CHEOPS precision phase curve of the Super-Earth 55 Cancri e

B. M. Morris; L. Delrez; A. Brandeker; A. C. Cameron; A. E. Simon; D. Futyan; G. Olofsson; S. Hoyer; A. Fortier; B.-O. Demory; M. Lendl; T. G. Wilson; M. Oshagh; K. Heng; D. Ehrenreich; S. Sulis; Y. Alibert; R. Alonso; G. Anglada Escudé; D. Barrado; S. C. C. Barros; W. Baumjohann; M. Beck; T. Beck; A. Bekkelien; W. Benz; M. Bergomi; N. Billot; X. Bonfils; V. Bourrier; C. Broeg; T. Bárczy; J. Cabrera; S. Charnoz; M. B. Davies; D. De Miguel Ferreras; M. Deleuil; A. Deline; O. D. S. Demangeon; A. Erikson; H. G. Floren; L. Fossati; M. Fridlund; D. Gandolfi; A. García Muñoz; M. Gillon; M. Guedel; P. Guterman; K. Isaak; L. Kiss; J. Laskar; A. Lecavelier Des Etangs; M. Lieder; C. Lovis; D. Magrin; P. F. L. Maxted; V. Nascimbeni; R. Ottensamer; I. Pagano; E. Pallé; G. Peter; G. Piotto; A. Pizarro Rubio; D. Pollacco; F. J. Pozuelos; D. Queloz; R. Ragazzoni; N. Rando; H. Rauer; I. Ribas; N. C. Santos; G. Scandariato; A. M. S. Smith; S. G. Sousa; M. Steller; Gy. M. Szabó; D. Ségransan; N. Thomas; S. Udry; B. Ulmer; V. Van Grootel; N. A. Walton

doi:10.1051/0004-6361/202140892

CHEOPS precision phase curve of the Super-Earth 55 Cancri e

B. M. Morris^*, L. Delrez, A. Brandeker, A. C. Cameron, A. E. Simon, D. Futyan, G. Olofsson, S. Hoyer, A. Fortier, B.-O. Demory, M. Lendl, T. G. Wilson, M. Oshagh, K. Heng, D. Ehrenreich, S. Sulis, Y. Alibert, R. Alonso, G. Anglada Escudé, D. BarradoS. C. C. Barros, W. Baumjohann, M. Beck, T. Beck, A. Bekkelien, W. Benz, M. Bergomi, N. Billot, X. Bonfils, V. Bourrier, C. Broeg, T. Bárczy, J. Cabrera, S. Charnoz, M. B. Davies, D. De Miguel Ferreras, M. Deleuil, A. Deline, O. D. S. Demangeon, A. Erikson, H. G. Floren, L. Fossati, M. Fridlund, D. Gandolfi, A. García Muñoz, M. Gillon, M. Guedel, P. Guterman, K. Isaak, L. Kiss, J. Laskar, A. Lecavelier Des Etangs, M. Lieder, C. Lovis, D. Magrin, P. F. L. Maxted, V. Nascimbeni, R. Ottensamer, I. Pagano, E. Pallé, G. Peter, G. Piotto, A. Pizarro Rubio, D. Pollacco, F. J. Pozuelos, D. Queloz, R. Ragazzoni, N. Rando, H. Rauer, I. Ribas, N. C. Santos, G. Scandariato, A. M. S. Smith, S. G. Sousa, M. Steller, Gy. M. Szabó, D. Ségransan, N. Thomas, S. Udry, B. Ulmer, V. Van Grootel, N. A. Walton

^*Corresponding author for this work

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

Abstract

Context. 55 Cnc e is a transiting super-Earth (radius 1.88 R_⊕ and mass 8 M_⊕) orbiting a G8V host star on a 17-h orbit. Spitzer observations of the planet's phase curve at 4.5 μm revealed a time-varying occultation depth, and MOST optical observations are consistent with a time-varying phase curve amplitude and phase offset of maximum light. Both broadband and high-resolution spectroscopic analyses are consistent with either a high mean molecular weight atmosphere or no atmosphere for planet e. A long-term photometric monitoring campaign on an independent optical telescope is needed to probe the variability in this system.

Aims. We seek to measure the phase variations of 55 Cnc e with a broadband optical filter with the 30 cm effective aperture space telescope CHEOPS and explore how the precision photometry narrows down the range of possible scenarios.

Methods. We observed 55 Cnc for 1.6 orbital phases in March of 2020. We designed a phase curve detrending toolkit for CHEOPS photometry which allowed us to study the underlying flux variations in the 55 Cnc system.

