HD 213885b: A transiting 1-d-period super-Earth with an Earth-like composition around a bright (V = 7.9) star unveiled by TESS

Néstor Espinoza; Rafael Brahm; Thomas Henning; Andrés Jordán; Caroline Dorn; Felipe Rojas; Paula Sarkis; Diana Kossakowski; Martin Schlecker; Matías R. Díaz; James S. Jenkins; Claudia Aguilera-Gomez; Jon M. Jenkins; Joseph D. Twicken; Karen A. Collins; Jack Lissauer; David J. Armstrong; Vardan Adibekyan; David Barrado; Susana C.C. Barros; Matthew Battley; Daniel Bayliss; François Bouchy; Edward M. Bryant; Benjamin F. Cooke; Olivier D.S. demangeon; Xavier Dumusque; Pedro Figueira; Helen Giles; Jorge Lillo-Box; Christophe Lovis; Louise D. Nielsen; Francesco Pepe; Don Pollacco; Nuno C. Santos; Sergio G. Sousa; Stéphane Udry; Peter J. Wheatley; Oliver Turner; Maxime Marmier; Damien Ségransan; George Ricker; David Latham; Sara Seager; Joshua N. Winn; John F. Kielkopf; Rhodes Hart; Geof Wingham; Eric L.N. Jensen; Krzysztof G. Hełminiak; A. Tokovinin; C. Briceño; Carl Ziegler; Nicholas M. Law; Andrew W. Mann; Tansu Daylan; John P. Doty; Natalia Guerrero; Patricia Boyd; Ian Crossfield; Robert L. Morris; Christopher E. Henze; Aaron Dean Chacon

doi:10.1093/mnras/stz3150

HD 213885b: A transiting 1-d-period super-Earth with an Earth-like composition around a bright (V = 7.9) star unveiled by TESS

Néstor Espinoza, Rafael Brahm, Thomas Henning, Andrés Jordán, Caroline Dorn, Felipe Rojas, Paula Sarkis, Diana Kossakowski, Martin Schlecker, Matías R. Díaz, James S. Jenkins, Claudia Aguilera-Gomez, Jon M. Jenkins, Joseph D. Twicken, Karen A. Collins, Jack Lissauer, David J. Armstrong, Vardan Adibekyan, David Barrado, Susana C.C. BarrosMatthew Battley, Daniel Bayliss, François Bouchy, Edward M. Bryant, Benjamin F. Cooke, Olivier D.S. demangeon, Xavier Dumusque, Pedro Figueira, Helen Giles, Jorge Lillo-Box, Christophe Lovis, Louise D. Nielsen, Francesco Pepe, Don Pollacco, Nuno C. Santos, Sergio G. Sousa, Stéphane Udry, Peter J. Wheatley, Oliver Turner, Maxime Marmier, Damien Ségransan, George Ricker, David Latham, Sara Seager, Joshua N. Winn, John F. Kielkopf, Rhodes Hart, Geof Wingham, Eric L.N. Jensen, Krzysztof G. Hełminiak, A. Tokovinin, C. Briceño, Carl Ziegler, Nicholas M. Law, Andrew W. Mann, Tansu Daylan, John P. Doty, Natalia Guerrero, Patricia Boyd, Ian Crossfield, Robert L. Morris, Christopher E. Henze, Aaron Dean Chacon

Astrophysical Sciences

Research output: Contribution to journal › Article › peer-review

35 Scopus citations

Abstract

We report the discovery of the 1.008-d, ultrashort period (USP) super-Earth HD 213885b (TOI-141b) orbiting the bright (V= 7.9) star HD 213885 (TOI-141, TIC 403224672), detected using photometry from the recently launched TESS mission. Using FEROS, HARPS, and CORALIE radial velocities, we measure a precise mass of 8.8 ±0.6M_⊙ for this 1.74±0.05R_⊙ exoplanet, which provides enough information to constrain its bulk composition - similar to Earth's but enriched in iron. The radius, mass, and stellar irradiation of HD 213885b are, given our data, very similar to 55 Cancri e, making this exoplanet a good target to perform comparative exoplanetology of short period, highly irradiated super-Earths. Our precise radial velocities reveal an additional 4.78-d signal which we interpret as arising from a second, non-transiting planet in the system, HD 213885c, whose minimum mass of 19.9 ± 1.4 M_⊙ makes it consistent with being a Neptune-mass exoplanet. The HD 213885 system is very interesting from the perspective of future atmospheric characterization, being the second brightest star to host an USP transiting super-Earth (with the brightest star being, in fact, 55 Cancri). Prospects for characterization with present and future observatories are discussed.

