Transit detection of the long-period volatile-rich super-Earth ν2 Lupi d with CHEOPS

Delrez, Laetitia; Ehrenreich, D.; Alibert, Yann; Bonfanti, A.; Borsato, L.; Fossati, L.; Hooton, Matthew J.; Hoyer, S.; Pozuelos, F. J.; Salmon, Sébastien; Sulis, S.; Wilson, T. G.; Adibekyan, V.; Bourrier, V.; Brandeker, Alexis; Charnoz, Sébastien; Deline, A.; Guterman, P.; Haldemann, Jonas; Hara, N.; Oshagh, M.; Sousa, S. G.; Grootel, Valérie Van; Alonso, R.; Anglada-Escudé, G.; Bárczy, T.; Barrado, D.; Barros, S. C. C.; Baumjohann, W.; Beck, M.; Bekkelien, A.; Benz, W.; Billot, N.; Bonfils, X.; Broeg, C.; Cabrera, J.; Cameron, A. Collier; Davies, Melvyn B.; Deleuil, M.; Delisle, J.-B.; Demangeon, O.; Demory, Brice-Olivier; Erikson, A.; Fortier, A.; Fridlund, M.; Futyan, D.; Gandolfi, D.; Muñoz, A. García; Gillon, M.; Guêdel, M.; Heng, Kevin; Kiss, L. L.; Laskar, Jacques; Étangs, A. Lecavelier des; Lendl, M.; Lovis, C.; Maxted, P. F. L.; Nascimbeni, V.; Olofsson, G.; Osborn, H.; Pagano, I.; Πάλλη, Ε.; Piotto, G.; Pollacco, D.; Queloz, D.; Rauer, H.; Ragazzoni, Roberto; Ribas, I.; Santos, N. C.; Scandariato, G.; Ségransan, D.; Simon, A. E.; Smith, A. M. S.; Steller, M.; Szabó, Gyula; Thomas, Nicolas; Udry, S.; Walton, N. A.

doi:10.1038/s41550-021-01381-5

Cited by 67 publications

(56 citation statements)

References 145 publications

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“…CHEOPS met its precision requirements both on bright and faint stars, achieving a noise level of ∼ 15 ppm per 6 h intervals for 𝑉 ∼ 9 mag stars, and 75 ppm per 3 h for 𝑉 ∼ 12 mag stars (Benz et al 2021). The importance of such a high photometric precision is reflected in CHEOPS' first scientific results, which span a variety of different fields (Lendl et al 2020;Bonfanti et al 2021b;Leleu et al 2021;Delrez et al 2021;Morris et al 2021a;Borsato et al 2021;Van Grootel et al 2021;Szabó et al 2021;Hooton et al 2021;Swayne et al 2021;Maxted et al 2021;Barros et al 2022;Wilson et al 2022;Deline et al 2022). As part of its main scientific goals, CHEOPS is refining the radii of known exoplanets to achieve the precision on the bulk density needed for internal structure and atmospheric evolution modelling.…”

Section: Introductionmentioning

confidence: 99%

Investigating the architecture and internal structure of the TOI-561 system planets with CHEOPS, HARPS-N and TESS

