TOI-1416: A system with a super-Earth planet with a 1.07 d period

H. J. Deeg; I. Y. Georgieva; G. Nowak; C. M. Persson; B. L. Cale; F. Murgas; E. Pallé; D. Godoy-Rivera; F. Dai; D. R. Ciardi; J. M.Akana Murphy; P. G. Beck; C. J. Burke; J. Cabrera; I. Carleo; W. D. Cochran; K. A. Collins; Sz Csizmadia; M. El Mufti; M. Fridlund; A. Fukui; D. Gandolfi; R. A. García; E. W. Guenther; P. Guerra; S. Grziwa; H. Isaacson; K. Isogai; J. M. Jenkins; P. Kábath; J. Korth; K. W.F. Lam; D. W. Latham; R. Luque; M. B. Lund; J. H. Livingston; S. Mathis; S. Mathur; N. Narita; J. Orell-Miquel; H. L.M. Osborne; H. Parviainen; P. P. Plavchan; S. Redfield; D. R. Rodriguez; R. P. Schwarz; S. Seager; A. M.S. Smith; V. Van Eylen; J. Van Zandt; J. N. Winn; C. Ziegler

doi:10.1051/0004-6361/202346370

TOI-1416: A system with a super-Earth planet with a 1.07 d period

H. J. Deeg, I. Y. Georgieva, G. Nowak, C. M. Persson, B. L. Cale, F. Murgas, E. Pallé, D. Godoy-Rivera, F. Dai, D. R. Ciardi, J. M.Akana Murphy, P. G. Beck, C. J. Burke, J. Cabrera, I. Carleo, W. D. Cochran, K. A. Collins, Sz Csizmadia, M. El Mufti, M. FridlundA. Fukui, D. Gandolfi, R. A. García, E. W. Guenther, P. Guerra, S. Grziwa, H. Isaacson, K. Isogai, J. M. Jenkins, P. Kábath, J. Korth, K. W.F. Lam, D. W. Latham, R. Luque, M. B. Lund, J. H. Livingston, S. Mathis, S. Mathur, N. Narita, J. Orell-Miquel, H. L.M. Osborne, H. Parviainen, P. P. Plavchan, S. Redfield, D. R. Rodriguez, R. P. Schwarz, S. Seager, A. M.S. Smith, V. Van Eylen, J. Van Zandt, J. N. Winn, C. Ziegler

Physics and Astronomy

Producción científica: Article › revisión exhaustiva

Resumen

TOI-1416 is a late G or early K-type dwarf star. TESS detected transits of a planet, TOI-1416 b, around it with a period of 1.07 days. The planet's mass is approximately 3.48 M•, and its radius is about 1.62 R•, resulting in a density slightly less than Earth's. There might be another planet, "c", but it's uncertain due to interference related to the Moon's period. TOI-1416 b is a hot super-Earth-like planet with a temperature of roughly 1570 K. Its composition might be like molten magma with dissolved water, making its atmosphere potentially interesting for transmission spectroscopy using JWST. This planet doesn't fall into a unique category but suggests that planets like it, with ultra-short periods, fall in a broad range up to about 30 days. These are differentiated from other types by the "Neptune Desert" and a valley distinguishing super-Earths from sub-Neptune planets. A pattern has emerged with many small, short-period planets between 0.6-1.4 days. The Neptune Desert's parameters need adjustment due to the discovery of more short-period planets. The defined lower limit of this desert is a radius of 1.6 R• and a mass of 0.028 Mjup. Limits against the planets' insolation and effective temperatures are also provided.

