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101. New limits from microlensing on Galactic Black Holes in the mass range 10xMsun < M < 1000xMsun

Author: Blaineau, T., Moniez, M., Afonso, C., Albert, J. -N., Ansari, R., Aubourg, E., Coutures, C., Glicenstein, J. -F., Goldman, B., Hamadache, C., Lasserre, T., LeGuillou, L., Lesquoy, E., Magneville, C., Marquette, J. -B., Palanque-Delabrouille, N., Perdereau, O., Rich, J., Spiro, M., Tisserand, P., Blaineau, T., Moniez, M., Afonso, C., Albert, J. -N., Ansari, R., Aubourg, E., Coutures, C., Glicenstein, J. -F., Goldman, B., Hamadache, C., Lasserre, T., LeGuillou, L., Lesquoy, E., Magneville, C., Marquette, J. -B., Palanque-Delabrouille, N., Perdereau, O., Rich, J., Spiro, M., and Tisserand, P.
Abstract: We have searched for long duration microlensing events originating from intermediate mass Black Holes (BH) in the halo of the Milky Way, using archival data from EROS-2 and MACHO photometric surveys towards the Large Magellanic Cloud. We combined data from these two surveys to create a common database of light curves for 14.1 million objects in LMC, covering a total duration of 10.6 years, with flux series measured through 4 wide band filters. We have carried out a microlensing search on these light curves, complemented by 22.7 million light curves, observed by EROS-2 only or MACHO only over about 7 years, with flux series measured through only 2 filters. A likelihood analysis, taking into account LMC self lensing and Milky Way disk contributions allows us to conclude that compact objects with masses in the range 10 - 100 Msun cannot make up more than ~15% of a standard halo total mass (at 95% confidence level). Our analysis sensitivity weakens for heavier objects, although we still exclude that ~ 50% of the halo be made of ~ 1000xMsun BHs. Combined with previous EROS results, an upper limit of ~ 15% of the total halo mass can be obtained for the contribution of compact halo objects in the mass range 10^{-6} - 10^2 Msun., Comment: 7 pages, 4 figures
Published: 2022

102. ExoClock Project. II. A Large-scale Integrated Study with 180 Updated Exoplanet Ephemerides

Author: Kokori, A., primary, Tsiaras, A., additional, Edwards, B., additional, Rocchetto, M., additional, Tinetti, G., additional, Bewersdorff, L., additional, Jongen, Y., additional, Lekkas, G., additional, Pantelidou, G., additional, Poultourtzidis, E., additional, Wünsche, A., additional, Aggelis, C., additional, Agnihotri, V. K., additional, Arena, C., additional, Bachschmidt, M., additional, Bennett, D., additional, Benni, P., additional, Bernacki, K., additional, Besson, E., additional, Betti, L., additional, Biagini, A., additional, Brandebourg, P., additional, Bretton, M., additional, Brincat, S. M., additional, Caló, M., additional, Campos, F., additional, Casali, R., additional, Ciantini, R., additional, Crow, M. V., additional, Dauchet, B., additional, Dawes, S., additional, Deldem, M., additional, Deligeorgopoulos, D., additional, Dymock, R., additional, Eenmäe, T., additional, Evans, P., additional, Esseiva, N., additional, Falco, C., additional, Ferratfiat, S., additional, Fowler, M., additional, Futcher, S. R., additional, Gaitan, J., additional, Horta, F. Grau, additional, Guerra, P., additional, Hurter, F., additional, Jones, A., additional, Kang, W., additional, Kiiskinen, H., additional, Kim, T., additional, Laloum, D., additional, Lee, R., additional, Lomoz, F., additional, Lopresti, C., additional, Mallonn, M., additional, Mannucci, M., additional, Marino, A., additional, Mario, J.-C., additional, Marquette, J.-B., additional, Michelet, J., additional, Miller, M., additional, Mollier, T., additional, Molina, D., additional, Montigiani, N., additional, Mortari, F., additional, Morvan, M., additional, Mugnai, L. V., additional, Naponiello, L., additional, Nastasi, A., additional, Neito, R., additional, Pace, E., additional, Papadeas, P., additional, Paschalis, N., additional, Pereira, C., additional, Perroud, V., additional, Phillips, M., additional, Pintr, P., additional, Pioppa, J.-B., additional, Popowicz, A., additional, Raetz, M., additional, Regembal, F., additional, Rickard, K., additional, Roberts, M., additional, Rousselot, L., additional, Rubia, X., additional, Savage, J., additional, Sedita, D., additional, Shave-Wall, D., additional, Sioulas, N., additional, Školník, V., additional, Smith, M., additional, St-Gelais, D., additional, Stouraitis, D., additional, Strikis, I., additional, Thurston, G., additional, Tomacelli, A., additional, Tomatis, A., additional, Trevan, B., additional, Valeau, P., additional, Vignes, J.-P., additional, Vora, K., additional, Vrašťák, M., additional, Walter, F., additional, Wenzel, B., additional, Wright, D. E., additional, and Zíbar, M., additional
Published: 2022
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103. The EChO science case

Author: Tinetti, Giovanna, primary, Drossart, Pierre, additional, Eccleston, Paul, additional, Hartogh, Paul, additional, Isaak, Kate, additional, Linder, Martin, additional, Lovis, Christophe, additional, Micela, Giusi, additional, Ollivier, Marc, additional, Puig, Ludovic, additional, Ribas, Ignasi, additional, Snellen, Ignas, additional, Swinyard, Bruce, additional, Allard, France, additional, Barstow, Joanna, additional, Cho, James, additional, Coustenis, Athena, additional, Cockell, Charles, additional, Correia, Alexandre, additional, Decin, Leen, additional, de Kok, Remco, additional, Deroo, Pieter, additional, Encrenaz, Therese, additional, Forget, Francois, additional, Glasse, Alistair, additional, Griffith, Caitlin, additional, Guillot, Tristan, additional, Koskinen, Tommi, additional, Lammer, Helmut, additional, Leconte, Jeremy, additional, Maxted, Pierre, additional, Mueller-Wodarg, Ingo, additional, Nelson, Richard, additional, North, Chris, additional, Pallé, Enric, additional, Pagano, Isabella, additional, Piccioni, Guseppe, additional, Pinfield, David, additional, Selsis, Franck, additional, Sozzetti, Alessandro, additional, Stixrude, Lars, additional, Tennyson, Jonathan, additional, Turrini, Diego, additional, Zapatero-Osorio, Mariarosa, additional, Beaulieu, Jean-Philippe, additional, Grodent, Denis, additional, Guedel, Manuel, additional, Luz, David, additional, Nørgaard-Nielsen, Hans Ulrik, additional, Ray, Tom, additional, Rickman, Hans, additional, Selig, Avri, additional, Swain, Mark, additional, Banaszkiewicz, Marek, additional, Barlow, Mike, additional, Bowles, Neil, additional, Branduardi-Raymont, Graziella, additional, du Foresto, Vincent Coudé, additional, Gerard, Jean-Claude, additional, Gizon, Laurent, additional, Hornstrup, Allan, additional, Jarchow, Christopher, additional, Kerschbaum, Franz, additional, Kovacs, Géza, additional, Lagage, Pierre-Olivier, additional, Lim, Tanya, additional, Lopez-Morales, Mercedes, additional, Malaguti, Giuseppe, additional, Pace, Emanuele, additional, Pascale, Enzo, additional, Vandenbussche, Bart, additional, Wright, Gillian, additional, Ramos Zapata, Gonzalo, additional, Adriani, Alberto, additional, Azzollini, Ruymán, additional, Balado, Ana, additional, Bryson, Ian, additional, Burston, Raymond, additional, Colomé, Josep, additional, Crook, Martin, additional, Di Giorgio, Anna, additional, Griffin, Matt, additional, Hoogeveen, Ruud, additional, Ottensamer, Roland, additional, Irshad, Ranah, additional, Middleton, Kevin, additional, Morgante, Gianluca, additional, Pinsard, Frederic, additional, Rataj, Mirek, additional, Reess, Jean-Michel, additional, Savini, Giorgio, additional, Schrader, Jan-Rutger, additional, Stamper, Richard, additional, Winter, Berend, additional, Abe, L., additional, Abreu, M., additional, Achilleos, N., additional, Ade, P., additional, Adybekian, V., additional, Affer, L., additional, Agnor, C., additional, Agundez, M., additional, Alard, C., additional, Alcala, J., additional, Prieto, C. Allende, additional, Alonso Floriano, F. J., additional, Altieri, F., additional, Alvarez Iglesias, C. A., additional, Amado, P., additional, Andersen, A., additional, Aylward, A., additional, Baffa, C., additional, Bakos, G., additional, Ballerini, P., additional, Banaszkiewicz, M., additional, Barber, R. J., additional, Barrado, D., additional, Barton, E. J., additional, Batista, V., additional, Bellucci, G., additional, Belmonte Avilés, J. A., additional, Berry, D., additional, Bézard, B., additional, Biondi, D., additional, Błęcka, M., additional, Boisse, I., additional, Bonfond, B., additional, Bordé, P., additional, Börner, P., additional, Bouy, H., additional, Brown, L., additional, Buchhave, L., additional, Budaj, J., additional, Bulgarelli, A., additional, Burleigh, M., additional, Cabral, A., additional, Capria, M. T., additional, Cassan, A., additional, Cavarroc, C., additional, Cecchi-Pestellini, C., additional, Cerulli, R., additional, Chadney, J., additional, Chamberlain, S., additional, Christian Jessen, N., additional, Ciaravella, A., additional, Claret, A., additional, Claudi, R., additional, Coates, A., additional, Cole, R., additional, Collur, A., additional, Cordier, D., additional, Covino, E., additional, Danielski, C., additional, Damasso, M., additional, Deeg, H. J., additional, Delgado-Mena, E., additional, Del Vecchio, C., additional, Demangeon, O., additional, De Sio, A., additional, De Wit, J., additional, Dobrijévi, M., additional, Doel, P., additional, Dominic, C., additional, Dorfi, E., additional, Eales, S., additional, Eiroa, C., additional, Espinoza Contreras, M., additional, Esposito, M., additional, Eymet, V., additional, Fabrizio, N., additional, Fernández, M., additional, Femenía Castella, B., additional, Figueira, P., additional, Filacchione, G., additional, Fletcher, L., additional, Focardi, M., additional, Fossey, S., additional, Fouqué, P., additional, Frith, J., additional, Galand, M., additional, Gambicorti, L., additional, Gaulme, P., additional, García López, R. J., additional, Garcia-Piquer, A., additional, Gear, W., additional, Gerard, J. -C., additional, Gesa, L., additional, Giani, E., additional, Gianotti, F., additional, Gillon, M., additional, Giro, E., additional, Giuranna, M., additional, Gomez, H., additional, Gomez-Leal, I., additional, Gonzalez Hernandez, J., additional, GonzÁlez Merino, B., additional, Graczyk, R., additional, Grassi, D., additional, Guardia, J., additional, Guio, P., additional, Gustin, J., additional, Hargrave, P., additional, Haigh, J., additional, Hébrard, E., additional, Heiter, U., additional, Heredero, R. L., additional, Herrero, E., additional, Hersant, F., additional, Heyrovsky, D., additional, Hollis, M., additional, Hubert, B., additional, Hueso, R., additional, Israelian, G., additional, Iro, N., additional, Irwin, P., additional, Jacquemoud, S., additional, Jones, G., additional, Jones, H., additional, Justtanont, K., additional, Kehoe, T., additional, Kerschbaum, F., additional, Kerins, E., additional, Kervell, P., additional, Kipping, D., additional, Koskinen, T., additional, Krupp, N., additional, Lahav, O., additional, Laken, B., additional, Lanza, N., additional, Lellouch, E., additional, Leto, G., additional, Goldaracena, J. Licandro, additional, Bertelloni, C. Lithgow, additional, Liu, S. J., additional, Cicero, U. Lo, additional, Lodieu, N., additional, Lognonné, P., additional, Puertas, M. Lopez, additional, Valverde, M. A. Lopez, additional, Rasmussen, I. Lundgaard, additional, Luntzer, A., additional, Machado, P., additional, Tavish, C. Mac, additional, Maggio, A., additional, Maillard, J. P., additional, Magnes, W., additional, Maldonado, J., additional, Mall, U., additional, Marquette, J. B., additional, Mauskopf, P., additional, Massi, F., additional, Maurin, A. S., additional, Medvedev, A., additional, Michaut, C., additional, Paez, P. Miles, additional, Montalto, M., additional, Rodríguez, P. Montañés, additional, Monteiro, M., additional, Montes, D., additional, Morais, H., additional, Morale, J. C., additional, Morales-Calderón, M., additional, Morello, G., additional, Martín, A. Moro, additional, Moses, J., additional, Bedon, A. Moya, additional, Alcaino, F. Murgas, additional, Oliva, E., additional, Orton, G., additional, Palla, F., additional, Pancrazzi, M., additional, Pantin, E., additional, Parmentier, V., additional, Parviainen, H., additional, Ramirez, Y. Pena, additional, Peralta, J., additional, Perez-Hoyos, S., additional, Petrov, R., additional, Pezzuto, S., additional, Pietrzak, R., additional, Pilat-Lohinger, E., additional, Piskunov, N., additional, Prinja, R., additional, Prisinzano, L., additional, Polichtchouk, I., additional, Poretti, E., additional, Radioti, A., additional, Ramos, A., additional, Rank-Luftinger, T., additional, Read, P., additional, Readorn, K., additional, Lopez, R. Rebolo, additional, Rebordao, J., additional, Rengel, M., additional, Rezac, L., additional, Rocchetto, M., additional, Rodler, F., additional, Bejar, J. Sanchez, additional, Sanchez Lavega, A., additional, Sanroma, E., additional, Santos, N., additional, Forcada, J. Sanz, additional, Scandariato, G., additional, Schmider, F.- X., additional, Scholz, A., additional, Scuderi, S., additional, Sethenadh, J., additional, Shore, S., additional, Showman, A., additional, Sicardy, B., additional, Sitek, P., additional, Smith, A., additional, Soret, L., additional, Sousa, S., additional, Stiepen, A., additional, Stolarski, M., additional, Strazzulla, G., additional, Tabernero, H. M., additional, Tanga, P., additional, Tecsa, M., additional, Temple, J., additional, Terenzi, L., additional, Tessenyi, M., additional, Testi, L., additional, Thompson, S., additional, Thrastarson, H., additional, Tingley, B. W., additional, Trifoglio, M., additional, Torres, J. Martin, additional, Tozzi, A., additional, Turrini, D., additional, Varley, R., additional, Vakili, F., additional, de Val-Borro, M., additional, Valdivieso, M. L., additional, Venot, O., additional, Villaver, E., additional, Vinatier, S., additional, Viti, S., additional, Waldmann, I., additional, Waltham, D., additional, Ward-Thompson, D., additional, Waters, R., additional, Watkins, C., additional, Watson, D., additional, Wawer, P., additional, Wawrzaszk, A., additional, White, G., additional, Widemann, T., additional, Winek, W., additional, Wi.niowski, T., additional, Yelle, R., additional, Yung, Y., additional, and Yurchenko, S. N., additional
Published: 2015
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104. EROS-II Variable Stars: Eclipsing Binaries in the EROS Microlensing Surveys

Author: Pritchard, J., Marquette, J. B., Tisserand, Patrick, Beaulieu, J. P., Lesquoy, E., Milsztajn, A., Giménez, Àlvaro, editor, Guinan, Edward, editor, Niarchos, Panagiotis, editor, and Rucinski, Slavek, editor
Published: 2006
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105. SF2A-2021: Proceedings of the Annual meeting of the French Society of Astronomy and Astrophysics

