CHEOPS observations confirm nodal precession in the WASP-33 system

A. M. S. Smith; Sz Csizmadia; V. Van Grootel; M. Lendl; C. M. Persson; G. Olofsson; D. Ehrenreich; M. N. Günther; A. Heitzmann; S. C. C. Barros; A. Bonfanti; A. Brandeker; J. Cabrera; O. D. S. Demangeon; L. Fossati; J. -V. Harre; M. J. Hooton; S. Hoyer; Sz Kalman; S. Salmon; S. G. Sousa; Gy M. Szabó; T. G. Wilson; Y. Alibert; R. Alonso; J. Asquier; T. Bárczy; D. Barrado; W. Baumjohann; W. Benz; N. Billot; L. Borsato; C. Broeg; A. Collier Cameron; A. C. M. Correia; P. E. Cubillos; M. B. Davies; M. Deleuil; A. Deline; B. -O. Demory; A. Derekas; B. Edwards; J. A. Egger; A. Erikson; A. Fortier; M. Fridlund; D. Gandolfi; K. Gazeas; M. Gillon; M. Güdel; J. Hasiba; Ch Helling; K. G. Isaak; L. L. Kiss; J. Korth; K. W. F. Lam; J. Laskar; A. Lecavelier des Etangs; D. Magrin; P. F. L. Maxted; B. Merín; C. Mordasini; V. Nascimbeni; R. Ottensamer; I. Pagano; E. Pallé; G. Peter; D. Piazza; G. Piotto; D. Pollacco; D. Queloz; R. Ragazzoni; N. Rando; H. Rauer; I. Ribas; N. C. Santos; G. Scandariato; D. Ségransan; A. E. Simon; M. Stalport; S. Sulis; S. Udry; S. Ulmer-Moll; J. Venturini; E. Villaver; V. Viotto; I. Walter; N. A. Walton; S. Wolf

CHEOPS observations confirm nodal precession in the WASP-33 system

A. M. S. Smith, Sz Csizmadia, V. Van Grootel, M. Lendl, C. M. Persson, G. Olofsson, D. Ehrenreich, M. N. Günther, A. Heitzmann, S. C. C. Barros, A. Bonfanti, A. Brandeker, J. Cabrera, O. D. S. Demangeon, L. Fossati, J. -V. Harre, M. J. Hooton, S. Hoyer, Sz Kalman, S. SalmonS. G. Sousa, Gy M. Szabó, T. G. Wilson, Y. Alibert, R. Alonso, J. Asquier, T. Bárczy, D. Barrado, W. Baumjohann, W. Benz, N. Billot, L. Borsato, C. Broeg, A. Collier Cameron, A. C. M. Correia, P. E. Cubillos, M. B. Davies, M. Deleuil, A. Deline, B. -O. Demory, A. Derekas, B. Edwards, J. A. Egger, A. Erikson, A. Fortier, M. Fridlund, D. Gandolfi, K. Gazeas, M. Gillon, M. Güdel, J. Hasiba, Ch Helling, K. G. Isaak, L. L. Kiss, J. Korth, K. W. F. Lam, J. Laskar, A. Lecavelier des Etangs, D. Magrin, P. F. L. Maxted, B. Merín, C. Mordasini, V. Nascimbeni, R. Ottensamer, I. Pagano, E. Pallé, G. Peter, D. Piazza, G. Piotto, D. Pollacco, D. Queloz, R. Ragazzoni, N. Rando, H. Rauer, I. Ribas, N. C. Santos, G. Scandariato, D. Ségransan, A. E. Simon, M. Stalport, S. Sulis, S. Udry, S. Ulmer-Moll, J. Venturini, E. Villaver, V. Viotto, I. Walter, N. A. Walton, S. Wolf

