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117 results on '"Sullivan, D.J."'

3. Multisite observations of the DAV white dwarf R 548

Author

Kepler S.O., Giovannini O., Costa A.F.M., Winget D.E., Nather R. E., Kanaan A., Kleinman S.J., Marar T.M.K., Ashoka B.N., Mahra H.S., Solheim J.-E., Emanuelsen P.-I., Olsen Ø., Meištas E.G., Tereshchenko V., Kardapolov V., Rspaev F., Sullivan D.J., Wickramasinghe D.T., Bessell M.S., Wu K., O’Donoghue D., Buckley D.A., Warner B., Haswell C., Baptista R., Neill D., and Birch P.

Subjects
Astronomy, QB1-991
Published
1995
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4. Discovery of a Jupiter/Saturn analog with gravitational microlensing

Author

Gaudi, B.S., Bennett, D.P., Udalski, A., Gould, A., Christie, G.W., Maoz, D., Dong, S., McCormick, J., Szymanski, M.K., Tristram, P.J., Nikolaev, S., Paczynski, B., Kubiak, M., Pietrzynski, G., Soszynski, I., Szewczyk, O., Ulaczyk, K., Wyrzykowski, L., DePoy, D.L., Han, C., Kaspi, S., Lee, C.-U., Mallia, F., Natusch, T., Pogge, R.W., Park, B.-G., Abe, F., Bond, I.A., Botzler, C.S., Fukui, A., Hearnshaw, J.B., Itow, Y., Kamiya, K., Korpela, A.V., Kilmartin, P.M., Lin, W, Masuda, K., Matsubara, Y., Motomura, M., Muraki, Y., Nakamura, S., Okumura, T., Ohnishi, K., Rattenbury, N.J., Sako, T., Saito, To., Sato, S., Skuljan, L., Sullivan, D.J., Sumi, T., Sweatman, W.L., Yock, P.C.M., Albrow, M.D., Allan, A., Beaulieu, J.-P., Burgdorf, M.J., Cook, K.H., Coutures, C., Dominik, M., Dieters, S., Fouque, P., Greenhill, J., Horne, K., Steele, I., Tsapras, Y., Chaboyer, B., Crocker, A., Frank, S., and Macintosh, B.

Subjects
Extrasolar planets -- Discovery and exploration, Gravitational lenses -- Observations
Published
2008

13. Search for low-mass exoplanets by gravitational microlensing at high magnification

Author

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., Rakich, A., Rattenbury, N.J., Sako, T., Sekiguchi, T., Sullivan, D.J., Sumi, T., Tristram, P.J., Yanagisawa, T., Yock, P.C.M., Gal-Yam, A., Lipkin, Y., Maoz, D., Ofek, E.O., Udalski, A., Szewczyk, O., Zebrun, K., Soszynski, I., Szymanski, M.K., Kubiak, M., Pietrzynski, G., and Wyrzykowski, L.

Subjects
Observations, Research, Extrasolar planets -- Observations -- Research, Astronomy -- Observations -- Research
Abstract

Gravitational microlensing events of high magnification occur when the foreground lens system comes into near-perfect alignment with the background source star. Suitable alignments are most readily found in the dense [...], Observations of the gravitational microlensing event MOA 2003-BLG-32/OGLE 2003-BLG-219 are presented, for which the peak magnification was over 500, the highest yet reported. Continuous observations around the peak enabled a sensitive search for planets orbiting the lens star. No planets were detected. Planets 1.3 times heavier than Earth were excluded from more than 50% of the projected annular region from approximately 2.3 to 3.6 astronomical units surrounding the lens star, Uranus-mass planets were excluded from 0.9 to 8.7 astronomical units, and planets 1.3 times heavier than Saturn were excluded from 0.2 to 60 astronomical units. These are the largest regions of sensitivity vet achieved in searches for extrasolar planets orbiting any star.

