55 Cancri e's occultation captured with CHEOPS

B.-O. Demory; S. Sulis; E. Meier Valdés; L. Delrez; A. Brandeker; N. Billot; A. Fortier; S. Hoyer; S. G. Sousa; K. Heng; M. Lendl; A. Krenn; B. M. Morris; J. A. Patel; Y. Alibert; R. Alonso; G. Anglada; T. Bárczy; D. Barrado; S. C. C. Barros; W. Baumjohann; M. Beck; T. Beck; W. Benz; X. Bonfils; C. Broeg; M. Buder; J. Cabrera; S. Charnoz; A. Collier Cameron; H. Cottard; Sz. Csizmadia; M. B. Davies; M. Deleuil; O. D. S. Demangeon; D. Ehrenreich; A. Erikson; L. Fossati; M. Fridlund; D. Gandolfi; M. Gillon; M. Güdel; K. G. Isaak; L. L. Kiss; J. Laskar; A. Lecavelier des Etangs; C. Lovis; A. Luntzer; D. Magrin; L. Marafatto; P. F. L. Maxted; V. Nascimbeni; G. Olofsson; R. Ottensamer; I. Pagano; E. Pallé; G. Peter; G. Piotto; D. Pollacco; D. Queloz; R. Ragazzoni; N. Rando; F. Ratti; H. Rauer; I. Ribas; N. C. Santos; G. Scandariato; D. Ségransan; A. E. Simon; A. M. S. Smith; M. Steller; Gy. M. Szabó; N. Thomas; S. Udry; V. Van Grootel; N. A. Walton

doi:10.1051/0004-6361/202244894

55 Cancri e's occultation captured with CHEOPS

B.-O. Demory^*, S. Sulis, E. Meier Valdés, L. Delrez, A. Brandeker, N. Billot, A. Fortier, S. Hoyer, S. G. Sousa, K. Heng, M. Lendl, A. Krenn, B. M. Morris, J. A. Patel, Y. Alibert, R. Alonso, G. Anglada, T. Bárczy, D. Barrado, S. C. C. BarrosW. Baumjohann, M. Beck, T. Beck, W. Benz, X. Bonfils, C. Broeg, M. Buder, J. Cabrera, S. Charnoz, A. Collier Cameron, H. Cottard, Sz. Csizmadia, M. B. Davies, M. Deleuil, O. D. S. Demangeon, D. Ehrenreich, A. Erikson, L. Fossati, M. Fridlund, D. Gandolfi, M. Gillon, M. Güdel, K. G. Isaak, L. L. Kiss, J. Laskar, A. Lecavelier des Etangs, C. Lovis, A. Luntzer, D. Magrin, L. Marafatto, P. F. L. Maxted, V. Nascimbeni, G. Olofsson, R. Ottensamer, I. Pagano, E. Pallé, G. Peter, G. Piotto, D. Pollacco, D. Queloz, R. Ragazzoni, N. Rando, F. Ratti, H. Rauer, I. Ribas, N. C. Santos, G. Scandariato, D. Ségransan, A. E. Simon, A. M. S. Smith, M. Steller, Gy. M. Szabó, N. Thomas, S. Udry, V. Van Grootel, N. A. Walton

^*Corresponding author for this work

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

Abstract

Past occultation and phase-curve observations of the ultra-short period super-Earth 55 Cnc e obtained at visible and infrared wavelengths have been challenging to reconcile with a planetary reflection and emission model. In this study, we analyse a set of 41 occultations obtained over a two-year timespan with the CHEOPS satellite. We report the detection of 55 Cnc e’s occultation with an average depth of 12 ± 3 ppm. We derive a corresponding 2σ upper limit on the geometric albedo of A_g < 0.55 once decontaminated from the thermal emission measured by Spitzer at 4.5 µm. CHEOPS’s photometric performance enables, for the first time, the detection of individual occultations of this super-Earth in the visible and identifies short-timescale photometric corrugations likely induced by stellar granulation. We also find a clear 47.3-day sinusoidal pattern in the time-dependent occultation depths that we are unable to relate to stellar noise, nor instrumental systematics, but whose planetary origin could be tested with upcoming JWST occultation observations of this iconic super-Earth.

Original language	English
Article number	A64
Number of pages	10
Journal	Astronomy & Astrophysics
Volume	669
Early online date	11 Jan 2023
DOIs	https://doi.org/10.1051/0004-6361/202244894
Publication status	Published - Jan 2023

Keywords

Planets and satellites: individual: 55 Cnc e
Techniques: photometric
Methods: observational

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10.1051/0004-6361/202244894Licence: CC BY

Demory-2023-55-Cancri es-occulation-A&A-669-A64-CCBY
Copyright © 2023 The Authors. Open Access article, published by EDP Sciences, under the terms of the Creative Commons Attribution License (https://creativecommons.org/licenses/by/4.0), which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited.
Final published version, 1.87 MBLicence: CC BY

http://arxiv.org/abs/2211.03582Licence: CC BY

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

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Demory, B.-O., Sulis, S., Meier Valdés, E., Delrez, L., Brandeker, A., Billot, N., Fortier, A., Hoyer, S., Sousa, S. G., Heng, K., Lendl, M., Krenn, A., Morris, B. M., Patel, J. A., Alibert, Y., Alonso, R., Anglada, G., Bárczy, T., Barrado, D., ... Walton, N. A. (2023). 55 Cancri e's occultation captured with CHEOPS. Astronomy & Astrophysics, 669, Article A64. https://doi.org/10.1051/0004-6361/202244894

