Kepler / TESS (And Gaia): 6 Little Information on Their Detailed Properties 0 0.2 0.4 0.6 0.8 1.0 1.2 1.4 Jmag-Kmag ASJ-Kteros ASTERO CHRONOMETRY CHRONOMETRY

ASTEROSEISMOLOGY MODEL CALIBRATION

A. Miglio, J. Montalban, B. Mosser, P. Ventura WP127: seismic constraints from ageing stars

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Logo on white background Logo on dark background aim TESS S-CVZ

-6 what which stars are we referring to -4

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Logo on white background Logo on dark background aim TESS S-CVZ

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Logo on white background Logo on dark background what TESS S-CVZ G-K giants -6

radii up to 10 Rsun -4

-2 M ~ 0.8 - 4 Msun s

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all metallicities [-2, 0.5] 2 kmag+5*log10(parallax)-10

4 prior to CoRoT / Kepler / TESS (and Gaia): 6 little information on their detailed properties 0 0.2 0.4 0.6 0.8 1.0 1.2 1.4 jmag-kmag ASJ-KTEROs ASTERO CHRONOMETRY CHRONOMETRY

Logo on white background Logo on dark background what TESS S-CVZ G-K giants -6

radii up to 10 Rsun -4

-2 M ~ 0.8 - 4 Msun s

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all metallicities [-2, 0.5] 2 kmag+5*log10(parallax)-10

4 prior to CoRoT / Kepler / TESS (and Gaia): 6 little information on their detailed properties 0 0.2 0.4 0.6 0.8 1.0 1.2 1.4 jmag-kmag ASJ-KTEROs ASTERO CHRONOMETRY CHRONOMETRY

Logo on white background Logo on dark background what + asteroseismology

gravity acoustic mode mode νi

Hz] 30 / μ 2 He core 15

120 140 160 200

H-burning shell [ppm PSD Frequency [μHz]

H-rich radiative transport of angular momentum core talk by Charlotte Gehan later today constraints on internal mixing

precise and accurate global parameters ASTERO ASTERO CHRONOMETRY CHRONOMETRY

Logo on white background Logo on dark background 2 whyCampante et al. (Received January 1, 2018; Revised January 7, 2018; Accepted September 16, 2019) Submitted to ApJ

