Connecting photometric and spectroscopic granulation signals with CHEOPS and ESPRESSO

S. Sulis; M. Lendl; H. M. Cegla; L. F. Rodríguez Díaz; L. Bigot; V. Van Grootel; A. Bekkelien; A. Collier Cameron; P. F.L. Maxted; A. E. Simon; C. Lovis; G. Scandariato; G. Bruno; D. Nardiello; A. Bonfanti; M. Fridlund; C. M. Persson; S. Salmon; S. G. Sousa; T. G. Wilson; A. Krenn; S. Hoyer; A. Santerne; D. Ehrenreich; Y. Alibert; R. Alonso; G. Anglada; T. Bárczy; D. Barrado Y Navascues; S. C.C. Barros; W. Baumjohann; M. Beck; T. Beck; W. Benz; N. Billot; X. Bonfils; L. Borsato; A. Brandeker; C. Broeg; J. Cabrera; S. Charnoz; C. Corral Van Damme; Sz Csizmadia; M. B. Davies; M. Deleuil; A. Deline; L. Delrez; O. D.S. Demangeon; B. O. Demory; A. Erikson; A. Fortier; L. Fossati; D. Gandolfi; M. Gillon; M. Güdel; K. Heng; K. G. Isaak; L. L. Kiss; J. Laskar; A. Lecavelier Des Etangs; D. Magrin; M. Munari; V. Nascimbeni; G. Olofsson; R. Ottensamer; I. Pagano; E. Pallé; G. Peter; G. Piotto; D. Pollacco; D. Queloz; R. Ragazzoni; N. Rando; H. Rauer; I. Ribas; M. Rieder; N. C. Santos; D. Ségransan; A. M.S. Smith; M. Steinberger; M. Steller; Gy M. Szabó; N. Thomas; S. Udry; N. A. Walton; D. Wolter

doi:10.1051/0004-6361/202244223

Connecting photometric and spectroscopic granulation signals with CHEOPS and ESPRESSO

S. Sulis
, M. Lendl
, H. M. Cegla
, L. F. Rodríguez Díaz
, L. Bigot
, V. Van Grootel
, A. Bekkelien
, A. Collier Cameron
, P. F.L. Maxted
, A. E. Simon
, C. Lovis
, G. Scandariato
, G. Bruno
, D. Nardiello
, A. Bonfanti
, M. Fridlund
, C. M. Persson
, S. Salmon
, S. G. Sousa
, T. G. Wilson

A. Krenn, S. Hoyer, A. Santerne, D. Ehrenreich, Y. Alibert, R. Alonso, G. Anglada, T. Bárczy, D. Barrado Y Navascues, S. C.C. Barros, W. Baumjohann, M. Beck, T. Beck, W. Benz, N. Billot, X. Bonfils, L. Borsato, A. Brandeker, C. Broeg, J. Cabrera, S. Charnoz, C. Corral Van Damme, Sz Csizmadia, M. B. Davies, M. Deleuil, A. Deline, L. Delrez, O. D.S. Demangeon, B. O. Demory, A. Erikson, A. Fortier, L. Fossati, D. Gandolfi, M. Gillon, M. Güdel, K. Heng, K. G. Isaak, L. L. Kiss, J. Laskar, A. Lecavelier Des Etangs, D. Magrin, M. Munari, V. Nascimbeni, G. Olofsson, R. Ottensamer, I. Pagano, E. Pallé, G. Peter, G. Piotto, D. Pollacco, D. Queloz, R. Ragazzoni, N. Rando, H. Rauer, I. Ribas, M. Rieder, N. C. Santos, D. Ségransan, A. M.S. Smith, M. Steinberger, M. Steller, Gy M. Szabó, N. Thomas, S. Udry, N. A. Walton, D. Wolter