Idioma original	English
Número de artículo	A12
Publicación	Astronomy and Astrophysics
Volumen	677
DOI	https://doi.org/10.1051/0004-6361/202346370
Estado	Published - sept 1 2023

ASJC Scopus Subject Areas

Astronomy and Astrophysics
Space and Planetary Science

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10.1051/0004-6361/202346370

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Deeg, H. J., Georgieva, I. Y., Nowak, G., Persson, C. M., Cale, B. L., Murgas, F., Pallé, E., Godoy-Rivera, D., Dai, F., Ciardi, D. R., Murphy, J. M. A., Beck, P. G., Burke, C. J., Cabrera, J., Carleo, I., Cochran, W. D., Collins, K. A., Csizmadia, S., El Mufti, M., ... Ziegler, C. (2023). TOI-1416: A system with a super-Earth planet with a 1.07 d period. Astronomy and Astrophysics, 677, Artículo A12. https://doi.org/10.1051/0004-6361/202346370

Deeg, HJ, Georgieva, IY, Nowak, G, Persson, CM, Cale, BL, Murgas, F, Pallé, E, Godoy-Rivera, D, Dai, F, Ciardi, DR, Murphy, JMA, Beck, PG, Burke, CJ, Cabrera, J, Carleo, I, Cochran, WD, Collins, KA, Csizmadia, S, El Mufti, M, Fridlund, M, Fukui, A, Gandolfi, D, García, RA, Guenther, EW, Guerra, P, Grziwa, S, Isaacson, H, Isogai, K, Jenkins, JM, Kábath, P, Korth, J, Lam, KWF, Latham, DW, Luque, R, Lund, MB, Livingston, JH, Mathis, S, Mathur, S, Narita, N, Orell-Miquel, J, Osborne, HLM, Parviainen, H, Plavchan, PP, Redfield, S, Rodriguez, DR, Schwarz, RP, Seager, S, Smith, AMS, Van Eylen, V, Van Zandt, J, Winn, JN & Ziegler, C 2023, 'TOI-1416: A system with a super-Earth planet with a 1.07 d period', Astronomy and Astrophysics, vol. 677, A12. https://doi.org/10.1051/0004-6361/202346370

@article{599896b7564a4a66b354275dd56bc08a,

title = "TOI-1416: A system with a super-Earth planet with a 1.07 d period",

abstract = "TOI-1416 is a late G or early K-type dwarf star. TESS detected transits of a planet, TOI-1416 b, around it with a period of 1.07 days. The planet's mass is approximately 3.48 M•, and its radius is about 1.62 R•, resulting in a density slightly less than Earth's. There might be another planet, {"}c{"}, but it's uncertain due to interference related to the Moon's period. TOI-1416 b is a hot super-Earth-like planet with a temperature of roughly 1570 K. Its composition might be like molten magma with dissolved water, making its atmosphere potentially interesting for transmission spectroscopy using JWST. This planet doesn't fall into a unique category but suggests that planets like it, with ultra-short periods, fall in a broad range up to about 30 days. These are differentiated from other types by the {"}Neptune Desert{"} and a valley distinguishing super-Earths from sub-Neptune planets. A pattern has emerged with many small, short-period planets between 0.6-1.4 days. The Neptune Desert's parameters need adjustment due to the discovery of more short-period planets. The defined lower limit of this desert is a radius of 1.6 R• and a mass of 0.028 Mjup. Limits against the planets' insolation and effective temperatures are also provided.",

keywords = "Planetary systems, Planets and satellites: composition, Planets and satellites: detection, Planets and satellites: individual: TOI-1416 b, Planets and satellites: terrestrial planets, Techniques: radial velocities",

