TOI-1201 b: A mini-Neptune transiting a bright and moderately young M dwarf
We present the discovery of a transiting mini-Neptune around TOI-1201, a relatively bright and moderately young early M dwarf ( J ≈ 9.5 mag, ~600–800 Myr) in an equal-mass ~8 arcsecond-wide binary system, using data from the Transiting Exoplanet Survey Satellite, along with follow-up transit observa...
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| Veröffentlicht in: | Astronomy and astrophysics (Berlin) 2021-12, Vol.656, p.A124 |
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| creator | Kossakowski, D. Kemmer, J. Bluhm, P. Stock, S. Caballero, J. A. Béjar, V. J. S. Guillén, C. Cardona Lodieu, N. Collins, K. A. Oshagh, M. Schlecker, M. Espinoza, N. Pallé, E. Henning, Th Kreidberg, L. Kürster, M. Amado, P. J. Anderson, D. R. Morales, J. C. Cartwright, S. Charbonneau, D. Chaturvedi, P. Cifuentes, C. Conti, D. M. Cortés-Contreras, M. Dreizler, S. Galadí-Enríquez, D. Guerra, P. Hart, R. Hellier, C. Henze, C. Herrero, E. Jeffers, S. V. Jenkins, J. M. Jensen, E. L. N. Kaminski, A. Kielkopf, J. F. Kunimoto, M. Lafarga, M. Latham, D. W. Lillo-Box, J. Luque, R. Molaverdikhani, K. Montes, D. Morello, G. Morgan, E. H. Nowak, G. Pavlov, A. Perger, M. Quintana, E. V. Quirrenbach, A. Reffert, S. Reiners, A. Ricker, G. Ribas, I. López, C. Rodríguez Osorio, M. R. Zapatero Seager, S. Schöfer, P. Schweitzer, A. Trifonov, T. Vanaverbeke, S. Vanderspek, R. West, R. Winn, J. Zechmeister, M. |
| description | We present the discovery of a transiting mini-Neptune around TOI-1201, a relatively bright and moderately young early M dwarf (
J
≈ 9.5 mag, ~600–800 Myr) in an equal-mass ~8 arcsecond-wide binary system, using data from the Transiting Exoplanet Survey Satellite, along with follow-up transit observations. With an orbital period of 2.49 d, TOI-1201 b is a warm mini-Neptune with a radius of
R
b
= 2.415 ± 0.090
R
⊕
. This signal is also present in the precise radial velocity measurements from CARMENES, confirming the existence of the planet and providing a planetary mass of
M
b
= 6.28 ± 0.88
M
⊕
and, thus, an estimated bulk density of 2.45
−0.42
+0.48
g cm
−3
. The spectroscopic observations additionally show evidence of a signal with a period of 19 d and a long periodic variation of undetermined origin. In combination with ground-based photometric monitoring from WASP-South and ASAS-SN, we attribute the 19 d signal to the stellar rotation period (
P
rot
= 19–23 d), although we cannot rule out that the variation seen in photometry belongs to the visually close binary companion. We calculate precise stellar parameters for both TOI-1201 and its companion. The transiting planet is anexcellent target for atmosphere characterization (the transmission spectroscopy metric is 97
−16
+21
) with the upcoming
James Webb
Space Telescope. It is also feasible to measure its spin-orbit alignment via the Rossiter-McLaughlin effect using current state-of-the-art spectrographs with submeter per second radial velocity precision. |
| doi_str_mv | 10.1051/0004-6361/202141587 |
| format | Article |
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J
≈ 9.5 mag, ~600–800 Myr) in an equal-mass ~8 arcsecond-wide binary system, using data from the Transiting Exoplanet Survey Satellite, along with follow-up transit observations. With an orbital period of 2.49 d, TOI-1201 b is a warm mini-Neptune with a radius of
