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112 results on '"Donachie, M."'

1. MOA-2006-BLG-074: recognizing xallarap contaminants in planetary microlensing

Author: Rota, P., Hirao, Y., Bozza, V., Abe, F., Barry, R., Bennett, D. P., Bhattacharya, A., Bond, I. A., Donachie, M., Fukui, A., Fujii, H., Silva, S. Ishitani, Itow, Y., Kirikawa, R., Koshimoto, N., Li, M. C. A., Matsubara, Y., Miyazaki, S., Muraki, Y., Olmschenk, G., Ranc, C., Satoh, Y., Sumi, T., Suzuki, D., Tristram, P. J., Yonehara, A., Rota, P., Hirao, Y., Bozza, V., Abe, F., Barry, R., Bennett, D. P., Bhattacharya, A., Bond, I. A., Donachie, M., Fukui, A., Fujii, H., Silva, S. Ishitani, Itow, Y., Kirikawa, R., Koshimoto, N., Li, M. C. A., Matsubara, Y., Miyazaki, S., Muraki, Y., Olmschenk, G., Ranc, C., Satoh, Y., Sumi, T., Suzuki, D., Tristram, P. J., and Yonehara, A.
Abstract: MOA-2006-BLG-074 was selected as one of the most promising planetary candidates in a retrospective analysis of the MOA collaboration: its asymmetric high-magnification peak can be perfectly explained by a source passing across a central caustic deformed by a small planet. However, after a detailed analysis of the residuals, we have realized that a single lens and a source orbiting with a faint companion provides a more satisfactory explanation for all the observed deviations from a Paczynski curve and the only physically acceptable interpretation. Indeed the orbital motion of the source is constrained enough to allow a very good characterization of the binary source from the microlensing light curve. The case of MOA-2006-BLG-074 suggests that the so-called xallarap effect must be taken seriously in any attempts to obtain accurate planetary demographics from microlensing surveys., Comment: 14 pages, 8 figures, accepted by AAS
Published: 2021
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2. MOA-2006-BLG-074: recognizing xallarap contaminants in planetary microlensing

Author: Rota, P., Hirao, Y., Bozza, V., Abe, F., Barry, R., Bennett, D. P., Bhattacharya, A., Bond, I. A., Donachie, M., Fukui, A., Fujii, H., Silva, S. Ishitani, Itow, Y., Kirikawa, R., Koshimoto, N., Li, M. C. A., Matsubara, Y., Miyazaki, S., Muraki, Y., Olmschenk, G., Ranc, C., Satoh, Y., Sumi, T., Suzuki, D., Tristram, P. J., Yonehara, A., Rota, P., Hirao, Y., Bozza, V., Abe, F., Barry, R., Bennett, D. P., Bhattacharya, A., Bond, I. A., Donachie, M., Fukui, A., Fujii, H., Silva, S. Ishitani, Itow, Y., Kirikawa, R., Koshimoto, N., Li, M. C. A., Matsubara, Y., Miyazaki, S., Muraki, Y., Olmschenk, G., Ranc, C., Satoh, Y., Sumi, T., Suzuki, D., Tristram, P. J., and Yonehara, A.
Abstract: MOA-2006-BLG-074 was selected as one of the most promising planetary candidates in a retrospective analysis of the MOA collaboration: its asymmetric high-magnification peak can be perfectly explained by a source passing across a central caustic deformed by a small planet. However, after a detailed analysis of the residuals, we have realized that a single lens and a source orbiting with a faint companion provides a more satisfactory explanation for all the observed deviations from a Paczynski curve and the only physically acceptable interpretation. Indeed the orbital motion of the source is constrained enough to allow a very good characterization of the binary source from the microlensing light curve. The case of MOA-2006-BLG-074 suggests that the so-called xallarap effect must be taken seriously in any attempts to obtain accurate planetary demographics from microlensing surveys., Comment: 14 pages, 8 figures, accepted by AAS
Published: 2021
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3. OGLE-2018-BLG-1185b : A Low-Mass Microlensing Planet Orbiting a Low-Mass Dwarf

Author: Kondo, Iona, Yee, Jennifer C., Bennett, David P., Sumi, Takahiro, Koshimoto, Naoki, Bond, Ian A., Gould, Andrew, Udalski, Andrzej, Shvartzvald, Yossi, Jung, Youn Kil, Zang, Weicheng, Bozza, Valerio, Bachelet, Etienne, Hundertmark, Markus P. G., Rattenbury, Nicholas J., Abe, F., Barry, R., Bhattacharya, A., Donachie, M., Fukui, A., Fujii, H., Hirao, Y., Silva, S. Ishitani, Itow, Y., Kirikawa, R., Li, M. C. A., Matsubara, Y., Miyazaki, S., Muraki, Y., Olmschenk, G., Ranc, C., Satoh, Y., Shoji, H., Suzuki, D., Tanaka, Y., Tristram, P. J., Yamawaki, T., Yonehara, A., Mróz, P., Poleski, R., Skowron, J., Szymański, M. K., Soszyński, I., Kozłowski, S., Ulaczyk, P. Pietrukowicz K., Rybicki, K. A., Iwanek, P., Wrona, M., Albrow, M. D., Chung, S. -J., Han, C., Hwang, K. -H., Kim, H. -W., Shin, I. -G., Cha, S. -M., Kim, D. -J., Kim, S. -L., Lee, C. -U., Lee, D. -J., Lee, Y., Park, B. -G., Pogge, R. W., Ryu, Y. -H., Beichman, C. A., Bryden, G., Novati, S. Calchi, Carey, S., Gaudi, B. S., Henderson, C. B., Zhu, W., Maoz, D., Penny, M. T., Dominik, M., Jørgensen, U. G., n}}a, P. Longa-Pe{\~{, Peixinho, N., Sajadian, S., Skottfelt, J., Snodgrass, C., Tregloan-Reed, J., Burgdorf, M. J., Campbell-White, J., Dib, S., Fujii, Y. I., Hinse, T. C., Khalouei, E., Rahvar, S., Rabus, M., Southworth, J., Tsapras, Y., Street, R. A., Bramich, D. M., Cassan, A., Horne, K., Wambsganss, J., Mao, S., Saha, A., Kondo, Iona, Yee, Jennifer C., Bennett, David P., Sumi, Takahiro, Koshimoto, Naoki, Bond, Ian A., Gould, Andrew, Udalski, Andrzej, Shvartzvald, Yossi, Jung, Youn Kil, Zang, Weicheng, Bozza, Valerio, Bachelet, Etienne, Hundertmark, Markus P. G., Rattenbury, Nicholas J., Abe, F., Barry, R., Bhattacharya, A., Donachie, M., Fukui, A., Fujii, H., Hirao, Y., Silva, S. Ishitani, Itow, Y., Kirikawa, R., Li, M. C. A., Matsubara, Y., Miyazaki, S., Muraki, Y., Olmschenk, G., Ranc, C., Satoh, Y., Shoji, H., Suzuki, D., Tanaka, Y., Tristram, P. J., Yamawaki, T., Yonehara, A., Mróz, P., Poleski, R., Skowron, J., Szymański, M. K., Soszyński, I., Kozłowski, S., Ulaczyk, P. Pietrukowicz K., Rybicki, K. A., Iwanek, P., Wrona, M., Albrow, M. D., Chung, S. -J., Han, C., Hwang, K. -H., Kim, H. -W., Shin, I. -G., Cha, S. -M., Kim, D. -J., Kim, S. -L., Lee, C. -U., Lee, D. -J., Lee, Y., Park, B. -G., Pogge, R. W., Ryu, Y. -H., Beichman, C. A., Bryden, G., Novati, S. Calchi, Carey, S., Gaudi, B. S., Henderson, C. B., Zhu, W., Maoz, D., Penny, M. T., Dominik, M., Jørgensen, U. G., n}}a, P. Longa-Pe{\~{, Peixinho, N., Sajadian, S., Skottfelt, J., Snodgrass, C., Tregloan-Reed, J., Burgdorf, M. J., Campbell-White, J., Dib, S., Fujii, Y. I., Hinse, T. C., Khalouei, E., Rahvar, S., Rabus, M., Southworth, J., Tsapras, Y., Street, R. A., Bramich, D. M., Cassan, A., Horne, K., Wambsganss, J., Mao, S., and Saha, A.
Abstract: We report the analysis of planetary microlensing event OGLE-2018-BLG-1185, which was observed by a large number of ground-based telescopes and by the $Spitzer$ Space Telescope. The ground-based light curve indicates a low planet-host star mass ratio of $q = (6.9 \pm 0.2) \times 10^{-5}$, which is near the peak of the wide-orbit exoplanet mass-ratio distribution. We estimate the host star and planet masses with a Bayesian analysis using the measured angular Einstein radius under the assumption that stars of all masses have an equal probability to host this planet. The flux variation observed by $Spitzer$ was marginal, but still places a constraint on the microlens parallax. Imposing a conservative constraint that this flux variation should be $\Delta f_{\rm Spz} < 4$ instrumental flux units indicates a host mass of $M_{\rm host} = 0.37^{+0.35}_{-0.21}\ M_\odot$ and a planet mass of $m_{\rm p} = 8.4^{+7.9}_{-4.7}\ M_\oplus$. A Bayesian analysis including the full parallax constraint from $Spitzer$ suggests smaller host star and planet masses of $M_{\rm host} = 0.091^{+0.064}_{-0.018}\ M_\odot$ and $m_{\rm p} = 2.1^{+1.5}_{-0.4}\ M_\oplus$, respectively. Future high-resolution imaging observations with $HST$ or ELTs could distinguish between these two scenarios and help to reveal the planetary system properties in more detail., Comment: 30 pages, 11 figures, 5 tables, Accepted for publication in Astronomical Journal (AJ)
Published: 2021
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4. OGLE-2018-BLG-1185b:A Low-mass Microlensing Planet Orbiting a Low-mass Dwarf

Author: Kondo, Iona, Yee, Jennifer C., Bennett, David P., Sumi, Takahiro, Koshimoto, Naoki, Bond, Ian A., Gould, Andrew, Udalski, Andrzej, Shvartzvald, Yossi, Jung, Youn Kil, Zang, Weicheng, Bozza, Valerio, Bachelet, Etienne, Hundertmark, Markus P. G., Rattenbury, Nicholas J., Abe, F., Barry, R., Bhattacharya, A., Donachie, M., Fukui, A., Fujii, H., Hirao, Y., Silva, S. Ishitani, Itow, Y., Kirikawa, R., Li, M. C. A., Matsubara, Y., Miyazaki, S., Muraki, Y., Olmschenk, G., Ranc, C., Satoh, Y., Shoji, H., Suzuki, D., Tanaka, Y., Tristram, P. J., Yamawaki, T., Yonehara, A., Mroz, P., Poleski, R., Skowron, J., Szymanski, M. K., Kim, H-W, Kim, S-L, Lee, C-U, Lee, Y., Jorgensen, U. G., Skottfelt, J., Dib, S., Fujii, Y., Kondo, Iona, Yee, Jennifer C., Bennett, David P., Sumi, Takahiro, Koshimoto, Naoki, Bond, Ian A., Gould, Andrew, Udalski, Andrzej, Shvartzvald, Yossi, Jung, Youn Kil, Zang, Weicheng, Bozza, Valerio, Bachelet, Etienne, Hundertmark, Markus P. G., Rattenbury, Nicholas J., Abe, F., Barry, R., Bhattacharya, A., Donachie, M., Fukui, A., Fujii, H., Hirao, Y., Silva, S. Ishitani, Itow, Y., Kirikawa, R., Li, M. C. A., Matsubara, Y., Miyazaki, S., Muraki, Y., Olmschenk, G., Ranc, C., Satoh, Y., Shoji, H., Suzuki, D., Tanaka, Y., Tristram, P. J., Yamawaki, T., Yonehara, A., Mroz, P., Poleski, R., Skowron, J., Szymanski, M. K., Kim, H-W, Kim, S-L, Lee, C-U, Lee, Y., Jorgensen, U. G., Skottfelt, J., Dib, S., and Fujii, Y.
Abstract: We report an analysis of the planetary microlensing event OGLE-2018-BLG-1185, which was observed by a large number of ground-based telescopes and by the Spitzer Space Telescope. The ground-based light curve indicates a low planet-host star mass ratio of q = (6.9 +/- 0.2) x 10(-5), which is near the peak of the wide-orbit exoplanet mass-ratio distribution. We estimate the host star and planet masses with a Bayesian analysis using the measured angular Einstein radius under the assumption that stars of all masses have an equal probability of hosting the planet. The flux variation observed by Spitzer is marginal, but still places a constraint on the microlens parallax. Imposing a conservative constraint that this flux variation should be Delta f (Spz) < 4 instrumental flux units yields a host mass of M-host = 0.37(-0.21)(+0.35) M-circle dot and a planet mass of m(p) = 8.4(-4.7)(+7.9) M-circle plus. A Bayesian analysis including the full parallax constraint from Spitzer suggests smaller host star and planet masses of M-host = 0.091(-0.018)(+0.064) M-circle dot m(p) = 2.1(-0.4)(+1.5) M-circle plus, respectively. Future high-resolution imaging observations with the Hubble Space Telescope or Extremely Large Telescope could distinguish between these two scenarios and help reveal the planetary system properties in more detail.
Published: 2021

5. OGLE-2013-BLG-0911Lb: A Secondary on the Brown-Dwarf Planet Boundary around an M-dwarf

Author: Miyazaki, Shota, Sumi, Takahiro, Bennett, David P., Udalski, Andrzej, Shvartzvald, Yossi, Street, Rachel, Bozza, Valerio, Yee, Jennifer C., Bond, Ian A., Rattenbury, Nicholas, Koshimoto, Naoki, Suzuki, Daisuke, Fukui, Akihiko, Abe, F., Bhattacharya, A., Barry, R., Donachie, M., Fujii, H., Hirao, Y., Itow, Y., Kamei, Y., Kondo, I., Li, M. C. A., Ling, C. H., Matsubara, Y., Matsuo, T., Muraki, Y., Nagakane, M., Ohnishi, K., Ranc, C., Saito, T., Sharan, A., Shibai, H., Suematsu, H., Sullivan, D. J., Tristram, P. J., Yamakawa, T., Yonehara, A., Skowron, J., Poleski, R., Mr'oz, P., Szyma'nski, M. K., Soszy'nski, I., Pietrukowicz, P., KozLowski, S., Ulaczyk, K., Wyrzykowski, L., Friedmann, Matan, Kaspi, Shai, Maoz, Dan, Albrow, M., Christie, G., DePoy, D. L., Gal-Yam, A., Gould, A., Lee, C. -U., Manulis, I., McCormick, J., Natusch, T., Ngan, H., Pogge, R. W., Porritt, I., Tsapras, Y., Bachelet, E., Hundertmark, M. P. G., Dominik, M., Bramich, D. M., Cassan, A., Jaimes, R. Figuera, Horne, K., Schmidt, R., Snodgrass, C., Wambsganss, J., Steele, I. A., Menzies, J., Mao, S., Jorgensen, U. G., Burgdorf, M. J., Ciceri, S., Novati, S. Calchi, D'Ago, G., Evans, D. F., Hinse, T. C., Kains, N., Kerins, E., Korhonen, H., Mancini, L., Popovas, A., Rabus, M., Rahvar, S., Scarpetta, G., Skottfelt, J., Southworth, J., Peixinho, N., Verma, P., Miyazaki, Shota, Sumi, Takahiro, Bennett, David P., Udalski, Andrzej, Shvartzvald, Yossi, Street, Rachel, Bozza, Valerio, Yee, Jennifer C., Bond, Ian A., Rattenbury, Nicholas, Koshimoto, Naoki, Suzuki, Daisuke, Fukui, Akihiko, Abe, F., Bhattacharya, A., Barry, R., Donachie, M., Fujii, H., Hirao, Y., Itow, Y., Kamei, Y., Kondo, I., Li, M. C. A., Ling, C. H., Matsubara, Y., Matsuo, T., Muraki, Y., Nagakane, M., Ohnishi, K., Ranc, C., Saito, T., Sharan, A., Shibai, H., Suematsu, H., Sullivan, D. J., Tristram, P. J., Yamakawa, T., Yonehara, A., Skowron, J., Poleski, R., Mr'oz, P., Szyma'nski, M. K., Soszy'nski, I., Pietrukowicz, P., KozLowski, S., Ulaczyk, K., Wyrzykowski, L., Friedmann, Matan, Kaspi, Shai, Maoz, Dan, Albrow, M., Christie, G., DePoy, D. L., Gal-Yam, A., Gould, A., Lee, C. -U., Manulis, I., McCormick, J., Natusch, T., Ngan, H., Pogge, R. W., Porritt, I., Tsapras, Y., Bachelet, E., Hundertmark, M. P. G., Dominik, M., Bramich, D. M., Cassan, A., Jaimes, R. Figuera, Horne, K., Schmidt, R., Snodgrass, C., Wambsganss, J., Steele, I. A., Menzies, J., Mao, S., Jorgensen, U. G., Burgdorf, M. J., Ciceri, S., Novati, S. Calchi, D'Ago, G., Evans, D. F., Hinse, T. C., Kains, N., Kerins, E., Korhonen, H., Mancini, L., Popovas, A., Rabus, M., Rahvar, S., Scarpetta, G., Skottfelt, J., Southworth, J., Peixinho, N., and Verma, P.
Abstract: We present the analysis of the binary-lens microlensing event OGLE-2013-BLG-0911. The best-fit solutions indicate the binary mass ratio of q~0.03 which differs from that reported in Shvartzvald+2016. The event suffers from the well-known close/wide degeneracy, resulting in two groups of solutions for the projected separation normalized by the Einstein radius of s~0.15 or s~7. The finite source and the parallax observations allow us to measure the lens physical parameters. The lens system is an M-dwarf orbited by a massive Jupiter companion at very close (M_{host}=0.30^{+0.08}_{-0.06} M_{Sun}, M_{comp}=10.1^{+2.9}_{-2.2} M_{Jup}, a_{exp}=0.40^{+0.05}_{-0.04} au) or wide (M_{host}=0.28^{+0.10}_{-0.08} M_{Sun}, M_{comp}=9.9^{+3.8}_{-3.5}M_{Jup}, a_{exp}=18.0^{+3.2}_{-3.2} au) separation. Although the mass ratio is slightly above the planet-brown dwarf (BD) mass-ratio boundary of q=0.03 which is generally used, the median physical mass of the companion is slightly below the planet-BD mass boundary of 13M_{Jup}. It is likely that the formation mechanisms for BDs and planets are different and the objects near the boundaries could have been formed by either mechanism. It is important to probe the distribution of such companions with masses of ~13M_{Jup} in order to statistically constrain the formation theories for both BDs and massive planets. In particular, the microlensing method is able to probe the distribution around low-mass M-dwarfs and even BDs which is challenging for other exoplanet detection methods., Comment: 22 pages, 10 figures, Accepted for publication in The Astronomical Journal
Published: 2019
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6. An analysis of binary microlensing event OGLE-2015-BLG-0060

