Search

Your search keyword '"Novati A"' showing total 96 results
Start Over Author "Novati A" Journal monthly notices of the royal astronomical society
96 results on '"Novati A"'

1. Kepler K2Campaign 9 – II. First space-based discovery of an exoplanet using microlensing

Author

D Specht, R Poleski, M T Penny, E Kerins, I McDonald, Chung-Uk Lee, A Udalski, I A Bond, Y Shvartzvald, Weicheng Zang, R A Street, D W Hogg, B S Gaudi, T Barclay, G Barentsen, S B Howell, F Mullally, C B Henderson, S T Bryson, D A Caldwell, M R Haas, J E Van Cleve, K Larson, K McCalmont, C Peterson, D Putnam, S Ross, M Packard, L Reedy, Michael D Albrow, Sun-Ju Chung, Youn Kil Jung, Andrew Gould, Cheongho Han, Kyu-Ha Hwang, Yoon-Hyun Ryu, In-Gu Shin, Hongjing Yang, Jennifer C Yee, Sang-Mok Cha, Dong-Jin Kim, Seung-Lee Kim, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W Pogge, M K Szymański, I Soszyński, K Ulaczyk, P Pietrukowicz, Sz Kozłowski, J Skowron, P Mróz, Shude Mao, Pascal Fouqué, Wei Zhu, F Abe, R Barry, D P Bennett, A Bhattacharya, A Fukui, H Fujii, Y Hirao, Y Itow, R Kirikawa, I Kondo, N Koshimoto, Y Matsubara, S Matsumoto, S Miyazaki, Y Muraki, G Olmschenk, C Ranc, A Okamura, N J Rattenbury, Y Satoh, T Sumi, D Suzuki, S I Silva, T Toda, P J Tristram, A Vandorou, H Yama, C Beichman, G Bryden, and S Calchi Novati

Published
2023
Full Text
View/download PDF

2. OGLE-2015-BLG-0845L: a low-mass M dwarf from the microlensing parallax and xallarap effects.

Author

(胡哲程), Zhecheng Hu, (祝伟), Wei Zhu, Gould, Andrew, Udalski, Andrzej, Sumi, Takahiro, (陈平), Ping Chen, Calchi Novati, Sebastiano, Yee, Jennifer C, Beichman, Charles A, Bryden, Geoffery, Carey, Sean, Fausnaugh, Michael, Gaudi, B Scott, Henderson, Calen B, Shvartzvald, Yossi, Wibking, Benjamin, Mróz, Przemek, Skowron, Jan, Poleski, Radosław, and Szymański, Michał K

Subjects
GRAVITATIONAL lenses, PARALLAX, MASS measurement, MICROLENSES, DATA analysis
Abstract

We present the analysis of the microlensing event OGLE-2015-BLG-0845, which was affected by both the microlensing parallax and xallarap effects. The former was detected via the simultaneous observations from the ground and Spitzer , and the latter was caused by the orbital motion of the source star in a relatively close binary. The combination of these two effects led to a mass measurement of the lens object, revealing a low-mass (⁠|$0.14 \pm 0.05 \, \mathrm{ M}_{\odot }$|⁠) M dwarf at the bulge distance (⁠|$7.6 \pm 1.0$| kpc). The source binary consists of a late F-type subgiant and a K-type dwarf of |$\sim 1.2$| and |$\sim 0.9 \mathrm{ M}_{\odot }$|⁠ , respectively, and the orbital period is |$70 \pm 10$| d. OGLE-2015-BLG-0845 is the first single-lens event in which the lens mass is measured via the binarity of the source. Given the abundance of binary systems as potential microlensing sources, the xallarap effect may not be a rare phenomenon. Our work thus highlights the application of the xallarap effect in the mass determination of microlenses, and the same method can be used to identify isolated dark lenses. [ABSTRACT FROM AUTHOR]

Published
2024
Full Text
View/download PDF

3. Ogle-2018-BLG-0799lb: A Q ∼ 2.7 × 10(−3) Planet With Spitzer Parallax

Author

Weicheng Zang, Yossi Shvartzvald, Andrzej Udalski, Jennifer C. Yee, Chung-Uk Lee, Takahiro Sumi, Xiangyu Zhang, Hongjing Yang, Shude Mao, Sebastiano Calchi Novati, Andrew Gould, Wei Zhu, Charles A. Beichman, Geoffery Bryden, Sean Carey, B. Scott Gaudi, Calen B. Henderson, Przemek Mroz, Jan Skowron, Radoslaw Poleski, Michał K. Szymanski, Igor Soszynski, Paweł Pietrukowicz, Szymon Kozłowski, Krzysztof Ulaczyk, Krzysztof A. Rybicki, Patryk Iwanek, Marcin Wrona, Michael D. Albrow, Sun-Ju Chung, Cheongho Han, Kyu-Ha Hwang, Youn Kil Jung, Yoon-Hyun Ryu, In-Gu Shin, Richard Barry, and David P. Bennett

Subjects
Astrophysics
Abstract

We report the discovery and analysis of a planet in the microlensing event OGLE-2018-BLG-0799. The planetary signal was observed by several ground-based telescopes, and the planet-host mass ratio is q = (2.65 ± 0.16) × 10(−3). The ground-based observations yield a constraint on the angular Einstein radius θE, and the microlensing parallax vector πE, is strongly constrained by the Spitzer data. However, the 2019 Spitzer baseline data reveal systematics in the Spitzer photometry, so there is ambiguity in the magnitude of the parallax. In our preferred interpretation, a full Bayesian analysis using a Galactic model indicates that the planetary system is composed of an Mplanet = 0.26+0.22 −0.11M(J) planet orbiting an Mhost = 0.093+0.082 −0.038 Mʘ , at a distance of DL = 3.71+3.24 −1.70 kpc. An alternate interpretation of the data shifts the localization of the minima along the arc-shaped microlens parallax constraints. This, in turn, yields a more massive host with median mass of 0.13 Mʘ at a distance of 6.3 kpc. This analysis demonstrates the robustness of the osculating circles formalism, but shows that further investigation is needed to assess how systematics affect the specific localization of the microlens parallax vector and, consequently, the inferred physical parameters.

Published
2022
Full Text
View/download PDF

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

Author

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

Published
2019
Full Text
View/download PDF

5. An analysis of binary microlensing event OGLE-2015-BLG-0060

Author

Y Tsapras, A Cassan, C Ranc, E Bachelet, R Street, A Udalski, M Hundertmark, V Bozza, J P Beaulieu, J B Marquette, E Euteneuer, D M Bramich, M Dominik, R Figuera Jaimes, K Horne, S Mao, J Menzies, R Schmidt, C Snodgrass, I A Steele, J Wambsganss, P Mróz, M K Szymański, I Soszyński, J Skowron, P Pietrukowicz, S Kozłowski, R Poleski, K Ulaczyk, M Pawlak, U G Jørgensen, J Skottfelt, A Popovas, S Ciceri, H Korhonen, M Kuffmeier, D F Evans, N Peixinho, T C Hinse, M J Burgdorf, J Southworth, R Tronsgaard, E Kerins, M I Andersen, S Rahvar, Y Wang, O Wertz, M Rabus, S Calchi Novati, G D’Ago, G Scarpetta, L Mancini, F Abe, Y Asakura, D P Bennett, A Bhattacharya, M Donachie, P Evans, A Fukui, Y Hirao, Y Itow, K Kawasaki, N Koshimoto, M C A Li, C H Ling, K Masuda, Y Matsubara, Y Muraki, S Miyazaki, M Nagakane, K Ohnishi, N Rattenbury, To Saito, A Sharan, H Shibai, D J Sullivan, T Sumi, D Suzuki, P J Tristram, T Yamada, A Yonehara, G D'Ago, and T o Saito