Author: Siebert, Arnaud, Baillie, Kevin, Lagadec, Eric, Lagarde, Nadège, Malzac, Julien, Marquette, J. B., N'Diaye, Mamadou, Richard, Johan, Venot, Olivia, Observatoire astronomique de Strasbourg (ObAS), Université de Strasbourg (UNISTRA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut de Mécanique Céleste et de Calcul des Ephémérides (IMCCE), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Lille-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Observatoire de la Côte d'Azur (OCA), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Interuniversitaire des Systèmes Atmosphériques (LISA (UMR_7583)), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Est Créteil Val-de-Marne - Paris 12 (UPEC UP12)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), and Baillie, Kevin
Subjects: [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], [SDU.ASTR] Sciences of the Universe [physics]/Astrophysics [astro-ph]
Published: 2021

106. A Jovian analogue orbiting a white dwarf star

Author: Blackman, J. W., primary, Beaulieu, J. P., additional, Bennett, D. P., additional, Danielski, C., additional, Alard, C., additional, Cole, A. A., additional, Vandorou, A., additional, Ranc, C., additional, Terry, S. K., additional, Bhattacharya, A., additional, Bond, I., additional, Bachelet, E., additional, Veras, D., additional, Koshimoto, N., additional, Batista, V., additional, and Marquette, J. B., additional
Published: 2021
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107. Characterizing Microlensing Planetary System OGLE-2014-BLG-0676Lb with Adaptive Optics Imaging

Author: Xie, Xiao-Jia, primary, Dong, Subo, additional, Shvartzvald, Yossi, additional, Andrew, Gould, additional, Udalski, Andrzej, additional, Beaulieu, J.-P., additional, Beichman, Charles, additional, Close, L. M., additional, Henderson, Calen B., additional, Males, J. R., additional, Marquette, J.-B., additional, Morzinski, K. M., additional, and Gelino, Christopher R., additional
Published: 2021
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108. A Jovian analogue orbiting a white dwarf star

Author: National Aeronautics and Space Administration (US), European Commission, Ministerio de Economía y Competitividad (España), Ministerio de Ciencia, Innovación y Universidades (España), Blackman, J. W., Beaulieu, J. P., Bennett, D. P., Danielski, Camilla, Alard, C., Cole, A. A., Vandorou, A., Ranc, C., Terry, S. K., Bhattacharya, A., Bond, I., Bachelet, E., Veras, D., Koshimoto, N., Batista, V., Marquette, J. B., National Aeronautics and Space Administration (US), European Commission, Ministerio de Economía y Competitividad (España), Ministerio de Ciencia, Innovación y Universidades (España), Blackman, J. W., Beaulieu, J. P., Bennett, D. P., Danielski, Camilla, Alard, C., Cole, A. A., Vandorou, A., Ranc, C., Terry, S. K., Bhattacharya, A., Bond, I., Bachelet, E., Veras, D., Koshimoto, N., Batista, V., and Marquette, J. B.
Abstract: Studies1,2 have shown that the remnants of destroyed planets and debris-disk planetesimals can survive the volatile evolution of their host stars into white dwarfs3,4, but few intact planetary bodies around white dwarfs have been detected5–8. Simulations predict9–11 that planets in Jupiter-like orbits around stars of ≲8 M☉ (solar mass) avoid being destroyed by the strong tidal forces of their stellar host, but as yet, there has been no observational confirmation of such a survivor. Here we report the non-detection of a main-sequence lens star in the microlensing event MOA-2010-BLG-477Lb12 using near-infrared observations from the Keck Observatory. We determine that this system contains a 0.53 ± 0.11 M☉ white-dwarf host orbited by a 1.4 ± 0.3 Jupiter-mass planet with a separation on the plane of the sky of 2.8 ± 0.5 astronomical units, which implies a semi-major axis larger than this. This system is evidence that planets around white dwarfs can survive the giant and asymptotic giant phases of their host’s evolution, and supports the prediction that more than half of white dwarfs have Jovian planetary companions13. Located at approximately 2.0 kiloparsecs towards the centre of our Galaxy, it is likely to represent an analogue to the end stages of the Sun and Jupiter in our own Solar System. © 2021, The Author(s), under exclusive licence to Springer Nature Limited.
Published: 2021

109. EChO: Exoplanet characterisation observatory

Author: Tinetti, G., Beaulieu, J. P., Henning, T., Meyer, M., Micela, G., Ribas, I., Stam, D., Swain, M., Krause, O., Ollivier, M., Pace, E., Swinyard, B., Aylward, A., van Boekel, R., Coradini, A., Encrenaz, T., Snellen, I., Zapatero-Osorio, M. R., Bouwman, J., Cho, J. Y-K., Coudé de Foresto, V., Guillot, T., Lopez-Morales, M., Mueller-Wodarg, I., Palle, E., Selsis, F., Sozzetti, A., Ade, P. A. R., Achilleos, N., Adriani, A., Agnor, C. B., Afonso, C., Prieto, C. Allende, Bakos, G., Barber, R. J., Barlow, M., Batista, V., Bernath, P., Bézard, B., Bordé, P., Brown, L. R., Cassan, A., Cavarroc, C., Ciaravella, A., Cockell, C., Coustenis, A., Danielski, C., Decin, L., Kok, R. De, Demangeon, O., Deroo, P., Doel, P., Drossart, P., Fletcher, L. N., Focardi, M., Forget, F., Fossey, S., Fouqué, P., Frith, J., Galand, M., Gaulme, P., Hernández, J. I. González, Grasset, O., Grassi, D., Grenfell, J. L., Griffin, M. J., Griffith, C. A., Grözinger, U., Guedel, M., Guio, P., Hainaut, O., Hargreaves, R., Hauschildt, P. H., Heng, K., Heyrovsky, D., Hueso, R., Irwin, P., Kaltenegger, L., Kervella, P., Kipping, D., Koskinen, T. T., Kovács, G., La Barbera, A., Lammer, H., Lellouch, E., Leto, G., Lopez Morales, M., Lopez Valverde, M. A., Lopez-Puertas, M., Lovis, C., Maggio, A., Maillard, J. P., Maldonado Prado, J., Marquette, J. B., Martin-Torres, F. J., Maxted, P., Miller, S., Molinari, S., Montes, D., Moro-Martin, A., Moses, J. I., Mousis, O., Nguyen Tuong, N., Nelson, R., Orton, G. S., Pantin, E., Pascale, E., Pezzuto, S., Pinfield, D., Poretti, E., Prinja, R., Prisinzano, L., Rees, J. M., Reiners, A., Samuel, B., Sánchez-Lavega, A., Forcada, J. Sanz, Sasselov, D., Savini, G., Sicardy, B., Smith, A., Stixrude, L., Strazzulla, G., Tennyson, J., Tessenyi, M., Vasisht, G., Vinatier, S., Viti, S., Waldmann, I., White, G. J., Widemann, T., Wordsworth, R., Yelle, R., Yung, Y., and Yurchenko, S. N.
Published: 2012
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110. OGLE-2017-BLG-1434Lb: Confirmation of a Cold Super-Earth Using Keck Adaptive Optics

Author: Blackman, J. W., primary, Beaulieu, J.-P., additional, Cole, A. A., additional, Koshimoto, N., additional, Vandorou, A., additional, Bhattacharya, A., additional, Marquette, J.-B., additional, and Bennett, D. P., additional
Published: 2021
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111. MagAO Observations of the Binary Microlens OGLE-2014-BLG-1050 Prefer the Higher-mass Solution

Author: Xie, Xiaojia, primary, Dong, Subo, additional, Zhu, Wei, additional, Gould, A., additional, Udalski, A., additional, Beaulieu, J.-P., additional, Close, L. M., additional, Males, J. R., additional, Marquette, J.-B., additional, Morzinski, K. M., additional, Pogge, R. W., additional, and Yee, J. C., additional
Published: 2021
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112. A Super-Jupiter Orbiting A Late-Type Star: A Refined Analysis of Microlensing Event OGLE-2012-BLG-0406

Author: Tsapras, Y, Choi, J.-Y, Street, R. A, Han, C, Bozza, V, Gould, A, Dominik, M, Beaulieu, J.-P, Udalski, A, Jørgensen, U. G, Sumi, T, Bramich, D. M, Browne, P, Horne, K, Hundertmark, M, Kains, N, Snodgrass, C, Steele, I. A, Andersen, J. M, Novati, S. Calchi, Diehl, C, Giannini, E, Hardis, S, Harpsøe, K, Hinse, T. C, Juncher, D, Kerins, E, Korhonen, H, Liebig, C, Mancini, L, Mathiasen, M, Penny, M. T, Rabus, M, Rahvar, S, Scarpetta, G, Skottfelt, J, Southworth, J, Tregloan-Reed, J, Vilela, C, Wambsganss, J, Skowron, J, Poleski, R, Kozłowski, S, Wyrzykowski, Ł, Szymański, M. K, Kubiak, M, Pietrukowicz, P, Pietrzyński, G, Soszyński, I, Ulaczyk, K, Albrow, M. D, Bachelet, E, Barry, R, Batista, V, Bhattacharya, A, Brillant, S, Caldwell, J. A. R, Cassan, A, Cole, A, Corrales, E, Coutures, Ch, Dieters, S, Prester, D. Dominis, Donatowicz, J, Fouqu, P, Greenhill, J, Kane, S. R, Kubas, D, Marquette, J. B, Menzies, J, Père, C, Pollard, K. R, Zub, M, Christie, G, DePoy, D. L, Dong, S, Gaudi, B. S, Henderson, C. B, Hwang, K. H, Jung, Y. K, Kavka, A, Koo, J.-R, Lee, C.-U, Maoz, D, Natusch, T, Ngan, H, Park, H, Pogge, R. W, Shin, I. G, Shvartzvald, Y, Yee, J. C, Abe, F, Bennett, D. P, Bond, I. A, Botzler, C. S, Freeman, M, Fukui, A, Fukunaga, D, Itow, Y, Koshimoto, N, Ling, C. H, Masuda, K, Matsubara, Y, Muraki, Y, Namba, S, Ohnishi, K, Rattenbury, N. J, Saito, To, Sullivan, D. J, Sweatman, W. L, Suzuki, D, Tristram, P. J, Tsurumi, N, Wada, K, Yamai, N, Yock, P. C. M, and Yonehara, A
Subjects: Astronomy, Astrophysics
Abstract: We present a detailed analysis of survey and follow-up observations of microlensing event OGLE-2012-BLG-0406 based on data obtained from 10 different observatories. Intensive coverage of the light curve, especially the perturbation part, allowed us to accurately measure the parallax effect and lens orbital motion. Combining our measurement of the lens parallax with the angular Einstein radius determined from finite-source effects, we estimate the physical parameters of the lens system. We find that the event was caused by a 2.73 plus or minus 0.43 M (sub J) planet orbiting a 0.44 plus or minus 0.07 solar mass early M-type star. The distance to the lens is 4.97 plus or minus 0.29 kpc and the projected separation between the host star and its planet at the time of the event is 3.45 plus or minus 0.26 AU. We find that the additional coverage provided by follow-up observations, especially during the planetary perturbation, leads to a more accurate determination of the physical parameters of the lens.
Published: 2014
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113. MICADO, the ELT first-light imager

Author: Matteo, P.D., Creevey, O., Crida, A., Kordopatis, G., Malzas, J., Marquette, J.-B., N'Diaye, M., Venot, O., and Astronomy
Subjects: ELT, observing modes, MCAO, MICADO, SCAO, science cases
Abstract: The MICADO instrument is the first light imager of the European ELT. It will work in the near-infrared (0.8-2.4 μm), over a large field (up to 50") and high sensitivity (similar to JWST). MICADO will benefit from two modes of adaptive optics correction: a MCAO correction, uniform on the field of MICADO and developed by the MAORY consortium, and a classic correction of the SCAO type, with high performance in the direction of the star guide and developed under the responsibility of the MICADO consortium. In a phased approach of the integration of adaptive optics to the ELT, MICADO will first be operational in SCAO mode. Offering four observing modes (imaging mode, astrometry, long-slit spectroscopy with R̃20000 and high contrast imaging), MICADO aims to scan a wide range of scientific objectives: small bodies and planets of the solar system, exoplanets and exo-disks, stellar populations in distant galaxies, black holes and the center of our galaxy, evolution and dynamics of galaxies.
Published: 2019

114. Discovery of a cool planet of 5.5 Earth masses through gravitational microlensing

Author: Beaulieu, J.-P., Bennett, D. P., Fouqué, P., Williams, A., Dominik, M., Jørgensen, U. G., Kubas, D., Cassan, A., Coutures, C., Greenhill, J., Hill, K., Menzies, J., Sackett, P. D., Albrow, M., Brillant, S., Caldwell, J. A. R., Calitz, J. J., Cook, K. H., Corrales, E., Desort, M., Dieters, S., Dominis, D., Donatowicz, J., Hoffman, M., Kane, S., Marquette, J.-B., Martin, R., Meintjes, P., Pollard, K., Sahu, K., Vinter, C., Wambsganss, J., Woller, K., Horne, K., Steele, I., Bramich, D. M., Burgdorf, M., Snodgrass, C., Bode, M., Udalski, A., Szymański, M. K., Kubiak, M., Więckowski, T., Pietrzyński, G., Soszyński, I., Szewczyk, O., Wyrzykowski, Ł., Paczyński, B., Abe, F., Bond, I. A., Britton, T. R., Gilmore, A. C., Hearnshaw, J. B., Itow, Y., Kamiya, K., Kilmartin, P. M., Korpela, A. V., Masuda, K., Matsubara, Y., Motomura, M., Muraki, Y., Nakamura, S., Okada, C., Ohnishi, K., Rattenbury, N. J., Sako, T., Sato, S., Sasaki, M., Sekiguchi, T., Sullivan, D. J., Tristram, P. J., Yock, P. C. M., and Yoshioka, T.
Published: 2006

115. Ion-Molecule Reactions at Dense Interstellar Cloud Temperatures: The Cresus Apparatus

Author: Marquette, J.-B., Greenberg, J. M., editor, and Pirronello, V., editor
Published: 1991
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116. A chemical survey of exoplanets with ARIEL