Research output: Working paper › Preprint

Abstract

Aims: We aim to observe the transits and occultations of WASP-33b, which orbits a rapidly-rotating $\delta$ Scuti pulsator, with the goal of measuring the orbital obliquity via the gravity-darkening effect, and constraining the geometric albedo via the occultation depth. Methods: We observed four transits and four occultations with CHEOPS, and employ a variety of techniques to remove the effects of the stellar pulsations from the light curves, as well as the usual CHEOPS systematic effects. We also performed a comprehensive analysis of low-resolution spectral and Gaia data to re-determine the stellar properties of WASP-33. Results: We measure an orbital obliquity 111.3 +0.2 -0.7 degrees, which is consistent with previous measurements made via Doppler tomography. We also measure the planetary impact parameter, and confirm that this parameter is undergoing rapid secular evolution as a result of nodal precession of the planetary orbit. This precession allows us to determine the second-order fluid Love number of the star, which we find agrees well with the predictions of theoretical stellar models. We are unable to robustly measure a unique value of the occultation depth, and emphasise the need for long-baseline observations to better measure the pulsation periods.

Original language	Undefined/Unknown
Publication status	Published - 11 Dec 2024

Keywords

astro-ph.EP
astro-ph.SR

Cite this

Smith, A. M. S., Csizmadia, S., Grootel, V. V., Lendl, M., Persson, C. M., Olofsson, G., Ehrenreich, D., Günther, M. N., Heitzmann, A., Barros, S. C. C., Bonfanti, A., Brandeker, A., Cabrera, J., Demangeon, O. D. S., Fossati, L., Harre, J. .-V., Hooton, M. J., Hoyer, S., Kalman, S., ... Wolf, S. (2024). CHEOPS observations confirm nodal precession in the WASP-33 system.

@techreport{887d16589f174b8ebf220b6b84fa4e5b,

title = "CHEOPS observations confirm nodal precession in the WASP-33 system",

abstract = "Aims: We aim to observe the transits and occultations of WASP-33b, which orbits a rapidly-rotating $\delta$ Scuti pulsator, with the goal of measuring the orbital obliquity via the gravity-darkening effect, and constraining the geometric albedo via the occultation depth. Methods: We observed four transits and four occultations with CHEOPS, and employ a variety of techniques to remove the effects of the stellar pulsations from the light curves, as well as the usual CHEOPS systematic effects. We also performed a comprehensive analysis of low-resolution spectral and Gaia data to re-determine the stellar properties of WASP-33. Results: We measure an orbital obliquity 111.3 +0.2 -0.7 degrees, which is consistent with previous measurements made via Doppler tomography. We also measure the planetary impact parameter, and confirm that this parameter is undergoing rapid secular evolution as a result of nodal precession of the planetary orbit. This precession allows us to determine the second-order fluid Love number of the star, which we find agrees well with the predictions of theoretical stellar models. We are unable to robustly measure a unique value of the occultation depth, and emphasise the need for long-baseline observations to better measure the pulsation periods.",

keywords = "astro-ph.EP, astro-ph.SR",

author = "Smith, {A. M. S.} and Sz Csizmadia and Grootel, {V. Van} and M. Lendl and Persson, {C. M.} and G. Olofsson and D. Ehrenreich and G{\"u}nther, {M. N.} and A. Heitzmann and Barros, {S. C. C.} and A. Bonfanti and A. Brandeker and J. Cabrera and Demangeon, {O. D. S.} and L. Fossati and Harre, {J. -V.} and Hooton, {M. J.} and S. Hoyer and Sz Kalman and S. Salmon and Sousa, {S. G.} and Szab{\'o}, {Gy M.} and Wilson, {T. G.} and Y. Alibert and R. Alonso and J. Asquier and T. B{\'a}rczy and D. Barrado and W. Baumjohann and W. Benz and N. Billot and L. Borsato and C. Broeg and Cameron, {A. Collier} and Correia, {A. C. M.} and Cubillos, {P. E.} and Davies, {M. B.} and M. Deleuil and A. Deline and Demory, {B. -O.} and A. Derekas and B. Edwards and Egger, {J. A.} and A. Erikson and A. Fortier and M. Fridlund and D. Gandolfi and K. Gazeas and M. Gillon and M. G{\"u}del and J. Hasiba and Ch Helling and Isaak, {K. G.} and Kiss, {L. L.} and J. Korth and Lam, {K. W. F.} and J. Laskar and Etangs, {A. Lecavelier des} and D. Magrin and Maxted, {P. F. L.} and B. Mer{\'i}n and C. Mordasini and V. Nascimbeni and R. Ottensamer and I. Pagano and E. Pall{\'e} and G. Peter and D. Piazza and G. Piotto and D. Pollacco and D. Queloz and R. Ragazzoni and N. Rando and H. Rauer and I. Ribas and Santos, {N. C.} and G. Scandariato and D. S{\'e}gransan and Simon, {A. E.} and M. Stalport and S. Sulis and S. Udry and S. Ulmer-Moll and J. Venturini and E. Villaver and V. Viotto and I. Walter and Walton, {N. A.} and S. Wolf",

