The CARMENES search for exoplanets around M dwarfs
We announce the discovery of two planetary companions orbiting around the low-mass stars Ross 1020 (GJ 3779, M4.0V) and LP 819-052 (GJ 1265, M4.5V). The discovery is based on the analysis of CARMENES radial velocity (RV) observations in the visual channel as part of its survey for exoplanets around...
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| creator | Luque, R. Nowak, G. Pallé, E. Kossakowski, D. Trifonov, T. Zechmeister, M. Béjar, V. J. S. Cardona Guillén, C. Tal-Or, L. Hidalgo, D. Ribas, I. Reiners, A. Caballero, J. A. Amado, P. J. Quirrenbach, A. Aceituno, J. Cortés-Contreras, M. Díez-Alonso, E. Dreizler, S. Guenther, E. W. Henning, T. Jeffers, S. V. Kaminski, A. Kürster, M. Lafarga, M. Montes, D. Morales, J. C. Passegger, V. M. Schmitt, J. H. M. M. Schweitzer, A. |
| description | We announce the discovery of two planetary companions orbiting around the low-mass stars Ross 1020 (GJ 3779, M4.0V) and LP 819-052 (GJ 1265, M4.5V). The discovery is based on the analysis of CARMENES radial velocity (RV) observations in the visual channel as part of its survey for exoplanets around M dwarfs. In the case of GJ 1265, CARMENES observations were complemented with publicly available Doppler measurements from HARPS. The datasets reveal two planetary companions, one for each star, that share very similar properties: minimum masses of 8.0 ± 0.5 M⊕ and 7.4 ± 0.5 M⊕ in low-eccentricity orbits with periods of 3.023 ± 0.001 d and 3.651 ± 0.001 d for GJ 3779 b and GJ 1265 b, respectively. The periodic signals around 3 d found in the RV data have no counterpart in any spectral activity indicator. Furthermore, we collected available photometric data for the two host stars, which confirm that the additional Doppler variations found at periods of approximately 95 d can be attributed to the rotation of the stars. The addition of these planets to a mass-period diagram of known planets around M dwarfs suggests a bimodal distribution with a lack of short-period low-mass planets in the range of 2–5 M⊕. It also indicates that super-Earths (>5 M⊕) currently detected by RV and transit techniques around M stars are usually found in systems dominated by a single planet. |
| doi_str_mv | 10.1051/0004-6361/201833423 |
| format | Article |
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J. S. ; Cardona Guillén, C. ; Tal-Or, L. ; Hidalgo, D. ; Ribas, I. ; Reiners, A. ; Caballero, J. A. ; Amado, P. J. ; Quirrenbach, A. ; Aceituno, J. ; Cortés-Contreras, M. ; Díez-Alonso, E. ; Dreizler, S. ; Guenther, E. W. ; Henning, T. ; Jeffers, S. V. ; Kaminski, A. ; Kürster, M. ; Lafarga, M. ; Montes, D. ; Morales, J. C. ; Passegger, V. M. ; Schmitt, J. H. M. M. ; Schweitzer, A.</creator><creatorcontrib>Luque, R. ; Nowak, G. ; Pallé, E. ; Kossakowski, D. ; Trifonov, T. ; Zechmeister, M. ; Béjar, V. J. S. ; Cardona Guillén, C. ; Tal-Or, L. ; Hidalgo, D. ; Ribas, I. ; Reiners, A. ; Caballero, J. A. ; Amado, P. J. ; Quirrenbach, A. ; Aceituno, J. ; Cortés-Contreras, M. ; Díez-Alonso, E. ; Dreizler, S. ; Guenther, E. W. ; Henning, T. ; Jeffers, S. V. ; Kaminski, A. ; Kürster, M. ; Lafarga, M. ; Montes, D. ; Morales, J. C. ; Passegger, V. M. ; Schmitt, J. H. M. M. ; Schweitzer, A.</creatorcontrib><description>We announce the discovery of two planetary companions orbiting around the low-mass stars Ross 1020 (GJ 3779, M4.0V) and LP 819-052 (GJ 1265, M4.5V). The discovery is based on the analysis of CARMENES radial velocity (RV) observations in the visual channel as part of its survey for exoplanets around M dwarfs. In the case of GJ 1265, CARMENES observations were complemented with publicly available Doppler measurements from HARPS. The datasets reveal two planetary companions, one for each star, that share very similar properties: minimum masses of 8.0 ± 0.5 M⊕ and 7.4 ± 0.5 M⊕ in low-eccentricity orbits with periods of 3.023 ± 0.001 d and 3.651 ± 0.001 d for GJ 3779 b and GJ 1265 b, respectively. The periodic signals around 3 d found in the RV data have no counterpart in any spectral activity indicator. Furthermore, we collected available photometric data for the two host stars, which confirm that the additional Doppler variations found at periods of approximately 95 d can be attributed to the rotation of the stars. The addition of these planets to a mass-period diagram of known planets around M dwarfs suggests a bimodal distribution with a lack of short-period low-mass planets in the range of 2–5 M⊕. It also indicates that super-Earths (>5 M⊕) currently detected by RV and transit techniques around M stars are usually found in systems dominated by a single planet.