Author: Tsapras, Y., Cassan, A., Ranc, C., Bachelet, E., Street, R., Udalski, A., Hundertmark, M., Bozza, V., Beaulieu, J. P., Marquette, J. B., Euteneuer, E., team, The RoboNet, Bramich, D. M., Dominik, M., Jaimes, R. Figuera, Horne, K., Mao, S., Menzies, J., Schmidt, R., Snodgrass, C., Steele, I. A., Wambsganss, J., collaboration, The OGLE, Mróz, P., Szymański, M. K., Soszyński, I., Skowron, J., Pietrukowicz, P., Kozłowski, S., Poleski, R., Ulaczyk, K., Pawlak, M., collaboration, The MiNDSTEp, Jørgensen, U. G., Skottfelt, J., Popovas, A., Ciceri, S., Korhonen, H., Kuffmeier, M., Evans, D. F., Peixinho, N., Hinse, T. C., Burgdorf, M. J., Southworth, J., Tronsgaard, R., Kerins, E., Andersen, M. I., Rahvar, S., Wang, Y., Wertz, O., Rabus, M., Novati, S. Calchi, D'Ago, G., Scarpetta, G., Mancini, L., collaboration, The MOA, Abe, F., Asakura, Y., Bennett, D. P., Bhattacharya, A., Donachie, M., Evans, P., Fukui, A., Hirao, Y., Itow, Y., Kawasaki, K., Koshimoto, N., Li, M. C. A., Ling, C. H., Masuda, K., Matsubara, Y., Muraki, Y., Miyazaki, S., Nagakane, M., Ohnishi, K., Rattenbury, N., Saito, To., Sharan, A., Shibai, H., Sullivan, D. J., Sumi, T., Suzuki, D., Tristram, P. J., Yamada, T., Yonehara, A., Tsapras, Y., Cassan, A., Ranc, C., Bachelet, E., Street, R., Udalski, A., Hundertmark, M., Bozza, V., Beaulieu, J. P., Marquette, J. B., Euteneuer, E., team, The RoboNet, Bramich, D. M., Dominik, M., Jaimes, R. Figuera, Horne, K., Mao, S., Menzies, J., Schmidt, R., Snodgrass, C., Steele, I. A., Wambsganss, J., collaboration, The OGLE, Mróz, P., Szymański, M. K., Soszyński, I., Skowron, J., Pietrukowicz, P., Kozłowski, S., Poleski, R., Ulaczyk, K., Pawlak, M., collaboration, The MiNDSTEp, Jørgensen, U. G., Skottfelt, J., Popovas, A., Ciceri, S., Korhonen, H., Kuffmeier, M., Evans, D. F., Peixinho, N., Hinse, T. C., Burgdorf, M. J., Southworth, J., Tronsgaard, R., Kerins, E., Andersen, M. I., Rahvar, S., Wang, Y., Wertz, O., Rabus, M., Novati, S. Calchi, D'Ago, G., Scarpetta, G., Mancini, L., collaboration, The MOA, Abe, F., Asakura, Y., Bennett, D. P., Bhattacharya, A., Donachie, M., Evans, P., Fukui, A., Hirao, Y., Itow, Y., Kawasaki, K., Koshimoto, N., Li, M. C. A., Ling, C. H., Masuda, K., Matsubara, Y., Muraki, Y., Miyazaki, S., Nagakane, M., Ohnishi, K., Rattenbury, N., Saito, To., Sharan, A., Shibai, H., Sullivan, D. J., Sumi, T., Suzuki, D., Tristram, P. J., Yamada, T., and Yonehara, A.
Abstract: We present the analysis of stellar binary microlensing event OGLE-2015-BLG-0060 based on observations obtained from 13 different telescopes. Intensive coverage of the anomalous parts of the light curve was achieved by automated follow-up observations from the robotic telescopes of the Las Cumbres Observatory. We show that, for the first time, all main features of an anomalous microlensing event are well covered by follow-up data, allowing us to estimate the physical parameters of the lens. The strong detection of second-order effects in the event light curve necessitates the inclusion of longer-baseline survey data in order to constrain the parallax vector. We find that the event was most likely caused by a stellar binary-lens with masses $M_{\star1} = 0.87 \pm 0.12 M_{\odot}$ and $M_{\star2} = 0.77 \pm 0.11 M_{\odot}$. The distance to the lensing system is 6.41 $\pm 0.14$ kpc and the projected separation between the two components is 13.85 $\pm 0.16$ AU. Alternative interpretations are also considered., Comment: 13 pages, 5 figures, Published in MNRAS
Published: 2019
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7. The 2L1S/1L2S Degeneracy for Two Microlensing Planet Candidates Discovered by the KMTNet Survey in 2017

Author: Shin, I. -G., Yee, J. C., Gould, A., Penny, M. T., Bond, I. A., Albrow, M. D., Chung, S. -J., Han, C., Hwang, K. -H., Jung, Y. K., Ryu, Y. -H., Shvartzvald, Y., Cha, S. -M., Kim, D. -J., Kim, H. -W., Kim, S. -L., Lee, C. -U., Lee, D. -J., Lee, Y., Park, B. -G., Pogge, R. W., Abe, F., Barry, R., Bennett, D. P., Bhattacharya, A., Donachie, M., Fujii, H., Fukui, A., Hirao, Y., Itow, Y., Kamei, Y., Kondo, Iona, Koshimoto, N., Li, M. C. A., Matsubara, Y., Miyazaki, S., Muraki, Y., Nagakane, M., Ranc, C., Rattenbury, N. J., Suematsu, Harmon, Sullivan, D. J., Sumi, T., Suzuki, Daisuke, Tristram, P. J., Yamakawa, T., Yonehara, A., Fouqué, P., Zang, W., Shin, I. -G., Yee, J. C., Gould, A., Penny, M. T., Bond, I. A., Albrow, M. D., Chung, S. -J., Han, C., Hwang, K. -H., Jung, Y. K., Ryu, Y. -H., Shvartzvald, Y., Cha, S. -M., Kim, D. -J., Kim, H. -W., Kim, S. -L., Lee, C. -U., Lee, D. -J., Lee, Y., Park, B. -G., Pogge, R. W., Abe, F., Barry, R., Bennett, D. P., Bhattacharya, A., Donachie, M., Fujii, H., Fukui, A., Hirao, Y., Itow, Y., Kamei, Y., Kondo, Iona, Koshimoto, N., Li, M. C. A., Matsubara, Y., Miyazaki, S., Muraki, Y., Nagakane, M., Ranc, C., Rattenbury, N. J., Suematsu, Harmon, Sullivan, D. J., Sumi, T., Suzuki, Daisuke, Tristram, P. J., Yamakawa, T., Yonehara, A., Fouqué, P., and Zang, W.
Abstract: We report two microlensing planet candidates discovered by the KMTNet survey in $2017$. However, both events have the 2L1S/1L2S degeneracy, which is an obstacle to claiming the discovery of the planets with certainty unless the degeneracy can be resolved. For KMT-2017-BLG-0962, the degeneracy cannot be resolved. If the 2L1S solution is correct, KMT-2017-BLG-0962 might be produced by a super Jupiter-mass planet orbiting a mid-M dwarf host star. For KMT-2017-BLG-1119, the light curve modeling favors the 2L1S solution but higher-resolution observations of the baseline object tend to support the 1L2S interpretation rather than the planetary interpretation. This degeneracy might be resolved by a future measurement of the lens-source relative proper motion. This study shows the problem of resolving 2L1S/1L2S degeneracy exists over a much wider range of conditions than those considered by the theoretical study of Gaudi (1998)., Comment: 15 pages, 12 figures, 4 tables, accepted in AJ
Published: 2019
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8. An analysis of binary microlensing event OGLE-2015-BLG-0060

Author: Tsapras, Y., Cassan, A., Ranc, C., Bachelet, E., Street, R., Udalski, A., Hundertmark, M., Bozza, V., Beaulieu, J. P., Marquette, J. B., Euteneuer, E., team, The RoboNet, Bramich, D. M., Dominik, M., Jaimes, R. Figuera, Horne, K., Mao, S., Menzies, J., Schmidt, R., Snodgrass, C., Steele, I. A., Wambsganss, J., collaboration, The OGLE, Mróz, P., Szymański, M. K., Soszyński, I., Skowron, J., Pietrukowicz, P., Kozłowski, S., Poleski, R., Ulaczyk, K., Pawlak, M., collaboration, The MiNDSTEp, Jørgensen, U. G., Skottfelt, J., Popovas, A., Ciceri, S., Korhonen, H., Kuffmeier, M., Evans, D. F., Peixinho, N., Hinse, T. C., Burgdorf, M. J., Southworth, J., Tronsgaard, R., Kerins, E., Andersen, M. I., Rahvar, S., Wang, Y., Wertz, O., Rabus, M., Novati, S. Calchi, D'Ago, G., Scarpetta, G., Mancini, L., collaboration, The MOA, Abe, F., Asakura, Y., Bennett, D. P., Bhattacharya, A., Donachie, M., Evans, P., Fukui, A., Hirao, Y., Itow, Y., Kawasaki, K., Koshimoto, N., Li, M. C. A., Ling, C. H., Masuda, K., Matsubara, Y., Muraki, Y., Miyazaki, S., Nagakane, M., Ohnishi, K., Rattenbury, N., Saito, To., Sharan, A., Shibai, H., Sullivan, D. J., Sumi, T., Suzuki, D., Tristram, P. J., Yamada, T., Yonehara, A., Tsapras, Y., Cassan, A., Ranc, C., Bachelet, E., Street, R., Udalski, A., Hundertmark, M., Bozza, V., Beaulieu, J. P., Marquette, J. B., Euteneuer, E., team, The RoboNet, Bramich, D. M., Dominik, M., Jaimes, R. Figuera, Horne, K., Mao, S., Menzies, J., Schmidt, R., Snodgrass, C., Steele, I. A., Wambsganss, J., collaboration, The OGLE, Mróz, P., Szymański, M. K., Soszyński, I., Skowron, J., Pietrukowicz, P., Kozłowski, S., Poleski, R., Ulaczyk, K., Pawlak, M., collaboration, The MiNDSTEp, Jørgensen, U. G., Skottfelt, J., Popovas, A., Ciceri, S., Korhonen, H., Kuffmeier, M., Evans, D. F., Peixinho, N., Hinse, T. C., Burgdorf, M. J., Southworth, J., Tronsgaard, R., Kerins, E., Andersen, M. I., Rahvar, S., Wang, Y., Wertz, O., Rabus, M., Novati, S. Calchi, D'Ago, G., Scarpetta, G., Mancini, L., collaboration, The MOA, Abe, F., Asakura, Y., Bennett, D. P., Bhattacharya, A., Donachie, M., Evans, P., Fukui, A., Hirao, Y., Itow, Y., Kawasaki, K., Koshimoto, N., Li, M. C. A., Ling, C. H., Masuda, K., Matsubara, Y., Muraki, Y., Miyazaki, S., Nagakane, M., Ohnishi, K., Rattenbury, N., Saito, To., Sharan, A., Shibai, H., Sullivan, D. J., Sumi, T., Suzuki, D., Tristram, P. J., Yamada, T., and Yonehara, A.
Abstract: We present the analysis of stellar binary microlensing event OGLE-2015-BLG-0060 based on observations obtained from 13 different telescopes. Intensive coverage of the anomalous parts of the light curve was achieved by automated follow-up observations from the robotic telescopes of the Las Cumbres Observatory. We show that, for the first time, all main features of an anomalous microlensing event are well covered by follow-up data, allowing us to estimate the physical parameters of the lens. The strong detection of second-order effects in the event light curve necessitates the inclusion of longer-baseline survey data in order to constrain the parallax vector. We find that the event was most likely caused by a stellar binary-lens with masses $M_{\star1} = 0.87 \pm 0.12 M_{\odot}$ and $M_{\star2} = 0.77 \pm 0.11 M_{\odot}$. The distance to the lensing system is 6.41 $\pm 0.14$ kpc and the projected separation between the two components is 13.85 $\pm 0.16$ AU. Alternative interpretations are also considered., Comment: 13 pages, 5 figures, Published in MNRAS
Published: 2019
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9. The 2L1S/1L2S Degeneracy for Two Microlensing Planet Candidates Discovered by the KMTNet Survey in 2017

Author: Shin, I. -G., Yee, J. C., Gould, A., Penny, M. T., Bond, I. A., Albrow, M. D., Chung, S. -J., Han, C., Hwang, K. -H., Jung, Y. K., Ryu, Y. -H., Shvartzvald, Y., Cha, S. -M., Kim, D. -J., Kim, H. -W., Kim, S. -L., Lee, C. -U., Lee, D. -J., Lee, Y., Park, B. -G., Pogge, R. W., Abe, F., Barry, R., Bennett, D. P., Bhattacharya, A., Donachie, M., Fujii, H., Fukui, A., Hirao, Y., Itow, Y., Kamei, Y., Kondo, Iona, Koshimoto, N., Li, M. C. A., Matsubara, Y., Miyazaki, S., Muraki, Y., Nagakane, M., Ranc, C., Rattenbury, N. J., Suematsu, Harmon, Sullivan, D. J., Sumi, T., Suzuki, Daisuke, Tristram, P. J., Yamakawa, T., Yonehara, A., Fouqué, P., Zang, W., Shin, I. -G., Yee, J. C., Gould, A., Penny, M. T., Bond, I. A., Albrow, M. D., Chung, S. -J., Han, C., Hwang, K. -H., Jung, Y. K., Ryu, Y. -H., Shvartzvald, Y., Cha, S. -M., Kim, D. -J., Kim, H. -W., Kim, S. -L., Lee, C. -U., Lee, D. -J., Lee, Y., Park, B. -G., Pogge, R. W., Abe, F., Barry, R., Bennett, D. P., Bhattacharya, A., Donachie, M., Fujii, H., Fukui, A., Hirao, Y., Itow, Y., Kamei, Y., Kondo, Iona, Koshimoto, N., Li, M. C. A., Matsubara, Y., Miyazaki, S., Muraki, Y., Nagakane, M., Ranc, C., Rattenbury, N. J., Suematsu, Harmon, Sullivan, D. J., Sumi, T., Suzuki, Daisuke, Tristram, P. J., Yamakawa, T., Yonehara, A., Fouqué, P., and Zang, W.
Abstract: We report two microlensing planet candidates discovered by the KMTNet survey in $2017$. However, both events have the 2L1S/1L2S degeneracy, which is an obstacle to claiming the discovery of the planets with certainty unless the degeneracy can be resolved. For KMT-2017-BLG-0962, the degeneracy cannot be resolved. If the 2L1S solution is correct, KMT-2017-BLG-0962 might be produced by a super Jupiter-mass planet orbiting a mid-M dwarf host star. For KMT-2017-BLG-1119, the light curve modeling favors the 2L1S solution but higher-resolution observations of the baseline object tend to support the 1L2S interpretation rather than the planetary interpretation. This degeneracy might be resolved by a future measurement of the lens-source relative proper motion. This study shows the problem of resolving 2L1S/1L2S degeneracy exists over a much wider range of conditions than those considered by the theoretical study of Gaudi (1998)., Comment: 15 pages, 12 figures, 4 tables, accepted in AJ
Published: 2019
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10. OGLE-2013-BLG-0911Lb: A Secondary on the Brown-Dwarf Planet Boundary around an M-dwarf

Author: Miyazaki, Shota, Sumi, Takahiro, Bennett, David P., Udalski, Andrzej, Shvartzvald, Yossi, Street, Rachel, Bozza, Valerio, Yee, Jennifer C., Bond, Ian A., Rattenbury, Nicholas, Koshimoto, Naoki, Suzuki, Daisuke, Fukui, Akihiko, Abe, F., Bhattacharya, A., Barry, R., Donachie, M., Fujii, H., Hirao, Y., Itow, Y., Kamei, Y., Kondo, I., Li, M. C. A., Ling, C. H., Matsubara, Y., Matsuo, T., Muraki, Y., Nagakane, M., Ohnishi, K., Ranc, C., Saito, T., Sharan, A., Shibai, H., Suematsu, H., Sullivan, D. J., Tristram, P. J., Yamakawa, T., Yonehara, A., Skowron, J., Poleski, R., Mr'oz, P., Szyma'nski, M. K., Soszy'nski, I., Pietrukowicz, P., KozLowski, S., Ulaczyk, K., Wyrzykowski, L., Friedmann, Matan, Kaspi, Shai, Maoz, Dan, Albrow, M., Christie, G., DePoy, D. L., Gal-Yam, A., Gould, A., Lee, C. -U., Manulis, I., McCormick, J., Natusch, T., Ngan, H., Pogge, R. W., Porritt, I., Tsapras, Y., Bachelet, E., Hundertmark, M. P. G., Dominik, M., Bramich, D. M., Cassan, A., Jaimes, R. Figuera, Horne, K., Schmidt, R., Snodgrass, C., Wambsganss, J., Steele, I. A., Menzies, J., Mao, S., Jorgensen, U. G., Burgdorf, M. J., Ciceri, S., Novati, S. Calchi, D'Ago, G., Evans, D. F., Hinse, T. C., Kains, N., Kerins, E., Korhonen, H., Mancini, L., Popovas, A., Rabus, M., Rahvar, S., Scarpetta, G., Skottfelt, J., Southworth, J., Peixinho, N., Verma, P., Miyazaki, Shota, Sumi, Takahiro, Bennett, David P., Udalski, Andrzej, Shvartzvald, Yossi, Street, Rachel, Bozza, Valerio, Yee, Jennifer C., Bond, Ian A., Rattenbury, Nicholas, Koshimoto, Naoki, Suzuki, Daisuke, Fukui, Akihiko, Abe, F., Bhattacharya, A., Barry, R., Donachie, M., Fujii, H., Hirao, Y., Itow, Y., Kamei, Y., Kondo, I., Li, M. C. A., Ling, C. H., Matsubara, Y., Matsuo, T., Muraki, Y., Nagakane, M., Ohnishi, K., Ranc, C., Saito, T., Sharan, A., Shibai, H., Suematsu, H., Sullivan, D. J., Tristram, P. J., Yamakawa, T., Yonehara, A., Skowron, J., Poleski, R., Mr'oz, P., Szyma'nski, M. K., Soszy'nski, I., Pietrukowicz, P., KozLowski, S., Ulaczyk, K., Wyrzykowski, L., Friedmann, Matan, Kaspi, Shai, Maoz, Dan, Albrow, M., Christie, G., DePoy, D. L., Gal-Yam, A., Gould, A., Lee, C. -U., Manulis, I., McCormick, J., Natusch, T., Ngan, H., Pogge, R. W., Porritt, I., Tsapras, Y., Bachelet, E., Hundertmark, M. P. G., Dominik, M., Bramich, D. M., Cassan, A., Jaimes, R. Figuera, Horne, K., Schmidt, R., Snodgrass, C., Wambsganss, J., Steele, I. A., Menzies, J., Mao, S., Jorgensen, U. G., Burgdorf, M. J., Ciceri, S., Novati, S. Calchi, D'Ago, G., Evans, D. F., Hinse, T. C., Kains, N., Kerins, E., Korhonen, H., Mancini, L., Popovas, A., Rabus, M., Rahvar, S., Scarpetta, G., Skottfelt, J., Southworth, J., Peixinho, N., and Verma, P.
Abstract: We present the analysis of the binary-lens microlensing event OGLE-2013-BLG-0911. The best-fit solutions indicate the binary mass ratio of q~0.03 which differs from that reported in Shvartzvald+2016. The event suffers from the well-known close/wide degeneracy, resulting in two groups of solutions for the projected separation normalized by the Einstein radius of s~0.15 or s~7. The finite source and the parallax observations allow us to measure the lens physical parameters. The lens system is an M-dwarf orbited by a massive Jupiter companion at very close (M_{host}=0.30^{+0.08}_{-0.06} M_{Sun}, M_{comp}=10.1^{+2.9}_{-2.2} M_{Jup}, a_{exp}=0.40^{+0.05}_{-0.04} au) or wide (M_{host}=0.28^{+0.10}_{-0.08} M_{Sun}, M_{comp}=9.9^{+3.8}_{-3.5}M_{Jup}, a_{exp}=18.0^{+3.2}_{-3.2} au) separation. Although the mass ratio is slightly above the planet-brown dwarf (BD) mass-ratio boundary of q=0.03 which is generally used, the median physical mass of the companion is slightly below the planet-BD mass boundary of 13M_{Jup}. It is likely that the formation mechanisms for BDs and planets are different and the objects near the boundaries could have been formed by either mechanism. It is important to probe the distribution of such companions with masses of ~13M_{Jup} in order to statistically constrain the formation theories for both BDs and massive planets. In particular, the microlensing method is able to probe the distribution around low-mass M-dwarfs and even BDs which is challenging for other exoplanet detection methods., Comment: 22 pages, 10 figures, Accepted for publication in The Astronomical Journal
Published: 2019
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11. OGLE-2017-BLG-1186: first application of asteroseismology and Gaussian processes to microlensing

Author: Li, S. -S., Zang, W., Udalski, A., Shvartzvald, Y., Huber, D., Lee, C. -U., Sumi, T., Gould, A., Mao, S., Fouque, P., Wang, T., Dong, S., Jorgensen, U. G., Cole, A., Mroz, P., Szymanski, M. K., Skowron, J., Poleski, R., Soszynski, I., Pietrukowicz, P., Kozlowski, S., Ulaczyk, K., Rybicki, K. A., Iwanek, P., Yee, J. C., Novati, S. Calchi, Beichman, C. A., Bryden, G., Carey, S., Gaudi, B. S., Henderson, C. B., Zhu, W., Albrow, M. D., Chung, S. -J., Han, C., Hwang, K. -H., Jung, Y. K., Ryu, Y. -H., Shin, I. -G., Cha, S. -M., Kim, D. -J., Kim, H. -W., Kim, S. -L., Lee, D. -J., Lee, Y., Park, B. -G., Pogge, R. W., Bond, I. A., Abe, F., Barry, R., Bennett, D. P., Bhattacharya, A., Donachie, M., Fukui, A., Hirao, Y., Itow, Y., Kondo, I., Koshimoto, N., Li, M. C. A., Matsubara, Y., Muraki, Y., Miyazaki, S., Nagakane, M., Ranc, C., Rattenbury, N. J., Suematsu, H., Sullivan, D. J., Suzuki, D., Tristram, P. J., Yonehara, A., Christie, G., Drummond, J., Green, J., Hennerley, S., Natusch, T., Porritt, I., Bachelet, E., Maoz, D., Street, R. A., Tsapras, Y., Bozza, V., Dominik, M., Hundertmark, M., Peixinho, N., Sajadian, S., Burgdorf, M. J., Evans, D. F., Jaimes, R. Figuera, Fujii, Y. I., Haikala, L. K., Helling, C., Henning, T., Hinse, T. C., Mancini, L., Longa-Pena, P., Rahvar, S., Rabus, M., Skottfelt, J., Snodgrass, C., Southworth, J., Unda-Sanzana, E., von Essen, C., Beaulieu, J. -P., Blackman, J., Hill, K., Li, S. -S., Zang, W., Udalski, A., Shvartzvald, Y., Huber, D., Lee, C. -U., Sumi, T., Gould, A., Mao, S., Fouque, P., Wang, T., Dong, S., Jorgensen, U. G., Cole, A., Mroz, P., Szymanski, M. K., Skowron, J., Poleski, R., Soszynski, I., Pietrukowicz, P., Kozlowski, S., Ulaczyk, K., Rybicki, K. A., Iwanek, P., Yee, J. C., Novati, S. Calchi, Beichman, C. A., Bryden, G., Carey, S., Gaudi, B. S., Henderson, C. B., Zhu, W., Albrow, M. D., Chung, S. -J., Han, C., Hwang, K. -H., Jung, Y. K., Ryu, Y. -H., Shin, I. -G., Cha, S. -M., Kim, D. -J., Kim, H. -W., Kim, S. -L., Lee, D. -J., Lee, Y., Park, B. -G., Pogge, R. W., Bond, I. A., Abe, F., Barry, R., Bennett, D. P., Bhattacharya, A., Donachie, M., Fukui, A., Hirao, Y., Itow, Y., Kondo, I., Koshimoto, N., Li, M. C. A., Matsubara, Y., Muraki, Y., Miyazaki, S., Nagakane, M., Ranc, C., Rattenbury, N. J., Suematsu, H., Sullivan, D. J., Suzuki, D., Tristram, P. J., Yonehara, A., Christie, G., Drummond, J., Green, J., Hennerley, S., Natusch, T., Porritt, I., Bachelet, E., Maoz, D., Street, R. A., Tsapras, Y., Bozza, V., Dominik, M., Hundertmark, M., Peixinho, N., Sajadian, S., Burgdorf, M. J., Evans, D. F., Jaimes, R. Figuera, Fujii, Y. I., Haikala, L. K., Helling, C., Henning, T., Hinse, T. C., Mancini, L., Longa-Pena, P., Rahvar, S., Rabus, M., Skottfelt, J., Snodgrass, C., Southworth, J., Unda-Sanzana, E., von Essen, C., Beaulieu, J. -P., Blackman, J., and Hill, K.
Published: 2019

