132 results on '"Mathiasen, M."'
Search Results
2. MiNDSTEp differential photometry of the gravitationally lensed quasars WFI2033-4723 and HE0047-1756: Microlensing and a new time delay
- Author
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Giannini, E., Schmidt, R. W., Wambsganss, J., Alsubai, K., Andersen, J. M., Anguita, T., Bozza, V., Bramich, D. M., Browne, P., Calchi Novati, S., Hardis, S., Harpsøe, K., Hornstrup, Allan, Hundertmark, M., Jørgensen, U. G., Juncher, D., Korhonen, H., Mathiasen, M., Skottfelt, J., Giannini, E., Schmidt, R. W., Wambsganss, J., Alsubai, K., Andersen, J. M., Anguita, T., Bozza, V., Bramich, D. M., Browne, P., Calchi Novati, S., Hardis, S., Harpsøe, K., Hornstrup, Allan, Hundertmark, M., Jørgensen, U. G., Juncher, D., Korhonen, H., Mathiasen, M., and Skottfelt, J.
- Abstract
Aims. We present V and R photometry of the gravitationally lensed quasars WFI 2033-4723 and HE 0047-1756. The data were taken by the MiNDSTEp collaboration with the 1.54 m Danish telescope at the ESO La Silla observatory from 2008 to 2012.Methods. Differential photometry has been carried out using the image subtraction method as implemented in the HOTPAnTS package, additionally using GALFIT for quasar photometry.Results. The quasar WFI 2033-4723 showed brightness variations of order 0.5 mag in V and R during the campaign. The two lensed components of quasar HE 0047-1756 varied by 0.2–0.3 mag within five years. We provide, for the first time, an estimate of the time delay of component B with respect to A of Δt = (7.6 ± 1.8) days for this object. We also find evidence for a secular evolution of the magnitude difference between components A and B in both filters, which we explain as due to a long-duration microlensing event. Finally we find that both quasars WFI 2033-4723 and HE 0047-1756 become bluer when brighter, which is consistent with previous studies.
- Published
- 2017
3. Faint-source-star planetary microlensing:the discovery of the cold gas-giant planet OGLE-2014-BLG-0676Lb
- Author
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Rattenbury, N. J., Bennett, D. P., Sumi, T., Koshimoto, N., Bond, I. A., Udalski, A., Shvartzvald, Y., Maoz, Dan, Jørgensen, Uffe Gråe, Dominik, M., Street, R. A., Tsapras, Y., Abe, F., Asakura, Y., Barry, R., Bhattacharya, A., Donachie, M., Evans, P., Freeman, M., 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., Saito, To., Sharan, A., Sullivan, D. J., Suzuki, D., Tristram, P. J., Yonehara, A., Poleski, R., Skowron, J., Mróz, P., Szymański, M. K., Soszyński, I., Pietrukowicz, P., Kozlowski, S., Ulaczyk, K., Wyrzykowski, L., Friedmann, M., Kaspi, S., Alsubai, K., Browne, P., Andersen, J. M., Bozza, V., Novati, S. Calchi, Damerdji, Y., Diehl, C., Dreizler, S., Elyiv, A., Giannini, E., Hardis, S., Harpsøe, Kennet Bomann West, Hinse, T. C., Liebig, C., Hundertmark, M., Juncher, Diana, Kains, N., Kerins, E., Korhonen, Heidi Helena, Mancini, L., Martin, R., Mathiasen, M., Rabus, M., Rahvar, S., Scarpetta, G., Skottfelt, Jesper Mirsa, Snodgrass, C., Surdej, J., Taylor, J., Tregloan-Reed, J., Vilela, C., Wambsganss, J., Williams, A., D'Ago, G., Bachelet, E., Bramich, D. M., Jaimes, R. Figuera, Horne, K., Menzies, J., Schmidt, R., Steele, I. A., Rattenbury, N. J., Bennett, D. P., Sumi, T., Koshimoto, N., Bond, I. A., Udalski, A., Shvartzvald, Y., Maoz, Dan, Jørgensen, Uffe Gråe, Dominik, M., Street, R. A., Tsapras, Y., Abe, F., Asakura, Y., Barry, R., Bhattacharya, A., Donachie, M., Evans, P., Freeman, M., 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., Saito, To., Sharan, A., Sullivan, D. J., Suzuki, D., Tristram, P. J., Yonehara, A., Poleski, R., Skowron, J., Mróz, P., Szymański, M. K., Soszyński, I., Pietrukowicz, P., Kozlowski, S., Ulaczyk, K., Wyrzykowski, L., Friedmann, M., Kaspi, S., Alsubai, K., Browne, P., Andersen, J. M., Bozza, V., Novati, S. Calchi, Damerdji, Y., Diehl, C., Dreizler, S., Elyiv, A., Giannini, E., Hardis, S., Harpsøe, Kennet Bomann West, Hinse, T. C., Liebig, C., Hundertmark, M., Juncher, Diana, Kains, N., Kerins, E., Korhonen, Heidi Helena, Mancini, L., Martin, R., Mathiasen, M., Rabus, M., Rahvar, S., Scarpetta, G., Skottfelt, Jesper Mirsa, Snodgrass, C., Surdej, J., Taylor, J., Tregloan-Reed, J., Vilela, C., Wambsganss, J., Williams, A., D'Ago, G., Bachelet, E., Bramich, D. M., Jaimes, R. Figuera, Horne, K., Menzies, J., Schmidt, R., and Steele, I. A.
- Published
- 2017
4. Faint-source-star planetary microlensing: The discovery of the cold gas-giant planet OGLE-2014-BLG-0676Lb
- Author
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Rattenbury, N., Bennett, D., Sumi, T., Koshimoto, N., Bond, I., Udalski, A., Shvartzvald, Y., Maoz, D., Jørgensen, U., Dominik, M., Street, R., Tsapras, Y., Abe, F., Asakura, Y., Barry, R., Bhattacharya, A., Donachie, M., Evans, P., Freeman, M., Fukui, A., Hirao, Y., Itow, Y., Li, M., Ling, C., Masuda, K., Matsubara, Y., Muraki, Y., Nagakane, M., Ohnishi, K., Oyokawa, H., Saito, T., Sharan, A., Sullivan, D., Suzuki, D., Tristram, P., Yonehara, A., Poleski, R., Skowron, J., Mróz, P., Szymanski, M., Soszynski, I., Pietrukowicz, P., Kozlowski, S., Ulaczyk, K., Wyrzykowski, Friedmann, M., Kaspi, S., Alsubai, K., Browne, P., Andersen, J., Bozza, V., Calchi Novati, S., Damerdji, Y., Diehl, C., Dreizler, S., Elyiv, A., Giannini, E., Hardis, S., Harpsøe, K., Hinse, T., Liebig, C., Hundertmark, M., Juncher, D., Kains, N., Kerins, E., Korhonen, H., Mancini, L., Martin, R., Mathiasen, M., Rabus, M., Rahvar, S., Scarpetta, G., Skottfelt, J., Snodgrass, C., Surdej, J., Taylor, J., Tregloan-Reed, J., Vilela, C., Wambsganss, J., Williams, Andrew, D'Ago, G., Bachelet, E., Bramich, D., Figuera Jaimes, R., Horne, K., Menzies, J., Schmidt, R., Steele, I., Rattenbury, N., Bennett, D., Sumi, T., Koshimoto, N., Bond, I., Udalski, A., Shvartzvald, Y., Maoz, D., Jørgensen, U., Dominik, M., Street, R., Tsapras, Y., Abe, F., Asakura, Y., Barry, R., Bhattacharya, A., Donachie, M., Evans, P., Freeman, M., Fukui, A., Hirao, Y., Itow, Y., Li, M., Ling, C., Masuda, K., Matsubara, Y., Muraki, Y., Nagakane, M., Ohnishi, K., Oyokawa, H., Saito, T., Sharan, A., Sullivan, D., Suzuki, D., Tristram, P., Yonehara, A., Poleski, R., Skowron, J., Mróz, P., Szymanski, M., Soszynski, I., Pietrukowicz, P., Kozlowski, S., Ulaczyk, K., Wyrzykowski, Friedmann, M., Kaspi, S., Alsubai, K., Browne, P., Andersen, J., Bozza, V., Calchi Novati, S., Damerdji, Y., Diehl, C., Dreizler, S., Elyiv, A., Giannini, E., Hardis, S., Harpsøe, K., Hinse, T., Liebig, C., Hundertmark, M., Juncher, D., Kains, N., Kerins, E., Korhonen, H., Mancini, L., Martin, R., Mathiasen, M., Rabus, M., Rahvar, S., Scarpetta, G., Skottfelt, J., Snodgrass, C., Surdej, J., Taylor, J., Tregloan-Reed, J., Vilela, C., Wambsganss, J., Williams, Andrew, D'Ago, G., Bachelet, E., Bramich, D., Figuera Jaimes, R., Horne, K., Menzies, J., Schmidt, R., and Steele, I.
- Abstract
© 2016 The Authors. We report the discovery of a planet - OGLE-2014-BLG-0676Lb- via gravitational microlensing. Observations for the lensing event were made by the following groups: Microlensing Observations in Astrophysics; Optical Gravitational Lensing Experiment; Wise Observatory; RoboNET/Las Cumbres Observatory Global Telescope; Microlensing Network for the Detection of Small Terrestrial Exoplanets; and µ-FUN. All analyses of the light-curve data favour a lens system comprising a planetary mass orbiting a host star. The most-favoured binary lens model has a mass ratio between the two lens masses of (4.78 ± 0.13) × 10-3. Subject to some important assumptions, a Bayesian probability density analysis suggests the lens system comprises a 3.09-1.12+1.02 MJ planet orbiting a 0.62-0.22+0.20 M? host star at a deprojected orbital separation of 4.40-1.46+2.16 au. The distance to the lens system is 2.22-0.83+0.96 kpc. Planet OGLE- 2014-BLG-0676Lb provides additional data to the growing number of cool planets discovered using gravitational microlensing against which planetary formation theories may be tested. Most of the light in the baseline of this event is expected to come from the lens and thus high-resolution imaging observations could confirm our planetary model interpretation.
- Published
- 2017
5. Faint source star planetary microlensing: the discovery of the cold gas giant planet OGLE-2014-BLG-0676Lb
- Author
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Rattenbury, N. J., Bennett, D. P., Sumi, T., Koshimoto, N., Bond, I. A., Udalski, A., Shvartzvald, Y., Maoz, D., Jorgensen, U. G., Dominik, M., Street, R. A., Tsapras, Y., Abe, F., Asakura, Y., Barry, R., Bhattacharya, A., Donachie, M., Evans, P., Freeman, M., 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., Saito, To., Sharan, A., Sullivan, D. J., Suzuki, D., Tristram, P. J., Yonehara, A., Poleski, R., Skowron, J., Mroz, P., Szymanski, M. K., Soszynski, I., Pietrukowicz, P., Kozlowski, S., Ulaczyk, K., Wyrzykowski, L., Friedmann, M., Kaspi, S., Alsubai, K., Browne, P., Andersen, J. M., Bozza, V., Novati, S. Calchi, Damerdji, Y., Diehl, C., Dreizler, S., Elyiv, A., Giannini, E., Hardis, S., Harpsoe, K., Hinse, T. C., Liebig, C., Hundertmark, M., Juncher, D., Kains, N., Kerins, E., Korhonen, H., Mancini, L., Martin, R., Mathiasen, M., Rabus, M., Rahvar, S., Scarpetta, G., Skottfelt, J., Snodgrass, C., Surdej, J., Taylor, J., Tregloan-Reed, J., Vilela, C., Wambsganss, J., Williams, A., D'Ago, G., Bachelet, E., Bramich, D. M., Jaimes, R. Figuera, Horne, K., Menzies, J., Schmidt, R., Steele, I. A., Rattenbury, N. J., Bennett, D. P., Sumi, T., Koshimoto, N., Bond, I. A., Udalski, A., Shvartzvald, Y., Maoz, D., Jorgensen, U. G., Dominik, M., Street, R. A., Tsapras, Y., Abe, F., Asakura, Y., Barry, R., Bhattacharya, A., Donachie, M., Evans, P., Freeman, M., 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., Saito, To., Sharan, A., Sullivan, D. J., Suzuki, D., Tristram, P. J., Yonehara, A., Poleski, R., Skowron, J., Mroz, P., Szymanski, M. K., Soszynski, I., Pietrukowicz, P., Kozlowski, S., Ulaczyk, K., Wyrzykowski, L., Friedmann, M., Kaspi, S., Alsubai, K., Browne, P., Andersen, J. M., Bozza, V., Novati, S. Calchi, Damerdji, Y., Diehl, C., Dreizler, S., Elyiv, A., Giannini, E., Hardis, S., Harpsoe, K., Hinse, T. C., Liebig, C., Hundertmark, M., Juncher, D., Kains, N., Kerins, E., Korhonen, H., Mancini, L., Martin, R., Mathiasen, M., Rabus, M., Rahvar, S., Scarpetta, G., Skottfelt, J., Snodgrass, C., Surdej, J., Taylor, J., Tregloan-Reed, J., Vilela, C., Wambsganss, J., Williams, A., D'Ago, G., Bachelet, E., Bramich, D. M., Jaimes, R. Figuera, Horne, K., Menzies, J., Schmidt, R., and Steele, I. A.
- Abstract
We report the discovery of a planet --- OGLE-2014-BLG-0676Lb --- via gravitational microlensing. Observations for the lensing event were made by the MOA, OGLE, Wise, RoboNET/LCOGT, MiNDSTEp and $\mu$FUN groups. All analyses of the light curve data favour a lens system comprising a planetary mass orbiting a host star. The most favoured binary lens model has a mass ratio between the two lens masses of $(4.78 \pm 0.13)\times 10^{-3}$. Subject to some important assumptions, a Bayesian probability density analysis suggests the lens system comprises a $3.09_{-1.12}^{+1.02}$ M_jup planet orbiting a $0.62_{-0.22}^{+0.20}$ M_sun host star at a deprojected orbital separation of $4.40_{-1.46}^{+2.16}$ AU. The distance to the lens system is $2.22_{-0.83}^{+0.96}$ kpc. Planet OGLE-2014-BLG-0676Lb provides additional data to the growing number of cool planets discovered using gravitational microlensing against which planetary formation theories may be tested. Most of the light in the baseline of this event is expected to come from the lens and thus high-resolution imaging observations could confirm our planetary model interpretation., Comment: 10 pages, 5 figures, MNRAS accepted
- Published
- 2016
- Full Text
- View/download PDF
6. MiNDSTEp differential photometry of the gravitationally lensed quasars WFI2033-4723 and HE0047-1756: Microlensing and a new time delay
- Author
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Giannini, E., Schmidt, R. W., Wambsganß, J., Alsubai, K., Andersen, J. M., Anguita, T., Bozza, V., Bramich, D. M., Browne, P., Novati, S. Calchi, Damerdji, Y., Diehl, C., Dodds, P., Dominik, M., Elyiv, A., Fang, X., Jaimes, R. Figuera, Finet, F., Gerner, T., Gu, S., Hardis, S., Harpsøe, K., Hinse, T. C., Hornstrup, A., Hundertmark, M., Jessen-Hansen, J., Jørgensen, U. G., Juncher, D., Kains, N., Kerins, E., Korhonen, H., Liebig, C., Lund, M. N., Lundkvist, M. S., Maier, G., Mancini, L., Masi, G., Mathiasen, M., Penny, M., Proft, S., Rabus, M., Rahvar, S., Ricci, D., Scarpetta, G., Sahu, K., Schäfer, S., Schönebeck, F., Skottfelt, J., Snodgrass, C., Southworth, J., Surdej, J., Tregloan-Reed, J., Vilela, C., Wertz, O., Zimmer, F., Giannini, E., Schmidt, R. W., Wambsganß, J., Alsubai, K., Andersen, J. M., Anguita, T., Bozza, V., Bramich, D. M., Browne, P., Novati, S. Calchi, Damerdji, Y., Diehl, C., Dodds, P., Dominik, M., Elyiv, A., Fang, X., Jaimes, R. Figuera, Finet, F., Gerner, T., Gu, S., Hardis, S., Harpsøe, K., Hinse, T. C., Hornstrup, A., Hundertmark, M., Jessen-Hansen, J., Jørgensen, U. G., Juncher, D., Kains, N., Kerins, E., Korhonen, H., Liebig, C., Lund, M. N., Lundkvist, M. S., Maier, G., Mancini, L., Masi, G., Mathiasen, M., Penny, M., Proft, S., Rabus, M., Rahvar, S., Ricci, D., Scarpetta, G., Sahu, K., Schäfer, S., Schönebeck, F., Skottfelt, J., Snodgrass, C., Southworth, J., Surdej, J., Tregloan-Reed, J., Vilela, C., Wertz, O., and Zimmer, F.
