Physical Properties of the 0.94-Day Period Transiting Planetary System WASP-18
We present high-precision photometry of five consecutive transits of WASP-18, an extrasolar planetary system with one of the shortest orbital periods known. Through the use of telescope defocusing we achieve a photometric precision of 0.47-0.83 mmag per observation over complete transit events. The...
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| Veröffentlicht in: | The Astrophysical journal 2009-12, Vol.707 (1), p.167-172 |
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| creator | Southworth, John Hinse, T. C Dominik, M Glitrup, M Jørgensen, U. G Liebig, C Mathiasen, M Anderson, D. R Bozza, V Browne, P Burgdorf, M Calchi Novati, S Dreizler, S Finet, F Harpsøe, K Hessman, F Hundertmark, M Maier, G Mancini, L Maxted, P. F. L Rahvar, S Ricci, D Scarpetta, G Skottfelt, J Snodgrass, C Surdej, J Zimmer, F |
| description | We present high-precision photometry of five consecutive transits of WASP-18, an extrasolar planetary system with one of the shortest orbital periods known. Through the use of telescope defocusing we achieve a photometric precision of 0.47-0.83 mmag per observation over complete transit events. The data are analyzed using the JKTEBOP code and three different sets of stellar evolutionary models. We find the mass and radius of the planet to be M b = 10.43 +/- 0.30 +/- 0.24 M Jup and R b = 1.165 +/- 0.055 +/- 0.014 R Jup (statistical and systematic errors), respectively. The systematic errors in the orbital separation and the stellar and planetary masses, arising from the use of theoretical predictions, are of a similar size to the statistical errors and set a limit on our understanding of the WASP-18 system. We point out that seven of the nine known massive transiting planets (M b > 3 M Jup) have eccentric orbits, whereas significant orbital eccentricity has been detected for only four of the 46 less-massive planets. This may indicate that there are two different populations of transiting planets, but could also be explained by observational biases. Further radial velocity observations of low-mass planets will make it possible to choose between these two scenarios. |
| doi_str_mv | 10.1088/0004-637X/707/1/167 |
| format | Article |
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C ; Dominik, M ; Glitrup, M ; Jørgensen, U. G ; Liebig, C ; Mathiasen, M ; Anderson, D. R ; Bozza, V ; Browne, P ; Burgdorf, M ; Calchi Novati, S ; Dreizler, S ; Finet, F ; Harpsøe, K ; Hessman, F ; Hundertmark, M ; Maier, G ; Mancini, L ; Maxted, P. F. L ; Rahvar, S ; Ricci, D ; Scarpetta, G ; Skottfelt, J ; Snodgrass, C ; Surdej, J ; Zimmer, F</creator><creatorcontrib>Southworth, John ; Hinse, T. C ; Dominik, M ; Glitrup, M ; Jørgensen, U. G ; Liebig, C ; Mathiasen, M ; Anderson, D. R ; Bozza, V ; Browne, P ; Burgdorf, M ; Calchi Novati, S ; Dreizler, S ; Finet, F ; Harpsøe, K ; Hessman, F ; Hundertmark, M ; Maier, G ; Mancini, L ; Maxted, P. F. L ; Rahvar, S ; Ricci, D ; Scarpetta, G ; Skottfelt, J ; Snodgrass, C ; Surdej, J ; Zimmer, F</creatorcontrib><description>We present high-precision photometry of five consecutive transits of WASP-18, an extrasolar planetary system with one of the shortest orbital periods known. Through the use of telescope defocusing we achieve a photometric precision of 0.47-0.83 mmag per observation over complete transit events. The data are analyzed using the JKTEBOP code and three different sets of stellar evolutionary models. We find the mass and radius of the planet to be M b = 10.43 +/- 0.30 +/- 0.24 M Jup and R b = 1.165 +/- 0.055 +/- 0.014 R Jup (statistical and systematic errors), respectively. The systematic errors in the orbital separation and the stellar and planetary masses, arising from the use of theoretical predictions, are of a similar size to the statistical errors and set a limit on our understanding of the WASP-18 system. We point out that seven of the nine known massive transiting planets (M b > 3 M Jup) have eccentric orbits, whereas significant orbital eccentricity has been detected for only four of the 46 less-massive planets. This may indicate that there are two different populations of transiting planets, but could also be explained by observational biases. 