Published
2004

14. 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
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15. 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., Ipatov, S., Kains, N., Snodgrass, C., Steele, I.A., Alsubai, K.A., Andersen, J.M., Novati, S.C., Damerdji, Y., Diehl, C., Elyiv, A., 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., Surdej, 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, C., Dieters, S., Dominis Prester, D., Donatowicz, J., Fouqué, 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., Drummond, J., Gaudi, B.S., Henderson, C.B., Hwang, K.H., Jung, Y.K., Kavka, A., Koo, J.-R., Lee, C.-U., Maoz, D., Monard, L.A.G., Natusch, T., Ngan, H., Park, H., Pogge, R.W., Porritt, I., Shin, I.-G., Shvartzvald, Y., Tan, T.G., 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, T., Sullivan, D.J., Sweatman, W.L., Suzuki, D., Tristram, P.J., Tsurumi, N., Wada, K., Yamai, N., Yock, P.C.M., Yonehara, A., The Royal Society, Science & Technology Facilities Council, and University of St Andrews. School of Physics and Astronomy

Subjects
Perturbation (astronomy), FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Gravitational microlensing, Einstein radius, micro [Gravitational lensing], Super-Jupiter, Settore FIS/05 - Astronomia e Astrofisica, Planet, QB Astronomy, Astrophysics::Solar and Stellar Astrophysics, QC, Astrophysics::Galaxy Astrophysics, QB, Physics, Earth and Planetary Astrophysics (astro-ph.EP), general [Binaries], Astronomy and Astrophysics, Planetary systems, QC Physics, Space and Planetary Science, Orbital motion, Astrophysics::Earth and Planetary Astrophysics, Late-type star, Parallax, Astrophysics - Earth and Planetary 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 lightcurve, 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 $2.73\pm 0.43\ M_{\rm J}$ planet orbiting a $0.44\pm 0.07\ M_{\odot}$ early M-type star. The distance to the lens is $4.97\pm 0.29$\ kpc and the projected separation between the host star and its planet at the time of the event is $3.45\pm 0.26$ 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., 9 pages, 4 figures, accepted by ApJ

Published
2013

16. A giant planet beyond the snow line in microlensing event OGLE-2011-BLG-0251

Author

Kains, N., Street, R.A., Choi, J.-Y., Han, C., Udalski, A., Almeida, L.A., Jablonski, F., Tristram, P.J., Jørgensen, Uffe Gråe, Szymański, M.K., Kubiak, M., Pietrzyński, G., Soszyński, I., Poleski, R., Kozłowski, S., Pietrukowicz, P., Ulaczyk, K., Wyrzykowski, Ł., Skowron, J., Tsapras, Y., Alsubai, K.A., Bozza, V., Browne, P., Burgdorf, M. J., Calchi Novati, S., Dodds, P., Dominik, M., Dreizler, S., Fang, X.-S., Grundahl, F., Gu, C.-H., Hardis, S., Harpsøe, Kennet Bomann West, Hessman, F. V., Hinse, T. C., Hornstrup, Allan, Hundertmark, M., Jessen-Hansen, Jens, Kerins, E., Liebig, C., Lund, M., Lundkvist, M., Mancini, L., Mathiasen, M., Penny, M. T., Rahvar, S., Ricci, D., Sahu, K.C., Scarpetta, G., Skottfelt, J., Snodgrass, C., Southworth, J., Surdej, J., Tregloan-Reed, J., Wambsganss, J., Wertz, O., Bajek, D., Bramich, D.M., Horne, K., Ipatov, S., Steele, I.A., Abe, F., Bennett, D.P., 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., Saito, T., Sullivan, D.J., Sumi, T., Suzuki, D., Suzuki, K., Sweatman, W.L., Takino, S., Wada, K., Yock, P.C.M., Allen, W., Batista, V., Chung, S.-J., Christie, G., Depoy, D.L., Drummond, J., Gaudi, B.S., Gould, A., Henderson, C., Jung, Y.K., Koo, J.-R., Lee, C.-U., McCormick, J., McGregor, D., Muñoz, J.A., Natusch, T., Ngan, H., Park, H., Pogge, R.W., Shin, I.-G., Yee, J., Albrow, M.D., Bachelet, E., Beaulieu, J.-P., Brillant, S., Caldwell, J.A.R., Cassan, A., Cole, A., Corrales, E., Coutures, Ch., Dieters, S., Dominis Prester, D., Donatowicz, J., Fouqué, P., Greenhill, J., Kane, S.R., Kubas, D., Marquette, J.-B., Martin, R., Meintjes, P., Menzies, J., Pollard, K.R., Williams, A., Wouters, D., Zub, M., Science & Technology Facilities Council, and University of St Andrews. School of Physics and Astronomy

