Connecting photometric and spectroscopic granulation signals with CHEOPS and ESPRESSO

S. Sulis; M. Lendl; H. Cegla; L. F. Rodriguez Diaz; 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. Lecavalier 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. Cegla, L. F. Rodriguez Diaz, 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. WilsonA. 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. Lecavalier 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

^*Corresponding author for this work

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

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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 (T_eff = 5833 K 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 data set. We compared them to Kepler observations and 3D hydrodynamic models. While isolating the granulation-induced changes by attenuating 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 vs RV) and with specific spectroscopic observables (shape of the cross-correlation functions) are however difficult to isolate due to signal-to-noise 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.

Original language	English
Article number	A24
Number of pages	30
Journal	Astronomy & Astrophysics
Volume	670
DOIs	https://doi.org/10.1051/0004-6361/202244223
Publication status	Published - 1 Feb 2023

Keywords

Techniques: radial velocities and photometric
Sun: granulation
Stars: atmospheres
Methods: data analysis
Techniques: photometric

Access to Document

10.1051/0004-6361/202244223Licence: CC BY

Sulis_2023_AA_Connecting-photometric_CC
Copyright © The Authors 2023. 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, 7.06 MBLicence: CC BY

https://arxiv.org/abs/2211.14398Licence: 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
Support for the PLATO Development: Support for the PLATO Development Phase 2017-2022: Planet candidate ranking and validation
Cameron, A. C. (PI)
Science & Technology Facilities Council
1/08/17 → 31/12/22
Project: Standard

Photometric and spectroscopic granulation signals : J/A+A/670/A24
Cameron, A. C. (Creator) & Wilson, T. G. (Creator), VizieR On-line Data Catalog, 2023
https://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/670/A24
Dataset

Cite this

Sulis, S., Lendl, M., Cegla, H., Diaz, L. F. R., Bigot, L., Grootel, V. 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 & Astrophysics, 670, Article A24. https://doi.org/10.1051/0004-6361/202244223

@article{1d945a5ac8a448db9815c998b991fbd2,

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 K 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 data set. We compared them to Kepler observations and 3D hydrodynamic models. While isolating the granulation-induced changes by attenuating 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 vs RV) and with specific spectroscopic observables (shape of the cross-correlation functions) are however difficult to isolate due to signal-to-noise 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 = "Techniques: radial velocities and photometric, Sun: granulation, Stars: atmospheres, Methods: data analysis, Techniques: photometric",

author = "S. Sulis and M. Lendl and H. Cegla and Diaz, {L. F. Rodriguez} and L. Bigot and Grootel, {V. Van} 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 Navascues, {D. Barrado y} 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 Damme, {C. Corral van} 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 K.G. Isaak and L.L. Kiss and J. Laskar and {Lecavalier 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 N.C. Santos 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 N.A. Walton and D. Wolter",

note = "Funding: ACC and TGW acknowledge support from STFC consolidated grant numbers ST/R000824/1 and ST/V000861/1, and UKSA grant number ST/R003203/1.",

year = "2023",

month = feb,

day = "1",

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

language = "English",

volume = "670",

journal = "Astronomy & Astrophysics",

issn = "0004-6361",

publisher = "EDP SCIENCES S A",

}

Sulis, S, Lendl, M, Cegla, H, Diaz, LFR, Bigot, L, Grootel, VV, 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, Navascues, DBY, Barros, SCC, Baumjohann, W, Beck, M, Beck, T, Benz, W, Billot, N, Bonfils, X, Borsato, L, Brandeker, A, Broeg, C, Cabrera, J, Charnoz, S, Damme, CCV, Csizmadia, S, Davies, MB, Deleuil, M, Deline, A, Delrez, L, Demangeon, ODS, Demory, B-O, Erikson, A, Fortier, A, Fossati, L, Gandolfi, D, Gillon, M, Güdel, M, Heng, K, Isaak, KG, Kiss, LL, Laskar, J, Lecavalier 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 & 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.

AU - Diaz, L. F. Rodriguez

AU - Bigot, L.

AU - Grootel, V. Van

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 - Navascues, D. Barrado y

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 - Damme, C. Corral van

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 - Lecavalier 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.

N1 - Funding: ACC and TGW acknowledge support from STFC consolidated grant numbers ST/R000824/1 and ST/V000861/1, and UKSA grant number ST/R003203/1.

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 K 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 data set. We compared them to Kepler observations and 3D hydrodynamic models. While isolating the granulation-induced changes by attenuating 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 vs RV) and with specific spectroscopic observables (shape of the cross-correlation functions) are however difficult to isolate due to signal-to-noise 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 K 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 data set. We compared them to Kepler observations and 3D hydrodynamic models. While isolating the granulation-induced changes by attenuating 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 vs RV) and with specific spectroscopic observables (shape of the cross-correlation functions) are however difficult to isolate due to signal-to-noise 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 - Techniques: radial velocities and photometric

KW - Sun: granulation

KW - Stars: atmospheres

KW - Methods: data analysis

KW - Techniques: photometric

U2 - 10.1051/0004-6361/202244223

DO - 10.1051/0004-6361/202244223

M3 - Article

SN - 0004-6361

VL - 670

JO - Astronomy & Astrophysics

JF - Astronomy & Astrophysics

M1 - A24

ER -

Connecting photometric and spectroscopic granulation signals with CHEOPS and ESPRESSO

Abstract

Keywords

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Projects

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

Support for the PLATO Development: Support for the PLATO Development Phase 2017-2022: Planet candidate ranking and validation

Datasets

Photometric and spectroscopic granulation signals : J/A+A/670/A24

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