R
b
= 2.415 ± 0.090
R
⊕
. This signal is also present in the precise radial velocity measurements from CARMENES, confirming the existence of the planet and providing a planetary mass of
M
b
= 6.28 ± 0.88
M
⊕
and, thus, an estimated bulk density of 2.45
−0.42
+0.48
g cm
−3
. The spectroscopic observations additionally show evidence of a signal with a period of 19 d and a long periodic variation of undetermined origin. In combination with ground-based photometric monitoring from WASP-South and ASAS-SN, we attribute the 19 d signal to the stellar rotation period (
P
rot
= 19–23 d), although we cannot rule out that the variation seen in photometry belongs to the visually close binary companion. We calculate precise stellar parameters for both TOI-1201 and its companion. The transiting planet is anexcellent target for atmosphere characterization (the transmission spectroscopy metric is 97
−16
+21
) with the upcoming
James Webb
Space Telescope. It is also feasible to measure its spin-orbit alignment via the Rossiter-McLaughlin effect using current state-of-the-art spectrographs with submeter per second radial velocity precision.</description><identifier>ISSN: 0004-6361</identifier><identifier>EISSN: 1432-0746</identifier><identifier>DOI: 10.1051/0004-6361/202141587</identifier><language>eng</language><publisher>Heidelberg: EDP Sciences</publisher><subject>Binary stars ; Bulk density ; Extrasolar planets ; James Webb Space Telescope ; Mathematical analysis ; Neptune ; Orbits ; Periodic variations ; Photometry ; Planet detection ; Planetary mass ; Radial velocity ; Red dwarf stars ; Space telescopes ; Spectrographs ; Stellar rotation ; Transit</subject><ispartof>Astronomy and astrophysics (Berlin), 2021-12, Vol.656, p.A124</ispartof><rights>2021. This work is licensed under https://creativecommons.org/licenses/by/4.0 (the “License”). Notwithstanding the ProQuest Terms and conditions, you may use this content in accordance with the terms of the License.</rights><lds50>peer_reviewed</lds50><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed><citedby>FETCH-LOGICAL-c388t-84e54edcc8e610b4576ff81e371730270d7a9659b697fd01818500814e5039b3</citedby><cites>FETCH-LOGICAL-c388t-84e54edcc8e610b4576ff81e371730270d7a9659b697fd01818500814e5039b3</cites><orcidid>0000-0002-4715-9460 ; 0000-0001-5664-2852 ; 0000-0003-4946-5653 ; 0000-0001-8355-2107 ; 0000-0003-2239-0567 ; 0000-0001-8012-3788 ; 0000-0003-1242-5922 ; 0000-0002-5969-3708 ; 0000-0002-4265-047X ; 0000-0002-6892-6948 ; 0000-0002-3439-1439 ; 0000-0001-8602-6639 ; 0000-0003-1715-5087 ; 0000-0002-9003-484X ; 0000-0002-6532-4378 ; 0000-0003-0231-2676 ; 0000-0003-0497-2651 ; 0000-0002-1887-1192 ; 0000-0001-7098-0372 ; 0000-0001-9513-1449 ; 0000-0002-0374-8466 ; 0000-0002-4625-7333 ; 0000-0003-0061-518X ; 0000-0002-3612-8968 ; 0000-0002-8815-9416 ; 0000-0001-9911-7388 ; 0000-0002-0236-775X ; 0000-0002-2198-4200 ; 0000-0002-1166-9338 ; 0000-0003-1447-6344 ; 0000-0002-2606-9239 ; 0000-0003-0203-8208 ; 0000-0003-0514-1147 ; 0000-0002-0436-7833 ; 0000-0002-7349-1387 ; 0000-0003-3929-1442 ; 0000-0003-3742-1987 ; 0000-0002-6689-0312 ; 0000-0003-0987-1593 ; 0000-0002-7031-7754 ; 0000-0003-3734-9866 ; 0000-0001-9269-8060 ; 0000-0002-0460-8289 ; 0000-0002-4308-2339 ; 0000-0001-5559-7850 ; 0000-0002-1765-9907</orcidid></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><link.rule.ids>314,776,780,3714,27901,27902</link.rule.ids></links><search><creatorcontrib>Kossakowski, D.