; Han, C ; Bennett, D. P ; An, J ; Abe, F ; Botzler, C. S ; Douchin, D ; Freeman, M ; Fukui, A ; Furusawa, K ; Hearnshaw, J.B ; Hosaka, S ; Itow, Y ; Kamiya, K ; Kilmartin, P. M ; Korpela, A ; Lin, W ; Ling, C. H ; Makita, S ; Masuda, K ; Matsubara, Y ; Miyake, N ; Muraki, Y ; Nagaya, M ; Nishimoto, K ; Ohnishi, K ; Okumura, T ; Perrott, Y. C ; Rattenbury, N ; Saito, T ; Sullivan, D. J ; Sumi, T ; Sweatman, W. L ; Tristram, P. J ; Von Seggern, E ; Yock, P. C. M ; Brillant, S ; Calitz, J. J ; Cassan, A ; Cole, A ; Cook, K ; Coutures, C ; Dominis Prester, D ; Donatowicz, J ; Greenhill, J ; Hoffman, M ; Jablonski, F ; Kane, S.R ; Kains, N ; Marquette, J.-B ; Martin, R ; Martioli, E ; Meintjes, P ; Menzies, J ; Pedretti, E ; Pollard, K ; Sahu, K.C ; Vinter, C ; Wambsganss, J ; Watson, R ; Williams, A ; Zub, M ; Allen, W ; Bolt, G ; Bos, M ; Depoy, D. L ; Drummond, J ; Eastman, J. D ; Gal-Yam, A ; Gorbikov, E ; Higgins, D ; Janczak, J ; Kaspi, S ; Lee, C. U ; Mallia, F ; Maury, A ; Monard, L. A. G ; Moorhouse, D ; Morgan, N ; Natusch, T ; Ofek, E. O ; Park, B. G ; Pogge, R. W ; Polishook, D ; Santallo, R ; Shporer, A ; Spector, O ; Thornley, G ; Yee, J. C ; Bozza, V ; Browne, P ; Dominik, M ; Dreizler, S ; Finet, F ; Glitrup, M ; Grundahl, F ; Harpsøe, K ; Hessman, F. V ; Hinse, T.C ; Hundertmark, M ; Jørgensen, U. G ; Liebig, C ; Maier, G ; Mancini, L ; Mathiasen, M ; Rahvar, S ; Ricci, D ; Scarpetta, G ; Southworth, J ; Surdej, J ; Zimmer, F ; Allan, A ; Bramich, D. M ; Snodgrass, C ; Steele, I. A ; Street, R. A ; Sharif University of Technology
2011
Abstract
Aims. We report the discovery of a planet with a high planet-to-star mass ratio in the microlensing event MOA-2009-BLG-387, which exhibited pronounced deviations over a 12-day interval, one of the longest for any planetary event. The host is an M dwarf, with a mass in the range 0.07 M ⊙ < Mhost < 0.49 M1 at 90% confidence. The planet-star mass ratio q = 0.0132 ± 0.003 has been measured extremely well, so at the best-estimated host mass, the planet mass is mp = 2.6 Jupiter masses for the median host mass, M = 0.19 M ⊙. Methods. The host mass is determined from two "higher order" microlensing parameters. One of these, the angular Einstein radius θE = 0.31 ± 0.03 mas has been accurately...