Lacedelli,

Wilson,

Malavolta

et al. 2022

Preprint

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We present a precise characterization of the TOI-561 planetary system obtained by combining previously published data with TESS and CHEOPS photometry, and a new set of 62 HARPS-N radial velocities (RVs). Our joint analysis confirms the presence of four transiting planets, namely TOI-561 b (𝑃 = 0.45 d, 𝑅 = 1.42 R ⊕ , 𝑀 = 2.0 M ⊕ ), c (𝑃 = 10.78 d, 𝑅 = 2.91 R ⊕ , 𝑀 = 5.4 M ⊕ ), d (𝑃 = 25.7 d, 𝑅 = 2.82 R ⊕ , 𝑀 = 13.2 M ⊕ ) and e (𝑃 = 77 d, 𝑅 = 2.55 R ⊕ , 𝑀 = 12.6 R ⊕ ). Moreover, we identify an additional, long-period signal (> 450 d) in the RVs, which could be due to either an external planetary companion or to stellar magnetic activity. The precise masses and radii obtained for the four planets allowed us to conduct interior structure and atmospheric escape modelling. TOI-561 b is confirmed to be the lowest density (𝜌 b = 3.8 ± 0.5 g cm −3 ) ultra-short period (USP) planet known to date, and the low metallicity of the host star makes it consistent with the general bulk density-stellar metallicity trend. According to our interior structure modelling, planet b has basically no gas envelope, and it could host a certain amount of water. In contrast, TOI-561 c, d, and e likely retained an H/He envelope, in addition to a possibly large water layer. The inferred planetary compositions suggest different atmospheric evolutionary paths, with planets b and c having experienced significant gas loss, and planets d and e showing an atmospheric content consistent with the original one. The uniqueness of the USP planet, the presence of the long-period planet TOI-561 e, and the complex architecture make this system an appealing target for follow-up studies.

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Section: Introductionmentioning

confidence: 99%

Investigating the architecture and internal structure of the TOI-561 system planets with CHEOPS, HARPS-N and TESS

Lacedelli,

Wilson,

Malavolta

et al. 2022

Preprint

View full text Add to dashboard Cite

show abstract

“…CHEOPS met its precision requirements both on bright and faint stars, achieving a noise level of ∼ 15 ppm per 6 h intervals for ∼ 9 mag stars, and 75 ppm per 3 h for ∼ 12 mag stars (Benz et al 2021). The importance of such a high photometric precision is reflected in CHEOPS' first scientific results, which span a variety of different fields (Lendl et al 2020;Bonfanti et al 2021b;Leleu et al 2021;Delrez et al 2021;Morris et al 2021a;Borsato et al 2021;Van Grootel et al 2021;Szabó et al 2021;Hooton et al 2021;Swayne et al 2021;Maxted et al 2021;Barros et al 2022;Wilson et al 2022;Deline et al 2022).…”

mentioning

confidence: 99%

Investigating the architecture and internal structure of the TOI-561 system planets with CHEOPS, HARPS-N, and TESS

Lacedelli

Wilson

Malavolta

et al. 2022

Monthly Notices of the Royal Astronomical Society

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We present a precise characterization of the TOI-561 planetary system obtained by combining previously published data with TESS and CHEOPS photometry, and a new set of 62 HARPS-N radial velocities (RVs). Our joint analysis confirms the presence of four transiting planets, namely TOI-561 b (P = 0.45 d, R = 1.42 R⊕, M = 2.0 M⊕), c (P = 10.78 d, R = 2.91 R⊕, M = 5.4 M⊕), d (P = 25.7 d, R = 2.82 R⊕, M = 13.2 M⊕) and e (P = 77 d, R = 2.55 R⊕, M = 12.6 R⊕). Moreover, we identify an additional, long-period signal (>450 d) in the RVs, which could be due to either an external planetary companion or to stellar magnetic activity. The precise masses and radii obtained for the four planets allowed us to conduct interior structure and atmospheric escape modelling. TOI-561 b is confirmed to be the lowest density (ρb = 3.8 ± 0.5 g cm−3) ultra-short period (USP) planet known to date, and the low metallicity of the host star makes it consistent with the general bulk density-stellar metallicity trend. According to our interior structure modelling, planet b has basically no gas envelope, and it could host a certain amount of water. In contrast, TOI-561 c, d, and e likely retained an H/He envelope, in addition to a possibly large water layer. The inferred planetary compositions suggest different atmospheric evolutionary paths, with planets b and c having experienced significant gas loss, and planets d and e showing an atmospheric content consistent with the original one. The uniqueness of the USP planet, the presence of the long-period planet TOI-561 e, and the complex architecture make this system an appealing target for follow-up studies.