</creatorcontrib><creatorcontrib>Kemmer, J.</creatorcontrib><creatorcontrib>Bluhm, P.</creatorcontrib><creatorcontrib>Stock, S.</creatorcontrib><creatorcontrib>Caballero, J. A.</creatorcontrib><creatorcontrib>Béjar, V. J. S.</creatorcontrib><creatorcontrib>Guillén, C. Cardona</creatorcontrib><creatorcontrib>Lodieu, N.</creatorcontrib><creatorcontrib>Collins, K. A.</creatorcontrib><creatorcontrib>Oshagh, M.</creatorcontrib><creatorcontrib>Schlecker, M.</creatorcontrib><creatorcontrib>Espinoza, N.</creatorcontrib><creatorcontrib>Pallé, E.</creatorcontrib><creatorcontrib>Henning, Th</creatorcontrib><creatorcontrib>Kreidberg, L.</creatorcontrib><creatorcontrib>Kürster, M.</creatorcontrib><creatorcontrib>Amado, P. J.</creatorcontrib><creatorcontrib>Anderson, D. R.</creatorcontrib><creatorcontrib>Morales, J. C.</creatorcontrib><creatorcontrib>Cartwright, S.</creatorcontrib><creatorcontrib>Charbonneau, D.</creatorcontrib><creatorcontrib>Chaturvedi, P.</creatorcontrib><creatorcontrib>Cifuentes, C.</creatorcontrib><creatorcontrib>Conti, D. M.</creatorcontrib><creatorcontrib>Cortés-Contreras, M.</creatorcontrib><creatorcontrib>Dreizler, S.</creatorcontrib><creatorcontrib>Galadí-Enríquez, D.</creatorcontrib><creatorcontrib>Guerra, P.</creatorcontrib><creatorcontrib>Hart, R.</creatorcontrib><creatorcontrib>Hellier, C.</creatorcontrib><creatorcontrib>Henze, C.</creatorcontrib><creatorcontrib>Herrero, E.</creatorcontrib><creatorcontrib>Jeffers, S. V.</creatorcontrib><creatorcontrib>Jenkins, J. M.</creatorcontrib><creatorcontrib>Jensen, E. L. N.</creatorcontrib><creatorcontrib>Kaminski, A.</creatorcontrib><creatorcontrib>Kielkopf, J. F.</creatorcontrib><creatorcontrib>Kunimoto, M.</creatorcontrib><creatorcontrib>Lafarga, M.</creatorcontrib><creatorcontrib>Latham, D. W.</creatorcontrib><creatorcontrib>Lillo-Box, J.</creatorcontrib><creatorcontrib>Luque, R.</creatorcontrib><creatorcontrib>Molaverdikhani, K.</creatorcontrib><creatorcontrib>Montes, D.</creatorcontrib><creatorcontrib>Morello, G.</creatorcontrib><creatorcontrib>Morgan, E. H.</creatorcontrib><creatorcontrib>Nowak, G.</creatorcontrib><creatorcontrib>Pavlov, A.</creatorcontrib><creatorcontrib>Perger, M.</creatorcontrib><creatorcontrib>Quintana, E. V.</creatorcontrib><creatorcontrib>Quirrenbach, A.</creatorcontrib><creatorcontrib>Reffert, S.</creatorcontrib><creatorcontrib>Reiners, A.</creatorcontrib><creatorcontrib>Ricker, G.</creatorcontrib><creatorcontrib>Ribas, I.</creatorcontrib><creatorcontrib>López, C. Rodríguez</creatorcontrib><creatorcontrib>Osorio, M. R. Zapatero</creatorcontrib><creatorcontrib>Seager, S.</creatorcontrib><creatorcontrib>Schöfer, P.</creatorcontrib><creatorcontrib>Schweitzer, A.</creatorcontrib><creatorcontrib>Trifonov, T.</creatorcontrib><creatorcontrib>Vanaverbeke, S.</creatorcontrib><creatorcontrib>Vanderspek, R.</creatorcontrib><creatorcontrib>West, R.</creatorcontrib><creatorcontrib>Winn, J.</creatorcontrib><creatorcontrib>Zechmeister, M.</creatorcontrib><title>TOI-1201 b: A mini-Neptune transiting a bright and moderately young M dwarf</title><title>Astronomy and astrophysics (Berlin)</title><description>We present the discovery of a transiting mini-Neptune around TOI-1201, a relatively bright and moderately young early M dwarf (