Original language	English (US)
Pages (from-to)	2982-2999
Number of pages	18
Journal	Monthly Notices of the Royal Astronomical Society
Volume	491
Issue number	2
DOIs	https://doi.org/10.1093/mnras/stz3150
State	Published - Jan 1 2020

All Science Journal Classification (ASJC) codes

Astronomy and Astrophysics
Space and Planetary Science

Keywords

HD213885
Planets and satellites: detection
Planets and satellites: fundamental parameters
Planets and satellites: individual: TOI-141
TIC 403224672
Techniques: photometric
Techniques: radial velocities

Access to Document

10.1093/mnras/stz3150

Cite this

Espinoza, N., Brahm, R., Henning, T., Jordán, A., Dorn, C., Rojas, F., Sarkis, P., Kossakowski, D., Schlecker, M., Díaz, M. R., Jenkins, J. S., Aguilera-Gomez, C., Jenkins, J. M., Twicken, J. D., Collins, K. A., Lissauer, J., Armstrong, D. J., Adibekyan, V., Barrado, D., ... Chacon, A. D. (2020). HD 213885b: A transiting 1-d-period super-Earth with an Earth-like composition around a bright (V = 7.9) star unveiled by TESS. Monthly Notices of the Royal Astronomical Society, 491(2), 2982-2999. https://doi.org/10.1093/mnras/stz3150

@article{7093b9a098b143a99c333066f1ead76c,

title = "HD 213885b: A transiting 1-d-period super-Earth with an Earth-like composition around a bright (V = 7.9) star unveiled by TESS",

abstract = "We report the discovery of the 1.008-d, ultrashort period (USP) super-Earth HD 213885b (TOI-141b) orbiting the bright (V= 7.9) star HD 213885 (TOI-141, TIC 403224672), detected using photometry from the recently launched TESS mission. Using FEROS, HARPS, and CORALIE radial velocities, we measure a precise mass of 8.8 ±0.6M⊙ for this 1.74±0.05R⊙ exoplanet, which provides enough information to constrain its bulk composition - similar to Earth's but enriched in iron. The radius, mass, and stellar irradiation of HD 213885b are, given our data, very similar to 55 Cancri e, making this exoplanet a good target to perform comparative exoplanetology of short period, highly irradiated super-Earths. Our precise radial velocities reveal an additional 4.78-d signal which we interpret as arising from a second, non-transiting planet in the system, HD 213885c, whose minimum mass of 19.9 ± 1.4 M⊙ makes it consistent with being a Neptune-mass exoplanet. The HD 213885 system is very interesting from the perspective of future atmospheric characterization, being the second brightest star to host an USP transiting super-Earth (with the brightest star being, in fact, 55 Cancri). Prospects for characterization with present and future observatories are discussed.",

keywords = "HD213885, Planets and satellites: detection, Planets and satellites: fundamental parameters, Planets and satellites: individual: TOI-141, TIC 403224672, Techniques: photometric, Techniques: radial velocities",