note = "18 pages, 12 figures. Accepted for publication in Astronomy & Astrophysics",

year = "2024",

month = dec,

day = "11",

language = "Undefined/Unknown",

type = "WorkingPaper",

}

Smith, AMS, Csizmadia, S, Grootel, VV, Lendl, M, Persson, CM, Olofsson, G, Ehrenreich, D, Günther, MN, Heitzmann, A, Barros, SCC, Bonfanti, A, Brandeker, A, Cabrera, J, Demangeon, ODS, Fossati, L, Harre, J-V, Hooton, MJ, Hoyer, S, Kalman, S, Salmon, S, Sousa, SG, Szabó, GM, Wilson, TG, Alibert, Y, Alonso, R, Asquier, J, Bárczy, T, Barrado, D, Baumjohann, W, Benz, W, Billot, N, Borsato, L, Broeg, C, Cameron, AC, Correia, ACM, Cubillos, PE, Davies, MB, Deleuil, M, Deline, A, Demory, B-O, Derekas, A, Edwards, B, Egger, JA, Erikson, A, Fortier, A, Fridlund, M, Gandolfi, D, Gazeas, K, Gillon, M, Güdel, M, Hasiba, J, Helling, C, Isaak, KG, Kiss, LL, Korth, J, Lam, KWF, Laskar, J, Etangs, ALD, Magrin, D, Maxted, PFL, Merín, B, Mordasini, C, Nascimbeni, V, Ottensamer, R, Pagano, I, Pallé, E, Peter, G, Piazza, D, Piotto, G, Pollacco, D, Queloz, D, Ragazzoni, R, Rando, N, Rauer, H, Ribas, I, Santos, NC, Scandariato, G, Ségransan, D, Simon, AE, Stalport, M, Sulis, S, Udry, S, Ulmer-Moll, S, Venturini, J, Villaver, E, Viotto, V, Walter, I, Walton, NA & Wolf, S 2024 'CHEOPS observations confirm nodal precession in the WASP-33 system'.

TY - UNPB

T1 - CHEOPS observations confirm nodal precession in the WASP-33 system

AU - Smith, A. M. S.

AU - Csizmadia, Sz

AU - Grootel, V. Van

AU - Lendl, M.

AU - Persson, C. M.

AU - Olofsson, G.

AU - Ehrenreich, D.

AU - Günther, M. N.

AU - Heitzmann, A.

AU - Barros, S. C. C.

AU - Bonfanti, A.

AU - Brandeker, A.

AU - Cabrera, J.

AU - Demangeon, O. D. S.

AU - Fossati, L.

AU - Harre, J. -V.

AU - Hooton, M. J.

AU - Hoyer, S.

AU - Kalman, Sz

AU - Salmon, S.

AU - Sousa, S. G.

AU - Szabó, Gy M.

AU - Wilson, T. G.

AU - Alibert, Y.

AU - Alonso, R.

AU - Asquier, J.

AU - Bárczy, T.

AU - Barrado, D.

AU - Baumjohann, W.

AU - Benz, W.

AU - Billot, N.

AU - Borsato, L.

AU - Broeg, C.

AU - Cameron, A. Collier

AU - Correia, A. C. M.

AU - Cubillos, P. E.