Author: Tinetti, Giovanna, Drossart, Pierre, Eccleston, Paul, Hartogh, Paul, Heske, Astrid, Leconte, J., Micela, Giusi, Ollivier, Marc, Pilbratt, Göran, Puig, Ludovic, Turrini, Diego, Vandenbussche, Bart, Wolkenberg, Paulina, Beaulieu, Jean-Philippe, Buchave, Lars A., Ferus, Martin, Griffin, Matt, Guedel, Manuel, Justtanont, Kay, Lagage, Pierre-Olivier, Machado, Pedro, Malaguti, Giuseppe, Min, Michiel, Nørgaard-Nielsen, Hans Ulrik, Rataj, Mirek, Ray, Tom, Ribas, Ignasi, Swain, Mark, Szabo, Robert, Werner, Stephanie, Barstow, Joanna, Burleigh, Matt, Cho, James, Du Foresto, Vincent Coudé, Coustenis, Athena, Decin, Leen, Encrenaz, Thérèse, Galand, Marina, Gillon, Michael, Helled, Ravit, Morales, Juan Carlos, Muñoz, Antonio García, Moneti, Andrea, Pagano, Isabella, Pascale, Enzo, Piccioni, Giuseppe, Pinfield, David, Sarkar, Subhajit, Selsis, Franck, Tennyson, Jonathan, Triaud, Amaury, Venot, Olivia, Waldmann, Ingo, Waltham, David, Wright, Gillian, Amiaux, Jerome, Auguères, Jean-Louis, Berthé, Michel, Bezawada, Naidu, Bishop, Georgia, Bowles, Neil, Coffey, Deirdre, Colomé, Josep, Crook, Martin, Crouzet, Pierre-Elie, Da Peppo, Vania, Sanz, Isabel Escudero, Focardi, Mauro, Frericks, Martin, Hunt, Tom, Kohley, Ralf, Middleton, Kevin, Morgante, Gianluca, Ottensamer, Roland, Pace, Emanuele, Pearson, Chris, Stamper, Richard, Symonds, Kate, Rengel, Miriam, Renotte, Etienne, Ade, Peter, Affer, Laura, Alard, Christophe, Allard, Nicole, Altieri, Francesca, André, Yves, Arena, Claudio, Argyriou, Ioannis, Aylward, Alan, Baccani, Cristian, Bakos, Gaspar, Banaszkiewicz, Marek, Barlow, Mike, Batista, Virginie, Bellucci, Giancarlo, Benatti, Serena, Bernardi, Pernelle, Bézard, Bruno, Blecka, Maria, Bolmont, Emeline, Bonfond, Bertrand, Bonito, Rosaria, Bonomo, Aldo S., Brucato, John Robert, Brun, Allan Sacha, Bryson, Ian, Bujwan, Waldemar, Casewell, Sarah, Charnay, Benjamin, Pestellini, Cesare Cecchi, Chen, Guo, Ciaravella, Angela, Claudi, Riccardo, Clédassou, Rodolphe, Damasso, Mario, Damiano, Mario, Danielski, Camilla, Deroo, Pieter, Di Giorgio, Anna Maria, Dominik, Carsten, Doublier, Vanessa, Doyle, Simon, Doyon, Rene, Drummond, Benjamin, Duong, Bastien, Eales, Stephen, Edwards, Billy, Farina, Maria, Flaccomio, Ettore, Fletcher, Leigh, Forget, François, Fossey, Steve, Fränz, Markus, Fujii, Yuka, García-Piquer, Álvaro, Gear, Walter, Geoffray, Hervé, Gérard, Jean Claude, Gesa, Lluis, Gomez, H., Graczyk, Rafał, Griffith, Caitlin, Grodent, Denis, Guarcello, Mario Giuseppe, Gustin, Jacques, Hamano, Keiko, Hargrave, Peter, Hello, Yann, Heng, Kevin, Herrero, Enrique, Hornstrup, Allan, Hubert, Benoît, Ida, Shigeru, Ikoma, Masahiro, Iro, Nicolas, Irwin, Patrick, Jarchow, Christopher, Jaubert, Jean, Jones, Hugh, Julien, Queyrel, Kameda, Shingo, Kerschbaum, Franz, Kervella, Pierre, Koskinen, Tommi, Krijger, Matthijs, Krupp, Norbert, Lafarga, Marina, Landini, Federico, Lellouch, Emmanuel, Leto, Giuseppe, Luntzer, A., Rank-Lüftinger, Theresa, Maggio, Antonio, Maldonado, Jesus, Maillard, Jean-Pierre, Mall, Urs, Marquette, J.-B., Mathis, Stéphane, Maxted, Pierre, Matsuo, Taro, Medvedev, Alexander, Miguel, Yamila, Minier, Vincent, Morello, Giuseppe, Mura, Alessandro, Narita, Norio, Nascimbeni, Valerio, Nguyen Tong, N., Noce, Vladimiro, Oliva, Fabrizio, Palle, Enric, Palmer, Paul, Pancrazzi, Maurizio, Papageorgiou, Andreas, Parmentier, Vivien, Perger, Manuel, Petralia, Antonino, Pezzuto, Stefano, Pierrehumbert, Ray, Pillitteri, Ignazio, Piotto, Giampaolo, Pisano, Giampaolo, Prisinzano, Loredana, Radioti, Aikaterini, Reess, Jean-Michel, Rezac, Ladislav, Rocchetto, Marco, Rosich, Albert, Sanna, Nicoletta, Santerne, Alexandre, Savini, Giorgio, Scandariato, Gaetano, Sicardy, Bruno, Sierra, Carles, Sindoni, Giuseppe, Skup, Konrad, Snellen, Ignas, Sobiecki, Mateusz, Soret, Lauriane, Sozzetti, Alessandro, Stiepen, Arnaud, Strugarek, Antoine, Taylor, Jake, Taylor, William, Terenzi, Luca, Tessenyi, Marcell, Tsiaras, Angelos, Tucker, C., Valencia, Diana, Vasisht, Gautam, Vazan, Allona, Vilardell, Francesc, Vinatier, Sandrine, Viti, Serena, Waters, Rens, Wawer, Piotr, Wawrzaszek, Anna, Whitworth, Anthony, Yung, Yuk L., Yurchenko, Sergey N., Osorio, María Rosa Zapatero, Zellem, Robert, Zingales, Tiziano, Zwart, Frans, Wolkenberg, Paul, Beaulieu, Jean, Buchave, A., Lagage, Pierre, Ray, Ray, Ribas, Ignas, du Foresto, Vincent, Muñoz, Antonio, Auguères, Jean, Crouzet, Pierre, Pace, Emanuel, Altieri, Francesc, Claudi, Claudio, Brun, Bruno, Bonomo, Aldo, Brucato, Robert, Brun, Allan, Di Giorgio, Anna, Fujii, Yuk, Gérard, Jean, Guarcello, Giuseppe, Maillard, Pierre, Yung, Yuk, Yurchenko, Sergey, Science and Technology Facilities Council (STFC), University College of London [London] (UCL), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Max Planck Institute for Solar System Research (MPS), Max-Planck-Gesellschaft, ECLIPSE 2018, Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), INAF - Osservatorio Astronomico di Palermo (OAPa), Istituto Nazionale di Astrofisica (INAF), Institut de Génomique Fonctionnelle de Lyon (IGFL), Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut National de la Recherche Agronomique (INRA)-École normale supérieure - Lyon (ENS Lyon), University of Valencia, Istituto di Fisica dello Spazio Interplanetario (IFSI), Consiglio Nazionale delle Ricerche (CNR), Space Research Centre of Polish Academy of Sciences (CBK), Polska Akademia Nauk = Polish Academy of Sciences (PAN), Institut d'Astrophysique de Paris (IAP), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), J. Heyrovský Institute of Physical Chemistry, Czech Academy of Sciences [Prague] (CAS), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Department of Genetics [Cambridge], University of Cambridge [UK] (CAM), Dpto. de Organización de Empresas, Escuela Técnica Superior de Ingeniería Industrial de Barcelona, Universitat Politècnica de Catalunya [Barcelona] (UPC), University of California, University of California [Davis] (UC Davis), University of California-University of California, Institute of Astronomy [Leuven], Catholic University of Leuven - Katholieke Universiteit Leuven (KU Leuven), Institut d'Astrophysique et de Géophysique [Liège], Université de Liège, Department of Earth and Space Sciences [Los Angeles], University of California [Los Angeles] (UCLA), Instituto de Investigaciones Químicas, CSIC, Istituto di Astrofisica e Planetologia Spaziali - INAF (IAPS), Cardiff University, Department of Physics and Astronomy [UCL London], School of Physics and Astronomy [Birmingham], University of Birmingham [Birmingham], Royal Holloway [University of London] (RHUL), CEA, Commissariat à l'Energie Atomique, Gyf Sur Yvette, France, Université Paris Diderot - Paris 7 (UPD7), Department of Atmospheric, Oceanic and Planetary Physics [Oxford] (AOPP), University of Oxford [Oxford], European Space Astronomy Centre (ESAC), European Space Agency (ESA), Galaxies, Etoiles, Physique, Instrumentation (GEPI), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Centre National de la Recherche Scientifique (CNRS), Centro di Ateneo di Studi e Attività Spaziali 'Giuseppe Colombo' (CISAS), Universita degli Studi di Padova, ECLIPSE 2014, Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux (L3AB), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Observatoire aquitain des sciences de l'univers (OASU), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS)-Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Bordeaux (UB), Laboratoire de Physique Atmosphérique et Planétaire (LPAP), INAF - Osservatorio Astrofisico di Arcetri (OAA), Tsinghua University [Beijing] (THU), Departement de physique and Observatoire du Mont Megantic, Université de Montréal (UdeM), Laboratoire de Météorologie Dynamique (UMR 8539) (LMD), Département des Géosciences - ENS Paris, École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-École des Ponts ParisTech (ENPC)-École polytechnique (X)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Service d'Hématologie, Earth-Life Science Institute [Tokyo] (ELSI), Tokyo Institute of Technology [Tokyo] (TITECH), Géoazur (GEOAZUR 6526), Institut de Recherche pour le Développement (IRD)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Instituto Universitario de Electroquimica, Universidad de Alicante, Laboratoire de paléontologie et paleogéographie du paleozoique (LPPP), Université de Lille, Sciences et Technologies-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Dept of Physics, University of Florida [Gainesville] (UF), Centre National d'Études Spatiales [Toulouse] (CNES), University of Hertfordshire [Hatfield] (UH), University of Vienna [Vienna], M2A 2018, Maintenance Myélinique et Neuropathies Périphériques (MMNP), Institut Génomique, Environnement, Immunité, Santé, Thérapeutique (GEIST), Université de Limoges (UNILIM)-Université de Limoges (UNILIM), Département Sciences de la Fabrication et Logistique (SFL-ENSMSE), École des Mines de Saint-Étienne (Mines Saint-Étienne MSE), Institut Mines-Télécom [Paris] (IMT)-Institut Mines-Télécom [Paris] (IMT)-CMP-GC, Joseph Louis LAGRANGE (LAGRANGE), Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), University of Verona (UNIVR), Interdisciplinary Centre for Security, Reliability and Trust [Luxembourg] (SnT), Université du Luxembourg (Uni.lu), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), IIIA, CSIC, Laboratory for Atmospheric and Space Physics [Boulder] (LASP), University of Colorado [Boulder], Indiana University [Bloomington], Indiana University System, Laboratoire de Cosmologie, Astrophysique Stellaire & Solaire, de Planétologie et de Mécanique des Fluides (CASSIOPEE), Université Nice Sophia Antipolis (... - 2019) (UNS), California Institute of Technology (CALTECH), Natural Resources Canada (NRCan), Computer Science Department of University of Malaga, Universidad de Málaga [Málaga] = University of Málaga [Málaga], BioWooEB (UPR BioWooEB), Centre de Coopération Internationale en Recherche Agronomique pour le Développement (Cirad), Max-Planck-Institut für Sonnensystemforschung = Max Planck Institute for Solar System Research (MPS), École normale supérieure de Lyon (ENS de Lyon)-Institut National de la Recherche Agronomique (INRA)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS), National Research Council of Italy | Consiglio Nazionale delle Ricerche (CNR), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), University of California (UC)-University of California (UC), University of Oxford, Agence Spatiale Européenne = European Space Agency (ESA), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Università degli Studi di Padova = University of Padua (Unipd), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Observatoire aquitain des sciences de l'univers (OASU), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS)-Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-École polytechnique (X)-École des Ponts ParisTech (ENPC)-Centre National de la Recherche Scientifique (CNRS)-Département des Géosciences - ENS Paris, École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS-PSL), Institut de Recherche pour le Développement (IRD)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Université Nice Sophia Antipolis (1965 - 2019) (UNS), Université Nice Sophia Antipolis (1965 - 2019) (UNS), Università degli studi di Verona = University of Verona (UNIVR), Centre de Coopération Internationale en Recherche Agronomique pour le Développement (Cirad)-Université de Montpellier (UM), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), École normale supérieure - Lyon (ENS Lyon)-Institut National de la Recherche Agronomique (INRA)-Université Claude Bernard Lyon 1 (UCBL), Polska Akademia Nauk (PAN), Czech Academy of Sciences [Prague] (ASCR), Department of Genetics, University of Cambridge, PSL Research University (PSL)-PSL Research University (PSL)-Centre National de la Recherche Scientifique (CNRS), Tsinghua University [Beijing], Université de Montréal [Montréal], École normale supérieure - Paris (ENS Paris)-École normale supérieure - Paris (ENS Paris), Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), University of Florida [Gainesville], Maintenance myélinique et neuropathies périphériques (MMNP), Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Observatoire de la Côte d'Azur, Università degli Studi di Verona, Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Universidad de Málaga [Málaga], BioWooEB (Cirad-Persyst-UPR 114 BioWooEB), Département Performances des systèmes de production et de transformation tropicaux (Cirad-PERSYST), Centre de Coopération Internationale en Recherche Agronomique pour le Développement (Cirad)-Centre de Coopération Internationale en Recherche Agronomique pour le Développement (Cirad), University of Zurich, Tinetti, Giovanna, Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Nice Sophia Antipolis (... - 2019) (UNS), Université Côte d'Azur (UCA)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), and Low Energy Astrophysics (API, FNWI)
Subjects: Solar System, STELLAR ACTIVITY, 010504 meteorology & atmospheric sciences, [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], 7. Clean energy, 01 natural sciences, Space missions, Astrobiology, Planet, QB460, TRANSMISSION SPECTRUM, Transit (astronomy), TRANSITING EXOPLANETS, 010303 astronomy & astrophysics, QC, Eclipse, QB, Super-Earth, 520 Astronomy, Exoplanets, Exoplanet, BROWN DWARF, IR spectroscopy, Spacemissions, Physical Sciences, 3103 Astronomy and Astrophysics, VALIDATED PLANETS, Molecular signatures, Astrophysics::Earth and Planetary Astrophysics, JUPITER EXOPLANETS, 530 Physics, Gas giant, Brown dwarf, SUPER-EARTH, Astronomy & Astrophysics, EXTRASOLAR GIANT PLANETS, INFRARED-EMISSION-SPECTRUM, 1912 Space and Planetary Science, 0103 physical sciences, QB600, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Science & Technology, Astronomy and Astrophysics, 500 Science, 0201 Astronomical And Space Sciences, 13. Climate action, Space and Planetary Science, 10231 Institute for Computational Science, SPACE-BASED PHOTOMETRY
Abstract: Thousands of exoplanets have now been discovered with a huge range of masses, sizes and orbits: from rocky Earth-like planets to large gas giants grazing the surface of their host star. However, the essential nature of these exoplanets remains largely mysterious: there is no known, discernible pattern linking the presence, size, or orbital parameters of a planet to the nature of its parent star. We have little idea whether the chemistry of a planet is linked to its formation environment, or whether the type of host star drives the physics and chemistry of the planet’s birth, and evolution. The Atmospheric Remote-sensing Infrared Exoplanet Large-survey (ARIEL) has been selected by the European Space Agency as the next mediumclass science mission, M4, to address these scientific questions. ARIEL was conceived to observe a large number (~1000) of transiting planets for statistical understanding, including gas giants, Neptunes, super-Earths and Earth-size planets around a range of host star types using transit spectroscopy in the 1.25-7.8 μm spectral range and multiple narrow-band photometry in the optical. ARIEL will focus on warm and hot planets to take advantage of their well-mixed atmospheres which should show minimal condensation and sequestration of high-Z materials compared to their colder Solar System siblings. Said warm and hot atmospheres are expected to be more representative of the planetary bulk composition. Observations of these warm/hot exoplanets, and in particular of their elemental composition (especially C, O, N, S, Si), will allow the understanding of the early stages of planetary and atmospheric formation during the nebular phase and the following few million years. ARIEL will thus provide a representative picture of the chemical nature of the exoplanets and relate this directly to the type and chemical environment of the host star. ARIEL is designed as a dedicated survey mission for combined-light spectroscopy, capable of observing a large and well-defined planet sample within its 4-year mission lifetime. Transit, eclipse and phase-curve spectroscopy methods, whereby the signal from the star and planet are differentiated using knowledge of the planetary ephemerides, allow us to measure atmospheric signals from the planet at levels of 10-100 part per million (ppm) relative to the star and, given the bright nature of targets, also allows more sophisticated techniques, such as eclipse mapping, to give a deeper insight into the nature of the atmosphere. These types of observations require a stable payload and satellite platform with broad, instantaneous wavelength coverage to detect many molecular species, probe the thermal structure, identify clouds and monitor the stellar activity. The wavelength range proposed covers all the expected major atmospheric gases from e.g. H2O, CO2, CH4 NH3, HCN, H2S through to the more exotic metallic compounds, such as TiO, VO, and condensed species. Simulations of ARIEL performance in conducting exoplanet surveys have been performed – using conservative estimates of mission performance and a full model of all significant noise sources in the measurement – using a list of potential ARIEL targets that incorporates the latest available exoplanet statistics. The conclusion at the end of the Phase A study, is that ARIEL – in line with the stated mission objectives – will be able to observe about 1000 exoplanets depending on the details of the adopted survey strategy, thus confirming the feasibility of the main science objectives.
Published: 2018