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

Author: 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., Jaimes, R. Figuera, Horne, K., Hundertmark, M., Mao, S., Menzies, J., Ranc, C., Schmidt, R., Snodgrass, C., Steele, I. A., Tsapras, Y., Wambsganss, J., Mroz, P., Soszynski, I., Szymanski, M. K., Skowron, J., Pietrukowicz, P., Kozlowski, S., Poleski, R., Ulaczyk, K., Pawlak, M., 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., 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., Jaimes, R. Figuera, Horne, K., Hundertmark, M., Mao, S., Menzies, J., Ranc, C., Schmidt, R., Snodgrass, C., Steele, I. A., Tsapras, Y., Wambsganss, J., Mroz, P., Soszynski, I., Szymanski, M. K., Skowron, J., Pietrukowicz, P., Kozlowski, S., Poleski, R., Ulaczyk, K., Pawlak, M., 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., and Sullivan, D. J.
Published: 2019

13. OGLE-2017-BLG-1186: first application of asteroseismology and Gaussian processes to microlensing

Author: Li, S. -S., Zang, W., Udalski, A., Shvartzvald, Y., Huber, D., Lee, C. -U., Sumi, T., Gould, A., Mao, S., Fouque, P., Wang, T., Dong, S., Jorgensen, U. G., Cole, A., Mroz, P., Szymanski, M. K., Skowron, J., Poleski, R., Soszynski, I., Pietrukowicz, P., Kozlowski, S., Ulaczyk, K., Rybicki, K. A., Iwanek, P., Yee, J. C., Novati, S. Calchi, Beichman, C. A., Bryden, G., Carey, S., Gaudi, B. S., Henderson, C. B., Zhu, W., Albrow, M. D., Chung, S. -J., Han, C., Hwang, K. -H., Jung, Y. K., Ryu, Y. -H., Shin, I. -G., Cha, S. -M., Kim, D. -J., Kim, H. -W., Kim, S. -L., Lee, D. -J., Lee, Y., Park, B. -G., Pogge, R. W., Bond, I. A., Abe, F., Barry, R., Bennett, D. P., Bhattacharya, A., Donachie, M., Fukui, A., Hirao, Y., Itow, Y., Kondo, I., Koshimoto, N., Li, M. C. A., Matsubara, Y., Muraki, Y., Miyazaki, S., Nagakane, M., Ranc, C., Rattenbury, N. J., Suematsu, H., Sullivan, D. J., Suzuki, D., Tristram, P. J., Yonehara, A., Christie, G., Drummond, J., Green, J., Hennerley, S., Natusch, T., Porritt, I., Bachelet, E., Maoz, D., Street, R. A., Tsapras, Y., Bozza, V., Dominik, M., Hundertmark, M., Peixinho, N., Sajadian, S., Burgdorf, M. J., Evans, D. F., Jaimes, R. Figuera, Fujii, Y. I., Haikala, L. K., Helling, C., Henning, T., Hinse, T. C., Mancini, L., Longa-Pena, P., Rahvar, S., Rabus, M., Skottfelt, J., Snodgrass, C., Southworth, J., Unda-Sanzana, E., von Essen, C., Beaulieu, J. -P., Blackman, J., Hill, K., Li, S. -S., Zang, W., Udalski, A., Shvartzvald, Y., Huber, D., Lee, C. -U., Sumi, T., Gould, A., Mao, S., Fouque, P., Wang, T., Dong, S., Jorgensen, U. G., Cole, A., Mroz, P., Szymanski, M. K., Skowron, J., Poleski, R., Soszynski, I., Pietrukowicz, P., Kozlowski, S., Ulaczyk, K., Rybicki, K. A., Iwanek, P., Yee, J. C., Novati, S. Calchi, Beichman, C. A., Bryden, G., Carey, S., Gaudi, B. S., Henderson, C. B., Zhu, W., Albrow, M. D., Chung, S. -J., Han, C., Hwang, K. -H., Jung, Y. K., Ryu, Y. -H., Shin, I. -G., Cha, S. -M., Kim, D. -J., Kim, H. -W., Kim, S. -L., Lee, D. -J., Lee, Y., Park, B. -G., Pogge, R. W., Bond, I. A., Abe, F., Barry, R., Bennett, D. P., Bhattacharya, A., Donachie, M., Fukui, A., Hirao, Y., Itow, Y., Kondo, I., Koshimoto, N., Li, M. C. A., Matsubara, Y., Muraki, Y., Miyazaki, S., Nagakane, M., Ranc, C., Rattenbury, N. J., Suematsu, H., Sullivan, D. J., Suzuki, D., Tristram, P. J., Yonehara, A., Christie, G., Drummond, J., Green, J., Hennerley, S., Natusch, T., Porritt, I., Bachelet, E., Maoz, D., Street, R. A., Tsapras, Y., Bozza, V., Dominik, M., Hundertmark, M., Peixinho, N., Sajadian, S., Burgdorf, M. J., Evans, D. F., Jaimes, R. Figuera, Fujii, Y. I., Haikala, L. K., Helling, C., Henning, T., Hinse, T. C., Mancini, L., Longa-Pena, P., Rahvar, S., Rabus, M., Skottfelt, J., Snodgrass, C., Southworth, J., Unda-Sanzana, E., von Essen, C., Beaulieu, J. -P., Blackman, J., and Hill, K.
Published: 2019

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

Author: 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., Jaimes, R. Figuera, Horne, K., Hundertmark, M., Mao, S., Menzies, J., Ranc, C., Schmidt, R., Snodgrass, C., Steele, I. A., Tsapras, Y., Wambsganss, J., Mroz, P., Soszynski, I., Szymanski, M. K., Skowron, J., Pietrukowicz, P., Kozlowski, S., Poleski, R., Ulaczyk, K., Pawlak, M., 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., 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., Jaimes, R. Figuera, Horne, K., Hundertmark, M., Mao, S., Menzies, J., Ranc, C., Schmidt, R., Snodgrass, C., Steele, I. A., Tsapras, Y., Wambsganss, J., Mroz, P., Soszynski, I., Szymanski, M. K., Skowron, J., Pietrukowicz, P., Kozlowski, S., Poleski, R., Ulaczyk, K., Pawlak, M., 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., and Sullivan, D. J.
Published: 2019

15. OGLE-2016-BLG-1190Lb : The First Spitzer Bulge Planet Lies Near the Planet/Brown-dwarf Boundary

Author: Ryu, Y. -H., Yee, J. C., Udalski, A., Bond, I. A., Shvartzvald, Y., Zang, W., Jaimes, R. Figuera, Jorgensen, U. G., Zhu, W., Huang, C. X., Jung, Y. K., Albrow, M. D., Chung, S. -J., Gould, A., Han, C., Hwang, K. -H., Shin, I. -G., Cha, S. -M., Kim, D. -J., Kim, H. -W., Kim, S. -L., Lee, C. -U., Lee, D. -J., Lee, Y., Park, B. -G., Pogge, R. W., Novati, S. Calchi, Carey, S., Henderson, C. B., Beichman, C., Gaudi, B. S., Mroz, P., Poleski, R., Skowron, J., Szymanski, M. K., Soszynski, I., Kozlowski, S., Pietrukowicz, P., Ulaczyk, K., Pawlak, M., Abe, F., Asakura, Y., Barry, R., Bennett, D. P., Bhattacharya, A., Donachie, M., Evans, P., Fukui, A., Hirao, Y., Itow, Y., Kawasaki, K., Koshimoto, N., Li, M. C. A., Ling, C. H., Masuda, K., Matsubara, Y., Miyazaki, S., Muraki, Y., Nagakane, M., Ohnishi, K., Ranc, C., Rattenbury, N. J., Saito, To, Sharan, A., Sullivan, D. J., Sumi, T., Suzuki, D., Tristram, P. J., Yamada, T., Yonehara, A., Bryden, G., Howell, S. B., Jacklin, S., Penny, M. T., Mao, S., Fouque, Pascal, Wang, T., Street, R. A., Tsapras, Y., Hundertmark, M., Bachelet, E., Dominik, M., Li, Z., Cross, S., Cassan, A., Horne, K., Schmidt, R., Wambsganss, J., Ment, S. K., Maoz, D., Snodgrass, C., Steele, I. A., Bozza, V., Burgdorf, M. J., Ciceri, Simona, D'Ago, G., Evans, D. F., Hinse, T. C., Kerins, E., Kokotanekova, R., Longa, P., MacKenzie, J., Popovas, A., Rabus, M., Rahvar, S., Sajadian, S., Skottfelt, J., Southworth, J., von Essen, C., Ryu, Y. -H., Yee, J. C., Udalski, A., Bond, I. A., Shvartzvald, Y., Zang, W., Jaimes, R. Figuera, Jorgensen, U. G., Zhu, W., Huang, C. X., Jung, Y. K., Albrow, M. D., Chung, S. -J., Gould, A., Han, C., Hwang, K. -H., Shin, I. -G., Cha, S. -M., Kim, D. -J., Kim, H. -W., Kim, S. -L., Lee, C. -U., Lee, D. -J., Lee, Y., Park, B. -G., Pogge, R. W., Novati, S. Calchi, Carey, S., Henderson, C. B., Beichman, C., Gaudi, B. S., Mroz, P., Poleski, R., Skowron, J., Szymanski, M. K., Soszynski, I., Kozlowski, S., Pietrukowicz, P., Ulaczyk, K., Pawlak, M., Abe, F., Asakura, Y., Barry, R., Bennett, D. P., Bhattacharya, A., Donachie, M., Evans, P., Fukui, A., Hirao, Y., Itow, Y., Kawasaki, K., Koshimoto, N., Li, M. C. A., Ling, C. H., Masuda, K., Matsubara, Y., Miyazaki, S., Muraki, Y., Nagakane, M., Ohnishi, K., Ranc, C., Rattenbury, N. J., Saito, To, Sharan, A., Sullivan, D. J., Sumi, T., Suzuki, D., Tristram, P. J., Yamada, T., Yonehara, A., Bryden, G., Howell, S. B., Jacklin, S., Penny, M. T., Mao, S., Fouque, Pascal, Wang, T., Street, R. A., Tsapras, Y., Hundertmark, M., Bachelet, E., Dominik, M., Li, Z., Cross, S., Cassan, A., Horne, K., Schmidt, R., Wambsganss, J., Ment, S. K., Maoz, D., Snodgrass, C., Steele, I. A., Bozza, V., Burgdorf, M. J., Ciceri, Simona, D'Ago, G., Evans, D. F., Hinse, T. C., Kerins, E., Kokotanekova, R., Longa, P., MacKenzie, J., Popovas, A., Rabus, M., Rahvar, S., Sajadian, S., Skottfelt, J., Southworth, J., and von Essen, C.
Abstract: We report the discovery of OGLE-2016-BLG-1190Lb, which is likely to be the first Spitzer microlensing planet in the Galactic bulge/ bar, an assignation that can be confirmed by two epochs of high-resolution imaging of the combined source-lens baseline object. The planet's mass, M-p = 13.4 +/- 0.9 M-J, places it right at the deuteriumburning limit, i. e., the conventional boundary between planets and brown dwarfs. Its existence raises the question of whether such objects are really planets (formed within the disks of their hosts) or failed stars (lowmass objects formed by gas fragmentation). This question may ultimately be addressed by comparing disk and bulge/bar planets, which is a goal of the Spitzer microlens program. The host is a G dwarf, M-host = 0.89. +/- 0.07 M-circle dot, and the planet has a semimajor axis a similar to 2.0 au. We use Kepler K2 Campaign 9 microlensing data to break the lens-mass degeneracy that generically impacts parallax solutions from Earth-Spitzer observations alone, which is the first successful application of this approach. The microlensing data, derived primarily from near-continuous, ultradense survey observations from OGLE, MOA, and three KMTNet telescopes, contain more orbital information than for any previous microlensing planet, but not quite enough to accurately specify the full orbit. However, these data do permit the first rigorous test of microlensing orbital-motion measurements, which are typically derived from data taken over < 1% of an orbital period.
Published: 2018
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16. Unique Science from a Coordinated LSST-WFIRST Survey of the Galactic Bulge

Author: Street, R. A., Lund, M. B., Donachie, M., Khakpash, S., Golovich, N., Penny, M., Bennett, D., Dawson, W. A., Pepper, J., Rabus, M., Szkody, P., Clarkson, W. I., Di Stefano, R., Rattenbury, N., Hundertmark, M. P. G., Tsapras, Y., Ridgway, S., Stassun, K., Bozza, V., Bhattacharya, A., Novati, S. Calchi, Shvartzvald, Y., Street, R. A., Lund, M. B., Donachie, M., Khakpash, S., Golovich, N., Penny, M., Bennett, D., Dawson, W. A., Pepper, J., Rabus, M., Szkody, P., Clarkson, W. I., Di Stefano, R., Rattenbury, N., Hundertmark, M. P. G., Tsapras, Y., Ridgway, S., Stassun, K., Bozza, V., Bhattacharya, A., Novati, S. Calchi, and Shvartzvald, Y.
Abstract: NASA's WFIRST mission will perform a wide-field, NIR survey of the Galactic Bulge to search for exoplanets via the microlensing techniques. As the mission is due to launch in the mid-2020s, around half-way through the LSST Main Survey, we have a unique opportunity to explore synergistic science from two landmark programs. LSST can survey the entire footprint of the WFIRST microlensing survey in a single Deep Drilling Field. Here we explore the great scientific potential of this proposal and recommend the most effective observing strategies., Comment: White Paper submitted to the 2018 call for LSST cadence proposals. arXiv admin note: text overlap with arXiv:1812.03137
Published: 2018

17. Two new free-floating or wide-orbit planets from microlensing

Author: Mroz, P., Udalski, A., Bennett, D. P., Ryu, Y. -H., Sumi, T., Shvartzvald, Y., Skowron, J., Poleski, R., Pietrukowicz, P., Kozlowski, S., Szymanski, M. K., Wyrzykowski, L., Soszynski, I., Ulaczyk, K., Rybicki, K., Iwanek, P., Albrow, M. D., Chung, S. -J., Gould, A., Han, C., Hwang, K. -H., Jung, Y. K., Shin, I. -G., Yee, J. C., Zang, W., Cha, S. -M., Kim, D. -J., Kim, H. -W., Kim, S. -L., Lee, C. -U., Lee, D. -J., Lee, Y., Park, B. -G., Pogge, R. W., Abe, F., Barry, R., Bhattacharya, A., Bond, I. A., Donachie, M., Fukui, A., Hirao, Y., Itow, Y., Kawasaki, K., Kondo, I., Koshimoto, N., Li, M. C. A., Matsubara, Y., Muraki, Y., Miyazaki, S., Nagakane, M., Ranc, C., Rattenbury, N. J., Suematsu, H., Sullivan, D. J., Suzuki, D., Tristram, P. J., Yonehara, A., Maoz, D., Kaspi, S., Friedmann, M., Mroz, P., Udalski, A., Bennett, D. P., Ryu, Y. -H., Sumi, T., Shvartzvald, Y., Skowron, J., Poleski, R., Pietrukowicz, P., Kozlowski, S., Szymanski, M. K., Wyrzykowski, L., Soszynski, I., Ulaczyk, K., Rybicki, K., Iwanek, P., Albrow, M. D., Chung, S. -J., Gould, A., Han, C., Hwang, K. -H., Jung, Y. K., Shin, I. -G., Yee, J. C., Zang, W., Cha, S. -M., Kim, D. -J., Kim, H. -W., Kim, S. -L., Lee, C. -U., Lee, D. -J., Lee, Y., Park, B. -G., Pogge, R. W., Abe, F., Barry, R., Bhattacharya, A., Bond, I. A., Donachie, M., Fukui, A., Hirao, Y., Itow, Y., Kawasaki, K., Kondo, I., Koshimoto, N., Li, M. C. A., Matsubara, Y., Muraki, Y., Miyazaki, S., Nagakane, M., Ranc, C., Rattenbury, N. J., Suematsu, H., Sullivan, D. J., Suzuki, D., Tristram, P. J., Yonehara, A., Maoz, D., Kaspi, S., and Friedmann, M.
Abstract: Planet formation theories predict the existence of free-floating planets that have been ejected from their parent systems. Although they emit little or no light, they can be detected during gravitational microlensing events. Microlensing events caused by rogue planets are characterized by very short timescales $t_{\rm E}$ (typically below two days) and small angular Einstein radii $\theta_{\rm E}$ (up to several uas). Here we present the discovery and characterization of two ultra-short microlensing events identified in data from the Optical Gravitational Lensing Experiment (OGLE) survey, which may have been caused by free-floating or wide-orbit planets. OGLE-2012-BLG-1323 is one of the shortest events discovered thus far ($t_{\rm E}$=0.155 +/- 0.005 d, $\theta_{\rm E}$=2.37 +/- 0.10 uas) and was caused by an Earth-mass object in the Galactic disk or a Neptune-mass planet in the Galactic bulge. OGLE-2017-BLG-0560 ($t_{\rm E}$=0.905 +/- 0.005 d, $\theta_{\rm E}$=38.7 +/- 1.6 uas) was caused by a Jupiter-mass planet in the Galactic disk or a brown dwarf in the bulge. We rule out stellar companions up to a distance of 6.0 and 3.9 au, respectively. We suggest that the lensing objects, whether located on very wide orbits or free-floating, may originate from the same physical mechanism. Although the sample of ultrashort microlensing events is small, these detections are consistent with low-mass wide-orbit or unbound planets being more common than stars in the Milky Way., Comment: accepted for publication in A&A, minor changes
Published: 2018
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18. The Diverse Science Return from a Wide-Area Survey of the Galactic Plane

Author: Street, R. A., Lund, M. B., Khakpash, S., Donachie, M., Dawson, W. A., Golovich, N., Wyrzykowski, L., Szkody, P., Naylor, T., Penny, M., Rattenbury, N., Dall'Ora, M., Clarkson, W. I., Bennett, D., Pepper, J., Rabus, M., Hundertmark, M. P. G., Tsapras, Y., Di Stefano, R., Ridgway, S., Liu, M., Lin, E., Street, R. A., Lund, M. B., Khakpash, S., Donachie, M., Dawson, W. A., Golovich, N., Wyrzykowski, L., Szkody, P., Naylor, T., Penny, M., Rattenbury, N., Dall'Ora, M., Clarkson, W. I., Bennett, D., Pepper, J., Rabus, M., Hundertmark, M. P. G., Tsapras, Y., Di Stefano, R., Ridgway, S., Liu, M., and Lin, E.
Abstract: The overwhelming majority of objects visible to LSST lie within the Galactic Plane. Though many previous surveys have avoided this region for fear of stellar crowding, LSST's spatial resolution combined with its state-of-the-art Difference Image Analysis mean that it can conduct a high cadence survey of most of the Galaxy for the first time. Here we outline the many areas of science that would greatly benefit from an LSST survey that included the Galactic Plane, Magellanic Clouds and Bulge at a cadence of 2-3 d. Particular highlights include measuring the mass spectrum of black holes, and mapping the population of exoplanets in the Galaxy in relation to variations in star forming environments. But the same survey data will provide a goldmine for a wide range of science, and we explore possible survey strategies which maximize the scientific return for a number of fields including young stellar objects, cataclysmic variables and Neptune Trojans., Comment: White Paper submitted in response to the 2018 call for LSST cadence proposals
Published: 2018