LAM
University of Geneva
University of Warwick
Aarhus University
Université Côte d’Azur
University of Liège
University of St Andrews
Keele University
University of Bern
INAF Osservatorio Astrofisico di Catania
INAF Osservatorio Astronomico di Padova
Space Research Institute
University of Leiden
Onsala Space Observatory
Ipatimup Diagnósticos
Instituto de Astrofisica de Canarias
Research Unit; CIBERNED and Universidad de La Laguna
Campus UAB
Institut d’Estudis Espacials de Catalunya (IEEC)
Admatis Ltd.
ESAC campus
Université Grenoble Alpes
Stockholm University
Center for Space and Habitability
DLR
Université Paris Diderot
ESTEC - European Space Research and Technology Centre
Lund University
University of Turin
University of Vienna
University of Warwick
Konkoly Observatory
Eötvös Loránd University
Sorbonne Univ.
Institut d’Astrophysique de Paris
University of Padova
ETH Zurich
University of Cambridge
TU Berlin
Free University of Berlin
Institute of Astronomy

Résultats de recherche: Contribution à un journal › Article › Revue par des pairs

Résumé

Context. Stellar granulation generates fluctuations in photometric and spectroscopic data whose properties depend on the stellar type, composition, and evolutionary state. Characterizing granulation is key for understanding stellar atmospheres and detecting planets. Aims. We aim to detect the signatures of stellar granulation, link spectroscopic and photometric signatures of convection for main-sequence stars, and test predictions from 3D hydrodynamic models. Methods. For the first time, we observed two bright stars (Teff = 5833 and 6205 K) with high-precision observations taken simultaneously with CHEOPS and ESPRESSO. We analyzed the properties of the stellar granulation signal in each individual dataset. We compared them to Kepler observations and 3D hydrodynamic models. While isolating the granulation-induced changes by attenuating and filtering the p-mode oscillation signals, we studied the relationship between photometric and spectroscopic observables. Results. The signature of stellar granulation is detected and precisely characterized for the hotter F star in the CHEOPS and ESPRESSO observations. For the cooler G star, we obtain a clear detection in the CHEOPS dataset only. The TESS observations are blind to this stellar signal. Based on CHEOPS observations, we show that the inferred properties of stellar granulation are in agreement with both Kepler observations and hydrodynamic models. Comparing their periodograms, we observe a strong link between spectroscopic and photometric observables. Correlations of this stellar signal in the time domain (flux versus radial velocities, RV) and with specific spectroscopic observables (shape of the cross-correlation functions) are however difficult to isolate due to S/N dependent variations. Conclusions. In the context of the upcoming PLATO mission and the extreme precision RV surveys, a thorough understanding of the properties of the stellar granulation signal is needed. The CHEOPS and ESPRESSO observations pave the way for detailed analyses of this stellar process.

langue originale	Anglais
Numéro d'article	A24
journal	Astronomy and Astrophysics
Volume	670
Les DOIs	https://doi.org/10.1051/0004-6361/202244223
état	Publié - 1 févr. 2023
Modification externe	Oui

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10.1051/0004-6361/202244223

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Sulis, S., Lendl, M., Cegla, H. M., Rodríguez Díaz, L. F., Bigot, L., Van Grootel, V., Bekkelien, A., Cameron, A. C., Maxted, P. F. L., Simon, A. E., Lovis, C., Scandariato, G., Bruno, G., Nardiello, D., Bonfanti, A., Fridlund, M., Persson, C. M., Salmon, S., Sousa, S. G., ... Wolter, D. (2023). Connecting photometric and spectroscopic granulation signals with CHEOPS and ESPRESSO. Astronomy and Astrophysics, 670, Article A24. https://doi.org/10.1051/0004-6361/202244223

