WASP-54b, WASP-56b and WASP-57b: Three new sub-Jupiter mass planets from SuperWASP
We present three newly discovered sub-Jupiter mass planets from the SuperWASP survey: WASP-54b is a heavily bloated planet of mass 0.636\(^{+0.025}_{-0.024}\) \mj and radius 1.653\(^{+0.090}_{-0.083}\) \rj. It orbits a F9 star, evolving off the main sequence, every 3.69 days. Our MCMC fit of the sys...
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| creator | Faedi, F Pollacco, D Barros, S C C Brown, D A Collier Cameron Doyle, A P Enoch, R Gillon, M Y Gomez Maqueo Chew Hebrard, G Lendl, M Liebig, C Smalley, B A H M J Triaud West, R G Wheatley, P J Alsubai, K A Anderson, D R Armstrong, D J Bento, J Bochinski, J Bouchy, F Busuttil, R Fossati, L Fumel, A Haswell, C A Hellier, C Holmes, S Jehin, E Kolb, U McCormac, J Miller, G R M Moutou, C Norton, A J Parley, N Queloz, D Santerne, A Skillen, I Smith, A M S Udry, S Watson, C |
| description | We present three newly discovered sub-Jupiter mass planets from the SuperWASP survey: WASP-54b is a heavily bloated planet of mass 0.636\(^{+0.025}_{-0.024}\) \mj and radius 1.653\(^{+0.090}_{-0.083}\) \rj. It orbits a F9 star, evolving off the main sequence, every 3.69 days. Our MCMC fit of the system yields a slightly eccentric orbit (\(e=0.067^{+0.033}_{-0.025}\)) for WASP-54b. We investigated further the veracity of our detection of the eccentric orbit for WASP-54b, and we find that it could be real. However, given the brightness of WASP-54 V=10.42 magnitudes, we encourage observations of a secondary eclipse to draw robust conclusions on both the orbital eccentricity and the thermal structure of the planet. WASP-56b and WASP-57b have masses of 0.571\(^{+0.034}_{-0.035}\) \mj and \(0.672^{+0.049}_{-0.046}\) \mj, respectively; and radii of \(1.092^{+0.035}_{-0.033}\) \rj for WASP-56b and \(0.916^{+0.017}_{-0.014}\) \rj for WASP-57b. They orbit main sequence stars of spectral type G6 every 4.67 and 2.84 days, respectively. WASP-56b and WASP-57b show no radius anomaly and a high density possibly implying a large core of heavy elements; possibly as high as \(\sim\)50 M\(_{\oplus}\) in the case of WASP-57b. However, the composition of the deep interior of exoplanets remain still undetermined. Thus, more exoplanet discoveries such as the ones presented in this paper, are needed to understand and constrain giant planets' physical properties. |
| doi_str_mv | 10.48550/arxiv.1210.2329 |
| format | Article |
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It orbits a F9 star, evolving off the main sequence, every 3.69 days. Our MCMC fit of the system yields a slightly eccentric orbit (\(e=0.067^{+0.033}_{-0.025}\)) for WASP-54b. We investigated further the veracity of our detection of the eccentric orbit for WASP-54b, and we find that it could be real. However, given the brightness of WASP-54 V=10.42 magnitudes, we encourage observations of a secondary eclipse to draw robust conclusions on both the orbital eccentricity and the thermal structure of the planet. WASP-56b and WASP-57b have masses of 0.571\(^{+0.034}_{-0.035}\) \mj and \(0.672^{+0.049}_{-0.046}\) \mj, respectively; and radii of \(1.092^{+0.035}_{-0.033}\) \rj for WASP-56b and \(0.916^{+0.017}_{-0.014}\) \rj for WASP-57b. They orbit main sequence stars of spectral type G6 every 4.67 and 2.84 days, respectively. WASP-56b and WASP-57b show no radius anomaly and a high density possibly implying a large core of heavy elements; possibly as high as \(\sim\)50 M\(_{\oplus}\) in the case of WASP-57b. However, the composition of the deep interior of exoplanets remain still undetermined. Thus, more exoplanet discoveries such as the ones presented in this paper, are needed to understand and constrain giant planets' physical properties.