MOA 2010-BLG-477Lb: Constraining the mass of a microlensing planet from microlensing parallax, orbital motion, and detection of blended light
, Article Astrophysical Journal ; Volume 754, Issue 1 , 2012 ; 0004637X (ISSN) ; Shin, I. G ; Han, C ; Fouqué, P ; Gould, A ; Menzies, J. W ; Beaulieu, J. P ; Bennett, D. P ; Bond, I. A ; Dong, S ; Heyrovsk, D ; Marquette, J. B ; Marshall, J ; Skowron, J ; Street, R. A ; Sumi, T ; Udalski, A ; Abe, L ; Agabi, K ; Albrow, M. D ; Allen, W ; Bertin, E ; Bos, M ; Bramich, D. M ; Chavez, J ; Christie, G. W ; Cole, A. A ; Crouzet, N ; Dieters, S ; Dominik, M ; Drummond, J ; Greenhill, J ; Guillot, T ; Henderson, C. B ; Hessman, F. V ; Horne, K ; Hundertmark, M ; Johnson, J. A ; Jorgensen, U. G ; Kandori, R ; Liebig, C ; Mékarnia, D ; McCormick, J ; Moorhouse, D ; Nagayama, T ; Nataf, D ; Natusch, T ; Nishiyama, S ; Rivet, J. P ; Sahu, K. C ; Shvartzvald, Y ; Thornley, G ; Tomczak, A. R ; Tsapras, Y ; Yee, J. C ; Batista, V ; Bennett, C. S ; Brillant, S ; Caldwell, J. A. R ; Cassan, A ; Corrales, E ; Coutures, C ; Dominis Prester, D ; Donatowicz, J ; Kubas, D ; Martin, R ; Williams, A ; Zub, M ; Andrade De Almeida, L ; Depoy, D. L ; Gaudi, B. S ; Hung, L. W ; Jablonski, F ; Kaspi, S ; Klein, N ; Lee, C. U ; Lee, Y ; Koo, J. R ; Maoz, D ; Muñoz, J. A ; Pogge, R. W ; Polishook, D ; Shporer, A ; Abe, F ; Botzler, C. S ; Chote, P ; Freeman, M ; Fukui, A ; Furusawa, K ; Harris, P ; Itow, Y ; Kobara, S ; Ling, C. H ; Masuda, K ; Matsubara, Y ; Miyake, N ; Ohmori, K ; Ohnishi, K ; Rattenbury, N. J ; Saito, T ; Sullivan, D. J ; Suzuki, D ; Sweatman, W. L ; Tristram, P. J ; Wada, K ; Yock, P. C. M ; Szymański, M. K ; Soszyński, I ; Kubiak, M ; Poleski, R ; Ulaczyk, K ; Pietrzyński, G ; Wyrzykowski, Ł ; Kains, N ; Snodgrass, C ; Steele, I. A ; Alsubai, K. A ; Bozza, V ; Browne, P ; Burgdorf, M. J ; Calchi Novati, S ; Dodds, P ; Dreizler, S ; Finet, F ; Gerner, T ; Hardis, S ; Harpsoe, K ; Hinse, T. C ; Kerins, E ; Mancini, L ; Mathiasen, M ; Penny, M. T ; Proft, S ; Rahvar, S ; Ricci, D ; Scarpetta, G ; Schäfer, S ; Schönebeck, F ; Southworth, J ; Surdej, J ; Wambsganss, J ; Sharif University of Technology
IOP
2012
Abstract
Microlensing detections of cool planets are important for the construction of an unbiased sample to estimate the frequency of planets beyond the snow line, which is where giant planets are thought to form according to the core accretion theory of planet formation. In this paper, we report the discovery of a giant planet detected from the analysis of the light curve of a high-magnification microlensing event MOA 2010-BLG-477. The measured planet-star mass ratio is q = (2.181 ± 0.004) × 10-3 and the projected separation is s = 1.1228 ± 0.0006 in units of the Einstein radius. The angular Einstein radius is unusually large θE = 1.38 ± 0.11 mas. Combining this measurement with constraints on the...