</description><identifier>ISSN: 0004-6361</identifier><identifier>EISSN: 1432-0746</identifier><identifier>DOI: 10.1051/0004-6361/201833423</identifier><language>eng</language><publisher>Heidelberg: EDP Sciences</publisher><subject>Eccentric orbits ; Extrasolar planets ; Low mass stars ; M stars ; Photometry ; Planetary rotation ; planetary systems ; Radial velocity ; Red dwarf stars ; stars: late-type ; stars: low-mass ; Stellar rotation ; techniques: radial velocities ; Visual observation</subject><ispartof>Astronomy and astrophysics (Berlin), 2018-12, Vol.620</ispartof><rights>Copyright EDP Sciences Dec 2018</rights><lds50>peer_reviewed</lds50><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed><citedby>FETCH-LOGICAL-c2273-8a0088fc3484b8002822fee7fe732e0896366a636ff595ab7a14f457e4e53b343</citedby></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><link.rule.ids>314,776,780,27901,27902</link.rule.ids></links><search><creatorcontrib>Luque, R.</creatorcontrib><creatorcontrib>Nowak, G.</creatorcontrib><creatorcontrib>Pallé, E.</creatorcontrib><creatorcontrib>Kossakowski, D.</creatorcontrib><creatorcontrib>Trifonov, T.</creatorcontrib><creatorcontrib>Zechmeister, M.</creatorcontrib><creatorcontrib>Béjar, V. J. S.</creatorcontrib><creatorcontrib>Cardona Guillén, C.</creatorcontrib><creatorcontrib>Tal-Or, L.</creatorcontrib><creatorcontrib>Hidalgo, D.</creatorcontrib><creatorcontrib>Ribas, I.</creatorcontrib><creatorcontrib>Reiners, A.</creatorcontrib><creatorcontrib>Caballero, J. A.</creatorcontrib><creatorcontrib>Amado, P. J.</creatorcontrib><creatorcontrib>Quirrenbach, A.</creatorcontrib><creatorcontrib>Aceituno, J.</creatorcontrib><creatorcontrib>Cortés-Contreras, M.</creatorcontrib><creatorcontrib>Díez-Alonso, E.</creatorcontrib><creatorcontrib>Dreizler, S.</creatorcontrib><creatorcontrib>Guenther, E. W.</creatorcontrib><creatorcontrib>Henning, T.</creatorcontrib><creatorcontrib>Jeffers, S. V.</creatorcontrib><creatorcontrib>Kaminski, A.</creatorcontrib><creatorcontrib>Kürster, M.</creatorcontrib><creatorcontrib>Lafarga, M.</creatorcontrib><creatorcontrib>Montes, D.</creatorcontrib><creatorcontrib>Morales, J. C.</creatorcontrib><creatorcontrib>Passegger, V. M.</creatorcontrib><creatorcontrib>Schmitt, J. H. M. M.</creatorcontrib><creatorcontrib>Schweitzer, A.</creatorcontrib><title>The CARMENES search for exoplanets around M dwarfs</title><title>Astronomy and astrophysics (Berlin)</title><description>We announce the discovery of two planetary companions orbiting around the low-mass stars Ross 1020 (GJ 3779, M4.0V) and LP 819-052 (GJ 1265, M4.5V). The discovery is based on the analysis of CARMENES radial velocity (RV) observations in the visual channel as part of its survey for exoplanets around M dwarfs. In the case of GJ 1265, CARMENES observations were complemented with publicly available Doppler measurements from HARPS. The datasets reveal two planetary companions, one for each star, that share very similar properties: minimum masses of 8.0 ± 0.5 M⊕ and 7.4 ± 0.5 M⊕ in low-eccentricity orbits with periods of 3.023 ± 0.001 d and 3.651 ± 0.001 d for GJ 3779 b and GJ 1265 b, respectively. The periodic signals around 3 d found in the RV data have no counterpart in any spectral activity indicator. Furthermore, we collected available photometric data for the two host stars, which confirm that the additional Doppler variations found at periods of approximately 95 d can be attributed to the rotation of the stars. The addition of these planets to a mass-period diagram of known planets around M dwarfs suggests a bimodal distribution with a lack of short-period low-mass planets in the range of 2–5 M⊕. It also indicates that super-Earths (>5 M⊕) currently detected by RV and transit techniques around M stars are usually found in systems dominated by a single planet.