- Abstract
We present V and R photometry of the gravitationally lensed quasars WFI2033-4723 and HE0047-1756. The data were taken by the MiNDSTEp collaboration with the 1.54 m Danish telescope at the ESO La Silla observatory from 2008 to 2012. Differential photometry has been carried out using the image subtraction method as implemented in the HOTPAnTS package, additionally using GALFIT for quasar photometry. The quasar WFI2033-4723 showed brightness variations of order 0.5 mag in V and R during the campaign. The two lensed components of quasar HE0047-1756 varied by 0.2-0.3 mag within five years. We provide, for the first time, an estimate of the time delay of component B with respect to A of $\Delta t= 7.6\pm1.8$ days for this object. We also find evidence for a secular evolution of the magnitude difference between components A and B in both filters, which we explain as due to a long-duration microlensing event. Finally we find that both quasars WFI2033-4723 and HE0047-1756 become bluer when brighter, which is consistent with previous studies., Comment: 16 pages, 15 figures, 10 tables. Accepted for publication in A&A
- Published
- 2016
- Full Text
- View/download PDF
7. Erratum: A detailed census of variable stars in the globular cluster NGC 6333 (M9) from CCD differential photometry
- Author
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Ferro, A. Arellano, Bramich, D. M., Jaimes, R. Figuera, Giridhar, Sunetra, Kains, N., Kuppuswamy, K., Jørgensen, Uffe Gråe, Alsubai, K. A., Andersen, J. M., Bozza, V., Browne, P., Novati, S. Calchi, Damerdji, Y., Diehl, C., Dominik, M., Dreizler, S., Elyiv, A., Giannini, E., Harpsøe, Kennet Bomann West, Hessman, F. V., Hinse, T. C., Hundertmark, Markus, Juncher, Diana, Kerins, E., Korhonen, Heidi Helena, Liebig, C., Mancini, L., Mathiasen, M., Penny, M. T., Rabus, M., Rahvar, S., Ricci, D., Scarpetta, G., Skottfelt, Jesper Mirsa, Snodgrass, C., Southworth, J., Surdej, J., Tregloan-Reed, J., Vilela, C., Wertz, O., Ferro, A. Arellano, Bramich, D. M., Jaimes, R. Figuera, Giridhar, Sunetra, Kains, N., Kuppuswamy, K., Jørgensen, Uffe Gråe, Alsubai, K. A., Andersen, J. M., Bozza, V., Browne, P., Novati, S. Calchi, Damerdji, Y., Diehl, C., Dominik, M., Dreizler, S., Elyiv, A., Giannini, E., Harpsøe, Kennet Bomann West, Hessman, F. V., Hinse, T. C., Hundertmark, Markus, Juncher, Diana, Kerins, E., Korhonen, Heidi Helena, Liebig, C., Mancini, L., Mathiasen, M., Penny, M. T., Rabus, M., Rahvar, S., Ricci, D., Scarpetta, G., Skottfelt, Jesper Mirsa, Snodgrass, C., Southworth, J., Surdej, J., Tregloan-Reed, J., Vilela, C., and Wertz, O.
- Published
- 2016
8. Faint source star planetary microlensing: the discovery of the cold gas giant planet OGLE-2014-BLG-0676Lb
- Author
-
Rattenbury, N. J., Bennett, D. P., Sumi, T., Koshimoto, N., Bond, I. A., Udalski, A., Shvartzvald, Y., Maoz, D., Jorgensen, U. G., Dominik, M., Street, R. A., Tsapras, Y., Abe, F., Asakura, Y., Barry, R., Bhattacharya, A., Donachie, M., Evans, P., Freeman, M., 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., Saito, To., Sharan, A., Sullivan, D. J., Suzuki, D., Tristram, P. J., Yonehara, A., Poleski, R., Skowron, J., Mroz, P., Szymanski, M. K., Soszynski, I., Pietrukowicz, P., Kozlowski, S., Ulaczyk, K., Wyrzykowski, L., Friedmann, M., Kaspi, S., Alsubai, K., Browne, P., Andersen, J. M., Bozza, V., Novati, S. Calchi, Damerdji, Y., Diehl, C., Dreizler, S., Elyiv, A., Giannini, E., Hardis, S., Harpsoe, K., Hinse, T. C., Liebig, C., Hundertmark, M., Juncher, D., Kains, N., Kerins, E., Korhonen, H., Mancini, L., Martin, R., Mathiasen, M., Rabus, M., Rahvar, S., Scarpetta, G., Skottfelt, J., Snodgrass, C., Surdej, J., Taylor, J., Tregloan-Reed, J., Vilela, C., Wambsganss, J., Williams, A., D'Ago, G., Bachelet, E., Bramich, D. M., Jaimes, R. Figuera, Horne, K., Menzies, J., Schmidt, R., Steele, I. A., Rattenbury, N. J., Bennett, D. P., Sumi, T., Koshimoto, N., Bond, I. A., Udalski, A., Shvartzvald, Y., Maoz, D., Jorgensen, U. G., Dominik, M., Street, R. A., Tsapras, Y., Abe, F., Asakura, Y., Barry, R., Bhattacharya, A., Donachie, M., Evans, P., Freeman, M., 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., Saito, To., Sharan, A., Sullivan, D. J., Suzuki, D., Tristram, P. J., Yonehara, A., Poleski, R., Skowron, J., Mroz, P., Szymanski, M. K., Soszynski, I., Pietrukowicz, P., Kozlowski, S., Ulaczyk, K., Wyrzykowski, L., Friedmann, M., Kaspi, S., Alsubai, K., Browne, P., Andersen, J. M., Bozza, V., Novati, S. Calchi, Damerdji, Y., Diehl, C., Dreizler, S., Elyiv, A., Giannini, E., Hardis, S., Harpsoe, K., Hinse, T. C., Liebig, C., Hundertmark, M., Juncher, D., Kains, N., Kerins, E., Korhonen, H., Mancini, L., Martin, R., Mathiasen, M., Rabus, M., Rahvar, S., Scarpetta, G., Skottfelt, J., Snodgrass, C., Surdej, J., Taylor, J., Tregloan-Reed, J., Vilela, C., Wambsganss, J., Williams, A., D'Ago, G., Bachelet, E., Bramich, D. M., Jaimes, R. Figuera, Horne, K., Menzies, J., Schmidt, R., and Steele, I. A.
- Abstract
We report the discovery of a planet --- OGLE-2014-BLG-0676Lb --- via gravitational microlensing. Observations for the lensing event were made by the MOA, OGLE, Wise, RoboNET/LCOGT, MiNDSTEp and $\mu$FUN groups. All analyses of the light curve data favour a lens system comprising a planetary mass orbiting a host star. The most favoured binary lens model has a mass ratio between the two lens masses of $(4.78 \pm 0.13)\times 10^{-3}$. Subject to some important assumptions, a Bayesian probability density analysis suggests the lens system comprises a $3.09_{-1.12}^{+1.02}$ M_jup planet orbiting a $0.62_{-0.22}^{+0.20}$ M_sun host star at a deprojected orbital separation of $4.40_{-1.46}^{+2.16}$ AU. The distance to the lens system is $2.22_{-0.83}^{+0.96}$ kpc. Planet OGLE-2014-BLG-0676Lb provides additional data to the growing number of cool planets discovered using gravitational microlensing against which planetary formation theories may be tested. Most of the light in the baseline of this event is expected to come from the lens and thus high-resolution imaging observations could confirm our planetary model interpretation., Comment: 10 pages, 5 figures, MNRAS accepted
- Published
- 2016
- Full Text
- View/download PDF
9. MiNDSTEp differential photometry of the gravitationally lensed quasars WFI2033-4723 and HE0047-1756: Microlensing and a new time delay
- Author
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Giannini, E., Schmidt, R. W., Wambsganß, J., Alsubai, K., Andersen, J. M., Anguita, T., Bozza, V., Bramich, D. M., Browne, P., Novati, S. Calchi, Damerdji, Y., Diehl, C., Dodds, P., Dominik, M., Elyiv, A., Fang, X., Jaimes, R. Figuera, Finet, F., Gerner, T., Gu, S., Hardis, S., Harpsøe, K., Hinse, T. C., Hornstrup, A., Hundertmark, M., Jessen-Hansen, J., Jørgensen, U. G., Juncher, D., Kains, N., Kerins, E., Korhonen, H., Liebig, C., Lund, M. N., Lundkvist, M. S., Maier, G., Mancini, L., Masi, G., Mathiasen, M., Penny, M., Proft, S., Rabus, M., Rahvar, S., Ricci, D., Scarpetta, G., Sahu, K., Schäfer, S., Schönebeck, F., Skottfelt, J., Snodgrass, C., Southworth, J., Surdej, J., Tregloan-Reed, J., Vilela, C., Wertz, O., Zimmer, F., Giannini, E., Schmidt, R. W., Wambsganß, J., Alsubai, K., Andersen, J. M., Anguita, T., Bozza, V., Bramich, D. M., Browne, P., Novati, S. Calchi, Damerdji, Y., Diehl, C., Dodds, P., Dominik, M., Elyiv, A., Fang, X., Jaimes, R. Figuera, Finet, F., Gerner, T., Gu, S., Hardis, S., Harpsøe, K., Hinse, T. C., Hornstrup, A., Hundertmark, M., Jessen-Hansen, J., Jørgensen, U. G., Juncher, D., Kains, N., Kerins, E., Korhonen, H., Liebig, C., Lund, M. N., Lundkvist, M. S., Maier, G., Mancini, L., Masi, G., Mathiasen, M., Penny, M., Proft, S., Rabus, M., Rahvar, S., Ricci, D., Scarpetta, G., Sahu, K., Schäfer, S., Schönebeck, F., Skottfelt, J., Snodgrass, C., Southworth, J., Surdej, J., Tregloan-Reed, J., Vilela, C., Wertz, O., and Zimmer, F.
- Abstract
We present V and R photometry of the gravitationally lensed quasars WFI2033-4723 and HE0047-1756. The data were taken by the MiNDSTEp collaboration with the 1.54 m Danish telescope at the ESO La Silla observatory from 2008 to 2012. Differential photometry has been carried out using the image subtraction method as implemented in the HOTPAnTS package, additionally using GALFIT for quasar photometry. The quasar WFI2033-4723 showed brightness variations of order 0.5 mag in V and R during the campaign. The two lensed components of quasar HE0047-1756 varied by 0.2-0.3 mag within five years. We provide, for the first time, an estimate of the time delay of component B with respect to A of $\Delta t= 7.6\pm1.8$ days for this object. We also find evidence for a secular evolution of the magnitude difference between components A and B in both filters, which we explain as due to a long-duration microlensing event. Finally we find that both quasars WFI2033-4723 and HE0047-1756 become bluer when brighter, which is consistent with previous studies., Comment: 16 pages, 15 figures, 10 tables. Accepted for publication in A&A
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- 2016
- Full Text
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10. Estimating the parameters of globular cluster M 30 (NGC 7099) from time-series photometry (Corrigendum)
- Author
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Kains, N., Bramich, D. M., Ferro, A. Arellano, Jaimes, R. Figuera, Jorgensen, U. G., Giridhar, S., Penny, M. T., Alsubai, Khalid A., Andersen, J. M., Bozza, V., Browne, P., Burgdorf, M., Novati, S. Calchi, Damerdji, Y., Diehl, C., Dodds, P., Dominik, M., Elyiv, A., Fang, X.-S, Giannini, Edward H, Hardis, S., Harpsoe, K., Hinse, T. C., Hornstrup, A., Hundertmark, M., Jessen-Hansen, Jens, Juncher, D., Kerins, E., Kjeldsen, H, Korhonen, H., Liebig, C., Lund, M. N., Lundkvist, M., Mancini, L., Martin, R., Mathiasen, M., Rabus, M., Rahvar, S., Ricci, D., Sahu, K., Scarpetta, G., Skottfelt, J., Snodgrass, C., Southworth, J., Surdej, J., Tregloan-Reed, J., Vilela, C., Wertz, O., Williams, A., Kains, N., Bramich, D. M., Ferro, A. Arellano, Jaimes, R. Figuera, Jorgensen, U. G., Giridhar, S., Penny, M. T., Alsubai, Khalid A., Andersen, J. M., Bozza, V., Browne, P., Burgdorf, M., Novati, S. Calchi, Damerdji, Y., Diehl, C., Dodds, P., Dominik, M., Elyiv, A., Fang, X.-S, Giannini, Edward H, Hardis, S., Harpsoe, K., Hinse, T. C., Hornstrup, A., Hundertmark, M., Jessen-Hansen, Jens, Juncher, D., Kerins, E., Kjeldsen, H, Korhonen, H., Liebig, C., Lund, M. N., Lundkvist, M., Mancini, L., Martin, R., Mathiasen, M., Rabus, M., Rahvar, S., Ricci, D., Sahu, K., Scarpetta, G., Skottfelt, J., Snodgrass, C., Southworth, J., Surdej, J., Tregloan-Reed, J., Vilela, C., Wertz, O., and Williams, A.
- Published
- 2016
11. Erratum: Estimating the parameters of globular cluster M 30 (NGC 7099) from time-series photometry (Astronomy and Astrophysics (2013) 555 (A36))
- Author
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Kains, N., Bramich, D., Arellano Ferro, A., Figuera Jaimes, R., Jørgensen, U., Giridhar, S., Penny, M., Alsubai, K., Andersen, J., Bozza, V., Browne, P., Burgdorf, M., Calchi Novati, S., Damerdji, Y., Diehl, C., Dodds, P., Dominik, M., Elyiv, A., Fang, X., Giannini, E., Gu, S., Hardis, S., Harpsøe, K., Hinse, T., Hornstrup, A., Hundertmark, M., Jessen-Hansen, J., Juncher, D., Kerins, E., Kjeldsen, H., Korhonen, H., Liebig, C., Lund, M., Lundkvist, M., Mancini, L., Martin, R., Mathiasen, M., Rabus, M., Rahvar, S., Ricci, D., Sahu, K., Scarpetta, G., Skottfelt, J., Snodgrass, C., Southworth, J., Surdej, J., Tregloan-Reed, J., Vilela, C., Wertz, O., Williams, Andrew, Kains, N., Bramich, D., Arellano Ferro, A., Figuera Jaimes, R., Jørgensen, U., Giridhar, S., Penny, M., Alsubai, K., Andersen, J., Bozza, V., Browne, P., Burgdorf, M., Calchi Novati, S., Damerdji, Y., Diehl, C., Dodds, P., Dominik, M., Elyiv, A., Fang, X., Giannini, E., Gu, S., Hardis, S., Harpsøe, K., Hinse, T., Hornstrup, A., Hundertmark, M., Jessen-Hansen, J., Juncher, D., Kerins, E., Kjeldsen, H., Korhonen, H., Liebig, C., Lund, M., Lundkvist, M., Mancini, L., Martin, R., Mathiasen, M., Rabus, M., Rahvar, S., Ricci, D., Sahu, K., Scarpetta, G., Skottfelt, J., Snodgrass, C., Southworth, J., Surdej, J., Tregloan-Reed, J., Vilela, C., Wertz, O., and Williams, Andrew
- Published
- 2016
12. High-precision photometry by telescope defocussing. VIII. WASP-22, WASP-41, WASP-42 and WASP-55
- Author
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Southworth, John, Tregloan-Reed, J., Andersen, M. I., Novati, S. Calchi, Ciceri, S., Colque, J. P., D'Ago, G., Dominik, M., Evans, D., Gu, S. -H., Herrera-Cruces, A., Hinse, T. C., Jorgensen, U. G., Juncher, D., Kuffmeier, M., Mancini, L., Peixinho, N., Popovas, A., Rabus, M., Skottfelt, J., Tronsgaard, R., Unda-Sanzana, E., Wang, X. -B., Wertz, O., Alsubai, K. A., Andersen, J. M., Bozza, V., Bramich, D. M., Burgdorf, M., Damerdji, Y., Diehl, C., Elyiv, A., Jaimes, R. Figuera, Haugbolle, T., Hundertmark, M., Kains, N., Kerins, E., Korhonen, H., Liebig, C., Mathiasen, M., Penny, M. T., Rahvar, S., Scarpetta, G., Schmidt, R. W., Snodgrass, C., Starkey, D., Surdej, J., Vilela, C., von Essen, C., Wang, Y., Southworth, John, Tregloan-Reed, J., Andersen, M. I., Novati, S. Calchi, Ciceri, S., Colque, J. P., D'Ago, G., Dominik, M., Evans, D., Gu, S. -H., Herrera-Cruces, A., Hinse, T. C., Jorgensen, U. G., Juncher, D., Kuffmeier, M., Mancini, L., Peixinho, N., Popovas, A., Rabus, M., Skottfelt, J., Tronsgaard, R., Unda-Sanzana, E., Wang, X. -B., Wertz, O., Alsubai, K. A., Andersen, J. M., Bozza, V., Bramich, D. M., Burgdorf, M., Damerdji, Y., Diehl, C., Elyiv, A., Jaimes, R. Figuera, Haugbolle, T., Hundertmark, M., Kains, N., Kerins, E., Korhonen, H., Liebig, C., Mathiasen, M., Penny, M. T., Rahvar, S., Scarpetta, G., Schmidt, R. W., Snodgrass, C., Starkey, D., Surdej, J., Vilela, C., von Essen, C., and Wang, Y.