Published
2019
Full Text
View/download PDF

6. Kepler K2Campaign 9 – II. First space-based discovery of an exoplanet using microlensing

Author

Specht, D, primary, Poleski, R, additional, Penny, M T, additional, Kerins, E, additional, McDonald, I, additional, Lee, Chung-Uk, additional, Udalski, A, additional, Bond, I A, additional, Shvartzvald, Y, additional, Zang, Weicheng, additional, Street, R A, additional, Hogg, D W, additional, Gaudi, B S, additional, Barclay, T, additional, Barentsen, G, additional, Howell, S B, additional, Mullally, F, additional, Henderson, C B, additional, Bryson, S T, additional, Caldwell, D A, additional, Haas, M R, additional, Van Cleve, J E, additional, Larson, K, additional, McCalmont, K, additional, Peterson, C, additional, Putnam, D, additional, Ross, S, additional, Packard, M, additional, Reedy, L, additional, Albrow, Michael D, additional, Chung, Sun-Ju, additional, Kil Jung, Youn, additional, Gould, Andrew, additional, Han, Cheongho, additional, Hwang, Kyu-Ha, additional, Ryu, Yoon-Hyun, additional, Shin, In-Gu, additional, Yang, Hongjing, additional, Yee, Jennifer C, additional, Cha, Sang-Mok, additional, Kim, Dong-Jin, additional, Kim, Seung-Lee, additional, Lee, Dong-Joo, additional, Lee, Yongseok, additional, Park, Byeong-Gon, additional, Pogge, Richard W, additional, Szymański, M K, additional, Soszyński, I, additional, Ulaczyk, K, additional, Pietrukowicz, P, additional, Kozłowski, Sz, additional, Skowron, J, additional, Mróz, P, additional, Mao, Shude, additional, Fouqué, Pascal, additional, Zhu, Wei, additional, Abe, F, additional, Barry, R, additional, Bennett, D P, additional, Bhattacharya, A, additional, Fukui, A, additional, Fujii, H, additional, Hirao, Y, additional, Itow, Y, additional, Kirikawa, R, additional, Kondo, I, additional, Koshimoto, N, additional, Matsubara, Y, additional, Matsumoto, S, additional, Miyazaki, S, additional, Muraki, Y, additional, Olmschenk, G, additional, Ranc, C, additional, Okamura, A, additional, Rattenbury, N J, additional, Satoh, Y, additional, Sumi, T, additional, Suzuki, D, additional, Silva, S I, additional, Toda, T, additional, Tristram, P J, additional, Vandorou, A, additional, Yama, H, additional, Beichman, C, additional, Bryden, G, additional, and Calchi Novati, S, additional

Published
2023
Full Text
View/download PDF

7. OGLE-2018-BLG-0799Lb: a q ∼ 2.7 × 10−3 planet with Spitzer parallax

Author

Zang, Weicheng, primary, Shvartzvald, Yossi, additional, Udalski, Andrzej, additional, Yee, Jennifer C, additional, Lee, Chung-Uk, additional, Sumi, Takahiro, additional, Zhang, Xiangyu, additional, Yang, Hongjing, additional, Mao, Shude, additional, Novati, Sebastiano Calchi, additional, Gould, Andrew, additional, Zhu, Wei, additional, Beichman, Charles A, additional, Bryden, Geoffery, additional, Carey, Sean, additional, Gaudi, B Scott, additional, Henderson, Calen B, additional, Mróz, Przemek, additional, Skowron, Jan, additional, Poleski, Radoslaw, additional, Szymański, Michał K, additional, Soszyński, Igor, additional, Pietrukowicz, Paweł, additional, Kozłowski, Szymon, additional, Ulaczyk, Krzysztof, additional, Rybicki, Krzysztof A, additional, Iwanek, Patryk, additional, Wrona, Marcin, additional, Albrow, Michael D, additional, Chung, Sun-Ju, additional, Han, Cheongho, additional, Hwang, Kyu-Ha, additional, Jung, Youn Kil, additional, Ryu, Yoon-Hyun, additional, Shin, In-Gu, additional, Cha, Sang-Mok, additional, Kim, Dong-Jin, additional, Kim, Hyoun-Woo, additional, Kim, Seung-Lee, additional, Lee, Dong-Joo, additional, Lee, Yongseok, additional, Park, Byeong-Gon, additional, Pogge, Richard W, additional, Bond, Ian A, additional, Abe, Fumio, additional, Barry, Richard, additional, Bennett, David P, additional, Bhattacharya, Aparna, additional, Donachie, Martin, additional, Fujii, Hirosane, additional, Fukui, Akihiko, additional, Hirao, Yuki, additional, Itow, Yoshitaka, additional, Kirikawa, Rintaro, additional, Kondo, Iona, additional, Koshimoto, Naoki, additional, Li, Man Cheung Alex, additional, Matsubara, Yutaka, additional, Muraki, Yasushi, additional, Miyazaki, Shota, additional, Ranc, Clément, additional, Rattenbury, Nicholas J, additional, Satoh, Yuki, additional, Shoji, Hikaru, additional, Suzuki, Daisuke, additional, Tanaka, Yuzuru, additional, Tristram, Paul J, additional, Yamawaki, Tsubasa, additional, Yonehara, Atsunori, additional, Bachelet, Etienne, additional, Hundertmark, Markus P G, additional, Jaimes, R Figuera, additional, Maoz, Dan, additional, Penny, Matthew T, additional, Street, Rachel A, additional, and Tsapras, Yiannis, additional

Published
2022
Full Text
View/download PDF

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, and Steele, I. A

Subjects
Astrophysics
Abstract

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; RoboNETLas Cumbres Observatory Global Telescope; Microlensing Network for the Detection of Small Terrestrial Exoplanets; and -FUN. All analyses of the light-curve data favoura 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(exp -3). Subject to some important assumptions, a Bayesian probability density analysis suggests the lens system comprises a 3.09(+1.02/-1.12) MJ planet orbiting a 0.62(+0.20/-0.22) solar mass host star at a deprojected orbital separation of 4.40(+2.16/-1.46) au. The distance to the lens system is 2.22(+0.96/-0.83) kpc. Planet OGLE-2014-BLG-0676Lb provides additional data to the growing number of cool planets discover redusing 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
2016
Full Text
View/download PDF

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

Author

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

Published
2019
Full Text
View/download PDF

11. OGLE-2014-BLG-1186: gravitational microlensing providing evidence for a planet orbiting the foreground star or for a close binary source?

Author

Dominik, M, primary, Bachelet, E, additional, Bozza, V, additional, Street, R A, additional, Han, C, additional, Hundertmark, M, additional, Udalski, A, additional, Bramich, D M, additional, Alsubai, K A, additional, Calchi Novati, S, additional, Ciceri, S, additional, D’Ago, G, additional, Figuera Jaimes, R, additional, Haugbølle, T, additional, Hinse, T C, additional, Horne, K, additional, Jørgensen, U G, additional, Juncher, D, additional, Kains, N, additional, Korhonen, H, additional, Mancini, L, additional, Menzies, J, additional, Popovas, A, additional, Rabus, M, additional, Rahvar, S, additional, Scarpetta, G, additional, Schmidt, R, additional, Skottfelt, J, additional, Snodgrass, C, additional, Southworth, J, additional, Starkey, D, additional, Steele, I A, additional, Surdej, J, additional, Tsapras, Y, additional, Wambsganss, J, additional, Wertz, O, additional, Pietrukowicz, P, additional, Szymański, M K, additional, Mróz, P, additional, Skowron, J, additional, Soszyński, I, additional, Ulaczyk, K, additional, Poleski, R, additional, Wyrzykowski, Ł, additional, and Kozłowski, S, additional

Published
2019
Full Text
View/download PDF

12. Transits and starspots in the WASP-6 planetary system

Author

S. Prof, K. B. W. Harpsøe, U. G. Jørgensen, M. Hundertmark, Sohrab Rahvar, Tobias C. Hinse, S. Calchi Novati, S. Schäfer, T. Gerner, Gaetano Scarpetta, Martin Burgdorf, P. Browne, Luigi Mancini, C. Liebig, Jesper Skottfelt, N. Kains, Martin Dominik, F. Schönebeck, Colin Snodgrass, Eamonn Kerins, Matthew T. Penny, Peter N. Dodds, Kailash C. Sahu, G. Maier, Davide Ricci, Jean Surdej, J. Tregloan-Reed, François Finet, Valerio Bozza, John Southworth, The Royal Society, University of St Andrews. School of Physics and Astronomy, ITA, USA, GBR, FRA, DEU, ESP, DNK, and MEX

Subjects
Rotation period, NDAS, FOS: Physical sciences, Astrophysics, Parameter space, fundamental parameters [Stars], 01 natural sciences, Latitude, Settore FIS/05 - Astronomia e Astrofisica, 0103 physical sciences, QB Astronomy, Transit (astronomy), 010303 astronomy & astrophysics, QC, QB, Earth and Planetary Astrophysics (astro-ph.EP), Physics, 010308 nuclear & particles physics, photometric [Techniques], Starspot, Astronomy, Astronomy and Astrophysics, Planetary system, Light curve, Starspots, Maxima and minima, Planetary systems, QC Physics, 13. Climate action, Space and Planetary Science, individual: WASP-6 [Stars], Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract

We present updates to \textsc{prism}, a photometric transit-starspot model, and \textsc{gemc}, a hybrid optimisation code combining MCMC and a genetic algorithm. We then present high-precision photometry of four transits in the WASP-6 planetary system, two of which contain a starspot anomaly. All four transits were modelled using \textsc{prism} and \textsc{gemc}, and the physical properties of the system calculated. We find the mass and radius of the host star to be $0.836\pm 0.063\,{\rm M}_\odot$ and $0.864\pm0.024\,{\rm R}_\odot$, respectively. For the planet we find a mass of $0.485\pm 0.027\,{\rm M}_{\rm Jup}$, a radius of $1.230\pm0.035\,{\rm R}_{\rm Jup}$ and a density of $0.244\pm0.014\,\rho_{\rm Jup}$. These values are consistent with those found in the literature. In the likely hypothesis that the two spot anomalies are caused by the same starspot or starspot complex, we measure the stars rotation period and velocity to be $23.80 \pm 0.15$\,d and $1.78 \pm 0.20$\,km\,s$^{-1}$, respectively, at a co-latitude of 75.8$^\circ$. We find that the sky-projected angle between the stellar spin axis and the planetary orbital axis is $\lambda = 7.2^{\circ} \pm 3.7^{\circ}$, indicating axial alignment. Our results are consistent with and more precise than published spectroscopic measurements of the Rossiter-McLaughlin effect. These results suggest that WASP-6\,b formed at a much greater distance from its host star and suffered orbital decay through tidal interactions with the protoplanetary disc., Comment: 11 Pages, 6 Figures, MNRAS accepted

Published
2015
Full Text
View/download PDF

13. Pixel lensing as a way to detect extrasolar planets in M31

Author

Alexander F. Zakharov, Ph. Jetzer, S. Calchi Novati, Achille A. Nucita, G. Ingrosso, F. De Paolis, University of Zurich, Ingrosso, G, Ingrosso, Gabriele, Calchi Novati, S., DE PAOLIS, Francesco, Jetzer, P. h., Nucita, Achille, and Zakharov, A. F.

Subjects
530 Physics, gravitational lensing, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Gravitational microlensing, Jupiter, 1912 Space and Planetary Science, Planet, halo [Galaxy], Astrophysics::Galaxy Astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Earth and Planetary Astrophysics (astro-ph.EP), Physics, Order (ring theory), Astronomy and Astrophysics, Giant star, Light curve, Exoplanet, Galaxy: halo, M31 [galaxies], Astrophysics - Solar and Stellar Astrophysics, galaxies: individual: M31, Space and Planetary Science, 10231 Institute for Computational Science, 3103 Astronomy and Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Planetary mass, Astrophysics - Earth and Planetary Astrophysics
Abstract

We study the possibility to detect extrasolar planets in M31 through pixel-lensing observations. Using a Monte Carlo approach, we select the physical parameters of the binary lens system, a star hosting a planet, and we calculate the pixel-lensing light curve taking into account the finite source effects. Indeed, their inclusion is crucial since the sources in M31 microlensing events are mainly giant stars. Light curves with detectable planetary features are selected by looking for significant deviations from the corresponding Paczy\'{n}ski shapes. We find that the time scale of planetary deviations in light curves increase (up to 3-4 days) as the source size increases. This means that only few exposures per day, depending also on the required accuracy, may be sufficient to reveal in the light curve a planetary companion. Although the mean planet mass for the selected events is about $2 M_{\rm {Jupiter}}$, even small mass planets ($M_{\rm P} < 20 M_{\oplus}$) can cause significant deviations, at least in the observations with large telescopes. However, even in the former case, the probability to find detectable planetary features in pixel-lensing light curves is at most a few percent of the detectable events, and therefore many events have to be collected in order to detect an extrasolar planet in M31. Our analysis also supports the claim that the anomaly found in the candidate event PA-99-N2 towards M31 can be explained by a companion object orbiting the lens star., Comment: Accepted for publication on Monthly Notices of the Royal Astronomical Society (MNRAS), 2009

Published
2009
Full Text
View/download PDF

14. ExELS: an exoplanet legacy science proposal for the ESA Euclid mission – I. Cold exoplanets

Author

Arnaud Cassan, J. B. Marquette, M. R. Zapatero Osorio, Nicholas J. Rattenbury, Matthew T. Penny, V. Batista, Patrick Tisserand, Annie C. Robin, S. Calchi Novati, J. P. Beaulieu, Eamonn Kerins, Shude Mao, Iain McDonald, Pascal Fouqué, Jodrell Bank Centre for Astrophysics (JBCA), University of Manchester [Manchester], Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Univers, Transport, Interfaces, Nanostructures, Atmosphère et environnement, Molécules (UMR 6213) (UTINAM), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Franche-Comté (UFC), Université Bourgogne Franche-Comté [COMUE] (UBFC)-Université Bourgogne Franche-Comté [COMUE] (UBFC), Ohio State University [Columbus] (OSU), Università degli Studi di Salerno (UNISA), Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Research School of Astronomy and Astrophysics [Canberra] (RSAA), Australian National University (ANU), Centro de Astrobiologia [Madrid] (CAB), and Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC)

Subjects
planets and satellites: detection, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Cosmic Vision, FOS: Physical sciences, gravitational lensing: micro, Astrophysics::Cosmology and Extragalactic Astrophysics, Gravitational microlensing, 7. Clean energy, 01 natural sciences, Galaxy: bulge, Astrobiology, stars: low-mass, Planet, 0103 physical sciences, planetary systems, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Weak gravitational lensing, Earth and Planetary Astrophysics (astro-ph.EP), Physics, 010308 nuclear & particles physics, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, Astronomy and Astrophysics, Planetary system, Earth mass, Exoplanet, 13. Climate action, Space and Planetary Science, Dark energy, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Euclid is the second M-class mission of the ESA Cosmic Vision programme, with the principal science goal of studying dark energy. Euclid is also expected to undertake additional Legacy Science programmes. One proposal is the Exoplanet Euclid Legacy Survey (ExELS) which will be the first survey able to measure the abundance of exoplanets down to Earth mass for host separations from ~1AU out to the free-floating (unbound) regime. The cold and free-floating exoplanet regimes represent a crucial discovery space for testing planet formation theories. ExELS will use the gravitational microlensing technique and will detect 1000 microlensing events per month over 1.6 deg^2 of the Galactic bulge. We assess how many of these events will have detectable planetary signatures using a detailed multi-wavelength microlensing simulator (MABuLS) which incorporates the Besancon Galactic model with 3D extinction. MABuLS is the first theoretical simulation of microlensing to treat the effects of point spread function (PSF) blending self-consistently with the underlying Galactic model. We use MABuLS, together with current numerical models for the Euclid PSFs, to explore a number of designs and de-scope options for ExELS, including the exoplanet yield as a function of filter choice and slewing time, and the effect of systematic photometry errors. Using conservative extrapolations of current empirical exoplanet mass functions determined from ground-based microlensing and radial velocity surveys, ExELS can expect to detect a few hundred cold exoplanets around mainly G, K and M-type stellar hosts, including ~45 Earth-mass planets and ~6 Mars-mass planets for an observing programme totalling 10 months. ExELS will be capable of measuring the cold exoplanet mass function down to Earth mass or below, with orbital separations from ~1AU to the free-floating regime. (Abridged), Comment: 22 pages. Submitted to MNRAS. New version re-normalises the Besancon model predictions using current luminosity function and microlensing data towards the bulge. Exoplanet predictions are revised (upwards) accordingly. The Euclid exoplanet sensitivity contours shown in Fig 10 are available to download as an ancillary data file

