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 | |
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
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In: Monthly Notices of the Royal Astronomical Society, Vol. 491, No. 2, 01.01.2020, p. 2982-2999.
Research output: Contribution to journal › Article › peer-review
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 -