- Abstract
We present 13 high-precision and four additional light curves of four bright southern-hemisphere transiting planetary systems: WASP-22, WASP-41, WASP-42 and WASP-55. In the cases of WASP-42 and WASP-55, these are the first follow-up observations since their discovery papers. We present refined measurements of the physical properties and orbital ephemerides of all four systems. No indications of transit timing variations were seen. All four planets have radii inflated above those expected from theoretical models of gas-giant planets; WASP-55b is the most discrepant with a mass of 0.63 Mjup and a radius of 1.34 Rjup. WASP-41 shows brightness anomalies during transit due to the planet occulting spots on the stellar surface. Two anomalies observed 3.1 d apart are very likely due to the same spot. We measure its change in position and determine a rotation period for the host star of 18.6 +/- 1.5 d, in good agreement with a published measurement from spot-induced brightness modulation, and a sky-projected orbital obliquity of lambda = 6 +/- 11 degrees. We conclude with a compilation of obliquity measurements from spot-tracking analyses and a discussion of this technique in the study of the orbital configurations of hot Jupiters., Comment: 13 pages, 8 tables, 11 figures. Version 2 is the final accepted version of the paper
- Published
- 2015
- Full Text
- View/download PDF
13. High-precision photometry by telescope defocussing. VIII. WASP-22, WASP-41, WASP-42 and WASP-55
- Author
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Southworth, John, Tregloan-Reed, J., Andersen, M. I., Novati, S. Calchi, Ciceri, S., Colque, J. P., D'Ago, G., Dominik, M., Evans, D., Gu, S. -H., Herrera-Cruces, A., Hinse, T. C., Jorgensen, U. G., Juncher, D., Kuffmeier, M., Mancini, L., Peixinho, N., Popovas, A., Rabus, M., Skottfelt, J., Tronsgaard, R., Unda-Sanzana, E., Wang, X. -B., Wertz, O., Alsubai, K. A., Andersen, J. M., Bozza, V., Bramich, D. M., Burgdorf, M., Damerdji, Y., Diehl, C., Elyiv, A., Jaimes, R. Figuera, Haugbolle, T., Hundertmark, M., Kains, N., Kerins, E., Korhonen, H., Liebig, C., Mathiasen, M., Penny, M. T., Rahvar, S., Scarpetta, G., Schmidt, R. W., Snodgrass, C., Starkey, D., Surdej, J., Vilela, C., von Essen, C., Wang, Y., Southworth, John, Tregloan-Reed, J., Andersen, M. I., Novati, S. Calchi, Ciceri, S., Colque, J. P., D'Ago, G., Dominik, M., Evans, D., Gu, S. -H., Herrera-Cruces, A., Hinse, T. C., Jorgensen, U. G., Juncher, D., Kuffmeier, M., Mancini, L., Peixinho, N., Popovas, A., Rabus, M., Skottfelt, J., Tronsgaard, R., Unda-Sanzana, E., Wang, X. -B., Wertz, O., Alsubai, K. A., Andersen, J. M., Bozza, V., Bramich, D. M., Burgdorf, M., Damerdji, Y., Diehl, C., Elyiv, A., Jaimes, R. Figuera, Haugbolle, T., Hundertmark, M., Kains, N., Kerins, E., Korhonen, H., Liebig, C., Mathiasen, M., Penny, M. T., Rahvar, S., Scarpetta, G., Schmidt, R. W., Snodgrass, C., Starkey, D., Surdej, J., Vilela, C., von Essen, C., and Wang, Y.
- Abstract
We present 13 high-precision and four additional light curves of four bright southern-hemisphere transiting planetary systems: WASP-22, WASP-41, WASP-42 and WASP-55. In the cases of WASP-42 and WASP-55, these are the first follow-up observations since their discovery papers. We present refined measurements of the physical properties and orbital ephemerides of all four systems. No indications of transit timing variations were seen. All four planets have radii inflated above those expected from theoretical models of gas-giant planets; WASP-55b is the most discrepant with a mass of 0.63 Mjup and a radius of 1.34 Rjup. WASP-41 shows brightness anomalies during transit due to the planet occulting spots on the stellar surface. Two anomalies observed 3.1 d apart are very likely due to the same spot. We measure its change in position and determine a rotation period for the host star of 18.6 +/- 1.5 d, in good agreement with a published measurement from spot-induced brightness modulation, and a sky-projected orbital obliquity of lambda = 6 +/- 11 degrees. We conclude with a compilation of obliquity measurements from spot-tracking analyses and a discussion of this technique in the study of the orbital configurations of hot Jupiters., Comment: 13 pages, 8 tables, 11 figures. Version 2 is the final accepted version of the paper
- Published
- 2015
- Full Text
- View/download PDF
14. OGLE-2011-BLG-0265Lb: A JOVIAN MICROLENSING PLANET ORBITING AN M DWARF
- Author
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Skowron, J., Shin, I. -G., Udalski, A., Han, C., Sumi, T., Shvartzvald, Y., Gould, A., Prester, D. Dominis, Street, R. A., Jorgensen, U. G., Bennett, D. P., Bozza, V., Szymanski, M. K., Kubiak, M., Pietrzynski, G., Soszynski, I., Poleski, R., Kozlowski, S., Pietrukowicz, P., Ulaczyk, K., Wyrzykowski, L., 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., Maoz, D., Kaspi, S., Friedmann, M., 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., Albrow, M. D., Bachelet, E., Beaulieu, J. -P., Brillant, S., Caldwell, J. A. R., Cassan, A., Cole, A., Corrales, E., Coutures, C. H., Dieters, S., Donatowicz, J., Fouque, 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., Tsapras, Y., Bramich, D. M., Horne, K., Hundertmark, M., Snodgrass, C., Steele, I. A., Alsubai, K. A., Browne, P., Burgdorf, M. J., Novati, S. Calchi, Dodds, P., Dominik, M., Dreizler, S., Fang, X. -S., Gu, C. -H., Hardis, Harpsøe, Kennet Bomann West, 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, D., Scarpetta, G., Skottfelt, J., Southworth, J., Surdej, J., Tregloan-Reed, J., Wertz, O., Skowron, J., Shin, I. -G., Udalski, A., Han, C., Sumi, T., Shvartzvald, Y., Gould, A., Prester, D. Dominis, Street, R. A., Jorgensen, U. G., Bennett, D. P., Bozza, V., Szymanski, M. K., Kubiak, M., Pietrzynski, G., Soszynski, I., Poleski, R., Kozlowski, S., Pietrukowicz, P., Ulaczyk, K., Wyrzykowski, L., 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., Maoz, D., Kaspi, S., Friedmann, M., 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., Albrow, M. D., Bachelet, E., Beaulieu, J. -P., Brillant, S., Caldwell, J. A. R., Cassan, A., Cole, A., Corrales, E., Coutures, C. H., Dieters, S., Donatowicz, J., Fouque, 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., Tsapras, Y., Bramich, D. M., Horne, K., Hundertmark, M., Snodgrass, C., Steele, I. A., Alsubai, K. A., Browne, P., Burgdorf, M. J., Novati, S. Calchi, Dodds, P., Dominik, M., Dreizler, S., Fang, X. -S., Gu, C. -H., Hardis, Harpsøe, Kennet Bomann West, 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, D., Scarpetta, G., Skottfelt, J., Southworth, J., Surdej, J., Tregloan-Reed, J., and Wertz, O.
- Published
- 2015
15. OGLE-2011-BLG-0265Lb: a Jovian Microlensing Planet Orbiting an M Dwarf
- Author
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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., 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., Maoz, D., Kaspi, S., Friedman, M., 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., 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., Tsapras, Y., Bramich, D. M., Horne, K., Hundertmark, M., Snodgrass, C., Steele, I. A., Alsubai, K. A., Browne, P., Burgdorf, M. J., Novati, S. Calchi, 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, D., Scarpetta, G., Skottfelt, J., Southworth, J., Surdej, J., Tregloan-Reed, J., Wertz, O., 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., 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., Maoz, D., Kaspi, S., Friedman, M., 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., 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., Tsapras, Y., Bramich, D. M., Horne, K., Hundertmark, M., Snodgrass, C., Steele, I. A., Alsubai, K. A., Browne, P., Burgdorf, M. J., Novati, S. Calchi, 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, D., Scarpetta, G., Skottfelt, J., Southworth, J., Surdej, J., Tregloan-Reed, J., and Wertz, O.
- 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
- 2014
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- View/download PDF
16. High-precision photometry by telescope defocussing. VI. WASP-24, WASP-25 and WASP-26
- Author
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Southworth, John, Hinse, T. C., Burgdorf, M., Novati, S. Calchi, Dominik, M., Galianni, P., Gerner, T., Giannini, E., Gu, S. -H., Hundertmark, M., Jorgensen, U. G., Juncher, D., Kerins, E., Mancini, L., Rabus, M., Ricci, D., Schaefer, S., Skottfelt, J., Tregloan-Reed, J., Wang, X. -B., Wertz, O., Alsubai, K. A., Andersen, J. M., Bozza, V., Bramich, D. M., Browne, P., Ciceri, S., D'Ago, G., Damerdji, Y., Diehl, C., Dodds, P., Elyiv, A., Fang, X. -S., Finet, F., Jaimes, R. Figuera, Hardis, S., Harpsoe, K., Jessen-Hansen, J., Kains, N., Kjeldsen, H., Korhonen, H., Liebig, C., Lund, M. N., Lundkvist, M., Mathiasen, M., Penny, M. T., Popovas, A., Proft, S., Rahvar, S., Sahu, K., Scarpetta, G., Schmidt, R. W., Schoenebeck, F., Snodgrass, C., Street, R. A., Surdej, J., Tsapras, Y., Vilela, C., Southworth, John, Hinse, T. C., Burgdorf, M., Novati, S. Calchi, Dominik, M., Galianni, P., Gerner, T., Giannini, E., Gu, S. -H., Hundertmark, M., Jorgensen, U. G., Juncher, D., Kerins, E., Mancini, L., Rabus, M., Ricci, D., Schaefer, S., Skottfelt, J., Tregloan-Reed, J., Wang, X. -B., Wertz, O., Alsubai, K. A., Andersen, J. M., Bozza, V., Bramich, D. M., Browne, P., Ciceri, S., D'Ago, G., Damerdji, Y., Diehl, C., Dodds, P., Elyiv, A., Fang, X. -S., Finet, F., Jaimes, R. Figuera, Hardis, S., Harpsoe, K., Jessen-Hansen, J., Kains, N., Kjeldsen, H., Korhonen, H., Liebig, C., Lund, M. N., Lundkvist, M., Mathiasen, M., Penny, M. T., Popovas, A., Proft, S., Rahvar, S., Sahu, K., Scarpetta, G., Schmidt, R. W., Schoenebeck, F., Snodgrass, C., Street, R. A., Surdej, J., Tsapras, Y., and Vilela, C.
- Abstract
We present time-series photometric observations of thirteen transits in the planetary systems WASP-24, WASP-25 and WASP-26. All three systems have orbital obliquity measurements, WASP-24 and WASP-26 have been observed with Spitzer, and WASP-25 was previously comparatively neglected. Our light curves were obtained using the telescope-defocussing method and have scatters of 0.5 to 1.2 mmag relative to their best-fitting geometric models. We used these data to measure the physical properties and orbital ephemerides of the systems to high precision, finding that our improved measurements are in good agreement with previous studies. High-resolution Lucky Imaging observations of all three targets show no evidence for faint stars close enough to contaminate our photometry. We confirm the eclipsing nature of the star closest to WASP-24 and present the detection of a detached eclipsing binary within 4.25 arcmin of WASP-26., Comment: Accepted for publication in MNRAS. 14 pages, 10 figures, 8 tables. Data and supplementary information are available on request
- Published
- 2014
- Full Text
- View/download PDF
17. OGLE-2011-BLG-0265Lb: a Jovian Microlensing Planet Orbiting an M Dwarf
- Author
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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., 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., Maoz, D., Kaspi, S., Friedman, M., 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., 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., Tsapras, Y., Bramich, D. M., Horne, K., Hundertmark, M., Snodgrass, C., Steele, I. A., Alsubai, K. A., Browne, P., Burgdorf, M. J., Novati, S. Calchi, 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, D., Scarpetta, G., Skottfelt, J., Southworth, J., Surdej, J., Tregloan-Reed, J., Wertz, O., 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., 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., Maoz, D., Kaspi, S., Friedman, M., 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., 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., Tsapras, Y., Bramich, D. M., Horne, K., Hundertmark, M., Snodgrass, C., Steele, I. A., Alsubai, K. A., Browne, P., Burgdorf, M. J., Novati, S. Calchi, 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, D., Scarpetta, G., Skottfelt, J., Southworth, J., Surdej, J., Tregloan-Reed, J., and Wertz, O.
- 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
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- 2014
- Full Text
- View/download PDF
18. High-precision photometry by telescope defocussing. VI. WASP-24, WASP-25 and WASP-26
- Author
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Southworth, John, Hinse, T. C., Burgdorf, M., Novati, S. Calchi, Dominik, M., Galianni, P., Gerner, T., Giannini, E., Gu, S. -H., Hundertmark, M., Jorgensen, U. G., Juncher, D., Kerins, E., Mancini, L., Rabus, M., Ricci, D., Schaefer, S., Skottfelt, J., Tregloan-Reed, J., Wang, X. -B., Wertz, O., Alsubai, K. A., Andersen, J. M., Bozza, V., Bramich, D. M., Browne, P., Ciceri, S., D'Ago, G., Damerdji, Y., Diehl, C., Dodds, P., Elyiv, A., Fang, X. -S., Finet, F., Jaimes, R. Figuera, Hardis, S., Harpsoe, K., Jessen-Hansen, J., Kains, N., Kjeldsen, H., Korhonen, H., Liebig, C., Lund, M. N., Lundkvist, M., Mathiasen, M., Penny, M. T., Popovas, A., Proft, S., Rahvar, S., Sahu, K., Scarpetta, G., Schmidt, R. W., Schoenebeck, F., Snodgrass, C., Street, R. A., Surdej, J., Tsapras, Y., Vilela, C., Southworth, John, Hinse, T. C., Burgdorf, M., Novati, S. Calchi, Dominik, M., Galianni, P., Gerner, T., Giannini, E., Gu, S. -H., Hundertmark, M., Jorgensen, U. G., Juncher, D., Kerins, E., Mancini, L., Rabus, M., Ricci, D., Schaefer, S., Skottfelt, J., Tregloan-Reed, J., Wang, X. -B., Wertz, O., Alsubai, K. A., Andersen, J. M., Bozza, V., Bramich, D. M., Browne, P., Ciceri, S., D'Ago, G., Damerdji, Y., Diehl, C., Dodds, P., Elyiv, A., Fang, X. -S., Finet, F., Jaimes, R. Figuera, Hardis, S., Harpsoe, K., Jessen-Hansen, J., Kains, N., Kjeldsen, H., Korhonen, H., Liebig, C., Lund, M. N., Lundkvist, M., Mathiasen, M., Penny, M. T., Popovas, A., Proft, S., Rahvar, S., Sahu, K., Scarpetta, G., Schmidt, R. W., Schoenebeck, F., Snodgrass, C., Street, R. A., Surdej, J., Tsapras, Y., and Vilela, C.
- Abstract
We present time-series photometric observations of thirteen transits in the planetary systems WASP-24, WASP-25 and WASP-26. All three systems have orbital obliquity measurements, WASP-24 and WASP-26 have been observed with Spitzer, and WASP-25 was previously comparatively neglected. Our light curves were obtained using the telescope-defocussing method and have scatters of 0.5 to 1.2 mmag relative to their best-fitting geometric models. We used these data to measure the physical properties and orbital ephemerides of the systems to high precision, finding that our improved measurements are in good agreement with previous studies. High-resolution Lucky Imaging observations of all three targets show no evidence for faint stars close enough to contaminate our photometry. We confirm the eclipsing nature of the star closest to WASP-24 and present the detection of a detached eclipsing binary within 4.25 arcmin of WASP-26., Comment: Accepted for publication in MNRAS. 14 pages, 10 figures, 8 tables. Data and supplementary information are available on request
- Published
- 2014
- Full Text
- View/download PDF
19. A SUPER-JUPITER ORBITING A LATE-TYPE STAR:A REFINED ANALYSIS OF MICROLENSING EVENT OGLE-2012-BLG-0406
- Author
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Tsapras, Y., Choi, J. -Y., Street, R. A., Han, C., Bozza, V., Gould, A., Dominik, M., Beaulieu, J. -P., Udalski, A., Jorgensen, U. G., Sumi, T., Bramich, D. M., Browne, P., Horne, K., Hundertmark, Markus Peter Gerhard, Ipatov, S., Kains, N., Snodgrass, C., Steele, I. A., Alsubai, K. A., Andersen, J. M., Novati, S. Calchi, Damerdji, Y., Diehl, C., Elyiv, A., Giannini, E., Hardis, S., Harpsøe, Kennet Bomann West, 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., Kozllowski, S., Wyrzykowski, E., Szymanski, M. K., Kubiak, M., Pietrukowicz, P., Pietrzynski, G., Soszynski, 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., Fouque, P., Greenhill, J., Kane, S. R., Kubas, D., Marquette, J. -B., Menzies, J., Ere, C. P., 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, To., Sullivan, D. J., Sweatman, W. L., Suzuki, D., Tristram, P. J., Tsurumi, N., Wada, K., Yamai, N., Yock, P. C. M., Yonehara, A., Tsapras, Y., Choi, J. -Y., Street, R. A., Han, C., Bozza, V., Gould, A., Dominik, M., Beaulieu, J. -P., Udalski, A., Jorgensen, U. G., Sumi, T., Bramich, D. M., Browne, P., Horne, K., Hundertmark, Markus Peter Gerhard, Ipatov, S., Kains, N., Snodgrass, C., Steele, I. A., Alsubai, K. A., Andersen, J. M., Novati, S. Calchi, Damerdji, Y., Diehl, C., Elyiv, A., Giannini, E., Hardis, S., Harpsøe, Kennet Bomann West, 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., Kozllowski, S., Wyrzykowski, E., Szymanski, M. K., Kubiak, M., Pietrukowicz, P., Pietrzynski, G., Soszynski, 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., Fouque, P., Greenhill, J., Kane, S. R., Kubas, D., Marquette, J. -B., Menzies, J., Ere, C. P., 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, 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.