Published
2013
Full Text
View/download PDF

15. High-precision photometry by telescope defocusing - IV. Confirmation of the huge radius of WASP-17 b

Author

David R. Anderson, Sohrab Rahvar, Khalid Al-Subai, J. Tregloan-Reed, C. Liebig, X-S Fang, Kasper Harpsøe, Eamonn Kerins, S-H Gu, N. Kains, John Southworth, H. Kjeldsen, Mikkel N. Lund, J. Skottfelt, Tobias C. Hinse, V. Bozza, U. G. Jørgensen, Olivier Wertz, M. Mathiasen, Jens Jessen-Hansen, M. Hundertmark, S. Dreizler, Martin Dominik, Gaetano Scarpetta, S. Calchi Novati, L. Mancini, Barry Smalley, Jean Surdej, M. T. Penny, Davide Ricci, Colin Snodgrass, and M. Lundkvist

Subjects
Physics, Astronomy and Astrophysics, Orbital eccentricity, Astrophysics::Cosmology and Extragalactic Astrophysics, Radius, Astrophysics, Planetary system, Light curve, Orbital period, 01 natural sciences, Photometry (optics), Stars, Space and Planetary Science, Planet, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, 010306 general physics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

We present photometric observations of four transits in the WASP-17 planetary system, obtained using telescope defocussing techniques and with scatters reaching 0.5 mmag per point. Our revised orbital period is 4.0 +/- 0.6 s longer than previous measurements, a difference of 6.6 sigma, and does not support the published detections of orbital eccentricity in this system. We model the light curves using the JKTEBOP code and calculate the physical properties of the system by recourse to five sets of theoretical stellar model predictions. The resulting planetary radius, Rb = 1.932 +/- 0.052 +/- 0.010 Rjup (statistical and systematic errors respectively), provides confirmation that WASP-17b is the largest planet currently known. All fourteen planets with radii measured to be greater than 1.6 Rjup are found around comparatively hot (Teff > 5900 K) and massive (MA > 1.15 Msun) stars. Chromospheric activity indicators are available for eight of these stars, and all imply a low activity level. The planets have small or zero orbital eccentricities, so tidal effects struggle to explain their large radii. The observed dearth of large planets around small stars may be natural but could also be due to observational biases against deep transits, if these are mistakenly labelled as false positives and so not followed up.

Published
2012
Full Text
View/download PDF

16. Polarization in microlensing events towards the Galactic bulge

Author

Ph. Jetzer, F. De Paolis, Alexander F. Zakharov, G. Ingrosso, A. A. Nucita, Francesco Strafella, and S. Calchi Novati

Subjects
Physics, Very Large Telescope, 010308 nuclear & particles physics, Polarization in astronomy, Stellar atmosphere, Astronomy, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Polarization (waves), Gravitational microlensing, 01 natural sciences, Exoplanet, Stars, Space and Planetary Science, Bulge, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

Gravitational microlensing, when finite size source effects are relevant, provides a unique tool for the study of source star stellar atmospheres through an enhancement of a characteristic polarization signal. This is due to the differential magnification induced during the crossing of the source star. In this paper, we consider a specific set of reported highly magnified, both single and binary exoplanetary systems, microlensing events towards the Galactic bulge and evaluate the expected polarization signal. For this purpose, we consider several polarization models which apply to different types of source stars: hot, late type main sequence and cool giants. As a result we compute the polarization signal P, which goes up to P = 0.04 per cent for late-type stars and up to a few per cent for cool giants, depending on the underlying physical polarization processes and atmosphere model parameters. Given an I-band magnitude at a maximum magnification of about 12 and a typical duration of the polarization signal up to 1 d, we conclude that the currently available technology, in particular the polarimeter in FOcal Reducer and low dispersion Spectrograph 2 (FORS2) on the Very Large Telescope (VLT), potentially may allow the detection of such signals. This observational programme may take advantage of the currently available surveys plus follow-up strategy already routinely used for microlensing monitoring towards the Galactic bulge (aimed at the detection of exoplanets). In particular, this allows one to predict in advance for which events and at which exact time the observing resources may be focused to make intensive polarization measurements.

Published
2012
Full Text
View/download PDF

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

Author

Valerio Bozza, Allan Hornstrup, U. G. Joergensen, Timo Anguita, V. Batista, J. Janczak, S. Calchi Novati, C. C. Thoene, Y. C. Perrott, J.-Y. Choi, To. Saito, Luigi Mancini, M. Zub, Kailash C. Sahu, K. Wada, Philip Yock, Jean Surdej, K. Harpsoee, K. R. Pollard, J. A. R. Caldwell, In-Gu Shin, Joachim Wambsganss, S. H. Lee, A. Kniazev, K. Ulaczyk, M. Hundertmark, Fumio Abe, Y. Muraki, Yiannis Tsapras, R. A. Street, G. Masi, S. Dong, D. Kubas, D. M. Bramich, C. Liebig, R. W. Pogge, Radosław Poleski, L. Wyrzykowski, Ian A. Bond, Tobias C. Hinse, P. M. Kilmartin, John B. Hearnshaw, Eamonn Kerins, Y. Matsubara, Gaetano Scarpetta, D. Dominis Prester, L. Skuljan, Winston L. Sweatman, Akihiko Fukui, C.-U. Lee, Grzegorz Pietrzyński, K. Ohnishi, Kimiaki Masuda, Takahiro Nagayama, K. Furusawa, Igor Soszyński, Denis J. Sullivan, Andrew A. Cole, Martin Dominik, Yasuhiro Hashimoto, Sohrab Rahvar, Chang S. Han, S. R. Kane, A. V. Korpela, J. G. Greenhill, Iain A. Steele, Martin Burgdorf, N. Miyake, M. Mathiasen, C. Coutures, Takahiro Sumi, J. P. Beaulieu, Colin Snodgrass, P. J. Tristram, Nicholas J. Rattenbury, Amanda A. S. Gulbis, Petri Väisänen, M. Kubiak, Andrzej Udalski, R. M. Martin, Michał K. Szymański, S. Dieters, N. Kains, J. Donatowicz, K. H. Cook, Daisuke Suzuki, Arnaud Cassan, J. B. Marquette, Michael D. Albrow, Andrew Williams, David P. Bennett, Andrew Gould, Yoshitaka Itow, Per Kjaergaard, D. A. H. Buckley, Davide Ricci, John Southworth, J. W. Menzies, W. Lin, Alasdair Allan, Keith Horne, Darren L. DePoy, Shude Mao, P. Fouque, Seong-Hong Park, and C. H. Ling

Subjects
Physics, 010504 meteorology & atmospheric sciences, Event (relativity), Brown dwarf, Binary number, Astronomy and Astrophysics, Astrophysics, Parameter space, Light curve, Gravitational microlensing, 01 natural sciences, Space and Planetary Science, 0103 physical sciences, Orbital motion, Anomaly (physics), 010303 astronomy & astrophysics, 0105 earth and related environmental sciences
Abstract

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

Published
2012
Full Text
View/download PDF

18. Microlensing towards the Large Magellanic Cloud: self-lensing for OGLE-II and OGLE-III

Author

S. Calchi Novati and Luigi Mancini

Subjects
Physics, Stars, Line-of-sight, Space and Planetary Science, Milky Way, Dark matter, Astronomy and Astrophysics, Halo, Astrophysics, Massive compact halo object, Gravitational microlensing, Large Magellanic Cloud
Abstract

We present an analysis of the results of the OGLE-III microlensing campaign towards the Large Magellanic Cloud (LMC). We evaluate for all the possible lens populations along the line of sight the expected microlensing quantities, number of events and duration. In particular we consider lensing by massive compact halo objects (MACHOs) in the dark matter haloes of both the Milky Way (MW) and the LMC, and “self lensing” by stars in the LMC bar and disc, in the MW disc and in the stellar haloes of both the LMC and the MW. As a result we find that the self-lensing signal is able to explain the 2 OGLE -III microlensing candidates. In particular, we estimate the expected MW disc signal to be almost as large as that from LMC stars and able, by itself, to explain the observed rate. We evaluate a 95% CL upper limit for f , the halo mass fraction in form of MACHOs, in the range 10-20% for (10 −2 0.5) M⊙, and f = 24% for 1 M⊙ (below 10% in this full range, and in particular below 5% for (10 −2 0.1) M⊙) for the Bright (All) samples of source stars. Furthermore, we find that these limits do not rise much even if we assume the observed events are MACHOs. For the All sample we also evaluate a rather significant constraint on f for larger values of the MACHO mass, in particular f � 50% (95% CL) for100 M⊙, to date the stronger bound coming from microlensing analyses in this mass range. Finally, we discuss these results in the framework of the previous observational campaigns towards the LMC, that of the MACHO and the EROS collaborations, and we present a joint analysis of the OGLE-II and the OGLE-III campaigns.