Subjects
planets and satellites: detection, 010504 meteorology & atmospheric sciences, Satellites, bulge [Galaxy], FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Discovery, Gravitational microlensing, 01 natural sciences, Galaxy: bulge, Einstein radius, Lens, gravitational lensing: weak, Settore FIS/05 - Astronomia e Astrofisica, Planet, Snow, 0103 physical sciences, gravitational lensing, weak, planets and satellites, detection, planetary systems, Galaxy, bulge, Binary, QB Astronomy, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, QB, Physics, Earth and Planetary Astrophysics (astro-ph.EP), Giant planet, Systems, Search, Astronomy and Astrophysics, Radius, Frequency, Planetary system, Mass ratio, Mass, Light curve, Stars, Algorithm, detection [Planets and satellites], Planetary systems, Space and Planetary Science, Dwarf, Astrophysics::Earth and Planetary Astrophysics, weak [Gravitational lensing], Astrophysics - Earth and Planetary Astrophysics
Abstract

We present the analysis of the gravitational microlensing event OGLE-2011-BLG-0251. This anomalous event was observed by several survey and follow-up collaborations conducting microlensing observations towards the Galactic Bulge. Based on detailed modelling of the observed light curve, we find that the lens is composed of two masses with a mass ratio q=1.9 x 10^-3. Thanks to our detection of higher-order effects on the light curve due to the Earth's orbital motion and the finite size of source, we are able to measure the mass and distance to the lens unambiguously. We find that the lens is made up of a planet of mass 0.53 +- 0.21,M_Jup orbiting an M dwarf host star with a mass of 0.26 +- 0.11 M_Sun. The planetary system is located at a distance of 2.57 +- 0.61 kpc towards the Galactic Centre. The projected separation of the planet from its host star is d=1.408 +- 0.019, in units of the Einstein radius, which corresponds to 2.72 +- 0.75 AU in physical units. We also identified a competitive model with similar planet and host star masses, but with a smaller orbital radius of 1.50 +- 0.50 AU. The planet is therefore located beyond the snow line of its host star, which we estimate to be around 1-1.5 AU., 12 pages, 7 figures, 3 tables; A&A in press

Published
2013
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17. MOA-2010-BLG-477Lb: constraining the mass of a microlensing planet from microlensing parallax, orbital motion and detection of blended light

Author

Bachelet, E., Shin, I.-G., Han, C., Fouqué, P., Gould, A., Menzies, J.W., Beaulieu, J.-P., Bennett, D.P., Bond, I.A., Dong, Subo, Heyrovský, D., Marquette, J.-B., Marshall, J., Skowron, J., Street, R.A., Sumi, T., Udalski, A., Abe, L., Agabi, K., Albrow, M.D., Allen, W., Bertin, E., Bos, M., Bramich, D.M., Chavez, J., Christie, G.W., Cole, A.A., Crouzet, N., Dieters, S., Dominik, M., Drummond, J., Greenhill, J., Guillot, T., Henderson, C.B., Hessman, F.V., Horne, K., Hundertmark, M., Johnson, J.A., Jørgensen, U.G., Kandori, R., Liebig, C., Mékarnia, D., McCormick, J., Moorhouse, D., Nagayama, T., Nataf, D., Natusch, T., Nishiyama, S., Rivet, J.P., Sahu, K.C., Shvartzvald, Y., Thornley, G., Tomczak, A.R., Tsapras, Y., Yee, J.C., Batista, V., Bennett, C.S., Brillant, S., Caldwell, J.A.R., Cassan, A., Corrales, E., Coutures, C., Dominis Prester, D., Donatowicz, J., Kubas, D., Martin, Roland, Williams, A., Zub, M., The PLANET Collaboration, De Almeida, L., Depoy, D.L., Gaudi, B.S., Hung, L.-W., Jablonski, F., Kaspi, S., Klein, N., Lee, C.-U., Lee, Y., Koo, J.-R., Maoz, D., Muñoz, J.A., Pogge, R.W., Polishook, D., Shporer, A., The FUN Collaboration, Abe, F., Botzler, C.S., Chote, P., Freeman, M., Fukui, A., Furusawa, K., Harris, P., Itow, Y., Kobara, S., Ling, C.H., Masuda, K., Matsubara, Y., Miyake, N., Ohmori, K., Ohnishi, K., Rattenbury, N.J., Saito, To., Sullivan, D.J., Suzuki, D., Sweatman, W.L., Tristram, P.J., Wada, K., Yock, P.C.M., The MOA Collaboration, Szymanski, M.K., Soszynski, I., Kubiak, M., Poleski, R., Ulaczyk, K., Pietrzynski, G., Wyrzykowski, L., The OGLE Collaboration, Kains, N., Snodgrass, C., Steele, I.A., The RoboNet Collaboration, Alsubai, K.A., Bozza, V., Browne, P., Burgdorf, M.J., Calchi Novati, S., Dodds, P., Dreizler, S., Finet, F., Gerner, T., Hardis, S., Harpsøe, K., Hinse, T.C., Kerins, E., Mancini, L., Mathiasen, M., Penny, M.T., Proft, S., Rahvar, S., Ricci, D., Scarpetta, G., Schäfer, S., Schönebeck, F., Southworth, J., Surdej, J., Wambsganss, J., The MiNDSTEp Consortium, Joseph Louis LAGRANGE (LAGRANGE), 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, Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), and Laboratoire de Cosmologie, Astrophysique Stellaire & Solaire, de Planétologie et de Mécanique des Fluides (CASSIOPEE)