@article{a02cbfd59f37483998376634ac7e56e0,

title = "55 Cancri e's occultation captured with CHEOPS",

abstract = "Past occultation and phase-curve observations of the ultra-short period super-Earth 55 Cnc e obtained at visible and infrared wavelengths have been challenging to reconcile with a planetary reflection and emission model. In this study, we analyse a set of 41 occultations obtained over a two-year timespan with the CHEOPS satellite. We report the detection of 55 Cnc e{\textquoteright}s occultation with an average depth of 12 ± 3 ppm. We derive a corresponding 2σ upper limit on the geometric albedo of Ag < 0.55 once decontaminated from the thermal emission measured by Spitzer at 4.5 µm. CHEOPS{\textquoteright}s photometric performance enables, for the first time, the detection of individual occultations of this super-Earth in the visible and identifies short-timescale photometric corrugations likely induced by stellar granulation. We also find a clear 47.3-day sinusoidal pattern in the time-dependent occultation depths that we are unable to relate to stellar noise, nor instrumental systematics, but whose planetary origin could be tested with upcoming JWST occultation observations of this iconic super-Earth.",

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

author = "B.-O. Demory and S. Sulis and {Meier Vald{\'e}s}, E. and L. Delrez and A. Brandeker and N. Billot and A. Fortier and S. Hoyer and Sousa, {S. G.} and K. Heng and M. Lendl and A. Krenn and Morris, {B. M.} and Patel, {J. A.} and Y. Alibert and R. Alonso and G. Anglada and T. B{\'a}rczy and D. Barrado and Barros, {S. C. C.} and W. Baumjohann and M. Beck and T. Beck and W. Benz and X. Bonfils and C. Broeg and M. Buder and J. Cabrera and S. Charnoz and {Collier Cameron}, A. and H. Cottard and Sz. Csizmadia and Davies, {M. B.} and M. Deleuil and Demangeon, {O. D. S.} and D. Ehrenreich and A. Erikson and L. Fossati and M. Fridlund and D. Gandolfi and M. Gillon and M. G{\"u}del and Isaak, {K. G.} and Kiss, {L. L.} and J. Laskar and {Lecavelier des Etangs}, A. and C. Lovis and A. Luntzer and D. Magrin and L. Marafatto and Maxted, {P. F. L.} and V. Nascimbeni and G. Olofsson and R. Ottensamer and I. Pagano and E. Pall{\'e} and G. Peter and G. Piotto and D. Pollacco and D. Queloz and R. Ragazzoni and N. Rando and F. Ratti and H. Rauer and I. Ribas and Santos, {N. C.} and G. Scandariato and D. S{\'e}gransan and Simon, {A. E.} and Smith, {A. M. S.} and M. Steller and Szab{\'o}, {Gy. M.} and N. Thomas and S. Udry and {Van Grootel}, V. and Walton, {N. A.}",

note = "Funding: s. A.C.C. acknowledges support from STFC consolidated grant numbers ST/R000824/1 and ST/V000861/1, and UKSA grant number ST/R003203/1.",

year = "2023",

month = jan,

doi = "10.1051/0004-6361/202244894",

language = "English",

volume = "669",

journal = "Astronomy & Astrophysics",

issn = "0004-6361",

publisher = "EDP SCIENCES S A",

}

Demory, B-O, Sulis, S, Meier Valdés, E, Delrez, L, Brandeker, A, Billot, N, Fortier, A, Hoyer, S, Sousa, SG, Heng, K, Lendl, M, Krenn, A, Morris, BM, Patel, JA, Alibert, Y, Alonso, R, Anglada, G, Bárczy, T, Barrado, D, Barros, SCC, Baumjohann, W, Beck, M, Beck, T, Benz, W, Bonfils, X, Broeg, C, Buder, M, Cabrera, J, Charnoz, S, Collier Cameron, A, Cottard, H, Csizmadia, S, Davies, MB, Deleuil, M, Demangeon, ODS, Ehrenreich, D, Erikson, A, Fossati, L, Fridlund, M, Gandolfi, D, Gillon, M, Güdel, M, Isaak, KG, Kiss, LL, Laskar, J, Lecavelier des Etangs, A, Lovis, C, Luntzer, A, Magrin, D, Marafatto, L, Maxted, PFL, Nascimbeni, V, Olofsson, G, Ottensamer, R, Pagano, I, Pallé, E, Peter, G, Piotto, G, Pollacco, D, Queloz, D, Ragazzoni, R, Rando, N, Ratti, F, Rauer, H, Ribas, I, Santos, NC, Scandariato, G, Ségransan, D, Simon, AE, Smith, AMS, Steller, M, Szabó, GM, Thomas, N, Udry, S, Van Grootel, V & Walton, NA 2023, '55 Cancri e's occultation captured with CHEOPS', Astronomy & Astrophysics, vol. 669, A64. https://doi.org/10.1051/0004-6361/202244894

TY - JOUR

T1 - 55 Cancri e's occultation captured with CHEOPS

AU - Demory, B.-O.