author = "N{\'e}stor Espinoza and Rafael Brahm and Thomas Henning and Andr{\'e}s Jord{\'a}n and Caroline Dorn and Felipe Rojas and Paula Sarkis and Diana Kossakowski and Martin Schlecker and D{\'i}az, {Mat{\'i}as R.} and Jenkins, {James S.} and Claudia Aguilera-Gomez and Jenkins, {Jon M.} and Twicken, {Joseph D.} and Collins, {Karen A.} and Jack Lissauer and Armstrong, {David J.} and Vardan Adibekyan and David Barrado and Barros, {Susana C.C.} and Matthew Battley and Daniel Bayliss and Fran{\c c}ois Bouchy and Bryant, {Edward M.} and Cooke, {Benjamin F.} and demangeon, {Olivier D.S.} and Xavier Dumusque and Pedro Figueira and Helen Giles and Jorge Lillo-Box and Christophe Lovis and Nielsen, {Louise D.} and Francesco Pepe and Don Pollacco and Santos, {Nuno C.} and Sousa, {Sergio G.} and St{\'e}phane Udry and Wheatley, {Peter J.} and Oliver Turner and Maxime Marmier and Damien S{\'e}gransan and George Ricker and David Latham and Sara Seager and Winn, {Joshua N.} and Kielkopf, {John F.} and Rhodes Hart and Geof Wingham and Jensen, {Eric L.N.} and He{\l}miniak, {Krzysztof G.} and A. Tokovinin and C. Brice{\~n}o and Carl Ziegler and Law, {Nicholas M.} and Mann, {Andrew W.} and Tansu Daylan and Doty, {John P.} and Natalia Guerrero and Patricia Boyd and Ian Crossfield and Morris, {Robert L.} and Henze, {Christopher E.} and Chacon, {Aaron Dean}",

note = "Funding Information: the NASA Advanced Supercomputing (NAS) Division at Ames Research Center for the production of the SPOC data products. NE would like to thank the Gruber Foundation for its generous support to this research. RB, AJ, and FR acknowledge support from the Ministry for the Economy, Development, and Tourism{\textquoteright}s Programa Iniciativa Cient{\'i}fica Milenio through grant IC 120009, awarded to the Millennium Institute of Astrophysics (MAS). RB acknowledges additional support from FONDECYT Postdoctoral Fellowship Project 3180246. AJ acknowledges additional support from FONDECYT project 1171208. JSJ acknowledges support by FONDECYT grant 1161218 and partial support from CON-ICYT project Basal AFB-170002. CAG acknowledges support from CONICYT FONDECYT Postdoctoral Fellowship Project 3180668. DJA acknowledges support from the STFC via an Ernest Rutherford Fellowship (ST/R00384X/1). XD, HG, CL, LDN, FP, SU, OT, MM, and DS acknowledge Swiss National Science Foundation (SNSF) for the continuous support of the Swiss EULER-Telescope facility. PJW is supported by an STFC consolidated grant (ST/P000495/1). SCCB acknowledges support from FEDER – Fundo Europeu de Desenvolvimento Regional funds through the COMPETE 2020 – Operacional Programme for Competitiveness and Internationalisation (POCI), and by Portuguese funds through FCT – Fundacao para a Ciencia e a Tecnologia in the framework of the project POCI-01-0145-FEDER-028953 and the Investigador FCT contract IF/01312/2014/CP1215/CT0004. NSC acknowledges the support by FCT – Fundacao para a Ciencia e a Tecnologia through national funds and by FEDER through COMPETE2020 – Programa Operacional Competitividade e Internacionalizacao by these grants: UID/FIS/04434/2013 and POCI-01-0145-FEDER-007672; PTDC/FIS-AST/28953/2017 and POCI-01-0145-FEDER-028953; and PTDC/FIS-AST/32113/2017 and POCI-01-0145-FEDER-032113. VA acknowledges support from FCT through Investigador FCT contract IF/00650/2015/CP1273/CT0001. Work by JNW was supported by Heising-Simons foundation. TD acknowledges support from MIT{\textquoteright}s Kavli Institute as a Kavli postdoctoral fellow. This work was made possible thanks to ESO Projects 0101.C-0510(C) (PI: A. Jord{\'a}n), 1102.C-0249(A) (PI: D. Armstrong), 0102.C-0525(A) (PI: M D{\'i}az) and 0102.A-9006(A) (PI: P. Sarkis). CD acknowledges the support of the Swiss National Foundation under grant PZ00P2 174028, and that this work was in part carried out within the frame of the National Center for Competence in Research PlanetS. KGH is supported by the Polish National Science Center through grant no. 2016/21/B/ST9/01613. Funding Information: Funding for the TESS mission is provided by NASA{\textquoteright}s Science Mission directorate. We acknowledge the use of TESS Alert data, which is currently in a beta test phase, from pipelines at the TESS Science Office and at the TESS Science Processing Operations Center. This research has made use of the Exoplanet Follow-up Observation Program website, which is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program. Resources supporting this work were provided by the NASA High-End Computing (HEC) Program through Funding Information: The TESS mission is provided by NASA's Science Mission directorate. We acknowledge the use of TESS Alert data, which is currently in a beta test phase, from pipelines at the TESS Science Office and at the TESS Science Processing Operations Center. This research has made use of the Exoplanet Follow-up Observation Program website, which is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program. 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. NE would like to thank the Gruber Foundation for its generous support to this research. RB, AJ, and FR acknowledge support from the Ministry for the Economy, Development, and Tourism's Programa Iniciativa Cient?fica Milenio through grant IC 120009, awarded to the Millennium Institute of Astrophysics (MAS). RB acknowledges additional support from FONDECYT Postdoctoral Fellowship Project 3180246. AJ acknowledges additional support from FONDECYT project 1171208. JSJ acknowledges support by FONDECYT grant 1161218 and partial support from CONICYT project Basal AFB-170002. CAG acknowledges support from CONICYT FONDECYT Postdoctoral Fellowship Project 3180668. DJA acknowledges support from the STFC via an Ernest Rutherford Fellowship (ST/R00384X/1). XD, HG, CL, LDN, FP, SU, OT, MM, and DS acknowledge Swiss National Science Foundation (SNSF) for the continuous support of the Swiss EULER-Telescope facility. PJW is supported by an STFC consolidated grant (ST/P000495/1). SCCB acknowledges support from FEDER - Fundo Europeu de Desenvolvimento Regional funds through the COMPETE 2020 - Operacional Programme for Competitiveness and Internationalisation (POCI), and by Portuguese funds through FCT - Fundacao para a Ciencia e a Tecnologia in the framework of the project POCI-01-0145-FEDER-028953 and the Investigador FCT contract IF/01312/2014/CP1215/CT0004. NSC acknowledges the support by FCT - Fundacao para a Ciencia e a Tecnologia through national funds and by FEDER through COMPETE2020 - Programa Operacional Competitividade e Internacionalizacao by these grants: UID/FIS/04434/2013 and POCI-01-0145-FEDER-007672; PTDC/FIS-AST/28953/2017 and POCI-01-0145-FEDER-028953; and PTDC/FIS-AST/32113/2017 and POCI-01-0145-FEDER-032113. VA acknowledges support from FCT through Investigador FCT contract IF/00650/2015/CP1273/CT0001. Work by JNW was supported by Heising-Simons foundation. TD acknowledges support from MIT's Kavli Institute as a Kavli postdoctoral fellow. This work was made possible thanks to ESO Projects 0101.C-0510(C) (PI: A. Jord?n), 1102.C-0249(A) (PI: D. Armstrong), 0102.C-0525(A) (PI: M D?az) and 0102.A-9006(A) (PI: P. Sarkis). CD acknowledges the support of the Swiss National Foundation under grant PZ00P2 174028, and that this work was in part carried out within the frame of the National Center for Competence in Research PlanetS. KGH is supported by the Polish National Science Center through grant no. 2016/21/B/ST9/01613. Publisher Copyright: {\textcopyright} 2019 The Author(s).",