117. 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., The MOA Collaboration, Szymański, M. K., Poleski, R., Soszyński, I., Ulaczyk, K., Wyrzykowski, Ł., The OGLE Collaboration, DePoy, D., Gould, A., Pogge, R. W., Yee, J. C., The μFUN Collaboration, Albrow, M. D., Bachelet, E., Batista, V., Bowens- Rubin, R., Brillant, S., Caldwell, J. A. R., Cole, A., Coutures, C., Dieters, S., Dominis Prester, Dijana, 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.
Subjects: gravitational lensin, micro, planetary systems, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: 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 ⊙, and planet, m p = 0.54 ± 0.10M Jup, at a projected star– planet separation of a ⊥ = 2.42 ± 0.26 au, corresponding to a semimajor axis of a=2.9≥nfrac{; ; ; ; ; ; ; }; ; ; ; ; ; ; {; ; ; ; ; ; ; }; ; ; ; ; ; ; {; ; ; ; ; ; ; 0em}; ; ; ; ; ; ; {; ; ; ; ; ; ; }; ; ; ; ; ; ; {; ; ; ; ; ; ; +1.6}; ; ; ; ; ; ; {; ; ; ; ; ; ; -0.6}; ; ; ; ; ; ; 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 D S = 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

118. WFIRST Exoplanet Mass-measurement Method Finds a Planetary Mass of 39 ± 8 M ⊕ for OGLE-2012-BLG-0950Lb

Author: Bhattacharya, A., primary, Beaulieu, J.-P., additional, Bennett, D. P., additional, Anderson, J., additional, Koshimoto, N., additional, Lu, J. R., additional, Batista, V., additional, Blackman, J. W., additional, Bond, I. A., additional, Fukui, A., additional, Henderson, C. B., additional, Hirao, Y., additional, Marquette, J. B., additional, Mroz, P., additional, Ranc, C., additional, and Udalski, A., additional
Published: 2018
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119. MOA-2016-BLG-227Lb: A Massive Planet Characterized by Combining Light-curve Analysis and Keck AO Imaging

Author: Koshimoto, N., Shvartzvald, Y., Bennett, D. P., Penny, M. T., Hundertmark, M., Bond, I. A., Zang, W. C., Henderson, C. B., Suzuki, D., Rattenbury, N. J., Sumi, T., Abe, F., Asakura, Y., Bhattacharya, A., Donachie, M., Evans, P., Fukui, A., Hirao, Y., Itow, Y., Li, M. C. A., Ling, C. H., Masuda, K., Matsubara, Y., Matsuo, T., Muraki, Y., Nagakane, M., Ohnishi, K., Ranc, C., Saito, To., Sharan, A., Shibai, H., Sullivan, D. J., Tristram, P. J., Yamada, T., Yonehara, A., Gelino, C. R., Beichman, C., Beaulieu, J.-P., Marquette, J.-B., Batista, V., Friedmann, M., Hallakoun, N., Kaspi, S., Maoz, D., Bryden, G., Novati, S. Calchi, Howell, S. B., Wang, T. S., Mao, S., Fouqué, P., Korhonen, H., Jørgensen, U. G., Street, R., Tsapras, Y., Dominik, M., Kerins, E., Cassan, A., Snodgrass, C., Bachelet, E., Bozza, V., Bramich, D. M., University of St Andrews. St Andrews Centre for Exoplanet Science, and University of St Andrews. School of Physics and Astronomy
Subjects: Proper motion, NDAS, Flux, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Gravitational microlensing, 01 natural sciences, micro [Gravitational lensing], law.invention, Telescope, law, Planet, 0103 physical sciences, QB Astronomy, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, QC, Astrophysics::Galaxy Astrophysics, QB, Physics, Earth and Planetary Astrophysics (astro-ph.EP), 010308 nuclear & particles physics, Astronomy and Astrophysics, Mass ratio, Light curve, Planetary systems, Stars, QC Physics, Space and Planetary Science, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract: We report the discovery of a microlensing planet --- MOA-2016-BLG-227Lb --- with a large planet/host mass ratio of $q \simeq 9 \times 10^{-3}$. This event was located near the $K2$ Campaign 9 field that was observed by a large number of telescopes. As a result, the event was in the microlensing survey area of a number of these telescopes, and this enabled good coverage of the planetary light curve signal. High angular resolution adaptive optics images from the Keck telescope reveal excess flux at the position of the source above the flux of the source star, as indicated by the light curve model. This excess flux could be due to the lens star, but it could also be due to a companion to the source or lens star, or even an unrelated star. We consider all these possibilities in a Bayesian analysis in the context of a standard Galactic model. Our analysis indicates that it is unlikely that a large fraction of the excess flux comes from the lens, unless solar type stars are much more likely to host planets of this mass ratio than lower mass stars. We recommend that a method similar to the one developed in this paper be used for other events with high angular resolution follow-up observations when the follow-up observations are insufficient to measure the lens-source relative proper motion., Comment: 35 pages, 7 figures, 6 tables, Accepted for publication in AJ
Published: 2017

120. CombiningSpitzerParallax and Keck II Adaptive Optics Imaging to Measure the Mass of a Solar-like Star Orbited by a Cold Gaseous Planet Discovered by Microlensing

Author: Beaulieu, J.-P., primary, Batista, V., additional, Bennett, D. P., additional, Marquette, J.-B., additional, Blackman, J. W., additional, Cole, A. A., additional, Coutures, C., additional, Danielski, C., additional, Prester, D. Dominis, additional, Donatowicz, J., additional, Fukui, A., additional, Koshimoto, N., additional, Lončarić, K., additional, Morales, J. C., additional, Sumi, T., additional, Suzuki, D., additional, Henderson, C., additional, Shvartzvald, Y., additional, and Beichman, C., additional
Published: 2018
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121. MOA-2016-BLG-227Lb:A Massive Planet Characterized by Combining Light-curve Analysis and Keck AO Imaging

Author: Koshimoto, N., Shvartzvald, Y., Bennett, D. P., Penny, M. T., Hundertmark, M., Bond, I. A., Zang, W. C., Henderson, Calen B., Suzuki, D., Rattenbury, N. J., Sumi, T., Abe, Fumiko, Asakura, Y., Bhattacharya, A., Donachie, A.M., Evans, Tom P., Li, M. C. A., Ling, C. H., Masuda, K., Matsubara, Yoichi, Matsuo, T., Muraki, Y., Nagakane, M., Ohnishi, K., Ranc, C., Saito, To., Sharan, A., Shibai, H., Sullivan, D. J., Tristram, P.J., Yamada, T., Yonehara, A., Gelino, C. R., Beichman, C. A., Beaulieu, J.-P, Marquette, J.-B, Batista, V., Friedmann, M., Hallakoun, N., Kaspi, S., Maoz, Dan, Bryden, G., Novati, S. Calchi, Howell, Steve B., Wang, T. S., Mao, Shenlan, Fouque, P., Korhonen, H., Jorgensen, U. G., Street, R., Kerins, E., Bachelet, E., Bozza, V., Bramich, D. M., Koshimoto, N., Shvartzvald, Y., Bennett, D. P., Penny, M. T., Hundertmark, M., Bond, I. A., Zang, W. C., Henderson, Calen B., Suzuki, D., Rattenbury, N. J., Sumi, T., Abe, Fumiko, Asakura, Y., Bhattacharya, A., Donachie, A.M., Evans, Tom P., Li, M. C. A., Ling, C. H., Masuda, K., Matsubara, Yoichi, Matsuo, T., Muraki, Y., Nagakane, M., Ohnishi, K., Ranc, C., Saito, To., Sharan, A., Shibai, H., Sullivan, D. J., Tristram, P.J., Yamada, T., Yonehara, A., Gelino, C. R., Beichman, C. A., Beaulieu, J.-P, Marquette, J.-B, Batista, V., Friedmann, M., Hallakoun, N., Kaspi, S., Maoz, Dan, Bryden, G., Novati, S. Calchi, Howell, Steve B., Wang, T. S., Mao, Shenlan, Fouque, P., Korhonen, H., Jorgensen, U. G., Street, R., Kerins, E., Bachelet, E., Bozza, V., and Bramich, D. M.
Published: 2017

122. Searching for Periodic Variables in the EROS-2 Database

Author: Dubath, P., Lecoeur, I., Rimoldini, L., Süveges, M., Blomme, J., López, M., Sarro, L. M., De Ridder, J., Cuypers, J., Guy, L., Nienartowicz, K., Jan, A., Beck, M., Mowlavi, N., Ordóñez-Blanco, D., Marquette, J. B., Beaulieu, J. P., Tisserand, P., Lesquoy, É., Eyer, L., Dubath, P., Lecoeur, I., Rimoldini, L., Süveges, M., Blomme, J., López, M., Sarro, L. M., De Ridder, J., Cuypers, J., Guy, L., Nienartowicz, K., Jan, A., Beck, M., Mowlavi, N., Ordóñez-Blanco, D., Marquette, J. B., Beaulieu, J. P., Tisserand, P., Lesquoy, É., and Eyer, L.
Abstract: We started a systematic search for periodic variable-star candidates in the EROS-2 database in the context of preparatory work for the Gaia satellite mission. The goal is to evaluate different classification tools and strategies, and to identify a large sample of variable candidates. In this paper we present the results of an assessment study of a three-step identification and classification process. In the study we took a sample of about 80,000 stars from one of the LMC EROS fields
Published: 2017

123. Measurements Of Ion-Molecule Reaction Rate Coefficients Between 8 and 160 K by the Cresu Technique

Author: Rowe, B. R., Marquette, J. B., Dupeyrat, G., Diercksen, G. H. F., editor, Huebner, W. F., editor, and Langhoff, P. W., editor
Published: 1985
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124. SUB-SATURN PLANET MOA-2008-BLG-310Lb: LIKELY TO BE IN THE GALACTIC BULGE

Author: Janczak, Julia, Fukui, A., Dong, Subo, Monard, B., Kozlowski, Szymon, Gould, A., Beaulieu, J. P., Kubas, Daniel, Marquette, J. B., Sumi, T., Bond, I. A., Bennett, D. P., collaboration, the MOA, collaboration, the MicroFUN, collaboration, the MiNDSTEp, and collaboration, the PLANET
Subjects: Earth and Planetary Astrophysics (astro-ph.EP), Physics, 010308 nuclear & particles physics, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Mass ratio, Light curve, Gravitational microlensing, Astrophysics - Astrophysics of Galaxies, 01 natural sciences, Exoplanet, Einstein radius, 13. Climate action, Space and Planetary Science, Primary (astronomy), Planet, Astrophysics of Galaxies (astro-ph.GA), 0103 physical sciences, Astrophysics::Earth and Planetary Astrophysics, 010303 astronomy & astrophysics, Planetary mass, Astrophysics::Galaxy Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract: We report the detection of sub-Saturn-mass planet MOA-2008-BLG-310Lb and argue that it is the strongest candidate yet for a bulge planet. Deviations from the single-lens fit are smoothed out by finite-source effects and so are not immediately apparent from the light curve. Nevertheless, we find that a model in which the primary has a planetary companion is favored over the single-lens model by \Delta\chi^2 ~ 880 for an additional three degrees of freedom. Detailed analysis yields a planet/star mass ratio q=(3.3+/-0.3)x10^{-4} and an angular separation between the planet and star within 10% of the angular Einstein radius. The small angular Einstein radius, \theta_E=0.155+/-0.011 mas, constrains the distance to the lens to be D_L>6.0 kpc if it is a star (M_L>0.08 M_sun). This is the only microlensing exoplanet host discovered so far that must be in the bulge if it is a star. By analyzing VLT NACO adaptive optics images taken near the baseline of the event, we detect additional blended light that is aligned to within 130 mas of the lensed source. This light is plausibly from the lens, but could also be due to a companion to lens or source, or possibly an unassociated star. If the blended light is indeed due to the lens, we can estimate the mass of the lens, M_L=0.67+/-0.14 M_sun, planet mass m=74+/-17 M_Earth, and projected separation between the planet and host, 1.25+/-0.10 AU, putting it right on the "snow line". If not, then the planet has lower mass, is closer to its host and is colder. To distinguish among these possibilities on reasonable timescales would require obtaining Hubble Space Telescope images almost immediately, before the source-lens relative motion of \mu=5 mas yr^{-1} causes them to separate substantially., Comment: 36 pages, 8 figures, Submitted to ApJ
Published: 2010

125. A companion on the planet/brown dwarf mass boundary on a wide orbit discovered by gravitational microlensing

Author: Poleski, R., primary, Udalski, A., additional, Bond, I. A., additional, Beaulieu, J. P., additional, Clanton, C., additional, Gaudi, S., additional, Szymański, M. K., additional, Soszyński, I., additional, Pietrukowicz, P., additional, Kozłowski, Szymon, additional, Skowron, J., additional, Wyrzykowski, Ł., additional, Ulaczyk, K., additional, Bennett, D. P., additional, Sumi, T., additional, Suzuki, D., additional, Rattenbury, N. J., additional, Koshimoto, N., additional, Abe, F., additional, Asakura, Y., additional, Barry, R. K., additional, Bhattacharya, A., additional, Donachie, M., additional, Evans, P., additional, Fukui, A., additional, Hirao, Y., additional, Itow, Y., additional, Li, M. C. A., additional, Ling, C. H., additional, Masuda, K., additional, Matsubara, Y., additional, Muraki, Y., additional, Nagakane, M., additional, Ohnishi, K., additional, Ranc, C., additional, Saito, To., additional, Sharan, A., additional, Sullivan, D. J., additional, Tristram, P. J., additional, Yamada, T., additional, Yonehara, A., additional, Batista, V., additional, and Marquette, J. B., additional
Published: 2017
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126. The Star Blended with the MOA-2008-BLG-310 Source Is Not the Exoplanet Host Star

Author: Bhattacharya, A., primary, Bennett, D. P., additional, Anderson, J., additional, Bond, I. A., additional, Gould, A., additional, Batista, V., additional, Beaulieu, J. P., additional, Fouqué, P., additional, Marquette, J. B, additional, and Pogge, R., additional
Published: 2017
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127. Spectroscopic characterisation of microlensing events

Author: Santerne, A., primary, Beaulieu, J.-P., additional, Rojas Ayala, B., additional, Boisse, I., additional, Schlawin, E., additional, Almenara, J.-M., additional, Batista, V., additional, Bennett, D., additional, Díaz, R. F., additional, Figueira, P., additional, James, D. J., additional, Herter, T., additional, Lillo-Box, J., additional, Marquette, J. B., additional, Ranc, C., additional, Santos, N. C., additional, and Sousa, S. G., additional
Published: 2016
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128. Red noise versus planetary interpretations in the microlensing event OGLE-2013-BLG-446

