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3 results on '"Kubas, D"'

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

Author

Bozza, V., Dominik, M., Rattenbury, N. J., Joergensen, U. G., Tsapras, Y., Bramich, D. M., Udalski, A., Bond, I. A., Liebig, C., Cassan, A., Fouque, 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., Novati, S. Calchi, Harpsoee, K., Mancini, L., Scarpetta, G., 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., Prester, D. Dominis, 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, To., 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., Vaisanen, P., 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), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), and Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS)

Subjects
Earth and Planetary Astrophysics (astro-ph.EP), Settore FIS/05 - Astronomia e Astrofisica, Astrophysics - Solar and Stellar Astrophysics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], [SDU]Sciences of the Universe [physics], FOS: Physical sciences, gravitational lensing: micro, planetary systems, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics - Earth and Planetary Astrophysics
Abstract

The microlensing event OGLE-2008-BLG-510 is characterised by an evident asymmetric shape of the peak, promptly detected by the ARTEMiS system in real time. The skewness of the light curve appears to be compatible both with binary-lens and binary-source models, including the possibility that the lens system consists of an M dwarf orbited by a brown dwarf. The detection of this microlensing anomaly and our analysis demonstrates that: 1) automated real-time detection of weak microlensing anomalies with immediate feedback is feasible, efficient, and sensitive, 2) rather common weak features intrinsically come with ambiguities that are not easily resolved from photometric light curves, 3) a modelling approach that finds all features of parameter space rather than just the `favourite model' is required, and 4) the data quality is most crucial, where systematics can be confused with real features, in particular small higher-order effects such as orbital motion signatures. It moreover becomes apparent that events with weak signatures are a silver mine for statistical studies, although not easy to exploit. Clues about the apparent paucity of both brown-dwarf companions and binary-source microlensing events might hide here., 17 pages with 8 figures, MNRAS submitted

Published
2012

2. Limits on additional planetary companions to OGLE 2005-BLG-390L

Author

Kubas, D., Cassan, A., Dominik, M., Bennett, D. P., Wambsganss, J., Brillant, S., Beaulieu, J. P., Albrow, M. D., Batista, V., Bode, M., Bramich, D. M., Burgdorf, M., Caldwell, J. A. R., Calitz, H., Cook, K. H., Coutures, Ch., Dieters, S., Dominis Prester, D., Donatowicz, J., Fouqué, P., Greenhill, J., Hill, K., Hoffman, M., Horne, K., Jørgensen, U. G., Kains, N., Kane, S., Marquette, J. B., Martin, Roland, Meintjes, P., Menzies, J., Pollard, K. R., Sahu, K. C., Snodgrass, C., Steele, I., Tsapras, Y., Vinter, C., Williams, A., Woller, K., Zub, M., The PLANET/Robonet Collaboration, Astronomische Rechen-Institut [Heidelberg] (ARI), Zentrum für Astronomie der Universität Heidelberg (ZAH), Universität Heidelberg [Heidelberg] = Heidelberg University-Universität Heidelberg [Heidelberg] = Heidelberg University, Institut d'Astrophysique de Paris (IAP), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Astrophysique de Toulouse-Tarbes (LATT), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), PLANET, ANR-06-BLAN-0416,HOLMES,HOLMES (Hunting cOol Low Mass Extrasolar PlanetS)(2006), Universität Heidelberg [Heidelberg]-Universität Heidelberg [Heidelberg], Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), and 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)

Subjects
Gas giant, Milky Way, gravitational lensing, FOS: Physical sciences, Model parameters, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Gravitational microlensing, 01 natural sciences, Jovian, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Planet, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, 10. No inequality, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, 010308 nuclear & particles physics, Astrophysics (astro-ph), Astronomy and Astrophysics, Stars, Space and Planetary Science, Astrophysics::Earth and Planetary Astrophysics, stars: planetary systems, Planetary mass
Abstract