Published
2011
Full Text
View/download PDF

19. High-precision photometry by telescope defocusing - III. The transiting planetary system WASP-2★

Author

M. Hundertmark, Ivan Bruni, M. Mathiasen, S. Calchi Novati, F. Finet, Davide Ricci, P. Browne, Kasper Harpsøe, John Southworth, L. Mancini, F. Zimmer, S. Rahvar, V. Bozza, Tobias C. Hinse, Jean Surdej, Martin Burgdorf, Gaetano Scarpetta, Martin Dominik, J. Skottfelt, C. Liebig, Gernot Maier, U. G. Jørgensen, M. Glitrup, Barry Smalley, Massimo Dall'Ora, and Colin Snodgrass

Subjects
Physics, Telescope, Photometry (astronomy), Space and Planetary Science, law, Astronomy, Astronomy and Astrophysics, Planetary system, law.invention
Published
2010
Full Text
View/download PDF

20. Large Magellanic Cloud self-lensing for OGLE-II microlensing observations

Author

Lukasz Wyrzykowski, S. Calchi Novati, Luigi Mancini, and Gaetano Scarpetta

Subjects
Physics, 010308 nuclear & particles physics, Astronomy and Astrophysics, Astrophysics, Gravitational microlensing, 01 natural sciences, Settore FIS/05 - Astronomia e Astrofisica, Likelihood analysis, Space and Planetary Science, 0103 physical sciences, Optical depth (astrophysics), Halo, Large Magellanic Cloud, 010303 astronomy & astrophysics, Mass fraction
Abstract

In the framework of microlensing searches towards the Large Magellanic Cloud (LMC), we discuss the results presented by the OGLE collaboration for their OGLE-II campaign \citep{lukas09}. We evaluate the optical depth, the duration and the expected rate of events for the different possible lens populations: both luminous, dominated by the LMC self lensing, and "dark", the would be compact halo objects (MACHOs) belonging to either the Galactic or to the LMC halo. The OGLE-II observational results, 2 microlensing candidate events located in the LMC bar region with duration of 24.2 and 57.2 days, compare well with the expected signal from the luminous lens populations: $n_\mathrm{exp}=1.5$, with typical duration, for LMC self lensing, of about 50 days. Because of the small statistics at disposal, however, the conclusions that can be drawn as for the halo mass fraction, $f$, in form of compact halo objects are not too severe. By means of a likelihood analysis we find an \emph{upper} limit for $f$, at 95% confidence level, of about 15% in the mass range $(10^{-2}-10^{-1}) \mathrm{M}_\odot$ and 26% for $0.5 \mathrm{M}_\odot$.

Published
2009
Full Text
View/download PDF

21. The POINT-AGAPE survey - II. An unrestricted search for microlensing events towards M31

Author

Paul C. Hewett, Jin H. An, Yiannis Tsapras, E. Kerins, P. Baillon, Nick Evans, Bernard Carr, M. Creze, C. S. Stalin, M. J. Weston, S. Paulin-Henriksson, S. Calchi Novati, Ph. Jetzer, Stephen J. Smartt, J. Kaplan, Y. Giraud-Heraud, Andrew Gould, and Vasily Belokurov

Subjects
Physics, 010308 nuclear & particles physics, Astronomy and Astrophysics, Astrophysics, Gravitational microlensing, Light curve, 01 natural sciences, Monitoring program, Variable (computer science), Gravitational lens, Space and Planetary Science, 0103 physical sciences, Variable star, 010303 astronomy & astrophysics, Algorithm, Selection (genetic algorithm), Event (probability theory)
Abstract

An automated search is carried out for microlensing events using a catalogue of 44554 variable superpixel lightcurves derived from our three-year monitoring program of M31. Each step of our candidate selection is objective and reproducible by a computer. Our search is unrestricted, in the sense that it has no explicit timescale cut. So, it must overcome the awkward problem of distinguishing long-timescale microlensing events fro m long-period stellar variables. The basis of the selection algorithm is the fitting of the supe rpixel lightcurves to two different theoretical models, using variable star and blended microlensing templates. Only if microlensing is preferred is an event retained as a possible ca ndidate. Further cuts are made with

Published
2005
Full Text
View/download PDF

22. Classical novae from the POINT-AGAPE microlensing survey of M31 - I. The nova catalogue

Author

Yiannis Tsapras, Paul C. Hewett, Stephen J. Smartt, Andrew Gould, Nick Evans, A. M. Newsam, Bernard Carr, S. Paulin-Henriksson, M. Creze, Y. Giraud-Heraud, C. S. Stalin, Ph. Jetzer, Jin H. An, P. Baillon, Michael F. Bode, M. J. Darnley, J. Kaplan, E. Kerins, S. Calchi Novati, Physique Corpusculaire et Cosmologie - Collège de France (PCC), Collège de France (CdF (institution))-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), University of Zurich, and Darnley, M J

Subjects
Astrophysics and Astronomy, Andromeda Galaxy, 530 Physics, Population, FOS: Physical sciences, Astrophysics, Gravitational microlensing, 142-005 142-005, 01 natural sciences, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], 1912 Space and Planetary Science, Bulge, 0103 physical sciences, Range (statistics), Point (geometry), education, 010303 astronomy & astrophysics, Physics, education.field_of_study, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Astrophysics (astro-ph), Astronomy and Astrophysics, Nova (rocket), Space and Planetary Science, 3103 Astronomy and Astrophysics, Variable star
Abstract

The POINT-AGAPE survey is an optical search for gravitational microlensing events towards the Andromeda Galaxy (M31). As well as microlensing, the survey is sensitive to many different classes of variable stars and transients. Here we describe the automated detection and selection pipeline used to identify M31 classical novae (CNe) and we present the resulting catalogue of 20 CN candidates observed over three seasons. CNe are observed both in the bulge region as well as over a wide area of the M31 disk. Nine of the CNe are caught during the final rise phase and all are well sampled in at least two colours. The excellent light-curve coverage has allowed us to detect and classify CNe over a wide range of speed class, from very fast to very slow. Among the light-curves is a moderately fast CN exhibiting entry into a deep transition minimum, followed by its final decline. We have also observed in detail a very slow CN which faded by only 0.01 mag day$^{-1}$ over a 150 day period. We detect other interesting variable objects, including one of the longest period and most luminous Mira variables. The CN catalogue constitutes a uniquely well-sampled and objectively-selected data set with which to study the statistical properties of classical novae in M31, such as the global nova rate, the reliability of novae as standard-candle distance indicators and the dependence of the nova population on stellar environment. The findings of this statistical study will be reported in a follow-up paper., 21 pages, 13 figures, re-submitted for publication in MNRAS, typos corrected, references updated, figures 5-9 made clearer

Published
2004
Full Text
View/download PDF

23. Orbital alignment and star-spot properties in the WASP-52 planetary system

Author

Mancini, L., primary, Southworth, J., additional, Raia, G., additional, Tregloan-Reed, J., additional, Mollière, P., additional, Bozza, V., additional, Bretton, M., additional, Bruni, I., additional, Ciceri, S., additional, D'Ago, G., additional, Dominik, M., additional, Hinse, T. C., additional, Hundertmark, M., additional, Jørgensen, U. G., additional, Korhonen, H., additional, Rabus, M., additional, Rahvar, S., additional, Starkey, D., additional, Calchi Novati, S., additional, Figuera Jaimes, R., additional, Henning, Th., additional, Juncher, D., additional, Haugbølle, T., additional, Kains, N., additional, Popovas, A., additional, Schmidt, R. W., additional, Skottfelt, J., additional, Snodgrass, C., additional, Surdej, J., additional, and Wertz, O., additional

