Physical properties of the planetary systemsWASP-45 and WASP-46 from simultaneous multiband photometry

被引:18
作者
Ciceri, S. [1 ]
Mancini, L. [1 ,2 ]
Southworth, J. [3 ]
Lendl, M. [4 ,5 ]
Tregloan-Reed, J. [3 ,6 ]
Brahm, R. [7 ,8 ]
Chen, G. [9 ,10 ]
D'Ago, G. [11 ,12 ,13 ]
Dominik, M. [14 ]
Jaimes, R. Figuera [13 ,15 ]
Galianni, P. [13 ]
Harpsoe, K. [16 ,17 ]
Hinse, T. C. [18 ]
Jorgensen, U. G. [15 ]
Juncher, D. [15 ]
Korhonen, H. [15 ,19 ]
Liebig, C. [13 ]
Rabus, M. [1 ]
Bonomo, A. S. [2 ]
Bott, K. [20 ,21 ]
Henning, Th [1 ]
Jordan, A. [7 ,8 ]
Sozzetti, A. [2 ]
Alsubai, K. A. [22 ]
Andersen, J. M. [15 ,23 ]
Bajek, D. [13 ]
Bozza, V.
Bramich, D. M. [21 ]
Browne, P. [13 ]
Novati, S. Calchi [11 ,12 ,24 ]
Damerdji, Y. [25 ]
Diehl, C. [26 ,27 ]
Elyiv, A. [24 ,28 ,29 ]
Giannini, E. [25 ]
Gu, S-H. [30 ,31 ]
Hundertmark, M. [15 ]
Kains, N. [32 ]
Penny, M. [15 ,33 ]
Popovas, A. [15 ]
Rahvar, S. [34 ]
Scarpetta, G. [11 ,12 ,23 ]
Schmidt, R. W. [25 ]
Skottfelt, J. [15 ,35 ]
Snodgrass, C. [36 ,37 ]
Surdej, J. [24 ]
Vilela, C. [3 ]
Wang, X-B. [29 ,30 ]
Wertz, O. [24 ]
机构
[1] Max Planck Inst Astron, D-69117 Heidelberg, Germany
[2] Osserv Astron Torino, INAF, I-10025 Pino Torinese, Italy
[3] Keele Univ, Astrophys Grp, Keele ST5 5BG, Staffs, England
[4] Austrian Acad Sci, Space Res Inst, A-8042 Graz, Austria
[5] Univ Geneva, Observ Geneva, CH-1290 Sauverny, Switzerland
[6] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA
[7] Pontificia Univ Catolica Chile, Inst Astrofis, Santiago 7820436, Chile
[8] Millennium Inst Astrophys, Santiago 7820436, Chile
[9] Chinese Acad Sci, Purple Mt Observ, Key Lab Planetary Sci, Nanjing 210008, Jiangsu, Peoples R China
[10] Inst Astrofis Canarias, E-38205 Tenerife, Spain
[11] Int Inst Adv Sci Studies IIASS, I-84019 Vietri Sul Mare, SA, Italy
[12] Univ Salerno, Dept Phys ER Caianiello, Fisciano 84084, SA, Italy
[13] Ist Nazl Fis Nucl, Sez Napoli, I-80126 Naples, Italy
[14] Univ St Andrews, SUPA, Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland
[15] European So Observ, D-85748 Garching, Germany
[16] Univ Copenhagen, Niels Bohr Inst, DK-1350 Copenhagen K, Denmark
[17] Univ Copenhagen, Ctr Star & Planet Format, DK-1350 Copenhagen K, Denmark
[18] Korea Astron & Space Sci Inst, Daejeon 305348, South Korea
[19] Univ Turku, Finnish Ctr Astron ESO FINCA, FI-21500 Piikkio, Finland
[20] Univ New S Wales, Sch Phys, Sydney, NSW 2052, Australia
[21] Univ New S Wales, Australian Ctr Astrobiol, Sydney, NSW 2052, Australia
[22] Qatar Fdn, Qatar Environm & Energy Res Inst, Doha, Qatar
[23] Boston Univ, Dept Astron, Boston, MA 02215 USA
[24] CALTECH, NASA Exoplanet Sci Inst, Pasadena, CA 91125 USA
[25] Univ Liege, Inst Astrophys & Geophys, B-4000 Liege, Belgium
[26] Heidelberg Univ, Zentrum Astron, Astron Rech Inst, D-69120 Heidelberg, Germany
[27] Univ Hamburg, Hamburger Sternwarte, D-21029 Hamburg, Germany
[28] Univ Bologna, Dipartimento Fis & Astron, I-40127 Bologna, Italy
[29] Natl Acad Sci Ukraine, Main Astron Observ, UA-03680 Kiev, Ukraine
[30] Chinese Acad Sci, Yunnan Observ, Kunming 650011, Peoples R China
[31] Chinese Acad Sci, Key Lab Struct & Evolut Celestial Objects, Kunming 650011, Peoples R China
[32] Space Telescope Sci Inst, Baltimore, MD 21218 USA
[33] Ohio State Univ, Dept Astron, McPherson Lab, Columbus, OH 43210 USA
[34] Sharif Univ Technol, Dept Phys, Tehran, Iran
[35] Open Univ, Ctr Elect Imaging, Dept Phys Sci, Milton Keynes MK7 6AA, Bucks, England
[36] Open Univ, Dept Phys Sci, Planetary & Space Sci, Milton Keynes MK7 6AA, Bucks, England
[37] Max Planck Inst Solar Syst Res, D-37077 Gottingen, Germany
基金
中国国家自然科学基金;
关键词
planets and satellites: fundamental parameters; stars: fundamental parameters; stars: individual: WASP-45; stars: individual: WASP-46; TRANSITING EXTRASOLAR PLANETS; STELLAR EVOLUTION DATABASE; HIGH-PRECISION PHOTOMETRY; LIMB-DARKENING LAW; LIGHT-CURVE; TRANSMISSION SPECTRA; ATMOSPHERE MODELS; SURFACE GRAVITIES; LOW-MASS; TELESCOPE;
D O I
10.1093/mnras/stv2698
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
Accurate measurements of the physical characteristics of a large number of exoplanets are useful to strongly constrain theoretical models of planet formation and evolution, which lead to the large variety of exoplanets and planetary-system configurations that have been observed. We present a study of the planetary systems WASP-45 and WASP-46, both composed of a main-sequence star and a close-in hot Jupiter, based on 29 new high-quality light curves of transits events. In particular, one transit of WASP-45 b and four of WASP-46 b were simultaneously observed in four optical filters, while one transit of WASP-46 b was observed with the NTT obtaining a precision of 0.30 mmag with a cadence of roughly 3 min. We also obtained five new spectra of WASP-45 with the FEROS spectrograph. We improved by a factor of 4 the measurement of the radius of the planet WASP-45 b, and found that WASP-46 b is slightly less massive and smaller than previously reported. Both planets now have a more accurate measurement of the density (0.959 +/- 0.077 rho Jup instead of 0.64 +/- 0.30 rho Jup for WASP-45 b, and 1.103 +/- 0.052 rho Jup instead of 0.94 +/- 0.11 rho Jup for WASP-46 b). We tentatively detected radius variations with wavelength for both planets, in particular in the case of WASP-45 b we found a slightly larger absorption in the redder bands than in the bluer ones. No hints for the presence of an additional planetary companion in the two systems were found either from the photometric or radial velocity measurements.
引用
收藏
页码:990 / 1002
页数:13
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