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C</creatorcontrib><creatorcontrib>Dominik, M</creatorcontrib><creatorcontrib>Glitrup, M</creatorcontrib><creatorcontrib>Jørgensen, U. G</creatorcontrib><creatorcontrib>Liebig, C</creatorcontrib><creatorcontrib>Mathiasen, M</creatorcontrib><creatorcontrib>Anderson, D. R</creatorcontrib><creatorcontrib>Bozza, V</creatorcontrib><creatorcontrib>Browne, P</creatorcontrib><creatorcontrib>Burgdorf, M</creatorcontrib><creatorcontrib>Calchi Novati, S</creatorcontrib><creatorcontrib>Dreizler, S</creatorcontrib><creatorcontrib>Finet, F</creatorcontrib><creatorcontrib>Harpsøe, K</creatorcontrib><creatorcontrib>Hessman, F</creatorcontrib><creatorcontrib>Hundertmark, M</creatorcontrib><creatorcontrib>Maier, G</creatorcontrib><creatorcontrib>Mancini, L</creatorcontrib><creatorcontrib>Maxted, P. F. L</creatorcontrib><creatorcontrib>Rahvar, S</creatorcontrib><creatorcontrib>Ricci, D</creatorcontrib><creatorcontrib>Scarpetta, G</creatorcontrib><creatorcontrib>Skottfelt, J</creatorcontrib><creatorcontrib>Snodgrass, C</creatorcontrib><creatorcontrib>Surdej, J</creatorcontrib><creatorcontrib>Zimmer, F</creatorcontrib><title>Physical Properties of the 0.94-Day Period Transiting Planetary System WASP-18</title><title>The Astrophysical journal</title><description>We present high-precision photometry of five consecutive transits of WASP-18, an extrasolar planetary system with one of the shortest orbital periods known. Through the use of telescope defocusing we achieve a photometric precision of 0.47-0.83 mmag per observation over complete transit events. The data are analyzed using the JKTEBOP code and three different sets of stellar evolutionary models. We find the mass and radius of the planet to be M b = 10.43 +/- 0.30 +/- 0.24 M Jup and R b = 1.165 +/- 0.055 +/- 0.014 R Jup (statistical and systematic errors), respectively. The systematic errors in the orbital separation and the stellar and planetary masses, arising from the use of theoretical predictions, are of a similar size to the statistical errors and set a limit on our understanding of the WASP-18 system. We point out that seven of the nine known massive transiting planets (M b > 3 M Jup) have eccentric orbits, whereas significant orbital eccentricity has been detected for only four of the 46 less-massive planets. This may indicate that there are two different populations of transiting planets, but could also be explained by observational biases. 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C</au><au>Dominik, M</au><au>Glitrup, M</au><au>Jørgensen, U. G</au><au>Liebig, C</au><au>Mathiasen, M</au><au>Anderson, D. R</au><au>Bozza, V</au><au>Browne, P</au><au>Burgdorf, M</au><au>Calchi Novati, S</au><au>Dreizler, S</au><au>Finet, F</au><au>Harpsøe, K</au><au>Hessman, F</au><au>Hundertmark, M</au><au>Maier, G</au><au>Mancini, L</au><au>Maxted, P. F. L</au><au>Rahvar, S</au><au>Ricci, D</au><au>Scarpetta, G</au><au>Skottfelt, J</au><au>Snodgrass, C</au><au>Surdej, J</au><au>Zimmer, F</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Physical Properties of the 0.94-Day Period Transiting Planetary System WASP-18</atitle><jtitle>The Astrophysical journal</jtitle><date>2009-12-10</date><risdate>2009</risdate><volume>707</volume><issue>1</issue><spage>167</spage><epage>172</epage><pages>167-172</pages><issn>0004-637X</issn><issn>1538-4357</issn><eissn>1538-4357</eissn><coden>ASJOAB</coden><abstract>We present high-precision photometry of five consecutive transits of WASP-18, an extrasolar planetary system with one of the shortest orbital periods known. Through the use of telescope defocusing we achieve a photometric precision of 0.47-0.83 mmag per observation over complete transit events. The data are analyzed using the JKTEBOP code and three different sets of stellar evolutionary models. We find the mass and radius of the planet to be M b = 10.43 +/- 0.30 +/- 0.24 M Jup and R b = 1.165 +/- 0.055 +/- 0.014 R Jup (statistical and systematic errors), respectively. The systematic errors in the orbital separation and the stellar and planetary masses, arising from the use of theoretical predictions, are of a similar size to the statistical errors and set a limit on our understanding of the WASP-18 system. We point out that seven of the nine known massive transiting planets (M b > 3 M Jup) have eccentric orbits, whereas significant orbital eccentricity has been detected for only four of the 46 less-massive planets. This may indicate that there are two different populations of transiting planets, but could also be explained by observational biases. Further radial velocity observations of low-mass planets will make it possible to choose between these two scenarios.</abstract><cop>Bristol</cop><pub>IOP Publishing</pub><doi>10.1088/0004-637X/707/1/167</doi><tpages>6</tpages><oa>free_for_read</oa></addata></record> |
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| subjects | Astronomy ASTROPHYSICS, COSMOLOGY AND ASTRONOMY Aérospatiale, astronomie & astrophysique Earth, ocean, space Exact sciences and technology MASS PHOTOMETRY PHYSICAL PROPERTIES Physical, chemical, mathematical & earth Sciences Physique, chimie, mathématiques & sciences de la terre planetary systems PLANETS RADIAL VELOCITY Space science, astronomy & astrophysics STARS stars: individual: WASP-18 TELESCOPES VELOCITY |
| title | Physical Properties of the 0.94-Day Period Transiting Planetary System WASP-18 |
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