year = "2020",

month = jan,

day = "1",

doi = "10.1093/mnras/stz3150",

language = "English (US)",

volume = "491",

pages = "2982--2999",

journal = "Monthly Notices of the Royal Astronomical Society",

issn = "0035-8711",

publisher = "Oxford University Press",

number = "2",

}

Espinoza, N, Brahm, R, Henning, T, Jordán, A, Dorn, C, Rojas, F, Sarkis, P, Kossakowski, D, Schlecker, M, Díaz, MR, Jenkins, JS, Aguilera-Gomez, C, Jenkins, JM, Twicken, JD, Collins, KA, Lissauer, J, Armstrong, DJ, Adibekyan, V, Barrado, D, Barros, SCC, Battley, M, Bayliss, D, Bouchy, F, Bryant, EM, Cooke, BF, demangeon, ODS, Dumusque, X, Figueira, P, Giles, H, Lillo-Box, J, Lovis, C, Nielsen, LD, Pepe, F, Pollacco, D, Santos, NC, Sousa, SG, Udry, S, Wheatley, PJ, Turner, O, Marmier, M, Ségransan, D, Ricker, G, Latham, D, Seager, S, Winn, JN, Kielkopf, JF, Hart, R, Wingham, G, Jensen, ELN, Hełminiak, KG, Tokovinin, A, Briceño, C, Ziegler, C, Law, NM, Mann, AW, Daylan, T, Doty, JP, Guerrero, N, Boyd, P, Crossfield, I, Morris, RL, Henze, CE & Chacon, AD 2020, 'HD 213885b: A transiting 1-d-period super-Earth with an Earth-like composition around a bright (V = 7.9) star unveiled by TESS', Monthly Notices of the Royal Astronomical Society, vol. 491, no. 2, pp. 2982-2999. https://doi.org/10.1093/mnras/stz3150