@article{60aac502506d48c1ac6fcd5dd9505ef5,

title = "Connecting photometric and spectroscopic granulation signals with CHEOPS and ESPRESSO",

abstract = "Context. Stellar granulation generates fluctuations in photometric and spectroscopic data whose properties depend on the stellar type, composition, and evolutionary state. Characterizing granulation is key for understanding stellar atmospheres and detecting planets. Aims. We aim to detect the signatures of stellar granulation, link spectroscopic and photometric signatures of convection for main-sequence stars, and test predictions from 3D hydrodynamic models. Methods. For the first time, we observed two bright stars (Teff = 5833 and 6205 K) with high-precision observations taken simultaneously with CHEOPS and ESPRESSO. We analyzed the properties of the stellar granulation signal in each individual dataset. We compared them to Kepler observations and 3D hydrodynamic models. While isolating the granulation-induced changes by attenuating and filtering the p-mode oscillation signals, we studied the relationship between photometric and spectroscopic observables. Results. The signature of stellar granulation is detected and precisely characterized for the hotter F star in the CHEOPS and ESPRESSO observations. For the cooler G star, we obtain a clear detection in the CHEOPS dataset only. The TESS observations are blind to this stellar signal. Based on CHEOPS observations, we show that the inferred properties of stellar granulation are in agreement with both Kepler observations and hydrodynamic models. Comparing their periodograms, we observe a strong link between spectroscopic and photometric observables. Correlations of this stellar signal in the time domain (flux versus radial velocities, RV) and with specific spectroscopic observables (shape of the cross-correlation functions) are however difficult to isolate due to S/N dependent variations. Conclusions. In the context of the upcoming PLATO mission and the extreme precision RV surveys, a thorough understanding of the properties of the stellar granulation signal is needed. The CHEOPS and ESPRESSO observations pave the way for detailed analyses of this stellar process.",

keywords = "Methods: data analysis, Stars: Atmospheres, Sun: granulation, Techniques: photometric, Techniques: radial velocities",

author = "S. Sulis and M. Lendl and Cegla, \{H. M.\} and \{Rodr{\'i}guez D{\'i}az\}, \{L. F.\} and L. Bigot and \{Van Grootel\}, V. and A. Bekkelien and Cameron, \{A. Collier\} and Maxted, \{P. F.L.\} and Simon, \{A. E.\} and C. Lovis and G. Scandariato and G. Bruno and D. Nardiello and A. Bonfanti and M. Fridlund and Persson, \{C. M.\} and S. Salmon and Sousa, \{S. G.\} and Wilson, \{T. G.\} and A. Krenn and S. Hoyer and A. Santerne and D. Ehrenreich and Y. Alibert and R. Alonso and G. Anglada and T. B{\'a}rczy and \{Barrado Y Navascues\}, D. and Barros, \{S. C.C.\} and W. Baumjohann and M. Beck and T. Beck and W. Benz and N. Billot and X. Bonfils and L. Borsato and A. Brandeker and C. Broeg and J. Cabrera and S. Charnoz and \{Corral Van Damme\}, C. and Sz Csizmadia and Davies, \{M. B.\} and M. Deleuil and A. Deline and L. Delrez and Demangeon, \{O. D.S.\} and Demory, \{B. O.\} and A. Erikson and A. Fortier and L. Fossati and D. Gandolfi and M. Gillon and M. G{\"u}del and K. Heng and Isaak, \{K. G.\} and Kiss, \{L. L.\} and J. Laskar and \{Lecavelier Des Etangs\}, A. and D. Magrin and M. Munari 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 H. Rauer and I. Ribas and M. Rieder and Santos, \{N. C.\} and D. S{\'e}gransan and Smith, \{A. M.S.\} and M. Steinberger and M. Steller and Szab{\'o}, \{Gy M.\} and N. Thomas and S. Udry and Walton, \{N. A.\} and D. Wolter",

