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132 results on '"van Saders, Jennifer"'

103. Prospects for Galactic and stellar astrophysics with asteroseismology of giant stars in the TESS continuous viewing zones and beyond

Author

Mackereth, J Ted, primary, Miglio, Andrea, additional, Elsworth, Yvonne, additional, Mosser, Benoit, additional, Mathur, Savita, additional, Garcia, Rafael A, additional, Nardiello, Domenico, additional, Hall, Oliver J, additional, Vrard, Mathieu, additional, Ball, Warrick H, additional, Basu, Sarbani, additional, Beaton, Rachael L, additional, Beck, Paul G, additional, Bergemann, Maria, additional, Bossini, Diego, additional, Casagrande, Luca, additional, Campante, Tiago L, additional, Chaplin, William J, additional, Chiappini, Cristina, additional, Girardi, Léo, additional, Jørgensen, Andreas Christ Sølvsten, additional, Khan, Saniya, additional, Montalbán, Josefina, additional, Nielsen, Martin B, additional, Pinsonneault, Marc H, additional, Rodrigues, Thaíse S, additional, Serenelli, Aldo, additional, Silva Aguirre, Victor, additional, Stello, Dennis, additional, Tayar, Jamie, additional, Teske, Johanna, additional, van Saders, Jennifer L, additional, and Willett, Emma, additional

Published
2021
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104. Stellar Rotation in Kepler: Forward Modeling of the Kepler Period Distribution

Author

van Saders Jennifer L., Pinsonneault Marc H., García Rafael A., and Ceillier Tugdual

Subjects
Physics, QC1-999
Abstract

The Kepler mission has made it possible to detect the signatures of surface rotation in tens of thousands of stars across many different spectral types, ages, and evolutionary states. While it is tempting to use these rotation rates as a means to determine the ages of field stars in Kepler via the gyrochronology relationships, we show that 1) only a fraction of these stars should be viable targets for the existing period-age relationships due to “contamination” from hot stars and subgiants, and 2) that apparent age trends in the rotation distributions can be explained with an activity-based detection bias. We have performed a forward modeling exercise in an effort to reproduce the observed distribution of rotation periods.

Published
2015
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105. The Evolution of Rotation and Magnetic Activity in 94 Aqr Aa from Asteroseismology with TESS

Author

Metcalfe, Travis S., primary, van Saders, Jennifer L., additional, Basu, Sarbani, additional, Buzasi, Derek, additional, Chaplin, William J., additional, Egeland, Ricky, additional, Garcia, Rafael A., additional, Gaulme, Patrick, additional, Huber, Daniel, additional, Reinhold, Timo, additional, Schunker, Hannah, additional, Stassun, Keivan G., additional, Appourchaux, Thierry, additional, Ball, Warrick H., additional, Bedding, Timothy R., additional, Deheuvels, Sébastien, additional, González-Cuesta, Lucía, additional, Handberg, Rasmus, additional, Jiménez, Antonio, additional, Kjeldsen, Hans, additional, Li, Tanda, additional, Lund, Mikkel N., additional, Mathur, Savita, additional, Mosser, Benoit, additional, Nielsen, Martin B., additional, Noll, Anthony, additional, Çelik Orhan, Zeynep, additional, Örtel, Sibel, additional, Santos, Ângela R. G., additional, Yildiz, Mutlu, additional, Baliunas, Sallie, additional, and Soon, Willie, additional

Published
2020
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107. Exploring the Evolution of Stellar Rotation Using Galactic Kinematics

Author

Angus, Ruth, primary, Beane, Angus, additional, Price-Whelan, Adrian M., additional, Newton, Elisabeth, additional, Curtis, Jason L., additional, Berger, Travis, additional, van Saders, Jennifer, additional, Kiman, Rocio, additional, Foreman-Mackey, Daniel, additional, Lu, Yuxi (Lucy), additional, Anderson, Lauren, additional, and Faherty, Jacqueline K., additional

Published
2020
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110. Largest M Dwarf Flares from ASAS-SN

Author

Schmidt, Sarah J., Shappee, Benjamin J., van Saders, Jennifer L., Stanek, K. Z., Brown, Jonathan S., Kochanek, C. S., Dong, Subo, Drout, Maria R., Frank, Stephan, Holoien, T. W.-S., Johnson, Sean, Madore, Barry F., Prieto, J. L., Seibert, Mark, Seidel, Marja K., and Simonian, Gregory V. A.