planets around G-K giants ABSTRACT The Transiting Exoplanet Survey Satellite (TESS) is performing a near all-sky survey for planets thatimproved transit bright stellar stars. properties In addition, its excellent improved photometric planetary precision parameters enables asteroseismology of solar-type and red-giant stars, which exhibit convection-driven, solar-like oscillations. Simulations Draftpredict version that September TESS will 16, detect 2019 solar-like oscillations in nearly 100 stars already known to host planets. A TypesetIn this using paper, L TEX wetwocolumn presentstyle ane.g. asteroseismic in AASTeX62Campante analysis et ofal. the 2019, known in red-giant press host stars HD 212771 and HD 203949, both systems having a long-period planet detected through radial velocities. These are the first detections of oscillations in previously known exoplanet-host stars by TESS, further showcasing TESSthe mission’s ASTEROSEISMOLOGY potential to conduct OF THE asteroseismology KNOWN RED-GIANT of red-giant HOST stars. STARS We HD estimate 212771 the AND fundamental HD 203949 propertiesTiago L. of Campante both stars,1, 2, through 3 Enrico a Corsaro grid-based,4 Mikkel modeling N. Lund approach,5, 3 Beno thatˆıt uses Mosser global,6 Aldo asteroseismic Serenelli,7, param- 8, 3 9, 10, 3, 1 11 12, 5 13 eters asDimitri input. Veras We discuss, ⇤ theVardan evolutionary Adibekyan state, H. of M. HD Antia 203949, Warrick in depth Ball and, noteSarbani the large Basu discrepancy, Timothybetween R.its Bedding asteroseismic,14, 5, 3 Diego mass ( BossiniM =1,1.23Guy0 R..15 Davies M if,12, on 5 Elisa the red-giant Delgado branch Mena,1 orRafaelM =1 A..00 Garc0´.ıa16,15, M 16 Rasmus Handberg,5 Marc Hon,17 ⇤Stephen± R. Kane,18 Steven D. Kawaler,19, 3 James S.⇤ Kuszlewicz± ,20, 5 if in the clump)19 and the mass21, 22 quoted in the discovery23 paper (M =2.112, 5,0 24.1M ), implying a change25, 3 Miles Lucas, Savita Mathur, Nicolas Nardetto, Martin B. Nielsen⇤ , ± Marc H. Pinsonneault, >Sabine30 % Reffert in the, planet’s26 V´ıctor mass. Silva Aguirre Assuming,5 Keivan HD 203949 G. Stassun to be,27, in 28 Dennis the clump, Stello we,17, investigate 14, 5, 3 Stephan the Stock planet’s,26 past orbitalMathieu evolution Vrard,1 Mutlu and discuss Yıldız, how29 William it could J. Chaplin have avoided,12, 5, 3 Daniel engulfment Huber at,30, 3 theJacob tip L. of Bean the red-giant,31 29 1, 2 5, 3 5, 32 branch.Zeynep Finally, Çelik Orhan HD 212771, Margarida was observed S. Cunha by, K2Jørgen during Christensen-Dalsgaard its Campaign 3, thus allowing, Hans for Kjeldsen a preliminary, Travis S. Metcalfe,33, 20 Andrea Miglio,12, 5 Mario´ J. P. F. G. Monteiro,1, 2 Benard Nsamba,1 Sibel Ortel¨ ,29 comparisonFilipe of the Pereira asteroseismic,1 Sergio´ performances G. Sousa,1, 2 Maria of TESS Tsantaki and, K2.1 and We Margaret estimate C. the Turnbull ratio of34 the observed oscillation amplitudes for this star to be ATESS/AK2 =0.75 0.14, consistent with the expected ratio 1Instituto de Astrof´ısica e Ciências do Espa¸co, Universidademax max do Porto,± Rua das Estrelas, 4150-762 Porto, Portugal 2 of 0.85 due to the redder bandpass of TESS. ASTERO Departamento de F´ısica e Astronomia, Faculdade de Ciências da Universidade do Porto, Rua doAS Campo Alegre, s/n,TERO 4169-007 Porto, ⇠ Portugal Keywords:3Kavliasteroseismology Institute for Theoretical — planet-star Physics, University interactions of California, — stars: Santa Barbara, fundamental CACHRONOMETRY 93106-4030, parameters USA — stars: CHRONOMETRY 4 individualINAF (HD — Osservatorio 212771, HD Astrofisico 203949) di Catania, — techniques: via S. Sofia photometric 78, 95123 Catania, Italy 5Stellar Astrophysics Centre (SAC), Department of Physics and Astronomy, Aarhus University, Ny Munkegade 120, 8000 Aarhus C, Denmark 6LESIA, Observatoire1. INTRODUCTION de Paris, UniversitéPSL, CNRS, Sorbonne Université,ing Universitéde (e.g., Serenelli Paris, et 5 al.place2017 Jules; Janssen,Silva Aguirre 92195 Meudon, et al. 2017; France Nsamba et al. 2018) strategies, as well as on state-of-the- Major advances7 in stellar interiors physics and evolu- Institute of Space Sciences (ICE, CSIC) Campus UAB, Carrerart de optimization Can Magrans, s/n, procedures E-08193, Bellaterra, that make Spain use of individual tion have recently8 beenInstitut made d’Estudis possible Espacials by de asteroseismol- Catalunya (IEEC), C/Gran Capità, 2-4, E-08034, Barcelona, Spain ogy. This has largely9 beenCentre due for Exoplanets to the exquisite and Habitability, space- Universityoscillation of Warwick, frequencies Coventry CV4 (e.g., 7AL,Metcalfe UK et al. 2010; Mathur based data made available10 byDepartment CNES/ESA’s of Physics, CoRoT University of Warwick,et al. 2012 Coventry; Silva CV4 Aguirre 7AL, UK et al. 2015; Rendle et al. 2019). 