- Published
- 2014
20. A SUPER-JUPITER ORBITING A LATE-TYPE STAR:A REFINED ANALYSIS OF MICROLENSING EVENT OGLE-2012-BLG-0406
- Author
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Tsapras, Y., Choi, J. -Y., Street, R. A., Han, C., Bozza, V., Gould, A., Dominik, M., Beaulieu, J. -P., Udalski, A., Jorgensen, U. G., Sumi, T., Bramich, D. M., Browne, P., Horne, K., Hundertmark, Markus Peter Gerhard, Ipatov, S., Kains, N., Snodgrass, C., Steele, I. A., Alsubai, K. A., Andersen, J. M., Novati, S. Calchi, Damerdji, Y., Diehl, C., Elyiv, A., Giannini, E., Hardis, S., Harpsøe, Kennet Bomann West, 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., Kozllowski, S., Wyrzykowski, E., Szymanski, M. K., Kubiak, M., Pietrukowicz, P., Pietrzynski, G., Soszynski, 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., Fouque, P., Greenhill, J., Kane, S. R., Kubas, D., Marquette, J. -B., Menzies, J., Ere, C. P., 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, To., Sullivan, D. J., Sweatman, W. L., Suzuki, D., Tristram, P. J., Tsurumi, N., Wada, K., Yamai, N., Yock, P. C. M., Yonehara, A., Tsapras, Y., Choi, J. -Y., Street, R. A., Han, C., Bozza, V., Gould, A., Dominik, M., Beaulieu, J. -P., Udalski, A., Jorgensen, U. G., Sumi, T., Bramich, D. M., Browne, P., Horne, K., Hundertmark, Markus Peter Gerhard, Ipatov, S., Kains, N., Snodgrass, C., Steele, I. A., Alsubai, K. A., Andersen, J. M., Novati, S. Calchi, Damerdji, Y., Diehl, C., Elyiv, A., Giannini, E., Hardis, S., Harpsøe, Kennet Bomann West, 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., Kozllowski, S., Wyrzykowski, E., Szymanski, M. K., Kubiak, M., Pietrukowicz, P., Pietrzynski, G., Soszynski, 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., Fouque, P., Greenhill, J., Kane, S. R., Kubas, D., Marquette, J. -B., Menzies, J., Ere, C. P., 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, 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.
- Published
- 2014
21. A Super-Jupiter orbiting a late-type star: A refined analysis of microlensing event OGLE-2012-BLG-0406
- Author
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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. Calchi, 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, Łukasz, 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., Fouqué, P., Greenhill, J., Kane, S. R., Kubas, D., Marquette, J. -B., Menzies, J., P`ere, C., Pollard, K. R., Wouters, D., 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, To., Sullivan, D. J., Sweatman, W. L., Suzuki, D., Tristram, P. J., Tsurumi, N., Wada, K., Yamai, N., Yonehara, P. C. M. Yock A., 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. Calchi, 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, Łukasz, 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., Fouqué, P., Greenhill, J., Kane, S. R., Kubas, D., Marquette, J. -B., Menzies, J., P`ere, C., Pollard, K. R., Wouters, D., 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, To., Sullivan, D. J., Sweatman, W. L., Suzuki, D., Tristram, P. J., Tsurumi, N., Wada, K., Yamai, N., and Yonehara, P. C. M. Yock A.
- 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., Comment: 9 pages, 4 figures, accepted by ApJ
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- 2013
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22. MOA-2010-BLG-328Lb: a sub-Neptune orbiting very late M dwarf ?
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Furusawa, K., Udalski, A., Sumi, T., Bennett, D. P., Bond, I. A., Gould, A., Jorgensen, U. G., Snodgrass, C., Prester, D. Dominis, Albrow, M. D., Abe, F., Botzler, C. S., Chote, P., Freeman, M., Fukui, A., Harris, P., Itow, Y., Ling, C. H., Masuda, K., Matsubara, Y., Miyake, N., Muraki, Y., Ohnishi, K., Rattenbury, N. J., Saito, To., Sullivan, D. J., Suzuki, D., Sweatman, W. L., Tristram, P. J., Wada, K., Yock, P. C. M., Szymanski, M. K., Soszynski, I., Kubiak, M., Poleski, R., Ulaczyk, K., Pietrzynski, G., Wyrzykowski, L., Choi, J. Y., Christie, G. W., DePoy, D. L., Dong, S., Drummond, J., Gaudi, B. S., Han, C., Hung, L. -W., Jung, Y. -K., Lee, C. -U., McCormick, J., Moorhouse, D., Natusch, T., Nola, M., Ofek, E., Park, B. G., Park, H., Pogge, R. W., Shin, I. -G., Skowron, J., Thornley, G., Yee, J. C., Alsubai, K. A., Bozza, V., Browne, P., Burgdorf, M. J., Novati, S. Calchi, Dodds, P., Dominik, M., Finet, F., Gerner, T., Hardis, S., Harpsoe, K., Hinse, T. C., Hundertmark, M., Kains, N., Kerins, E., Liebig, C., Mancini, L., Mathiasen, M., Penny, M. T., Proft, S., Rahvar, S., Ricci, D., Scarpetta, G., Schafer, S., Schonebeck, F., Southworth, J., Surdej, J., Wambsganss, J., Street, R. A., Bramich, D. M., Steele, I. A., Tsapras, Y., Horne, K., Donatowicz, J., Sahu, K. C., Bachelet, E., Batista, V., Beatty, T. G., Beaulieu, J. -P., Bennett, C. S., Black, C., Bowens-Rubin, R., Brillant, S., Caldwell, J. A. R., Cassan, A., Cole, A. A., Corrales, E., Coutures, C., Dieters, S., Fouque, P., Greenhill, J., Henderson, C. B., Kubas, D., Marquette, J. -B., Martin, R., Menzies, J. W., Shappee, B., Williams, A., Wouters, D., van Saders, J., Zellem, R., Zub, M., Furusawa, K., Udalski, A., Sumi, T., Bennett, D. P., Bond, I. A., Gould, A., Jorgensen, U. G., Snodgrass, C., Prester, D. Dominis, Albrow, M. D., Abe, F., Botzler, C. S., Chote, P., Freeman, M., Fukui, A., Harris, P., Itow, Y., Ling, C. H., Masuda, K., Matsubara, Y., Miyake, N., Muraki, Y., Ohnishi, K., Rattenbury, N. J., Saito, To., Sullivan, D. J., Suzuki, D., Sweatman, W. L., Tristram, P. J., Wada, K., Yock, P. C. M., Szymanski, M. K., Soszynski, I., Kubiak, M., Poleski, R., Ulaczyk, K., Pietrzynski, G., Wyrzykowski, L., Choi, J. Y., Christie, G. W., DePoy, D. L., Dong, S., Drummond, J., Gaudi, B. S., Han, C., Hung, L. -W., Jung, Y. -K., Lee, C. -U., McCormick, J., Moorhouse, D., Natusch, T., Nola, M., Ofek, E., Park, B. G., Park, H., Pogge, R. W., Shin, I. -G., Skowron, J., Thornley, G., Yee, J. C., Alsubai, K. A., Bozza, V., Browne, P., Burgdorf, M. J., Novati, S. Calchi, Dodds, P., Dominik, M., Finet, F., Gerner, T., Hardis, S., Harpsoe, K., Hinse, T. C., Hundertmark, M., Kains, N., Kerins, E., Liebig, C., Mancini, L., Mathiasen, M., Penny, M. T., Proft, S., Rahvar, S., Ricci, D., Scarpetta, G., Schafer, S., Schonebeck, F., Southworth, J., Surdej, J., Wambsganss, J., Street, R. A., Bramich, D. M., Steele, I. A., Tsapras, Y., Horne, K., Donatowicz, J., Sahu, K. C., Bachelet, E., Batista, V., Beatty, T. G., Beaulieu, J. -P., Bennett, C. S., Black, C., Bowens-Rubin, R., Brillant, S., Caldwell, J. A. R., Cassan, A., Cole, A. A., Corrales, E., Coutures, C., Dieters, S., Fouque, P., Greenhill, J., Henderson, C. B., Kubas, D., Marquette, J. -B., Martin, R., Menzies, J. W., Shappee, B., Williams, A., Wouters, D., van Saders, J., Zellem, R., and Zub, M.
- Abstract
We analyze the planetary microlensing event MOA-2010-BLG-328. The best fit yields host and planetary masses of Mh = 0.11+/-0.01 M_{sun} and Mp = 9.2+/-2.2M_Earth, corresponding to a very late M dwarf and sub-Neptune-mass planet, respectively. The system lies at DL = 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., Comment: 30 pages, 6 figures. accepted for publication in ApJ. Figure 1 and 2 are updated
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23. Physical properties, transmission and emission spectra of the WASP-19 planetary system from multi-colour photometry
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Mancini, L., Ciceri, S., Chen, G., Tregloan-Reed, J., Fortney, J. J., Southworth, J., Tan, T. G., Burgdorf, M., Novati, S. Calchi, Dominik, M., Fang, X. -S., Finet, F., Gerner, T., Hardis, S., Hinse, T. C., Jorgensen, U. G., Liebig, C., Nikolov, N., Ricci, D., Schaefer, S., Schoenebeck, F., Skottfelt, J., Wertz, O., Alsubai, K. A., Bozza, V., Browne, P., Dodds, P., Gu, S. -H., Harpsoe, K., Henning, Th., Hundertmark, M., Jessen-Hansen, J., Kains, N., Kerins, E., Kjeldsen, H., Lund, M. N., Lundkvist, M., Madhusudhan, N., Mathiasen, M., Penny, M. T., Proft, S., Rahvar, S., Sahu, K., Scarpetta, G., Snodgrass, C., Surdej, J., Mancini, L., Ciceri, S., Chen, G., Tregloan-Reed, J., Fortney, J. J., Southworth, J., Tan, T. G., Burgdorf, M., Novati, S. Calchi, Dominik, M., Fang, X. -S., Finet, F., Gerner, T., Hardis, S., Hinse, T. C., Jorgensen, U. G., Liebig, C., Nikolov, N., Ricci, D., Schaefer, S., Schoenebeck, F., Skottfelt, J., Wertz, O., Alsubai, K. A., Bozza, V., Browne, P., Dodds, P., Gu, S. -H., Harpsoe, K., Henning, Th., Hundertmark, M., Jessen-Hansen, J., Kains, N., Kerins, E., Kjeldsen, H., Lund, M. N., Lundkvist, M., Madhusudhan, N., Mathiasen, M., Penny, M. T., Proft, S., Rahvar, S., Sahu, K., Scarpetta, G., Snodgrass, C., and Surdej, J.
- Abstract
We present new ground-based, multi-colour, broad-band photometric measurements of the physical parameters, transmission and emission spectra of the transiting extrasolar planet WASP-19b. The measurements are based on observations of 8 transits and four occultations using the 1.5m Danish Telescope, 14 transits at the PEST observatory, and 1 transit observed simultaneously through four optical and three near-infrared filters, using the GROND instrument on the ESO 2.2m telescope. We use these new data to measure refined physical parameters for the system. We find the planet to be more bloated and the system to be twice as old as initially thought. We also used published and archived datasets to study the transit timings, which do not depart from a linear ephemeris. We detected an anomaly in the GROND transit light curve which is compatible with a spot on the photosphere of the parent star. The starspot position, size, spot contrast and temperature were established. Using our new and published measurements, we assembled the planet's transmission spectrum over the 370-2350 nm wavelength range and its emission spectrum over the 750-8000 nm range. By comparing these data to theoretical models we investigated the theoretically-predicted variation of the apparent radius of WASP-19b as a function of wavelength and studied the composition and thermal structure of its atmosphere. We conclude that: there is no evidence for strong optical absorbers at low pressure, supporting the common idea that the planet's atmosphere lacks a dayside inversion; the temperature of the planet is not homogenized, because the high warming of its dayside causes the planet to be more efficient in re-radiating than redistributing energy to the night side; the planet seems to be outside of any current classification scheme., Comment: 18 pages, 12 figures, 11 tables
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24. High-precision photometry by telescope defocussing. V. WASP-15 and WASP-16
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Southworth, J., Mancini, L., Browne, P., Burgdorf, M., Novati, S. Calchi, Dominik, M., Gerner, T., Hinse, T. C., Jorgensen, U. G., Kains, N., Ricci, D., Schafer, S., Schonebeck, F., Tregloan-Reed, J., Alsubai, K. A., Bozza, V., Chen, G., Dodds, P., Dreizler, S., Fang, X. -S., Finet, F., Gu, S. -H., Hardis, S., Harpsoe, K., Henning, Th., Hundertmark, M., Jessen-Hansen, J., Kerins, E., Kjeldsen, H., Liebig, C., Lund, M. N., Lundkvist, M., Mathiasen, M., Nikolov, N., Penny, M. T., Proft, S., Rahvar, S., Sahu, K., Scarpetta, G., Skottfelt, J., Snodgrass, C., Surdej, J., Wertz, O., Southworth, J., Mancini, L., Browne, P., Burgdorf, M., Novati, S. Calchi, Dominik, M., Gerner, T., Hinse, T. C., Jorgensen, U. G., Kains, N., Ricci, D., Schafer, S., Schonebeck, F., Tregloan-Reed, J., Alsubai, K. A., Bozza, V., Chen, G., Dodds, P., Dreizler, S., Fang, X. -S., Finet, F., Gu, S. -H., Hardis, S., Harpsoe, K., Henning, Th., Hundertmark, M., Jessen-Hansen, J., Kerins, E., Kjeldsen, H., Liebig, C., Lund, M. N., Lundkvist, M., Mathiasen, M., Nikolov, N., Penny, M. T., Proft, S., Rahvar, S., Sahu, K., Scarpetta, G., Skottfelt, J., Snodgrass, C., Surdej, J., and Wertz, O.
- Abstract
We present new photometric observations of WASP-15 and WASP-16, two transiting extrasolar planetary systems with measured orbital obliquities but without photometric follow-up since their discovery papers. Our new data for WASP-15 comprise observations of one transit simultaneously in four optical passbands using GROND on the MPG/ESO 2.2m telescope, plus coverage of half a transit from DFOSC on the Danish 1.54m telescope, both at ESO La Silla. For WASP-16 we present observations of four complete transits, all from the Danish telescope. We use these new data to refine the measured physical properties and orbital ephemerides of the two systems. Whilst our results are close to the originally-determined values for WASP-15, we find that the star and planet in the WASP-16 system are both larger and less massive than previously thought., Comment: Accepted for publication in MNRAS; 9 pages, 7 tables, 6 figures. The light curves are available from http://www.astro.keele.ac.uk/jkt/data-teps.html and the results are included in TEPCat at http://www.astro.keele.ac.uk/jkt/tepcat
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25. A detailed census of variable stars in the globular cluster NGC 6333 (M9) from CCD differential photometry
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Ferro, A. Arellano, Bramich, D. M., Jaimes, R. Figuera, Giridhar, Sunetra, Kains, N., Kuppuswamy, K., Jørgensen, U. G., Alsubai, K. A., Andersen, J. M., Bozza, V., Browne, P., Novati, S. Calchi, Damerdji, Y., Diehl, C., Dominik, M., Dreizler, S., Elyiv, A., Giannini, E., Harpsøe, K., Hessman, F. V., Hinse, T. C., Hundertmark, M., Juncher, D., Kerins, E., Korhonen, H., Liebig, C., Mancini, L., Mathiasen, M., Penny, M. T., Rabus, M., Rahvar, S., Ricci, D., Scarpetta, G., Skottfelt, J., Snodgrass, C., Southworth, J., Surdej, J., Tregloan-Reed, J., Vilela, C., Wertz, O., Ferro, A. Arellano, Bramich, D. M., Jaimes, R. Figuera, Giridhar, Sunetra, Kains, N., Kuppuswamy, K., Jørgensen, U. G., Alsubai, K. A., Andersen, J. M., Bozza, V., Browne, P., Novati, S. Calchi, Damerdji, Y., Diehl, C., Dominik, M., Dreizler, S., Elyiv, A., Giannini, E., Harpsøe, K., Hessman, F. V., Hinse, T. C., Hundertmark, M., Juncher, D., Kerins, E., Korhonen, H., Liebig, C., Mancini, L., Mathiasen, M., Penny, M. T., Rabus, M., Rahvar, S., Ricci, D., Scarpetta, G., Skottfelt, J., Snodgrass, C., Southworth, J., Surdej, J., Tregloan-Reed, J., Vilela, C., and Wertz, O.
