PLATO <i>as it is</i>: A legacy mission for Galactic archaeology

Miglio, A.; Chiappini, Cristina; Mosser, B.; Davies, G. R.; Freeman, K. C.; Girardi, L.; Jofré, P.; Kawata, Daisuke; Rendle, B. M.; Valentini, M.; Casagrande, Luca; Chaplin, W. J.; Gilmore, G.; Hawkins, Keith; Holl, B.; Appourchaux, T.; Belkacem, K.; Bossini, D.; Brogaard, K.; Goupil, M. J.; Montalbán, J.; Noels, A.; Anders, F.; Rodrigues, Thaíse S.; Piotto, G.; Pollacco, D.; Rauer, H.; Prieto, C. Allende; Avelino, P. P.; Babusiaux, C.; Barban, C.; Barbuy, B.; Basu, Sarbani; Baudin, F.; Benomar, O.; Bienaymé, O.; Binney, James; Bland‐Hawthorn, J.; Bressan, A.; Cacciari, C.; Campante, Tiago L.; Cassisi, S.; Christensen‐Dalsgaard, J.; Combes, F.; Creevey, O.; Cunha, M. S.; Jong, Roelof S. de; Laverny, P. de; Degl’Innocenti, S.; Deheuvels, S.; Depagne, É.; Ridder, J. De; Matteo, P. Di; Mauro, M. P. Di; Dupret, Marc‐Antoine; Eggenberger, P.; Elsworth, Y.; Famaey, Benoît; Feltzing, Sofia; García, R. A.; Gerhard, Ortwin; Gibson, Brad K.; Gizon, Laurent; Haywood, M.; Handberg, R.; Heiter, U.; Hekker, S.; Huber, Daniel; Ibata, Rodrigo; Katz, David; Kawaler, S. D.; Kjeldsen, H.; Kurtz, D. W.; Lagarde, N.; Lebreton, Y.; Lund, Mikkel N.; Majewski, Steven R.; Marigo, Paola; Martig, Marie; Mathur, S.; Minchev, Ivan; Morel, Thierry; Ortolani, S.; Pinsonneault, Marc H.; Plez, B.; Moroni, P. G. Prada; Pricopi, D.; Recio–Blanco, A.; Reylé, C.; Robin, A. C.; Roxburgh, I. W.; Salaris, Maurizio; Santiago, B.; Schiavon, Ricardo P.; Serenelli, Aldo; Sharma, Sanjib; Aguirre, V. Silva; Soubiran, C.; Steinmetz, Matthias; Stello, Dennis; Strassmeier, K. G.; Ventura, P.; Ventura, R.; Walton, N. A.; Worley, C. C.

doi:10.1002/asna.201713385

Cited by 82 publications

(50 citation statements)

References 165 publications

(254 reference statements)

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“…(vii) Further investigations are needed to confirm with different techniques and with higher precision the age distribution of the stars in Enceladus. Asteroseismology techniques currently provide the best way to probe stellar interiors, to determine with very high accuracy stellar ages (Casagrande et al 2016;Silva Aguirre & Serenelli 2016;Miglio et al 2017). In the future, asteroseismology combined with chemodynamical simulations will allow us to study the mass assembly history of our Galaxy with unprecedented temporal resolution, and this will be the subject of our future work.…”

Section: Discussionmentioning

confidence: 99%

The Fall of a Giant. Chemical evolution of Enceladus, alias the Gaia Sausage

Vincenzo

Spitoni

Calura

et al. 2019

Monthly Notices of the Royal Astronomical Society: Letters

139

108

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We present the first chemical evolution model for Enceladus, alias the Gaia Sausage, to investigate the star formation history of one of the most massive satellites accreted by the Milky Way during a major merger event. Our best chemical evolution model for Enceladus nicely fits the observed stellar [α/Fe]-[Fe/H] chemical abundance trends, and reproduces the observed stellar metallicity distribution function, by assuming low star formation efficiency, fast infall time scale, and mild outflow intensity. We predict a median age for Enceladus stars 12.33 +0.92 −1.36 Gyr, and -at the time of the merger with our Galaxy (≈ 10 Gyr ago from Helmi et al.) -we predict for Enceladus a total stellar mass M ≈ 5 × 10 9 M . By looking at the predictions of our best model, we discuss that merger events between the Galaxy and systems like Enceladus may have inhibited the gas accretion onto the Galaxy disc at high redshifts, heating up the gas in the halo. This scenario could explain the extended period of quenching in the star formation activity of our Galaxy about 10 Gyr ago, which is predicted by Milky Way chemical evolution models, in order to reproduce the observed bimodality in [α/Fe]-[Fe/H] between thick-and thin-disc stars.