Characterizing lenses and lensed stars of high-magnification single-lens gravitational microlensing events with lenses passing over source stars
, Article Astrophysical Journal ; Volume 751, Issue 1 , May , 2012 ; 0004637X (ISSN) ; Shin, I. G ; Park, S. Y ; Han, C ; Gould, A ; Sumi, T ; Udalski, A ; Beaulieu, J. P ; Street, R ; Dominik, M ; Allen, W ; Almeida, L. A ; Bos, M ; Christie, G. W ; Depoy, D. L ; Dong, S ; Drummond, J ; Gal Yam, A ; Gaudi, B. S ; Henderson, C. B ; Hung, L. W ; Jablonski, F ; Janczak, J ; Lee, C. U ; Mallia, F ; Maury, A ; McCormick, J ; McGregor, D ; Monard, L. A. G ; Moorhouse, D ; Muñoz, J. A ; Natusch, T ; Nelson, C ; Park, B. G ; Pogge, R. W ; Tg Tan, T. G ; Thornley, G ; Yee, J. C ; Abe, F ; Barnard, E ; Baudry, J ; Bennett, D. P ; Bond, I. A ; Botzler, C. S ; Freeman, M ; Fukui, A ; Furusawa, K ; Hayashi, F ; Hearnshaw, J. B ; Hosaka, S ; Itow, Y ; Kamiya, K ; Kilmartin, P. M ; Kobara, S ; Korpela, A ; Lin, W ; Ling, C. H ; Makita, S ; Masuda, K ; Matsubara, Y ; Miyake, N ; Muraki, Y ; Nagaya, M ; Nishimoto, K ; Ohnishi, K ; Okumura, T ; Omori, K ; Perrott, Y. C ; Rattenbury, N ; Saito, T ; Skuljan, L ; Sullivan, D. J ; Suzuki, D ; Suzuki, K ; Sweatman, W. L ; Takino, S ; Tristram, P. J ; Wada, K ; Yock, P. C. M ; Szymański, M. K ; Kubiak, M ; Pietrzyński, G ; Soszyński, I ; Poleski, R ; Ulaczyk, K ; Wyrzykowski, Ł ; Kozłowski, S ; Pietrukowicz, P ; Albrow, M. D ; Bachelet, E ; Batista, V ; Bennett, C. S ; Bowens Rubin, R ; Brillant, S ; Cassan, A ; Cole, A ; Corrales, E ; Coutures, C ; Dieters, S ; Dominis Prester, D ; Donatowicz, J ; Fouqué, P ; Greenhill, J ; Kane, S. R ; Menzies, J ; Sahu, K. C ; Wambsganss, J ; Williams, A ; Zub, M ; Allan, A ; Bramich, D. M ; Browne, P ; Clay, N ; Fraser, S ; Horne, K ; Kains, N ; Mottram, C ; Snodgrass, C ; Steele, I ; Tsapras, Y ; Alsubai, K. A ; Bozza, V ; Burgdorf, M. J ; Calchi Novati, S ; Dodds, P ; Dreizler, S ; Finet, F ; Gerner, T ; Glitrup, M ; Grundahl, F ; Hardis, S ; Harpsoe, K ; Hinse, T. C ; Hundertmark, M ; Jorgensen, U. G ; Kerins, E ; Liebig, C ; Maier, G ; Mancini, L ; Mathiasen, M ; Penny, M. T ; Proft, S ; Rahvar, S ; Ricci, D ; Scarpetta, G ; Schäfer, S ; Schönebeck, F ; Skottfelt, J ; Surdej, J ; Southworth, J ; Zimmer, F ; Sharif University of Technology
Institute of Physics Publishing
2012
Abstract
We present the analysis of the light curves of nine high-magnification single-lens gravitational microlensing events with lenses passing over source stars, including OGLE-2004-BLG-254, MOA-2007-BLG-176, MOA-2007-BLG-233/OGLE- 2007-BLG-302, MOA-2009-BLG-174, MOA-2010-BLG-436, MOA-2011-BLG-093, MOA-2011-BLG-274, OGLE-2011-BLG-0990/MOA-2011-BLG-300, and OGLE-2011-BLG-1101/ MOA-2011-BLG-325. For all of the events, we measure the linear limb-darkening coefficients of the surface brightness profile of source stars by measuring the deviation of the light curves near the peak affected by the finite-source effect. For seven events, we measure the Einstein radii and the lens-source relative proper...