- Abstract
We report CCD $V$ and $I$ time-series photometry of the globular cluster NGC 6333 (M9). The technique of difference image analysis has been used, which enables photometric precision better than 0.05 mag for stars brighter than $V \sim 19.0$ mag, even in the crowded central regions of the cluster. The high photometric precision has resulted in the discovery of two new RRc stars, three eclipsing binaries, seven long-term variables and one field RRab star behind the cluster. A detailed identification chart and equatorial coordinates are given for all the variable stars in the field of our images of the cluster. Our data together with literature $V$-data obtained in 1994 and 1995 allowed us to refine considerably the periods for all RR Lyrae stars. The nature of the new variables is discussed. We argue that variable V12 is a cluster member and an Anomalous Cepheid. Secular period variations, double mode pulsations and/or the Blazhko-like modulations in some RRc variables are addressed. Through the light curve Fourier decomposition of 12 RR Lyrae stars we have calculated a mean metallicity of [Fe/H]$_{\rm ZW}$=$-1.70 \pm 0.01{\rm(statistical)} \pm 0.14{\rm(systematic)}$ or [Fe/H]$_{UVES}=-1.67 \pm 0.01{\rm(statistical)} \pm 0.19{\rm(systematic)}$.Absolute magnitudes, radii and masses are also estimated for the RR Lyrae stars. A detailed search for SX Phe stars in the Blue Straggler region was conducted but none were discovered. If SX Phe exist in the cluster then their amplitudes must be smaller than the detection limit of our photometry. The CMD has been corrected for heavy differential reddening using the detailed extinction map of the cluster of Alonso-Garc\'ia et al. (2012). This has allowed us to set the mean cluster distance from two independent estimates; from the RRab and RRc absolute magnitudes, we find $8.04\pm 0.19$ kpc and $7.88\pm0.30$ kpc respectively., Comment: 20 pages, 17 figures, 5 tables, 1 electronic table
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26. Estimating the parameters of globular cluster M 30 (NGC 7099) from time-series photometry
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Kains, N., Bramich, D. M., Ferro, A. Arellano, Jaimes, R. Figuera, Jørgensen, U. G., Giridhar, S., Alsubai, K. A., Andersen, J. M., Bozza, V., Browne, P., Burgdorf, M., Novati, S. Calchi, Damerdji, Y., Diehl, C., Dodds, P., Dominik, M., Elyiv, A., Fang, X. -S., Giannini, E., Gu, S. -H., Hardis, S., Harpsøe, K., Hinse, T. C., Hornstrup, A., Hundertmark, M., Jessen-Hansen, J., Juncher, D., Kerins, E., Kjeldsen, H., Korhonen, H., Liebig, C., Lund, M. N., Lundkvist, M., Mancini, L., Martin, R., Mathiasen, M., Penny, M. T., Rabus, M., Rahvar, S., Ricci, D., Sahu, K., Scarpetta, G., Skottfelt, J., Snodgrass, C., Southworth, J., Surdej, J., Tregloan-Reed, J., Vilela, C., Wertz, O., Williams, A., Kains, N., Bramich, D. M., Ferro, A. Arellano, Jaimes, R. Figuera, Jørgensen, U. G., Giridhar, S., Alsubai, K. A., Andersen, J. M., Bozza, V., Browne, P., Burgdorf, M., Novati, S. Calchi, Damerdji, Y., Diehl, C., Dodds, P., Dominik, M., Elyiv, A., Fang, X. -S., Giannini, E., Gu, S. -H., Hardis, S., Harpsøe, K., Hinse, T. C., Hornstrup, A., Hundertmark, M., Jessen-Hansen, J., Juncher, D., Kerins, E., Kjeldsen, H., Korhonen, H., Liebig, C., Lund, M. N., Lundkvist, M., Mancini, L., Martin, R., Mathiasen, M., Penny, M. T., Rabus, M., Rahvar, S., Ricci, D., Sahu, K., Scarpetta, G., Skottfelt, J., Snodgrass, C., Southworth, J., Surdej, J., Tregloan-Reed, J., Vilela, C., Wertz, O., and Williams, A.
- Abstract
We present the analysis of 26 nights of V and I time-series observations from 2011 and 2012 of the globular cluster M 30 (NGC 7099). We used our data to search for variable stars in this cluster and refine the periods of known variables; we then used our variable star light curves to derive values for the cluster's parameters. We used difference image analysis to reduce our data to obtain high-precision light curves of variable stars. We then estimated the cluster parameters by performing a Fourier decomposition of the light curves of RR Lyrae stars for which a good period estimate was possible. We also derive an estimate for the age of the cluster by fitting theoretical isochrones to our colour-magnitude diagram (CMD). Out of 13 stars previously catalogued as variables, we find that only 4 are bona fide variables. We detect two new RR Lyrae variables, and confirm two additional RR Lyrae candidates from the literature. We also detect four other new variables, including an eclipsing blue straggler system, and an SX Phoenicis star. This amounts to a total number of confirmed variable stars in M 30 of 12. We perform Fourier decomposition of the light curves of the RR Lyrae stars to derive cluster parameters using empirical relations. We find a cluster metallicity [Fe/H]_ZW=-2.01 +- 0.04, or [Fe/H]_UVES=-2.11 +- 0.06, and a distance of 8.32 +- 0.20 kpc (using RR0 variables), 8.10 kpc (using one RR1 variable), and 8.35 +- 0.42 kpc (using our SX Phoenicis star detection in M 30). Fitting isochrones to the CMD, we estimate an age of 13.0 +- 1.0 Gyr for M 30., Comment: 16 pages, 10 figures, 10 tables, A&A in press
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27. A Giant Planet beyond the Snow Line in Microlensing Event OGLE-2011-BLG-0251
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Kains, N., Street, R., Choi, J. -Y., Han, C., Udalski, A., Almeida, L. A., Jablonski, F., Tristram, P., Jorgensen, U. G., Szymanski, M. K., Kubiak, M., Pietrzynski, G., Soszynski, I., Poleski, R., Kozlowski, S., Pietrukowicz, P., Ulaczyk, K., Wyrzykowski, L., Skowron, J., Alsubai, K. A., Bozza, V., Browne, P., Burgdorf, M. J., Novati, S. Calchi, Dodds, P., Dominik, M., Dreizler, S., Fang, X. -S., Grundahl, F., Gu, C. -H., Hardis, S., Harpsoe, K., Hessman, F. V., Hinse, T. C., Hornstrup, A., Hundertmark, M., Jessen-Hansen, J., 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., Tsapras, Y., 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., Munoz, 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., Prester, D. Dominis, Donatowicz, J., Fouque, 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., Kains, N., Street, R., Choi, J. -Y., Han, C., Udalski, A., Almeida, L. A., Jablonski, F., Tristram, P., Jorgensen, U. G., Szymanski, M. K., Kubiak, M., Pietrzynski, G., Soszynski, I., Poleski, R., Kozlowski, S., Pietrukowicz, P., Ulaczyk, K., Wyrzykowski, L., Skowron, J., Alsubai, K. A., Bozza, V., Browne, P., Burgdorf, M. J., Novati, S. Calchi, Dodds, P., Dominik, M., Dreizler, S., Fang, X. -S., Grundahl, F., Gu, C. -H., Hardis, S., Harpsoe, K., Hessman, F. V., Hinse, T. C., Hornstrup, A., Hundertmark, M., Jessen-Hansen, J., 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., Tsapras, Y., 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., Munoz, 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., Prester, D. Dominis, Donatowicz, J., Fouque, P., Greenhill, J., Kane, S. R., Kubas, D., Marquette, J. -B., Martin, R., Meintjes, P., Menzies, J., Pollard, K. R., Williams, A., Wouters, D., and Zub, M.
- 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., Comment: 12 pages, 7 figures, 3 tables; A&A in press
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- 2013
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28. Microlensing Discovery of a Population of Very Tight, Very Low-mass Binary Brown Dwarfs
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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., Szymański, M. K., Kubiak, M., Pietrzyński, G., Soszyński, I., Skowron, J., Kozłowski, S., Poleski, R., Ulaczyk, K., Wyrzykowski, Ł., Pietrukowicz, P., 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., Munoz, J. A., Park, B. -G., Park, H., Pogge, R. W., Shvartzvald, Y., Shin, I. -G., Yee, J. C., Alsubai, K. A., Browne, P., Burgdorf, M. J., Novati, S. Calchi, 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., Jørgensen, 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., Albrow, M. D., Bachelet, E., Batista, V., Brillant, S., Cassan, A., Cole, A. A., Coutures, C., Dieters, S., Prester, D. Dominis, Donatowicz, J., Fouqué, P., Greenhill, J., Kubas, D., Marquette, J. -B., Menzies, J. W., Sahu, K. C., Zub, M., Bramich, D. M., Horne, K., Steele, I. A., Street, R. A., 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., Szymański, M. K., Kubiak, M., Pietrzyński, G., Soszyński, I., Skowron, J., Kozłowski, S., Poleski, R., Ulaczyk, K., Wyrzykowski, Ł., Pietrukowicz, P., 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., Munoz, J. A., Park, B. -G., Park, H., Pogge, R. W., Shvartzvald, Y., Shin, I. -G., Yee, J. C., Alsubai, K. A., Browne, P., Burgdorf, M. J., Novati, S. Calchi, 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., Jørgensen, 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., Albrow, M. D., Bachelet, E., Batista, V., Brillant, S., Cassan, A., Cole, A. A., Coutures, C., Dieters, S., Prester, D. Dominis, Donatowicz, J., Fouqué, P., Greenhill, J., Kubas, D., Marquette, J. -B., Menzies, J. W., Sahu, K. C., Zub, M., Bramich, D. M., Horne, K., Steele, I. A., and Street, R. A.
- 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., Comment: 7 pages, 5 figures, 3 tables, ApJ submitted
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- 2013
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29. Flux and color variations of the doubly imaged quasar UM673
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Ricci, D., Elyiv, A., Finet, F., Wertz, O., Alsubai, K., Anguita, T., Bozza, V., Browne, P., Burgdorf, M., Novati, S. Calchi, Dodds, P., Dominik, M., Dreizler, S., Gerner, T., Glitrup, M., Grundahl, F., Hardis, S., Harpsøe, K., Hinse, T. C., Hornstrup, A., Hundertmark, M., Jørgensen, U. G., Kains, N., Kerins, E., Liebig, C., Maier, G., Mancini, L., Masi, G., Mathiasen, M., Penny, M., Proft, S., Rahvar, S., Scarpetta, G., Sahu, K., Schäfer, S., Schönebeck, F., Schmidt, R., Skottfelt, J., Snodgrass, C., Southworth, J., Thöne, C. C., Wambsganss, J., Zimmer, F., Zub, M., Surdej, J., Ricci, D., Elyiv, A., Finet, F., Wertz, O., Alsubai, K., Anguita, T., Bozza, V., Browne, P., Burgdorf, M., Novati, S. Calchi, Dodds, P., Dominik, M., Dreizler, S., Gerner, T., Glitrup, M., Grundahl, F., Hardis, S., Harpsøe, K., Hinse, T. C., Hornstrup, A., Hundertmark, M., Jørgensen, U. G., Kains, N., Kerins, E., Liebig, C., Maier, G., Mancini, L., Masi, G., Mathiasen, M., Penny, M., Proft, S., Rahvar, S., Scarpetta, G., Sahu, K., Schäfer, S., Schönebeck, F., Schmidt, R., Skottfelt, J., Snodgrass, C., Southworth, J., Thöne, C. C., Wambsganss, J., Zimmer, F., Zub, M., and Surdej, J.
- Abstract
With the aim of characterizing the flux and color variations of the multiple components of the gravitationally lensed quasar UM673 as a function of time, we have performed multi-epoch and multi-band photometric observations with the Danish 1.54m telescope at the La Silla Observatory. The observations were carried out in the VRi spectral bands during four seasons (2008--2011). We reduced the data using the PSF (Point Spread Function) photometric technique as well as aperture photometry. Our results show for the brightest lensed component some significant decrease in flux between the first two seasons (+0.09/+0.11/+0.05 mag) and a subsequent increase during the following ones (-0.11/-0.11/-0.10 mag) in the V/R/i spectral bands, respectively. Comparing our results with previous studies, we find smaller color variations between these seasons as compared with previous ones. We also separate the contribution of the lensing galaxy from that of the fainter and close lensed component., Comment: 7 pages, 8 figures, 4 tables
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- 2013
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30. A giant planet beyond the snow line in microlensing event OGLE-2011-BLG-0251
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Kains, N., Street, R., Choi, J., Han, C., Udalski, A., Almeida, L., Jablonski, F., Tristram, P., Jorgensen, U., Szymanski, M., Kubiak, M., Pietrzynski, G., Soszynski, I., Poleski, R., Kozlowski, S., Pietrukowicz, P., Ulaczyk, K., Wyrzykowski, L., Skowron, J., Alsubai, K., Bozza, V., Browne, P., Burgdorf, M., Calchi Novati, S., Dodds, P., Dominik, M., Dreizler, S., Fang, X., Grundahl, F., Gu, C., Hardis, S., Harpsoe, K., Hessman, F., Hinse, T., Hornstrup, A., Hundertmark, M., Jessen-Hansen, J., Kerins, E., Liebig, C., Lund, M., Lundkvist, M., Mancini, L., Mathiasen, M., Penny, M., Rahvar, S., Ricci, D., Sahu, K., Scarpetta, G., Skottfelt, J., Snodgrass, C., Southworth, J., Surdej, J., Tregloan-Reed, J., Wambsganss, J., Wertz, O., Bajek, D., Bramich, D., Horne, K., Ipatov, S., Steele, I., Tsapras, Y., Abe, F., Bennett, D., Bond, I., Botzler, C., Chote, P., Freeman, M., Fukui, A., Furusawa, K., Itow, Y., Ling, C., Masuda, K., Matsubara, Y., Miyake, N., Muraki, Y., Ohnishi, K., Rattenbury, N., Saito, T., Sullivan, D., Sumi, T., Suzuki, D., Suzuki, K., Sweatman, W., Takino, S., Wada, K., Yock, P., Allen, W., Batista, V., Chung, S., Christie, G., DePoy, D., Drummond, J., Gaudi, B., Gould, A., Henderson, C., Jung, Y., Koo, J., Lee, C., McCormick, J., McGregor, D., Munoz, J., Natusch, T., Ngan, H., Park, H., Pogge, R., Shin, I., Yee, J., Albrow, M., Bachelet, E., Beaulieu, J., Brillant, S., Caldwell, J., Cassan, A., Cole, A., Corrales, E., Coutures, C., Dieters, S., Dominis Prester, D., Donatowicz, J., Fouque, P., Greenhill, J., Kane, S., Kubas, D., Marquette, J., Martin, R., Meintjes, P., Menzies, J., Pollard, K., Williams, Andrew, Wouters, D., Zub, M., Kains, N., Street, R., Choi, J., Han, C., Udalski, A., Almeida, L., Jablonski, F., Tristram, P., Jorgensen, U., Szymanski, M., Kubiak, M., Pietrzynski, G., Soszynski, I., Poleski, R., Kozlowski, S., Pietrukowicz, P., Ulaczyk, K., Wyrzykowski, L., Skowron, J., Alsubai, K., Bozza, V., Browne, P., Burgdorf, M., Calchi Novati, S., Dodds, P., Dominik, M., Dreizler, S., Fang, X., Grundahl, F., Gu, C., Hardis, S., Harpsoe, K., Hessman, F., Hinse, T., Hornstrup, A., Hundertmark, M., Jessen-Hansen, J., Kerins, E., Liebig, C., Lund, M., Lundkvist, M., Mancini, L., Mathiasen, M., Penny, M., Rahvar, S., Ricci, D., Sahu, K., Scarpetta, G., Skottfelt, J., Snodgrass, C., Southworth, J., Surdej, J., Tregloan-Reed, J., Wambsganss, J., Wertz, O., Bajek, D., Bramich, D., Horne, K., Ipatov, S., Steele, I., Tsapras, Y., Abe, F., Bennett, D., Bond, I., Botzler, C., Chote, P., Freeman, M., Fukui, A., Furusawa, K., Itow, Y., Ling, C., Masuda, K., Matsubara, Y., Miyake, N., Muraki, Y., Ohnishi, K., Rattenbury, N., Saito, T., Sullivan, D., Sumi, T., Suzuki, D., Suzuki, K., Sweatman, W., Takino, S., Wada, K., Yock, P., Allen, W., Batista, V., Chung, S., Christie, G., DePoy, D., Drummond, J., Gaudi, B., Gould, A., Henderson, C., Jung, Y., Koo, J., Lee, C., McCormick, J., McGregor, D., Munoz, J., Natusch, T., Ngan, H., Park, H., Pogge, R., Shin, I., Yee, J., Albrow, M., Bachelet, E., Beaulieu, J., Brillant, S., Caldwell, J., Cassan, A., Cole, A., Corrales, E., Coutures, C., Dieters, S., Dominis Prester, D., Donatowicz, J., Fouque, P., Greenhill, J., Kane, S., Kubas, D., Marquette, J., Martin, R., Meintjes, P., Menzies, J., Pollard, K., Williams, Andrew, Wouters, D., and Zub, M.
- Abstract
Aims. 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.Methods. Based on detailed modelling of the observed light curve, we find that the lens is composed of twomasses with a mass ratio q = 1.9 × 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.Results. We find that the lens is made up of a planet of mass 0.53 ± 0.21 MJ orbiting an M dwarf host star with a mass of 0.26 ± 0.11 M. 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.