11 (Baglin et al. 2009) and NASA’s KeplerTata Institute/K2 (Borucki of Fundamental Research,These Mumbai, techniques India make it possible to estimate precise 12School of Physics and Astronomy, University of Birmingham,properties Edgbaston, of large Birmingham numbers B15 of 2TT, field UK stars, for which such et al. 2010; Koch et13 al. 2010; Howell et al. 2014) missions. Department of Astronomy, Yale University, P.O. Boxinformation 208101, New Haven, is sparse. CT 06520-8101, As a result, USA asteroseismology is In particular, asteroseismology14Sydney Institute for has Astronomy vastly benefited (SIfA), School the of Physics, University of Sydney, NSW 2006, Australia having a profound impact on modern astrophysics, no- study of solar-type and red-giant15IRFU, stars, CEA, UniversitéParis-Saclay, which exhibit F-91191 Gif-sur-Yvette, France convection-driven,16AIM, CEA, CNRS,solar-like UniversitéParis-Saclay, oscillations (for UniversitéParis a review, Diderot,tably Sorbonne on the Paris field Cité, of F-91191 exoplanetary Gif-sur-Yvette, science France (Campante 17 see Chaplin & Miglio 2013School). The of Physics, revolution The University triggered of by New Southet Wales, al. 2018 Sydney). Characterization NSW 2052, Australia of exoplanet-host stars via 18Department of Earth and Planetary Sciences, Universityasteroseismology of California, Riverside, allows CA for 92521, unmatched USA precision in the CoRoT and Kepler/K219 is set to continue over the com- Department of Physics and Astronomy, Iowa Stateabsolute University, properties Ames, IA of 50011, their USA planets (Huber et al. 2013a; ing decade, with20 NASA’s TESS (Ricker et al. 2015) and Max-Planck-Institut fürSonnensystemforschung, Justus-von-Liebig-WegBallard et al. 3,2014 37077; Campante Göttingen, Germany et al. 2015; Silva Aguirre ESA’s PLATO (Rauer et21 al.Instituto2014) de missions Astrof´ısica expected de Canarias to (IAC), E-38205 La Laguna, Tenerife, Spain raise the number22 ofUniversidad known solar-like de La Laguna oscillators (ULL), Departamento by up to de Astrof´ısica,et al. 2015 E-38206; Lundkvist La Laguna, et Tenerife, al. 2016 Spain). Furthermore, aster- two orders of magnitude23UniversitéCôte (Huber 2018 d’Azur,). Observatoire de la Côte d’Azur,oseismology CNRS, Laboratoire enables Lagrange, constraints France on the spin-orbit align- 24 Logo on white background Logo on dark background Fueled by theCenter wealth for Space of high-quality Science, NYUAD seismic Institute, data, New the York Universityment Abu of Dhabi, exoplanet PO Box systems 129188, ( AbuChaplin Dhabi, et UAE al. 2013; Huber 25Department of Astronomy, The Ohio State University,et al. 2013b Columbus,; Campante OH 43210, et USAal. 2016a; Kamiaka et al. 2019) past few years26 have witnessed an ever-growing e↵ort be- Landessternwarte, Zentrum fürAstronomie der Universität Heidelberg,as well as Königstuhl statistical 12, 69117 inferences Heidelberg, on Germany orbital eccentricities ing devoted27Vanderbilt to the development University, Department of novel of techniques Physics and Astronomy, for 6301 Stevenson Center Ln., Nashville, TN 37235, USA thearXiv:1909.05961v1 [astro-ph.SR] 12 Sep 2019 estimation28Vanderbilt of fundamental Initiative in Data-intensive stellar properties. Astrophysics The (VIDA), 6301via Stevenson asterodensity Center Ln., profiling Nashville, (Sliski TN 37235, & Kipping USA 2014; Van focus has been29Department placed on of Astronomy uniform and data Space analysis Sciences, (e.g., Science Faculty,Eylen Ege & University, Albrecht 35100,2015 Bornova,; Van EylenIzmir,˙ Turkey et al. 2019). 30 Davies et al. 2016; LundInstitute et al. for Astronomy,2017b) and University stellar ofmodel- Hawai‘i, 2680 WoodlawnThe Transiting Drive, Honolulu, Exoplanet HI 96822, Survey USA Satellite (TESS) is 31Department of Astronomy and Astrophysics, University of Chicago,performing 5640 S. Ellis a near Avenue, all-sky Chicago, survey IL 60637, for planets USA that transit 32 Institute of Theoretical Physics and Astronomy, Vilnius University,bright Saul˙etekio stars. Moreover, av. 3, 10257 its Vilnius, excellent Lithuania photometric preci- 33Space Science Institute, 4750 Walnut Street, Suite 205, Boulder, CO 80301, USA ⇤ STFC Ernest Rutherford Fellow sion, combined with its fine time sampling and long in- 34SETI Institute, Carl Sagan Center for the Study of Life in the Universe, O↵-Site: 2801 She↵ord Drive, Madison, WI 53719, USA