</description><identifier>EISSN: 2331-8422</identifier><identifier>DOI: 10.48550/arxiv.1210.2329</identifier><language>eng</language><publisher>Ithaca: Cornell University Library, arXiv.org</publisher><subject>Eccentric orbits ; Extrasolar planets ; Gas giant planets ; Heavy elements ; Jupiter ; Main sequence stars ; Physical properties ; Physics - Earth and Planetary Astrophysics ; Physics - Solar and Stellar Astrophysics ; Planet detection ; Stellar evolution</subject><ispartof>arXiv.org, 2013-01</ispartof><rights>2013. This work is published under http://arxiv.org/licenses/nonexclusive-distrib/1.0/ (the “License”). Notwithstanding the ProQuest Terms and Conditions, you may use this content in accordance with the terms of the License.</rights><rights>http://arxiv.org/licenses/nonexclusive-distrib/1.0</rights><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><link.rule.ids>228,230,776,780,881,27902</link.rule.ids><backlink>$$Uhttps://doi.org/10.1051/0004-6361/201220520$$DView published paper (Access to full text may be restricted)$$Hfree_for_read</backlink><backlink>$$Uhttps://doi.org/10.48550/arXiv.1210.2329$$DView paper in arXiv$$Hfree_for_read</backlink></links><search><creatorcontrib>Faedi, F</creatorcontrib><creatorcontrib>Pollacco, D</creatorcontrib><creatorcontrib>Barros, S C C</creatorcontrib><creatorcontrib>Brown, D</creatorcontrib><creatorcontrib>A Collier Cameron</creatorcontrib><creatorcontrib>Doyle, A P</creatorcontrib><creatorcontrib>Enoch, R</creatorcontrib><creatorcontrib>Gillon, M</creatorcontrib><creatorcontrib>Y Gomez Maqueo Chew</creatorcontrib><creatorcontrib>Hebrard, G</creatorcontrib><creatorcontrib>Lendl, M</creatorcontrib><creatorcontrib>Liebig, C</creatorcontrib><creatorcontrib>Smalley, B</creatorcontrib><creatorcontrib>A H M J Triaud</creatorcontrib><creatorcontrib>West, R G</creatorcontrib><creatorcontrib>Wheatley, P J</creatorcontrib><creatorcontrib>Alsubai, K A</creatorcontrib><creatorcontrib>Anderson, D R</creatorcontrib><creatorcontrib>Armstrong, D J</creatorcontrib><creatorcontrib>Bento, J</creatorcontrib><creatorcontrib>Bochinski, J</creatorcontrib><creatorcontrib>Bouchy, F</creatorcontrib><creatorcontrib>Busuttil, R</creatorcontrib><creatorcontrib>Fossati, L</creatorcontrib><creatorcontrib>Fumel, A</creatorcontrib><creatorcontrib>Haswell, C A</creatorcontrib><creatorcontrib>Hellier, C</creatorcontrib><creatorcontrib>Holmes, S</creatorcontrib><creatorcontrib>Jehin, E</creatorcontrib><creatorcontrib>Kolb, U</creatorcontrib><creatorcontrib>McCormac, J</creatorcontrib><creatorcontrib>Miller, G R M</creatorcontrib><creatorcontrib>Moutou, C</creatorcontrib><creatorcontrib>Norton, A J</creatorcontrib><creatorcontrib>Parley, N</creatorcontrib><creatorcontrib>Queloz, D</creatorcontrib><creatorcontrib>Santerne, A</creatorcontrib><creatorcontrib>Skillen, I</creatorcontrib><creatorcontrib>Smith, A M S</creatorcontrib><creatorcontrib>Udry, S</creatorcontrib><creatorcontrib>Watson, C</creatorcontrib><title>WASP-54b, WASP-56b and WASP-57b: Three new sub-Jupiter mass planets from SuperWASP</title><title>arXiv.org</title><description>We present three newly discovered sub-Jupiter mass planets from the SuperWASP survey: WASP-54b is a heavily bloated planet of mass 0.636\(^{+0.025}_{-0.024}\) \mj and radius 1.653\(^{+0.090}_{-0.083}\) \rj. It orbits a F9 star, evolving off the main sequence, every 3.69 days. Our MCMC fit of the system yields a slightly eccentric orbit (\(e=0.067^{+0.033}_{-0.025}\)) for WASP-54b. We investigated further the veracity of our detection of the eccentric orbit for