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- 2013
31. A Giant Planet beyond the Snow Line in Microlensing Event OGLE-2011-BLG-0251
- Author
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Kains, N., Street, R., Choi, J. -Y., Han, C., Udalski, A., Almeida, L. A., Jablonski, F., Tristram, P., Jorgensen, U. G., Szymanski, M. K., Kubiak, M., Pietrzynski, G., Soszynski, I., Poleski, R., Kozlowski, S., Pietrukowicz, P., Ulaczyk, K., Wyrzykowski, L., Skowron, J., Alsubai, K. A., Bozza, V., Browne, P., Burgdorf, M. J., Novati, S. Calchi, Dodds, P., Dominik, M., Dreizler, S., Fang, X. -S., Grundahl, F., Gu, C. -H., Hardis, S., Harpsoe, K., Hessman, F. V., Hinse, T. C., Hornstrup, A., Hundertmark, M., Jessen-Hansen, J., 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., Tsapras, Y., 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., Munoz, 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., Prester, D. Dominis, Donatowicz, J., Fouque, 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., Kains, N., Street, R., Choi, J. -Y., Han, C., Udalski, A., Almeida, L. A., Jablonski, F., Tristram, P., Jorgensen, U. G., Szymanski, M. K., Kubiak, M., Pietrzynski, G., Soszynski, I., Poleski, R., Kozlowski, S., Pietrukowicz, P., Ulaczyk, K., Wyrzykowski, L., Skowron, J., Alsubai, K. A., Bozza, V., Browne, P., Burgdorf, M. J., Novati, S. Calchi, Dodds, P., Dominik, M., Dreizler, S., Fang, X. -S., Grundahl, F., Gu, C. -H., Hardis, S., Harpsoe, K., Hessman, F. V., Hinse, T. C., Hornstrup, A., Hundertmark, M., Jessen-Hansen, J., 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., Tsapras, Y., 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., Munoz, 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., Prester, D. Dominis, Donatowicz, J., Fouque, P., Greenhill, J., Kane, S. R., Kubas, D., Marquette, J. -B., Martin, R., Meintjes, P., Menzies, J., Pollard, K. R., Williams, A., Wouters, D., and Zub, M.
- 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., Comment: 12 pages, 7 figures, 3 tables; A&A in press
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- 2013
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32. A giant planet beyond the snow line in microlensing event OGLE-2011-BLG-0251
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Kains, N., Street, R., Choi, J., Han, C., Udalski, A., Almeida, L., Jablonski, F., Tristram, P., Jorgensen, U., Szymanski, M., Kubiak, M., Pietrzynski, G., Soszynski, I., Poleski, R., Kozlowski, S., Pietrukowicz, P., Ulaczyk, K., Wyrzykowski, L., Skowron, J., Alsubai, K., Bozza, V., Browne, P., Burgdorf, M., Calchi Novati, S., Dodds, P., Dominik, M., Dreizler, S., Fang, X., Grundahl, F., Gu, C., Hardis, S., Harpsoe, K., Hessman, F., Hinse, T., Hornstrup, A., Hundertmark, M., Jessen-Hansen, J., Kerins, E., Liebig, C., Lund, M., Lundkvist, M., Mancini, L., Mathiasen, M., Penny, M., Rahvar, S., Ricci, D., Sahu, K., Scarpetta, G., Skottfelt, J., Snodgrass, C., Southworth, J., Surdej, J., Tregloan-Reed, J., Wambsganss, J., Wertz, O., Bajek, D., Bramich, D., Horne, K., Ipatov, S., Steele, I., Tsapras, Y., Abe, F., Bennett, D., Bond, I., Botzler, C., Chote, P., Freeman, M., Fukui, A., Furusawa, K., Itow, Y., Ling, C., Masuda, K., Matsubara, Y., Miyake, N., Muraki, Y., Ohnishi, K., Rattenbury, N., Saito, T., Sullivan, D., Sumi, T., Suzuki, D., Suzuki, K., Sweatman, W., Takino, S., Wada, K., Yock, P., Allen, W., Batista, V., Chung, S., Christie, G., DePoy, D., Drummond, J., Gaudi, B., Gould, A., Henderson, C., Jung, Y., Koo, J., Lee, C., McCormick, J., McGregor, D., Munoz, J., Natusch, T., Ngan, H., Park, H., Pogge, R., Shin, I., Yee, J., Albrow, M., Bachelet, E., Beaulieu, J., Brillant, S., Caldwell, J., Cassan, A., Cole, A., Corrales, E., Coutures, C., Dieters, S., Dominis Prester, D., Donatowicz, J., Fouque, P., Greenhill, J., Kane, S., Kubas, D., Marquette, J., Martin, R., Meintjes, P., Menzies, J., Pollard, K., Williams, Andrew, Wouters, D., Zub, M., Kains, N., Street, R., Choi, J., Han, C., Udalski, A., Almeida, L., Jablonski, F., Tristram, P., Jorgensen, U., Szymanski, M., Kubiak, M., Pietrzynski, G., Soszynski, I., Poleski, R., Kozlowski, S., Pietrukowicz, P., Ulaczyk, K., Wyrzykowski, L., Skowron, J., Alsubai, K., Bozza, V., Browne, P., Burgdorf, M., Calchi Novati, S., Dodds, P., Dominik, M., Dreizler, S., Fang, X., Grundahl, F., Gu, C., Hardis, S., Harpsoe, K., Hessman, F., Hinse, T., Hornstrup, A., Hundertmark, M., Jessen-Hansen, J., Kerins, E., Liebig, C., Lund, M., Lundkvist, M., Mancini, L., Mathiasen, M., Penny, M., Rahvar, S., Ricci, D., Sahu, K., Scarpetta, G., Skottfelt, J., Snodgrass, C., Southworth, J., Surdej, J., Tregloan-Reed, J., Wambsganss, J., Wertz, O., Bajek, D., Bramich, D., Horne, K., Ipatov, S., Steele, I., Tsapras, Y., Abe, F., Bennett, D., Bond, I., Botzler, C., Chote, P., Freeman, M., Fukui, A., Furusawa, K., Itow, Y., Ling, C., Masuda, K., Matsubara, Y., Miyake, N., Muraki, Y., Ohnishi, K., Rattenbury, N., Saito, T., Sullivan, D., Sumi, T., Suzuki, D., Suzuki, K., Sweatman, W., Takino, S., Wada, K., Yock, P., Allen, W., Batista, V., Chung, S., Christie, G., DePoy, D., Drummond, J., Gaudi, B., Gould, A., Henderson, C., Jung, Y., Koo, J., Lee, C., McCormick, J., McGregor, D., Munoz, J., Natusch, T., Ngan, H., Park, H., Pogge, R., Shin, I., Yee, J., Albrow, M., Bachelet, E., Beaulieu, J., Brillant, S., Caldwell, J., Cassan, A., Cole, A., Corrales, E., Coutures, C., Dieters, S., Dominis Prester, D., Donatowicz, J., Fouque, P., Greenhill, J., Kane, S., Kubas, D., Marquette, J., Martin, R., Meintjes, P., Menzies, J., Pollard, K., Williams, Andrew, Wouters, D., and Zub, M.
- Abstract
Aims. 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.Methods. Based on detailed modelling of the observed light curve, we find that the lens is composed of twomasses with a mass ratio q = 1.9 × 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.Results. We find that the lens is made up of a planet of mass 0.53 ± 0.21 MJ orbiting an M dwarf host star with a mass of 0.26 ± 0.11 M. 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.
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- 2013
33. A Super-Jupiter orbiting a late-type star: A refined analysis of microlensing event OGLE-2012-BLG-0406
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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. Calchi, 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, Łukasz, 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., Fouqué, P., Greenhill, J., Kane, S. R., Kubas, D., Marquette, J. -B., Menzies, J., P`ere, C., Pollard, K. R., Wouters, D., 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, To., Sullivan, D. J., Sweatman, W. L., Suzuki, D., Tristram, P. J., Tsurumi, N., Wada, K., Yamai, N., Yonehara, P. C. M. Yock A., 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. Calchi, 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, Łukasz, 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., Fouqué, P., Greenhill, J., Kane, S. R., Kubas, D., Marquette, J. -B., Menzies, J., P`ere, C., Pollard, K. R., Wouters, D., 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, To., Sullivan, D. J., Sweatman, W. L., Suzuki, D., Tristram, P. J., Tsurumi, N., Wada, K., Yamai, N., and Yonehara, P. C. M. Yock A.
- 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., Comment: 9 pages, 4 figures, accepted by ApJ
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- 2013
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34. MOA-2010-BLG-328Lb: a sub-Neptune orbiting very late M dwarf ?
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Furusawa, K., Udalski, A., Sumi, T., Bennett, D. P., Bond, I. A., Gould, A., Jorgensen, U. G., Snodgrass, C., Prester, D. Dominis, Albrow, M. D., Abe, F., Botzler, C. S., Chote, P., Freeman, M., Fukui, A., Harris, P., Itow, Y., Ling, C. H., Masuda, K., Matsubara, Y., Miyake, N., Muraki, Y., Ohnishi, K., Rattenbury, N. J., Saito, To., Sullivan, D. J., Suzuki, D., Sweatman, W. L., Tristram, P. J., Wada, K., Yock, P. C. M., Szymanski, M. K., Soszynski, I., Kubiak, M., Poleski, R., Ulaczyk, K., Pietrzynski, G., Wyrzykowski, L., Choi, J. Y., Christie, G. W., DePoy, D. L., Dong, S., Drummond, J., Gaudi, B. S., Han, C., Hung, L. -W., Jung, Y. -K., Lee, C. -U., McCormick, J., Moorhouse, D., Natusch, T., Nola, M., Ofek, E., Park, B. G., Park, H., Pogge, R. W., Shin, I. -G., Skowron, J., Thornley, G., Yee, J. C., Alsubai, K. A., Bozza, V., Browne, P., Burgdorf, M. J., Novati, S. Calchi, Dodds, P., Dominik, M., Finet, F., Gerner, T., Hardis, S., Harpsoe, K., Hinse, T. C., Hundertmark, M., Kains, N., Kerins, E., Liebig, C., Mancini, L., Mathiasen, M., Penny, M. T., Proft, S., Rahvar, S., Ricci, D., Scarpetta, G., Schafer, S., Schonebeck, F., Southworth, J., Surdej, J., Wambsganss, J., Street, R. A., Bramich, D. M., Steele, I. A., Tsapras, Y., Horne, K., Donatowicz, J., Sahu, K. C., Bachelet, E., Batista, V., Beatty, T. G., Beaulieu, J. -P., Bennett, C. S., Black, C., Bowens-Rubin, R., Brillant, S., Caldwell, J. A. R., Cassan, A., Cole, A. A., Corrales, E., Coutures, C., Dieters, S., Fouque, P., Greenhill, J., Henderson, C. B., Kubas, D., Marquette, J. -B., Martin, R., Menzies, J. W., Shappee, B., Williams, A., Wouters, D., van Saders, J., Zellem, R., Zub, M., Furusawa, K., Udalski, A., Sumi, T., Bennett, D. P., Bond, I. A., Gould, A., Jorgensen, U. G., Snodgrass, C., Prester, D. Dominis, Albrow, M. D., Abe, F., Botzler, C. S., Chote, P., Freeman, M., Fukui, A., Harris, P., Itow, Y., Ling, C. H., Masuda, K., Matsubara, Y., Miyake, N., Muraki, Y., Ohnishi, K., Rattenbury, N. J., Saito, To., Sullivan, D. J., Suzuki, D., Sweatman, W. L., Tristram, P. J., Wada, K., Yock, P. C. M., Szymanski, M. K., Soszynski, I., Kubiak, M., Poleski, R., Ulaczyk, K., Pietrzynski, G., Wyrzykowski, L., Choi, J. Y., Christie, G. W., DePoy, D. L., Dong, S., Drummond, J., Gaudi, B. S., Han, C., Hung, L. -W., Jung, Y. -K., Lee, C. -U., McCormick, J., Moorhouse, D., Natusch, T., Nola, M., Ofek, E., Park, B. G., Park, H., Pogge, R. W., Shin, I. -G., Skowron, J., Thornley, G., Yee, J. C., Alsubai, K. A., Bozza, V., Browne, P., Burgdorf, M. J., Novati, S. Calchi, Dodds, P., Dominik, M., Finet, F., Gerner, T., Hardis, S., Harpsoe, K., Hinse, T. C., Hundertmark, M., Kains, N., Kerins, E., Liebig, C., Mancini, L., Mathiasen, M., Penny, M. T., Proft, S., Rahvar, S., Ricci, D., Scarpetta, G., Schafer, S., Schonebeck, F., Southworth, J., Surdej, J., Wambsganss, J., Street, R. A., Bramich, D. M., Steele, I. A., Tsapras, Y., Horne, K., Donatowicz, J., Sahu, K. C., Bachelet, E., Batista, V., Beatty, T. G., Beaulieu, J. -P., Bennett, C. S., Black, C., Bowens-Rubin, R., Brillant, S., Caldwell, J. A. R., Cassan, A., Cole, A. A., Corrales, E., Coutures, C., Dieters, S., Fouque, P., Greenhill, J., Henderson, C. B., Kubas, D., Marquette, J. -B., Martin, R., Menzies, J. W., Shappee, B., Williams, A., Wouters, D., van Saders, J., Zellem, R., and Zub, M.
- Abstract
We analyze the planetary microlensing event MOA-2010-BLG-328. The best fit yields host and planetary masses of Mh = 0.11+/-0.01 M_{sun} and Mp = 9.2+/-2.2M_Earth, corresponding to a very late M dwarf and sub-Neptune-mass planet, respectively. The system lies at DL = 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., Comment: 30 pages, 6 figures. accepted for publication in ApJ. Figure 1 and 2 are updated
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- 2013
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35. Physical properties, transmission and emission spectra of the WASP-19 planetary system from multi-colour photometry
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Mancini, L., Ciceri, S., Chen, G., Tregloan-Reed, J., Fortney, J. J., Southworth, J., Tan, T. G., Burgdorf, M., Novati, S. Calchi, Dominik, M., Fang, X. -S., Finet, F., Gerner, T., Hardis, S., Hinse, T. C., Jorgensen, U. G., Liebig, C., Nikolov, N., Ricci, D., Schaefer, S., Schoenebeck, F., Skottfelt, J., Wertz, O., Alsubai, K. A., Bozza, V., Browne, P., Dodds, P., Gu, S. -H., Harpsoe, K., Henning, Th., Hundertmark, M., Jessen-Hansen, J., Kains, N., Kerins, E., Kjeldsen, H., Lund, M. N., Lundkvist, M., Madhusudhan, N., Mathiasen, M., Penny, M. T., Proft, S., Rahvar, S., Sahu, K., Scarpetta, G., Snodgrass, C., Surdej, J., Mancini, L., Ciceri, S., Chen, G., Tregloan-Reed, J., Fortney, J. J., Southworth, J., Tan, T. G., Burgdorf, M., Novati, S. Calchi, Dominik, M., Fang, X. -S., Finet, F., Gerner, T., Hardis, S., Hinse, T. C., Jorgensen, U. G., Liebig, C., Nikolov, N., Ricci, D., Schaefer, S., Schoenebeck, F., Skottfelt, J., Wertz, O., Alsubai, K. A., Bozza, V., Browne, P., Dodds, P., Gu, S. -H., Harpsoe, K., Henning, Th., Hundertmark, M., Jessen-Hansen, J., Kains, N., Kerins, E., Kjeldsen, H., Lund, M. N., Lundkvist, M., Madhusudhan, N., Mathiasen, M., Penny, M. T., Proft, S., Rahvar, S., Sahu, K., Scarpetta, G., Snodgrass, C., and Surdej, J.
- Abstract
We present new ground-based, multi-colour, broad-band photometric measurements of the physical parameters, transmission and emission spectra of the transiting extrasolar planet WASP-19b. The measurements are based on observations of 8 transits and four occultations using the 1.5m Danish Telescope, 14 transits at the PEST observatory, and 1 transit observed simultaneously through four optical and three near-infrared filters, using the GROND instrument on the ESO 2.2m telescope. We use these new data to measure refined physical parameters for the system. We find the planet to be more bloated and the system to be twice as old as initially thought. We also used published and archived datasets to study the transit timings, which do not depart from a linear ephemeris. We detected an anomaly in the GROND transit light curve which is compatible with a spot on the photosphere of the parent star. The starspot position, size, spot contrast and temperature were established. Using our new and published measurements, we assembled the planet's transmission spectrum over the 370-2350 nm wavelength range and its emission spectrum over the 750-8000 nm range. By comparing these data to theoretical models we investigated the theoretically-predicted variation of the apparent radius of WASP-19b as a function of wavelength and studied the composition and thermal structure of its atmosphere. We conclude that: there is no evidence for strong optical absorbers at low pressure, supporting the common idea that the planet's atmosphere lacks a dayside inversion; the temperature of the planet is not homogenized, because the high warming of its dayside causes the planet to be more efficient in re-radiating than redistributing energy to the night side; the planet seems to be outside of any current classification scheme., Comment: 18 pages, 12 figures, 11 tables
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36. High-precision photometry by telescope defocussing. V. WASP-15 and WASP-16
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Southworth, J., Mancini, L., Browne, P., Burgdorf, M., Novati, S. Calchi, Dominik, M., Gerner, T., Hinse, T. C., Jorgensen, U. G., Kains, N., Ricci, D., Schafer, S., Schonebeck, F., Tregloan-Reed, J., Alsubai, K. A., Bozza, V., Chen, G., Dodds, P., Dreizler, S., Fang, X. -S., Finet, F., Gu, S. -H., Hardis, S., Harpsoe, K., Henning, Th., Hundertmark, M., Jessen-Hansen, J., Kerins, E., Kjeldsen, H., Liebig, C., Lund, M. N., Lundkvist, M., Mathiasen, M., Nikolov, N., Penny, M. T., Proft, S., Rahvar, S., Sahu, K., Scarpetta, G., Skottfelt, J., Snodgrass, C., Surdej, J., Wertz, O., Southworth, J., Mancini, L., Browne, P., Burgdorf, M., Novati, S. Calchi, Dominik, M., Gerner, T., Hinse, T. C., Jorgensen, U. G., Kains, N., Ricci, D., Schafer, S., Schonebeck, F., Tregloan-Reed, J., Alsubai, K. A., Bozza, V., Chen, G., Dodds, P., Dreizler, S., Fang, X. -S., Finet, F., Gu, S. -H., Hardis, S., Harpsoe, K., Henning, Th., Hundertmark, M., Jessen-Hansen, J., Kerins, E., Kjeldsen, H., Liebig, C., Lund, M. N., Lundkvist, M., Mathiasen, M., Nikolov, N., Penny, M. T., Proft, S., Rahvar, S., Sahu, K., Scarpetta, G., Skottfelt, J., Snodgrass, C., Surdej, J., and Wertz, O.