AU - Davies, M. B.

AU - Deleuil, M.

AU - Deline, A.

AU - Demory, B. -O.

AU - Derekas, A.

AU - Edwards, B.

AU - Egger, J. A.

AU - Erikson, A.

AU - Fortier, A.

AU - Fridlund, M.

AU - Gandolfi, D.

AU - Gazeas, K.

AU - Gillon, M.

AU - Güdel, M.

AU - Hasiba, J.

AU - Helling, Ch

AU - Isaak, K. G.

AU - Kiss, L. L.

AU - Korth, J.

AU - Lam, K. W. F.

AU - Laskar, J.

AU - Etangs, A. Lecavelier des

AU - Magrin, D.

AU - Maxted, P. F. L.

AU - Merín, B.

AU - Mordasini, C.

AU - Nascimbeni, V.

AU - Ottensamer, R.

AU - Pagano, I.

AU - Pallé, E.

AU - Peter, G.

AU - Piazza, D.

AU - Piotto, G.

AU - Pollacco, D.

AU - Queloz, D.

AU - Ragazzoni, R.

AU - Rando, N.

AU - Rauer, H.

AU - Ribas, I.

AU - Santos, N. C.

AU - Scandariato, G.

AU - Ségransan, D.

AU - Simon, A. E.

AU - Stalport, M.

AU - Sulis, S.

AU - Udry, S.

AU - Ulmer-Moll, S.

AU - Venturini, J.

AU - Villaver, E.

AU - Viotto, V.

AU - Walter, I.

AU - Walton, N. A.

AU - Wolf, S.

N1 - 18 pages, 12 figures. Accepted for publication in Astronomy & Astrophysics

PY - 2024/12/11

Y1 - 2024/12/11

N2 - Aims: We aim to observe the transits and occultations of WASP-33b, which orbits a rapidly-rotating $\delta$ Scuti pulsator, with the goal of measuring the orbital obliquity via the gravity-darkening effect, and constraining the geometric albedo via the occultation depth. Methods: We observed four transits and four occultations with CHEOPS, and employ a variety of techniques to remove the effects of the stellar pulsations from the light curves, as well as the usual CHEOPS systematic effects. We also performed a comprehensive analysis of low-resolution spectral and Gaia data to re-determine the stellar properties of WASP-33. Results: We measure an orbital obliquity 111.3 +0.2 -0.7 degrees, which is consistent with previous measurements made via Doppler tomography. We also measure the planetary impact parameter, and confirm that this parameter is undergoing rapid secular evolution as a result of nodal precession of the planetary orbit. This precession allows us to determine the second-order fluid Love number of the star, which we find agrees well with the predictions of theoretical stellar models. We are unable to robustly measure a unique value of the occultation depth, and emphasise the need for long-baseline observations to better measure the pulsation periods.

AB - Aims: We aim to observe the transits and occultations of WASP-33b, which orbits a rapidly-rotating $\delta$ Scuti pulsator, with the goal of measuring the orbital obliquity via the gravity-darkening effect, and constraining the geometric albedo via the occultation depth. Methods: We observed four transits and four occultations with CHEOPS, and employ a variety of techniques to remove the effects of the stellar pulsations from the light curves, as well as the usual CHEOPS systematic effects. We also performed a comprehensive analysis of low-resolution spectral and Gaia data to re-determine the stellar properties of WASP-33. Results: We measure an orbital obliquity 111.3 +0.2 -0.7 degrees, which is consistent with previous measurements made via Doppler tomography. We also measure the planetary impact parameter, and confirm that this parameter is undergoing rapid secular evolution as a result of nodal precession of the planetary orbit. This precession allows us to determine the second-order fluid Love number of the star, which we find agrees well with the predictions of theoretical stellar models. We are unable to robustly measure a unique value of the occultation depth, and emphasise the need for long-baseline observations to better measure the pulsation periods.

KW - astro-ph.EP

KW - astro-ph.SR

M3 - Preprint

BT - CHEOPS observations confirm nodal precession in the WASP-33 system

ER -