Subjects
gravitational lensing: micro, planetary systems, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Gravitational microlensing, 01 natural sciences, 7. Clean energy, Einstein radius, Settore FIS/05 - Astronomia e Astrofisica, Planet, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, 010306 general physics, 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, Astrophysics::Galaxy Astrophysics, Physics, Earth and Planetary Astrophysics (astro-ph.EP), Giant planet, Astronomy and Astrophysics, Mass ratio, Light curve, Orbit, 13. Climate action, Space and Planetary Science, Orbital motion, micro [gravitational lensing], gravitational lensing: micro, planetary systems, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Earth and Planetary Astrophysics
Abstract

Microlensing detections of cool planets are important for the construction of an unbiased sample to estimate the frequency of planets beyond the snow line, which is where giant planets are thought to form according to the core accretion theory of planet formation. In this paper, we report the discovery of a giant planet detected from the analysis of the light curve of a high-magnification microlensing event MOA-2010-BLG-477. The measured planet-star mass ratio is $q=(2.181\pm0.004)\times 10^{-3}$ and the projected separation is $s=1.1228\pm0.0006$ in units of the Einstein radius. The angular Einstein radius is unusually large $\theta_{\rm E}=1.38\pm 0.11$ mas. Combining this measurement with constraints on the "microlens parallax" and the lens flux, we can only limit the host mass to the range $0.13, Comment: 3 Tables, 12 Figures, accepted in ApJ

Published
2012
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18. The discovery of a persistent quasi-periodic oscillation in the intermediate polar TX Col

Author

Mhlahlo, N., Buckley, D.A.H., Dhillon, V.S., Potter, S.B., Warner, B., Woudt, P., Bolt, G., McCormick, J., Rea, R., Sullivan, D.J., and Velhuis, F.

Subjects
Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

We report on the detection of an ~5900 s quasi-periodic variation in the extensive photometry of TX Col spanning 12 years. We discuss five different models to explain this period. We favour a mechanism where the quasi-periodic variation results from the beating of the Keplerian frequency of the `blobs' orbiting in the outer accretion disc with the spin frequency, and from modulated accretion of these `blobs' taking place in a shocked region near the disc/magnetosphere boundary., 9 pages, 6 figures, 3 tables. Accepted by the Monthly Notices of the Royal Astronomical Society

Published
2007

20. Pushing the ground-based limit: 14-mumag photometric precision with the definitive Whole Earth Telescope asteroseismic data set for the rapidly oscillating Ap star HR1217

Author

Kurtz, D.W., Cameron, C., Cunha, M.S., Dolez, N., Vauclair, G., Pallier, E., Ulla, A., Kepler, S.O., Da Costa, A., Kanaan, A., Fraga, L., Giovannini, O., Wood, M.A., Silvestri, N., Kawaler, S.D., Riddle, R.L., Reed, M.D., Watson, T.K., Metcalfe, T.S., Mukadam, A., Nather, R.E., Winget, D.E., Nitta, A., Kleinman, S.J., Guzik, J.A., Bradley, P.A., Matthews, J.M., Sekiguchi, K., Sullivan, D.J., Sullivan, T., Shobbrook, R., Jiang, X., Birch, P.V., Ashoka, B.N., Seetha, S., Girish, V., Joshi, S., Moskalik, P., Zola, S., O'Donoghue, D., Handler, G., Mueller, M., Perez, J.M.G., Solheim, J.E., Johannessen, F., Bigot, Lionel, Laboratoire de Cosmologie, Astrophysique Stellaire & Solaire, de Planétologie et de Mécanique des Fluides (CASSIOPEE), 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, and Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS)