author = "Deeg, {H. J.} and Georgieva, {I. Y.} and G. Nowak and Persson, {C. M.} and Cale, {B. L.} and F. Murgas and E. Pall{\'e} and D. Godoy-Rivera and F. Dai and Ciardi, {D. R.} and Murphy, {J. M.Akana} and Beck, {P. G.} and Burke, {C. J.} and J. Cabrera and I. Carleo and Cochran, {W. D.} and Collins, {K. A.} and Sz Csizmadia and {El Mufti}, M. and M. Fridlund and A. Fukui and D. Gandolfi and Garc{\'i}a, {R. A.} and Guenther, {E. W.} and P. Guerra and S. Grziwa and H. Isaacson and K. Isogai and Jenkins, {J. M.} and P. K{\'a}bath and J. Korth and Lam, {K. W.F.} and Latham, {D. W.} and R. Luque and Lund, {M. B.} and Livingston, {J. H.} and S. Mathis and S. Mathur and N. Narita and J. Orell-Miquel and Osborne, {H. L.M.} and H. Parviainen and Plavchan, {P. P.} and S. Redfield and Rodriguez, {D. R.} and Schwarz, {R. P.} and S. Seager and Smith, {A. M.S.} and {Van Eylen}, V. and {Van Zandt}, J. and Winn, {J. N.} and C. Ziegler",

note = "Funding Information: This work was supported by the KESPRINT collaboration, an international consortium devoted to the characterization and research of exoplanets discovered with space-based missions ( http://www.kesprint.science ). This paper includes data collected by the TESS mission. Funding for the TESS mission is provided by the NASA Explorer Program. We acknowledge the use of public TOI Release data from pipelines at the TESS Science Office and at the TESS Science Processing Operations Center. Resources supporting this work were provided by the NASA High-End Computing (HEC) Program through the NASA Advanced Supercomputing (NAS) Division at Ames Research Center for the production of the SPOC data products. This research has made use of the Exoplanet Follow-up Observation Program (Exo-FOP; DOI: 10.26134/ExoFOP5 ) website, which is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program. This work has made use of data from the European Space Agency (ESA) mission Gaia ( https://www.cosmos.esa.int/Gaia ), processed by the Gaia Data Processing and Analysis Consortium (DPAC, https://www.cosmos.esa.int/web/Gaia/dpac/consortium ). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. Based on observations made with the Italian Telescopio Nazionale Galileo (TNG) operated on the island of La Palma by the Fundaci{\'o}n Galileo Galilei of the INAF (Instituto Nazionale di Astrofisica) at the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrof{\'i}sica de Canarias under programmes CAT19A_162, CAT21A_119, CAT22A_111 and ITP19_1. CARMENES is an instrument for the Centro Astron{\'o}mico Hispano-Alem{\'a}n de Calar Alto (CAHA, Almer{\'i}a, Spain). CARMENES is funded by the German Max-Planck-Gesellschaft (MPG), the Spanish Consejo Superior de Investigaciones Cient{\'i}ficas (CSIC), the European Union through FEDER/ERF FICTS-2011-02 funds, and the members of the CARMENES Consortium (Max-Planck-Institut f{\"u}r Astronomie, Instituto de Astrof{\'i}sica de Andaluc{\'i}a, Landessternwarte K{\"o}nigstuhl, Institut de Ci{\`e}ncies de l{\textquoteright}Espai, Institut f{\"u}r Astrophysik G{\"o}ttingen, Universidad Complutense de Madrid, Th{\"u}ringer Landessternwarte Tautenburg, Instituto de Astrof{\'i}sica de Canarias, Hamburger Sternwarte, Centro de Astrobiolog{\'i}a and Centro Astron{\'o}mico Hispano-Alem{\'a}n), with additional contributions by the Spanish Ministry of Economy, the German Science Foundation through the Major Research Instrumentation Programme and DFG Research Unit FOR2544 “Blue Planets around Red Stars”, the Klaus Tschira Stiftung, the states of Baden-W{\"u}rttemberg and Niedersachsen, and by the Junta de Andaluc{\'i}a. This article is partly based on observations made with the MuSCAT2 instrument, developed by ABC, at the Telescopio Carlos S{\'a}nchez operated on the island of Tenerife by the IAC in the Spanish Observatorio del Teide. This work makes use of observations from the LCOGT network. Part of the LCOGT telescope time was granted by NOIRLab through the Mid-Scale Innovations Program (MSIP). MSIP is funded by NSF. We thank the following iSHELL observers: Kevin I Collins, Michael Reefe, Farzaneh Zohrabi, Eric Gaidos, Angelle Tanner and Claire Geneser. We thank Annelies Mortier for the provision of the latest versions of her code for the BGLS and related plots. H.J.D. and S.M. acknowledge support from the Spanish Research Agency of the Ministry of Science and Innovation (AEI-MICINN) under grant {\textquoteleft}Contribution of the IAC to the PLATO Space Mission{\textquoteright} with references ESP2017-87676-C5-4-R and PID2019-107061GB-C66, DOI: 10.13039/501100011033 . S.M. and D.G.R. acknowledge support form the same source with the grant no. PID2019-107187GB-I00. S.M. acknowledges support from the same source through the Severo Ochoa Centres of Excellence Programme 2020–2023 (CEX2019-000920-S). P.G.B. acknowledges support from the same source with the Ram{\'o}ny Cajal fellowship number RYC-2021-033137-I. G.N. thanks for the research funding from the Polish Ministry of Education and Science programme the “Excellence Initiative – Research University{\textquoteright} conducted at the Centre of Excellence in Astrophysics and Astrochemistry of the Nicolaus Copernicus University in Toru{\'n}, Poland. This work is partly supported by JSPS KAKENHI Grant Number P17H04574, JP18H05439 and JP20K14521, and JST CREST Grant Number JPMJCR1761. J.M.A.M. is supported by the National Science Foundation Graduate Research Fellowship Program under Grant No. DGE-1842400. J.M.A.M. acknowledges the LSSTC Data Science Fellowship Program, which is funded by LSSTC, NSF Cybertraining Grant No. 1829740, the Brinson Foundation, and the Moore Foundation; his participation in the program has benefited this work. K.A.C. and D.W.L. acknowledge support from the TESS mission via sub-award s3449 from MIT. K.W.F.L. was supported by Deutsche Forschungsgemeinschaft grant RA714/14-1, within the DFG Schwerpunkt SPP 1992, “Exploring the Diversity of Extrasolar Planets{\textquoteright}. J. K. gratefully acknowledges support by the Swedish National Space Agency (SNSA; DNR 2020-00104) and by the Swedish Research Council (VR: Etableringsbidrag 2017-04945). Publisher Copyright: {\textcopyright} 2023 The Authors.",