J
≈ 9.5 mag, ~600–800 Myr) in an equal-mass ~8 arcsecond-wide binary system, using data from the Transiting Exoplanet Survey Satellite, along with follow-up transit observations. With an orbital period of 2.49 d, TOI-1201 b is a warm mini-Neptune with a radius of
R
b
= 2.415 ± 0.090
R
⊕
. This signal is also present in the precise radial velocity measurements from CARMENES, confirming the existence of the planet and providing a planetary mass of
M
b
= 6.28 ± 0.88
M
⊕
and, thus, an estimated bulk density of 2.45
−0.42
+0.48
g cm
−3
. The spectroscopic observations additionally show evidence of a signal with a period of 19 d and a long periodic variation of undetermined origin. In combination with ground-based photometric monitoring from WASP-South and ASAS-SN, we attribute the 19 d signal to the stellar rotation period (
P
rot
= 19–23 d), although we cannot rule out that the variation seen in photometry belongs to the visually close binary companion. We calculate precise stellar parameters for both TOI-1201 and its companion. The transiting planet is anexcellent target for atmosphere characterization (the transmission spectroscopy metric is 97
−16
+21
) with the upcoming
James Webb
Space Telescope. It is also feasible to measure its spin-orbit alignment via the Rossiter-McLaughlin effect using current state-of-the-art spectrographs with submeter per second radial velocity precision.</description><subject>Binary stars</subject><subject>Bulk density</subject><subject>Extrasolar planets</subject><subject>James Webb Space Telescope</subject><subject>Mathematical analysis</subject><subject>Neptune</subject><subject>Orbits</subject><subject>Periodic variations</subject><subject>Photometry</subject><subject>Planet detection</subject><subject>Planetary mass</subject><subject>Radial velocity</subject><subject>Red dwarf stars</subject><subject>Space telescopes</subject><subject>Spectrographs</subject><subject>Stellar rotation</subject><subject>Transit</subject><issn>0004-6361</issn><issn>1432-0746</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2021</creationdate><recordtype>article</recordtype><recordid>eNo9kE1Lw0AQhhdRsFZ_gZcFz7Ez-x1vpWgtVnvpfdkkm5rSJnV3g_Tfm1IpDAzD-8wMPIQ8IjwjSJwAgMgUVzhhwFCgNPqKjFBwloEW6pqMLsQtuYtxO4wMDR-Rj_VqkSEDpMULndJ90zbZlz-kvvU0BdfGJjXthjpahGbznahrK7rvKh9c8rsjPXb9kH7S6teF-p7c1G4X_cN_H5P12-t69p4tV_PFbLrMSm5MyozwUviqLI1XCIWQWtW1Qc81ag5MQ6VdrmReqFzXFaBBIwEMDmvA84KPydP57CF0P72PyW67PrTDR8sUyqEMYwPFz1QZuhiDr-0hNHsXjhbBnqTZkxJ7UmIv0vgft5dbMA</recordid><startdate>20211201</startdate><enddate>20211201</enddate><creator>Kossakowski, D.</creator><creator>Kemmer, J.</creator><creator>Bluhm, P.</creator><creator>Stock, S.</creator><creator>Caballero, J. 