Transiting exoplanets from the CoRoT space mission: XXIV. CoRoT-25b and CoRoT-26b: Two low-density giant planets

J. M. Almenara; F. Bouchy; P. Gaulme; M. Deleuil; M. Havel; D. Gandolfi; H. J. Deeg; G. Wuchterl; T. Guillot; B. Gardes; T. Pasternacki; S. Aigrain; R. Alonso; M. Auvergne; A. Baglin; A. S. Bonomo; P. Bordé; J. Cabrera; S. Carpano; W. D. Cochran; Sz Csizmadia; C. Damiani; R. F. Diaz; R. Dvorak; M. Endl; A. Erikson; S. Ferraz-Mello; M. Fridlund; G. Hébrard; M. Gillon; E. Guenther; A. Hatzes; A. Léger; H. Lammer; P. J. MacQueen; T. Mazeh; C. Moutou; M. Ollivier; A. Ofir; M. Pätzold; H. Parviainen; D. Queloz; H. Rauer; D. Rouan; A. Santerne; B. Samuel; J. Schneider; L. Tal-Or; B. Tingley; J. Weingrill

doi:10.1051/0004-6361/201321462

Transiting exoplanets from the CoRoT space mission: XXIV. CoRoT-25b and CoRoT-26b: Two low-density giant planets

J. M. Almenara
, F. Bouchy
, P. Gaulme
, M. Deleuil
, M. Havel
, D. Gandolfi
, H. J. Deeg
, G. Wuchterl
, T. Guillot
, B. Gardes
, T. Pasternacki
, S. Aigrain
, R. Alonso
, M. Auvergne
, A. Baglin
, A. S. Bonomo
, P. Bordé
, J. Cabrera
, S. Carpano
, W. D. Cochran

Sz Csizmadia, C. Damiani, R. F. Diaz, R. Dvorak, M. Endl, A. Erikson, S. Ferraz-Mello, M. Fridlund, G. Hébrard, M. Gillon, E. Guenther, A. Hatzes, A. Léger, H. Lammer, P. J. MacQueen, T. Mazeh, C. Moutou, M. Ollivier, A. Ofir, M. Pätzold, H. Parviainen, D. Queloz, H. Rauer, D. Rouan, A. Santerne, B. Samuel, J. Schneider, L. Tal-Or, B. Tingley, J. Weingrill

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

15 Scopus citations

Abstract

We report the discovery of two transiting exoplanets, CoRoT-25b and CoRoT-26b, both of low density, one of which is in the Saturn mass-regime. For each star, ground-based complementary observations through optical photometry and radial velocity measurements secured the planetary nature of the transiting body and allowed us to fully characterize them. For CoRoT-25b we found a planetary mass of 0.27 ± 0.04 M_Jup, a radius of 1.08 _-0.10^+0.3 R_Jup and hence a mean density of 0.15_-0.06^+0.15 g cm^-3. The planet orbits an F9 main-sequence star in a 4.86-day period, that has a V magnitude of 15.0, solar metallicity, and an age of 4.5_-2.0^+1.8-Gyr. CoRoT-26b orbits a slightly evolved G5 star of 9.06 ± 1.5-Gyr age in a 4.20-day period that hassolar metallicity and a V magnitude of 15.8. With a mass of 0.52 ± 0.05 M_Jup, a radius of 1.26_-0.07^+0.13 R_Jup, and a mean density of 0.28_-0.07^+0.09 g cm^-3, it belongs to the low-mass hot-Jupiter population. Planetary evolution models allowed us to estimate a core mass of a few tens of Earth mass for the two planets with heavy-element mass fractions of 0.52 _-0.15^+0.08 and 0.26_-0.08^+0.05, respectively, assuming that a small fraction of the incoming flux is dissipated at the center of the planet. In addition, these models indicate that CoRoT-26b is anomalously large compared with what standard models could account for, indicating that dissipation from stellar heating could cause this size.