Results. We detected a phase variation with a full-amplitude of 72 ± 7 ppm, but did not detect a significant secondary eclipse of the planet. The shape of the phase variation resembles that of a piecewise-Lambertian; however, the non-detection of the planetary secondary eclipse, and the large amplitude of the variations exclude reflection from the planetary surface as a possible origin of the observed phase variations. They are also likely incompatible with magnetospheric interactions between the star and planet, but may imply that circumplanetary or circumstellar material modulate the flux of the system.

Conclusions. This year, further precision photometry of 55 Cnc from CHEOPS will measure variations in the phase curve amplitude and shape over time.

Original language	English
Article number	A173
Number of pages	15
Journal	Astronomy & Astrophysics
Volume	653
Early online date	30 Sept 2021
DOIs	https://doi.org/10.1051/0004-6361/202140892
Publication status	Published - 30 Sept 2021

Keywords

Techniques: photometric
Methods: observational
Planets and satellites: atmospheres
Stars: individual: 55 Cnc
Planets and satellites: individual: 55 Cnc e
Instrumentation: photometers

Access to Document

10.1051/0004-6361/202140892Licence: Other

Morris_2021_AA_CHEOPS-precision-phase_VoR
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Final published version, 3.96 MB

https://arxiv.org/abs/2106.07443

Astronomy at St Andrews 2018-2021: Astronomy at St Andrews 2018-2021
Jardine, M. M. (PI), Bonnell, I. A. (CoI), Cameron, A. C. (CoI), Cyganowski, C. J. (CoI), Dominik, M. (CoI), Helling, C. (CoI), Horne, K. D. (CoI), Scholz, A. (CoI), Tojeiro, R. (CoI), Weijmans, A.-M. (CoI), Wild, V. (CoI), Woitke, P. (CoI), Wood, K. (CoI) & Zhao, H. (CoI)
1/04/18 → 31/03/22
Project: Standard

CHEOPS precision phase curve of the Super-Earth 55 Cancri e (dataset)
Cameron, A. C. (Creator) & Wilson, T. G. (Creator), VizieR On-line Data Catalog, 2021
http://cdsarc.u-strasbg.fr/viz-bin/cat/J/A+A/653/A173
Dataset

Cite this

Morris, B. M., Delrez, L., Brandeker, A., Cameron, A. C., Simon, A. E., Futyan, D., Olofsson, G., Hoyer, S., Fortier, A., Demory, B.-O., Lendl, M., Wilson, T. G., Oshagh, M., Heng, K., Ehrenreich, D., Sulis, S., Alibert, Y., Alonso, R., Anglada Escudé, G., ... Walton, N. A. (2021). CHEOPS precision phase curve of the Super-Earth 55 Cancri e. Astronomy & Astrophysics, 653, Article A173. https://doi.org/10.1051/0004-6361/202140892

@article{c21e468d51d8419f8b2620b9807949ac,

title = "CHEOPS precision phase curve of the Super-Earth 55 Cancri e",

abstract = "Context. 55 Cnc e is a transiting super-Earth (radius 1.88 R⊕ and mass 8 M⊕) orbiting a G8V host star on a 17-h orbit. Spitzer observations of the planet's phase curve at 4.5 μm revealed a time-varying occultation depth, and MOST optical observations are consistent with a time-varying phase curve amplitude and phase offset of maximum light. Both broadband and high-resolution spectroscopic analyses are consistent with either a high mean molecular weight atmosphere or no atmosphere for planet e. A long-term photometric monitoring campaign on an independent optical telescope is needed to probe the variability in this system. Aims. We seek to measure the phase variations of 55 Cnc e with a broadband optical filter with the 30 cm effective aperture space telescope CHEOPS and explore how the precision photometry narrows down the range of possible scenarios. Methods. We observed 55 Cnc for 1.6 orbital phases in March of 2020. We designed a phase curve detrending toolkit for CHEOPS photometry which allowed us to study the underlying flux variations in the 55 Cnc system. Results. We detected a phase variation with a full-amplitude of 72 ± 7 ppm, but did not detect a significant secondary eclipse of the planet. The shape of the phase variation resembles that of a piecewise-Lambertian; however, the non-detection of the planetary secondary eclipse, and the large amplitude of the variations exclude reflection from the planetary surface as a possible origin of the observed phase variations. They are also likely incompatible with magnetospheric interactions between the star and planet, but may imply that circumplanetary or circumstellar material modulate the flux of the system. Conclusions. This year, further precision photometry of 55 Cnc from CHEOPS will measure variations in the phase curve amplitude and shape over time.",