Subjects
[SDU]Sciences of the Universe [physics]
Abstract

Monthly Notices of the Royal Astronomical Society, 358, pp. 651-664; International audience; HR 1217 is one of the best-studied rapidly oscillating Ap (roAp) stars, with a frequency spectrum of alternating even-and odd-f modes that are distorted by the presence of a strong, global magnetic field. Several recent theoretical studies have found that within the observable

Published
2005

21. 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

24. P29.18 Universal screening for methicillin-resistant Staphylococcus aureus (MRSA) in an acute hospital

Author

Creamer, E., primary, Dolan, A., additional, Sherlock, O., additional, Fitzgerald-Hughes, D., additional, Thomas, T., additional, Walsh, J., additional, Shore, A.C., additional, Sullivan, D.J., additional, Kinnevey, P.M., additional, Rossney, A.S., additional, O'Lorcain, P., additional, Smyth, E.G., additional, Cunney, R., additional, Coleman, D.C., additional, and Humphreys, H., additional

Published
2010
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25. Identification of four distinct genotypes of Candida dubliniensis and detection of microevolution in vitro and in vivo.

Author

Gee, S.F., Joly, S., Soll, D.R., Meis, J.F.G.M., Verweij, P.E., Polacheck, I., Sullivan, D.J., Coleman, D.C., Gee, S.F., Joly, S., Soll, D.R., Meis, J.F.G.M., Verweij, P.E., Polacheck, I., Sullivan, D.J., and Coleman, D.C.

Abstract

Item does not contain fulltext, The present study investigates further the population structure of Candida dubliniensis and its ability to exhibit microevolution. Using 98 isolates (including 80 oral isolates) from 94 patients in 15 countries, we confirmed the existence of two distinct populations within the species C. dubliniensis, designated Cd25 group I and Cd25 group II, respectively, on the basis of DNA fingerprints generated with the C. dubliniensis-specific probe Cd25. The majority of Cd25 group I isolates (48 of 71, 67.6%) were from human immunodeficiency virus (HIV)-infected individuals, whereas the majority of Cd25 group II isolates (19 of 27, 70.4%) were from HIV-negative individuals (P < or = 0.001). Nucleotide sequence analysis of the internal transcribed spacer (ITS) regions of the rRNA genes from 19 representative isolates revealed the presence of four separate genotypes. All of the Cd25 group I isolates tested belonged to genotype 1, while the Cd25 group II population was comprised of three distinct genotypes (genotypes 2 to 4), which corresponded to distinct clades within the Cd25 group II population. These findings were confirmed using genotype-specific PCR primers with 70 isolates. We also showed that C. dubliniensis can exhibit microevolution in vivo and in vitro as occurs in other yeast species. DNA fingerprinting using the C. dubliniensis probes Cd25, Cd24, and Cd1 and karyotype analysis of multiple oral isolates recovered from the same specimen from each of eight separate patients revealed microevolution in six of eight of the clonal populations. Similarly, sequential clonal isolates from various anatomical sites in two separate patients exhibited microevolution. Microevolution was also shown to occur when two clinical isolates susceptible to fluconazole were exposed to the drug in vitro. The epidemiological significance of the four C. dubliniensis genotypes and the ability of C. dubliniensis to undergo microevolution has yet to be established.

Published
2002

27. 211

Author

Hafner, J.W., primary, Parrish, S.E., additional, Hubler, J.R., additional, and Sullivan, D.J., additional

Published
2006
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31. Photometry of Eclipsing Binary Stars in the Large and Small Magellanic Clouds

Author

Bayne, G.P., primary, Tobin, W., additional, Pritchard, J.D., additional, Bond, I., additional, Pollard, K.R., additional, Besier, S.C., additional, Noda, S., additional, Sumi, T., additional, Yanagisawa, T., additional, Sekiguchi, M., additional, Honda, M., additional, Muraki, Y., additional, Takeuti, M., additional, Hearnshaw, J.B., additional, Kilmartin, P.M., additional, Dodd, R.J., additional, Sullivan, D.J., additional, and Yock, P.C.M., additional