We investigate constraints on additional planets orbiting the distant M-dwarf star OGLE-2005-BLG-390L, around which photometric microlensing data has revealed the existence of the sub-Neptune-mass planet OGLE-2005-BLG-390Lb. We specifically aim to study potential Jovian companions and compare our findings with predictions from core-accretion and disc-instability models of planet formation. We also obtain an estimate of the detection probability for sub-Neptune mass planets similar to OGLE-2005-BLG-390Lb using a simplified simulation of a microlensing experiment. We compute the efficiency of our photometric data for detecting additional planets around OGLE-2005-BLG-390L, as a function of the microlensing model parameters and convert it into a function of the orbital axis and planet mass by means of an adopted model of the Milky Way. We find that more than 50 % of potential planets with a mass in excess of 1 M_J between 1.1 and 2.3 AU around OGLE-2005-BLG-390L would have revealed their existence, whereas for gas giants above 3 M_J in orbits between 1.5 and 2.2 AU, the detection efficiency reaches 70 %; however, no such companion was observed. Our photometric microlensing data therefore do not contradict the existence of gas giant planets at any separation orbiting OGLE-2005-BLG-390L. Furthermore we find a detection probability for an OGLE-2005-BLG-390Lb-like planet of around 2-5 %. In agreement with current planet formation theories, this quantitatively supports the prediction that sub-Neptune mass planets are common around low-mass stars., 10 pages, 4 figures, accepted by A&A

Published
2008

3. Potential Direct Single-Star Mass Measurement

Author

Ghosh, H., Depoy, D.L., Gal-Yam, A., Gaudi, B.S., Gould, A., Han, C., Lipkin, Y., Maoz, D., Ofek, E.O., Park, B.-G., Pogge, R.W., Salim, S., Abe, F., Bennett, D.P., Bond, I.A., Eguchi, S., Furuta, Y., Hearnshaw, J.B., Kamiya, K., Kilmartin, P.M., Kurata, Y., Masuda, K., Matsubara, Y., Muraki, Y., Noda, S., Okajima, K., Rattenbury, N.J., Sako, T., Sekiguchi, T., Sullivan, D.J., Sumi, T., Tristram, P.J., Yanagisawa, T., Yock, P.C.M., Udalski, A., Soszynski, I., Wyrzykowski, L., Kubiak, M., Szymanski, M.K., Pietrzynski, G., Szewczyk, O., Zebrun, K., Albrow, M.D., Beaulieu, J.-P., Caldwell, J.A.R., Cassan, A., Coutures, C., Dominik, M., Donatowicz, J., Fouqué, P., Greenhill, J., Hill, K., Horne, K., Jorgensen, U.G., Kane, S., Kubas, D., Martin, Roland, Menzies, J., Pollard, K.R., Sahu, K.C., Wambsganss, J., Watson, R., Williams, A., Fouqué, Pascal, Departement de recherche SPAtiale (DESPA), Observatoire de Paris, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)

Subjects
Physics, Proper motion, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Degenerate energy levels, Astrophysics (astro-ph), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrometry, Gravitational microlensing, [SDU.ASTR] Sciences of the Universe [physics]/Astrophysics [astro-ph], 01 natural sciences, Einstein radius, Distortion (mathematics), [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Space and Planetary Science, Coincident, [PHYS.ASTR.CO] Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], 0103 physical sciences, Astrophysics::Earth and Planetary Astrophysics, 010306 general physics, Degeneracy (mathematics), 010303 astronomy & astrophysics
Abstract

We analyze the lightcurve of the microlensing event OGLE-2003-BLG-175/MOA-2003-BLG-45 and show that it has two properties that, when combined with future high resolution astrometry, could lead to a direct, accurate measurement of the lens mass. First, the lightcurve shows clear signs of distortion due to the Earth's accelerated motion, which yields a measurement of the projected Einstein radius \tilde r_E. Second, from precise astrometric measurements, we show that the blended light in the event is coincident with the microlensed source to within about 15 mas. This argues strongly that this blended light is the lens and hence opens the possibility of directly measuring the lens-source relative proper motion \vec\mu_\rel and so the mass M=(c^2/4G)\mu_\rel t_E \tilde r_E, where t_E is the measured Einstein timescale. While the lightcurve-based measurement of \tilde r_E is, by itself, severely degenerate, we show that this degeneracy can be completely resolved by measuring the direction of proper motion \vec\mu_\rel., Comment: 28 pages including 7 figures. Submitted to ApJ

Published
2004

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