Original language	English
Article number	A118
Journal	Astronomy and Astrophysics
Volume	555
DOIs	https://doi.org/10.1051/0004-6361/201321462
State	Published - 2013

Funding

Funders	Funder number
???publication-publication-funding-organisation-not-added???	ST/G002266/1
National Aeronautics and Space Administration
W. M. Keck Foundation
Ames Research Center
Oak Ridge Associated Universities
NASA Exoplanet Science Institute
Science and Technology Facilities Council	ST/G002266/2
Schweizerischer Nationalfonds zur Förderung der Wissenschaftlichen Forschung	140442
Ministerio de Economía y Competitividad

Keywords

Planetary systems
Techniques: photometric
Techniques: radial velocities
Techniques: spectroscopic

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10.1051/0004-6361/201321462

Cite this

Almenara, J. M., Bouchy, F., Gaulme, P., Deleuil, M., Havel, M., Gandolfi, D., Deeg, H. J., Wuchterl, G., Guillot, T., Gardes, B., Pasternacki, T., Aigrain, S., Alonso, R., Auvergne, M., Baglin, A., Bonomo, A. S., Bordé, P., Cabrera, J., Carpano, S., ... Weingrill, J. (2013). Transiting exoplanets from the CoRoT space mission: XXIV. CoRoT-25b and CoRoT-26b: Two low-density giant planets. Astronomy and Astrophysics, 555, Article A118. https://doi.org/10.1051/0004-6361/201321462

@article{1d923a6eab4c427a93c88fc14c53df23,

title = "Transiting exoplanets from the CoRoT space mission: XXIV. CoRoT-25b and CoRoT-26b: Two low-density giant planets",

abstract = "We report the discovery of two transiting exoplanets, CoRoT-25b and CoRoT-26b, both of low density, one of which is in the Saturn mass-regime. For each star, ground-based complementary observations through optical photometry and radial velocity measurements secured the planetary nature of the transiting body and allowed us to fully characterize them. For CoRoT-25b we found a planetary mass of 0.27 ± 0.04 MJup, a radius of 1.08 -0.10+0.3 RJup and hence a mean density of 0.15-0.06+0.15 g cm-3. The planet orbits an F9 main-sequence star in a 4.86-day period, that has a V magnitude of 15.0, solar metallicity, and an age of 4.5-2.0+1.8-Gyr. CoRoT-26b orbits a slightly evolved G5 star of 9.06 ± 1.5-Gyr age in a 4.20-day period that hassolar metallicity and a V magnitude of 15.8. With a mass of 0.52 ± 0.05 MJup, a radius of 1.26-0.07+0.13 RJup, and a mean density of 0.28-0.07+0.09 g cm-3, it belongs to the low-mass hot-Jupiter population. Planetary evolution models allowed us to estimate a core mass of a few tens of Earth mass for the two planets with heavy-element mass fractions of 0.52 -0.15+0.08 and 0.26-0.08+0.05, respectively, assuming that a small fraction of the incoming flux is dissipated at the center of the planet. In addition, these models indicate that CoRoT-26b is anomalously large compared with what standard models could account for, indicating that dissipation from stellar heating could cause this size.",

keywords = "Planetary systems, Techniques: photometric, Techniques: radial velocities, Techniques: spectroscopic",

author = "Almenara, \{J. M.\} and F. Bouchy and P. Gaulme and M. Deleuil and M. Havel and D. Gandolfi and Deeg, \{H. J.\} and G. Wuchterl and T. Guillot and B. Gardes and T. Pasternacki and S. Aigrain and R. Alonso and M. Auvergne and A. Baglin and Bonomo, \{A. S.\} and P. Bord{\'e} and J. Cabrera and S. Carpano and Cochran, \{W. D.\} and Sz Csizmadia and C. Damiani and Diaz, \{R. F.\} and R. Dvorak and M. Endl and A. Erikson and S. Ferraz-Mello and M. Fridlund and G. H{\'e}brard and M. Gillon and E. Guenther and A. Hatzes and A. L{\'e}ger and H. Lammer and MacQueen, \{P. J.\} and T. Mazeh and C. Moutou and M. Ollivier and A. Ofir and M. P{\"a}tzold and H. Parviainen and D. Queloz and H. Rauer and D. Rouan and A. Santerne and B. Samuel and J. Schneider and L. Tal-Or and B. Tingley and J. Weingrill",