Published
2016
Full Text
View/download PDF

24. High-precision photometry by telescope defocussing – VIII. WASP-22, WASP-41, WASP-42 and WASP-55

Author

Southworth, John, primary, Tregloan-Reed, J., additional, Andersen, M. I., additional, Calchi Novati, S., additional, Ciceri, S., additional, Colque, J. P., additional, D'Ago, G., additional, Dominik, M., additional, Evans, D. F., additional, Gu, S.-H., additional, Herrera-Cordova, A., additional, Hinse, T. C., additional, Jørgensen, U. G., additional, Juncher, D., additional, Kuffmeier, M., additional, Mancini, L., additional, Peixinho, N., additional, Popovas, A., additional, Rabus, M., additional, Skottfelt, J., additional, Tronsgaard, R., additional, Unda-Sanzana, E., additional, Wang, X.-B., additional, Wertz, O., additional, Alsubai, K. A., additional, Andersen, J. M., additional, Bozza, V., additional, Bramich, D. M., additional, Burgdorf, M., additional, Damerdji, Y., additional, Diehl, C., additional, Elyiv, A., additional, Figuera Jaimes, R., additional, Haugbølle, T., additional, Hundertmark, M., additional, Kains, N., additional, Kerins, E., additional, Korhonen, H., additional, Liebig, C., additional, Mathiasen, M., additional, Penny, M. T., additional, Rahvar, S., additional, Scarpetta, G., additional, Schmidt, R. W., additional, Snodgrass, C., additional, Starkey, D., additional, Surdej, J., additional, Vilela, C., additional, Essen, C. von, additional, and Wang, Y., additional

Published
2016
Full Text
View/download PDF

25. Physical properties of the planetary systems WASP-45 and WASP-46 from simultaneous multiband photometry

Author

Ciceri, S., primary, Mancini, L., additional, Southworth, J., additional, Lendl, M., additional, Tregloan-Reed, J., additional, Brahm, R., additional, Chen, G., additional, D'Ago, G., additional, Dominik, M., additional, Figuera Jaimes, R., additional, Galianni, P., additional, Harpsøe, K., additional, Hinse, T. C., additional, Jørgensen, U. G., additional, Juncher, D., additional, Korhonen, H., additional, Liebig, C., additional, Rabus, M., additional, Bonomo, A. S., additional, Bott, K., additional, Henning, Th., additional, Jordán, A., additional, Sozzetti, A., additional, Alsubai, K. A., additional, Andersen, J. M., additional, Bajek, D., additional, Bozza, V., additional, Bramich, D. M., additional, Browne, P., additional, Calchi Novati, S., additional, Damerdji, Y., additional, Diehl, C., additional, Elyiv, A., additional, Giannini, E., additional, Gu, S-H., additional, Hundertmark, M., additional, Kains, N., additional, Penny, M., additional, Popovas, A., additional, Rahvar, S., additional, Scarpetta, G., additional, Schmidt, R. W., additional, Skottfelt, J., additional, Snodgrass, C., additional, Surdej, J., additional, Vilela, C., additional, Wang, X.-B., additional, and Wertz, O., additional

Published
2015
Full Text
View/download PDF

26. Larger and faster: revised properties and a shorter orbital period for the WASP-57 planetary system from a pro-am collaboration

Author

Southworth, John, primary, Mancini, L., additional, Tregloan-Reed, J., additional, Calchi Novati, S., additional, Ciceri, S., additional, D'Ago, G., additional, Delrez, L., additional, Dominik, M., additional, Evans, D. F., additional, Gillon, M., additional, Jehin, E., additional, Jørgensen, U. G., additional, Haugbølle, T., additional, Lendl, M., additional, Arena, C., additional, Barbieri, L., additional, Barbieri, M., additional, Corfini, G., additional, Lopresti, C., additional, Marchini, A., additional, Marino, G., additional, Alsubai, K. A., additional, Bozza, V., additional, Bramich, D. M., additional, Jaimes, R. Figuera, additional, Hinse, T. C., additional, Henning, Th., additional, Hundertmark, M., additional, Juncher, D., additional, Korhonen, H., additional, Popovas, A., additional, Rabus, M., additional, Rahvar, S., additional, Schmidt, R. W., additional, Skottfelt, J., additional, Snodgrass, C., additional, Starkey, D., additional, Surdej, J., additional, and Wertz, O., additional

Published
2015
Full Text
View/download PDF

27. Transits and starspots in the WASP-6 planetary system

Author

Tregloan-Reed, Jeremy, primary, Southworth, John, additional, Burgdorf, M., additional, Novati, S. Calchi, additional, Dominik, M., additional, Finet, F., additional, Jørgensen, U. G., additional, Maier, G., additional, Mancini, L., additional, Prof, S., additional, Ricci, D., additional, Snodgrass, C., additional, Bozza, V., additional, Browne, P., additional, Dodds, P., additional, Gerner, T., additional, Harpsøe, K., additional, Hinse, T. C., additional, Hundertmark, M., additional, Kains, N., additional, Kerins, E., additional, Liebig, C., additional, Penny, M. T., additional, Rahvar, S., additional, Sahu, K., additional, Scarpetta, G., additional, Schäfer, S., additional, Schönebeck, F., additional, Skottfelt, J., additional, and Surdej, J., additional

Published
2015
Full Text
View/download PDF

28. High-precision photometry by telescope defocusing – VII. The ultrashort period planet WASP-103★

Author

Southworth, John, primary, Mancini, L., additional, Ciceri, S., additional, Budaj, J., additional, Dominik, M., additional, Figuera Jaimes, R., additional, Haugbølle, T., additional, Jørgensen, U. G., additional, Popovas, A., additional, Rabus, M., additional, Rahvar, S., additional, von Essen, C., additional, Schmidt, R. W., additional, Wertz, O., additional, Alsubai, K. A., additional, Bozza, V., additional, Bramich, D. M., additional, Calchi Novati, S., additional, D'Ago, G., additional, Hinse, T. C., additional, Henning, Th., additional, Hundertmark, M., additional, Juncher, D., additional, Korhonen, H., additional, Skottfelt, J., additional, Snodgrass, C., additional, Starkey, D., additional, and Surdej, J., additional

Published
2014
Full Text
View/download PDF

30. ExELS: an exoplanet legacy science proposal for the ESA Euclid mission - II. Hot exoplanets and sub-stellar systems

Author

McDonald, I., primary, Kerins, E., additional, Penny, M., additional, Beaulieu, J.- P., additional, Batista, V., additional, Calchi Novati, S., additional, Cassan, A., additional, Fouque, P., additional, Mao, S., additional, Marquette, J. B., additional, Rattenbury, N., additional, Robin, A. C., additional, Tisserand, P., additional, and Zapatero Osorio, M. R., additional

Published
2014
Full Text
View/download PDF

31. High-precision photometry by telescope defocussing – VI. WASP-24, WASP-25 and WASP-26★

Author

Southworth, John, primary, Hinse, T. C., additional, Burgdorf, M., additional, Calchi Novati, S., additional, Dominik, M., additional, Galianni, P., additional, Gerner, T., additional, Giannini, E., additional, Gu, S.-H., additional, Hundertmark, M., additional, Jørgensen, U. G., additional, Juncher, D., additional, Kerins, E., additional, Mancini, L., additional, Rabus, M., additional, Ricci, D., additional, Schäfer, S., additional, Skottfelt, J., additional, Tregloan-Reed, J., additional, Wang, X.-B., additional, Wertz, O., additional, Alsubai, K. A., additional, Andersen, J. M., additional, Bozza, V., additional, Bramich, D. M., additional, Browne, P., additional, Ciceri, S., additional, D'Ago, G., additional, Damerdji, Y., additional, Diehl, C., additional, Dodds, P., additional, Elyiv, A., additional, Fang, X.-S., additional, Finet, F., additional, Figuera Jaimes, R., additional, Hardis, S., additional, Harpsøe, K., additional, Jessen-Hansen, J., additional, Kains, N., additional, Kjeldsen, H., additional, Korhonen, H., additional, Liebig, C., additional, Lund, M. N., additional, Lundkvist, M., additional, Mathiasen, M., additional, Penny, M. T., additional, Popovas, A., additional, Prof., S., additional, Rahvar, S., additional, Sahu, K., additional, Scarpetta, G., additional, Schmidt, R. W., additional, Schönebeck, F., additional, Snodgrass, C., additional, Street, R. A., additional, Surdej, J., additional, Tsapras, Y., additional, and Vilela, C., additional