note = "Publisher Copyright: {\textcopyright} Authors 2023",

year = "2023",

month = feb,

day = "1",

doi = "10.1051/0004-6361/202244223",

language = "English",

volume = "670",

journal = "Astronomy and Astrophysics",

issn = "0004-6361",

}

Sulis, S, Lendl, M, Cegla, HM, Rodríguez Díaz, LF, Bigot, L, Van Grootel, V, Bekkelien, A, Cameron, AC, Maxted, PFL, Simon, AE, Lovis, C, Scandariato, G, Bruno, G, Nardiello, D, Bonfanti, A, Fridlund, M, Persson, CM, Salmon, S, Sousa, SG, Wilson, TG, Krenn, A, Hoyer, S, Santerne, A, Ehrenreich, D, Alibert, Y, Alonso, R, Anglada, G, Bárczy, T, Barrado Y Navascues, D, Barros, SCC, Baumjohann, W, Beck, M, Beck, T, Benz, W, Billot, N, Bonfils, X, Borsato, L, Brandeker, A, Broeg, C, Cabrera, J, Charnoz, S, Corral Van Damme, C, Csizmadia, S, Davies, MB, Deleuil, M, Deline, A, Delrez, L, Demangeon, ODS, Demory, BO, Erikson, A, Fortier, A, Fossati, L, Gandolfi, D, Gillon, M, Güdel, M, Heng, K, Isaak, KG, Kiss, LL, Laskar, J, Lecavelier Des Etangs, A, Magrin, D, Munari, M, Nascimbeni, V, Olofsson, G, Ottensamer, R, Pagano, I, Pallé, E, Peter, G, Piotto, G, Pollacco, D, Queloz, D, Ragazzoni, R, Rando, N, Rauer, H, Ribas, I, Rieder, M, Santos, NC, Ségransan, D, Smith, AMS, Steinberger, M, Steller, M, Szabó, GM, Thomas, N, Udry, S, Walton, NA & Wolter, D 2023, 'Connecting photometric and spectroscopic granulation signals with CHEOPS and ESPRESSO', Astronomy and Astrophysics, VOL. 670, A24. https://doi.org/10.1051/0004-6361/202244223

TY - JOUR

T1 - Connecting photometric and spectroscopic granulation signals with CHEOPS and ESPRESSO

AU - Sulis, S.

AU - Lendl, M.

AU - Cegla, H. M.

AU - Rodríguez Díaz, L. F.

AU - Bigot, L.

AU - Van Grootel, V.

AU - Bekkelien, A.

AU - Cameron, A. Collier

AU - Maxted, P. F.L.

AU - Simon, A. E.

AU - Lovis, C.

AU - Scandariato, G.

AU - Bruno, G.

AU - Nardiello, D.

AU - Bonfanti, A.

AU - Fridlund, M.

AU - Persson, C. M.

AU - Salmon, S.

AU - Sousa, S. G.

AU - Wilson, T. G.

AU - Krenn, A.

AU - Hoyer, S.

AU - Santerne, A.

AU - Ehrenreich, D.

AU - Alibert, Y.

AU - Alonso, R.

AU - Anglada, G.

AU - Bárczy, T.

AU - Barrado Y Navascues, D.

AU - Barros, S. C.C.

AU - Baumjohann, W.

AU - Beck, M.

AU - Beck, T.

AU - Benz, W.

AU - Billot, N.

AU - Bonfils, X.

AU - Borsato, L.

AU - Brandeker, A.

AU - Broeg, C.

AU - Cabrera, J.

AU - Charnoz, S.

AU - Corral Van Damme, C.

AU - Csizmadia, Sz

AU - Davies, M. B.

AU - Deleuil, M.

AU - Deline, A.

AU - Delrez, L.

AU - Demangeon, O. D.S.

AU - Demory, B. O.

AU - Erikson, A.

AU - Fortier, A.

AU - Fossati, L.

AU - Gandolfi, D.

AU - Gillon, M.

AU - Güdel, M.

AU - Heng, K.

AU - Isaak, K. G.

AU - Kiss, L. L.

AU - Laskar, J.

AU - Lecavelier Des Etangs, A.

AU - Magrin, D.

AU - Munari, M.

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 - Rauer, H.

AU - Ribas, I.

AU - Rieder, M.

AU - Santos, N. C.

AU - Ségransan, D.

AU - Smith, A. M.S.

AU - Steinberger, M.

AU - Steller, M.

AU - Szabó, Gy M.

AU - Thomas, N.

AU - Udry, S.

AU - Walton, N. A.

AU - Wolter, D.