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A. ; Béjar, V. J. S. ; Guillén, C. Cardona ; Lodieu, N. ; Collins, K. A. ; Oshagh, M. ; Schlecker, M. ; Espinoza, N. ; Pallé, E. ; Henning, Th ; Kreidberg, L. ; Kürster, M. ; Amado, P. J. ; Anderson, D. R. ; Morales, J. C. ; Cartwright, S. ; Charbonneau, D. ; Chaturvedi, P. ; Cifuentes, C. ; Conti, D. M. ; Cortés-Contreras, M. ; Dreizler, S. ; Galadí-Enríquez, D. ; Guerra, P. ; Hart, R. ; Hellier, C. ; Henze, C. ; Herrero, E. ; Jeffers, S. V. ; Jenkins, J. M. ; Jensen, E. L. N. ; Kaminski, A. ; Kielkopf, J. F. ; Kunimoto, M. ; Lafarga, M. ; Latham, D. W. ; Lillo-Box, J. ; Luque, R. ; Molaverdikhani, K. ; Montes, D. ; Morello, G. ; Morgan, E. H. ; Nowak, G. ; Pavlov, A. ; Perger, M. ; Quintana, E. V. ; Quirrenbach, A. ; Reffert, S. ; Reiners, A. ; Ricker, G. ; Ribas, I. ; López, C. Rodríguez ; Osorio, M. R. Zapatero ; Seager, S. ; Schöfer, P. ; Schweitzer, A. ; Trifonov, T. ; Vanaverbeke, S. ; Vanderspek, R. ; West, R. ; Winn, J. ; Zechmeister, M.</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-c388t-84e54edcc8e610b4576ff81e371730270d7a9659b697fd01818500814e5039b3</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2021</creationdate><topic>Binary stars</topic><topic>Bulk density</topic><topic>Extrasolar planets</topic><topic>James Webb Space Telescope</topic><topic>Mathematical analysis</topic><topic>Neptune</topic><topic>Orbits</topic><topic>Periodic variations</topic><topic>Photometry</topic><topic>Planet detection</topic><topic>Planetary mass</topic><topic>Radial velocity</topic><topic>Red dwarf stars</topic><topic>Space telescopes</topic><topic>Spectrographs</topic><topic>Stellar rotation</topic><topic>Transit</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Kossakowski, D.</creatorcontrib><creatorcontrib>Kemmer, J.</creatorcontrib><creatorcontrib>Bluhm, P.</creatorcontrib><creatorcontrib>Stock, S.</creatorcontrib><creatorcontrib>Caballero, J. A.</creatorcontrib><creatorcontrib>Béjar, V. J. S.</creatorcontrib><creatorcontrib>Guillén, C. Cardona</creatorcontrib><creatorcontrib>Lodieu, N.</creatorcontrib><creatorcontrib>Collins, K. A.</creatorcontrib><creatorcontrib>Oshagh, M.</creatorcontrib><creatorcontrib>Schlecker, M.</creatorcontrib><creatorcontrib>Espinoza, N.</creatorcontrib><creatorcontrib>Pallé, E.</creatorcontrib><creatorcontrib>Henning, Th</creatorcontrib><creatorcontrib>Kreidberg, L.</creatorcontrib><creatorcontrib>Kürster, M.</creatorcontrib><creatorcontrib>Amado, P. J.</creatorcontrib><creatorcontrib>Anderson, D. R.</creatorcontrib><creatorcontrib>Morales, J. C.</creatorcontrib><creatorcontrib>Cartwright, S.</creatorcontrib><creatorcontrib>Charbonneau, D.</creatorcontrib><creatorcontrib>Chaturvedi, P.</creatorcontrib><creatorcontrib>Cifuentes, C.</creatorcontrib><creatorcontrib>Conti, D. 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Zapatero</creatorcontrib><creatorcontrib>Seager, S.</creatorcontrib><creatorcontrib>Schöfer, P.</creatorcontrib><creatorcontrib>Schweitzer, A.</creatorcontrib><creatorcontrib>Trifonov, T.</creatorcontrib><creatorcontrib>Vanaverbeke, S.</creatorcontrib><creatorcontrib>Vanderspek, R.</creatorcontrib><creatorcontrib>West, R.</creatorcontrib><creatorcontrib>Winn, J.</creatorcontrib><creatorcontrib>Zechmeister, M.</creatorcontrib><collection>CrossRef</collection><collection>Technology Research Database</collection><collection>Aerospace Database</collection><collection>Advanced Technologies Database with Aerospace</collection><jtitle>Astronomy and astrophysics (Berlin)</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Kossakowski, D.</au><au>Kemmer, J.</au><au>Bluhm, P.</au><au>Stock, S.</au><au>Caballero, J. A.</au><au>Béjar, V. J. S.</au><au>Guillén, C. Cardona</au><au>Lodieu, N.