AU - Sulis, S.

AU - Meier Valdés, E.

AU - Delrez, L.

AU - Brandeker, A.

AU - Billot, N.

AU - Fortier, A.

AU - Hoyer, S.

AU - Sousa, S. G.

AU - Heng, K.

AU - Lendl, M.

AU - Krenn, A.

AU - Morris, B. M.

AU - Patel, J. A.

AU - Alibert, Y.

AU - Alonso, R.

AU - Anglada, G.

AU - Bárczy, T.

AU - Barrado, D.

AU - Barros, S. C. C.

AU - Baumjohann, W.

AU - Beck, M.

AU - Beck, T.

AU - Benz, W.

AU - Bonfils, X.

AU - Broeg, C.

AU - Buder, M.

AU - Cabrera, J.

AU - Charnoz, S.

AU - Collier Cameron, A.

AU - Cottard, H.

AU - Csizmadia, Sz.

AU - Davies, M. B.

AU - Deleuil, M.

AU - Demangeon, O. D. S.

AU - Ehrenreich, D.

AU - Erikson, A.

AU - Fossati, L.

AU - Fridlund, M.

AU - Gandolfi, D.

AU - Gillon, M.

AU - Güdel, M.

AU - Isaak, K. G.

AU - Kiss, L. L.

AU - Laskar, J.

AU - Lecavelier des Etangs, A.

AU - Lovis, C.

AU - Luntzer, A.

AU - Magrin, D.

AU - Marafatto, L.

AU - Maxted, P. F. L.

AU - Nascimbeni, V.

AU - Olofsson, G.

AU - Ottensamer, R.

AU - Pagano, I.

AU - Pallé, E.

AU - Peter, G.

AU - Piotto, G.

AU - Pollacco, D.

AU - Queloz, D.

AU - Ragazzoni, R.

AU - Rando, N.

AU - Ratti, F.

AU - Rauer, H.

AU - Ribas, I.

AU - Santos, N. C.

AU - Scandariato, G.

AU - Ségransan, D.

AU - Simon, A. E.

AU - Smith, A. M. S.

AU - Steller, M.

AU - Szabó, Gy. M.

AU - Thomas, N.

AU - Udry, S.

AU - Van Grootel, V.

AU - Walton, N. A.

N1 - Funding: s. A.C.C. acknowledges support from STFC consolidated grant numbers ST/R000824/1 and ST/V000861/1, and UKSA grant number ST/R003203/1.

PY - 2023/1

Y1 - 2023/1

N2 - Past occultation and phase-curve observations of the ultra-short period super-Earth 55 Cnc e obtained at visible and infrared wavelengths have been challenging to reconcile with a planetary reflection and emission model. In this study, we analyse a set of 41 occultations obtained over a two-year timespan with the CHEOPS satellite. We report the detection of 55 Cnc e’s occultation with an average depth of 12 ± 3 ppm. We derive a corresponding 2σ upper limit on the geometric albedo of Ag < 0.55 once decontaminated from the thermal emission measured by Spitzer at 4.5 µm. CHEOPS’s photometric performance enables, for the first time, the detection of individual occultations of this super-Earth in the visible and identifies short-timescale photometric corrugations likely induced by stellar granulation. We also find a clear 47.3-day sinusoidal pattern in the time-dependent occultation depths that we are unable to relate to stellar noise, nor instrumental systematics, but whose planetary origin could be tested with upcoming JWST occultation observations of this iconic super-Earth.

AB - Past occultation and phase-curve observations of the ultra-short period super-Earth 55 Cnc e obtained at visible and infrared wavelengths have been challenging to reconcile with a planetary reflection and emission model. In this study, we analyse a set of 41 occultations obtained over a two-year timespan with the CHEOPS satellite. We report the detection of 55 Cnc e’s occultation with an average depth of 12 ± 3 ppm. We derive a corresponding 2σ upper limit on the geometric albedo of Ag < 0.55 once decontaminated from the thermal emission measured by Spitzer at 4.5 µm. CHEOPS’s photometric performance enables, for the first time, the detection of individual occultations of this super-Earth in the visible and identifies short-timescale photometric corrugations likely induced by stellar granulation. We also find a clear 47.3-day sinusoidal pattern in the time-dependent occultation depths that we are unable to relate to stellar noise, nor instrumental systematics, but whose planetary origin could be tested with upcoming JWST occultation observations of this iconic super-Earth.

KW - Planets and satellites: individual: 55 Cnc e

KW - Techniques: photometric

KW - Methods: observational

U2 - 10.1051/0004-6361/202244894

DO - 10.1051/0004-6361/202244894

M3 - Article

SN - 0004-6361

VL - 669

JO - Astronomy & Astrophysics

JF - Astronomy & Astrophysics

M1 - A64

ER -

55 Cancri e's occultation captured with CHEOPS

Abstract

Keywords

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

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