PY - 2023/2/1

Y1 - 2023/2/1

N2 - Context. Stellar granulation generates fluctuations in photometric and spectroscopic data whose properties depend on the stellar type, composition, and evolutionary state. Characterizing granulation is key for understanding stellar atmospheres and detecting planets. Aims. We aim to detect the signatures of stellar granulation, link spectroscopic and photometric signatures of convection for main-sequence stars, and test predictions from 3D hydrodynamic models. Methods. For the first time, we observed two bright stars (Teff = 5833 and 6205 K) with high-precision observations taken simultaneously with CHEOPS and ESPRESSO. We analyzed the properties of the stellar granulation signal in each individual dataset. We compared them to Kepler observations and 3D hydrodynamic models. While isolating the granulation-induced changes by attenuating and filtering the p-mode oscillation signals, we studied the relationship between photometric and spectroscopic observables. Results. The signature of stellar granulation is detected and precisely characterized for the hotter F star in the CHEOPS and ESPRESSO observations. For the cooler G star, we obtain a clear detection in the CHEOPS dataset only. The TESS observations are blind to this stellar signal. Based on CHEOPS observations, we show that the inferred properties of stellar granulation are in agreement with both Kepler observations and hydrodynamic models. Comparing their periodograms, we observe a strong link between spectroscopic and photometric observables. Correlations of this stellar signal in the time domain (flux versus radial velocities, RV) and with specific spectroscopic observables (shape of the cross-correlation functions) are however difficult to isolate due to S/N dependent variations. Conclusions. In the context of the upcoming PLATO mission and the extreme precision RV surveys, a thorough understanding of the properties of the stellar granulation signal is needed. The CHEOPS and ESPRESSO observations pave the way for detailed analyses of this stellar process.

AB - Context. Stellar granulation generates fluctuations in photometric and spectroscopic data whose properties depend on the stellar type, composition, and evolutionary state. Characterizing granulation is key for understanding stellar atmospheres and detecting planets. Aims. We aim to detect the signatures of stellar granulation, link spectroscopic and photometric signatures of convection for main-sequence stars, and test predictions from 3D hydrodynamic models. Methods. For the first time, we observed two bright stars (Teff = 5833 and 6205 K) with high-precision observations taken simultaneously with CHEOPS and ESPRESSO. We analyzed the properties of the stellar granulation signal in each individual dataset. We compared them to Kepler observations and 3D hydrodynamic models. While isolating the granulation-induced changes by attenuating and filtering the p-mode oscillation signals, we studied the relationship between photometric and spectroscopic observables. Results. The signature of stellar granulation is detected and precisely characterized for the hotter F star in the CHEOPS and ESPRESSO observations. For the cooler G star, we obtain a clear detection in the CHEOPS dataset only. The TESS observations are blind to this stellar signal. Based on CHEOPS observations, we show that the inferred properties of stellar granulation are in agreement with both Kepler observations and hydrodynamic models. Comparing their periodograms, we observe a strong link between spectroscopic and photometric observables. Correlations of this stellar signal in the time domain (flux versus radial velocities, RV) and with specific spectroscopic observables (shape of the cross-correlation functions) are however difficult to isolate due to S/N dependent variations. Conclusions. In the context of the upcoming PLATO mission and the extreme precision RV surveys, a thorough understanding of the properties of the stellar granulation signal is needed. The CHEOPS and ESPRESSO observations pave the way for detailed analyses of this stellar process.

KW - Methods: data analysis

KW - Stars: Atmospheres

KW - Sun: granulation

KW - Techniques: photometric

KW - Techniques: radial velocities

UR - https://www.scopus.com/pages/publications/85147676859

U2 - 10.1051/0004-6361/202244223

DO - 10.1051/0004-6361/202244223

M3 - Article

AN - SCOPUS:85147676859

SN - 0004-6361

VL - 670

JO - Astronomy and Astrophysics

JF - Astronomy and Astrophysics

M1 - A24

ER -

Connecting photometric and spectroscopic granulation signals with CHEOPS and ESPRESSO

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