19. First assessment of the binary lens OGLE-2015_BLG-0232

Author: Bachelet, E., Bozza, V., Han, C., Udalski, A., Bond, I. A., Beaulieu, J. -P., Street, R. A., Kim, J. -I, Bramich, D. M., Cassan, A., Dominik, M., Jaimes, R. Figuera, Horne, K., Hundertmark, M., Mao, S., Menzies, J., Ranc, C., Schmidt, R., Snodgrass, C., Steele, I. A., Tsapras, Y., Wambsganss, J., Mróz, P., Soszyński, I., Szymański, M. K., Skowron, J., Pietrukowicz, P., Kozłowski, S., Poleski, R., Ulaczyk, K., Pawlak, M., 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., Bachelet, E., Bozza, V., Han, C., Udalski, A., Bond, I. A., Beaulieu, J. -P., Street, R. A., Kim, J. -I, Bramich, D. M., Cassan, A., Dominik, M., Jaimes, R. Figuera, Horne, K., Hundertmark, M., Mao, S., Menzies, J., Ranc, C., Schmidt, R., Snodgrass, C., Steele, I. A., Tsapras, Y., Wambsganss, J., Mróz, P., Soszyński, I., Szymański, M. K., Skowron, J., Pietrukowicz, P., Kozłowski, S., Poleski, R., Ulaczyk, K., Pawlak, M., 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., and Yonehara, A.
Abstract: 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., Comment: Accepted in ApJ
Published: 2018
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20. OGLE-2017-BLG-0039: Microlensing Event with Light from the Lens Identified from Mass Measurement

Author: Han, C., Jung, Y. K., Udalski, A., Bond, I., Bozza, V., Albrow, M. D., Chung, S. -J., Gould, A., Hwang, K. -H., Kim, D., Lee, C. -U., Kim, H. -W., Ryu, Y. -H., Shin, I. -G., Yee, J. C., Shvartzvald, Y., Cha, S. -M., Kim, S. -L., Kim, D. -J., Lee, D. -J., Lee, Y., Park, B. -G., Pogge, R. W., Szymański, M. K., Mróz, P., Skowron, J., Poleski, R., Soszyński, I., Kozłowski, S., Pietrukowicz, P., Ulaczyk, K., Pawlak, M., Abe, F., Barry, R., Bennett, D. P., Bhattacharya, A., Donachie, M., Evans, P., Fukui, A., Hirao, Y., Itow, Y., Kawasaki, K., Koshimoto, N., Li, M. C. A., Ling, C. H., Matsubara, Y., Miyazaki, S., Munakata, H., Muraki, Y., Nagakane, M., Ohnishi, K., Ranc, C., Rattenbury, N., Saito, T., Sharan, A., Sullivan, D. J., Sumi, T., Suzuki, D., Tristram, P. J., Yamada, T., Yonehara, A., Han, C., Jung, Y. K., Udalski, A., Bond, I., Bozza, V., Albrow, M. D., Chung, S. -J., Gould, A., Hwang, K. -H., Kim, D., Lee, C. -U., Kim, H. -W., Ryu, Y. -H., Shin, I. -G., Yee, J. C., Shvartzvald, Y., Cha, S. -M., Kim, S. -L., Kim, D. -J., Lee, D. -J., Lee, Y., Park, B. -G., Pogge, R. W., Szymański, M. K., Mróz, P., Skowron, J., Poleski, R., Soszyński, I., Kozłowski, S., Pietrukowicz, P., Ulaczyk, K., Pawlak, M., Abe, F., Barry, R., Bennett, D. P., Bhattacharya, A., Donachie, M., Evans, P., Fukui, A., Hirao, Y., Itow, Y., Kawasaki, K., Koshimoto, N., Li, M. C. A., Ling, C. H., Matsubara, Y., Miyazaki, S., Munakata, H., Muraki, Y., Nagakane, M., Ohnishi, K., Ranc, C., Rattenbury, N., Saito, T., Sharan, A., Sullivan, D. J., Sumi, T., Suzuki, D., Tristram, P. J., Yamada, T., and Yonehara, A.
Abstract: We present the analysis of the caustic-crossing binary microlensing event OGLE-2017-BLG-0039. Thanks to the very long duration of the event, with an event time scale $t_{\rm E}\sim 130$ days, the microlens parallax is precisely measured despite its small value of $\pie\sim 0.06$. The analysis of the well-resolved caustic crossings during both the source star's entrance and exit of the caustic yields the angular Einstein radius $\thetae\sim 0.6$~mas. The measured $\pie$ and $\thetae$ indicate that the lens is a binary composed of two stars with masses $\sim 1.0~M_\odot$ and $\sim 0.15~M_\odot$, and it is located at a distance of $\sim 6$ kpc. From the color and brightness of the lens estimated from the determined lens mass and distance, it is expected that $\sim 2/3$ of the $I$-band blended flux comes from the lens. Therefore, the event is a rare case of a bright lens event for which high-resolution follow-up observations can confirm the nature of the lens., Comment: 8 pages, 6 figures, 5 tables
Published: 2018
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21. A Likely Detection of a Two-Planet System in a Low Magnification Microlensing Event

Author: Suzuki, D., Bennett, D. P., Udalski, A., Bond, I. A., Sumi, T., Han, C., Abe, F., Asakura, Y., Barry, R. K., Bhattacharya, A., Donachie, M., Freeman, M., Fukui, A., Hirao, Y., Itow, Y., Koshimoto, N., Li, M. C. A., Ling, C. H., Masuda, K., Matsubara, Y., Muraki, Y., Nagakane, M., Onishi, K., Oyokawa, H., Ranc, C., Rattenbury, N. J., Saito, To., Sharan, A., Sullivan, D. J., Tristram, P. J., Yonehara, A., Poleski, R., Mróz, P., Skowron, J., Szymański, M. K., Soszyński, I., Kozłowski, S., Pietrukowicz, P., Wyrzykowski, Ł., Ulaczyk, K., Suzuki, D., Bennett, D. P., Udalski, A., Bond, I. A., Sumi, T., Han, C., Abe, F., Asakura, Y., Barry, R. K., Bhattacharya, A., Donachie, M., Freeman, M., Fukui, A., Hirao, Y., Itow, Y., Koshimoto, N., Li, M. C. A., Ling, C. H., Masuda, K., Matsubara, Y., Muraki, Y., Nagakane, M., Onishi, K., Oyokawa, H., Ranc, C., Rattenbury, N. J., Saito, To., Sharan, A., Sullivan, D. J., Tristram, P. J., Yonehara, A., Poleski, R., Mróz, P., Skowron, J., Szymański, M. K., Soszyński, I., Kozłowski, S., Pietrukowicz, P., Wyrzykowski, Ł., and Ulaczyk, K.
Abstract: We report on the analysis of a microlensing event OGLE-2014-BLG-1722 that showed two distinct short term anomalies. The best fit model to the observed light curves shows that the two anomalies are explained with two planetary mass ratio companions to the primary lens. Although a binary source model is also able to explain the second anomaly, it is marginally ruled out by 3.1 $\sigma$. The 2-planet model indicates that the first anomaly was caused by planet "b" with a mass ratio of $q = (4.5_{-0.6}^{+0.7}) \times 10^{-4}$ and projected separation in unit of the Einstein radius, $s = 0.753 \pm 0.004$. The second anomaly reveals planet "c" with a mass ratio of $q_{2} = (7.0_{-1.7}^{+2.3}) \times 10^{-4}$ with $\Delta \chi^{2} \sim 170$ compared to the single planet model. Its separation has a so-called close-wide degeneracy. We estimated the physical parameters of the lens system from Bayesian analysis. This gives that the masses of planet b and c are $m_{\rm b} = 56_{-33}^{+51}\,M_{\oplus}$ and $m_{\rm c} = 85_{-51}^{+86}\,M_{\oplus}$, respectively, and they orbit a late type star with a mass of $M_{\rm host} = 0.40_{-0.24}^{+0.36}\,M_{\odot}$ located at $D_{\rm L} = 6.4_{-1.8}^{+1.3}\,\rm kpc$ from us. If the 2-planet model is true, this is the third multiple planet system detected by using the microlensing method, and the first multiple planet system detected in the low magnification events, which are dominant in the microlensing survey data. The occurrence rate of multiple cold gas giant systems is estimated using the two such detections and a simple extrapolation of the survey sensitivity of 6 year MOA microlensing survey (Suzuki et al. 2016) combined with the 4 year $\mu$FUN detection efficiency (Gould et al. 2010). It is estimated that $6 \pm 2\,\%$ of stars host two cold giant planets., Comment: Submitted to AAS
Published: 2018
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22. MOA-2015-BLG-337: A Planetary System with a Low-mass Brown Dwarf/Planetary Boundary Host, or a Brown Dwarf Binary

Author: Miyazaki, S., Sumi, T., Bennett, D. P., Gould, A., Udalski, A., Bond, I. A., Koshimoto, N., Nagakane, M., Rattenbury, N., Abe, F., Bhattacharya, A., Barry, R., Donachie, M., Fukui, A., Hirao, Y., Itow, Y., Kawasaki, K., Li, M. C., Ling, C. H., Matsubara, Y., Matsuo, T., Muraki, Y., Ohnishi, K., Ranc, C., Saito, T., Sharan, A., Shibai, H., Suematsu, H., Suzuki, D., Sullivan, D. J., Tristram, P. J., Yamada, T., Yonehara, A., owski, S., Mr'oz, P., Pawlak, M., Poleski, R., Pietrukowicz, P., Skowron, J., Soszy'nski, I., Szyma'nski, M. K., Ulaczyk, K., Albrow, M. D., Chung, S. -J., Han, C., Jung, Y. K., Hwang, K. -H., Ryu, Y. -H., Shin, I. -G., Shvartzvald, Y., Yee, J. C., Zang, W., Zhu, W., Cha, S. -M., Kim, D. -J., Kim, H. -W., Kim, S. -L., Lee, C. -U., Lee, D. -J., Lee, Y., Park, B. -G., Pogge, R. W., Miyazaki, S., Sumi, T., Bennett, D. P., Gould, A., Udalski, A., Bond, I. A., Koshimoto, N., Nagakane, M., Rattenbury, N., Abe, F., Bhattacharya, A., Barry, R., Donachie, M., Fukui, A., Hirao, Y., Itow, Y., Kawasaki, K., Li, M. C., Ling, C. H., Matsubara, Y., Matsuo, T., Muraki, Y., Ohnishi, K., Ranc, C., Saito, T., Sharan, A., Shibai, H., Suematsu, H., Suzuki, D., Sullivan, D. J., Tristram, P. J., Yamada, T., Yonehara, A., owski, S., Mr'oz, P., Pawlak, M., Poleski, R., Pietrukowicz, P., Skowron, J., Soszy'nski, I., Szyma'nski, M. K., Ulaczyk, K., Albrow, M. D., Chung, S. -J., Han, C., Jung, Y. K., Hwang, K. -H., Ryu, Y. -H., Shin, I. -G., Shvartzvald, Y., Yee, J. C., Zang, W., Zhu, W., Cha, S. -M., Kim, D. -J., Kim, H. -W., Kim, S. -L., Lee, C. -U., Lee, D. -J., Lee, Y., Park, B. -G., and Pogge, R. W.
Abstract: We report the discovery and the analysis of the short timescale binary-lens microlensing event, MOA-2015-BLG-337. The lens system could be a planetary system with a very low mass host, around the brown dwarf/planetary mass boundary, or a brown dwarf binary. We found two competing models that explain the observed light curves with companion/host mass ratios of q~0.01 and ~0.17, respectively. From the measurement of finite source effects in the best-fit planetary model, we find a relatively small angular Einstein radius of theta_E ~ 0.03 mas which favors a low mass lens. We conduct a Bayesian analysis to obtain the probability distribution of the lens properties. The results for the planetary models strongly depend on the minimum mass, M_min, in the assumed mass function. In summary, there are two solutions of the lens system: (1) a brown dwarf/planetary mass boundary object orbited by a super-Neptune (the planetary model with M_min=0.001 M_sun) and (2) a brown dwarf binary (the binary model). If the planetary models is correct, this system can be one of a new class of planetary system, having a low host mass and also a planetary mass ratio (q <0.03) between the host and its companion. The discovery of the event is important for the study of planetary formation in very low mass objects. In addition, it is important to consider all viable solutions in these kinds of ambiguous events in order for the future comprehensive statistical analyses of planetary/binary microlensing events., Comment: 17 pages, 7 figures, Accepted for publication in AJ
Published: 2018
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23. A study of light travel time effect in short-period MOA eclipsing binaries via eclipse timing

Author: Li, M. C. A., Rattenbury, N. J., Bond, I. A., Sumi, T., Bennett, D. P., Koshimoto, N., Abe, F., Asakura, Y., Barry, R., Bhattacharya, A., Donachie, M., Evans, P., Fukui, A., Hirao, Y., Itow, Y., Masuda, K., Matsubara, Y., Muraki, Y., Nagakane, M., Ohnishi, K., Saito, To., Sharan, A., Sullivan, D. J., Suzuki, D., Tristram, P. J., Yonehara, A., Li, M. C. A., Rattenbury, N. J., Bond, I. A., Sumi, T., Bennett, D. P., Koshimoto, N., Abe, F., Asakura, Y., Barry, R., Bhattacharya, A., Donachie, M., Evans, P., Fukui, A., Hirao, Y., Itow, Y., Masuda, K., Matsubara, Y., Muraki, Y., Nagakane, M., Ohnishi, K., Saito, To., Sharan, A., Sullivan, D. J., Suzuki, D., Tristram, P. J., and Yonehara, A.
Abstract: A sample of 542 eclipsing binaries (EBs) with periods shorter than 2 d were selected from the Microlensing Observations in Astrophysics (MOA) EB catalogue (Li et al. 2017) for eclipse-time variation analysis. For this sample we were able to obtain the time series from MOA-II that span 9.5yr. We discovered 91 EBs, out of the 542 EBs, with detected light-travel-time effect signals suggesting the presence of tertiary companions of orbiting periods from 250 d-28 yr. The frequency of EBs with tertiary companions in our sample increases as the period decreases and reaches a value of 0.65 for contact binaries with periods shorter than 0.3 d. If only the contact binaries of periods < 0.26d are considered, the frequency even goes to the unit. Our results suggest that contact binaries with periods close to the 0.22-d contact binary limit are commonly accompanied by relatively close tertiary companions., Comment: 22 pages, 17 figures, MNRAS accepted
Published: 2018
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24. OGLE-2017-BLG-0482Lb: A Microlensing Super-Earth Orbiting a Low-mass Host Star

Author: Han, C., Hirao, Y., Udalski, A., Lee, C. -U., Bozza, V., Gould, A., Abe, F., Barry, R., Bond, I. A., Bennett, D. P., Bhattacharya, A., Donachie, M., Evans, P., Fukui, A., Itow, Y., Kawasaki, K., Koshimoto, N., Li, M. C. A., Ling, C. H., Matsubara, Y., Miyazaki, S., Munakata, H., Muraki, Y., Nagakane, M., Ohnishi, K., Ranc, C., Rattenbury, N., Saito, T., Sharan, A., Sullivan, D. J., Sumi, T., Suzuki, D., Tristram, P. J., Yamada, T., Yonehara, A., Mróz, P., Poleski, R., Kozłowski, S., Soszyński, I., Pietrukowicz, P., Skowron, J., Szymańsk, M. K., Ulaczyk, K., Pawlak, M., Rybicki, K., Iwanek, P., Albrow, M. D., Chung, S. -J., Hwang, K. -H., Jung, Y. K., Kim, D., Kim, W. -T., Kim, H. -W., Ryu, Y. -H., Shin, I. -G., Shvartzvald, Y., Yee, J. C., Zhu, W., Cha, S. -M., Kim, S. -L., Kim, D. -J., Lee, D. -J., Lee, Y., Park, B. -G., Pogge, R. W., Han, C., Hirao, Y., Udalski, A., Lee, C. -U., Bozza, V., Gould, A., Abe, F., Barry, R., Bond, I. A., Bennett, D. P., Bhattacharya, A., Donachie, M., Evans, P., Fukui, A., Itow, Y., Kawasaki, K., Koshimoto, N., Li, M. C. A., Ling, C. H., Matsubara, Y., Miyazaki, S., Munakata, H., Muraki, Y., Nagakane, M., Ohnishi, K., Ranc, C., Rattenbury, N., Saito, T., Sharan, A., Sullivan, D. J., Sumi, T., Suzuki, D., Tristram, P. J., Yamada, T., Yonehara, A., Mróz, P., Poleski, R., Kozłowski, S., Soszyński, I., Pietrukowicz, P., Skowron, J., Szymańsk, M. K., Ulaczyk, K., Pawlak, M., Rybicki, K., Iwanek, P., Albrow, M. D., Chung, S. -J., Hwang, K. -H., Jung, Y. K., Kim, D., Kim, W. -T., Kim, H. -W., Ryu, Y. -H., Shin, I. -G., Shvartzvald, Y., Yee, J. C., Zhu, W., Cha, S. -M., Kim, S. -L., Kim, D. -J., Lee, D. -J., Lee, Y., Park, B. -G., and Pogge, R. W.
Abstract: We report the discovery of a planetary system in which a super-earth orbits a late M-dwarf host. The planetary system was found from the analysis of the microlensing event OGLE-2017-BLG-0482, wherein the planet signal appears as a short-term anomaly to the smooth lensing light curve produced by the host. Despite its weak signal and short duration, the planetary signal was firmly detected from the dense and continuous coverage by three microlensing surveys. We find a planet/host mass ratio of $q\sim 1.4\times 10^{-4}$. We measure the microlens parallax $\pi_{\rm E}$ from the long-term deviation in the observed lensing light curve, but the angular Einstein radius $\theta_{\rm E}$ cannot be measured because the source trajectory did not cross the planet-induced caustic. Using the measured event timescale and the microlens parallax, we find that the masses of the planet and the host are $M_{\rm p}=9.0_{-4.5}^{+9.0}\ M_\oplus$ and $M_{\rm host}=0.20_{-0.10}^{+0.20}\ M_\odot$, respectively, and the projected separation between them is $a_\perp=1.8_{-0.7}^{+0.6}$ au. The estimated distance to the lens is $D_{\rm L}=5.8_{-2.1}^{+1.8}$ kpc. The discovery of the planetary system demonstrates that microlensing provides an important method to detect low-mass planets orbiting low-mass stars., Comment: 10 pages, 10 figures, 2 tables
Published: 2018
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25. OGLE-2014-BLG-0289: Precise Characterization of a Quintuple-Peak Gravitational Microlensing Event

Author: Udalski, A., Han, C., Bozza, V., Gould, A., Bond, I. A., Mróz, P., Skowron, J., Wyrzykowski, Ł., Szymański, M. K., Soszyński, I., Ulaczyk, K., Poleski, R., Pietrukowicz, P., Kozłowski, S., Abe, F., Barry, R., Bennett, D. P., Bhattacharya, A., Donachie, M., Evans, P., Fukui, A., Hirao, Y., Itow, Y., Kawasaki, K., Koshimoto, N., Li, M. C. A., Ling, C. H., Masuda, K., Matsubara, Y., Miyazaki, S., Munakata, H., Muraki, Y., Nagakane, M., Ohnishi, K., Ranc, C., Rattenbury, N., Saito, T., Sharan, A., Sullivan, D. J., Sumi, T., Suzuki, D., Tristram, P. J., Yamada, T., Yonehara, A., Bachelet, E., Bramich, D. M., DÁgo, G., Dominik, M., Jaimes, R. Figuera, Horne, K., Hundertmark, M., Kains, N., Menzies, J., Schmidt, R., Snodgrass, C., Steele, I. A., Wambsganss, J., Pogge, R. W., Jung, Y. K., Shin, I. -G., Yee, J. C., Kim, W. -T., Beichman, C., Carey, S., Novati, S. Calchi, Zhu, W., Udalski, A., Han, C., Bozza, V., Gould, A., Bond, I. A., Mróz, P., Skowron, J., Wyrzykowski, Ł., Szymański, M. K., Soszyński, I., Ulaczyk, K., Poleski, R., Pietrukowicz, P., Kozłowski, S., Abe, F., Barry, R., Bennett, D. P., Bhattacharya, A., Donachie, M., Evans, P., Fukui, A., Hirao, Y., Itow, Y., Kawasaki, K., Koshimoto, N., Li, M. C. A., Ling, C. H., Masuda, K., Matsubara, Y., Miyazaki, S., Munakata, H., Muraki, Y., Nagakane, M., Ohnishi, K., Ranc, C., Rattenbury, N., Saito, T., Sharan, A., Sullivan, D. J., Sumi, T., Suzuki, D., Tristram, P. J., Yamada, T., Yonehara, A., Bachelet, E., Bramich, D. M., DÁgo, G., Dominik, M., Jaimes, R. Figuera, Horne, K., Hundertmark, M., Kains, N., Menzies, J., Schmidt, R., Snodgrass, C., Steele, I. A., Wambsganss, J., Pogge, R. W., Jung, Y. K., Shin, I. -G., Yee, J. C., Kim, W. -T., Beichman, C., Carey, S., Novati, S. Calchi, and Zhu, W.
Abstract: We present the analysis of the binary-microlensing event OGLE-2014-BLG-0289. The event light curve exhibits very unusual five peaks where four peaks were produced by caustic crossings and the other peak was produced by a cusp approach. It is found that the quintuple-peak features of the light curve provide tight constraints on the source trajectory, enabling us to precisely and accurately measure the microlensing parallax $\pi_{\rm E}$. Furthermore, the three resolved caustics allow us to measure the angular Einstein radius $\thetae$. From the combination of $\pi_{\rm E}$ and $\thetae$, the physical lens parameters are uniquely determined. It is found that the lens is a binary composed of two M dwarfs with masses $M_1 = 0.52 \pm 0.04\ M_\odot$ and $M_2=0.42 \pm 0.03\ M_\odot$ separated in projection by $a_\perp = 6.4 \pm 0.5$ au. The lens is located in the disk with a distance of $D_{\rm L} = 3.3 \pm 0.3$~kpc. It turns out that the reason for the absence of a lensing signal in the {\it Spitzer} data is that the time of observation corresponds to the flat region of the light curve., Comment: 10 pages, 7 figures
Published: 2018
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26. Spitzer Microlensing Parallax for OGLE-2016-BLG-1067: a sub-Jupiter Orbiting an M-dwarf in the Disk