Published
2004
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32. Observational properties of red variables in the LMC

Author

Takeuti, M., primary, Noda, S., additional, Abe, F., additional, Bond, I.A., additional, Dodd, R.J., additional, Hearnshaw, J.B., additional, Honda, M., additional, Honma, M., additional, Jugaku, J., additional, Kan-ya, Y., additional, Kato, Y., additional, Kilmartin, P.M., additional, Matsubara, Y., additional, Masuda, K., additional, Muraki, Y., additional, Nakamura, T., additional, Ohnishi, K., additional, Reid, M., additional, Rattenbury, N.J., additional, Saito, To., additional, Saito, Y., additional, Sato, H., additional, Sekiguchi, M., additional, Skuljan, J., additional, Sullivan, D.J., additional, Sumi, T., additional, Yamada, R., additional, Yanagisawa, T., additional, Yock, P.C.M., additional, and Yoshizawa, M., additional

Published
2004
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34. Study of variable stars in the MOA data base: long-period red variables in the Large Magellanic Cloud

Author

Noda, S., primary, Takeuti, M., additional, Abe, F., additional, Bond, I.A., additional, Dodd, R.J., additional, Hearnshaw, J.B., additional, Honda, M., additional, Honma, M., additional, Jugaku, J., additional, Kabe, S., additional, Kan-ya, Y., additional, Kato, Y., additional, Kilmartin, P.M., additional, Matsubara, Y., additional, Masuda, K., additional, Muraki, Y., additional, Nakamura, T., additional, Nankivell, G.R., additional, Noguchi, C., additional, Ohnishi, K., additional, Reid, M., additional, Rattenbury, N.J., additional, Saito, To., additional, Sato, H., additional, Sekiguchi, M., additional, Skuljan, J., additional, Sullivan, D.J., additional, Sumi, T., additional, Watase, Y., additional, Wilkinson, S., additional, Yamada, R., additional, Yanagisawa, T., additional, Yock, P.C.M., additional, and Yoshizawa, M., additional

Published
2002
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35. Long-period Red Variables in the Large Magellanic Cloud from the MOA Database

Author

Takeuti, Mine, primary, Noda, S., additional, Abe, F., additional, Bond, I. A., additional, Dodd, R. J., additional, Hearnshaw, J. B., additional, Honda, M., additional, Jugaku, J., additional, Kabe, S., additional, Kilmartin, P. M., additional, Matsubara, Y., additional, Masuda, K., additional, Muraki, Y., additional, Nakamura, T., additional, Nankivell, G. R., additional, Noguchi, C., additional, Ohnishi, K., additional, Rattenbury, N. J., additional, Reid, M., additional, Saito, To., additional, Sato, H., additional, Sekiguchi, M., additional, Skuljan, J., additional, Sullivan, D.J., additional, Sumi, T., additional, Watase, Y., additional, Yanagisawa, T., additional, Yock, P. C. M., additional, and Yoshizawa, M., additional

Published
2001
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42. Triclosan Antagonizes Fluconazole Activity against Candida albicans.

Author

Higgins, J., Pinjon, E., Oltean, H.N., White, T.C., Kelly, S.L., Martel, C.M., Sullivan, D.J., Coleman, D.C., and Moran, G.P.

Subjects
TRICLOSAN, CANDIDA albicans, ORAL hygiene products, STEROLS, FATTY acids, PROKARYOTES, DENTAL plaque, HYPHAE of fungi
Abstract

Triclosan is a broad-spectrum antimicrobial compound commonly used in oral hygiene products. Investigation of its activity against Candida albicans showed that triclosan was fungicidal at concentrations of 16 mg/L. However, at subinhibitory concentrations (0.5-2 mg/L), triclosan antagonized the activity of fluconazole. Although triclosan induced CDR1 expression in C. albicans, antagonism was still observed in cdr1Δ and cdr2Δ strains. Triclosan did not affect fluconazole uptake or alter total membrane sterol content, but did induce the expression of FAS1 and FAS2, indicating that its mode of action may involve inhibition of fatty acid synthesis, as it does in prokaryotes. However, FAS2 mutants did not exhibit increased susceptibility to triclosan, and overexpression of both FAS1 and FAS2 alleles did not alter triclosan susceptibility. Unexpectedly, the antagonistic effect was specific for C. albicans under hypha-inducing conditions and was absent in the non-filamentous efg1Δ strain. This antagonism may be due to the membranotropic activity of triclosan and the unique composition of hyphal membranes. [ABSTRACT FROM PUBLISHER]

Published
2012
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45. A Whole Earth Telescope campaign on the pulsating subdwarf B binary system PG 1336−018 (NY Vir).