WASP-54b, and we find that it could be real. However, given the brightness of WASP-54 V=10.42 magnitudes, we encourage observations of a secondary eclipse to draw robust conclusions on both the orbital eccentricity and the thermal structure of the planet. WASP-56b and WASP-57b have masses of 0.571\(^{+0.034}_{-0.035}\) \mj and \(0.672^{+0.049}_{-0.046}\) \mj, respectively; and radii of \(1.092^{+0.035}_{-0.033}\) \rj for WASP-56b and \(0.916^{+0.017}_{-0.014}\) \rj for WASP-57b. They orbit main sequence stars of spectral type G6 every 4.67 and 2.84 days, respectively. WASP-56b and WASP-57b show no radius anomaly and a high density possibly implying a large core of heavy elements; possibly as high as \(\sim\)50 M\(_{\oplus}\) in the case of WASP-57b. However, the composition of the deep interior of exoplanets remain still undetermined. Thus, more exoplanet discoveries such as the ones presented in this paper, are needed to understand and constrain giant planets' physical properties.</description><subject>Eccentric orbits</subject><subject>Extrasolar planets</subject><subject>Gas giant planets</subject><subject>Heavy elements</subject><subject>Jupiter</subject><subject>Main sequence stars</subject><subject>Physical properties</subject><subject>Physics - Earth and Planetary Astrophysics</subject><subject>Physics - Solar and Stellar Astrophysics</subject><subject>Planet detection</subject><subject>Stellar evolution</subject><issn>2331-8422</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2013</creationdate><recordtype>article</recordtype><sourceid>BENPR</sourceid><sourceid>GOX</sourceid><recordid>eNotj81LAzEQxYMgWGrvniTg1a3JZJJNvZXiJwXFFjwuk90Et7TbNen68d-7tT0Mb2Z485gfYxdSjNFqLW4o_tRfYwn9AhRMTtgAlJKZRYAzNkppJYQAk4PWasDe3qeL10yju-aHzjhOTXUccnfLlx_Re974b546lz13bb3zkW8oJd6uqfG7xEPcbviia33cn52z00Dr5EdHHbLl_d1y9pjNXx6eZtN5RlpOMlvmwVhF3viSnJWhyjGUSKYSLpAFxNL25a3VwgjUiJYAHaEI0jup1JBdHmL_eYs21huKv8Weu9hz94arg6GN28_Op12x2nax6V8qQFgwUgJO1B9D91dV</recordid><startdate>20130116</startdate><enddate>20130116</enddate><creator>Faedi, F</creator><creator>Pollacco, D</creator><creator>Barros, S C C</creator><creator>Brown, D</creator><creator>A Collier Cameron</creator><creator>Doyle, A P</creator><creator>Enoch, R</creator><creator>Gillon, M</creator><creator>Y Gomez Maqueo Chew</creator><creator>Hebrard, G</creator><creator>Lendl, M</creator><creator>Liebig, C</creator><creator>Smalley, B</creator><creator>A H M J Triaud</creator><creator>West, R G</creator><creator>Wheatley, P J</creator><creator>Alsubai, K A</creator><creator>Anderson, D R</creator><creator>Armstrong, D J</creator><creator>Bento, J</creator><creator>Bochinski, J</creator><creator>Bouchy, F</creator><creator>Busuttil, R</creator><creator>Fossati, L</creator><creator>Fumel, A</creator><creator>Haswell, C A</creator><creator>Hellier, C</creator><creator>Holmes, S</creator><creator>Jehin, E</creator><creator>Kolb, U</creator><creator>McCormac, J</creator><creator>Miller, G R M</creator><creator>Moutou, C</creator><creator>Norton, A J</creator><creator>Parley, N</creator><creator>Queloz, D</creator><creator>Santerne, A</creator><creator>Skillen, I</creator><creator>Smith, A M S</creator><creator>Udry, S</creator><creator>Watson, C</creator><general>Cornell University Library, arXiv.org</general><scope>8FE</scope><scope>8FG</scope><scope>ABJCF</scope><scope>ABUWG</scope><scope>AFKRA</scope><scope>AZQEC</scope><scope>BENPR</scope><scope>BGLVJ</scope><scope>CCPQU</scope><scope>DWQXO</scope><scope>HCIFZ</scope><scope>L6V</scope><scope>M7S</scope><scope>PIMPY</scope><scope>PQEST</scope><scope>PQQKQ</scope><scope>PQUKI</scope><scope>PRINS</scope><scope>PTHSS</scope><scope>GOX</scope></search><sort><creationdate>20130116</creationdate><title>WASP-54b, WASP-56b