- Abstract
We present new photometric observations of WASP-15 and WASP-16, two transiting extrasolar planetary systems with measured orbital obliquities but without photometric follow-up since their discovery papers. Our new data for WASP-15 comprise observations of one transit simultaneously in four optical passbands using GROND on the MPG/ESO 2.2m telescope, plus coverage of half a transit from DFOSC on the Danish 1.54m telescope, both at ESO La Silla. For WASP-16 we present observations of four complete transits, all from the Danish telescope. We use these new data to refine the measured physical properties and orbital ephemerides of the two systems. Whilst our results are close to the originally-determined values for WASP-15, we find that the star and planet in the WASP-16 system are both larger and less massive than previously thought., Comment: Accepted for publication in MNRAS; 9 pages, 7 tables, 6 figures. The light curves are available from http://www.astro.keele.ac.uk/jkt/data-teps.html and the results are included in TEPCat at http://www.astro.keele.ac.uk/jkt/tepcat
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37. A detailed census of variable stars in the globular cluster NGC 6333 (M9) from CCD differential photometry
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Ferro, A. Arellano, Bramich, D. M., Jaimes, R. Figuera, Giridhar, Sunetra, Kains, N., Kuppuswamy, K., Jørgensen, U. G., Alsubai, K. A., Andersen, J. M., Bozza, V., Browne, P., Novati, S. Calchi, Damerdji, Y., Diehl, C., Dominik, M., Dreizler, S., Elyiv, A., Giannini, E., Harpsøe, K., Hessman, F. V., Hinse, T. C., Hundertmark, M., Juncher, D., Kerins, E., Korhonen, H., Liebig, C., Mancini, L., Mathiasen, M., Penny, M. T., Rabus, M., Rahvar, S., Ricci, D., Scarpetta, G., Skottfelt, J., Snodgrass, C., Southworth, J., Surdej, J., Tregloan-Reed, J., Vilela, C., Wertz, O., Ferro, A. Arellano, Bramich, D. M., Jaimes, R. Figuera, Giridhar, Sunetra, Kains, N., Kuppuswamy, K., Jørgensen, U. G., Alsubai, K. A., Andersen, J. M., Bozza, V., Browne, P., Novati, S. Calchi, Damerdji, Y., Diehl, C., Dominik, M., Dreizler, S., Elyiv, A., Giannini, E., Harpsøe, K., Hessman, F. V., Hinse, T. C., Hundertmark, M., Juncher, D., Kerins, E., Korhonen, H., Liebig, C., Mancini, L., Mathiasen, M., Penny, M. T., Rabus, M., Rahvar, S., Ricci, D., Scarpetta, G., Skottfelt, J., Snodgrass, C., Southworth, J., Surdej, J., Tregloan-Reed, J., Vilela, C., and Wertz, O.
- Abstract
We report CCD $V$ and $I$ time-series photometry of the globular cluster NGC 6333 (M9). The technique of difference image analysis has been used, which enables photometric precision better than 0.05 mag for stars brighter than $V \sim 19.0$ mag, even in the crowded central regions of the cluster. The high photometric precision has resulted in the discovery of two new RRc stars, three eclipsing binaries, seven long-term variables and one field RRab star behind the cluster. A detailed identification chart and equatorial coordinates are given for all the variable stars in the field of our images of the cluster. Our data together with literature $V$-data obtained in 1994 and 1995 allowed us to refine considerably the periods for all RR Lyrae stars. The nature of the new variables is discussed. We argue that variable V12 is a cluster member and an Anomalous Cepheid. Secular period variations, double mode pulsations and/or the Blazhko-like modulations in some RRc variables are addressed. Through the light curve Fourier decomposition of 12 RR Lyrae stars we have calculated a mean metallicity of [Fe/H]$_{\rm ZW}$=$-1.70 \pm 0.01{\rm(statistical)} \pm 0.14{\rm(systematic)}$ or [Fe/H]$_{UVES}=-1.67 \pm 0.01{\rm(statistical)} \pm 0.19{\rm(systematic)}$.Absolute magnitudes, radii and masses are also estimated for the RR Lyrae stars. A detailed search for SX Phe stars in the Blue Straggler region was conducted but none were discovered. If SX Phe exist in the cluster then their amplitudes must be smaller than the detection limit of our photometry. The CMD has been corrected for heavy differential reddening using the detailed extinction map of the cluster of Alonso-Garc\'ia et al. (2012). This has allowed us to set the mean cluster distance from two independent estimates; from the RRab and RRc absolute magnitudes, we find $8.04\pm 0.19$ kpc and $7.88\pm0.30$ kpc respectively., Comment: 20 pages, 17 figures, 5 tables, 1 electronic table
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38. Estimating the parameters of globular cluster M 30 (NGC 7099) from time-series photometry
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Kains, N., Bramich, D. M., Ferro, A. Arellano, Jaimes, R. Figuera, Jørgensen, U. G., Giridhar, S., Alsubai, K. A., Andersen, J. M., Bozza, V., Browne, P., Burgdorf, M., Novati, S. Calchi, Damerdji, Y., Diehl, C., Dodds, P., Dominik, M., Elyiv, A., Fang, X. -S., Giannini, E., Gu, S. -H., Hardis, S., Harpsøe, K., Hinse, T. C., Hornstrup, A., Hundertmark, M., Jessen-Hansen, J., Juncher, D., Kerins, E., Kjeldsen, H., Korhonen, H., Liebig, C., Lund, M. N., Lundkvist, M., Mancini, L., Martin, R., Mathiasen, M., Penny, M. T., Rabus, M., Rahvar, S., Ricci, D., Sahu, K., Scarpetta, G., Skottfelt, J., Snodgrass, C., Southworth, J., Surdej, J., Tregloan-Reed, J., Vilela, C., Wertz, O., Williams, A., Kains, N., Bramich, D. M., Ferro, A. Arellano, Jaimes, R. Figuera, Jørgensen, U. G., Giridhar, S., Alsubai, K. A., Andersen, J. M., Bozza, V., Browne, P., Burgdorf, M., Novati, S. Calchi, Damerdji, Y., Diehl, C., Dodds, P., Dominik, M., Elyiv, A., Fang, X. -S., Giannini, E., Gu, S. -H., Hardis, S., Harpsøe, K., Hinse, T. C., Hornstrup, A., Hundertmark, M., Jessen-Hansen, J., Juncher, D., Kerins, E., Kjeldsen, H., Korhonen, H., Liebig, C., Lund, M. N., Lundkvist, M., Mancini, L., Martin, R., Mathiasen, M., Penny, M. T., Rabus, M., Rahvar, S., Ricci, D., Sahu, K., Scarpetta, G., Skottfelt, J., Snodgrass, C., Southworth, J., Surdej, J., Tregloan-Reed, J., Vilela, C., Wertz, O., and Williams, A.
- Abstract
We present the analysis of 26 nights of V and I time-series observations from 2011 and 2012 of the globular cluster M 30 (NGC 7099). We used our data to search for variable stars in this cluster and refine the periods of known variables; we then used our variable star light curves to derive values for the cluster's parameters. We used difference image analysis to reduce our data to obtain high-precision light curves of variable stars. We then estimated the cluster parameters by performing a Fourier decomposition of the light curves of RR Lyrae stars for which a good period estimate was possible. We also derive an estimate for the age of the cluster by fitting theoretical isochrones to our colour-magnitude diagram (CMD). Out of 13 stars previously catalogued as variables, we find that only 4 are bona fide variables. We detect two new RR Lyrae variables, and confirm two additional RR Lyrae candidates from the literature. We also detect four other new variables, including an eclipsing blue straggler system, and an SX Phoenicis star. This amounts to a total number of confirmed variable stars in M 30 of 12. We perform Fourier decomposition of the light curves of the RR Lyrae stars to derive cluster parameters using empirical relations. We find a cluster metallicity [Fe/H]_ZW=-2.01 +- 0.04, or [Fe/H]_UVES=-2.11 +- 0.06, and a distance of 8.32 +- 0.20 kpc (using RR0 variables), 8.10 kpc (using one RR1 variable), and 8.35 +- 0.42 kpc (using our SX Phoenicis star detection in M 30). Fitting isochrones to the CMD, we estimate an age of 13.0 +- 1.0 Gyr for M 30., Comment: 16 pages, 10 figures, 10 tables, A&A in press
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39. Microlensing Discovery of a Population of Very Tight, Very Low-mass Binary Brown Dwarfs
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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., Szymański, M. K., Kubiak, M., Pietrzyński, G., Soszyński, I., Skowron, J., Kozłowski, S., Poleski, R., Ulaczyk, K., Wyrzykowski, Ł., Pietrukowicz, P., 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., Munoz, J. A., Park, B. -G., Park, H., Pogge, R. W., Shvartzvald, Y., Shin, I. -G., Yee, J. C., Alsubai, K. A., Browne, P., Burgdorf, M. J., Novati, S. Calchi, 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., Jørgensen, 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., Albrow, M. D., Bachelet, E., Batista, V., Brillant, S., Cassan, A., Cole, A. A., Coutures, C., Dieters, S., Prester, D. Dominis, Donatowicz, J., Fouqué, P., Greenhill, J., Kubas, D., Marquette, J. -B., Menzies, J. W., Sahu, K. C., Zub, M., Bramich, D. M., Horne, K., Steele, I. A., Street, R. A., 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., Szymański, M. K., Kubiak, M., Pietrzyński, G., Soszyński, I., Skowron, J., Kozłowski, S., Poleski, R., Ulaczyk, K., Wyrzykowski, Ł., Pietrukowicz, P., 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., Munoz, J. A., Park, B. -G., Park, H., Pogge, R. W., Shvartzvald, Y., Shin, I. -G., Yee, J. C., Alsubai, K. A., Browne, P., Burgdorf, M. J., Novati, S. Calchi, 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., Jørgensen, 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., Albrow, M. D., Bachelet, E., Batista, V., Brillant, S., Cassan, A., Cole, A. A., Coutures, C., Dieters, S., Prester, D. Dominis, Donatowicz, J., Fouqué, P., Greenhill, J., Kubas, D., Marquette, J. -B., Menzies, J. W., Sahu, K. C., Zub, M., Bramich, D. M., Horne, K., Steele, I. A., and Street, R. A.
- 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., Comment: 7 pages, 5 figures, 3 tables, ApJ submitted
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40. Flux and color variations of the doubly imaged quasar UM673
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Ricci, D., Elyiv, A., Finet, F., Wertz, O., Alsubai, K., Anguita, T., Bozza, V., Browne, P., Burgdorf, M., Novati, S. Calchi, Dodds, P., Dominik, M., Dreizler, S., Gerner, T., Glitrup, M., Grundahl, F., Hardis, S., Harpsøe, K., Hinse, T. C., Hornstrup, A., Hundertmark, M., Jørgensen, U. G., Kains, N., Kerins, E., Liebig, C., Maier, G., Mancini, L., Masi, G., Mathiasen, M., Penny, M., Proft, S., Rahvar, S., Scarpetta, G., Sahu, K., Schäfer, S., Schönebeck, F., Schmidt, R., Skottfelt, J., Snodgrass, C., Southworth, J., Thöne, C. C., Wambsganss, J., Zimmer, F., Zub, M., Surdej, J., Ricci, D., Elyiv, A., Finet, F., Wertz, O., Alsubai, K., Anguita, T., Bozza, V., Browne, P., Burgdorf, M., Novati, S. Calchi, Dodds, P., Dominik, M., Dreizler, S., Gerner, T., Glitrup, M., Grundahl, F., Hardis, S., Harpsøe, K., Hinse, T. C., Hornstrup, A., Hundertmark, M., Jørgensen, U. G., Kains, N., Kerins, E., Liebig, C., Maier, G., Mancini, L., Masi, G., Mathiasen, M., Penny, M., Proft, S., Rahvar, S., Scarpetta, G., Sahu, K., Schäfer, S., Schönebeck, F., Schmidt, R., Skottfelt, J., Snodgrass, C., Southworth, J., Thöne, C. C., Wambsganss, J., Zimmer, F., Zub, M., and Surdej, J.
- Abstract
With the aim of characterizing the flux and color variations of the multiple components of the gravitationally lensed quasar UM673 as a function of time, we have performed multi-epoch and multi-band photometric observations with the Danish 1.54m telescope at the La Silla Observatory. The observations were carried out in the VRi spectral bands during four seasons (2008--2011). We reduced the data using the PSF (Point Spread Function) photometric technique as well as aperture photometry. Our results show for the brightest lensed component some significant decrease in flux between the first two seasons (+0.09/+0.11/+0.05 mag) and a subsequent increase during the following ones (-0.11/-0.11/-0.10 mag) in the V/R/i spectral bands, respectively. Comparing our results with previous studies, we find smaller color variations between these seasons as compared with previous ones. We also separate the contribution of the lensing galaxy from that of the fainter and close lensed component., Comment: 7 pages, 8 figures, 4 tables
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- 2013
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41. MOA-2010-BLG-073L:AN M-DWARF WITH A SUBSTELLAR COMPANION AT THE PLANET/BROWN DWARF BOUNDARY
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Street, R.A., Choi, J.-Y, Tsapras, Y., Han, C., Furusawa, K., Hundertmark, M., Gould, A., Sumi, T., Jørgensen, Uffe Gråe, Harpsøe, Kennet Bomann West, Mathiasen, M., Hardis, S., Street, R.A., Choi, J.-Y, Tsapras, Y., Han, C., Furusawa, K., Hundertmark, M., Gould, A., Sumi, T., Jørgensen, Uffe Gråe, Harpsøe, Kennet Bomann West, Mathiasen, M., and Hardis, S.
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- 2013
42. MOA-2010-BLG-523:'FAILED PLANET' = RS CVn STAR
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Could, A., Yee, J.C., Bond, I.A., Udalski, A., Han, C., Jørgensen, Uffe Gråe, Greenhill, J., Tsapras, Y., Pinsonneault, M.H., Bensby, T., Allen, W., Harpsøe, Kennet Bomann West, Mathiasen, M., Could, A., Yee, J.C., Bond, I.A., Udalski, A., Han, C., Jørgensen, Uffe Gråe, Greenhill, J., Tsapras, Y., Pinsonneault, M.H., Bensby, T., Allen, W., Harpsøe, Kennet Bomann West, and Mathiasen, M.
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- 2013
43. A detailed census of variable stars in the globular cluster NGC 6333 (M9) from CCD differential photometry
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Arellano Ferro, A., Bramich, D. M., Jaimes, R. Figuera, Giridhar, Sunetra, Kains, N., Kuppuswamy, K., Jørgensen, Uffe Gråe, Alsubai, K. A., Andersen, J. M., Bozza, V., Browne, P., Novati, S. Calchi, Damerdji, Y., Diehl, C., Dominik, M., Dreizler, S., Elyiv, A., Giannini, E., Harpsøe, Kennet Bomann West, Hessman, F. V., Hinse, T. C., Hundertmark, Markus, Juncher, Diana, Kerins, E., Korhonen, Heidi Helena, Liebig, C., Mancini, L., Mathiasen, M., Penny, M. T., Rabus, M., Rahvar, S., Ricci, D., Scarpetta, G., Skottfelt, Jesper Mirsa, Snodgrass, C., Southworth, J., Surdej, J., Tregloan-Reed, T., Vilela, C., Wertz, O., Arellano Ferro, A., Bramich, D. M., Jaimes, R. Figuera, Giridhar, Sunetra, Kains, N., Kuppuswamy, K., Jørgensen, Uffe Gråe, Alsubai, K. A., Andersen, J. M., Bozza, V., Browne, P., Novati, S. Calchi, Damerdji, Y., Diehl, C., Dominik, M., Dreizler, S., Elyiv, A., Giannini, E., Harpsøe, Kennet Bomann West, Hessman, F. V., Hinse, T. C., Hundertmark, Markus, Juncher, Diana, Kerins, E., Korhonen, Heidi Helena, Liebig, C., Mancini, L., Mathiasen, M., Penny, M. T., Rabus, M., Rahvar, S., Ricci, D., Scarpetta, G., Skottfelt, Jesper Mirsa, Snodgrass, C., Southworth, J., Surdej, J., Tregloan-Reed, T., Vilela, C., and Wertz, O.