TY - JOUR

T1 - HD 213885b

T2 - A transiting 1-d-period super-Earth with an Earth-like composition around a bright (V = 7.9) star unveiled by TESS

AU - Espinoza, Néstor

AU - Brahm, Rafael

AU - Henning, Thomas

AU - Jordán, Andrés

AU - Dorn, Caroline

AU - Rojas, Felipe

AU - Sarkis, Paula

AU - Kossakowski, Diana

AU - Schlecker, Martin

AU - Díaz, Matías R.

AU - Jenkins, James S.

AU - Aguilera-Gomez, Claudia

AU - Jenkins, Jon M.

AU - Twicken, Joseph D.

AU - Collins, Karen A.

AU - Lissauer, Jack

AU - Armstrong, David J.

AU - Adibekyan, Vardan

AU - Barrado, David

AU - Barros, Susana C.C.

AU - Battley, Matthew

AU - Bayliss, Daniel

AU - Bouchy, François

AU - Bryant, Edward M.

AU - Cooke, Benjamin F.

AU - demangeon, Olivier D.S.

AU - Dumusque, Xavier

AU - Figueira, Pedro

AU - Giles, Helen

AU - Lillo-Box, Jorge

AU - Lovis, Christophe

AU - Nielsen, Louise D.

AU - Pepe, Francesco

AU - Pollacco, Don

AU - Santos, Nuno C.

AU - Sousa, Sergio G.

AU - Udry, Stéphane

AU - Wheatley, Peter J.

AU - Turner, Oliver

AU - Marmier, Maxime

AU - Ségransan, Damien

AU - Ricker, George

AU - Latham, David

AU - Seager, Sara

AU - Winn, Joshua N.

AU - Kielkopf, John F.

AU - Hart, Rhodes

AU - Wingham, Geof

AU - Jensen, Eric L.N.

AU - Hełminiak, Krzysztof G.

AU - Tokovinin, A.

AU - Briceño, C.

AU - Ziegler, Carl

AU - Law, Nicholas M.

AU - Mann, Andrew W.

AU - Daylan, Tansu

AU - Doty, John P.

AU - Guerrero, Natalia

AU - Boyd, Patricia

AU - Crossfield, Ian

AU - Morris, Robert L.

AU - Henze, Christopher E.