Author: Bachelet, E, Bramich, DM, Han, C, Greenhill, J, Street, RA, Gould, A, D'Ago, G, AlSubai, K, Dominik, M, Jaimes, RF, Horne, K, Hundertmark, M, Kains, N, Snodgrass, C, Steele, IA, Tsapras, Y, Albrow, MD, Batista, V, Beaulieu, J-P, Bennett, DP, Brillant, S, Caldwell, JAR, Cassan, A, Cole, A, Coutures, C, Dieters, S, Prester, DD, Donatowicz, J, Fouque, P, Hill, K, Marquette, J-B, Menzies, J, Pere, C, Ranc, C, Wambsganss, J, Warren, D, De Almeida, LA, Choi, J-Y, DePoy, DL, Dong, S, Hung, L-W, Hwang, K-H, Jablonski, F, Jung, YK, Kaspi, S, Klein, N, Lee, C-U, Maoz, D, Munoz, JA, Nataf, D, Park, H, Pogge, RW, Polishook, D, Shin, I-G, Shporer, A, Yee, JC, Abe, F, Bhattacharya, A, Bond, IA, Botzler, CS, Freeman, M, Fukui, A, Itow, Y, Koshimoto, N, Ling, CH, Masuda, K, Matsubara, Y, Muraki, Y, Ohnishi, K, Philpott, LC, Rattenbury, N, Saito, T, Sullivan, DJ, Sumi, T, Suzuki, D, Tristram, PJ, Yonehara, A, Bozza, V, Novati, SC, Ciceri, S, Galianni, P, Gu, S-H, Harpsoe, K, Hinse, TC, Jorgensen, UG, Juncher, D, Korhonen, H, Mancini, L, Melchiorre, C, Popovas, A, Postiglione, A, Rabus, M, Rahvar, S, Schmidt, RW, Scarpetta, G, Skottfelt, J, Southworth, J, Stabile, A, Surdej, J, Wang, X-B, Wertz, O, Collaboration, R, Collaboration, PLANET, Collaboration, FUN, Collaboration, MOA, Collaboration, M, The Royal Society, Science & Technology Facilities Council, and University of St Andrews. School of Physics and Astronomy
Subjects: Nuclear and High Energy Physics, NDAS, gravitational lensing: micro, planetary systems, techniques: photometric, FOS: Physical sciences, Astrophysics, Gravitational microlensing, micro [Gravitational lensing], Settore FIS/05 - Astronomia e Astrofisica, False positive paradox, QB Astronomy, QC, QB, Event (probability theory), Physics, Earth and Planetary Astrophysics (astro-ph.EP), High magnification, photometric [Techniques], Astronomy and Astrophysics, Light curve, Exoplanet, Planetary systems, QC Physics, 13. Climate action, Space and Planetary Science, Colors of noise, Parallax, Astrophysics - Earth and Planetary Astrophysics
Abstract: For all exoplanet candidates, the reliability of a claimed detection needs to be assessed through a careful study of systematic errors in the data to minimize the false positives rate. We present a method to investigate such systematics in microlensing datasets using the microlensing event OGLE-2013-BLG-0446 as a case study. The event was observed from multiple sites around the world and its high magnification (A_{max} \sim 3000) allowed us to investigate the effects of terrestrial and annual parallax. Real-time modeling of the event while it was still ongoing suggested the presence of an extremely low-mass companion (\sim 3M_\oplus ) to the lensing star, leading to substantial follow-up coverage of the light curve. We test and compare different models for the light curve and conclude that the data do not favour the planetary interpretation when systematic errors are taken into account., Comment: accepted ApJ 2015
Published: 2015
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129. OGLE-2011-BLG-0265Lb: A JOVIAN MICROLENSING PLANET ORBITING AN M DWARF

Author: Skowron, J., Shin, I. -G., Udalski, A., Han, C., Sumi, T., Shvartzvald, Y., Gould, A., Dominis Prester, D., Street, R. A., Jørgensen, U. G., Bennett, D. P., Bozza, V., Szymański, M. K., Kubiak, M., Pietrzyński, G., Soszyński, I., Poleski, R., Kozłowski, S., Pietrukowicz, P., Ulaczyk, K., Wyrzykowski, Ł., OGLE Collaboration, Abe, F., Bhattacharya, A., Bond, I. A., Botzler, C. S., Freeman, M., Fukui, A., Fukunaga, D., Itow, Y., Ling, C. H., Koshimoto, N., Masuda, K., Matsubara, Y., Muraki, Y., Namba, S., Ohnishi, K., Philpott, L. C., Rattenbury, N., Saito, T., Sullivan, D. J., Suzuki, D., Tristram, P. J., Yock, P. C. M., MOA Collaboration, Maoz, D., Kaspi, S., Friedmann, M., Wise Group, Almeida, L. A., Batista, V., Christie, G., Choi, J. -Y., DePoy, D. L., Gaudi, B. S., Henderson, C., Hwang, K. -H., Jablonski, F., Jung, Y. K., Lee, C. -U., McCormick, J., Natusch, T., Ngan, H., Park, H., Pogge, R. W., Yee, J. C., μFUN Collaboration, Albrow, M. D., Bachelet, E., Beaulieu, J. -P., Brillant, S., Caldwell, J. A. R., Cassan, A., Cole, A., Corrales, E., Coutures, Ch., Dieters, S., Donatowicz, J., Fouqué, P., Greenhill, J., Kains, N., Kane, S. R., Kubas, D., Marquette, J. -B., Martin, R., Menzies, J., Pollard, K. R., Ranc, C., Sahu, K. C., Wambsganss, J., Williams, A., Wouters, D., PLANET Collaboration, Tsapras, Y., Bramich, D. M., Horne, K., Hundertmark, M., Snodgrass, C., Steele, I. A., RoboNet Collaboration, Alsubai, K. A., Browne, P., Burgdorf, M. J., Calchi Novati, S., Dodds, P., Dominik, M., Dreizler, S., Fang, X. -S., Gu, C. -H., Hardis, Harpsøe, K., Hessman, F. V., Hinse, T. C., Hornstrup, A., Jessen-Hansen, J., Kerins, E., Liebig, C., Lund, M., Lundkvist, M., Mancini, L., Mathiasen, M., Penny, M. T., Rahvar, S., RICCI, DAVIDE, Scarpetta, G., Skottfelt, J., Southworth, J., Surdej, J., Tregloan-Reed, J., Wertz, O., MiNDSTEp Consortium, ITA, USA, GBR, DEU, ESP, BEL, KOR, DNK, IND, IRN, MEX, The Royal Society, Science & Technology Facilities Council, and University of St Andrews. School of Physics and Astronomy
Subjects: Star (game theory), FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, GALACTIC BULGE, Gravitational microlensing, Jovian, JUPITER/SATURN ANALOG, Jupiter, Settore FIS/05 - Astronomia e Astrofisica, Planet, Bulge, ANGULAR SIZES, QB Astronomy, Astrophysics::Solar and Stellar Astrophysics, planetary systems, QC, Astrophysics::Galaxy Astrophysics, QB, Earth and Planetary Astrophysics (astro-ph.EP), Physics, Astronomy and Astrophysics, 3rd-DAS, Planetary system, MASS PLANET, Light curve, OGLE-III, SNOW LINE, GRAVITATIONAL BINARY-LENS, QC Physics, SURFACE BRIGHTNESS RELATIONS, GIANT PLANETS, Space and Planetary Science, micro [gravitational lensing], Astrophysics::Earth and Planetary Astrophysics, STARS, Astrophysics - Earth and Planetary Astrophysics
Abstract: We report the discovery of a Jupiter-mass planet orbiting an M-dwarf star that gave rise to the microlensing event OGLE-2011-BLG-0265. Such a system is very rare among known planetary systems and thus the discovery is important for theoretical studies of planetary formation and evolution. High-cadence temporal coverage of the planetary signal combined with extended observations throughout the event allows us to accurately model the observed light curve. The final microlensing solution remains, however, degenerate yielding two possible configurations of the planet and the host star. In the case of the preferred solution, the mass of the planet is $M_{\rm p} = 0.9\pm 0.3\ M_{\rm J}$, and the planet is orbiting a star with a mass $M = 0.22\pm 0.06\ M_\odot$. The second possible configuration (2$\sigma$ away) consists of a planet with $M_{\rm p}=0.6\pm 0.3\ M_{\rm J}$ and host star with $M=0.14\pm 0.06\ M_\odot$. The system is located in the Galactic disk 3 -- 4 kpc towards the Galactic bulge. In both cases, with an orbit size of 1.5 -- 2.0 AU, the planet is a "cold Jupiter" -- located well beyond the "snow line" of the host star. Currently available data make the secure selection of the correct solution difficult, but there are prospects for lifting the degeneracy with additional follow-up observations in the future, when the lens and source star separate., Comment: 10 pages, 2 tables, 5 figures. Accepted in ApJ
Published: 2015

130. 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, Bramich, D M, Dominik, M, Figuera Jaimes, R, Horne, K, Mao, S, Menzies, J, Schmidt, R, Snodgrass, C, and Steele, I A
Subjects: PARALLAX, STELLAR mass, TELESCOPES, GRAVITATIONAL lenses, GALACTIC bulges, CORONAL mass ejections, LIGHT curves
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 |$M_{\star 1} = 0.87 \pm 0.12 \, \mathrm{M}_{\odot }$| and |$M_{\star 2} = 0.77 \pm 0.11 \, \mathrm{M}_{\odot }$|⁠. The distance to the lensing system is 6.41 ± 0.14 kpc and the projected separation between the two components is 13.85 ± 0.16 au. Alternative interpretations are also considered. [ABSTRACT FROM AUTHOR]
Published: 2019
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131. Reactions of N+(3P) ions with normal, para, and deuterated hydrogens at low temperatures.

Author: Marquette, J. B., Rebrion, C., and Rowe, B. R.
Subjects: *NITROGEN, *IONS, *HYDROGEN, *DEUTERON reactions
Abstract: The reactions of N+(3P) ions with normal, para, and deuterated hydrogens have been examined at temperatures below 163 K by using the CRESU technique with both helium and nitrogen buffer gases. All these reactions have decreasing rate coefficients with decreasing temperature. Comparison of the data for normal and para-H2 reveals the drastic importance of rotational energy in promoting these processes. Analysis of these results shows a better agreement between the n-H2, p-H2, and HD data if the spin–orbit energy of N+(3P) is also considered as efficient as kinetic and rotational energies in driving the reactions. It follows that the endothermicity of the reaction N+(3P0) +H2(X 1Σ+g,J=0) →NH+(X 2Π,J=0) +H(2S) is (18±2) meV. This yields a proton affinity of N equal to (3.524±0.003) eV and a dissociation energy of NH of (3.42±0.01) eV. [ABSTRACT FROM AUTHOR]
Published: 1988
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132. Reactions of Ar+ with H2, N2, O2, and CO at 20, 30, and 70 K.

Author: Rebrion, C., Rowe, B. R., and Marquette, J. B.
Subjects: CHEMICAL reactions, ARGON, IONS, HELIUM, EXCHANGE reactions
Abstract: Reactions of Ar+(2P3/2) ions with H2, N2, O2, and CO have been studied with the CRESU apparatus at 30 K in argon buffer gas and with the newly developed mass-selected ion injector (CRESUS configuration) at 20 and 70 K in helium buffer gas. The atom exchange reaction with H2 is rather fast, with a rate coefficient k showing a small energy dependence well represented by k=1.5×10-9E0.16 cm3 s-1 with the collision energy in the center-of-mass frame, E, in the range 2.5×10-3-0.65 eV. This result is more compatible with a frozen-rotor capture model rather than with a threshold model for endoergic reactions. Concerning the reaction with N2, a competition between the two exit channels involving the two first vibrational levels of the N+2 product ion explains the minimum of the rate constant suggested at about 140 K by previous SIFT experiments [D. Smith and N. G. Adams, Phys. Rev. A 23, 2327 (1981)] and presently confirmed. The rate coefficients for the charge transfer reactions with O2 and CO increase with decreasing energy, i.e., k=9.6×10-12E-0.51 and k=1.1×10-11E-0.47 cm3 s-1, respectively, for E in the range 2.5×10-3-0.3 eV. Both these reactions proceed via an intimate collision mechanism. [ABSTRACT FROM AUTHOR]
Published: 1989
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133. Studies of the reaction of O+2 with deuterated methanes.

Author: Barlow, S. E., Van Doren, J. M., DePuy, C. H., Bierbaum, V. M., Dotan, I., Ferguson, E. E., Adams, N. G., Smith, D., Rowe, B. R., Marquette, J. B., Dupeyrat, G., and Durup-Ferguson, M.
Subjects: METHANE, MOLECULES, TEMPERATURE, DEUTERIUM
Abstract: In the gas phase O+2 reacts with methane at 300 K to produce a hydrogen atom and the CH3O+2 ion. The structure of this ion has recently been determined to be H2COOH+, methylene hydroperoxide ion. The reaction rate coefficients and product distributions have now been measured at 300 K for the CHnD4-n isotopes. The reaction shows both inter- and intramolecular isotope effects, e.g., CH2D2 reacts more slowly than methane and more rapidly than CD4, but loses hydrogen or deuterium with equal probability. The ion readily transfers HO+ to alkenes, CS2, and many other neutral molecules. The reaction with CS2 has been used to investigate the isotopic distribution within mixed isotope product ions. In addition, the reaction rate coefficients for both CH4 and CD4 have been measured as functions of temperature between 20 and 500 K; in both cases a clear minimum is observed in the reaction rate coefficient near room temperature. A mechanism for the reaction is proposed which allows us to model the temperature dependence of the reaction rate coefficient over the entire range for which there are data. [ABSTRACT FROM AUTHOR]
Published: 1986
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134. Study of the reactions N+2+2N2→N+4+N2 and O+2+2O2→O+4+O2 from 20 to 160 K by the CRESU technique.

Author: Rowe, B. R., Dupeyrat, G., Marquette, J. B., and Gaucherel, P.
Published: 1984
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135. The reaction O+2+CH4 → CH3O+2+H studied from 20 to 560 K in a supersonic jet and in a SIFT.

Author: Rowe, B. R., Dupeyrat, G., Marquette, J. B., Smith, D., Adams, N. G., and Ferguson, E. E.
Published: 1984
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136. MOA-2011-BLG-262Lb: A Sub-Earth-Mass Moon Orbiting a Gas Giant Primary or a High Velocity Planetary System in the Galactic Bulge