Author: Novati, S. Calchi, Suzuki, D., Udalski, A., Gould, A., Shvartzvald, Y., Bozza, V., Bennett, D. P., Beichman, C., Bryden, G., Carey, S., Gaudi, B. S., Henderson, C. B., Yee, J. C., Zhu, W., Abe, F., Asakura, Y., Barry, R., Bhattacharya, A., Bond, I. A., Donachie, M., Evans, P., Fukui, A., Hirao, Y., Itow, Y., Kawasaki, K., Koshimoto, N., Li, M. C. A., Ling, C. H., Matsubara, Y., Miyazaki, S., Muraki, Y., Nagakane, M., Ohnishi, K., Ranc, C., Rattenbury, N. J., Saito, To., Sharan, A., Sullivan, D. J., Sumi, T., Tristram, P. J., Yamada, T., Yonehara, A., Mróz, P., Poleski, R., Skowron, J., Szymański, M. K., Soszyński, I., Kozłowski, S., Pietrukowicz, P., Ulaczyk, K., Pawlak, M., Albrow, M. D., Chung, S. -J., Han, C., Hwang, K. -H., Jung, Y. K., Ryu, Y. -H., Shin, I. -G., Zang, W., Cha, S. -M., Kim, D. -J., Kim, H. -W., Kim, S. -L., Lee, C. -U., Lee, D. -J., Lee, Y., Park, B. -G., Pogge, R. W., Novati, S. Calchi, Suzuki, D., Udalski, A., Gould, A., Shvartzvald, Y., Bozza, V., Bennett, D. P., Beichman, C., Bryden, G., Carey, S., Gaudi, B. S., Henderson, C. B., Yee, J. C., Zhu, W., Abe, F., Asakura, Y., Barry, R., Bhattacharya, A., Bond, I. A., Donachie, M., Evans, P., Fukui, A., Hirao, Y., Itow, Y., Kawasaki, K., Koshimoto, N., Li, M. C. A., Ling, C. H., Matsubara, Y., Miyazaki, S., Muraki, Y., Nagakane, M., Ohnishi, K., Ranc, C., Rattenbury, N. J., Saito, To., Sharan, A., Sullivan, D. J., Sumi, T., Tristram, P. J., Yamada, T., Yonehara, A., Mróz, P., Poleski, R., Skowron, J., Szymański, M. K., Soszyński, I., Kozłowski, S., Pietrukowicz, P., Ulaczyk, K., Pawlak, M., Albrow, M. D., Chung, S. -J., Han, C., Hwang, K. -H., Jung, Y. K., Ryu, Y. -H., Shin, I. -G., Zang, W., Cha, S. -M., Kim, D. -J., Kim, H. -W., Kim, S. -L., Lee, C. -U., Lee, D. -J., Lee, Y., Park, B. -G., and Pogge, R. W.
Abstract: We report the discovery of a sub-Jupiter mass planet orbiting beyond the snow line of an M-dwarf most likely in the Galactic disk as part of the joint Spitzer and ground-based monitoring of microlensing planetary anomalies toward the Galactic bulge. The microlensing parameters are strongly constrained by the light curve modeling and in particular by the Spitzer-based measurement of the microlens parallax, $\pi_\mathrm{E}$. However, in contrast to many planetary microlensing events, there are no caustic crossings, so the angular Einstein radius, $\theta_\mathrm{E}$ has only an upper limit based on the light curve modeling alone. Additionally, the analysis leads us to identify 8 degenerate configurations: the four-fold microlensing parallax degeneracy being doubled by a degeneracy in the caustic structure present at the level of the ground-based solutions. To pinpoint the physical parameters, and at the same time to break the parallax degeneracy, we make use of a series of arguments: the $\chi^2$ hierarchy, the Rich argument, and a prior Galactic model. The preferred configuration is for a host at $D_L=3.73_{-0.67}^{+0.66}~\mathrm{kpc}$ with mass $M_\mathrm{L}=0.30_{-0.12}^{+0.15}~\mathrm{M_\odot}$, orbited by a Saturn-like planet with $M_\mathrm{planet}=0.43_{-0.17}^{+0.21}~\mathrm{M_\mathrm{Jup}}$ at projected separation $a_\perp = 1.70_{-0.39}^{+0.38}~\mathrm{au}$, about 2.1 times beyond the system snow line. Therefore, it adds to the growing population of sub-Jupiter planets orbiting near or beyond the snow line of M-dwarfs discovered by microlensing. Based on the rules of the real-time protocol for the selection of events to be followed up with Spitzer, this planet will not enter the sample for measuring the Galactic distribution of planets., Comment: Submitted to AAS Journals
Published: 2018
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27. OGLE-2015-BLG-1459L: The Challenges of Exo-moon Microlensing

Author: Hwang, K.-H., Udalski, A., Bond, I. A., Albrow, M. D., Chung, S.-J., Gould, A., Han, C., Jung, Y. K., Ryu, Y.-H., Shin, I.-G., Yee, J. C., Zhu, W., Cha, S.-M., Kim, D.-J., Kim, H.-W., Kim, S.-L., Lee, C.-U., Lee, D.-J., Lee, Y., Park, B.-G., Pogge, R. W., Pawlak, M., Poleski, R., Szymański, M. K., Skowron, J., Soszyński, I., Mróz, P., Kozłowski, S., Pietrukowicz, P., Ulaczyk, K., Abe, F., Asakura, Y., Barry, R., Bennett, D. P., Bhattacharya, A., Donachie, M., Evans, P., Fukui, A., Hirao, Y., Itow, Y., Kawasaki, K., Koshimoto, N., Li, M. C. A., Ling, C. H., Masuda, K., Matsubara, Y., Miyazaki, S., Muraki, Y., Nagakane, M., Ohnishi, K., Ranc, C., Rattenbury, N. J., Saito, To., Sharan, A., Sullivan, D. J., Sumi, T., Suzuki, Daisuke, Tristram, P. J., Yamada, T., Yonehara, A., Hwang, K.-H., Udalski, A., Bond, I. A., Albrow, M. D., Chung, S.-J., Gould, A., Han, C., Jung, Y. K., Ryu, Y.-H., Shin, I.-G., Yee, J. C., Zhu, W., Cha, S.-M., Kim, D.-J., Kim, H.-W., Kim, S.-L., Lee, C.-U., Lee, D.-J., Lee, Y., Park, B.-G., Pogge, R. W., Pawlak, M., Poleski, R., Szymański, M. K., Skowron, J., Soszyński, I., Mróz, P., Kozłowski, S., Pietrukowicz, P., Ulaczyk, K., Abe, F., Asakura, Y., Barry, R., Bennett, D. P., Bhattacharya, A., Donachie, M., Evans, P., Fukui, A., Hirao, Y., Itow, Y., Kawasaki, K., Koshimoto, N., Li, M. C. A., Ling, C. H., Masuda, K., Matsubara, Y., Miyazaki, S., Muraki, Y., Nagakane, M., Ohnishi, K., Ranc, C., Rattenbury, N. J., Saito, To., Sharan, A., Sullivan, D. J., Sumi, T., Suzuki, Daisuke, Tristram, P. J., Yamada, T., and Yonehara, A.
Abstract: 著者人数: 61名ほか (所属. 宇宙航空研究開発機構宇宙科学研究所(JAXA)(ISAS): 鈴木, 大介), Accepted: 2018-05-02
Published: 2018

28. The First Planetary Microlensing Event with Two Microlensed Source Stars

Author: Bennett, D. P., Udalski, A., Han, C., Bond, I. A., Beaulieu, J.-P., Skowron, J., Gaudi, B. S., Koshimoto, N., Abe, F., Asakura, Y., Barry, R. K., Bhattacharya, A., Donachie, M., Evans, P., Fukui, A., Hirao, Y., Itow, Y., Li, M. C. A., Ling, C. H., Masuda, K., Matsubara, Y., Muraki, Y., Nagakane, M., Ohnishi, K., Oyokawa, H., Ranc, C., Rattenbury, N. J., Rosenthal, M. M., Saito, To., Sharan, A., Sullivan, D. J., Sumi, T., Suzuki, Daisuke, Tristram, P. J., Yonehara, A., Szymański, M. K., Poleski, R., Soszyński, I., Ulaczyk, K., Wyrzykowski, Ł., DePoy, D., Gould, A., Pogge, R. W., Yee, J. C., Albrow, M. D., Bachelet, E., Batista, V., Bowens-Rubin, R., Brillant, S., Caldwell, J. A. R., Cole, A., Coutures, C., Dieters, S., Prester, D. Dominis, Donatowicz, J., Fouqué, P., Horne, K., Hundertmark, M., Kains, N., Kane, S. R., Marquette, J.-B., Menzies, J., Pollard, K. R., Sahu, K. C., Wambsganss, J., Williams, A., Zub, M., Bennett, D. P., Udalski, A., Han, C., Bond, I. A., Beaulieu, J.-P., Skowron, J., Gaudi, B. S., Koshimoto, N., Abe, F., Asakura, Y., Barry, R. K., Bhattacharya, A., Donachie, M., Evans, P., Fukui, A., Hirao, Y., Itow, Y., Li, M. C. A., Ling, C. H., Masuda, K., Matsubara, Y., Muraki, Y., Nagakane, M., Ohnishi, K., Oyokawa, H., Ranc, C., Rattenbury, N. J., Rosenthal, M. M., Saito, To., Sharan, A., Sullivan, D. J., Sumi, T., Suzuki, Daisuke, Tristram, P. J., Yonehara, A., Szymański, M. K., Poleski, R., Soszyński, I., Ulaczyk, K., Wyrzykowski, Ł., DePoy, D., Gould, A., Pogge, R. W., Yee, J. C., Albrow, M. D., Bachelet, E., Batista, V., Bowens-Rubin, R., Brillant, S., Caldwell, J. A. R., Cole, A., Coutures, C., Dieters, S., Prester, D. Dominis, Donatowicz, J., Fouqué, P., Horne, K., Hundertmark, M., Kains, N., Kane, S. R., Marquette, J.-B., Menzies, J., Pollard, K. R., Sahu, K. C., Wambsganss, J., Williams, A., and Zub, M.
Abstract: 著者人数: 68名(所属. 宇宙航空研究開発機構宇宙科学研究所(JAXA)(ISAS): 小林, 大輔), Accepted: 2018-02-06
Published: 2018

29. OGLE-2013-BLG-0132Lb and OGLE-2013-BLG-1721Lb: Two Saturn-mass Planets Discovered around M-dwarfs

Author: The OGLE Collaboration: Mroz, Przemek, Udalski, A., Bond, I. A., Skowron, J., Sumi, T., Han, C., Szymanski, M. K., Soszynski, I., Poleski, R., Pietrukowicz, P., Kozlowski, S., Wyrzykowski, L., Ulaczyk, K., The MOA Collaboration: Abe, Fumio, Asakura, Y., Barry, R. K., Bennett, D. P., Bhattacharya, A., Donachie, M., Evans, P., Fukui, Akihiko, Hirao, Y., Itow, Yoshitaka, Koshimoto, N., Li, M. C. A., Ling, C. H., Masuda, Kimiaki, Matsubara, Yutaka, Muraki, Yasushi, Nagakane, M., Ohnishi, K., Ranc, C., Rattenbury, N. J., Saito, To., Sharan, A., Sullivan, D. J., Suzuki, Daisuke, Tristram, P. J., Yamada, T., Yonehara, A., The MOA Collaboration: 阿部, 文雄, 福井, 暁彦, 伊藤, 好孝, 増田, 公明, 松原, 豊, 村木, 綏, 鈴木, 大介, The OGLE Collaboration: Mroz, Przemek, Udalski, A., Bond, I. A., Skowron, J., Sumi, T., Han, C., Szymanski, M. K., Soszynski, I., Poleski, R., Pietrukowicz, P., Kozlowski, S., Wyrzykowski, L., Ulaczyk, K., The MOA Collaboration: Abe, Fumio, Asakura, Y., Barry, R. K., Bennett, D. P., Bhattacharya, A., Donachie, M., Evans, P., Fukui, Akihiko, Hirao, Y., Itow, Yoshitaka, Koshimoto, N., Li, M. C. A., Ling, C. H., Masuda, Kimiaki, Matsubara, Yutaka, Muraki, Yasushi, Nagakane, M., Ohnishi, K., Ranc, C., Rattenbury, N. J., Saito, To., Sharan, A., Sullivan, D. J., Suzuki, Daisuke, Tristram, P. J., Yamada, T., Yonehara, A., The MOA Collaboration: 阿部, 文雄, 福井, 暁彦, 伊藤, 好孝, 増田, 公明, 松原, 豊, 村木, 綏, and 鈴木, 大介
Abstract: 著者人数: 41名, Accepted: 2017-09-25
Published: 2018

30. The Diverse Science Return from a Wide-Area Survey of the Galactic Plane

Author: Street, R. A., Lund, M. B., Khakpash, S., Donachie, M., Dawson, W. A., Golovich, N., Wyrzykowski, L., Szkody, P., Naylor, T., Penny, M., Rattenbury, N., Dall'Ora, M., Clarkson, W. I., Bennett, D., Pepper, J., Rabus, M., Hundertmark, M. P. G., Tsapras, Y., Di Stefano, R., Ridgway, S., Liu, M., Lin, E., Street, R. A., Lund, M. B., Khakpash, S., Donachie, M., Dawson, W. A., Golovich, N., Wyrzykowski, L., Szkody, P., Naylor, T., Penny, M., Rattenbury, N., Dall'Ora, M., Clarkson, W. I., Bennett, D., Pepper, J., Rabus, M., Hundertmark, M. P. G., Tsapras, Y., Di Stefano, R., Ridgway, S., Liu, M., and Lin, E.
Abstract: The overwhelming majority of objects visible to LSST lie within the Galactic Plane. Though many previous surveys have avoided this region for fear of stellar crowding, LSST's spatial resolution combined with its state-of-the-art Difference Image Analysis mean that it can conduct a high cadence survey of most of the Galaxy for the first time. Here we outline the many areas of science that would greatly benefit from an LSST survey that included the Galactic Plane, Magellanic Clouds and Bulge at a cadence of 2-3 d. Particular highlights include measuring the mass spectrum of black holes, and mapping the population of exoplanets in the Galaxy in relation to variations in star forming environments. But the same survey data will provide a goldmine for a wide range of science, and we explore possible survey strategies which maximize the scientific return for a number of fields including young stellar objects, cataclysmic variables and Neptune Trojans., Comment: White Paper submitted in response to the 2018 call for LSST cadence proposals
Published: 2018

31. Unique Science from a Coordinated LSST-WFIRST Survey of the Galactic Bulge

Author: Street, R. A., Lund, M. B., Donachie, M., Khakpash, S., Golovich, N., Penny, M., Bennett, D., Dawson, W. A., Pepper, J., Rabus, M., Szkody, P., Clarkson, W. I., Di Stefano, R., Rattenbury, N., Hundertmark, M. P. G., Tsapras, Y., Ridgway, S., Stassun, K., Bozza, V., Bhattacharya, A., Novati, S. Calchi, Shvartzvald, Y., Street, R. A., Lund, M. B., Donachie, M., Khakpash, S., Golovich, N., Penny, M., Bennett, D., Dawson, W. A., Pepper, J., Rabus, M., Szkody, P., Clarkson, W. I., Di Stefano, R., Rattenbury, N., Hundertmark, M. P. G., Tsapras, Y., Ridgway, S., Stassun, K., Bozza, V., Bhattacharya, A., Novati, S. Calchi, and Shvartzvald, Y.
Abstract: NASA's WFIRST mission will perform a wide-field, NIR survey of the Galactic Bulge to search for exoplanets via the microlensing techniques. As the mission is due to launch in the mid-2020s, around half-way through the LSST Main Survey, we have a unique opportunity to explore synergistic science from two landmark programs. LSST can survey the entire footprint of the WFIRST microlensing survey in a single Deep Drilling Field. Here we explore the great scientific potential of this proposal and recommend the most effective observing strategies., Comment: White Paper submitted to the 2018 call for LSST cadence proposals. arXiv admin note: text overlap with arXiv:1812.03137
Published: 2018

32. First assessment of the binary lens OGLE-2015_BLG-0232

Author: Bachelet, E., Bozza, V., Han, C., Udalski, A., Bond, I. A., Beaulieu, J. -P., Street, R. A., Kim, J. -I, Bramich, D. M., Cassan, A., Dominik, M., Jaimes, R. Figuera, Horne, K., Hundertmark, M., Mao, S., Menzies, J., Ranc, C., Schmidt, R., Snodgrass, C., Steele, I. A., Tsapras, Y., Wambsganss, J., Mróz, P., Soszyński, I., Szymański, M. K., Skowron, J., Pietrukowicz, P., Kozłowski, S., Poleski, R., Ulaczyk, K., Pawlak, M., 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., Bachelet, E., Bozza, V., Han, C., Udalski, A., Bond, I. A., Beaulieu, J. -P., Street, R. A., Kim, J. -I, Bramich, D. M., Cassan, A., Dominik, M., Jaimes, R. Figuera, Horne, K., Hundertmark, M., Mao, S., Menzies, J., Ranc, C., Schmidt, R., Snodgrass, C., Steele, I. A., Tsapras, Y., Wambsganss, J., Mróz, P., Soszyński, I., Szymański, M. K., Skowron, J., Pietrukowicz, P., Kozłowski, S., Poleski, R., Ulaczyk, K., Pawlak, M., 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., and Yonehara, A.
Abstract: 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., Comment: Accepted in ApJ
Published: 2018
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33. Two new free-floating or wide-orbit planets from microlensing

Author: Mroz, P., Udalski, A., Bennett, D. P., Ryu, Y. -H., Sumi, T., Shvartzvald, Y., Skowron, J., Poleski, R., Pietrukowicz, P., Kozlowski, S., Szymanski, M. K., Wyrzykowski, L., Soszynski, I., Ulaczyk, K., Rybicki, K., Iwanek, P., Albrow, M. D., Chung, S. -J., Gould, A., Han, C., Hwang, K. -H., Jung, Y. K., Shin, I. -G., Yee, J. C., Zang, W., Cha, S. -M., Kim, D. -J., Kim, H. -W., Kim, S. -L., Lee, C. -U., Lee, D. -J., Lee, Y., Park, B. -G., Pogge, R. W., Abe, F., Barry, R., Bhattacharya, A., Bond, I. A., Donachie, M., Fukui, A., Hirao, Y., Itow, Y., Kawasaki, K., Kondo, I., Koshimoto, N., Li, M. C. A., Matsubara, Y., Muraki, Y., Miyazaki, S., Nagakane, M., Ranc, C., Rattenbury, N. J., Suematsu, H., Sullivan, D. J., Suzuki, D., Tristram, P. J., Yonehara, A., Maoz, D., Kaspi, S., Friedmann, M., Mroz, P., Udalski, A., Bennett, D. P., Ryu, Y. -H., Sumi, T., Shvartzvald, Y., Skowron, J., Poleski, R., Pietrukowicz, P., Kozlowski, S., Szymanski, M. K., Wyrzykowski, L., Soszynski, I., Ulaczyk, K., Rybicki, K., Iwanek, P., Albrow, M. D., Chung, S. -J., Gould, A., Han, C., Hwang, K. -H., Jung, Y. K., Shin, I. -G., Yee, J. C., Zang, W., Cha, S. -M., Kim, D. -J., Kim, H. -W., Kim, S. -L., Lee, C. -U., Lee, D. -J., Lee, Y., Park, B. -G., Pogge, R. W., Abe, F., Barry, R., Bhattacharya, A., Bond, I. A., Donachie, M., Fukui, A., Hirao, Y., Itow, Y., Kawasaki, K., Kondo, I., Koshimoto, N., Li, M. C. A., Matsubara, Y., Muraki, Y., Miyazaki, S., Nagakane, M., Ranc, C., Rattenbury, N. J., Suematsu, H., Sullivan, D. J., Suzuki, D., Tristram, P. J., Yonehara, A., Maoz, D., Kaspi, S., and Friedmann, M.
Abstract: Planet formation theories predict the existence of free-floating planets that have been ejected from their parent systems. Although they emit little or no light, they can be detected during gravitational microlensing events. Microlensing events caused by rogue planets are characterized by very short timescales $t_{\rm E}$ (typically below two days) and small angular Einstein radii $\theta_{\rm E}$ (up to several uas). Here we present the discovery and characterization of two ultra-short microlensing events identified in data from the Optical Gravitational Lensing Experiment (OGLE) survey, which may have been caused by free-floating or wide-orbit planets. OGLE-2012-BLG-1323 is one of the shortest events discovered thus far ($t_{\rm E}$=0.155 +/- 0.005 d, $\theta_{\rm E}$=2.37 +/- 0.10 uas) and was caused by an Earth-mass object in the Galactic disk or a Neptune-mass planet in the Galactic bulge. OGLE-2017-BLG-0560 ($t_{\rm E}$=0.905 +/- 0.005 d, $\theta_{\rm E}$=38.7 +/- 1.6 uas) was caused by a Jupiter-mass planet in the Galactic disk or a brown dwarf in the bulge. We rule out stellar companions up to a distance of 6.0 and 3.9 au, respectively. We suggest that the lensing objects, whether located on very wide orbits or free-floating, may originate from the same physical mechanism. Although the sample of ultrashort microlensing events is small, these detections are consistent with low-mass wide-orbit or unbound planets being more common than stars in the Milky Way., Comment: accepted for publication in A&A, minor changes
Published: 2018
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34. OGLE-2017-BLG-0039: Microlensing Event with Light from the Lens Identified from Mass Measurement