keywords = "Techniques: photometric, Methods: observational, Planets and satellites: atmospheres, Stars: individual: 55 Cnc, Planets and satellites: individual: 55 Cnc e, Instrumentation: photometers",

author = "Morris, {B. M.} and L. Delrez and A. Brandeker and Cameron, {A. C.} and Simon, {A. E.} and D. Futyan and G. Olofsson and S. Hoyer and A. Fortier and B.-O. Demory and M. Lendl and Wilson, {T. G.} and M. Oshagh and K. Heng and D. Ehrenreich and S. Sulis and Y. Alibert and R. Alonso and {Anglada Escud{\'e}}, G. and D. Barrado and Barros, {S. C. C.} and W. Baumjohann and M. Beck and T. Beck and A. Bekkelien and W. Benz and M. Bergomi and N. Billot and X. Bonfils and V. Bourrier and C. Broeg and T. B{\'a}rczy and J. Cabrera and S. Charnoz and Davies, {M. B.} and {De Miguel Ferreras}, D. and M. Deleuil and A. Deline and Demangeon, {O. D. S.} and A. Erikson and Floren, {H. G.} and L. Fossati and M. Fridlund and D. Gandolfi and {Garc{\'i}a Mu{\~n}oz}, A. and M. Gillon and M. Guedel and P. Guterman and K. Isaak and L. Kiss and J. Laskar and {Lecavelier Des Etangs}, A. and M. Lieder and C. Lovis and D. Magrin and Maxted, {P. F. L.} and V. Nascimbeni and R. Ottensamer and I. Pagano and E. Pall{\'e} and G. Peter and G. Piotto and {Pizarro Rubio}, A. and D. Pollacco and Pozuelos, {F. J.} and D. Queloz and R. Ragazzoni and N. Rando and H. Rauer and I. Ribas and Santos, {N. C.} and G. Scandariato and Smith, {A. M. S.} and Sousa, {S. G.} and M. Steller and Szab{\'o}, {Gy. M.} and D. S{\'e}gransan and N. Thomas and S. Udry and B. Ulmer and {Van Grootel}, V. and Walton, {N. A.}",

note = "Funding: This project has received funding from the European Research Council (ERC) under the European Union{\textquoteright}s Horizon 2020 research and innovation programme (project FOUR ACES; grant agreement No 724427). This work was supported by FCT – Funda{\c c}{\~a}o para a Ci{\^e}ncia e a Tecnologia through national funds and by FEDER through COMPETE2020 - Programa Operacional Competitividade e Internacionaliza{\c c}{\~a}o by these grants: UID/FIS/04434/2019; UIDB/04434/2020; UIDP/04434/2020; PTDC/FIS-AST/32113/2017 and POCI-01-0145-FEDER-032113; PTDC/FIS-AST/28953/2017 and POCI-01-0145-FEDER-028953; PTDC/FIS-AST/28987/2017 and POCI-01-0145-FEDER-028987. S.C.C.B. and S.G.S. acknowledge support from FCT through FCT contracts nr. IF/01312/2014/CP1215/CT0004, IF/00028/2014/CP1215/CT0002. O.D.S.D. is supported in the form of work contract (DL 57/2016/CP1364/CT0004) funded by national funds through Funda{\c c}{\~a}o para a Ci{\^e}ncia e Tecnologia (FCT). X.B., S.C., D.G., M.F. and J.L. acknowledge their roles as ESA-appointed CHEOPS science team members. A.C.C. and T.W. acknowledge support from STFC consolidated grant number ST/R000824/1. This project was supported by the CNES. S.H. gratefully acknowledges CNES funding through the grant 837319. P.M. acknowledges support from STFC consolidated grant number ST/M001040/1. ",