</au><au>Collins, K. A.</au><au>Oshagh, M.</au><au>Schlecker, M.</au><au>Espinoza, N.</au><au>Pallé, E.</au><au>Henning, Th</au><au>Kreidberg, L.</au><au>Kürster, M.</au><au>Amado, P. J.</au><au>Anderson, D. R.</au><au>Morales, J. C.</au><au>Cartwright, S.</au><au>Charbonneau, D.</au><au>Chaturvedi, P.</au><au>Cifuentes, C.</au><au>Conti, D. M.</au><au>Cortés-Contreras, M.</au><au>Dreizler, S.</au><au>Galadí-Enríquez, D.</au><au>Guerra, P.</au><au>Hart, R.</au><au>Hellier, C.</au><au>Henze, C.</au><au>Herrero, E.</au><au>Jeffers, S. V.</au><au>Jenkins, J. M.</au><au>Jensen, E. L. N.</au><au>Kaminski, A.</au><au>Kielkopf, J. F.</au><au>Kunimoto, M.</au><au>Lafarga, M.</au><au>Latham, D. W.</au><au>Lillo-Box, J.</au><au>Luque, R.</au><au>Molaverdikhani, K.</au><au>Montes, D.</au><au>Morello, G.</au><au>Morgan, E. H.</au><au>Nowak, G.</au><au>Pavlov, A.</au><au>Perger, M.</au><au>Quintana, E. V.</au><au>Quirrenbach, A.</au><au>Reffert, S.</au><au>Reiners, A.</au><au>Ricker, G.</au><au>Ribas, I.</au><au>López, C. Rodríguez</au><au>Osorio, M. R. Zapatero</au><au>Seager, S.</au><au>Schöfer, P.</au><au>Schweitzer, A.</au><au>Trifonov, T.</au><au>Vanaverbeke, S.</au><au>Vanderspek, R.</au><au>West, R.</au><au>Winn, J.</au><au>Zechmeister, M.</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>TOI-1201 b: A mini-Neptune transiting a bright and moderately young M dwarf</atitle><jtitle>Astronomy and astrophysics (Berlin)</jtitle><date>2021-12-01</date><risdate>2021</risdate><volume>656</volume><spage>A124</spage><pages>A124-</pages><issn>0004-6361</issn><eissn>1432-0746</eissn><abstract>We present the discovery of a transiting mini-Neptune around TOI-1201, a relatively bright and moderately young early M dwarf (
J
≈ 9.5 mag, ~600–800 Myr) in an equal-mass ~8 arcsecond-wide binary system, using data from the Transiting Exoplanet Survey Satellite, along with follow-up transit observations. With an orbital period of 2.49 d, TOI-1201 b is a warm mini-Neptune with a radius of
R
b
= 2.415 ± 0.090
R
⊕
. This signal is also present in the precise radial velocity measurements from CARMENES, confirming the existence of the planet and providing a planetary mass of
M
b
= 6.28 ± 0.88
M
⊕
and, thus, an estimated bulk density of 2.45
−0.42
+0.48
g cm
−3
. The spectroscopic observations additionally show evidence of a signal with a period of 19 d and a long periodic variation of undetermined origin. In combination with ground-based photometric monitoring from WASP-South and ASAS-SN, we attribute the 19 d signal to the stellar rotation period (
P
rot
= 19–23 d), although we cannot rule out that the variation seen in photometry belongs to the visually close binary companion. We calculate precise stellar parameters for both TOI-1201 and its companion. The transiting planet is anexcellent target for atmosphere characterization (the transmission spectroscopy metric is 97
−16
+21
) with the upcoming
James Webb