year = "2023",

month = sep,

day = "1",

doi = "10.1051/0004-6361/202346370",

language = "English",

volume = "677",

}

TY - JOUR

T1 - TOI-1416

T2 - A system with a super-Earth planet with a 1.07 d period

AU - Deeg, H. J.

AU - Georgieva, I. Y.

AU - Nowak, G.

AU - Persson, C. M.

AU - Cale, B. L.

AU - Murgas, F.

AU - Pallé, E.

AU - Godoy-Rivera, D.

AU - Dai, F.

AU - Ciardi, D. R.

AU - Murphy, J. M.Akana

AU - Beck, P. G.

AU - Burke, C. J.

AU - Cabrera, J.

AU - Carleo, I.

AU - Cochran, W. D.

AU - Collins, K. A.

AU - Csizmadia, Sz

AU - El Mufti, M.

AU - Fridlund, M.

AU - Fukui, A.

AU - Gandolfi, D.

AU - García, R. A.

AU - Guenther, E. W.

AU - Guerra, P.

AU - Grziwa, S.

AU - Isaacson, H.

AU - Isogai, K.

AU - Jenkins, J. M.

AU - Kábath, P.

AU - Korth, J.

AU - Lam, K. W.F.

AU - Latham, D. W.

AU - Luque, R.

AU - Lund, M. B.

AU - Livingston, J. H.

AU - Mathis, S.

AU - Mathur, S.

AU - Narita, N.

AU - Orell-Miquel, J.

AU - Osborne, H. L.M.

AU - Parviainen, H.

AU - Plavchan, P. P.

AU - Redfield, S.