Author: Han, C., Jung, Y. K., Udalski, A., Bond, I., Bozza, V., Albrow, M. D., Chung, S. -J., Gould, A., Hwang, K. -H., Kim, D., Lee, C. -U., Kim, H. -W., Ryu, Y. -H., Shin, I. -G., Yee, J. C., Shvartzvald, Y., Cha, S. -M., Kim, S. -L., Kim, D. -J., Lee, D. -J., Lee, Y., Park, B. -G., Pogge, R. W., Szymański, M. K., Mróz, P., Skowron, J., Poleski, R., Soszyński, I., Kozłowski, S., Pietrukowicz, P., Ulaczyk, K., Pawlak, M., Abe, F., Barry, R., Bennett, D. P., Bhattacharya, A., Donachie, M., Evans, P., Fukui, A., Hirao, Y., Itow, Y., Kawasaki, K., Koshimoto, N., Li, M. C. A., Ling, C. H., Matsubara, Y., Miyazaki, S., Munakata, H., Muraki, Y., Nagakane, M., Ohnishi, K., Ranc, C., Rattenbury, N., Saito, T., Sharan, A., Sullivan, D. J., Sumi, T., Suzuki, D., Tristram, P. J., Yamada, T., Yonehara, A., Han, C., Jung, Y. K., Udalski, A., Bond, I., Bozza, V., Albrow, M. D., Chung, S. -J., Gould, A., Hwang, K. -H., Kim, D., Lee, C. -U., Kim, H. -W., Ryu, Y. -H., Shin, I. -G., Yee, J. C., Shvartzvald, Y., Cha, S. -M., Kim, S. -L., Kim, D. -J., Lee, D. -J., Lee, Y., Park, B. -G., Pogge, R. W., Szymański, M. K., Mróz, P., Skowron, J., Poleski, R., Soszyński, I., Kozłowski, S., Pietrukowicz, P., Ulaczyk, K., Pawlak, M., Abe, F., Barry, R., Bennett, D. P., Bhattacharya, A., Donachie, M., Evans, P., Fukui, A., Hirao, Y., Itow, Y., Kawasaki, K., Koshimoto, N., Li, M. C. A., Ling, C. H., Matsubara, Y., Miyazaki, S., Munakata, H., Muraki, Y., Nagakane, M., Ohnishi, K., Ranc, C., Rattenbury, N., Saito, T., Sharan, A., Sullivan, D. J., Sumi, T., Suzuki, D., Tristram, P. J., Yamada, T., and Yonehara, A.
Abstract: We present the analysis of the caustic-crossing binary microlensing event OGLE-2017-BLG-0039. Thanks to the very long duration of the event, with an event time scale $t_{\rm E}\sim 130$ days, the microlens parallax is precisely measured despite its small value of $\pie\sim 0.06$. The analysis of the well-resolved caustic crossings during both the source star's entrance and exit of the caustic yields the angular Einstein radius $\thetae\sim 0.6$~mas. The measured $\pie$ and $\thetae$ indicate that the lens is a binary composed of two stars with masses $\sim 1.0~M_\odot$ and $\sim 0.15~M_\odot$, and it is located at a distance of $\sim 6$ kpc. From the color and brightness of the lens estimated from the determined lens mass and distance, it is expected that $\sim 2/3$ of the $I$-band blended flux comes from the lens. Therefore, the event is a rare case of a bright lens event for which high-resolution follow-up observations can confirm the nature of the lens., Comment: 8 pages, 6 figures, 5 tables
Published: 2018
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35. A study of light travel time effect in short-period MOA eclipsing binaries via eclipse timing

Author: Li, M. C. A., Rattenbury, N. J., Bond, I. A., Sumi, T., Bennett, D. P., Koshimoto, N., Abe, F., Asakura, Y., Barry, R., Bhattacharya, A., Donachie, M., Evans, P., Fukui, A., Hirao, Y., Itow, Y., Masuda, K., Matsubara, Y., Muraki, Y., Nagakane, M., Ohnishi, K., Saito, To., Sharan, A., Sullivan, D. J., Suzuki, D., Tristram, P. J., Yonehara, A., Li, M. C. A., Rattenbury, N. J., Bond, I. A., Sumi, T., Bennett, D. P., Koshimoto, N., Abe, F., Asakura, Y., Barry, R., Bhattacharya, A., Donachie, M., Evans, P., Fukui, A., Hirao, Y., Itow, Y., Masuda, K., Matsubara, Y., Muraki, Y., Nagakane, M., Ohnishi, K., Saito, To., Sharan, A., Sullivan, D. J., Suzuki, D., Tristram, P. J., and Yonehara, A.
Abstract: A sample of 542 eclipsing binaries (EBs) with periods shorter than 2 d were selected from the Microlensing Observations in Astrophysics (MOA) EB catalogue (Li et al. 2017) for eclipse-time variation analysis. For this sample we were able to obtain the time series from MOA-II that span 9.5yr. We discovered 91 EBs, out of the 542 EBs, with detected light-travel-time effect signals suggesting the presence of tertiary companions of orbiting periods from 250 d-28 yr. The frequency of EBs with tertiary companions in our sample increases as the period decreases and reaches a value of 0.65 for contact binaries with periods shorter than 0.3 d. If only the contact binaries of periods < 0.26d are considered, the frequency even goes to the unit. Our results suggest that contact binaries with periods close to the 0.22-d contact binary limit are commonly accompanied by relatively close tertiary companions., Comment: 22 pages, 17 figures, MNRAS accepted
Published: 2018
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36. MOA-2015-BLG-337: A Planetary System with a Low-mass Brown Dwarf/Planetary Boundary Host, or a Brown Dwarf Binary

Author: Miyazaki, S., Sumi, T., Bennett, D. P., Gould, A., Udalski, A., Bond, I. A., Koshimoto, N., Nagakane, M., Rattenbury, N., Abe, F., Bhattacharya, A., Barry, R., Donachie, M., Fukui, A., Hirao, Y., Itow, Y., Kawasaki, K., Li, M. C., Ling, C. H., Matsubara, Y., Matsuo, T., Muraki, Y., Ohnishi, K., Ranc, C., Saito, T., Sharan, A., Shibai, H., Suematsu, H., Suzuki, D., Sullivan, D. J., Tristram, P. J., Yamada, T., Yonehara, A., owski, S., Mr'oz, P., Pawlak, M., Poleski, R., Pietrukowicz, P., Skowron, J., Soszy'nski, I., Szyma'nski, M. K., Ulaczyk, K., Albrow, M. D., Chung, S. -J., Han, C., Jung, Y. K., Hwang, K. -H., Ryu, Y. -H., Shin, I. -G., Shvartzvald, Y., Yee, J. C., Zang, W., Zhu, W., Cha, S. -M., Kim, D. -J., Kim, H. -W., Kim, S. -L., Lee, C. -U., Lee, D. -J., Lee, Y., Park, B. -G., Pogge, R. W., Miyazaki, S., Sumi, T., Bennett, D. P., Gould, A., Udalski, A., Bond, I. A., Koshimoto, N., Nagakane, M., Rattenbury, N., Abe, F., Bhattacharya, A., Barry, R., Donachie, M., Fukui, A., Hirao, Y., Itow, Y., Kawasaki, K., Li, M. C., Ling, C. H., Matsubara, Y., Matsuo, T., Muraki, Y., Ohnishi, K., Ranc, C., Saito, T., Sharan, A., Shibai, H., Suematsu, H., Suzuki, D., Sullivan, D. J., Tristram, P. J., Yamada, T., Yonehara, A., owski, S., Mr'oz, P., Pawlak, M., Poleski, R., Pietrukowicz, P., Skowron, J., Soszy'nski, I., Szyma'nski, M. K., Ulaczyk, K., Albrow, M. D., Chung, S. -J., Han, C., Jung, Y. K., Hwang, K. -H., Ryu, Y. -H., Shin, I. -G., Shvartzvald, Y., Yee, J. C., Zang, W., Zhu, W., Cha, S. -M., Kim, D. -J., Kim, H. -W., Kim, S. -L., Lee, C. -U., Lee, D. -J., Lee, Y., Park, B. -G., and Pogge, R. W.
Abstract: We report the discovery and the analysis of the short timescale binary-lens microlensing event, MOA-2015-BLG-337. The lens system could be a planetary system with a very low mass host, around the brown dwarf/planetary mass boundary, or a brown dwarf binary. We found two competing models that explain the observed light curves with companion/host mass ratios of q~0.01 and ~0.17, respectively. From the measurement of finite source effects in the best-fit planetary model, we find a relatively small angular Einstein radius of theta_E ~ 0.03 mas which favors a low mass lens. We conduct a Bayesian analysis to obtain the probability distribution of the lens properties. The results for the planetary models strongly depend on the minimum mass, M_min, in the assumed mass function. In summary, there are two solutions of the lens system: (1) a brown dwarf/planetary mass boundary object orbited by a super-Neptune (the planetary model with M_min=0.001 M_sun) and (2) a brown dwarf binary (the binary model). If the planetary models is correct, this system can be one of a new class of planetary system, having a low host mass and also a planetary mass ratio (q <0.03) between the host and its companion. The discovery of the event is important for the study of planetary formation in very low mass objects. In addition, it is important to consider all viable solutions in these kinds of ambiguous events in order for the future comprehensive statistical analyses of planetary/binary microlensing events., Comment: 17 pages, 7 figures, Accepted for publication in AJ
Published: 2018
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37. OGLE-2017-BLG-0482Lb: A Microlensing Super-Earth Orbiting a Low-mass Host Star

Author: Han, C., Hirao, Y., Udalski, A., Lee, C. -U., Bozza, V., Gould, A., Abe, F., Barry, R., Bond, I. A., Bennett, D. P., Bhattacharya, A., Donachie, M., Evans, P., Fukui, A., Itow, Y., Kawasaki, K., Koshimoto, N., Li, M. C. A., Ling, C. H., Matsubara, Y., Miyazaki, S., Munakata, H., Muraki, Y., Nagakane, M., Ohnishi, K., Ranc, C., Rattenbury, N., Saito, T., Sharan, A., Sullivan, D. J., Sumi, T., Suzuki, D., Tristram, P. J., Yamada, T., Yonehara, A., Mróz, P., Poleski, R., Kozłowski, S., Soszyński, I., Pietrukowicz, P., Skowron, J., Szymańsk, M. K., Ulaczyk, K., Pawlak, M., Rybicki, K., Iwanek, P., Albrow, M. D., Chung, S. -J., Hwang, K. -H., Jung, Y. K., Kim, D., Kim, W. -T., Kim, H. -W., Ryu, Y. -H., Shin, I. -G., Shvartzvald, Y., Yee, J. C., Zhu, W., Cha, S. -M., Kim, S. -L., Kim, D. -J., Lee, D. -J., Lee, Y., Park, B. -G., Pogge, R. W., Han, C., Hirao, Y., Udalski, A., Lee, C. -U., Bozza, V., Gould, A., Abe, F., Barry, R., Bond, I. A., Bennett, D. P., Bhattacharya, A., Donachie, M., Evans, P., Fukui, A., Itow, Y., Kawasaki, K., Koshimoto, N., Li, M. C. A., Ling, C. H., Matsubara, Y., Miyazaki, S., Munakata, H., Muraki, Y., Nagakane, M., Ohnishi, K., Ranc, C., Rattenbury, N., Saito, T., Sharan, A., Sullivan, D. J., Sumi, T., Suzuki, D., Tristram, P. J., Yamada, T., Yonehara, A., Mróz, P., Poleski, R., Kozłowski, S., Soszyński, I., Pietrukowicz, P., Skowron, J., Szymańsk, M. K., Ulaczyk, K., Pawlak, M., Rybicki, K., Iwanek, P., Albrow, M. D., Chung, S. -J., Hwang, K. -H., Jung, Y. K., Kim, D., Kim, W. -T., Kim, H. -W., Ryu, Y. -H., Shin, I. -G., Shvartzvald, Y., Yee, J. C., Zhu, W., Cha, S. -M., Kim, S. -L., Kim, D. -J., Lee, D. -J., Lee, Y., Park, B. -G., and Pogge, R. W.
Abstract: We report the discovery of a planetary system in which a super-earth orbits a late M-dwarf host. The planetary system was found from the analysis of the microlensing event OGLE-2017-BLG-0482, wherein the planet signal appears as a short-term anomaly to the smooth lensing light curve produced by the host. Despite its weak signal and short duration, the planetary signal was firmly detected from the dense and continuous coverage by three microlensing surveys. We find a planet/host mass ratio of $q\sim 1.4\times 10^{-4}$. We measure the microlens parallax $\pi_{\rm E}$ from the long-term deviation in the observed lensing light curve, but the angular Einstein radius $\theta_{\rm E}$ cannot be measured because the source trajectory did not cross the planet-induced caustic. Using the measured event timescale and the microlens parallax, we find that the masses of the planet and the host are $M_{\rm p}=9.0_{-4.5}^{+9.0}\ M_\oplus$ and $M_{\rm host}=0.20_{-0.10}^{+0.20}\ M_\odot$, respectively, and the projected separation between them is $a_\perp=1.8_{-0.7}^{+0.6}$ au. The estimated distance to the lens is $D_{\rm L}=5.8_{-2.1}^{+1.8}$ kpc. The discovery of the planetary system demonstrates that microlensing provides an important method to detect low-mass planets orbiting low-mass stars., Comment: 10 pages, 10 figures, 2 tables
Published: 2018
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38. A Likely Detection of a Two-Planet System in a Low Magnification Microlensing Event

Author: Suzuki, D., Bennett, D. P., Udalski, A., Bond, I. A., Sumi, T., Han, C., Abe, F., Asakura, Y., Barry, R. K., Bhattacharya, A., Donachie, M., Freeman, M., Fukui, A., Hirao, Y., Itow, Y., Koshimoto, N., Li, M. C. A., Ling, C. H., Masuda, K., Matsubara, Y., Muraki, Y., Nagakane, M., Onishi, K., Oyokawa, H., Ranc, C., Rattenbury, N. J., Saito, To., Sharan, A., Sullivan, D. J., Tristram, P. J., Yonehara, A., Poleski, R., Mróz, P., Skowron, J., Szymański, M. K., Soszyński, I., Kozłowski, S., Pietrukowicz, P., Wyrzykowski, Ł., Ulaczyk, K., Suzuki, D., Bennett, D. P., Udalski, A., Bond, I. A., Sumi, T., Han, C., Abe, F., Asakura, Y., Barry, R. K., Bhattacharya, A., Donachie, M., Freeman, M., Fukui, A., Hirao, Y., Itow, Y., Koshimoto, N., Li, M. C. A., Ling, C. H., Masuda, K., Matsubara, Y., Muraki, Y., Nagakane, M., Onishi, K., Oyokawa, H., Ranc, C., Rattenbury, N. J., Saito, To., Sharan, A., Sullivan, D. J., Tristram, P. J., Yonehara, A., Poleski, R., Mróz, P., Skowron, J., Szymański, M. K., Soszyński, I., Kozłowski, S., Pietrukowicz, P., Wyrzykowski, Ł., and Ulaczyk, K.
Abstract: We report on the analysis of a microlensing event OGLE-2014-BLG-1722 that showed two distinct short term anomalies. The best fit model to the observed light curves shows that the two anomalies are explained with two planetary mass ratio companions to the primary lens. Although a binary source model is also able to explain the second anomaly, it is marginally ruled out by 3.1 $\sigma$. The 2-planet model indicates that the first anomaly was caused by planet "b" with a mass ratio of $q = (4.5_{-0.6}^{+0.7}) \times 10^{-4}$ and projected separation in unit of the Einstein radius, $s = 0.753 \pm 0.004$. The second anomaly reveals planet "c" with a mass ratio of $q_{2} = (7.0_{-1.7}^{+2.3}) \times 10^{-4}$ with $\Delta \chi^{2} \sim 170$ compared to the single planet model. Its separation has a so-called close-wide degeneracy. We estimated the physical parameters of the lens system from Bayesian analysis. This gives that the masses of planet b and c are $m_{\rm b} = 56_{-33}^{+51}\,M_{\oplus}$ and $m_{\rm c} = 85_{-51}^{+86}\,M_{\oplus}$, respectively, and they orbit a late type star with a mass of $M_{\rm host} = 0.40_{-0.24}^{+0.36}\,M_{\odot}$ located at $D_{\rm L} = 6.4_{-1.8}^{+1.3}\,\rm kpc$ from us. If the 2-planet model is true, this is the third multiple planet system detected by using the microlensing method, and the first multiple planet system detected in the low magnification events, which are dominant in the microlensing survey data. The occurrence rate of multiple cold gas giant systems is estimated using the two such detections and a simple extrapolation of the survey sensitivity of 6 year MOA microlensing survey (Suzuki et al. 2016) combined with the 4 year $\mu$FUN detection efficiency (Gould et al. 2010). It is estimated that $6 \pm 2\,\%$ of stars host two cold giant planets., Comment: Submitted to AAS
Published: 2018
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39. Spitzer Microlensing Parallax for OGLE-2016-BLG-1067: a sub-Jupiter Orbiting an M-dwarf in the Disk

Author: Novati, S. Calchi, Suzuki, D., Udalski, A., Gould, A., Shvartzvald, Y., Bozza, V., Bennett, D. P., Beichman, C., Bryden, G., Carey, S., Gaudi, B. S., Henderson, C. B., Yee, J. C., Zhu, W., Abe, F., Asakura, Y., Barry, R., Bhattacharya, A., Bond, I. A., Donachie, M., Evans, P., Fukui, A., Hirao, Y., Itow, Y., Kawasaki, K., Koshimoto, N., Li, M. C. A., Ling, C. H., Matsubara, Y., Miyazaki, S., Muraki, Y., Nagakane, M., Ohnishi, K., Ranc, C., Rattenbury, N. J., Saito, To., Sharan, A., Sullivan, D. J., Sumi, T., Tristram, P. J., Yamada, T., Yonehara, A., Mróz, P., Poleski, R., Skowron, J., Szymański, M. K., Soszyński, I., Kozłowski, S., Pietrukowicz, P., Ulaczyk, K., Pawlak, M., Albrow, M. D., Chung, S. -J., Han, C., Hwang, K. -H., Jung, Y. K., Ryu, Y. -H., Shin, I. -G., Zang, W., Cha, S. -M., Kim, D. -J., Kim, H. -W., Kim, S. -L., Lee, C. -U., Lee, D. -J., Lee, Y., Park, B. -G., Pogge, R. W., Novati, S. Calchi, Suzuki, D., Udalski, A., Gould, A., Shvartzvald, Y., Bozza, V., Bennett, D. P., Beichman, C., Bryden, G., Carey, S., Gaudi, B. S., Henderson, C. B., Yee, J. C., Zhu, W., Abe, F., Asakura, Y., Barry, R., Bhattacharya, A., Bond, I. A., Donachie, M., Evans, P., Fukui, A., Hirao, Y., Itow, Y., Kawasaki, K., Koshimoto, N., Li, M. C. A., Ling, C. H., Matsubara, Y., Miyazaki, S., Muraki, Y., Nagakane, M., Ohnishi, K., Ranc, C., Rattenbury, N. J., Saito, To., Sharan, A., Sullivan, D. J., Sumi, T., Tristram, P. J., Yamada, T., Yonehara, A., Mróz, P., Poleski, R., Skowron, J., Szymański, M. K., Soszyński, I., Kozłowski, S., Pietrukowicz, P., Ulaczyk, K., Pawlak, M., Albrow, M. D., Chung, S. -J., Han, C., Hwang, K. -H., Jung, Y. K., Ryu, Y. -H., Shin, I. -G., Zang, W., Cha, S. -M., Kim, D. -J., Kim, H. -W., Kim, S. -L., Lee, C. -U., Lee, D. -J., Lee, Y., Park, B. -G., and Pogge, R. W.
Abstract: We report the discovery of a sub-Jupiter mass planet orbiting beyond the snow line of an M-dwarf most likely in the Galactic disk as part of the joint Spitzer and ground-based monitoring of microlensing planetary anomalies toward the Galactic bulge. The microlensing parameters are strongly constrained by the light curve modeling and in particular by the Spitzer-based measurement of the microlens parallax, $\pi_\mathrm{E}$. However, in contrast to many planetary microlensing events, there are no caustic crossings, so the angular Einstein radius, $\theta_\mathrm{E}$ has only an upper limit based on the light curve modeling alone. Additionally, the analysis leads us to identify 8 degenerate configurations: the four-fold microlensing parallax degeneracy being doubled by a degeneracy in the caustic structure present at the level of the ground-based solutions. To pinpoint the physical parameters, and at the same time to break the parallax degeneracy, we make use of a series of arguments: the $\chi^2$ hierarchy, the Rich argument, and a prior Galactic model. The preferred configuration is for a host at $D_L=3.73_{-0.67}^{+0.66}~\mathrm{kpc}$ with mass $M_\mathrm{L}=0.30_{-0.12}^{+0.15}~\mathrm{M_\odot}$, orbited by a Saturn-like planet with $M_\mathrm{planet}=0.43_{-0.17}^{+0.21}~\mathrm{M_\mathrm{Jup}}$ at projected separation $a_\perp = 1.70_{-0.39}^{+0.38}~\mathrm{au}$, about 2.1 times beyond the system snow line. Therefore, it adds to the growing population of sub-Jupiter planets orbiting near or beyond the snow line of M-dwarfs discovered by microlensing. Based on the rules of the real-time protocol for the selection of events to be followed up with Spitzer, this planet will not enter the sample for measuring the Galactic distribution of planets., Comment: Submitted to AAS Journals
Published: 2018
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40. OGLE-2014-BLG-0289: Precise Characterization of a Quintuple-Peak Gravitational Microlensing Event