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“…Several studies (e.g. Lendl et al 2020;Bonfanti et al 2021;Delrez et al 2021;Leleu et al 2021) have found success in removing these systematics by conducting a linear decorrelation using several basis vectors, such as background, contamination, orbital roll angle, and 𝑥 and 𝑦 centroid positions. Upon inspection of the CHEOPS observations of TOI-1064, we found significant flux variations on orbital timescales.…”

Section: Cheopsmentioning

confidence: 99%

“…After rejecting those thats do not fulfil the constraint imposed by the present-day atmospheric content derived in Section 5.1, we obtained the posterior distributions of the free parameters. Further details about the tool may be found in Delrez et al (2021). The results of the joint evolution of both planet b and c are shown in Figs.…”

Section: Atmospheric Evolutionmentioning

confidence: 99%

“…The first scientific results from CHEOPS show the range of science that can be achieved with such a high-precision instrument (Lendl et al 2020;Borsato et al 2021;Delrez et al 2021;Leleu et al 2021;Morris et al 2021;Szabó et al 2021;Van Grootel et al 2021;Maxted et al accepted). One such study reports on the improvement in precision of exoplanet sizes in the HD 108236 system (Bonfanti et al 2021), that highlights a key scientific goal of the CHEOPS mission: the refinement of exoplanet radii to decrease bulk density uncertainties, and thereby allowing internal structure and atmospheric evolution modelling.…”

Section: Cheopsmentioning

confidence: 99%

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A pair of Sub-Neptunes transiting the bright K-dwarf TOI-1064 characterised with CHEOPS

Wilson,

Goffo,

Alibert

et al. 2022

Preprint

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We report the discovery and characterisation of a pair of sub-Neptunes transiting the bright K-dwarf TOI-1064 (TIC 79748331), initially detected in TESS photometry. To characterise the system, we performed and retrieved CHEOPS, TESS, and ground-based photometry, HARPS high-resolution spectroscopy, and Gemini speckle imaging. We characterise the host star and determine 𝑇 eff,★ = 4734 ± 67 K, 𝑅 ★ = 0.726 ± 0.007 𝑅 , and 𝑀 ★ = 0.748 ± 0.032 𝑀 . We present a novel detrending method based on PSF shape-change modelling and demonstrate its suitability to correct flux variations in CHEOPS data. We confirm the planetary nature of both bodies and find that TOI-1064 b has an orbital period of 𝑃 b = 6.44387 ± 0.00003 d, a radius of 𝑅 b = 2.59 ± 0.04 𝑅 ⊕ , and a mass of 𝑀 b = 13.5 +1.7 −1.8 𝑀 ⊕ , whilst TOI-1064 c has an orbital period of 𝑃 c = 12.22657 +0.00005 −0.00004 d, a radius of 𝑅 c = 2.65 ± 0.04 𝑅 ⊕ , and a 3𝜎 upper mass limit of 8.5 M ⊕ . From the high-precision photometry we obtain radius uncertainties of ∼1.6%, allowing us to conduct internal structure and atmospheric escape modelling. TOI-1064 b is one of the densest, well-characterised sub-Neptunes, with a tenuous atmosphere that can be explained by the loss of a primordial envelope following migration through the protoplanetary disc. It is likely that TOI-1064 c has an extended atmosphere due to the tentative low density, however further RVs are needed to confirm this scenario and the similar radii, different masses nature of this system. The high-precision data and modelling of TOI-1064 b is important for planets in this region of mass-radius space, and it allows us to identify a trend in bulk density-stellar metallicity for massive sub-Neptunes that may hint at the formation of this population of planets.

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Transit detection of the long-period volatile-rich super-Earth ν2 Lupi d with CHEOPS

Cited by 67 publications

References 145 publications

Investigating the architecture and internal structure of the TOI-561 system planets with CHEOPS, HARPS-N and TESS

Investigating the architecture and internal structure of the TOI-561 system planets with CHEOPS, HARPS-N and TESS

Investigating the architecture and internal structure of the TOI-561 system planets with CHEOPS, HARPS-N, and TESS

A pair of Sub-Neptunes transiting the bright K-dwarf TOI-1064 characterised with CHEOPS

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