</description><subject>Eccentric orbits</subject><subject>Extrasolar planets</subject><subject>Low mass stars</subject><subject>M stars</subject><subject>Photometry</subject><subject>Planetary rotation</subject><subject>planetary systems</subject><subject>Radial velocity</subject><subject>Red dwarf stars</subject><subject>stars: late-type</subject><subject>stars: low-mass</subject><subject>Stellar rotation</subject><subject>techniques: radial velocities</subject><subject>Visual observation</subject><issn>0004-6361</issn><issn>1432-0746</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2018</creationdate><recordtype>article</recordtype><recordid>eNo9jkFLAzEUhIMoWKu_wEvA89okL5ukx7K0Kmwr6GqPIbt9oa21uyZdrP_eQMXLDAMfM0PILWf3nOV8xBiTmQLFR4JxAyAFnJEBlyAypqU6J4N_4pJcxbhNUSRwQES1RlpMXubTxfSVRnShWVPfBorHttu5PR4idaHt9ys6p6tvF3y8Jhfe7SLe_PmQvM2mVfGYlc8PT8WkzBohNGTGMWaMb0AaWZu0Z4TwiNqjBoHMjNMb5ZJ4n49zV2vHpZe5Rok51CBhSO5OvV1ov3qMB7tt-7BPk1ZwxcdgtGKJyk7UJh7waLuw-XThx7rwYZUGnVvDlnZZzWeLd7GwJfwCk5JTPA</recordid><startdate>20181201</startdate><enddate>20181201</enddate><creator>Luque, R.</creator><creator>Nowak, G.</creator><creator>Pallé, E.</creator><creator>Kossakowski, D.</creator><creator>Trifonov, T.</creator><creator>Zechmeister, M.</creator><creator>Béjar, V. 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M.</creator><creator>Schweitzer, A.</creator><general>EDP Sciences</general><scope>BSCLL</scope><scope>8FD</scope><scope>H8D</scope><scope>L7M</scope></search><sort><creationdate>20181201</creationdate><title>The CARMENES search for exoplanets around M dwarfs</title><author>Luque, R. ; Nowak, G. ; Pallé, E. ; Kossakowski, D. ; Trifonov, T. ; Zechmeister, M. ; Béjar, V. J. S. ; Cardona Guillén, C. ; Tal-Or, L. ; Hidalgo, D. ; Ribas, I. ; Reiners, A. ; Caballero, J. A. ; Amado, P. J. ; Quirrenbach, A. ; Aceituno, J. ; Cortés-Contreras, M. ; Díez-Alonso, E. ; Dreizler, S. ; Guenther, E. W. ; Henning, T. ; Jeffers, S. V. ; Kaminski, A. ; Kürster, M. ; Lafarga, M. ; Montes, D. ; Morales, J. C. ; Passegger, V. M. ; Schmitt, J. H. M. 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V.</au><au>Kaminski, A.</au><au>Kürster, M.</au><au>Lafarga, M.</au><au>Montes, D.</au><au>Morales, J. C.</au><au>Passegger, V. M.</au><au>Schmitt, J. H. M. M.</au><au>Schweitzer, A.</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>The CARMENES search for exoplanets around M dwarfs</atitle><jtitle>Astronomy and astrophysics (Berlin)</jtitle><date>2018-12-01</date><risdate>2018</risdate><volume>620</volume><issn>0004-6361</issn><eissn>1432-0746</eissn><abstract>We announce the discovery of two planetary companions orbiting around the low-mass stars Ross 1020 (GJ 3779, M4.0V) and LP 819-052 (GJ 1265, M4.5V). The discovery is based on the analysis of CARMENES radial velocity (RV) observations in the visual channel as part of its survey for exoplanets around M dwarfs. In the case of GJ 1265, CARMENES observations were complemented with publicly available Doppler measurements from HARPS. The datasets reveal two planetary companions, one for each star, that share very similar properties: minimum masses of 8.0 ± 0.5 M⊕ and 7.4 ± 0.5 M⊕ in low-eccentricity orbits with periods of 3.023 ± 0.001 d and 3.651 ± 0.001 d for GJ 3779 b and GJ 1265 b, respectively. The periodic signals around 3 d found in the RV data have no counterpart in any spectral activity indicator. Furthermore, we collected available photometric data for the two host stars, which confirm that the additional Doppler variations found at periods of approximately 95 d can be attributed to the rotation of the stars. The addition of these planets to a mass-period diagram of known planets around M dwarfs suggests a bimodal distribution with a lack of short-period low-mass planets in the range of 2–5 M⊕. It also indicates that super-Earths (>5 M⊕) currently detected by RV and transit techniques around M stars are usually found in systems dominated by a single planet.</abstract><cop>Heidelberg</cop><pub>EDP Sciences</pub><doi>10.1051/0004-6361/201833423</doi><oa>free_for_read</oa></addata></record> |
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| source | Bacon EDP Sciences France Licence nationale-ISTEX-PS-Journals-PFISTEX; EDP Sciences; EZB-FREE-00999 freely available EZB journals |
| subjects | Eccentric orbits Extrasolar planets Low mass stars M stars Photometry Planetary rotation planetary systems Radial velocity Red dwarf stars stars: late-type stars: low-mass Stellar rotation techniques: radial velocities Visual observation |
| title | The CARMENES search for exoplanets around M dwarfs |
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