Author: Bennett, D.P., Batista, V., Bond, I.A., Bennett, C.S., Suzuki, D., Beaulieu, J.-P., Udalski, A., Donatowicz, J., Bozza, V., Abe, F., Botzler, C.S., Freeman, M., Fukunaga, D., Fukui, A., Itow, Y., Koshimoto, N., Ling, C.H., Masuda, K., Matsubara, Y., Muraki, Y., Namba, S., Ohnishi, K., Rattenbury, N.J., Saito, T., Sullivan, D.J., Sumi, T., Sweatman, W.L., Tristram, P.J., Tsurumi, N., Wada, K., Yock, P.C.M., Albrow, M.D., Bachelet, E., Brillant, S., Caldwell, J.A.R., Cassan, A., Cole, A.A., Corrales, E., Coutures, C., Dieters, S., Dominis Prester, D., Fouqué, P., Greenhill, J., Horne, K., Koo, J.-R., Kubas, D., Marquette, J.-B., Martin, R., Menzies, J.W., Sahu, K.C., Wambsganss, J., Williams, A., Zub, M., Choi, J.Y., Depoy, D.L., Dong, S., Gaudi, B.S., Gould, A., Han, C., Henderson, C.B., McGregor, D., Lee, C.-U., Pogge, R.W., Shin, I.-G., Yee, J.C., Szymański, M.K., Skowron, J., Poleski, R., Kozłowski, S., Wyrzykowski, Ł., Kubiak, M., Pietrukowicz, P., Pietrzyński, G., Soszyński, I., Ulaczyk, K., Tsapras, Y., Street, R.A., Dominik, M., Bramich, D.M., Browne, P., Hundertmark, M., Kains, N., Snodgrass, C., Steele, I.A., Dekany, I., Gonzalez, O.A., Heyrovský, D., Kandori, R., Kerins, E., Lucas, P.W., Minniti, D., Nagayama, T., Rejkuba, M., Robin, A.C., Saito, A.R., The Royal Society, Science & Technology Facilities Council, University of St Andrews. School of Physics and Astronomy, Ohio State University [Columbus] (OSU), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Astronomical Observatory [Warsaw], Faculty of Physics [Warsaw] (FUW), University of Warsaw (UW)-University of Warsaw (UW), Okayama Astrophysical Observatory, National Astronomical Observatory of Japan (NAOJ), Nagoya University, Osaka University [Osaka], Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Univers, Transport, Interfaces, Nanostructures, Atmosphère et environnement, Molécules (UMR 6213) (UTINAM), Université de Franche-Comté (UFC), and Université Bourgogne Franche-Comté [COMUE] (UBFC)-Université Bourgogne Franche-Comté [COMUE] (UBFC)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)
Subjects: Proper motion, 010504 meteorology & atmospheric sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Gravitational microlensing, 7. Clean energy, 01 natural sciences, micro [Gravitational lensing], Jupiter, Planet, 0103 physical sciences, QB Astronomy, 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, QC, Astrophysics::Galaxy Astrophysics, QB, 0105 earth and related environmental sciences, Physics, Exomoon, Giant planet, Astronomy, Astronomy and Astrophysics, Planetary system, Exoplanet, Planetary systems, QC Physics, 13. Climate action, Space and Planetary Science, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], BDC
Abstract: D.P.B. was supported by grants NASA-NNX12AF54G, JPL-RSA 1453175 and NSF AST-1211875. This MOA project is supported by the grants JSPS18253002 and JSPS20340052. T.S. acknowledges the financial support from the JSPS, JSPS23340044, JSPS24253004. This work was partially supported by a NASA Keck PI Data Award, administered by the NASA Exoplanet Science Institute. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. B.S.G. and A.G. were supported by NSF grant AST 110347. B.S.G., A.G., R.P.G. were supported by NASA grant NNX12AB99G. S.D. was partly supported through a Ralph E. and Doris M. Hansmann Membership at the IAS and by NSF grant AST-0807444. Work by J.C.Y. was performed in part under contract with the California Institute of Technology (Caltech) funded by NASA through the Sagan Fellowship Program. The OGLE project has received funding from the European Research Council under the European Community's Seventh Framework Programme (FP7/2007-2013)/ERC grant agreement No. 246678 to A.U. D.H. was supported by Czech Science Foundation grant GACR P209/10/1318. D.M.B., M.D., K.H., C.S., R.A.S., M.H. and Y.T. are supported by NPRP grant NPRP-09-476-1-78 from the Qatar National Research Fund (a member of the Qatar Foundation). We present the first microlensing candidate for a free-floating exoplanet-exomoon system, MOA-2011-BLG-262, with a primary lens mass of M host ~ 4 Jupiter masses hosting a sub-Earth mass moon. The argument for an exomoon hinges on the system being relatively close to the Sun. The data constrain the product MLπrel where ML is the lens system mass and πrel is the lens-source relative parallax. If the lens system is nearby (large πrel), then ML is small (a few Jupiter masses) and the companion is a sub-Earth-mass exomoon. The best-fit solution has a large lens-source relative proper motion, μrel = 19.6 ± 1.6 mas yr–1, which would rule out a distant lens system unless the source star has an unusually high proper motion. However, data from the OGLE collaboration nearly rule out a high source proper motion, so the exoplanet+exomoon model is the favored interpretation for the best fit model. However, there is an alternate solution that has a lower proper motion and fits the data almost as well. This solution is compatible with a distant (so stellar) host. A Bayesian analysis does not favor the exoplanet+exomoon interpretation, so Occam's razor favors a lens system in the bulge with host and companion masses of M host = 0.12 +0.19-0.06 MΘ and mcomp = 18+28-10M⊕, at a projected separation of a⊥ = 0.84+0.25−0.14 AU. The existence of this degeneracy is an unlucky accident, so current microlensing experiments are in principle sensitive to exomoons. In some circumstances, it will be possible to definitively establish the mass of such lens systems through the microlensing parallax effect. Future experiments will be sensitive to less extreme exomoons. Publisher PDF
Published: 2014

137. MOA-2010-BLG-328Lb: A SUB-NEPTUNE ORBITING VERY LATE M DWARF?

Author: Furusawa, K, Udalski, A, Sumi, T, Bennett, DP, Bond, IA, Gould, A, Jorgensen, UG, Snodgrass, C, Prester, DD, Albrow, MD, Abe, F, Botzler, CS, Chote, P, Freeman, M, Fukui, A, Harris, P, Itow, Y, Ling, CH, Masuda, K, Matsubara, Y, Miyake, N, Muraki, Y, Ohnishi, K, Rattenbury, NJ, Saito, T, Sullivan, DJ, Suzuki, D, Sweatman, WL, Tristram, PJ, Wada, K, Yock, PCM, Szymanski, MK, Soszynski, I, Kubiak, M, Poleski, R, Ulaczyk, K, Pietrzynski, G, Wyrzykowski, L, Choi, J-Y, Christie, GW, Depoy, DL, Dong, S, Drummond, J, Gaudi, BS, Han, C, Hung, L-W, Hwang, K-H, Lee, C-U, McCormick, J, Moorhouse, D, Natusch, T, Nola, M, Ofek, E, Pogge, RW, Shin, I-G, Skowron, J, Thornley, G, Yee, JC, Alsubai, KA, Bozza, V, Browne, P, Burgdorf, MJ, Novati, SC, Dodds, P, Dominik, M, Finet, F, Gerner, T, Hardis, S, Harpsoe, K, Hinse, TC, Hundertmark, M, Kains, N, Kerins, E, Liebig, C, Mancini, L, Mathiasen, M, Penny, MT, Proft, S, Rahvar, S, Ricci, D, Scarpetta, G, Schafer, S, Schonebeck, F, Southworth, J, Surdej, J, Wambsganss, J, Street, RA, Bramich, DM, Steele, IA, Tsapras, Y, Horne, K, Donatowicz, J, Sahu, KC, Bachelet, E, Batista, V, Beatty, TG, Beaulieu, J-P, Bennett, CS, Black, C, Bowens-Rubin, R, Brillant, S, Caldwell, JAR, Cassan, A, Cole, AA, Corrales, E, Coutures, C, Dieters, S, Fouque, P, Greenhill, J, Henderson, CB, Kubas, D, Marquette, J-B, Martin, R, Menzies, JW, Shappee, B, Williams, A, Wouters, D, Van Saders, J, Zellem, R, Zub, M, Collaboration, O, Collaboration, FUN, Consortium, M, Collaboration, R, Collaboration, P, and Collaboration, TMOA
Subjects: QB460
Abstract: We analyze the planetary microlensing event MOA-2010-BLG-328. The best fit yields host and planetary masses of M h = 0.11 ± 0.01 M ☉ and M p = 9.2 ± 2.2 M ⊕, corresponding to a very late M dwarf and sub-Neptune-mass planet, respectively. The system lies at D L = 0.81 ± 0.10 kpc with projected separation r ⊥ = 0.92 ± 0.16 AU. Because of the host's a priori unlikely close distance, as well as the unusual nature of the system, we consider the possibility that the microlens parallax signal, which determines the host mass and distance, is actually due to xallarap (source orbital motion) that is being misinterpreted as parallax. We show a result that favors the parallax solution, even given its close host distance. We show that future high-resolution astrometric measurements could decisively resolve the remaining ambiguity of these solutions.
Published: 2013

138. The VMC ESO Public Survey

Author: Cioni, M. -R L., Anders, P., Bagheri, G., Bekki, K., Clementini, G., Emerson, J., Evans, C. J., For, B. -Q, Grijs, R., Gibson, B., Girardi, L., Groenewegen, M. A. T., Guandalini, R., Gullieuszik, M., Valentin Ivanov, Kamath, D., Marconi, M., Marquette, J. -B, Miszalski, B., Moore, B., Moretti, M. I., Muraveva, T., Napiwotzki, R., Oliveira, J. M., Piatti, A. E., Ripepi, V., Romita, K., Rubele, S., Sturm, R., Tatton, B., Loon, J. Th, Wilkinson, M. I., Wood, P. R., and Zaggia, S.
Subjects: Astrophysics of Galaxies (astro-ph.GA), MAGALLANIC, CLOUDS, FOS: Physical sciences, Astrophysics - Astrophysics of Galaxies
Abstract: The VISTA near-infrared YJKs survey of the Magellanic Clouds system (VMC) has entered its core phase: about 40% of the observations across the Large and Small Magellanic Clouds (LMC, SMC), the Magellanic Bridge and Stream have already been secured and the data are processed and analysed regularly. The initial analyses, concentrated in the first two completed tiles in the LMC (6_6 including 30 Doradus and 8_8 including the South Ecliptic Pole), show the superior quality of the data. The depth of the VMC survey allows the derivation of the star formation history (SFH) with unprecedented quality compared to previous wide-area surveys while reddening maps of high angular resolution are constructed using red clump stars. The multi-epoch Ks-band data reveal tight period-luminosity relations for variable stars and they permit the measurement of accurate proper motions of the stellar populations. The VMC survey continues to acquire data that will address many issues in the field of star and galaxy evolution., Comment: 3 pages, 4 figures
Published: 2013

139. Combined analysis of the binary lens caustic-crossing event MACHO 98-SMC-1

Author: Afonso, C, Alard, C, Albert, J N, Andersen, J, Ansari, R, Aubourg, E, Bareyre, P, Bauer, F, Beaulieu, J P, Bouquet, A, Char, S, Charlot, X, Couchot, F, Coutures, C, Derue, F, Ferlet, R, Glicenstein, J F, Goldman, B, Gould, A, Graff, D, Gros, M, Haissinski, J, Hamilton, J C, Hardin, D, de Kat, J, Kim, A, Lasserre, T, Lesquoy, E, Loup, C, Magneville, C, Marquette, J B, Maurice, E, Milsztajn, A, Moniez, M, Palanque-Delabrouille, N, Perdereau, O, Prevot, L, Regnault, N, Rich, J, Spiro, M, Vidal-Madjar, A, Vigroux, L, Zylberajch, S, Alcock, C, Allsman, R A, Alves, D, Axelrod, TS, Becker, A C, Peterson, B A, Szymanski, M, Dominik, Martin, Naber, R M, Sackett, Penny D, Kapteyn Astronomical Institute, and Astronomy
Subjects: Lens (geometry), Physics, Proper motion, MICROLENSING EVENT, 010308 nuclear & particles physics, Astrophysics (astro-ph), gravitational lensing, FOS: Physical sciences, Binary number, Astronomy and Astrophysics, Astrophysics, Mass ratio, Gravitational microlensing, 01 natural sciences, dark matter, Einstein radius, Space and Planetary Science, Limb darkening, 0103 physical sciences, Magellanic Clouds, astrometry, PHOTOMETRY, Small Magellanic Cloud, 010303 astronomy & astrophysics
Abstract: We fit the data for the binary-lens microlensing event MACHO 98-SMC-1 from 5 different microlensing collaborations and find two distinct solutions characterized by binary separation d and mass ratio q: (d,q)=(0.54,0.50) and (d,q)=(3.65,0.36), where d is in units of the Einstein radius. However, the relative proper motion of the lens is very similar in the two solutions, 1.30 km/s/kpc and 1.48 km/s/kpc, thus confirming that the lens is in the Small Magellanic Cloud. The close binary can be either rotating or approximately static but the wide binary must be rotating at close its maximum allowed rate to be consistent with all the data. We measure limb-darkening coefficients for five bands ranging from I to V. As expected, these progressively decrease with rising wavelength. This is the first measurement of limb darkening for a metal-poor A star., 29 pages + 9 figures + 2 tables, submitted to ApJ
Published: 2000

140. REVISITING THE MICROLENSING EVENT OGLE 2012-BLG-0026: A SOLAR MASS STAR WITH TWO COLD GIANT PLANETS

Author: Beaulieu, J.-P., primary, Bennett, D. P., additional, Batista, V., additional, Fukui, A., additional, Marquette, J.-B., additional, Brillant, S., additional, Cole, A. A., additional, Rogers, L. A., additional, Sumi, T., additional, Abe, F., additional, Bhattacharya, A., additional, Koshimoto, N., additional, Suzuki, D., additional, Tristram, P. J., additional, Han, C., additional, Gould, A., additional, Pogge, R., additional, and Yee, J., additional
Published: 2016
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141. Microlensing Discovery of a Population of Very Tight, Very Low-mass Binary Brown Dwarfs

Author: Choi, J.-Y., Han, C., Udalski, A., Sumi, T., Gaudi, B. S., Gould, A., Bennett, D. P., Dominik, M., Beaulieu, J.-P., Tsapras, Y., Bozza, V., Abe, F., Bond, I. A., Botzler, C. S., Chote, P., Freeman, M., Fukui, A., Furusawa, K., Itow, Y., Ling, C. H., Masuda, K., Matsubara, Y., Miyake, N., Muraki, Y., Ohnishi, K., Rattenbury, N. J., Saito, To., Sullivan, D. J., Suzuki, K., Sweatman, W. L., Suzuki, D., Takino, S., Tristram, P. J., Wada, K., Yock, P. C. M., The MOA Collaboration, Szymański, M. K., Kubiak, M., Pietrzyński, G., Soszyński, I., Skowron, J., Kozłowski, S., Poleski, R., Ulaczyk, K., Wyrzykowski, Ł., Pietrukowicz, P., The OGLE Collaboration, Almeida, L. A., DePoy, D. L., Dong, Subo, Gorbikov, E., Jablonski, F., Henderson, C. B., Hwang, K.-H., Janczak, J., Jung, Y.-K., Kaspi, S., Lee, C.-U., Malamud, U., Maoz, D., McGregor, D., Muñoz, J. A., Park, B.-G., Park, H., Pogge, R. W., Shvartzvald, Y., Shin, I.-G., Yee, J. C., The μFUN Collaboration, Alsubai, K. A., Browne, P., Burgdorf, M. J., Calchi Novati, S., Dodds, P., Fang, X.-S., Finet, F., Glitrup, M., Grundahl, F., Gu, S.-H., Hardis, S., Harpsøe, K., Hinse, T. C., Hornstrup, A., Hundertmark, M., Jessen-Hansen, J., Jrgensen, U. G., Kains, N., Kerins, E., Liebig, C., Lund, M. N., Lundkvist, M., Maier, G., Mancini, L., Mathiasen, M., Penny, M. T., Rahvar, S., Ricci, D., Scarpetta, G., Skottfelt, J., Snodgrass, C., Southworth, J., Surdej, J., Tregloan-Reed, J., Wambsganss, J., Wertz, O., Zimmer, F., MiNDSTEp Consortium, The, Albrow, M. D., Bachelet, E., Batista, V., Brillant, S., Cassan, A., Cole, A. A., Coutures, C., Dieters, S., Dominis Prester, D., Donatowicz, J., Fouqué, P., Greenhill, J., Kubas, D., Marquette, J.-B., Menzies, J. W., Sahu, K. C., Zub, M., The PLANET Collaboration, Bramich, D. M., Horne, K., Steele, I. A., Street, R. A., The RoboNet Collaboration, Science & Technology Facilities Council, and University of St Andrews. School of Physics and Astronomy
Subjects: binaries: general, gravitational lensing: micro, 010504 meteorology & atmospheric sciences, Population, Events, Brown dwarf, Minimum mass, Binary number, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Gravitational microlensing, 01 natural sciences, micro [Gravitational lensing], Settore FIS/05 - Astronomia e Astrofisica, 0103 physical sciences, QB Astronomy, Astrophysics::Solar and Stellar Astrophysics, education, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, QB, Physics, education.field_of_study, Galactic bulge, general [Binaries], Systems, Search, Astronomy and Astrophysics, Stars, Extrasolar planets, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Astrophysics::Earth and Planetary Astrophysics, Low Mass, Gravitational lens
Abstract: Although many models have been proposed, the physical mechanisms responsible for the formation of low-mass brown dwarfs are poorly understood. The multiplicity properties and minimum mass of the brown-dwarf mass function provide critical empirical diagnostics of these mechanisms. We present the discovery via gravitational microlensing of two very low-mass, very tight binary systems. These binaries have directly and precisely measured total system masses of 0.025 Msun and 0.034 Msun, and projected separations of 0.31 AU and 0.19 AU, making them the lowest-mass and tightest field brown-dwarf binaries known. The discovery of a population of such binaries indicates that brown dwarf binaries can robustly form at least down to masses of ~0.02 Msun. Future microlensing surveys will measure a mass-selected sample of brown-dwarf binary systems, which can then be directly compared to similar samples of stellar binaries., 7 pages, 5 figures, 3 tables, ApJ submitted
Published: 2013