and WASP-57b: Three new sub-Jupiter mass planets from SuperWASP</title><author>Faedi, F ; Pollacco, D ; Barros, S C C ; Brown, D ; A Collier Cameron ; Doyle, A P ; Enoch, R ; Gillon, M ; Y Gomez Maqueo Chew ; Hebrard, G ; Lendl, M ; Liebig, C ; Smalley, B ; A H M J Triaud ; West, R G ; Wheatley, P J ; Alsubai, K A ; Anderson, D R ; Armstrong, D J ; Bento, J ; Bochinski, J ; Bouchy, F ; Busuttil, R ; Fossati, L ; Fumel, A ; Haswell, C A ; Hellier, C ; Holmes, S ; Jehin, E ; Kolb, U ; McCormac, J ; Miller, G R M ; Moutou, C ; Norton, A J ; Parley, N ; Queloz, D ; Santerne, A ; Skillen, I ; Smith, A M S ; Udry, S ; Watson, C</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-a519-8c7f683ae6ecab81fd74fc4a6d0bfa8244c844ce88506045448a24ba40f1eb133</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2013</creationdate><topic>Eccentric orbits</topic><topic>Extrasolar planets</topic><topic>Gas giant planets</topic><topic>Heavy elements</topic><topic>Jupiter</topic><topic>Main sequence stars</topic><topic>Physical properties</topic><topic>Physics - Earth and Planetary Astrophysics</topic><topic>Physics - Solar and Stellar Astrophysics</topic><topic>Planet detection</topic><topic>Stellar evolution</topic><toplevel>online_resources</toplevel><creatorcontrib>Faedi, F</creatorcontrib><creatorcontrib>Pollacco, D</creatorcontrib><creatorcontrib>Barros, S C C</creatorcontrib><creatorcontrib>Brown, D</creatorcontrib><creatorcontrib>A Collier Cameron</creatorcontrib><creatorcontrib>Doyle, A P</creatorcontrib><creatorcontrib>Enoch, R</creatorcontrib><creatorcontrib>Gillon, M</creatorcontrib><creatorcontrib>Y Gomez Maqueo Chew</creatorcontrib><creatorcontrib>Hebrard, G</creatorcontrib><creatorcontrib>Lendl, M</creatorcontrib><creatorcontrib>Liebig, C</creatorcontrib><creatorcontrib>Smalley, B</creatorcontrib><creatorcontrib>A H M J Triaud</creatorcontrib><creatorcontrib>West, R G</creatorcontrib><creatorcontrib>Wheatley, P J</creatorcontrib><creatorcontrib>Alsubai, K A</creatorcontrib><creatorcontrib>Anderson, D R</creatorcontrib><creatorcontrib>Armstrong, D J</creatorcontrib><creatorcontrib>Bento, J</creatorcontrib><creatorcontrib>Bochinski, J</creatorcontrib><creatorcontrib>Bouchy, F</creatorcontrib><creatorcontrib>Busuttil, R</creatorcontrib><creatorcontrib>Fossati, L</creatorcontrib><creatorcontrib>Fumel, A</creatorcontrib><creatorcontrib>Haswell, C A</creatorcontrib><creatorcontrib>Hellier, C</creatorcontrib><creatorcontrib>Holmes, S</creatorcontrib><creatorcontrib>Jehin, E</creatorcontrib><creatorcontrib>Kolb, U</creatorcontrib><creatorcontrib>McCormac, J</creatorcontrib><creatorcontrib>Miller, G R M</creatorcontrib><creatorcontrib>Moutou, C</creatorcontrib><creatorcontrib>Norton, A J</creatorcontrib><creatorcontrib>Parley, N</creatorcontrib><creatorcontrib>Queloz, D</creatorcontrib><creatorcontrib>Santerne, A</creatorcontrib><creatorcontrib>Skillen, I</creatorcontrib><creatorcontrib>Smith, A M S</creatorcontrib><creatorcontrib>Udry, S</creatorcontrib><creatorcontrib>Watson, C</creatorcontrib><collection>ProQuest SciTech Collection</collection><collection>ProQuest Technology Collection</collection><collection>Materials Science & Engineering Collection</collection><collection>ProQuest Central (Alumni Edition)</collection><collection>ProQuest Central UK/Ireland</collection><collection>ProQuest Central Essentials</collection><collection>ProQuest Central</collection><collection>Technology Collection (ProQuest)</collection><collection>ProQuest One Community College</collection><collection>ProQuest Central Korea</collection><collection>SciTech