AU - Chacon, Aaron Dean

N1 - Funding Information: the NASA Advanced Supercomputing (NAS) Division at Ames Research Center for the production of the SPOC data products. NE would like to thank the Gruber Foundation for its generous support to this research. RB, AJ, and FR acknowledge support from the Ministry for the Economy, Development, and Tourism’s Programa Iniciativa Científica Milenio through grant IC 120009, awarded to the Millennium Institute of Astrophysics (MAS). RB acknowledges additional support from FONDECYT Postdoctoral Fellowship Project 3180246. AJ acknowledges additional support from FONDECYT project 1171208. JSJ acknowledges support by FONDECYT grant 1161218 and partial support from CON-ICYT project Basal AFB-170002. CAG acknowledges support from CONICYT FONDECYT Postdoctoral Fellowship Project 3180668. DJA acknowledges support from the STFC via an Ernest Rutherford Fellowship (ST/R00384X/1). XD, HG, CL, LDN, FP, SU, OT, MM, and DS acknowledge Swiss National Science Foundation (SNSF) for the continuous support of the Swiss EULER-Telescope facility. PJW is supported by an STFC consolidated grant (ST/P000495/1). SCCB acknowledges support from FEDER – Fundo Europeu de Desenvolvimento Regional funds through the COMPETE 2020 – Operacional Programme for Competitiveness and Internationalisation (POCI), and by Portuguese funds through FCT – Fundacao para a Ciencia e a Tecnologia in the framework of the project POCI-01-0145-FEDER-028953 and the Investigador FCT contract IF/01312/2014/CP1215/CT0004. NSC acknowledges the support by FCT – Fundacao para a Ciencia e a Tecnologia through national funds and by FEDER through COMPETE2020 – Programa Operacional Competitividade e Internacionalizacao by these grants: UID/FIS/04434/2013 and POCI-01-0145-FEDER-007672; PTDC/FIS-AST/28953/2017 and POCI-01-0145-FEDER-028953; and PTDC/FIS-AST/32113/2017 and POCI-01-0145-FEDER-032113. VA acknowledges support from FCT through Investigador FCT contract IF/00650/2015/CP1273/CT0001. Work by JNW was supported by Heising-Simons foundation. TD acknowledges support from MIT’s Kavli Institute as a Kavli postdoctoral fellow. This work was made possible thanks to ESO Projects 0101.C-0510(C) (PI: A. Jordán), 1102.C-0249(A) (PI: D. Armstrong), 0102.C-0525(A) (PI: M Díaz) and 0102.A-9006(A) (PI: P. Sarkis). CD acknowledges the support of the Swiss National Foundation under grant PZ00P2 174028, and that this work was in part carried out within the frame of the National Center for Competence in Research PlanetS. KGH is supported by the Polish National Science Center through grant no. 2016/21/B/ST9/01613. Funding Information: Funding for the TESS mission is provided by NASA’s Science Mission directorate. We acknowledge the use of TESS Alert data, which is currently in a beta test phase, from pipelines at the TESS Science Office and at the TESS Science Processing Operations Center. This research has made use of the Exoplanet Follow-up Observation Program website, which is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program. Resources supporting this work were provided by the NASA High-End Computing (HEC) Program through Funding Information: The TESS mission is provided by NASA's Science Mission directorate. We acknowledge the use of TESS Alert data, which is currently in a beta test phase, from pipelines at the TESS Science Office and at the TESS Science Processing Operations Center. This research has made use of the Exoplanet Follow-up Observation Program website, which is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program. 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. NE would like to thank the Gruber Foundation for its generous support to this research. RB, AJ, and FR acknowledge support from the Ministry for the Economy, Development, and Tourism's Programa Iniciativa Cient?fica Milenio through grant IC 120009, awarded to the Millennium Institute of Astrophysics (MAS). RB acknowledges additional support from FONDECYT Postdoctoral Fellowship Project 3180246. AJ acknowledges additional support from FONDECYT project 1171208. JSJ acknowledges support by FONDECYT grant 1161218 and partial support from CONICYT project Basal AFB-170002. CAG acknowledges support from CONICYT FONDECYT Postdoctoral Fellowship Project 3180668. DJA acknowledges support from the STFC via an Ernest Rutherford Fellowship (ST/R00384X/1). XD, HG, CL, LDN, FP, SU, OT, MM, and DS acknowledge Swiss National Science Foundation (SNSF) for the continuous support of the Swiss EULER-Telescope facility. PJW is supported by an STFC consolidated grant (ST/P000495/1). SCCB acknowledges support from FEDER - Fundo Europeu de Desenvolvimento Regional funds through the COMPETE 2020 - Operacional Programme for Competitiveness and Internationalisation (POCI), and by Portuguese funds through FCT - Fundacao para a Ciencia e a Tecnologia in the framework of the project POCI-01-0145-FEDER-028953 and the Investigador FCT contract IF/01312/2014/CP1215/CT0004. NSC acknowledges the support by FCT - Fundacao para a Ciencia e a Tecnologia through national funds and by FEDER through COMPETE2020 - Programa Operacional Competitividade e Internacionalizacao by these grants: UID/FIS/04434/2013 and POCI-01-0145-FEDER-007672; PTDC/FIS-AST/28953/2017 and POCI-01-0145-FEDER-028953; and PTDC/FIS-AST/32113/2017 and POCI-01-0145-FEDER-032113. VA acknowledges support from FCT through Investigador FCT contract IF/00650/2015/CP1273/CT0001. Work by JNW was supported by Heising-Simons foundation. TD acknowledges support from MIT's Kavli Institute as a Kavli postdoctoral fellow. This work was made possible thanks to ESO Projects 0101.C-0510(C) (PI: A. Jord?n), 1102.C-0249(A) (PI: D. Armstrong), 0102.C-0525(A) (PI: M D?az) and 0102.A-9006(A) (PI: P. Sarkis). CD acknowledges the support of the Swiss National Foundation under grant PZ00P2 174028, and that this work was in part carried out within the frame of the National Center for Competence in Research PlanetS. KGH is supported by the Polish National Science Center through grant no. 2016/21/B/ST9/01613. Publisher Copyright: © 2019 The Author(s).