year = "2021",

month = sep,

day = "30",

doi = "10.1051/0004-6361/202140892",

language = "English",

volume = "653",

journal = "Astronomy & Astrophysics",

issn = "0004-6361",

publisher = "EDP SCIENCES S A",

}

Morris, BM, Delrez, L, Brandeker, A, Cameron, AC, Simon, AE, Futyan, D, Olofsson, G, Hoyer, S, Fortier, A, Demory, B-O, Lendl, M, Wilson, TG, Oshagh, M, Heng, K, Ehrenreich, D, Sulis, S, Alibert, Y, Alonso, R, Anglada Escudé, G, Barrado, D, Barros, SCC, Baumjohann, W, Beck, M, Beck, T, Bekkelien, A, Benz, W, Bergomi, M, Billot, N, Bonfils, X, Bourrier, V, Broeg, C, Bárczy, T, Cabrera, J, Charnoz, S, Davies, MB, De Miguel Ferreras, D, Deleuil, M, Deline, A, Demangeon, ODS, Erikson, A, Floren, HG, Fossati, L, Fridlund, M, Gandolfi, D, García Muñoz, A, Gillon, M, Guedel, M, Guterman, P, Isaak, K, Kiss, L, Laskar, J, Lecavelier Des Etangs, A, Lieder, M, Lovis, C, Magrin, D, Maxted, PFL, Nascimbeni, V, Ottensamer, R, Pagano, I, Pallé, E, Peter, G, Piotto, G, Pizarro Rubio, A, Pollacco, D, Pozuelos, FJ, Queloz, D, Ragazzoni, R, Rando, N, Rauer, H, Ribas, I, Santos, NC, Scandariato, G, Smith, AMS, Sousa, SG, Steller, M, Szabó, GM, Ségransan, D, Thomas, N, Udry, S, Ulmer, B, Van Grootel, V & Walton, NA 2021, 'CHEOPS precision phase curve of the Super-Earth 55 Cancri e', Astronomy & Astrophysics, vol. 653, A173. https://doi.org/10.1051/0004-6361/202140892

TY - JOUR

T1 - CHEOPS precision phase curve of the Super-Earth 55 Cancri e

AU - Morris, B. M.

AU - Delrez, L.

AU - Brandeker, A.

AU - Cameron, A. C.

AU - Simon, A. E.

AU - Futyan, D.

AU - Olofsson, G.

AU - Hoyer, S.

AU - Fortier, A.

AU - Demory, B.-O.

AU - Lendl, M.

AU - Wilson, T. G.

AU - Oshagh, M.

AU - Heng, K.

AU - Ehrenreich, D.

AU - Sulis, S.

AU - Alibert, Y.

AU - Alonso, R.

AU - Anglada Escudé, G.

AU - Barrado, D.

AU - Barros, S. C. C.

AU - Baumjohann, W.

AU - Beck, M.

AU - Beck, T.

AU - Bekkelien, A.

AU - Benz, W.

AU - Bergomi, M.

AU - Billot, N.

AU - Bonfils, X.

AU - Bourrier, V.

AU - Broeg, C.

AU - Bárczy, T.

AU - Cabrera, J.

AU - Charnoz, S.

AU - Davies, M. B.

AU - De Miguel Ferreras, D.

AU - Deleuil, M.

AU - Deline, A.

AU - Demangeon, O. D. S.

AU - Erikson, A.

AU - Floren, H. G.

AU - Fossati, L.

AU - Fridlund, M.

AU - Gandolfi, D.

AU - García Muñoz, A.

AU - Gillon, M.

AU - Guedel, M.

AU - Guterman, P.

AU - Isaak, K.

AU - Kiss, L.

AU - Laskar, J.

AU - Lecavelier Des Etangs, A.

AU - Lieder, M.

AU - Lovis, C.

AU - Magrin, D.

AU - Maxted, P. F. L.

AU - Nascimbeni, V.

AU - Ottensamer, R.

AU - Pagano, I.

AU - Pallé, E.

AU - Peter, G.

AU - Piotto, G.

AU - Pizarro Rubio, A.

AU - Pollacco, D.

AU - Pozuelos, F. J.

AU - Queloz, D.

AU - Ragazzoni, R.

AU - Rando, N.

AU - Rauer, H.

AU - Ribas, I.

AU - Santos, N. C.

AU - Scandariato, G.

AU - Smith, A. M. S.

AU - Sousa, S. G.

AU - Steller, M.

AU - Szabó, Gy. M.

AU - Ségransan, D.

AU - Thomas, N.

AU - Udry, S.

AU - Ulmer, B.

AU - Van Grootel, V.

AU - Walton, N. A.

N1 - Funding: This project has received funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (project FOUR ACES; grant agreement No 724427). This work was supported by FCT – Fundação para a Ciência e a Tecnologia through national funds and by FEDER through COMPETE2020 - Programa Operacional Competitividade e Internacionalização by these grants: UID/FIS/04434/2019; UIDB/04434/2020; UIDP/04434/2020; PTDC/FIS-AST/32113/2017 and POCI-01-0145-FEDER-032113; PTDC/FIS-AST/28953/2017 and POCI-01-0145-FEDER-028953; PTDC/FIS-AST/28987/2017 and POCI-01-0145-FEDER-028987. S.C.C.B. and S.G.S. acknowledge support from FCT through FCT contracts nr. IF/01312/2014/CP1215/CT0004, IF/00028/2014/CP1215/CT0002. O.D.S.D. is supported in the form of work contract (DL 57/2016/CP1364/CT0004) funded by national funds through Fundação para a Ciência e Tecnologia (FCT). X.B., S.C., D.G., M.F. and J.L. acknowledge their roles as ESA-appointed CHEOPS science team members. A.C.C. and T.W. acknowledge support from STFC consolidated grant number ST/R000824/1. This project was supported by the CNES. S.H. gratefully acknowledges CNES funding through the grant 837319. P.M. acknowledges support from STFC consolidated grant number ST/M001040/1.