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- 2013
44. High-precision photometry by telescope defocusing - V. WASP-15 and WASP-16
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Southworth, John, Mancini, L., Browne, P., Burgdorf, M., Novati, S. Calchi, Dominik, M., Gerner, T., Hinse, T. C., Jørgensen, Uffe Gråe, Kains, N., Ricci, D., Schäfer, S., Schönebeck, F., Tregloan-Reed, J., Alsubai, K. A., Bozza, V., Chen, G., Dodds, P., Dreizler, S., Fang, X.-S., Finet, F., Gu, S.-H., Hardis, S., Harpsøe, Kennet Bomann West, Henning, Th., Hundertmark, M., Jessen-Hansen, Jens, Kerins, E., Kjeldsen, Hans, Liebig, C., Lund, Mikkel Nørup, Lundkvist, Mia, Mathiasen, M., Nikolov, N., Penny, M. T., Proft, S., Rahvar, S., Sahu, K., Scarpetta, G., Skottfelt, Jesper Mirsa, Snodgrass, C., Surdej, J., Wertz, O., Southworth, John, Mancini, L., Browne, P., Burgdorf, M., Novati, S. Calchi, Dominik, M., Gerner, T., Hinse, T. C., Jørgensen, Uffe Gråe, Kains, N., Ricci, D., Schäfer, S., Schönebeck, F., Tregloan-Reed, J., Alsubai, K. A., Bozza, V., Chen, G., Dodds, P., Dreizler, S., Fang, X.-S., Finet, F., Gu, S.-H., Hardis, S., Harpsøe, Kennet Bomann West, Henning, Th., Hundertmark, M., Jessen-Hansen, Jens, Kerins, E., Kjeldsen, Hans, Liebig, C., Lund, Mikkel Nørup, Lundkvist, Mia, Mathiasen, M., Nikolov, N., Penny, M. T., Proft, S., Rahvar, S., Sahu, K., Scarpetta, G., Skottfelt, Jesper Mirsa, Snodgrass, C., Surdej, J., and Wertz, O.
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- 2013
45. Physical properties, transmission and emission spectra of the WASP-19 planetary system from multi-colour photometry
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Mancini, L., Ciceri, S., Chen, G., Tregloan-Reed, J., Fortney, J.J., Southworth, J., Tan, T.G., Burgdorf, M., Jørgensen, Uffe Gråe, Harpsøe, Kennet Bomann West, Mathiasen, M., Skottfelt, Jesper Fælling, Mancini, L., Ciceri, S., Chen, G., Tregloan-Reed, J., Fortney, J.J., Southworth, J., Tan, T.G., Burgdorf, M., Jørgensen, Uffe Gråe, Harpsøe, Kennet Bomann West, Mathiasen, M., and Skottfelt, Jesper Fælling
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- 2013
46. The transiting system GJ1214:high-precision defocused transit observations and a search for evidence of transit timing variation
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Harpsøe, Kennet Bomann West, Hardis, S., Hinse, T.C., Jørgensen, Uffe Gråe, Mancini, L., Southworth, J., Alsubai, K.A., Bozza, V., Browne, P., Burgdorf, M. J., Novati, S. Calchi, Dodds, P., Dominik, M., Fang, X. -S., Finet, F., Gerner, T., Gu, S. -H, Hundertmark, M., Jessen-Hansen, Jens, Kains, N., Kerins, E., Kjeldsen, H., Liebig, C., Lund, M.N., Lundkvist, Mia, Mathiasen, M., Nesvorny, D., Nikolov, N., Penny, M. T., Proft, S., Rahvar, S., Ricci, D., Sahu, K. C., Scarpetta, G., Schaefer, S., Schoenebeck, F., Snodgrass, C., Skottfelt, Jesper Fælling, Surdej, J., Tregloan-Reed, J., Wertz, O., Harpsøe, Kennet Bomann West, Hardis, S., Hinse, T.C., Jørgensen, Uffe Gråe, Mancini, L., Southworth, J., Alsubai, K.A., Bozza, V., Browne, P., Burgdorf, M. J., Novati, S. Calchi, Dodds, P., Dominik, M., Fang, X. -S., Finet, F., Gerner, T., Gu, S. -H, Hundertmark, M., Jessen-Hansen, Jens, Kains, N., Kerins, E., Kjeldsen, H., Liebig, C., Lund, M.N., Lundkvist, Mia, Mathiasen, M., Nesvorny, D., Nikolov, N., Penny, M. T., Proft, S., Rahvar, S., Ricci, D., Sahu, K. C., Scarpetta, G., Schaefer, S., Schoenebeck, F., Snodgrass, C., Skottfelt, Jesper Fælling, Surdej, J., Tregloan-Reed, J., and Wertz, O.
- Abstract
Aims. We present 11 high-precision photometric transit observations of the transiting super-Earth planet GJ 1214 b. Combining these data with observations from other authors, we investigate the ephemeris for possible signs of transit timing variations (TTVs) using a Bayesian approach. Methods. The observations were obtained using telescope-defocusing techinques, and achieve a high precision with random errors in the photometry as low as 1 mmag per point. To investigate the possiblity of TTVs in the light curve, we calculate the overall probability of a TTV signal using Bayesian methods. Results. The observations are used to determine the photometric parameters and the physical properties of the GJ 1214 system. Our results are in good agreement with published values. Individual times of mid-transit are measured with uncertainites as low as 10 s, allowing us to reduce the uncertainity in the orbital period by a factor or two. Conclusions. A Bayesian analysis reveals that it is highly improbable that the observed transit times is explained by TTV caused by a planet in the nominal habitable zone, when compared with the simpler alternative of a linear ephemeris.
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- 2013
47. A giant planet beyond the snow line in microlensing event OGLE-2011-BLG-0251
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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., 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., and Zub, M.
- Abstract
Aims. 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. Methods. 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 × 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. Results. We find that the lens is made up of a planet of mass 0.53 ± 0.21 M J orbiting an M dwarf host star with a mass of 0.26 ± 0.11 M⊙. 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. © 2013 ESO.
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- 2013
48. Flux and color variations of the doubly imaged quasar UM673
- Author
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Ricci, D., Elyiv, A., Finet, F., Wertz, O., Alsubai, K., Anguita, T., Bozza, V., Browne, P., Burgdorf, M., Calchi Novati, S., Dodds, P., Dominik, M., Dreizler, S., Gerner, T., Glitrup, M., Grundahl, F., Hardis, S., Harpsøe, K., Hinse, T.C., Hornstrup, Allan, Hundertmark, M., Jørgensen, U.G., Kains, N., Kerins, E., Liebig, C., Maier, G., Mancini, L., Masi, G., Mathiasen, M., Penny, M., Proft, S., Rahvar, S., Scarpetta, G., Sahu, K., Schäfer, S., Schönebeck, F., Schmidt, R., Skottfelt, J., Snodgrass, C., Southworth, J., Thöne, C.C., Wambsganss, J., Zimmer, F., Zub, M., Surdej, J., Ricci, D., Elyiv, A., Finet, F., Wertz, O., Alsubai, K., Anguita, T., Bozza, V., Browne, P., Burgdorf, M., Calchi Novati, S., Dodds, P., Dominik, M., Dreizler, S., Gerner, T., Glitrup, M., Grundahl, F., Hardis, S., Harpsøe, K., Hinse, T.C., Hornstrup, Allan, Hundertmark, M., Jørgensen, U.G., Kains, N., Kerins, E., Liebig, C., Maier, G., Mancini, L., Masi, G., Mathiasen, M., Penny, M., Proft, S., Rahvar, S., Scarpetta, G., Sahu, K., Schäfer, S., Schönebeck, F., Schmidt, R., Skottfelt, J., Snodgrass, C., Southworth, J., Thöne, C.C., Wambsganss, J., Zimmer, F., Zub, M., and Surdej, J.
- Abstract
Aims. With the aim of characterizing the flux and color variations of the multiple components of the gravitationally lensed quasar UM673 as a function of time, we have performed multiepoch and multiband photometric observations with the Danish telescope at the La Silla Observatory. Methods. The observations were carried out in the VRi spectral bands during four seasons (2008-2011). We reduced the data using the point spread function photometric technique as well as aperture photometry. Results. Our results show for the brightest lensed component some significant decrease in flux between the first two seasons (+ 0.09/+ 0.11/+ 0.05 mag) and a subsequent increase during the following ones (- 0.11/- 0.11/- 0.10 mag) in the V/R/i spectral bands, respectively. Comparing our results with previous studies, we find smaller color variations between these seasons as compared with previous ones. We also separate the contribution of the lensing galaxy from that of the fainter and close lensed component. © ESO, 2013.
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- 2013
49. Estimating the parameters of globular cluster M 30 (NGC 7099) from time-series photometry
- Author
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Kains, N., Bramich, D., Arellano Ferro, A., Figuera Jaimes, R., Jørgensen, U., Giridhar, S., Penny, M., Alsubai, K., Andersen, J., Bozza, V., Browne, P., Burgdorf, M., Calchi Novati, S., Damerdji, Y., Diehl, C., Dodds, P., Dominik, M., Elyiv, A., Fang, X., Giannini, E., Gu, S., Hardis, S., Harpsoe, K., Hinse, T., Hornstrup, A., Hundertmark, M., Jessen-Hansen, J., Juncher, D., Kerins, E., Kjeldsen, H., Korhonen, H., Liebig, C., Lund, M., Lundkvist, M., Mancini, L., Martin, R., Mathiasen, M., Rabus, M., Rahvar, S., Ricci, D., Sahu, K., Scarpetta, G., Skottfelt, J., Snodgrass, C., Southworth, J., Surdej, J., Tregloan-Reed, J., Vilela, C., Wertz, O., Williams, Andrew, Kains, N., Bramich, D., Arellano Ferro, A., Figuera Jaimes, R., Jørgensen, U., Giridhar, S., Penny, M., Alsubai, K., Andersen, J., Bozza, V., Browne, P., Burgdorf, M., Calchi Novati, S., Damerdji, Y., Diehl, C., Dodds, P., Dominik, M., Elyiv, A., Fang, X., Giannini, E., Gu, S., Hardis, S., Harpsoe, K., Hinse, T., Hornstrup, A., Hundertmark, M., Jessen-Hansen, J., Juncher, D., Kerins, E., Kjeldsen, H., Korhonen, H., Liebig, C., Lund, M., Lundkvist, M., Mancini, L., Martin, R., Mathiasen, M., Rabus, M., Rahvar, S., Ricci, D., Sahu, K., Scarpetta, G., Skottfelt, J., Snodgrass, C., Southworth, J., Surdej, J., Tregloan-Reed, J., Vilela, C., Wertz, O., and Williams, Andrew
- Abstract
Aims. We present the analysis of 26 nights of V and I time-series observations from 2011 and 2012 of the globular cluster M30 (NGC 7099). Weused our data to search for variable stars in this cluster and refine the periods of known variables; we then used our variable star light curves toderive values for the cluster’s parameters.Methods. We used difference image analysis to reduce our data to obtain high-precision light curves of variable stars.We then estimated the clusterparameters by performing a Fourier decomposition of the light curves of RR Lyrae stars for which a good period estimate was possible. We alsoderived an estimate for the age of the cluster by fitting theoretical isochrones to our colour-magnitude diagram (CMD).Results. Out of 13 stars previously catalogued as variables, we find that only 4 are bona fide variables. We detect two new RR Lyrae variables,and confirm two additional RR Lyrae candidates from the literature. We also detect four other new variables, including an eclipsing blue stragglersystem, and an SX Phoenicis star. This amounts to a total number of confirmed variable stars in M30 of 12. We perform Fourier decomposition ofthe light curves of the RR Lyrae stars to derive cluster parameters using empirical relations.We find a cluster metallicity [Fe/H]ZW = -2.01±0.04,or [Fe/H]UVES = -2.11 ± 0.06, and a distance of 8.32 ± 0.20 kpc (using RR0 variables), 8.10 kpc (using one RR1 variable), and 8.35 ± 0.42 kpc(using our SX Phoenicis star detection in M30). Fitting isochrones to the CMD, we estimate an age of 13.0 ± 1.0 Gyr for M30.
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- 2013
50. Moa-2010-BLG-073L: An m-dwarf with a substellar companion at the planet/brown dwarf boundary
- Author
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Street, R., Choi, J., Tsapras, Y., Han, C., Furusawa, K., Hundertmark, M., Gould, A., Sumi, T., Bond, I., Wouters, D., Zellem, R., Udalski, A., Snodgrass, C., Horne, K., Dominik, M., Browne, P., Kains, N., Bramich, D., Bajek, D., Steele, I., Ipatov, S., Abe, F., Bennett, D., Botzler, C., Chote, P., Freeman, M., Fukui, A., Harris, P., Itow, Y., Ling, C., Masuda, K., Matsubara, Y., Miyake, N., Muraki, Y., Nagayama, T., Nishimaya, S., Ohnishi, K., Rattenbury, N., Saito, T., Sullivan, D., Suzuki, D., Sweatman, W., Tristram, P., Wada, K., Yock, P., Szymanski, M., Kubiak, M., Pietrzynski, G., Soszynski, I., Poleski, R., Ulaczyk, K., Wyrzykowski, L., Yee, J., Dong, S., Shin, I., Lee, C., Skowron, J., Andrade de Almeida, L., DePoy, D., Gaudi, B., Hung, L., Jablonski, F., Kaspi, S., Klein, N., Hwang, K., Koo, J., Maoz, D., Munoz, J., Pogge, R., Polishhook, D., Shporer, A., McCormick, J., Christie, G., Natusch, T., Allen, B., Drummond, J., Moorhouse, D., Thornley, G., Knowler, M., Bos, M., Bolt, G., Beaulieu, J., Albrow, M., Batista, V., Brillant, S., Caldwell, J., Cassan, A., Cole, A., Corrales, E., Coutures, C., Dieters, S., Dominis Prester, D., Donatowicz, J., Fouque, P., Bachelet, E., Greenhill, J., Kane, S., Kubas, D., Marquette, J., Martin, R., Menzies, J., Pollard, K., Sahu, K., Wambsganss, J., Williams, Andrew, Zub, M., Alsubai, K., Bozza, V., Burgdorf, M., Calchi Novati, S., Dodds, P., Dreizler, S., Finet, F., Gerner, T., Hardis, S., Harpsoe, K., Hessman, F., Hinse, T., Jorgensen, U., Kerins, E., Liebig, C., Mancini, L., Mathiasen, M., Penny, M., Proft, S., Rahvar, S., Ricci, D., Scarpetta, G., Schafer, S., Schonebeck, F., Southworth, J., Surdej, J., Street, R., Choi, J., Tsapras, Y., Han, C., Furusawa, K., Hundertmark, M., Gould, A., Sumi, T., Bond, I., Wouters, D., Zellem, R., Udalski, A., Snodgrass, C., Horne, K., Dominik, M., Browne, P., Kains, N., Bramich, D., Bajek, D., Steele, I., Ipatov, S., Abe, F., Bennett, D., Botzler, C., Chote, P., Freeman, M., Fukui, A., Harris, P., Itow, Y., Ling, C., Masuda, K., Matsubara, Y., Miyake, N., Muraki, Y., Nagayama, T., Nishimaya, S., Ohnishi, K., Rattenbury, N., Saito, T., Sullivan, D., Suzuki, D., Sweatman, W., Tristram, P., Wada, K., Yock, P., Szymanski, M., Kubiak, M., Pietrzynski, G., Soszynski, I., Poleski, R., Ulaczyk, K., Wyrzykowski, L., Yee, J., Dong, S., Shin, I., Lee, C., Skowron, J., Andrade de Almeida, L., DePoy, D., Gaudi, B., Hung, L., Jablonski, F., Kaspi, S., Klein, N., Hwang, K., Koo, J., Maoz, D., Munoz, J., Pogge, R., Polishhook, D., Shporer, A., McCormick, J., Christie, G., Natusch, T., Allen, B., Drummond, J., Moorhouse, D., Thornley, G., Knowler, M., Bos, M., Bolt, G., Beaulieu, J., Albrow, M., Batista, V., Brillant, S., Caldwell, J., Cassan, A., Cole, A., Corrales, E., Coutures, C., Dieters, S., Dominis Prester, D., Donatowicz, J., Fouque, P., Bachelet, E., Greenhill, J., Kane, S., Kubas, D., Marquette, J., Martin, R., Menzies, J., Pollard, K., Sahu, K., Wambsganss, J., Williams, Andrew, Zub, M., Alsubai, K., Bozza, V., Burgdorf, M., Calchi Novati, S., Dodds, P., Dreizler, S., Finet, F., Gerner, T., Hardis, S., Harpsoe, K., Hessman, F., Hinse, T., Jorgensen, U., Kerins, E., Liebig, C., Mancini, L., Mathiasen, M., Penny, M., Proft, S., Rahvar, S., Ricci, D., Scarpetta, G., Schafer, S., Schonebeck, F., Southworth, J., and Surdej, J.
- Abstract
We present an analysis of the anomalous microlensing event,MOA-2010-BLG-073, announced by the Microlensing Observations in Astrophysics survey on 2010 March 18. This event was remarkable because the source was previously known to be photometrically variable. Analyzing the pre-event source light curve, we demonstrate that it is an irregular variable over timescales >200 days. Its dereddened color, (V - I )S,0, is 1.221 ± 0.051 mag, and from our lens model we derive a source radius of 14.7 ± 1.3 R, suggesting that it is a red giant star. We initially explored a number of purely microlensing models for the event but found a residual gradient in the data taken prior to and after the event. This is likely to be due to the variability of the source rather than part of the lensing event, so we incorporated a slope parameter in our model in order to derive the true parameters of the lensing system. Wefind that the lensing system has a mass ratio of q = 0.0654 ± 0.0006. The Einstein crossing time of the event, tE = 44.3±0.1 days, was sufficiently long that the light curve exhibited parallax effects. In addition, the source trajectory relative to the large caustic structure allowed the orbital motion of the lens system to be detected. Combining the parallax with the Einstein radius, we were able to derive the distance to the lens, DL = 2.8 ± 0.4 kpc, and the massesof the lensing objects. The primary of the lens is an M-dwarf with ML,1 = 0.16 ± 0.03 M, while the companion has ML,2 = 11.0 ± 2.0 MJ, putting it in the boundary zone between planets and brown dwarfs.
- Published
- 2013
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