AU - Rodriguez, D. R.

AU - Schwarz, R. P.

AU - Seager, S.

AU - Smith, A. M.S.

AU - Van Eylen, V.

AU - Van Zandt, J.

AU - Winn, J. N.

AU - Ziegler, C.

N1 - Funding Information: This work was supported by the KESPRINT collaboration, an international consortium devoted to the characterization and research of exoplanets discovered with space-based missions ( http://www.kesprint.science ). This paper includes data collected by the TESS mission. Funding for the TESS mission is provided by the NASA Explorer Program. We acknowledge the use of public TOI Release data from pipelines at the TESS Science Office and at the TESS Science Processing Operations Center. Resources supporting this work were provided by the NASA High-End Computing (HEC) Program through the NASA Advanced Supercomputing (NAS) Division at Ames Research Center for the production of the SPOC data products. This research has made use of the Exoplanet Follow-up Observation Program (Exo-FOP; DOI: 10.26134/ExoFOP5 ) website, which is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program. This work has made use of data from the European Space Agency (ESA) mission Gaia ( https://www.cosmos.esa.int/Gaia ), processed by the Gaia Data Processing and Analysis Consortium (DPAC, https://www.cosmos.esa.int/web/Gaia/dpac/consortium ). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. Based on observations made with the Italian Telescopio Nazionale Galileo (TNG) operated on the island of La Palma by the Fundación Galileo Galilei of the INAF (Instituto Nazionale di Astrofisica) at the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofísica de Canarias under programmes CAT19A_162, CAT21A_119, CAT22A_111 and ITP19_1. CARMENES is an instrument for the Centro Astronómico Hispano-Alemán de Calar Alto (CAHA, Almería, Spain). CARMENES is funded by the German Max-Planck-Gesellschaft (MPG), the Spanish Consejo Superior de Investigaciones Científicas (CSIC), the European Union through FEDER/ERF FICTS-2011-02 funds, and the members of the CARMENES Consortium (Max-Planck-Institut für Astronomie, Instituto de Astrofísica de Andalucía, Landessternwarte Königstuhl, Institut de Ciències de l’Espai, Institut für Astrophysik Göttingen, Universidad Complutense de Madrid, Thüringer Landessternwarte Tautenburg, Instituto de Astrofísica de Canarias, Hamburger Sternwarte, Centro de Astrobiología and Centro Astronómico Hispano-Alemán), with additional contributions by the Spanish Ministry of Economy, the German Science Foundation through the Major Research Instrumentation Programme and DFG Research Unit FOR2544 “Blue Planets around Red Stars”, the Klaus Tschira Stiftung, the states of Baden-Württemberg and Niedersachsen, and by the Junta de Andalucía. This article is partly based on observations made with the MuSCAT2 instrument, developed by ABC, at the Telescopio Carlos Sánchez operated on the island of Tenerife by the IAC in the Spanish Observatorio del Teide. This work makes use of observations from the LCOGT network. Part of the LCOGT telescope time was granted by NOIRLab through the Mid-Scale Innovations Program (MSIP). MSIP is funded by NSF. We thank the following iSHELL observers: Kevin I Collins, Michael Reefe, Farzaneh Zohrabi, Eric Gaidos, Angelle Tanner and Claire Geneser. We thank Annelies Mortier for the provision of the latest versions of her code for the BGLS and related plots. H.J.D. and S.M. acknowledge support from the Spanish Research Agency of the Ministry of Science and Innovation (AEI-MICINN) under grant ‘Contribution of the IAC to the PLATO Space Mission’ with references ESP2017-87676-C5-4-R and PID2019-107061GB-C66, DOI: 10.13039/501100011033 . S.M. and D.G.R. acknowledge support form the same source with the grant no. PID2019-107187GB-I00. S.M. acknowledges support from the same source through the Severo Ochoa Centres of Excellence Programme 2020–2023 (CEX2019-000920-S). P.G.B. acknowledges support from the same source with the Ramóny Cajal fellowship number RYC-2021-033137-I. G.N. thanks for the research funding from the Polish Ministry of Education and Science programme the “Excellence Initiative – Research University’ conducted at the Centre of Excellence in Astrophysics and Astrochemistry of the Nicolaus Copernicus University in Toruń, Poland. This work is partly supported by JSPS KAKENHI Grant Number P17H04574, JP18H05439 and JP20K14521, and JST CREST Grant Number JPMJCR1761. J.M.A.M. is supported by the National Science Foundation Graduate Research Fellowship Program under Grant No. DGE-1842400. J.M.A.M. acknowledges the LSSTC Data Science Fellowship Program, which is funded by LSSTC, NSF Cybertraining Grant No. 1829740, the Brinson Foundation, and the Moore Foundation; his participation in the program has benefited this work. K.A.C. and D.W.L. acknowledge support from the TESS mission via sub-award s3449 from MIT. K.W.F.L. was supported by Deutsche Forschungsgemeinschaft grant RA714/14-1, within the DFG Schwerpunkt SPP 1992, “Exploring the Diversity of Extrasolar Planets’. J. K. gratefully acknowledges support by the Swedish National Space Agency (SNSA; DNR 2020-00104) and by the Swedish Research Council (VR: Etableringsbidrag 2017-04945). Publisher Copyright: © 2023 The Authors.