Author: Udalski, A., Han, C., Bozza, V., Gould, A., Bond, I. A., Mróz, P., Skowron, J., Wyrzykowski, Ł., Szymański, M. K., Soszyński, I., Ulaczyk, K., Poleski, R., Pietrukowicz, P., Kozłowski, S., Abe, F., Barry, R., Bennett, D. P., Bhattacharya, A., Donachie, M., Evans, P., Fukui, A., Hirao, Y., Itow, Y., Kawasaki, K., Koshimoto, N., Li, M. C. A., Ling, C. H., Masuda, K., Matsubara, Y., Miyazaki, S., Munakata, H., Muraki, Y., Nagakane, M., Ohnishi, K., Ranc, C., Rattenbury, N., Saito, T., Sharan, A., Sullivan, D. J., Sumi, T., Suzuki, D., Tristram, P. J., Yamada, T., Yonehara, A., Bachelet, E., Bramich, D. M., DÁgo, G., Dominik, M., Jaimes, R. Figuera, Horne, K., Hundertmark, M., Kains, N., Menzies, J., Schmidt, R., Snodgrass, C., Steele, I. A., Wambsganss, J., Pogge, R. W., Jung, Y. K., Shin, I. -G., Yee, J. C., Kim, W. -T., Beichman, C., Carey, S., Novati, S. Calchi, Zhu, W., Udalski, A., Han, C., Bozza, V., Gould, A., Bond, I. A., Mróz, P., Skowron, J., Wyrzykowski, Ł., Szymański, M. K., Soszyński, I., Ulaczyk, K., Poleski, R., Pietrukowicz, P., Kozłowski, S., Abe, F., Barry, R., Bennett, D. P., Bhattacharya, A., Donachie, M., Evans, P., Fukui, A., Hirao, Y., Itow, Y., Kawasaki, K., Koshimoto, N., Li, M. C. A., Ling, C. H., Masuda, K., Matsubara, Y., Miyazaki, S., Munakata, H., Muraki, Y., Nagakane, M., Ohnishi, K., Ranc, C., Rattenbury, N., Saito, T., Sharan, A., Sullivan, D. J., Sumi, T., Suzuki, D., Tristram, P. J., Yamada, T., Yonehara, A., Bachelet, E., Bramich, D. M., DÁgo, G., Dominik, M., Jaimes, R. Figuera, Horne, K., Hundertmark, M., Kains, N., Menzies, J., Schmidt, R., Snodgrass, C., Steele, I. A., Wambsganss, J., Pogge, R. W., Jung, Y. K., Shin, I. -G., Yee, J. C., Kim, W. -T., Beichman, C., Carey, S., Novati, S. Calchi, and Zhu, W.
Abstract: We present the analysis of the binary-microlensing event OGLE-2014-BLG-0289. The event light curve exhibits very unusual five peaks where four peaks were produced by caustic crossings and the other peak was produced by a cusp approach. It is found that the quintuple-peak features of the light curve provide tight constraints on the source trajectory, enabling us to precisely and accurately measure the microlensing parallax $\pi_{\rm E}$. Furthermore, the three resolved caustics allow us to measure the angular Einstein radius $\thetae$. From the combination of $\pi_{\rm E}$ and $\thetae$, the physical lens parameters are uniquely determined. It is found that the lens is a binary composed of two M dwarfs with masses $M_1 = 0.52 \pm 0.04\ M_\odot$ and $M_2=0.42 \pm 0.03\ M_\odot$ separated in projection by $a_\perp = 6.4 \pm 0.5$ au. The lens is located in the disk with a distance of $D_{\rm L} = 3.3 \pm 0.3$~kpc. It turns out that the reason for the absence of a lensing signal in the {\it Spitzer} data is that the time of observation corresponds to the flat region of the light curve., Comment: 10 pages, 7 figures
Published: 2018
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41. The First Planetary Microlensing Event with Two Microlensed Source Stars

Author: Bennett, D. P., Udalski, A., Han, C., Bond, I. A., Beaulieu, J. -P., Skowron, J., Gaudi, B. S., Koshimoto, N., Abe, F., Asakura, Y., Barry, R. K., Bhattacharya, A., Donachie, M., Evans, P., Fukui, A., Hirao, Y., Itow, Y., Li, M. C. A., Ling, C. H., Masuda, K., Matsubara, Y., Muraki, Y., Nagakane, M., Ohnishi, K., Oyokawa, H., Ranc, C., Rattenbury, N. J., Rosenthal, M. M., Saito, To., Sharan, A., Sullivan, D. J., Sumi, T., Suzuki, D., Tristram, P. J., Yonehara, A., Szymanski, M. K., Poleski, R., Soszynski, I., Ulaczyk, K., Wyrzykowski, L., Depoy, D., Gould, A., Pogge, R. W., Yee, J. C., Albrow, M. D., Bachelet, E., Batista, V., Bowens-Rubin, R., Brillant, S., Caldwell, J. A. R., Cole, A., Coutures, C., Dieters, S., Prester, D. Dominis, Donatowicz, J., Fouque, P., Horne, K., Hundertmark, M., Kains, N., Kane, S. R., Marquette, J. -B., Menzies, J., Pollard, K. R., Sahu, K. C., Wambsganss, J., Williams, A., Zub, M., Bennett, D. P., Udalski, A., Han, C., Bond, I. A., Beaulieu, J. -P., Skowron, J., Gaudi, B. S., Koshimoto, N., Abe, F., Asakura, Y., Barry, R. K., Bhattacharya, A., Donachie, M., Evans, P., Fukui, A., Hirao, Y., Itow, Y., Li, M. C. A., Ling, C. H., Masuda, K., Matsubara, Y., Muraki, Y., Nagakane, M., Ohnishi, K., Oyokawa, H., Ranc, C., Rattenbury, N. J., Rosenthal, M. M., Saito, To., Sharan, A., Sullivan, D. J., Sumi, T., Suzuki, D., Tristram, P. J., Yonehara, A., Szymanski, M. K., Poleski, R., Soszynski, I., Ulaczyk, K., Wyrzykowski, L., Depoy, D., Gould, A., Pogge, R. W., Yee, J. C., Albrow, M. D., Bachelet, E., Batista, V., Bowens-Rubin, R., Brillant, S., Caldwell, J. A. R., Cole, A., Coutures, C., Dieters, S., Prester, D. Dominis, Donatowicz, J., Fouque, P., Horne, K., Hundertmark, M., Kains, N., Kane, S. R., Marquette, J. -B., Menzies, J., Pollard, K. R., Sahu, K. C., Wambsganss, J., Williams, A., and Zub, M.
Published: 2018

42. OGLE-2014-BLG-0289: Precise Characterization of a Quintuple-peak Gravitational Microlensing Event

Author: Udalski, A., Han, C., Bozza, V., Gould, A., Bond, I. A., Mroz, P., Skowron, J., Wyrzykowski, L., Szymanski, M. K., Soszynski, I., Ulaczyk, K., Poleski, R., Pietrukowicz, P., Kozlowski, S., Abe, F., Barry, R., Bennett, D. P., Bhattacharya, A., Donachie, M., Evans, P., Fukui, A., Hirao, Y., Itow, Y., Kawasaki, K., Koshimoto, N., Li, M. C. A., Ling, C. H., Masuda, K., Matsubara, Y., Miyazaki, S., Munakata, H., Muraki, Y., Nagakane, M., Ohnishi, K., Ranc, C., Rattenbury, N., Saito, T., Sharan, A., Sullivan, D. J., Sumi, T., Suzuki, D., Tristram, P. J., Yamada, T., Yonehara, A., Bachelet, E., Bramich, D. M., DAgo, G., Dominik, M., Jaimes, R. Figuera, Horne, K., Hundertmark, M., Kains, N., Menzies, J., Schmidt, R., Snodgrass, C., Steele, I. A., Wambsganss, J., Pogge, R. W., Jung, Y. K., Shin, I. -G., Yee, J. C., Kim, W. -T., Beichman, C., Carey, S., Novati, S. Calchi, Zhu, W., Udalski, A., Han, C., Bozza, V., Gould, A., Bond, I. A., Mroz, P., Skowron, J., Wyrzykowski, L., Szymanski, M. K., Soszynski, I., Ulaczyk, K., Poleski, R., Pietrukowicz, P., Kozlowski, S., Abe, F., Barry, R., Bennett, D. P., Bhattacharya, A., Donachie, M., Evans, P., Fukui, A., Hirao, Y., Itow, Y., Kawasaki, K., Koshimoto, N., Li, M. C. A., Ling, C. H., Masuda, K., Matsubara, Y., Miyazaki, S., Munakata, H., Muraki, Y., Nagakane, M., Ohnishi, K., Ranc, C., Rattenbury, N., Saito, T., Sharan, A., Sullivan, D. J., Sumi, T., Suzuki, D., Tristram, P. J., Yamada, T., Yonehara, A., Bachelet, E., Bramich, D. M., DAgo, G., Dominik, M., Jaimes, R. Figuera, Horne, K., Hundertmark, M., Kains, N., Menzies, J., Schmidt, R., Snodgrass, C., Steele, I. A., Wambsganss, J., Pogge, R. W., Jung, Y. K., Shin, I. -G., Yee, J. C., Kim, W. -T., Beichman, C., Carey, S., Novati, S. Calchi, and Zhu, W.
Published: 2018

43. The First Planetary Microlensing Event with Two Microlensed Source Stars

Author: Bennett, D., Udalski, A., Han, C., Bond, I., Beaulieu, J., Skowron, J., Gaudi, B., Koshimoto, N., Abe, F., Asakura, Y., Barry, R., Bhattacharya, A., Donachie, M., Evans, P., Fukui, A., Hirao, Y., Itow, Y., Li, M., Ling, C., Masuda, K., Matsubara, Y., Muraki, Y., Nagakane, M., Ohnishi, K., Oyokawa, H., Ranc, C., Rattenbury, N., Rosenthal, M., Saito, T., Sharan, A., Sullivan, D., Sumi, T., Suzuki, D., Tristram, P., Yonehara, A., Szymanski, M., Poleski, R., Soszynski, I., Ulaczyk, K., Wyrzykowski, Depoy, D., Gould, A., Pogge, R., Yee, J., Albrow, M., Bachelet, E., Batista, V., Bowens-Rubin, R., Brillant, S., Caldwell, J., Cole, A., Coutures, C., Dieters, S., Prester, D., Donatowicz, J., Fouqué, P., Horne, K., Hundertmark, M., Kains, N., Kane, S., Marquette, J., Menzies, J., Pollard, K., Sahu, K., Wambsganss, J., Williams, Andrew, Zub, M., Bennett, D., Udalski, A., Han, C., Bond, I., Beaulieu, J., Skowron, J., Gaudi, B., Koshimoto, N., Abe, F., Asakura, Y., Barry, R., Bhattacharya, A., Donachie, M., Evans, P., Fukui, A., Hirao, Y., Itow, Y., Li, M., Ling, C., Masuda, K., Matsubara, Y., Muraki, Y., Nagakane, M., Ohnishi, K., Oyokawa, H., Ranc, C., Rattenbury, N., Rosenthal, M., Saito, T., Sharan, A., Sullivan, D., Sumi, T., Suzuki, D., Tristram, P., Yonehara, A., Szymanski, M., Poleski, R., Soszynski, I., Ulaczyk, K., Wyrzykowski, Depoy, D., Gould, A., Pogge, R., Yee, J., Albrow, M., Bachelet, E., Batista, V., Bowens-Rubin, R., Brillant, S., Caldwell, J., Cole, A., Coutures, C., Dieters, S., Prester, D., Donatowicz, J., Fouqué, P., Horne, K., Hundertmark, M., Kains, N., Kane, S., Marquette, J., Menzies, J., Pollard, K., Sahu, K., Wambsganss, J., Williams, Andrew, and Zub, M.
Abstract: © 2018. The American Astronomical Society. All rights reserved. We present the analysis of the microlensing event MOA-2010-BLG-117, and show that the light curve can only be explained by the gravitational lensing of a binary source star system by a star with a Jupiter-mass ratio planet. It was necessary to modify standard microlensing modeling methods to find the correct light curve solution for this binary source, binary-lens event. We are able to measure a strong microlensing parallax signal, which yields the masses of the host star, M * = 0.58 ±0.11 M o, and planet, m p = 0.54 ±0.10MJup, at a projected star-planet separation of a = 2.42 ±0.26 au, corresponding to a semimajor axis of a = 2.9-0.6+1.6 au. Thus, the system resembles a half-scale model of the Sun-Jupiter system with a half-Jupiter0mass planet orbiting a half-solar-mass star at very roughly half of Jupiter's orbital distance from the Sun. The source stars are slightly evolved, and by requiring them to lie on the same isochrone, we can constrain the source to lie in the near side of the bulge at a distance of DS = 6.9 ±0.7 kpc, which implies a distance to the planetary lens system of D L = 3.5 ±0.4 kpc. The ability to model unusual planetary microlensing events, like this one, will be necessary to extract precise statistical information from the planned large exoplanet microlensing surveys, such as the WFIRST microlensing survey.
Published: 2018

44. OGLE-2015-BLG-1459L: The Challenges of Exo-Moon Microlensing

Author: Hwang, K. -H., Udalski, A., Bond, I. A., Albrow, M. D., Chung, S. -J., Gould, A., Han, C., Jung, Y. K., Ryu, Y. -H., Shin, I. -G., Yee, J. C., Zhu, W., Cha, S. -M., Kim, D. -J., Kim, H. -W., Kim, S. -L., Lee, C. -U., Lee, D. -J., Lee, Y., Park, B. -G., Pogge, R. W., Pawlak, M., Poleski, R., Szymański, M. K., Skowron, J., Soszyński, I., Mróz, P., Kozłowski, S., Pietrukowicz, P., Ulaczyk, K., Abe, F., Asakura, Y., Barry, R., Bennett, D. P., Bhattacharya, A., Donachie, M., Evans, P., Fukui, A., Hirao, Y., Itow, Y., Kawasaki, K., Koshimoto, N., Li, M. C. A., Ling, C. H., Masuda, K., Matsubara, Y., Miyazaki, S., Muraki, Y., Nagakane, M., Ohnishi, K., Ranc, C., Rattenbury, N. J., Saito, To., Sharan, A., Sullivan, D. J., Sumi, T., Suzuki, D., Tristram, P. J., Yamada, T., Yonehara, A., Hwang, K. -H., Udalski, A., Bond, I. A., Albrow, M. D., Chung, S. -J., Gould, A., Han, C., Jung, Y. K., Ryu, Y. -H., Shin, I. -G., Yee, J. C., Zhu, W., Cha, S. -M., Kim, D. -J., Kim, H. -W., Kim, S. -L., Lee, C. -U., Lee, D. -J., Lee, Y., Park, B. -G., Pogge, R. W., Pawlak, M., Poleski, R., Szymański, M. K., Skowron, J., Soszyński, I., Mróz, P., Kozłowski, S., Pietrukowicz, P., Ulaczyk, K., Abe, F., Asakura, Y., Barry, R., Bennett, D. P., Bhattacharya, A., Donachie, M., Evans, P., Fukui, A., Hirao, Y., Itow, Y., Kawasaki, K., Koshimoto, N., Li, M. C. A., Ling, C. H., Masuda, K., Matsubara, Y., Miyazaki, S., Muraki, Y., Nagakane, M., Ohnishi, K., Ranc, C., Rattenbury, N. J., Saito, To., Sharan, A., Sullivan, D. J., Sumi, T., Suzuki, D., Tristram, P. J., Yamada, T., and Yonehara, A.
Abstract: We show that dense OGLE and KMTNet $I$-band survey data require four bodies (sources plus lenses) to explain the microlensing light curve of OGLE-2015-BLG-1459. However, these can equally well consist of three lenses and one source (3L1S), two lenses and two sources (2L2S) or one lens and three sources (1L3S). In the 3L1S and 2L2S interpretations, the host is a brown dwarf and the dominant companion is a Neptune-class planet, with the third body (in the 3L1S case) being a Mars-class object that could have been a moon of the planet. In the 1L3S solution, the light curve anomalies are explained by a tight (five stellar radii) low-luminosity binary source that is offset from the principal source of the event by $\sim 0.17\,\au$. These degeneracies are resolved in favor of the 1L3S solution by color effects derived from comparison to MOA data, which are taken in a slightly different ($R/I$) passband. To enable current and future ($WFIRST$) surveys to routinely characterize exomoons and distinguish among such exotic systems requires an observing strategy that includes both a cadence faster than 9 min$^{-1}$ and observations in a second band on a similar timescale., Comment: 29 pages, 8 figures, accepted for publication in AJ
Published: 2017
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45. An Isolated Microlens Observed from K2, Spitzer and Earth

Author: Zhu, Wei, Udalski, A., Huang, C., Novati, S. Calchi, Sumi, T., Poleski, R., Skowron, J., Mroz, P., Szymanski, M. K., Soszynski, I., Pietrukowicz, P., Kozlowski, S., Ulaczyk, K., Pawlak, M., Beichman, C, Bryden, G., Carey, S., Gaudi, B. S., Gould, A., Henderson, C. B., Shvartzvald, Y., Yee, J. C., Bond, I. A., Bennett, D. P., Suzuki, D., Rattenbury, N. J., Koshimoto, N., Abe, F., Asakura, Y., Barry, R. K., Bhattacharya, A., Donachie, M., Evans, P., Fukui, A., Hirao, Y., Itow, Y., Kawasaki, K., Li, M. C. A., Ling, C. H., Masuda, K., Matsubara, Y., Miyazaki, S., Munakata, H., Muraki, Y., Nagakane, M., Ohnishi, K., Ranc, C., Saito, To., Sharan, A., Sullivan, D. J., Tristram, P. J., Yamada, T., Yonehara, A., Zhu, Wei, Udalski, A., Huang, C., Novati, S. Calchi, Sumi, T., Poleski, R., Skowron, J., Mroz, P., Szymanski, M. K., Soszynski, I., Pietrukowicz, P., Kozlowski, S., Ulaczyk, K., Pawlak, M., Beichman, C, Bryden, G., Carey, S., Gaudi, B. S., Gould, A., Henderson, C. B., Shvartzvald, Y., Yee, J. C., Bond, I. A., Bennett, D. P., Suzuki, D., Rattenbury, N. J., Koshimoto, N., Abe, F., Asakura, Y., Barry, R. K., Bhattacharya, A., Donachie, M., Evans, P., Fukui, A., Hirao, Y., Itow, Y., Kawasaki, K., Li, M. C. A., Ling, C. H., Masuda, K., Matsubara, Y., Miyazaki, S., Munakata, H., Muraki, Y., Nagakane, M., Ohnishi, K., Ranc, C., Saito, To., Sharan, A., Sullivan, D. J., Tristram, P. J., Yamada, T., and Yonehara, A.
Abstract: We present the result of microlensing event MOA-2016-BLG-290, which received observations from the two-wheel Kepler (K2), Spitzer, as well as ground-based observatories. A joint analysis of data from K2 and the ground leads to two degenerate solutions of the lens mass and distance. This degeneracy is effectively broken once the (partial) Spitzer light curve is included. Altogether, the lens is found to be an extremely low-mass star located in the Galactic bulge. MOA-2016-BLG-290 is the first microlensing event for which we have signals from three well-separated ($\sim1$ AU) locations. It demonstrates the power of two-satellite microlensing experiment in reducing the ambiguity of lens properties, as pointed out independently by S. Refsdal and A. Gould several decades ago., Comment: 8 pages, 4 figures, 1 table; submitted to ApJ Letters
Published: 2017
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46. OGLE-2016-BLG-1190Lb: First Spitzer Bulge Planet Lies Near the Planet/Brown-Dwarf Boundary