PY - 2021/9/30

Y1 - 2021/9/30

N2 - Context. 55 Cnc e is a transiting super-Earth (radius 1.88 R⊕ and mass 8 M⊕) orbiting a G8V host star on a 17-h orbit. Spitzer observations of the planet's phase curve at 4.5 μm revealed a time-varying occultation depth, and MOST optical observations are consistent with a time-varying phase curve amplitude and phase offset of maximum light. Both broadband and high-resolution spectroscopic analyses are consistent with either a high mean molecular weight atmosphere or no atmosphere for planet e. A long-term photometric monitoring campaign on an independent optical telescope is needed to probe the variability in this system. Aims. We seek to measure the phase variations of 55 Cnc e with a broadband optical filter with the 30 cm effective aperture space telescope CHEOPS and explore how the precision photometry narrows down the range of possible scenarios. Methods. We observed 55 Cnc for 1.6 orbital phases in March of 2020. We designed a phase curve detrending toolkit for CHEOPS photometry which allowed us to study the underlying flux variations in the 55 Cnc system. Results. We detected a phase variation with a full-amplitude of 72 ± 7 ppm, but did not detect a significant secondary eclipse of the planet. The shape of the phase variation resembles that of a piecewise-Lambertian; however, the non-detection of the planetary secondary eclipse, and the large amplitude of the variations exclude reflection from the planetary surface as a possible origin of the observed phase variations. They are also likely incompatible with magnetospheric interactions between the star and planet, but may imply that circumplanetary or circumstellar material modulate the flux of the system. Conclusions. This year, further precision photometry of 55 Cnc from CHEOPS will measure variations in the phase curve amplitude and shape over time.

AB - Context. 55 Cnc e is a transiting super-Earth (radius 1.88 R⊕ and mass 8 M⊕) orbiting a G8V host star on a 17-h orbit. Spitzer observations of the planet's phase curve at 4.5 μm revealed a time-varying occultation depth, and MOST optical observations are consistent with a time-varying phase curve amplitude and phase offset of maximum light. Both broadband and high-resolution spectroscopic analyses are consistent with either a high mean molecular weight atmosphere or no atmosphere for planet e. A long-term photometric monitoring campaign on an independent optical telescope is needed to probe the variability in this system. Aims. We seek to measure the phase variations of 55 Cnc e with a broadband optical filter with the 30 cm effective aperture space telescope CHEOPS and explore how the precision photometry narrows down the range of possible scenarios. Methods. We observed 55 Cnc for 1.6 orbital phases in March of 2020. We designed a phase curve detrending toolkit for CHEOPS photometry which allowed us to study the underlying flux variations in the 55 Cnc system. Results. We detected a phase variation with a full-amplitude of 72 ± 7 ppm, but did not detect a significant secondary eclipse of the planet. The shape of the phase variation resembles that of a piecewise-Lambertian; however, the non-detection of the planetary secondary eclipse, and the large amplitude of the variations exclude reflection from the planetary surface as a possible origin of the observed phase variations. They are also likely incompatible with magnetospheric interactions between the star and planet, but may imply that circumplanetary or circumstellar material modulate the flux of the system. Conclusions. This year, further precision photometry of 55 Cnc from CHEOPS will measure variations in the phase curve amplitude and shape over time.

KW - Techniques: photometric

KW - Methods: observational

KW - Planets and satellites: atmospheres

KW - Stars: individual: 55 Cnc

KW - Planets and satellites: individual: 55 Cnc e

KW - Instrumentation: photometers

U2 - 10.1051/0004-6361/202140892

DO - 10.1051/0004-6361/202140892

M3 - Article

SN - 0004-6361

VL - 653

JO - Astronomy & Astrophysics

JF - Astronomy & Astrophysics

M1 - A173

ER -

CHEOPS precision phase curve of the Super-Earth 55 Cancri e

Abstract

Keywords

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Projects

Astronomy at St Andrews 2018-2021: Astronomy at St Andrews 2018-2021

Datasets

CHEOPS precision phase curve of the Super-Earth 55 Cancri e (dataset)

Cite this