Space Telescope. It is also feasible to measure its spin-orbit alignment via the Rossiter-McLaughlin effect using current state-of-the-art spectrographs with submeter per second radial velocity precision.</abstract><cop>Heidelberg</cop><pub>EDP Sciences</pub><doi>10.1051/0004-6361/202141587</doi><orcidid>https://orcid.org/0000-0002-4715-9460</orcidid><orcidid>https://orcid.org/0000-0001-5664-2852</orcidid><orcidid>https://orcid.org/0000-0003-4946-5653</orcidid><orcidid>https://orcid.org/0000-0001-8355-2107</orcidid><orcidid>https://orcid.org/0000-0003-2239-0567</orcidid><orcidid>https://orcid.org/0000-0001-8012-3788</orcidid><orcidid>https://orcid.org/0000-0003-1242-5922</orcidid><orcidid>https://orcid.org/0000-0002-5969-3708</orcidid><orcidid>https://orcid.org/0000-0002-4265-047X</orcidid><orcidid>https://orcid.org/0000-0002-6892-6948</orcidid><orcidid>https://orcid.org/0000-0002-3439-1439</orcidid><orcidid>https://orcid.org/0000-0001-8602-6639</orcidid><orcidid>https://orcid.org/0000-0003-1715-5087</orcidid><orcidid>https://orcid.org/0000-0002-9003-484X</orcidid><orcidid>https://orcid.org/0000-0002-6532-4378</orcidid><orcidid>https://orcid.org/0000-0003-0231-2676</orcidid><orcidid>https://orcid.org/0000-0003-0497-2651</orcidid><orcidid>https://orcid.org/0000-0002-1887-1192</orcidid><orcidid>https://orcid.org/0000-0001-7098-0372</orcidid><orcidid>https://orcid.org/0000-0001-9513-1449</orcidid><orcidid>https://orcid.org/0000-0002-0374-8466</orcidid><orcidid>https://orcid.org/0000-0002-4625-7333</orcidid><orcidid>https://orcid.org/0000-0003-0061-518X</orcidid><orcidid>https://orcid.org/0000-0002-3612-8968</orcidid><orcidid>https://orcid.org/0000-0002-8815-9416</orcidid><orcidid>https://orcid.org/0000-0001-9911-7388</orcidid><orcidid>https://orcid.org/0000-0002-0236-775X</orcidid><orcidid>https://orcid.org/0000-0002-2198-4200</orcidid><orcidid>https://orcid.org/0000-0002-1166-9338</orcidid><orcidid>https://orcid.org/0000-0003-1447-6344</orcidid><orcidid>https://orcid.org/0000-0002-2606-9239</orcidid><orcidid>https://orcid.org/0000-0003-0203-8208</orcidid><orcidid>https://orcid.org/0000-0003-0514-1147</orcidid><orcidid>https://orcid.org/0000-0002-0436-7833</orcidid><orcidid>https://orcid.org/0000-0002-7349-1387</orcidid><orcidid>https://orcid.org/0000-0003-3929-1442</orcidid><orcidid>https://orcid.org/0000-0003-3742-1987</orcidid><orcidid>https://orcid.org/0000-0002-6689-0312</orcidid><orcidid>https://orcid.org/0000-0003-0987-1593</orcidid><orcidid>https://orcid.org/0000-0002-7031-7754</orcidid><orcidid>https://orcid.org/0000-0003-3734-9866</orcidid><orcidid>https://orcid.org/0000-0001-9269-8060</orcidid><orcidid>https://orcid.org/0000-0002-0460-8289</orcidid><orcidid>https://orcid.org/0000-0002-4308-2339</orcidid><orcidid>https://orcid.org/0000-0001-5559-7850</orcidid><orcidid>https://orcid.org/0000-0002-1765-9907</orcidid><oa>free_for_read</oa></addata></record> |
| fulltext | fulltext |
| identifier | ISSN: 0004-6361 |
| ispartof | Astronomy and astrophysics (Berlin), 2021-12, Vol.656, p.A124 |
| issn | 0004-6361 1432-0746 |
| language | eng |
| recordid | cdi_proquest_journals_2615615822 |
| source | Bacon EDP Sciences France Licence nationale-ISTEX-PS-Journals-PFISTEX; EDP Sciences; EZB-FREE-00999 freely available EZB journals |
| subjects | Binary stars Bulk density Extrasolar planets James Webb Space Telescope Mathematical analysis Neptune Orbits Periodic variations Photometry Planet detection Planetary mass Radial velocity Red dwarf stars Space telescopes Spectrographs Stellar rotation Transit |
| title | TOI-1201 b: A mini-Neptune transiting a bright and moderately young M dwarf |
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