Published
2014
Full Text
View/download PDF

32. Physical properties, transmission and emission spectra of the WASP-19 planetary system from multi-colour photometry★

Author

Mancini, L., primary, Ciceri, S., additional, Chen, G., additional, Tregloan-Reed, J., additional, Fortney, J. J., additional, Southworth, J., additional, Tan, T. G., additional, Burgdorf, M., additional, Calchi Novati, S., additional, Dominik, M., additional, Fang, X.-S., additional, Finet, F., additional, Gerner, T., additional, Hardis, S., additional, Hinse, T. C., additional, Jørgensen, U. G., additional, Liebig, C., additional, Nikolov, N., additional, Ricci, D., additional, Schäfer, S., additional, Schönebeck, F., additional, Skottfelt, J., additional, Wertz, O., additional, Alsubai, K. A., additional, Bozza, V., additional, Browne, P., additional, Dodds, P., additional, Gu, S.-H., additional, Harpsøe, K., additional, Henning, Th., additional, Hundertmark, M., additional, Jessen-Hansen, J., additional, Kains, N., additional, Kerins, E., additional, Kjeldsen, H., additional, Lund, M. N., additional, Lundkvist, M., additional, Madhusudhan, N., additional, Mathiasen, M., additional, Penny, M. T., additional, Prof, S., additional, Rahvar, S., additional, Sahu, K., additional, Scarpetta, G., additional, Snodgrass, C., additional, and Surdej, J., additional

Published
2013
Full Text
View/download PDF

34. A detailed census of variable stars in the globular cluster NGC 6333 (M9) from CCD differential photometry★

Author

Arellano Ferro, A., primary, Bramich, D. M., additional, Figuera Jaimes, R., additional, Giridhar, Sunetra, additional, Kains, N., additional, Kuppuswamy, K., additional, Jørgensen, U. G., additional, Alsubai, K. A., additional, Andersen, J. M., additional, Bozza, V., additional, Browne, P., additional, Calchi Novati, S., additional, Damerdji, Y., additional, Diehl, C., additional, Dominik, M., additional, Dreizler, S., additional, Elyiv, A., additional, Giannini, E., additional, Harpsøe, K., additional, Hessman, F. V., additional, Hinse, T. C., additional, Hundertmark, M., additional, Juncher, D., additional, Kerins, E., additional, Korhonen, H., additional, Liebig, C., additional, Mancini, L., additional, Mathiasen, M., additional, Penny, M. T., additional, Rabus, M., additional, Rahvar, S., additional, Ricci, D., additional, Scarpetta, G., additional, Skottfelt, J., additional, Snodgrass, C., additional, Southworth, J., additional, Surdej, J., additional, Tregloan-Reed, J., additional, Vilela, C., additional, and Wertz, O., additional

Published
2013
Full Text
View/download PDF

35. ExELS: an exoplanet legacy science proposal for the ESA Euclid mission – I. Cold exoplanets

Author

Penny, M. T., primary, Kerins, E., additional, Rattenbury, N., additional, Beaulieu, J.-P., additional, Robin, A. C., additional, Mao, S., additional, Batista, V., additional, Calchi Novati, S., additional, Cassan, A., additional, Fouqué, P., additional, McDonald, I., additional, Marquette, J. B., additional, Tisserand, P., additional, and Zapatero Osorio, M. R., additional

Published
2013
Full Text
View/download PDF

36. High-precision photometry by telescope defocusing – V. WASP-15 and WASP-16★

Author

Southworth, John, primary, Mancini, L., additional, Browne, P., additional, Burgdorf, M., additional, Calchi Novati, S., additional, Dominik, M., additional, Gerner, T., additional, Hinse, T. C., additional, Jørgensen, U. G., additional, Kains, N., additional, Ricci, D., additional, Schäfer, S., additional, Schönebeck, F., additional, Tregloan-Reed, J., additional, Alsubai, K. A., additional, Bozza, V., additional, Chen, G., additional, Dodds, P., additional, Dreizler, S., additional, Fang, X.-S., additional, Finet, F., additional, Gu, S.-H., additional, Hardis, S., additional, Harpsøe, K., additional, Henning, Th., additional, Hundertmark, M., additional, Jessen-Hansen, J., additional, Kerins, E., additional, Kjeldsen, H., additional, Liebig, C., additional, Lund, M. N., additional, Lundkvist, M., additional, Mathiasen, M., additional, Nikolov, N., additional, Penny, M. T., additional, Proft, S., additional, Rahvar, S., additional, Sahu, K., additional, Scarpetta, G., additional, Skottfelt, J., additional, Snodgrass, C., additional, Surdej, J., additional, and Wertz, O., additional

Published
2013
Full Text
View/download PDF

37. High-precision photometry by telescope defocussing - VIII.WASP-22, WASP-41,WASP-42 and WASP-55.

Author

Southworth, John, Tregloan-Reed, J., Andersen, M. I., Novati, S. Calchi, Ciceri, S., Colque, J. P., D'Ago, G., Dominik, M., Evans, D. F., Gu, S.-H., Herrera-Cordova, A., Hinse, T. C., Jørgensen, U. G., Juncher, D., Kuffmeier, M., Mancini, L., Peixinho, N., Popovas, A., Rabus, M., and Skottfelt, J.

Subjects
ASTRONOMICAL photometry, ASTRONOMICAL observations, PLANETARY orbits, LIGHT curves, TELESCOPES
Abstract

We present 13 high-precision and four additional light curves of four bright southernhemisphere 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-55 b is the most discrepant with a mass of 0.63MJup 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 λ = 6 ± 11°. 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. [ABSTRACT FROM AUTHOR]

Published
2016
Full Text
View/download PDF

39. High-precision photometry by telescope defocusing - IV. Confirmation of the huge radius of WASP-17 b

Author

Southworth, John, primary, Hinse, T. C., additional, Dominik, M., additional, Fang, X.-S., additional, Harpsøe, K., additional, Jørgensen, U. G., additional, Kerins, E., additional, Liebig, C., additional, Mancini, L., additional, Skottfelt, J., additional, Anderson, D. R., additional, Smalley, B., additional, Tregloan-Reed, J., additional, Wertz, O., additional, Alsubai, K. A., additional, Bozza, V., additional, Calchi Novati, S., additional, Dreizler, S., additional, Gu, S.-H., additional, Hundertmark, M., additional, Jessen-Hansen, J., additional, Kains, N., additional, Kjeldsen, H., additional, Lund, M. N., additional, Lundkvist, M., additional, Mathiasen, M., additional, Penny, M. T., additional, Rahvar, S., additional, Ricci, D., additional, Scarpetta, G., additional, Snodgrass, C., additional, and Surdej, J., additional

Published
2012
Full Text
View/download PDF

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

Author

Bozza, V., primary, Dominik, M., additional, Rattenbury, N. J., additional, Jørgensen, U. G., additional, Tsapras, Y., additional, Bramich, D. M., additional, Udalski, A., additional, Bond, I. A., additional, Liebig, C., additional, Cassan, A., additional, Fouqué, P., additional, Fukui, A., additional, Hundertmark, M., additional, Shin, I.-G., additional, Lee, S. H., additional, Choi, J.-Y., additional, Park, S.-Y., additional, Gould, A., additional, Allan, A., additional, Mao, S., additional, Wyrzykowski, Ł., additional, Street, R. A., additional, Buckley, D., additional, Nagayama, T., additional, Mathiasen, M., additional, Hinse, T. C., additional, Novati, S. Calchi, additional, Harpsøe, K., additional, Mancini, L., additional, Scarpetta, G., additional, Anguita, T., additional, Burgdorf, M. J., additional, Horne, K., additional, Hornstrup, A., additional, Kains, N., additional, Kerins, E., additional, Kjaergaard, P., additional, Masi, G., additional, Rahvar, S., additional, Ricci, D., additional, Snodgrass, C., additional, Southworth, J., additional, Steele, I. A., additional, Surdej, J., additional, Thöne, C. C., additional, Wambsganss, J., additional, Zub, M., additional, Albrow, M. D., additional, Batista, V., additional, Beaulieu, J.-P., additional, Bennett, D. P., additional, Caldwell, J. A. R., additional, Cole, A. A., additional, Cook, K. H., additional, Coutures, C., additional, Dieters, S., additional, Prester, D. Dominis, additional, Donatowicz, J., additional, Greenhill, J., additional, Kane, S. R., additional, Kubas, D., additional, Marquette, J.-B., additional, Martin, R., additional, Menzies, J., additional, Pollard, K. R., additional, Sahu, K. C., additional, Williams, A., additional, Szymański, M. K., additional, Kubiak, M., additional, Pietrzyński, G., additional, Soszyński, I., additional, Poleski, R., additional, Ulaczyk, K., additional, DePoy, D. L., additional, Dong, Subo, additional, Han, C., additional, Janczak, J., additional, Lee, C.-U., additional, Pogge, R. W., additional, Abe, F., additional, Furusawa, K., additional, Hearnshaw, J. B., additional, Itow, Y., additional, Kilmartin, P. M., additional, Korpela, A. V., additional, Lin, W., additional, Ling, C. H., additional, Masuda, K., additional, Matsubara, Y., additional, Miyake, N., additional, Muraki, Y., additional, Ohnishi, K., additional, Perrott, Y. C., additional, Saito, To., additional, Skuljan, L., additional, Sullivan, D. J., additional, Sumi, T., additional, Suzuki, D., additional, Sweatman, W. L., additional, Tristram, P. J., additional, Wada, K., additional, Yock, P. C. M., additional, Gulbis, A., additional, Hashimoto, Y., additional, Kniazev, A., additional, and Vaisanen, P., additional