142. Microlensing Binaries with Candidate Brown Dwarf Companions

Author: Shin, I.-G., Han, C., Gould, A., Udalski, A., Sumi, T., Dominik, M., Beaulieu, J.-P., Tsapras, Y., Bozza, V., Szymański, M. K., Kubiak, M., Soszyński, I., Pietrzyński, G., Poleski, R., Ulaczyk, K., Pietrukowicz, P., Kozłowski, S., Skowron, J., Wyrzykowski, Ł., The OGLE Collaboration, Abe, F., Bennett, D. P., Bond, I. A., Botzler, C. S., Freeman, M., Fukui, A., Furusawa, K., Hayashi, F., Hearnshaw, J. B., Hosaka, S., Itow, Y., Kamiya, K., Kilmartin, P. M., Kobara, S., Korpela, A., Lin, W., Ling, C. H., Makita, S., Masuda, K., Matsubara, Y., Miyake, N., Muraki, Y., Nagaya, M., Nishimoto, K., Ohnishi, K., Okumura, T., Omori, K., Perrott, Y. C., Rattenbury, N., Saito, To., Skuljan, L., Sullivan, D. J., Suzuki, D., Sweatman, W. L., Tristram, P. J., Wada, K., Yock, P. C. M., The MOA Collaboration, Christie, G. W., Depoy, D. L., Dong, S., Gal-Yam, A., Gaudi, B. S., Hung, L.-W., Janczak, J., Kaspi, S., Maoz, D., McCormick, J., McGregor, D., Moorhouse, D., Muñoz, J. A., Natusch, T., Nelson, C., Pogge, R. W., Tan, T.-G., Polishook, D., Shvartzvald, Y., Shporer, A., Thornley, G., Malamud, U., Yee, J. C., Choi, J.-Y., Jung, Y.-K., Park, H., Lee, C.-U., Park, B.-G., Koo, J.-R., The μFUN Collaboration, Bajek, D., Bramich, D. M., Browne, P., Horne, K., Ipatov, S., Snodgrass, C., Steele, I., Street, R., Alsubai, K. A., Burgdorf, M. J., Calchi Novati, S., Dodds, P., Dreizler, S., Fang, X.-S., Grundahl, F., Gu, C.-H., Hardis, S., Harpsøe, Kennet Bomann West, Hinse, T. C., Hundertmark, M., Jessen-Hansen, J., Jørgensen, U. G., Kains, N., Kerins, E., Liebig, C., Lund, Mikkel Nørup, Lundkvist, M., Mancini, L., Mathiasen, M., Hornstrup, A., Penny, M. T., Proft, S., Rahvar, S., Ricci, D., Scarpetta, G., Skottfelt, Jesper Fælling, Southworth, J., Surdej, J., Tregloan-Reed, J., Wertz, O., Zimmer, F., Albrow, M. D., Batista, V., Brillant, S., Caldwell, J. A. R., Calitz, J. J., Cassan, A., Cole, A., Cook, K. H., Corrales, E., Coutures, Ch., Dieters, S., Dominis Prester, D., Donatowicz, J., Fouqué, P., Greenhill, J., Hill, K., Hoffman, M., Kane, S. R., Kubas, D., Marquette, J.-B., Martin, R., Meintjes, P., Menzies, J., Pollard, K. R., Sahu, K. C., Wambsganss, J., Williams, A., Vinter, Christian, and Zub, M.
Subjects: Physics, 010308 nuclear & particles physics, Brown dwarf, FOS: Physical sciences, Astronomy and Astrophysics, gravitational lensing: micro, Astrophysics, Light curve, Gravitational microlensing, 01 natural sciences, Einstein radius, Stars, binaries: general, Settore FIS/05 - Astronomia e Astrofisica, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Planet, 0103 physical sciences, brown dwarfs, Parallax, Low Mass, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR)
Abstract: Brown dwarfs are important objects because they may provide a missing link between stars and planets, two populations that have dramatically different formation history. In this paper, we present the candidate binaries with brown dwarf companions that are found by analyzing binary microlensing events discovered during 2004 - 2011 observation seasons. Based on the low mass ratio criterion of q < 0.2, we found 7 candidate events, including OGLE-2004-BLG-035, OGLE-2004-BLG-039, OGLE-2007-BLG-006, OGLE-2007-BLG-399/MOA-2007-BLG-334, MOA-2011-BLG-104/OGLE-2011-BLG-0172, MOA-2011-BLG-149, and MOA-201-BLG-278/OGLE-2011-BLG-012N. Among them, we are able to confirm that the companions of the lenses of MOA-2011-BLG-104/OGLE-2011-BLG-0172 and MOA-2011-BLG-149 are brown dwarfs by determining the mass of the lens based on the simultaneous measurement of the Einstein radius and the lens parallax. The measured mass of the brown dwarf companions are (0.02 +/- 0.01) M_Sun and (0.019 +/- 0.002) M_Sun for MOA-2011-BLG-104/OGLE-2011-BLG-0172 and MOA-2011-BLG-149, respectively, and both companions are orbiting low mass M dwarf host stars. More microlensing brown dwarfs are expected to be detected as the number of lensing events with well covered light curves increases with new generation searches., 10 pages, 9 figures, 4 tables
Published: 2012

143. EChO

Author: Tinetti, G., Beaulieu, J. P., Henning, T., Meyer, M., Micela, G., Ribas, I., Stam, D., Swain, M., Krause, O., Ollivier, M., Pace, E., Swinyard, B., Aylward, A., van Boekel, R., Coradini, A., Encrenaz, T., Snellen, I., Zapatero-Osorio, M. R., Bouwman, J., Cho, J. Y-K., Coudé de Foresto, V., Guillot, T., Lopez-Morales, M., Mueller-Wodarg, I., Palle, E., Selsis, F., Sozzetti, A., Ade, P. A. R., Achilleos, N., Adriani, A., Agnor, C. B., Afonso, C., Prieto, C. Allende, Bakos, G., Barber, R. J., Barlow, M., Batista, V., Bernath, P., Bézard, B., Bordé, P., Brown, L. R., Cassan, A., Cavarroc, C., Ciaravella, A., Cockell, C., Coustenis, A., Danielski, C., Decin, L., Kok, R. De, Demangeon, O., Deroo, P., Doel, P., Drossart, P., Fletcher, L. N., Focardi, M., Forget, F., Fossey, S., Fouqué, P., Frith, J., Galand, M., Gaulme, P., Hernández, J. I. González, Grasset, O., Grassi, D., Grenfell, J. L., Griffin, M. J., Griffith, C. A., Grözinger, U., Guedel, M., Guio, P., Hainaut, O., Hargreaves, R., Hauschildt, P. H., Heng, Kevin, Heyrovsky, D., Hueso, R., Irwin, P., Kaltenegger, L., Kervella, P., Kipping, D., Koskinen, T. T., Kovács, G., La Barbera, A., Lammer, H., Lellouch, E., Leto, G., Lopez Morales, M., Lopez Valverde, M. A., Lopez-Puertas, M., Lovis, C., Maggio, A., Maillard, J. P., Maldonado Prado, J., Marquette, J. B., Martin-Torres, F. J., Maxted, P., Miller, S., Molinari, S., Montes, D., Moro-Martin, A., Moses, J. I., Mousis, O., Nguyen Tuong, N., Nelson, R., Orton, G. S., Pantin, E., Pascale, E., Pezzuto, S., Pinfield, D., Poretti, E., Prinja, R., Prisinzano, L., Rees, J. M., Reiners, A., Samuel, B., Sánchez-Lavega, A., Forcada, J. Sanz, Sasselov, D., Savini, G., Sicardy, B., Smith, A., Stixrude, L., Strazzulla, G., Tennyson, J., Tessenyi, M., Vasisht, G., Vinatier, S., Viti, S., Waldmann, I., White, G. J., Widemann, T., Wordsworth, R., Yelle, R., Yung, Y., and Yurchenko, S. N.
Subjects: 530 Physics, 520 Astronomy, Astrophysics::Earth and Planetary Astrophysics
Abstract: A dedicated mission to investigate exoplanetary atmospheres represents a major milestone in our quest to understand our place in the universe by placing our Solar System in context and by addressing the suitability of planets for the presence of life. EChO—the Exoplanet Characterisation Observatory—is a mission concept specifically geared for this purpose. EChO will provide simultaneous, multi-wavelength spectroscopic observations on a stable platform that will allow very long exposures. The use of passive cooling, few moving parts and well established technology gives a low-risk and potentially long-lived mission. EChO will build on observations by Hubble, Spitzer and ground-based telescopes, which discovered the first molecules and atoms in exoplanetary atmospheres. However, EChO’s configuration and specifications are designed to study a number of systems in a consistent manner that will eliminate the ambiguities affecting prior observations. EChO will simultaneously observe a broad enough spectral region—from the visible to the mid-infrared—to constrain from one single spectrum the temperature structure of the atmosphere, the abundances of the major carbon and oxygen bearing species, the expected photochemically-produced species and magnetospheric signatures. The spectral range and resolution are tailored to separate bands belonging to up to 30 molecules and retrieve the composition and temperature structure of planetary atmospheres. The target list for EChO includes planets ranging from Jupiter-sized with equilibrium temperatures T eq up to 2,000 K, to those of a few Earth masses, with T eq \u223c 300 K. The list will include planets with no Solar System analog, such as the recently discovered planets GJ1214b, whose density lies between that of terrestrial and gaseous planets, or the rocky-iron planet 55 Cnc e, with day-side temperature close to 3,000 K. As the number of detected exoplanets is growing rapidly each year, and the mass and radius of those detected steadily decreases, the target list will be constantly adjusted to include the most interesting systems. We have baselined a dispersive spectrograph design covering continuously the 0.4–16 μm spectral range in 6 channels (1 in the visible, 5 in the InfraRed), which allows the spectral resolution to be adapted from several tens to several hundreds, depending on the target brightness. The instrument will be mounted behind a 1.5 m class telescope, passively cooled to 50 K, with the instrument structure and optics passively cooled to \u223c45 K. EChO will be placed in a grand halo orbit around L2. This orbit, in combination with an optimised thermal shield design, provides a highly stable thermal environment and a high degree of visibility of the sky to observe repeatedly several tens of targets over the year. Both the baseline and alternative designs have been evaluated and no critical items with Technology Readiness Level (TRL) less than 4–5 have been identified. We have also undertaken a first-order cost and development plan analysis and find that EChO is easily compatible with the ESA M-class mission framework.
Published: 2012
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144. Characterizing Low-Mass Binaries From Observation of Long Time-scale Caustic-crossing Gravitational Microlensing Events

Author: Shin, I.-G, Han, C., Choi, J.-Y, Udalski, A., Sumi, T., Gould, A., Bozza, V., Dominik, M., Fouque´, P., Horne, K., Szyman´ski, M. K., Kubiak, M., Soszyn´ski, I., Pietrzyn´ski, G., Poleski, R., Ulaczyk, K., Pietrukowicz, P., Kozłowski, S., Skowron, J., Wyrzykowski, Ł., Abe, F., Bennett, D. P., Bond, I. A., Botzler, C. S., Chote, P., Freeman, M., Fukui, A., Furusawa, K., Itow, Y., Kobara, S., Ling, C. H., Masuda, K., Matsubara, Y., Miyake, N., Muraki, Y., Ohmori, K., Ohnishi, K., Rattenbury, N. J., Saito, To, Sullivan, D. J., Suzuki, D., Suzuki, K., Sweatman, W. L., Takino, S., Tristram, P. J., Wada, K., Yock, P. C. M., MOA Collaboration, Bramich, D. M., Snodgrass, C., Steele, I. A., Street, R. A., Tsapras, Y., RoboNet Collaboration, Alsubai, K. A., Browne, P., Burgdorf, M. J., Calchi Novati, S., Dodds, P., Dreizler, S., Fang, X.-S, Grundahl, Frank, Gu, C.-H, Hardis, S., Harpsøe, Kennet Bomann West, Hinse, T. C., Hornstrup, Allan, Hundertmark, M., Jessen-Hansen, Jens, Jørgensen, U. G., Kains, N., Kerins, E., Liebig, C., Lund, M., Lunkkvist, M., Mancini, L., Mathiasen, M., Penny, M. T., Rahvar, S., Ricci, D., Scarpetta, G., Skottfelt, J., Southworth, J., Surdej, J., Tregloan-Reed, J., Wambsganss, J., Wertz, O., Almeida, L. A., Batista, V., Christie, G., DePoy, D. L., Dong, Subo, Gaudi, B. S., Henderson, C., Jablonski, F., Lee, C.-U, McCormick, J., McGregor, D., Moorhouse, D., Natusch, T., Ngan, H., Park, S.-Y., Pogge, R. W., Tan, T.-G, Thornley, G., Yee, J. C., Albrow, M. D., Bachelet, E., Beaulieu, J.-P, Brillant, S., Cassan, A., Cole, A. A., Corrales, E., Coutures, C., Dieters, S., Dominis Prester, D., Donatowicz, J., Greenhill, J., Kubas, D., Marquette, J.-B, Menzies, J. W., Sahu, K. C., and Zub, M.
Subjects: binaries: general, gravitational lensing: micro, 010504 meteorology & atmospheric sciences, Binary number, FOS: Physical sciences, Astrophysics, Gravitational microlensing, 01 natural sciences, Einstein radius, micro [Gravitational lensing], Settore FIS/05 - Astronomia e Astrofisica, 0103 physical sciences, Binary star, binaries: general, gravitational lensing: micro, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), 0105 earth and related environmental sciences, Orbital elements, Physics, general [Binaries], Observational techniques, Astronomy and Astrophysics, Light curve, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Low Mass
Abstract: Despite astrophysical importance of binary star systems, detections are limited to those located in small ranges of separations, distances, and masses and thus it is necessary to use a variety of observational techniques for a complete view of stellar multiplicity across a broad range of physical parameters. In this paper, we report the detections and measurements of 2 binaries discovered from observations of microlensing events MOA-2011-BLG-090 and OGLE-2011-BLG-0417. Determinations of the binary masses are possible by simultaneously measuring the Einstein radius and the lens parallax. The measured masses of the binary components are 0.43 $M_{\odot}$ and 0.39 $M_{\odot}$ for MOA-2011-BLG-090 and 0.57 $M_{\odot}$ and 0.17 $M_{\odot}$ for OGLE-2011-BLG-0417 and thus both lens components of MOA-2011-BLG-090 and one component of OGLE-2011-BLG-0417 are M dwarfs, demonstrating the usefulness of microlensing in detecting binaries composed of low-mass components. From modeling of the light curves considering full Keplerian motion of the lens, we also measure the orbital parameters of the binaries. The blended light of OGLE-2011-BLG-0417 comes very likely from the lens itself, making it possible to check the microlensing orbital solution by follow-up radial-velocity observation. For both events, the caustic-crossing parts of the light curves, which are critical for determining the physical lens parameters, were resolved by high-cadence survey observations and thus it is expected that the number of microlensing binaries with measured physical parameters will increase in the future., Comment: 8 pages, 5 figures, 4 tables
Published: 2012

145. OGLE-2008-BLG-510: first automated real-time detection of a weak microlensing anomaly - brown dwarf or stellar binary?