Premium Collection</collection><collection>ProQuest Engineering Collection</collection><collection>Engineering Database</collection><collection>Publicly Available Content Database</collection><collection>ProQuest One Academic Eastern Edition (DO NOT USE)</collection><collection>ProQuest One Academic</collection><collection>ProQuest One Academic UKI Edition</collection><collection>ProQuest Central China</collection><collection>Engineering Collection</collection><collection>arXiv.org</collection><jtitle>arXiv.org</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Faedi, F</au><au>Pollacco, D</au><au>Barros, S C C</au><au>Brown, D</au><au>A Collier Cameron</au><au>Doyle, A P</au><au>Enoch, R</au><au>Gillon, M</au><au>Y Gomez Maqueo Chew</au><au>Hebrard, G</au><au>Lendl, M</au><au>Liebig, C</au><au>Smalley, B</au><au>A H M J Triaud</au><au>West, R G</au><au>Wheatley, P J</au><au>Alsubai, K A</au><au>Anderson, D R</au><au>Armstrong, D J</au><au>Bento, J</au><au>Bochinski, J</au><au>Bouchy, F</au><au>Busuttil, R</au><au>Fossati, L</au><au>Fumel, A</au><au>Haswell, C A</au><au>Hellier, C</au><au>Holmes, S</au><au>Jehin, E</au><au>Kolb, U</au><au>McCormac, J</au><au>Miller, G R M</au><au>Moutou, C</au><au>Norton, A J</au><au>Parley, N</au><au>Queloz, D</au><au>Santerne, A</au><au>Skillen, I</au><au>Smith, A M S</au><au>Udry, S</au><au>Watson, C</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>WASP-54b, WASP-56b and WASP-57b: Three new sub-Jupiter mass planets from SuperWASP</atitle><jtitle>arXiv.org</jtitle><date>2013-01-16</date><risdate>2013</risdate><eissn>2331-8422</eissn><abstract>We present three newly discovered sub-Jupiter mass planets from the SuperWASP survey: WASP-54b is a heavily bloated planet of mass 0.636\(^{+0.025}_{-0.024}\) \mj and radius 1.653\(^{+0.090}_{-0.083}\) \rj. It orbits a F9 star, evolving off the main sequence, every 3.69 days. Our MCMC fit of the system yields a slightly eccentric orbit (\(e=0.067^{+0.033}_{-0.025}\)) for WASP-54b. We investigated further the veracity of our detection of the eccentric orbit for WASP-54b, and we find that it could be real. However, given the brightness of WASP-54 V=10.42 magnitudes, we encourage observations of a secondary eclipse to draw robust conclusions on both the orbital eccentricity and the thermal structure of the planet. WASP-56b and WASP-57b have masses of 0.571\(^{+0.034}_{-0.035}\) \mj and \(0.672^{+0.049}_{-0.046}\) \mj, respectively; and radii of \(1.092^{+0.035}_{-0.033}\) \rj for WASP-56b and \(0.916^{+0.017}_{-0.014}\) \rj for WASP-57b. They orbit main sequence stars of spectral type G6 every 4.67 and 2.84 days, respectively. WASP-56b and WASP-57b show no radius anomaly and a high density possibly implying a large core of heavy elements; possibly as high as \(\sim\)50 M\(_{\oplus}\) in the case of WASP-57b. However, the composition of the deep interior of exoplanets remain still undetermined. Thus, more exoplanet discoveries such as the ones presented in this paper, are needed to understand and constrain giant planets' physical properties.</abstract><cop>Ithaca</cop><pub>Cornell University Library, arXiv.org</pub><doi>10.48550/arxiv.1210.2329</doi><oa>free_for_read</oa></addata></record> |
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| subjects | Eccentric orbits Extrasolar planets Gas giant planets Heavy elements Jupiter Main sequence stars Physical properties Physics - Earth and Planetary Astrophysics Physics - Solar and Stellar Astrophysics Planet detection Stellar evolution |
| title | WASP-54b, WASP-56b and WASP-57b: Three new sub-Jupiter mass planets from SuperWASP |
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