Author

Kilkenny, D., Reed, M.D., O'Donoghue, D., Kawaler, S.d., Mukadam, A., Kleinman, S.J., Nitta, A., Metcalfe, T.S., Provencal, J.L., Watson, T.K., Sullivan, D.J., Sullivan, T., Shobbrook, R., Jiang, X.J., Joshi, S., Ashoka, B.N., Seetha, S., Leibowitz, E., and Ibbetson, P.

Subjects
BINARY stars, ECLIPSING binaries, ASTRONOMICAL photometry, VARIABLE stars, ASTROPHYSICS
Abstract

We present results from a multisite (‘Whole Earth Telescope’) photometric campaign on PG 1336−018, the close eclipsing binary system containing a pulsating subdwarf B (sdB) star. The main part of the campaign (1999 April) resulted in ∼172 h of observations, representing a coverage of about 47 per cent, and additional data were obtained outside the core campaign. Periodogram analysis shows that the light variations are dominated by three frequencies near 5757, 5585 and 5369 μHz (∼174, 179 and 186 s, respectively), although many frequencies are present, particularly in the range 5000–6000 μHz (∼200–170 s). We identify, with some confidence, 28 frequencies down to a semi-amplitude of 0.0005 in fractional intensity (equivalent to about 0.5 mmag). It is clear that the pulsation frequencies of PG 1336−018 have changed substantially since the 1996 discovery observations were made, and that amplitude changes occur, at least in the dominant three frequencies, on relatively short time-scales (of the order of a day). On the assumption that the pulsating star is phase-locked in the binary system, we have searched for rotational splitting of frequencies near the orbital and half of the orbital period, but the results are confused by aliasing at those frequencies (due to the data gaps caused by the eclipses). A preliminary model qualitatively matches the distribution of frequencies in PG 1336−018, with some good individual correspondences, but cannot be considered adequate because geometric cancellation should hide some of the modes which are apparently detected. Analysis of the pulsations during eclipse recovers three of the strongest modes, but the limited eclipse data – which can, at best, be only about 9 per cent of the total – do not allow mode identification at this stage. Simulations indicate that an overall coverage of about 80 per cent would be required for this to be viable. An attempt was made to determine phase shifts in the pulsation frequencies as a way of directly measuring the size of the binary orbit, but the uncertainties in the method are comparable to the light travel time across the orbit (probably less than a second). [ABSTRACT FROM AUTHOR]

Published
2003
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46. A multisite campaign on the pulsating subdwarf B star PG 1047+003.

Author

Kilkenny, D., Billères, M., Stobie, R.S., Fontaine, G., Shobbrook, R.R., O'Donoghue, D., Brassard, P., Sullivan, D.J., Burleigh, M.R., and Barstow, M.A.

Subjects
DWARF stars, ASTRONOMICAL photometry, PULSATING stars
Abstract

Results are presented from a multisite photometric campaign on the pulsating subdwarf B star, PG 1047+003. Approximately 98 h of data were obtained from three sites, with a duty cycle of ∼30 per cent. The light curve of PG 1047+003 is dominated by several frequencies in the range ∼6880–7500 μHz (periods 133–145 s). We identify, with some confidence, 18 frequencies between 5700 and 9605 μHz (104–175 s) down to an amplitude of 0.0004 in fractional intensity (0.04 per cent), thus doubling the number of published pulsation frequencies for this star. These pulsations correspond to low-order and low-degree acoustic modes. Several frequency spacings near 1.05 μHz suggest a rotation period for the star of 11.0 d. [ABSTRACT FROM AUTHOR]

Published
2002
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49. Contributors (Mar. 1960 [T-MTT]).

Author

Jaynes, E.T., Mount, E., Stitch, M.L., Parkes, D.A., Sullivan, D.J., Eaton, J.E., Deam, A.P., Forrer, M.P., Finnila, C.A., Chisholm, R.M., Sharpe, C.B., King, H.E., Kogo, H., Hunton, J.K., Robinson, N.O., Silvey, W., Jones, E.M.T., Culshaw, W., Owyang, G.H., and Begg, B.A.

Published
1960
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