Author: Bozza, Valerio, Dominik, M., Rattenbury, N. J., Joergensen, U. G., Tsapras, Y., Bramich, D. M., Udalski, A., Bond, I. A., Liebig, C., Fouque, A. Cassan P., Fukui, A., Hundertmark, M., Shin, I. G., Lee, S. H., Choi, J. Y., Park, S. Y., Gould, A., Allan, A., Mao, S., Wyrzykowski, L., Street, R. A., Buckley, D., Nagayama, T., Mathiasen, M., Hinse, T. C., CALCHI NOVATI, Sebastiano, Harpsoee, K., Mancini, Luigi, Scarpetta, Gaetano, Anguita, T., Burgdorf, M. J., Horne, K., Hornstrup, A., Kains, N., Kerins, E., Kjaergaard, P., Masi, G., Rahvar, S., Ricci, D., Snodgrass, C., Southworth, J., Steele, I. A., Surdej, J., Thoene, C. C., Wambsganss, J., Zub, M., Albrow, M. D., Batista, V., Beaulieu, J. P., Bennett, D. P., Caldwell, J. A. R., Cole, A., Cook, K. H., Coutures, C., Dieters, S., Dominis Prester, D., Donatowicz, J., Greenhill, J., Kane, S. R., Kubas, D., Marquette, J. B., Martin, R., Menzies, J., Pollard, K. R., Sahu, K. C., Williams, A., Szymanski, M. K., Kubiak, M., Pietrzynski, G., Soszynski, I., Poleski, R., Ulaczyk, K., Depoy, D. L., Dong, S., Han, C., Janczak, J., Lee, C. U., Pogge, R. W., Abe, F., Furusawa, K., Hearnshaw, J. B., Itow, Y., Kilmartin, P. M., Korpela, A. V., Lin, W., Ling, C. H., Masuda, K., Matsubara, Y., Miyake, N., Muraki, Y., Ohnishi, K., Perrott, Y. C., Saito, T. o., Skuljan, L., Sullivan, D. J., Sumi, T., Suzuki, D., Sweatman, W. L., Tristram, P. J., Wada, K., Yock, P. C. M., Gulbis, A., Hashimoto, Y., Kniazev, A., and Vaisanen, P.
Subjects: gravitational lensing: micro, planetary systems
Published: 2012

146. Microlensing Binaries Discovered through High-Magnification Channel

Author: Shin, I.-G., Choi, J.-Y., Park, S.-Y., Han, C., Gould, A., Sumi, T., Udalski, A., Beaulieu, J.-P., Dominik, M., Allen, W., Bos, M., Christie, G. W., Depoy, D. L., Dong, S., Drummond, J., Gal-Yam, A., Gaudi, B. S., Hung, L.-W., Janczak, J., Kaspi, S., Lee, C.-U., Mallia, F., Maoz, D., Maury, A., McCormick, J., Monard, L. A. G., Moorhouse, D., Muñoz, J. A., Natusch, T., Nelson, C., Park, B.-G., Pogge, R. W., Polishook, D., Shvartzvald, Y., Shporer, A., Thornley, G., Yee, J. C., μFUN Collaboration, Abe, F., Bennett, D. P., Bond, I. A., Botzler, C. S., Fukui, A., Furusawa, K., Hayashi, F., Hearnshaw, J. B., Hosaka, S., Itow, Y., Kamiya, K., Kilmartin, P. M., Kobara, S., Korpela, A., Lin, W., Ling, C. H., Makita, S., Masuda, K., Matsubara, Y., Miyake, N., Muraki, Y., Nagaya, M., Nishimoto, K., Ohnishi, K., Okumura, T., Omori, K., Perrott, Y. C., Rattenbury, N., Saito, To., Skuljan, L., Sullivan, D. J., Suzuki, D., Sweatman, W. L., Tristram, P. J., Wada, K., Yock, P. C. M., MOA Collaboration, Szymański, M. K., Kubiak, M., Pietrzyński, G., Soszyński, I., Poleski, R., Ulaczyk, K., Wyrzykowski, Ł., Kozłowski, S., Pietrukowicz, P., OGLE Collaboration, Albrow, M. D., Batista, V., Bramich, D. M., Brillant, S., Caldwell, J. A. R., Calitz, J. J., Cassan, A., Cole, A., Cook, K. H., Corrales, E., Coutures, Ch., Dieters, S., Dominis Prester, D., Donatowicz, J., Fouqué, P., Greenhill, J., Hoffman, M., Jørgensen, U. G., Kane, S. R., Kubas, D., Marquette, J.-B., Martin, R., Meintjes, P., Menzies, J., Pollard, K. R., Sahu, K. C., Wambsganss, J., Williams, A., Vinter, Christian, Zub, M., PLANET Collaboration, Allan, A., Browne, P., Horne, K., Snodgrass, C., Steele, I., Street, R., Tsapras, Y., RoboNet Collaboration, Alsubai, K. A., Bozza, V., Burgdorf, M. J., Calchi Novati, S., Dodds, P., Dreizler, S., Finet, F., Gerner, T., Glitrup, M., Grundahl, F., Hardis, S., Harpsøe, Kennet Bomann West, Hessman, F. V., Hinse, T. C., Hundertmark, M., Kains, N., Kerins, E., Liebig, C., Maier, G., Mancini, L., Mathiasen, M., Penny, M. T., Proft, S., Rahvar, S., Ricci, D., Scarpetta, G., Schäfer, S., Schönebeck, F., Skottfelt, Jesper Fælling, Surdej, J., Southworth, J., Zimmer, F., and MiNDSTEp Consortium
Subjects: binaries: general, gravitational lensing: micro, Binary number, FOS: Physical sciences, Astrophysics, Gravitational microlensing, 01 natural sciences, law.invention, Settore FIS/05 - Astronomia e Astrofisica, Planet, law, 0103 physical sciences, binaries: general, gravitational lensing: micro, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Physics, 010308 nuclear & particles physics, Astronomy and Astrophysics, Mass ratio, Light curve, 3. Good health, Lens (optics), Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Astrophysics::Earth and Planetary Astrophysics, Degeneracy (mathematics), Event (particle physics)
Abstract: Microlensing can provide a useful tool to probe binary distributions down to low-mass limits of binary companions. In this paper, we analyze the light curves of 8 binary lensing events detected through the channel of high-magnification events during the seasons from 2007 to 2010. The perturbations, which are confined near the peak of the light curves, can be easily distinguished from the central perturbations caused by planets. However, the degeneracy between close and wide binary solutions cannot be resolved with a $3\sigma$ confidence level for 3 events, implying that the degeneracy would be an important obstacle in studying binary distributions. The dependence of the degeneracy on the lensing parameters is consistent with a theoretic prediction that the degeneracy becomes severe as the binary separation and the mass ratio deviate from the values of resonant caustics. The measured mass ratio of the event OGLE-2008-BLG-510/MOA-2008-BLG-369 is $q\sim 0.1$, making the companion of the lens a strong brown-dwarf candidate., Comment: 10 figures, 6 tables, 26 pages
Published: 2011

147. MOA-2009-BLG-387Lb: A massive planet orbiting an M dwarf

Author: Batista, V., Gould, A., Dieters, S., Dong, S., Bond, I., Beaulieu, J. P., Maoz, D., Monard, B., Christie, G. W., Mccormick, J., Albrow, M. D., Horne, K., Tsapras, Y., Burgdorf, M. J., Calchi Novati, S., Skottfelt, J., Caldwell, J., Kozłowski, S., Kubas, D., Gaudi, B. S., Han, C., Bennett, D. P., An, J., Abe, F., Botzler, C. S., Douchin, D., Freeman, M., Fukui, A., Furusawa, K., Hearnshaw, J. B., Hosaka, S., Itow, Y., Kamiya, K., Kilmartin, P. M., Korpela, A., Lin, W., Ling, C. H., Makita, B. S., Masuda, K., Matsubara, Y., Miyake, N., Muraki, Y., Nagaya, M., Nishimoto, K., Ohnishi, K., Okumura, T., Perrott, Y. C., Rattenbury, N., Saito, T. o., Sullivan, D. J., Sumi, T., Sweatman, W. L., Tristram, P. J., von Seggern, E., Yock, P. C. M., Brillant, S., Calitz, J. J., Cassan, A., Cole, A., Cook, K., Coutures, C., Dominis Prester, D., Donatowicz, J., Greenhill, J., Hoffman, M., Jablonski, F., Kane, S. R., Kains, N., Marquette, J. B., Martin, R., Martioli, E., Meintjes, P., Menzies, J., Pedretti, E., Pollard, K., Sahu, K. C., Vinter, C., Wambsganss, J., Watson, R., Williams, A., Zub, M., Allen, W., Bolt, G., Bos, M., Depoy, D. L., Drummond, J., Eastman, J. D., Gal Yam, A., Gorbikov, E., Higgins, D., Janczak, J., Kaspi, S., Lee, C. U., Mallia, F., Maury, A., Monard, L. A. G., Moorhouse, D., Morgan, N., Natusch, T., Ofek, E. O., Park, B. G., Pogge, R. W., Polishook, D., Santallo, R., Shporer, A., Spector, O., Thornley, G., Yee, J. C., Bozza, Valerio, Browne, P., Dominik, M., Dreizler, S., Finet, F., Glitrup, M., Grundahl, F., Harpsøe, K., Hessman, F. V., Hinse, T. C., Hundertmark, M., Jørgensen, U. G., Liebig, C., Maier, G., Mancini, L., Mathiasen, M., Rahvar, S., Ricci, D., Scarpetta, Gaetano, Southworth, J., Surdej, J., Zimmer, F., Allan, A., Bramich, D. M., Snodgrass, C., Steele, I. A., and Street, R. A.
Subjects: Physics, Earth and Planetary Astrophysics (astro-ph.EP), 010308 nuclear & particles physics, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Mass ratio, Gravitational microlensing, 01 natural sciences, Einstein radius, Jupiter, Settore FIS/05 - Astronomia e Astrofisica, 13. Climate action, Space and Planetary Science, Planet, 0103 physical sciences, Orbital motion, High Energy Physics::Experiment, gravitational lensing, micro methods, data analysis, planets, satellites, detection, methods, numerical, instrumentation, adaptive optics, photometers, Astrophysics::Earth and Planetary Astrophysics, 010303 astronomy & astrophysics, Planetary mass, Astrophysics::Galaxy Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract: We report the discovery of a planet with a high planet-to-star mass ratio in the microlensing event MOA-2009-BLG-387, which exhibited pronounced deviations over a 12-day interval, one of the longest for any planetary event. The host is an M dwarf, with a mass in the range 0.07 M_sun < M_host < 0.49M_sun at 90% confidence. The planet-star mass ratio q = 0.0132 +- 0.003 has been measured extremely well, so at the best-estimated host mass, the planet mass is m_p = 2.6 Jupiter masses for the median host mass, M = 0.19 M_sun. The host mass is determined from two "higher order" microlensing parameters. One of these, the angular Einstein radius ��_E = 0.31 +- 0.03 mas, is very well measured, but the other (the microlens parallax ��_E, which is due to the Earth's orbital motion) is highly degenate with the orbital motion of the planet. We statistically resolve the degeneracy between Earth and planet orbital effects by imposing priors from a Galactic model that specifies the positions and velocities of lenses and sources and a Kepler model of orbits. The 90% confidence intervals for the distance, semi-major axis, and period of the planet are 3.5 kpc < D_L < 7.9 kpc, 1.1 AU < a < 2.7AU, and 3.8 yr < P < 7.6 yr, respectively., 20 pages including 8 figures. A&A 529 102 (2011)
Published: 2011
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148. The VMC survey: I. strategy and first data

Author: Cioni, M- R L, Clementini, G, Girardi, L, Guandalini, R, Gullieuszik, M, Miszalski, B, Moretti, M-I, Ripepi, V, Rubele, S, Bagheri, G, Bekki, K, Cross, N, de Blok, W J G, de Grijs, R, Emerson, J P, Evans, C J, Gibson, B, Gonzales-Solares, E, Groenewegen, M A T, Irwin, M, Ivanov, V D, Lewis, J, Marconi, M, Marquette, J-B, Mastropietro, C, Moore, B, Napiwotzki, R, Naylor, T, Oliveira, J M, Read, M, Sutorius, E, van Loon, J Th, Department of Astronomy, and Faculty of Science
Subjects: stars: variables: RR Lyrae, Hertzsprung-Russell and C-M diagrams, survey, infrared: stars, magellanic clouds, stars: variables: Cepheids
Abstract: Context. The new VISual and Infrared Telescope for Astronomy (VISTA) has started operations. Over its first five years it will be collecting data for six public surveys, one of which is the near-infrared YJK(s) VISTA survey of the Magellanic Clouds system (VMC). This survey comprises the Large Magellanic Cloud (LMC), the Small Magellanic Cloud, the Magellanic Bridge connecting the two galaxies and two fields in the Magellanic Stream. Aims. This paper provides an overview of the VMC survey strategy and presents first science results. The main goals of the VMC survey are the determination of the spatially-resolved star-formation history and the three-dimensional structure of the Magellanic system. The VMC survey is therefore designed to reach stars as faint as the oldest main sequence turn-off point and to constrain the mean magnitude of pulsating variables such as RR Lyrae stars and Cepheids. This paper focuses on observations of VMC fields in the LMC obtained between November 2009 and March 2010. These observations correspond to a completeness of 7% of the planned LMC fields. Methods. The VMC data are comprised of multi-epoch observations which are executed following specific time constraints. The data were reduced using the VISTA Data Flow System pipeline with source catalogues, including astrometric and photometric corrections, produced and made available via the VISTA Science Archive. The VMC data will be released to the astronomical community following the European Southern Observatorys Public Survey policy. The analysis of the data shows that the sensitivity in each wave band agrees with expectations. Uncertainties and completeness of the data are also derived. Results. The first science results, aimed at assessing the scientific quality of the VMC data, include an overview of the distribution of stars in colour-magnitude and colour-colour diagrams, the detection of planetary nebulae and stellar clusters, and the K-s band light-curves of variable stars. Conclusions. The VMC survey represents a tremendous improvement, in spatial resolution and sensitivity, on previous panoramic observations of the Magellanic system in the near-infrared, providing a powerful complement to deep observations at other wavelengths.
Published: 2011
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149. MOA-2007-BLG-197: Exploring the brown dwarf desert

Author: Ranc, C., primary, Cassan, A., additional, Albrow, M. D., additional, Kubas, D., additional, Bond, I. A., additional, Batista, V., additional, Beaulieu, J.-P., additional, Bennett, D. P., additional, Dominik, M., additional, Dong, Subo, additional, Fouqué, P., additional, Gould, A., additional, Greenhill, J., additional, Jørgensen, U. G., additional, Kains, N., additional, Menzies, J., additional, Sumi, T., additional, Bachelet, E., additional, Coutures, C., additional, Dieters, S., additional, Dominis Prester, D., additional, Donatowicz, J., additional, Gaudi, B. S., additional, Han, C., additional, Hundertmark, M., additional, Horne, K., additional, Kane, S. R., additional, Lee, C.-U., additional, Marquette, J.-B., additional, Park, B.-G., additional, Pollard, K. R., additional, Sahu, K. C., additional, Street, R., additional, Tsapras, Y., additional, Wambsganss, J., additional, Williams, A., additional, Zub, M., additional, Abe, F., additional, Fukui, A., additional, Itow, Y., additional, Masuda, K., additional, Matsubara, Y., additional, Muraki, Y., additional, Ohnishi, K., additional, Rattenbury, N., additional, Saito, To., additional, Sullivan, D. J., additional, Sweatman, W. L., additional, Tristram, P. J., additional, Yock, P. C. M., additional, and Yonehara, A., additional
Published: 2015
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150. CONFIRMATION OF THE OGLE-2005-BLG-169 PLANET SIGNATURE AND ITS CHARACTERISTICS WITH LENS–SOURCE PROPER MOTION DETECTION

Author: Batista, V., primary, Beaulieu, J.-P., additional, Bennett, D. P., additional, Gould, A., additional, Marquette, J.-B., additional, Fukui, A., additional, and Bhattacharya, A., additional
Published: 2015
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