PY - 2023/9/1

Y1 - 2023/9/1

N2 - TOI-1416 is a late G or early K-type dwarf star. TESS detected transits of a planet, TOI-1416 b, around it with a period of 1.07 days. The planet's mass is approximately 3.48 M•, and its radius is about 1.62 R•, resulting in a density slightly less than Earth's. There might be another planet, "c", but it's uncertain due to interference related to the Moon's period. TOI-1416 b is a hot super-Earth-like planet with a temperature of roughly 1570 K. Its composition might be like molten magma with dissolved water, making its atmosphere potentially interesting for transmission spectroscopy using JWST. This planet doesn't fall into a unique category but suggests that planets like it, with ultra-short periods, fall in a broad range up to about 30 days. These are differentiated from other types by the "Neptune Desert" and a valley distinguishing super-Earths from sub-Neptune planets. A pattern has emerged with many small, short-period planets between 0.6-1.4 days. The Neptune Desert's parameters need adjustment due to the discovery of more short-period planets. The defined lower limit of this desert is a radius of 1.6 R• and a mass of 0.028 Mjup. Limits against the planets' insolation and effective temperatures are also provided.

AB - TOI-1416 is a late G or early K-type dwarf star. TESS detected transits of a planet, TOI-1416 b, around it with a period of 1.07 days. The planet's mass is approximately 3.48 M•, and its radius is about 1.62 R•, resulting in a density slightly less than Earth's. There might be another planet, "c", but it's uncertain due to interference related to the Moon's period. TOI-1416 b is a hot super-Earth-like planet with a temperature of roughly 1570 K. Its composition might be like molten magma with dissolved water, making its atmosphere potentially interesting for transmission spectroscopy using JWST. This planet doesn't fall into a unique category but suggests that planets like it, with ultra-short periods, fall in a broad range up to about 30 days. These are differentiated from other types by the "Neptune Desert" and a valley distinguishing super-Earths from sub-Neptune planets. A pattern has emerged with many small, short-period planets between 0.6-1.4 days. The Neptune Desert's parameters need adjustment due to the discovery of more short-period planets. The defined lower limit of this desert is a radius of 1.6 R• and a mass of 0.028 Mjup. Limits against the planets' insolation and effective temperatures are also provided.

KW - Planetary systems

KW - Planets and satellites: composition

KW - Planets and satellites: detection

KW - Planets and satellites: individual: TOI-1416 b

KW - Planets and satellites: terrestrial planets

KW - Techniques: radial velocities

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