Author: Ryu, Y. -H., Yee, J. C., Udalski, A., Bond, I. A., Shvartzvald, Y., Zang, W., Jaimes, R. Figuera, Jorgensen, U. G., Zhu, W., Huang, C. X., Jung, Y. K., Albrow, M. D., Chung, S. -J., Gould, A., Han, C., Hwang, K. -H., Shin, I. -G., Cha, S. -M., Kim, D. -J., Kim, H. -W., Kim, S. -L., Lee, C. -U., Lee, D. -J., Lee, Y., Park, B. -G., Pogge, R. W., Novati, S. Calchi, Carey, S., Henderson, C. B., Beichman, C., Gaudi, B. S., Mróz, P., Poleski, R., Skowron, J., Szymanski, M. K., Soszynski, I., Kozlowski, S., Pietrukowicz, P., Ulaczyk, K., Pawlak, M., Abe, F., Asakura, Y., Barry, R., Bennett, D. P., Bhattacharya, A., Donachie, M., Evans, P., Fukui, A., Hirao, Y., Itow, Y., Kawasaki, K., Koshimoto, N., Li, M. C. A., Ling, C. H., Masuda, K., Matsubara, Y., Miyazaki, S., Muraki, Y., Nagakane, M., Ohnishi, K., Ranc, C., Rattenbury, N. J., Saito, To., Sharan, A., Sullivan, D. J., Sumi, T., Suzuki, D., Tristram, P. J., Yamada, T., Yonehara, A., Bryden, G., Howell, S. B., Jacklin, S., Penny, M. T., Mao, S., Fouque, Pascal, Wang, T., Street, R. A., Tsapras, Y., Hundertmark, M., Bachelet, E., Dominik, M., Li, Z., Cross, S., Cassan, A., Horne, K., Schmidt, R., Wambsganss, J., Ment, S. K., Maoz, D., Snodgrass, C., Steele, I. A., Bozza, V., Burgdorf, M. J., Ciceri, S., D'Ago, G., Evans, D. F., Hinse, T. C., Kerins, E., Kokotanekova, R., Longa, P., MacKenzie, J., Popovas, A., Rabus, M., Rahvar, S., Sejadian, S., Skottfelt, J., Southworth, J., von Essen, C., Ryu, Y. -H., Yee, J. C., Udalski, A., Bond, I. A., Shvartzvald, Y., Zang, W., Jaimes, R. Figuera, Jorgensen, U. G., Zhu, W., Huang, C. X., Jung, Y. K., Albrow, M. D., Chung, S. -J., Gould, A., Han, C., Hwang, K. -H., Shin, I. -G., Cha, S. -M., Kim, D. -J., Kim, H. -W., Kim, S. -L., Lee, C. -U., Lee, D. -J., Lee, Y., Park, B. -G., Pogge, R. W., Novati, S. Calchi, Carey, S., Henderson, C. B., Beichman, C., Gaudi, B. S., Mróz, P., Poleski, R., Skowron, J., Szymanski, M. K., Soszynski, I., Kozlowski, S., Pietrukowicz, P., Ulaczyk, K., Pawlak, M., Abe, F., Asakura, Y., Barry, R., Bennett, D. P., Bhattacharya, A., Donachie, M., Evans, P., Fukui, A., Hirao, Y., Itow, Y., Kawasaki, K., Koshimoto, N., Li, M. C. A., Ling, C. H., Masuda, K., Matsubara, Y., Miyazaki, S., Muraki, Y., Nagakane, M., Ohnishi, K., Ranc, C., Rattenbury, N. J., Saito, To., Sharan, A., Sullivan, D. J., Sumi, T., Suzuki, D., Tristram, P. J., Yamada, T., Yonehara, A., Bryden, G., Howell, S. B., Jacklin, S., Penny, M. T., Mao, S., Fouque, Pascal, Wang, T., Street, R. A., Tsapras, Y., Hundertmark, M., Bachelet, E., Dominik, M., Li, Z., Cross, S., Cassan, A., Horne, K., Schmidt, R., Wambsganss, J., Ment, S. K., Maoz, D., Snodgrass, C., Steele, I. A., Bozza, V., Burgdorf, M. J., Ciceri, S., D'Ago, G., Evans, D. F., Hinse, T. C., Kerins, E., Kokotanekova, R., Longa, P., MacKenzie, J., Popovas, A., Rabus, M., Rahvar, S., Sejadian, S., Skottfelt, J., Southworth, J., and von Essen, C.
Abstract: We report the discovery of OGLE-2016-BLG-1190Lb, which is likely to be the first Spitzer microlensing planet in the Galactic bulge/bar, an assignation that can be confirmed by two epochs of high-resolution imaging of the combined source-lens baseline object. The planet's mass M_p= 13.4+-0.9 M_J places it right at the deuterium burning limit, i.e., the conventional boundary between "planets" and "brown dwarfs". Its existence raises the question of whether such objects are really "planets" (formed within the disks of their hosts) or "failed stars" (low mass objects formed by gas fragmentation). This question may ultimately be addressed by comparing disk and bulge/bar planets, which is a goal of the Spitzer microlens program. The host is a G dwarf M_host = 0.89+-0.07 M_sun and the planet has a semi-major axis a~2.0 AU. We use Kepler K2 Campaign 9 microlensing data to break the lens-mass degeneracy that generically impacts parallax solutions from Earth-Spitzer observations alone, which is the first successful application of this approach. The microlensing data, derived primarily from near-continuous, ultra-dense survey observations from OGLE, MOA, and three KMTNet telescopes, contain more orbital information than for any previous microlensing planet, but not quite enough to accurately specify the full orbit. However, these data do permit the first rigorous test of microlensing orbital-motion measurements, which are typically derived from data taken over <1% of an orbital period., Comment: 63 pages, 13 figures, 7 tables, AJ, in press
Published: 2017
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47. OGLE-2016-BLG-0263L\lowercase{b}: Microlensing Detection of a Very Low-mass Binary Companion Through a Repeating Event Channel

Author: Han, C., Udalski, A., Gould, A., Bond, I. A., Albrow, M. D., Chung, S. -J., Jung, Y. K., Ryu, Y. -H., Shin, I. -G., Yee, J. C., Zhu, W., Cha, S. -M., Kim, S. -L., Kim, D. -J., Lee, C. -U., Lee, Y., Park, B. -G., Skowron, J., Mróz, P., Pietrukowicz, P., Kozłowski, S., Poleski, R., Szymański, M. K., Soszyński, I., Ulaczyk, K., Pawlak, M., Abe, F., Asakura, Y., Barry, R., Bennett, D. P., Bhattacharya, A., Donachie, M., Evans, P., Fukui, A., Hirao, Y., Itow, Y., Koshimoto, N., Li, M. C. A., Ling, C. H., Masuda, K., Matsubara, Y., Muraki, Y., Nagakane, M., Ohnishi, K., Ranc, C., Rattenbury, N. J., Saito, To., Sharan, A., Sullivan, D. J., Sumi, T., Suzuki, D., Tristram, P. J., Yamada, T., Yonehara, A., Han, C., Udalski, A., Gould, A., Bond, I. A., Albrow, M. D., Chung, S. -J., Jung, Y. K., Ryu, Y. -H., Shin, I. -G., Yee, J. C., Zhu, W., Cha, S. -M., Kim, S. -L., Kim, D. -J., Lee, C. -U., Lee, Y., Park, B. -G., Skowron, J., Mróz, P., Pietrukowicz, P., Kozłowski, S., Poleski, R., Szymański, M. K., Soszyński, I., Ulaczyk, K., Pawlak, M., Abe, F., Asakura, Y., Barry, R., Bennett, D. P., Bhattacharya, A., Donachie, M., Evans, P., Fukui, A., Hirao, Y., Itow, Y., Koshimoto, N., Li, M. C. A., Ling, C. H., Masuda, K., Matsubara, Y., Muraki, Y., Nagakane, M., Ohnishi, K., Ranc, C., Rattenbury, N. J., Saito, To., Sharan, A., Sullivan, D. J., Sumi, T., Suzuki, D., Tristram, P. J., Yamada, T., and Yonehara, A.
Abstract: We report the discovery of a planet-mass companion to the microlens OGLE-2016-BLG-0263L. Unlike most low-mass companions that were detected through perturbations to the smooth and symmetric light curves produced by the primary, the companion was discovered through the channel of a repeating event, in which the companion itself produced its own single-mass light curve after the event produced by the primary had ended. Thanks to the continuous coverage of the second peak by high-cadence surveys, the possibility of the repeating nature due to source binarity is excluded with a $96\%$ confidence level. The mass of the companion estimated by a Bayesian analysis is $M_{\rm p}=4.1_{-2.5}^{+6.5}\ M_{\rm J}$. The projected primary-companion separation is $a_\perp = 6.5^{+1.3}_{-1.9}$ au. The ratio of the separation to the snow-line distance of $a_\perp/a_{\rm sl}\sim 15.4$ corresponds to the region beyond Neptune, the outermost planet of the solar system. We discuss the importance of high-cadence surveys in expanding the range of microlensing detections of low-mass companions and future space-based microlensing surveys., Comment: 10 pages, 8 figures
Published: 2017
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48. The First Planetary Microlensing Event with Two Microlensed Source Stars

Author: Bennett, D. P., Udalski, A., Han, C., Bond, I. A., Beaulieu, J. -P., Skowron, J., Gaudi, B. S., Koshimoto, N., Abe, F., Asakura, Y., Barry, R. K., Bhattacharya, A., Donachie, M., Evans, P., Fukui, A., Hirao, Y., Itow, Y., Li, M. C. A., Ling, C. H., Masuda, K., Matsubara, Y., Muraki, Y., Nagakane, M., Ohnishi, K., Oyokawa, H., Ranc, C., Rattenbury, N. J., Rosenthal, M. K., Saito, To., Sharan, A., Sullivan, D. J., Sumi, T., Suzuki, D., Tristram, P. J., Yonehara, A., Szymanski, M. K., Poleski, R., Soszynski, I., Ulaczyk, K., Wyrzykowski, L., DePoy, D., Gould, A., Pogge, R. W., Yee, J. C., Albrow, M. D., Bachelet, E., Batista, V., Bowens-Rubin, R., Brillant, S., Caldwell, J. A. R., Cole, A., Coutures, C., Dieters, S., Prester, D. Dominis, Donatowicz, J., Fouque, P., Horne, K., Hundertmark, M., Kains, N., Kane, S. R., Marquette, J. -B., Menzies, J., Pollard, K. R., Sahu, K. C., Wambsganss, J., Williams, A., Zub, M., Bennett, D. P., Udalski, A., Han, C., Bond, I. A., Beaulieu, J. -P., Skowron, J., Gaudi, B. S., Koshimoto, N., Abe, F., Asakura, Y., Barry, R. K., Bhattacharya, A., Donachie, M., Evans, P., Fukui, A., Hirao, Y., Itow, Y., Li, M. C. A., Ling, C. H., Masuda, K., Matsubara, Y., Muraki, Y., Nagakane, M., Ohnishi, K., Oyokawa, H., Ranc, C., Rattenbury, N. J., Rosenthal, M. K., Saito, To., Sharan, A., Sullivan, D. J., Sumi, T., Suzuki, D., Tristram, P. J., Yonehara, A., Szymanski, M. K., Poleski, R., Soszynski, I., Ulaczyk, K., Wyrzykowski, L., DePoy, D., Gould, A., Pogge, R. W., Yee, J. C., Albrow, M. D., Bachelet, E., Batista, V., Bowens-Rubin, R., Brillant, S., Caldwell, J. A. R., Cole, A., Coutures, C., Dieters, S., Prester, D. Dominis, Donatowicz, J., Fouque, P., Horne, K., Hundertmark, M., Kains, N., Kane, S. R., Marquette, J. -B., Menzies, J., Pollard, K. R., Sahu, K. C., Wambsganss, J., Williams, A., and Zub, M.
Abstract: We present the analysis of microlensing event MOA-2010-BLG-117, and show that the light curve can only be explained by the gravitational lensing of a binary source star system by a star with a Jupiter mass ratio planet. It was necessary to modify standard microlensing modeling methods to find the correct light curve solution for this binary-source, binary-lens event. We are able to measure a strong microlensing parallax signal, which yields the masses of the host star, $M_* = 0.58\pm 0.11 M_\odot$, and planet $m_p = 0.54\pm 0.10 M_{\rm Jup}$ at a projected star-planet separation of $a_\perp = 2.42\pm 0.26\,$AU, corresponding to a semi-major axis of $a = 2.9{+1.6\atop -0.6}\,$AU. Thus, the system resembles a half-scale model of the Sun-Jupiter system with a half-Jupiter mass planet orbiting a half-solar mass star at very roughly half of Jupiter's orbital distance from the Sun. The source stars are slightly evolved, and by requiring them to lie on the same isochrone, we can constrain the source to lie in the near side of the bulge at a distance of $D_S = 6.9 \pm 0.7\,$kpc, which implies a distance to the planetary lens system of $D_L = 3.5\pm 0.4\,$kpc. The ability to model unusual planetary microlensing events, like this one, will be necessary to extract precise statistical information from the planned large exoplanet microlensing surveys, such as the WFIRST microlensing survey., Comment: Accepted version. Now published in AJ
Published: 2017
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49. Ground-based parallax confirmed by Spitzer: binary microlensing event MOA-2015-BLG-020

Author: Wang, Tianshu, Zhu, Wei, Mao, Shude, Bond, I. A., Gould, A., Udalski, A., Sumi, T., Bozza, V., Ranc, C., Cassan, A., Yee, J. C., Han, C., Abe, F., Asakura, Y., Barry, R., Bennett, D. P., Bhattacharya, A., Donachie, M., Evans, P., Fukui, A., Hirao, Y., Itow, Y., Kawasaki, K., Koshimoto, N., Li, M. C. A., Ling, C. H., Masuda, K., Matsubara, Y., Miyazaki, S., Muraki, Y., Nagakane, M., Ohnishi, K., Rattenbury, N., Saito, To., Sharan, A., Shibai, H., Sullivan, D. J., Suzuki, D., Tristram, P. J., Yamada, T., Yonehara, A., Pawlak, M., Pietrukowicz, P., Poleski, R., Skowron, J., Soszynski, I., KozLowski, S., Mroz, P., Ulaczyk, K., Szymanski, M. K., Beichman, C., Bryden, G., Novati, S. Calchi, Carey, S., Fausnaugh, M., Gaudi, B. S., Henderson, C. B., Shvartzvald, Y., Wibking, B., Albrow, M. D., Chung, S. -J., Hwang, K. -H., Jung, Y. K., Ryu, Y. -H., Shin, I. -G., Cha, S. -M., Kim, D. -J., Kim, H. -W., Kim, S. -L., Lee, C. -U., Yee, Y., Park, B. -G., Pogge, R. W., Street, R. A., Tsapras, Y., Hundertmark, M., Bachelet, E., Dominik, M., Horne, K., Jaimes, R. Figuera, Wambsganss, J., Bramich, D. M., Schmidt, R., Snodgrass, C., Steele, I. A., Menzies, J., Wang, Tianshu, Zhu, Wei, Mao, Shude, Bond, I. A., Gould, A., Udalski, A., Sumi, T., Bozza, V., Ranc, C., Cassan, A., Yee, J. C., Han, C., Abe, F., Asakura, Y., Barry, R., Bennett, D. P., Bhattacharya, A., Donachie, M., Evans, P., Fukui, A., Hirao, Y., Itow, Y., Kawasaki, K., Koshimoto, N., Li, M. C. A., Ling, C. H., Masuda, K., Matsubara, Y., Miyazaki, S., Muraki, Y., Nagakane, M., Ohnishi, K., Rattenbury, N., Saito, To., Sharan, A., Shibai, H., Sullivan, D. J., Suzuki, D., Tristram, P. J., Yamada, T., Yonehara, A., Pawlak, M., Pietrukowicz, P., Poleski, R., Skowron, J., Soszynski, I., KozLowski, S., Mroz, P., Ulaczyk, K., Szymanski, M. K., Beichman, C., Bryden, G., Novati, S. Calchi, Carey, S., Fausnaugh, M., Gaudi, B. S., Henderson, C. B., Shvartzvald, Y., Wibking, B., Albrow, M. D., Chung, S. -J., Hwang, K. -H., Jung, Y. K., Ryu, Y. -H., Shin, I. -G., Cha, S. -M., Kim, D. -J., Kim, H. -W., Kim, S. -L., Lee, C. -U., Yee, Y., Park, B. -G., Pogge, R. W., Street, R. A., Tsapras, Y., Hundertmark, M., Bachelet, E., Dominik, M., Horne, K., Jaimes, R. Figuera, Wambsganss, J., Bramich, D. M., Schmidt, R., Snodgrass, C., Steele, I. A., and Menzies, J.
Abstract: We present the analysis of the binary gravitational microlensing event MOA-2015-BLG-020. The event has a fairly long timescale (about 63 days) and thus the light curve deviates significantly from the lensing model that is based on the rectilinear lens-source relative motion. This enables us to measure the microlensing parallax through the annual parallax effect. The microlensing parallax parameters constrained by the ground-based data are confirmed by the Spitzer observations through the satellite parallax method. By additionally measuring the angular Einstein radius from the analysis of the resolved caustic crossing, the physical parameters of the lens are determined. It is found that the binary lens is composed of two dwarf stars with masses $M_1 = 0.606 \pm 0.028M_\odot$ and $M_2 = 0.125 \pm 0.006M_\odot$ in the Galactic disk. Assuming the source star is at the same distance as the bulge red clump stars, we find the lens is at a distance $D_L = 2.44 \pm 0.10 kpc$. In the end, we provide a summary and short discussion of all published microlensing events in which the annual parallax effect is confirmed by other independent observations., Comment: 16 pages, 5 figures
Published: 2017
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50. OGLE-2013-BLG-0132Lb and OGLE-2013-BLG-1721Lb: Two Saturn-mass Planets Discovered around M-dwarfs

Author: Mroz, Przemek, Udalski, A., Bond, I. A., Skowron, J., Sumi, T., Han, C., Szymanski, M. K., Soszynski, I., Poleski, R., Pietrukowicz, P., Kozlowski, S., Wyrzykowski, L., Ulaczyk, K., Abe, F., Asakura, Y., Barry, R. K., Bennett, D. P., Bhattacharya, A., Donachie, M., Evans, P., Fukui, A., Hirao, Y., Itow, Y., Koshimoto, N., Li, M. C. A., Ling, C. H., Masuda, K., Matsubara, Y., Muraki, Y., Nagakane, M., Ohnishi, K., Ranc, C., Rattenbury, N. J., Saito, To., Sharan, A., Sullivan, D. J., Suzuki, D., Tristram, P. J., Yamada, T., Yonehara, A., Mroz, Przemek, Udalski, A., Bond, I. A., Skowron, J., Sumi, T., Han, C., Szymanski, M. K., Soszynski, I., Poleski, R., Pietrukowicz, P., Kozlowski, S., Wyrzykowski, L., Ulaczyk, K., Abe, F., Asakura, Y., Barry, R. K., Bennett, D. P., Bhattacharya, A., Donachie, M., Evans, P., Fukui, A., Hirao, Y., Itow, Y., Koshimoto, N., Li, M. C. A., Ling, C. H., Masuda, K., Matsubara, Y., Muraki, Y., Nagakane, M., Ohnishi, K., Ranc, C., Rattenbury, N. J., Saito, To., Sharan, A., Sullivan, D. J., Suzuki, D., Tristram, P. J., Yamada, T., and Yonehara, A.
Abstract: We present the discovery of two planetary systems consisting of a Saturn-mass planet orbiting an M-dwarf, which were detected in faint microlensing events OGLE-2013-BLG-0132 and OGLE-2013-BLG-1721. The planetary anomalies were covered with high cadence by OGLE and MOA photometric surveys. The light curve modeling indicates that the planet-to-host mass ratios are $(5.15 \pm 0.28)\times 10^{-4}$ and $(13.18 \pm 0.72)\times 10^{-4}$, respectively. Both events were too short and too faint to measure a reliable parallax signal and hence the lens mass. We therefore used a Bayesian analysis to estimate the masses of both planets: $0.29^{+0.16}_{-0.13}\ M_{Jup}$ (OGLE-2013-BLG-0132Lb) and $0.64^{+0.35}_{-0.31}\ M_{Jup}$ (OGLE-2013-BLG-1721Lb). Thanks to a high relative proper motion, OGLE-2013-BLG-0132 is a promising candidate for the high-resolution imaging follow-up. Both planets belong to an increasing sample of sub-Jupiter-mass planets orbiting M-dwarfs beyond the snow line., Comment: Accepted to AJ
Published: 2017
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