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Section: Discussionmentioning

confidence: 99%

The Fall of a Giant. Chemical evolution of Enceladus, alias the Gaia Sausage

Vincenzo

Spitoni

Calura

et al. 2019

Monthly Notices of the Royal Astronomical Society: Letters

139

108

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“…Having in mind that only 30% of bright (V < 8 mag) FGK main sequence stars have spectroscopic determinations of atmospheric parameters, we emphasize the importance of high-resolution spectral analysis of bright stars, especially for the 'hot'-regions of the sky such as the TESS continuous viewing zones (Sharma et al 2017), Kepler and K2 fields (Molenda-Żakowicz et al 2017;Niemczura et al 2017;Petigura et al 2017), and the PLATO fields (Miglio et al 2017).…”

Section: Discussionmentioning

confidence: 99%

Spectroscopy of Dwarf Stars Around the North Celestial Pole

Mikolaitis¹,

Tautvaišienė²,

Drazdauskas³

et al. 2018

PASP

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New space missions (e.g. NASA-TESS and ESA-PLATO) will perform an in-depth analysis of bright stars in large fields of the celestial sphere searching for extraterrestrial planets and investigating their host-stars. Asteroseismic observations will search for exoplanet-hosting stars with solar-like oscillations. In order to achieve all the goals, a full characterization of the stellar objects is important. However, accurate atmospheric parameters are available for less than 30% of bright dwarf stars of the Solar neighborhood. In this study we observed high-resolution (R=60000) spectra for all bright (V < 8 mag) and cooler than F5 spectral class dwarf stars in the northern-most field of the celestial sphere with radius of 20 degrees from the α(2000) = 161.03 • and δ(2000) = 86.60 • that is a centre of one of the preliminary ESO-PLATO fields. Spectroscopic atmospheric parameters were determined for 140 slowly rotating stars, for 73% of them for the first time. The majority (83%) of the investigated stars are in the TESS object lists and all of them are in the preliminary PLATO field. Our results have no systematic differences when compared with other recent studies. We have 119 stars in common with the Geneva-Copenhagen Survey, where stellar parameters were determined photometrically, and find a 14 ± 125 K difference in effective temperatures, 0.01 ± 0.16 in log g, and −0.02 ± 0.09 dex in metallicities. Comparing our results for 39 stars with previous high-resolution spectral determinations, we find only a 7 ± 73 K difference in effective temperatures, 0.02 ± 0.09 in log g, and −0.02 ± 0.09 dex in metallicities. We also determined basic kinematic and orbital parameters for this sample of stars. From the kinematical point of view, almost all our stars belong to the thin disk substructure of the Milky Way. The derived galactocentric metallicity gradient is −0.066 ± 0.024 dex kpc −1 (2.5 σ significance) and the vertical metallicity gradient is −0.102 ± 0.099 dex kpc −1 (1σ significance) that comply with the latest inside-out thin disk formation models, including those with stellar migration taken into account.

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“…The success of the CoRoT 1 and Kepler space-borne missions has opened a new era for stellar physics (e.g., Michel et al 2008;Appourchaux et al 2008;Chaplin et al 2011c). Asteroseismology provides unique information on the stars, which is crucial for probing stellar structure and stellar evolution, but also for assessing the physical properties of exoplanets (e.g., Lebreton & Goupil 2014) and for Galactic archaeology (e.g., Miglio et al 2009Miglio et al , 2013Rodrigues et al 2014;Anders et al 2017b,a;Miglio et al 2017). This success is partly based on the seismic scaling relations that provide relevant estimates of the stellar masses and radii.…”

Section: Introductionmentioning

confidence: 99%

Seismic performance

Mosser

Michel

Samadi

et al. 2019

A&A

Self Cite

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Context. Asteroseismology is a unique tool that can be used to study the interior of stars and hence deliver unique information for the studiy of stellar physics, stellar evolution, and Galactic archaeology. Aims. We aim to develop a simple model of the information content of asteroseismology and to characterize the ability and precision with which fundamental properties of stars can be estimated for different space missions. Methods. We defined and calibrated metrics of the seismic performance. The metrics, expressed by a seismic index E defined by simple scaling relations, are calculated for an ensemble of stars. We studied the relations between the properties of mission observations, fundamental stellar properties, and the performance index. We also defined thresholds for asteroseismic detection and measurement of different stellar properties Results. We find two regimes of asteroseismic performance: the first where the signal strength is dominated by stellar properties and not by observational noise; and the second where observational properties dominate. Typically, for evolved stars, stellar properties provide the dominant terms in estimating the information content, while main sequence stars fall in the regime where the observational properties, especially stellar magnitude, dominate. We estimate scaling relations to predict E with an intrinsic scatter of around 21%. Incidentally, the metrics allow us to distinguish stars burning either hydrogen or helium. Conclusions. Our predictions will help identify the nature of the cohort of existing and future asteroseismic observations. In addition, the predicted performance for PLATO will help define optimal observing strategies for defined scientific goals.

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PLATO as it is: A legacy mission for Galactic archaeology

Cited by 82 publications

References 165 publications

The Fall of a Giant. Chemical evolution of Enceladus, alias the Gaia Sausage

The Fall of a Giant. Chemical evolution of Enceladus, alias the Gaia Sausage

Spectroscopy of Dwarf Stars Around the North Celestial Pole

Seismic performance

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