note = "Funding Information: The team at IAC acknowledges support by grants AYA2010-20982-C02-02 and AYA2012-39346-C02-02 of the Spanish Ministerio de Econom{\'i}a y Competividad. Some of the data presented was acquired with the IAC80 telescope operated at Teide Observatory on the island of Tenerife by the Instituto de Astrof{\'i}sica de Canarias. This research has made use of the Exoplanet Orbit Database and the Exoplanet Data Explorer at exoplanets.org. Part of this work was supported by a NASA Keck PI Data Award, administered by the NASA Exoplanet Science Institute. Some of the data presented herein were obtained at the W.M. Keck Observatory from telescope time allocated to the National Aeronautics and Space Administration through the agency{\textquoteright}s scientific partnership with the California Institute of Technology and the University of California. The Observatory was made possible by the generous financial support of the W.M. Keck Foundation. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. This research was supported by an appointment to the NASA Postdoctoral Program at the Ames Research Center, administered by Oak Ridge Associated Universities through a contract with NASA.",

year = "2013",

doi = "10.1051/0004-6361/201321462",

language = "אנגלית",

volume = "555",

journal = "Astronomy and Astrophysics",

issn = "0004-6361",

publisher = "EDP Sciences",

}

Almenara, JM, Bouchy, F, Gaulme, P, Deleuil, M, Havel, M, Gandolfi, D, Deeg, HJ, Wuchterl, G, Guillot, T, Gardes, B, Pasternacki, T, Aigrain, S, Alonso, R, Auvergne, M, Baglin, A, Bonomo, AS, Bordé, P, Cabrera, J, Carpano, S, Cochran, WD, Csizmadia, S, Damiani, C, Diaz, RF, Dvorak, R, Endl, M, Erikson, A, Ferraz-Mello, S, Fridlund, M, Hébrard, G, Gillon, M, Guenther, E, Hatzes, A, Léger, A, Lammer, H, MacQueen, PJ, Mazeh, T, Moutou, C, Ollivier, M, Ofir, A, Pätzold, M, Parviainen, H, Queloz, D, Rauer, H, Rouan, D, Santerne, A, Samuel, B, Schneider, J, Tal-Or, L, Tingley, B & Weingrill, J 2013, 'Transiting exoplanets from the CoRoT space mission: XXIV. CoRoT-25b and CoRoT-26b: Two low-density giant planets', Astronomy and Astrophysics, vol. 555, A118. https://doi.org/10.1051/0004-6361/201321462

TY - JOUR

T1 - Transiting exoplanets from the CoRoT space mission

T2 - XXIV. CoRoT-25b and CoRoT-26b: Two low-density giant planets

AU - Almenara, J. M.

AU - Bouchy, F.

AU - Gaulme, P.

AU - Deleuil, M.

AU - Havel, M.

AU - Gandolfi, D.

AU - Deeg, H. J.

AU - Wuchterl, G.

AU - Guillot, T.

AU - Gardes, B.

AU - Pasternacki, T.

AU - Aigrain, S.

AU - Alonso, R.

AU - Auvergne, M.

AU - Baglin, A.

AU - Bonomo, A. S.

AU - Bordé, P.

AU - Cabrera, J.

AU - Carpano, S.

AU - Cochran, W. D.

AU - Csizmadia, Sz

AU - Damiani, C.

AU - Diaz, R. F.

AU - Dvorak, R.

AU - Endl, M.

AU - Erikson, A.

AU - Ferraz-Mello, S.

AU - Fridlund, M.

AU - Hébrard, G.

AU - Gillon, M.

AU - Guenther, E.

AU - Hatzes, A.

AU - Léger, A.

AU - Lammer, H.

AU - MacQueen, P. J.

AU - Mazeh, T.

AU - Moutou, C.

AU - Ollivier, M.

AU - Ofir, A.

AU - Pätzold, M.

AU - Parviainen, H.

AU - Queloz, D.

AU - Rauer, H.

AU - Rouan, D.

AU - Santerne, A.

AU - Samuel, B.

AU - Schneider, J.

AU - Tal-Or, L.

AU - Tingley, B.

AU - Weingrill, J.