Published
2012
Full Text
View/download PDF

42. High-precision photometry by telescope defocusing - III. The transiting planetary system WASP-2★

Author

Southworth, John, primary, Mancini, L., additional, Novati, S. Calchi, additional, Dominik, M., additional, Glitrup, M., additional, Hinse, T. C., additional, Jørgensen, U. G., additional, Mathiasen, M., additional, Ricci, D., additional, Maier, G., additional, Zimmer, F., additional, Bozza, V., additional, Browne, P., additional, Bruni, I., additional, Burgdorf, M., additional, Dall’Ora, M., additional, Finet, F., additional, Harpsøe, K., additional, Hundertmark, M., additional, Liebig, C., additional, Rahvar, S., additional, Scarpetta, G., additional, Skottfelt, J., additional, Smalley, B., additional, Snodgrass, C., additional, and Surdej, J., additional

Published
2010
Full Text
View/download PDF

44. High-precision photometry by telescope defocussing - II. The transiting planetary system WASP-4

Author

Southworth, John, primary, Hinse, T. C., additional, Burgdorf, M. J., additional, Dominik, M., additional, Hornstrup, A., additional, Jørgensen, U. G., additional, Liebig, C., additional, Ricci, D., additional, Thöne, C. C., additional, Anguita, T., additional, Bozza, V., additional, Novati, S. Calchi, additional, Harpsøe, K., additional, Mancini, L., additional, Masi, G., additional, Mathiasen, M., additional, Rahvar, S., additional, Scarpetta, G., additional, Snodgrass, C., additional, Surdej, J., additional, and Zub, M., additional

Published
2009
Full Text
View/download PDF

46. High-precision photometry by telescope defocusing - I. The transiting planetary system WASP-5

Author

Southworth, John, primary, Hinse, T. C., additional, Jørgensen, U. G., additional, Dominik, M., additional, Ricci, D., additional, Burgdorf, M. J., additional, Hornstrup, A., additional, Wheatley, P. J., additional, Anguita, T., additional, Bozza, V., additional, Novati, S. Calchi, additional, Harpsøe, K., additional, Kjaergaard, P., additional, Liebig, C., additional, Mancini, L., additional, Masi, G., additional, Mathiasen, M., additional, Rahvar, S., additional, Scarpetta, G., additional, Snodgrass, C., additional, Surdej, J., additional, Thöne, C. C., additional, and Zub, M., additional

Published
2009
Full Text
View/download PDF

47. High-precision photometry by telescope defocusing - VII. The ultrashort period planetWASP-103.

Author

Southworth, John, Mancini, L., Ciceri, S., Budaj, J., Dominik, M., Jaimes, R. Figuera, Haugbølle, T., Jørgensen, U. G., Popovas, A., Rabus, M., Rahvar, S., von Essen, C., Schmidt, R. W., Wertz, O., Alsubai, K. A., Bozza, V., Bramich, D. M., Novati, S. Calchi, D'Ago, G., and Hinse, T. C.

Subjects
ASTRONOMICAL photometry, TELESCOPES, ULTRASHORT laser pulses, STELLAR evolution, RAYLEIGH scattering, IMAGE analysis
Abstract

We present 17 transit light curves of the ultrashort period planetary system WASP-103, a strong candidate for the detection of tidally-induced orbital decay. We use these to establish a high-precision reference epoch for transit timing studies. The time of the reference transit mid-point is now measured to an accuracy of 4.8 s, versus 67.4 s in the discovery paper, aiding future searches for orbital decay. With the help of published spectroscopic measurements and theoretical stellar models, we determine the physical properties of the system to high precision and present a detailed error budget for these calculations. The planet has a Roche lobe filling factor of 0.58, leading to a significant asphericity; we correct its measured mass and mean density for this phenomenon. A high-resolution Lucky Imaging observation shows no evidence for faint stars close enough to contaminate the point spread function of WASP-103. Our data were obtained in the Bessell RI and the SDSS griz passbands and yield a larger planet radius at bluer optical wavelengths, to a confidence level of 7.3σ. Interpreting this as an effect of Rayleigh scattering in the planetary atmosphere leads to a measurement of the planetary mass which is too small by a factor of 5, implying that Rayleigh scattering is not the main cause of the variation of radius with wavelength. [ABSTRACT FROM AUTHOR]

Published
2015
Full Text
View/download PDF

48. Measuring polarization in microlensing events.

Author

Ingrosso, G., Calchi Novati, S., De Paolis, F., Jetzer, Ph., Nucita, A. A., and Strafella, F.

Subjects
*MICROLENSING (Astrophysics), *POLARIZATION (Nuclear physics), *GIANT stars, *MAGNIFICATION (Optics), *PHOTON scattering, *STELLAR winds
Abstract

We reconsider the polarization of the star light that may arise during microlensing events due to the high gradient of magnification across the atmosphere of the source star, by exploring the full range of microlensing and stellar physical parameters. Since it is already known that only cool evolved giant stars give rise to the highest polarization signals, we follow the model by Simmons et al. to compute the polarization as due to the photon scattering on dust grains in the stellar wind. Motivated by the possibility to perform a polarization measurement during an ongoing microlensing event, we consider the recently reported event catalogue by the Optical Gravitational Lensing Experiment (OGLE)collaboration covering the 2001–2009 campaigns (OGLE-III events), that makes available the largest and more comprehensive set of single-lens microlensing events towards the Galactic bulge. The study of these events, integrated by a Monte Carlo analysis, allows us to estimate the expected polarization profiles and to predict for which source stars and at which time is most convenient to perform a polarization measurement in an ongoing event. We find that about two dozens of OGLE-III events (about 1 per cent of the total) have maximum polarization degree in the range 0.1 < Pmax < 1 per cent, corresponding to source stars with apparent magnitude I ≲ 14.5, being very cool red giants. This signal is measurable by using the FOcal Reducer and low dispersion Spectrograph (FORS2) polarimeter at Very Large Telescope (VLT) telescope with about 1 h integration time. [ABSTRACT FROM AUTHOR]

Published
2015
Full Text
View/download PDF

49. Classical novae from the POINT–AGAPE microlensing survey of M31 – II. Rate and statistical characteristics of the nova population

Author

Darnley, M. J., primary, Bode, M. F., additional, Kerins, E., additional, Newsam, A. M., additional, An, J., additional, Baillon, P., additional, Belokurov, V., additional, Novati, S. Calchi, additional, Carr, B. J., additional, Crézé, M., additional, Evans, N. W., additional, Giraud-Héraud, Y., additional, Gould, A., additional, Hewett, P., additional, Jetzer, Ph., additional, Kaplan, J., additional, Paulin-Henriksson, S., additional, Smartt, S. J., additional, Tsapras, Y., additional, and Weston, M., additional

Published
2006
Full Text
View/download PDF

50. Classical novae from the POINT-AGAPE microlensing survey of M31 - I. The nova catalogue

Author

Darnley, M. J., primary, Bode, M. F., additional, Kerins, E., additional, Newsam, A. M., additional, An, J., additional, Baillon, P., additional, Novati, S. Calchi, additional, Carr, B. J., additional, Crézé, M., additional, Evans, N. W., additional, Giraud-Héraud, Y., additional, Gould, A., additional, Hewett, P., additional, Jetzer, Ph., additional, Kaplan, J., additional, Paulin-Henriksson, S., additional, Smartt, S. J., additional, Stalin, C. S., additional, and Tsapras, Y., additional

Published
2004
Full Text
View/download PDF

Catalog

Books, media, physical & digital resources
See catalog results