PY - 2020/1/1

Y1 - 2020/1/1

N2 - We report the discovery of the 1.008-d, ultrashort period (USP) super-Earth HD 213885b (TOI-141b) orbiting the bright (V= 7.9) star HD 213885 (TOI-141, TIC 403224672), detected using photometry from the recently launched TESS mission. Using FEROS, HARPS, and CORALIE radial velocities, we measure a precise mass of 8.8 ±0.6M⊙ for this 1.74±0.05R⊙ exoplanet, which provides enough information to constrain its bulk composition - similar to Earth's but enriched in iron. The radius, mass, and stellar irradiation of HD 213885b are, given our data, very similar to 55 Cancri e, making this exoplanet a good target to perform comparative exoplanetology of short period, highly irradiated super-Earths. Our precise radial velocities reveal an additional 4.78-d signal which we interpret as arising from a second, non-transiting planet in the system, HD 213885c, whose minimum mass of 19.9 ± 1.4 M⊙ makes it consistent with being a Neptune-mass exoplanet. The HD 213885 system is very interesting from the perspective of future atmospheric characterization, being the second brightest star to host an USP transiting super-Earth (with the brightest star being, in fact, 55 Cancri). Prospects for characterization with present and future observatories are discussed.

AB - We report the discovery of the 1.008-d, ultrashort period (USP) super-Earth HD 213885b (TOI-141b) orbiting the bright (V= 7.9) star HD 213885 (TOI-141, TIC 403224672), detected using photometry from the recently launched TESS mission. Using FEROS, HARPS, and CORALIE radial velocities, we measure a precise mass of 8.8 ±0.6M⊙ for this 1.74±0.05R⊙ exoplanet, which provides enough information to constrain its bulk composition - similar to Earth's but enriched in iron. The radius, mass, and stellar irradiation of HD 213885b are, given our data, very similar to 55 Cancri e, making this exoplanet a good target to perform comparative exoplanetology of short period, highly irradiated super-Earths. Our precise radial velocities reveal an additional 4.78-d signal which we interpret as arising from a second, non-transiting planet in the system, HD 213885c, whose minimum mass of 19.9 ± 1.4 M⊙ makes it consistent with being a Neptune-mass exoplanet. The HD 213885 system is very interesting from the perspective of future atmospheric characterization, being the second brightest star to host an USP transiting super-Earth (with the brightest star being, in fact, 55 Cancri). Prospects for characterization with present and future observatories are discussed.

KW - HD213885

KW - Planets and satellites: detection

KW - Planets and satellites: fundamental parameters

KW - Planets and satellites: individual: TOI-141

KW - TIC 403224672

KW - Techniques: photometric

KW - Techniques: radial velocities

UR - http://www.scopus.com/inward/record.url?scp=85079690485&partnerID=8YFLogxK

UR - http://www.scopus.com/inward/citedby.url?scp=85079690485&partnerID=8YFLogxK

U2 - 10.1093/mnras/stz3150

DO - 10.1093/mnras/stz3150

M3 - Article

AN - SCOPUS:85079690485

SN - 0035-8711

VL - 491

SP - 2982

EP - 2999

JO - Monthly Notices of the Royal Astronomical Society

JF - Monthly Notices of the Royal Astronomical Society

IS - 2

ER -

HD 213885b: A transiting 1-d-period super-Earth with an Earth-like composition around a bright (V = 7.9) star unveiled by TESS

Abstract

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