Corresponding author: Tiago L. Campante [email protected] why planets around G-K giants

improved stellar properties improved planetary parameters

evolution of planetary systems e.g. Veras et al. 2016

occurrence rates of planets e.g. Johnson et al. ,

around stars M> 1.5 Msun Campante et al. North et al.

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Logo on white background Logo on dark background why planets around G-K giants

improved stellar properties improved planetary parameters

evolution of planetary systems e.g. Veras et al. 2016

occurrence rates of planets e.g. Johnson et al. ,

around stars M> 1.5 Msun Campante et al. North et al. population studies talk by Cristina Chiappini later today

ASTERO ASTERO CHRONOMETRY CHRONOMETRY

Logo on white background Logo on dark background why planets around G-K giants

improved stellar properties improved planetary parameters

evolution of planetary systems e.g. Veras et al. 2016

occurrence rates of planets e.g. Johnson et al. ,

around stars M> 1.5 Msun Campante et al. North et al. population studies talk by Cristina Chiappini later today to constrain stellar physics which is relevant to inferring ages of MS stars “calibrators" ASTERO ASTERO CHRONOMETRY CHRONOMETRY

Logo on white background Logo on dark background age uncertainties of MS stars are typically fractional uncertaintiesY. Lebreton, M.J. of Goupil the & total J. Montalb´an: MS Stellarlifetime Models Uncertainties 71 at the MS turnoff systematic uncertainties on age are dominated by:

Fig. 43. Synthesis of the rangesLebreton, of relative Goupil age & di Montalban↵erences at2014 TO, as obtained when ASTERO changing one of the inputs of the reference model (deﬁned in Sect. 2.4.3). FromAS left TERO to right, the case labels on the abscissae correspond to the following changes: [1, 2] [Fe/H] abundance by 0.1 dex with respect to solar, [3, 4] initial helium abundanceCHRONOMETRY by CHRONOMETRY ± 0.03 with respect to solar, [5] Y/Z by +3 with respect to solar, [6,7] ↵-elements ± enhancement of +0.4 dex at [Fe/H]=0.0 (a) and 1.0 dex (b), [8] solar mixture (AGSS09 vs GN93 mixture), [9] opacity (increased by 10 per cent), [10] conductive opacity, Iben

(1975) vs Cassisi et al. (2007) formalism, [11] pp reaction rate (decreased by 15 per 14 15 cent), [12, 13] CNO (LUNA vs NACRE rate for the N(p, ) O rate) at [Fe/H]= 0.0 dex (a) and 2.0 dex (c), [14] screening factor in nuclear reaction rates (no screening vs screening), [15, 16] atomic di↵usion for (d) di↵usion vs no di↵usion and (e) no di↵usion vs

di↵usion with di↵usion velocities increased by 20 per cent, [17, 18] ↵MLT value by 0.20 ± dex with respect to solar, [19] prescription for convection (MLT vs FST), [20] convective 1 core overshooting (↵ov =0.20 vs no overshooting), [21, 22] rotation (⌦ =50kms vs no rotation), at [Fe/H]=0.0 dex (a) and 1.0dex(b). ⇠

exactly the prescribed input physics and constants (blue symbols in Fig. 42), the di↵erences are reduced by a factor of about two. In this case, we can consider that the di↵erences between the code results are only due to di↵erences in numerical treatments, that is the handling of table interpolation (to get the opacity, EoS outputs, etc.), the methods used to solve the equations, and hidden numerical

A initial He abundance

A B initial He mass of the He core, abundance hence near-core mixing

Logo on white background Logo on dark background why e.g. A and B cannot be inferred from Sun-like pulsators alone:

A YSURF difficult to determine with seismology and we can map Y=Y(Z) affected by diffusion + rotation (e.g. Verma et al. 2019)

limited inference on core overshooting because B we can map of low sensitivity of acoustic modes, and stars OVcore=OVcore(M,Z) with convective cores being too hot

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Logo on white background Logo on dark background why e.g. A and B cannot be inferred from Sun-like pulsators alone:

A YSURF difficult to determine with seismology and we can map Y=Y(Z) affected by diffusion + rotation (e.g. Verma et al. 2019)

limited inference on core overshooting because B we can map of low sensitivity of acoustic modes, and stars OVcore=OVcore(M,Z) with convective cores being too hot

this is possible looking at low-luminosity giants / subgiants, red-clump and secondary clump stars ASTERO ASTERO CHRONOMETRY CHRONOMETRY

Logo on white background Logo on dark background why e.g. A and B cannot be inferred from Sun-like pulsators alone:

A YSURF difficult to determine with seismology and we can map Y=Y(Z) affected by diffusion + rotation (e.g. Verma et al. 2019)

limited inference on core overshooting because B we can map of low sensitivity of acoustic modes, and stars OVcore=OVcore(M,Z) with convective cores being too hot

this is possible looking at low-luminosity giants / subgiants, red-clump and secondary clump stars

more examples + numbers in: "WP127 seismic constraints from ageing stars; from seismic goalsAS to quantitativeTERO needs” ASTERO CHRONOMETRY CHRONOMETRY

Logo on white background Logo on dark background why

! Kepler / TESS have observed / are observing G-K giants (intentionally)

PLATO will live in a landscape enriched by results from CoRoT/Kepler/K2/TESS

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Logo on white background Logo on dark background why

! Kepler / TESS have observed / are observing G-K giants (intentionally)

PLATO will live in a landscape enriched by results from CoRoT/Kepler/K2/TESS however: Kepler target selection based on CMD cuts + estimates of R (pre Gaia)

Kepler limited exploration of [Fe/H], mass distribution

dominated by 1.2-1.4 Msun

K2, TESS: limited duration of the observations ASTERO ASTERO CHRONOMETRY CHRONOMETRY

Logo on white background Logo on dark background how

WP127 happy to help / provide resources to aid the selection

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Logo on white background Logo on dark background how

WP127 happy to help / provide resources to aid the selection

a lot of progress since CoRoT and Kepler, we can be smart about how we select stars, ensuring we cover relevant mass / metallicity bins

Gaia spectroscopic characterisation of targets PIC (e.g. synergies with 4MOST)

“low-resolution”/ survey asteroseismology from TESS ASTERO ASTERO CHRONOMETRY CHRONOMETRY

Logo on white background Logo on dark background how

WP127 happy to help / provide resources to aid the selection

iterate with core science to define in detail the needs

(e.g. σage) and parameter range (M, [Fe/H])

needs for red giant seismology: long-cadence light curves (no short-cadence data, no imagette)

ASTERO ASTERO CHRONOMETRY CHRONOMETRY

Logo on white background Logo on dark background how

WP127 happy to help / provide resources to aid the selection

iterate with core science to define in detail the needs

(e.g. σage) and parameter range (M, [Fe/H])

needs for red giant seismology: long-cadence light curves (no short-cadence data, no imagette)

define suitable&affordable telemetry cost / number of targets ASTERO ASTERO CHRONOMETRY CHRONOMETRY

Logo on white background Logo on dark background summary science with solar-like oscillating G-K giants

field is mature optimise the scientific return/number of targets

ASTERO ASTERO CHRONOMETRY CHRONOMETRY

Logo on white background Logo on dark background summary science with solar-like oscillating G-K giants

field is mature optimise the scientific return/number of targets

PLATO can go beyond Kepler / K2 / TESS and use G-K giants as calibrators for MS stars

+ for the same “price” exoplanets around evolved stars stellar population studies ASTERO ASTERO CHRONOMETRY CHRONOMETRY

Logo on white background Logo on dark background summary science with solar-like oscillating G-K giants

field is mature optimise the scientific return/number of targets

PLATO can go beyond Kepler / K2 / TESS high scientific return and use G-K giants as calibrators for MS stars no interference with + for the same “price” high-priority targets exoplanets around evolved stars direct benefit to core science stellar population studies ASTERO ASTERO CHRONOMETRY CHRONOMETRY

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add to S5 a carefully selected sample of G-K giants?

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add to S5 a carefully selected sample of G-K giants? G -6 -6 IAMPAOLO

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… almost there! ASTERO ASTERO CHRONOMETRY CHRONOMETRY

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