N1 - Funding Information: The team at IAC acknowledges support by grants AYA2010-20982-C02-02 and AYA2012-39346-C02-02 of the Spanish Ministerio de Economía y Competividad. Some of the data presented was acquired with the IAC80 telescope operated at Teide Observatory on the island of Tenerife by the Instituto de Astrofísica de Canarias. This research has made use of the Exoplanet Orbit Database and the Exoplanet Data Explorer at exoplanets.org. Part of this work was supported by a NASA Keck PI Data Award, administered by the NASA Exoplanet Science Institute. Some of the data presented herein were obtained at the W.M. Keck Observatory from telescope time allocated to the National Aeronautics and Space Administration through the agency’s scientific partnership with the California Institute of Technology and the University of California. The Observatory was made possible by the generous financial support of the W.M. Keck Foundation. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. This research was supported by an appointment to the NASA Postdoctoral Program at the Ames Research Center, administered by Oak Ridge Associated Universities through a contract with NASA.

PY - 2013

Y1 - 2013

N2 - We report the discovery of two transiting exoplanets, CoRoT-25b and CoRoT-26b, both of low density, one of which is in the Saturn mass-regime. For each star, ground-based complementary observations through optical photometry and radial velocity measurements secured the planetary nature of the transiting body and allowed us to fully characterize them. For CoRoT-25b we found a planetary mass of 0.27 ± 0.04 MJup, a radius of 1.08 -0.10+0.3 RJup and hence a mean density of 0.15-0.06+0.15 g cm-3. The planet orbits an F9 main-sequence star in a 4.86-day period, that has a V magnitude of 15.0, solar metallicity, and an age of 4.5-2.0+1.8-Gyr. CoRoT-26b orbits a slightly evolved G5 star of 9.06 ± 1.5-Gyr age in a 4.20-day period that hassolar metallicity and a V magnitude of 15.8. With a mass of 0.52 ± 0.05 MJup, a radius of 1.26-0.07+0.13 RJup, and a mean density of 0.28-0.07+0.09 g cm-3, it belongs to the low-mass hot-Jupiter population. Planetary evolution models allowed us to estimate a core mass of a few tens of Earth mass for the two planets with heavy-element mass fractions of 0.52 -0.15+0.08 and 0.26-0.08+0.05, respectively, assuming that a small fraction of the incoming flux is dissipated at the center of the planet. In addition, these models indicate that CoRoT-26b is anomalously large compared with what standard models could account for, indicating that dissipation from stellar heating could cause this size.

AB - We report the discovery of two transiting exoplanets, CoRoT-25b and CoRoT-26b, both of low density, one of which is in the Saturn mass-regime. For each star, ground-based complementary observations through optical photometry and radial velocity measurements secured the planetary nature of the transiting body and allowed us to fully characterize them. For CoRoT-25b we found a planetary mass of 0.27 ± 0.04 MJup, a radius of 1.08 -0.10+0.3 RJup and hence a mean density of 0.15-0.06+0.15 g cm-3. The planet orbits an F9 main-sequence star in a 4.86-day period, that has a V magnitude of 15.0, solar metallicity, and an age of 4.5-2.0+1.8-Gyr. CoRoT-26b orbits a slightly evolved G5 star of 9.06 ± 1.5-Gyr age in a 4.20-day period that hassolar metallicity and a V magnitude of 15.8. With a mass of 0.52 ± 0.05 MJup, a radius of 1.26-0.07+0.13 RJup, and a mean density of 0.28-0.07+0.09 g cm-3, it belongs to the low-mass hot-Jupiter population. Planetary evolution models allowed us to estimate a core mass of a few tens of Earth mass for the two planets with heavy-element mass fractions of 0.52 -0.15+0.08 and 0.26-0.08+0.05, respectively, assuming that a small fraction of the incoming flux is dissipated at the center of the planet. In addition, these models indicate that CoRoT-26b is anomalously large compared with what standard models could account for, indicating that dissipation from stellar heating could cause this size.

KW - Planetary systems

KW - Techniques: photometric

KW - Techniques: radial velocities

KW - Techniques: spectroscopic

UR - https://www.scopus.com/pages/publications/84880120954

U2 - 10.1051/0004-6361/201321462

DO - 10.1051/0004-6361/201321462

M3 - ???researchoutput.researchoutputtypes.contributiontojournal.article???

AN - SCOPUS:84880120954

SN - 0004-6361

VL - 555

JO - Astronomy and Astrophysics

JF - Astronomy and Astrophysics

M1 - A118

ER -

Transiting exoplanets from the CoRoT space mission: XXIV. CoRoT-25b and CoRoT-26b: Two low-density giant planets

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