Abstract

The All-sky Automated Survey for Supernovae (ASAS-SN) is the only project in existence to scan the entire sky in optical light approximately every day, reaching a depth of g ~ 18 mag. Over the course of its first 4 yr of transient alerts (2013–2016), ASAS-SN observed 53 events classified as likely M dwarf flares. We present follow-up photometry and spectroscopy of all 53 candidates, confirming flare events on 47 M dwarfs, one K dwarf, and one L dwarf. The remaining four objects include a previously identified T Tauri star, a young star with outbursts, and two objects too faint to confirm. A detailed examination of the 49 flare star light curves revealed an additional six flares on five stars, resulting in a total of 55 flares on 49 objects ranging in V-band contrast from ΔV = −1 to −10.2 mag. Using an empirical flare model to estimate the unobserved portions of the flare light curve, we obtain lower limits on the V-band energy emitted during each flare, spanning log(E_V/erg) = 32–35, which are among the most energetic flares detected on M dwarfs. The ASAS-SN M dwarf flare stars show a higher fraction of Hα emission, as well as stronger Hα emission, compared to M dwarfs selected without reference to activity, consistent with belonging to a population of more magnetically active stars. We also examined the distribution of tangential velocities, finding that the ASAS-SN flaring M dwarfs are likely to be members of the thin disk and are neither particularly young nor old.

Published
2019

111. Surface rotation of Kepler solar-type stars

Author

Santos, Ângela R. G., García, Rafael A., Mathur, Savita, Metcalfe, Travis S., Simonian, Gregory V., Pinsonneault, Marc H., van Saders, Jennifer L., and Scott Wolk

Subjects
starspots, techniques: photometric, stars: rotation, stars: activity, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Earth and Planetary Astrophysics, methods: data analysis, Astrophysics::Galaxy Astrophysics
Abstract

Dark spots crossing the stellar disk lead to periodic modulations in stellar light-curves that encode information on surface rotation and magnetic activity. Here, we analyze Kepler long-cadence data (four different time-series) for ~50,000 solar-type main-sequence and subgiant stars cooler than 5500 K and with surface gravity log g larger than 3.5 dex. Surface rotation period estimates are obtained through the implementation of a method which combines a wavelet analysis with the autocorrelation of the light-curve. We obtain reliable rotation periods for 23,494 stars. Only 16,600 of these are common to McQuillan (2013, 2014), with an agreement of ~99% within 2sigma. We also take special care to identify and remove possible polluters, such as classical pulsators, misclassified Red Giants, photometric pollution and other instrumental issues in light-curves., {"references":["Aigrain, S., Llama, J., Ceillier, T., et al. 2015, MNRAS, 450, 3211","Barnes, S. A. 2007, ApJ, 669, 1167","Berger, T. A., Huber, D., Gaidos, E., & van Saders, J. L. 2018, ApJ, 866, 99","Borucki, W. J., Koch, D., Basri, G., et al. 2010, Science, 327, 977","Brun, A. S. & Browning, M. K. 2017, Living Rev. Solar Phys., 14, 4","Ceillier, T., Tayar, J., Mathur, S., et al. 2017, A&A, 605, A111","Ceillier, T., van Saders, J., García, R. A., et al. 2016, MNRAS, 456, 119","García, R. A., Ceillier, T., Salabert, D., et al. 2014a, A&A, 572, A34","García, R. A., Hekker, S., Stello, D., et al. 2011, MNRAS, 414, L6","García, R. A., Mathur, S., Pires, S., et al. 2014b, A&A, 568, A10","Jenkins, J. M., Caldwell, D. A., Chandrasekaran, H., et al. 2010, ApJL, 713, L87","Mathur, S., García, R. A., Ballot, J., et al. 2014, A&A, 562, A124","Mathur, S., García, R. A., Régulo, C., et al. 2010, A&A, 511, A46","Mathur, S., Huber, D., Batalha, N. M., et al. 2017, ApJS, 229, 30","McQuillan, A., Aigrain, S., & Mazeh, T. 2013a, MNRAS, 432, 1203","McQuillan, A., Mazeh, T., & Aigrain, S. 2013b, ApJ, 775, L11","McQuillan, A., Mazeh, T., & Aigrain, S. 2014, ApJS, 211, 24","Nielsen, M. B., Gizon, L., Schunker, H., & Karoff, C. 2013, A&A, 557, L10","Pires, S., Mathur, S., García, R. A., et al. 2015, A&A, 574, A18","Reinhold, T., Reiners, A., & Basri, G. 2013, A&A, 560, A4","Simonian, G. V. A., Pinsonneault, M. H., & Terndrup, D. M. 2018, arXiv:1809.02141","Skumanich, A. 1972, ApJ, 171, 565","Torrence, C. & Compo, G. P. 1998, Bull. Amer. Meteor. Soc., 79, 61","Wilson, O. C. 1963, ApJ, 138, 832","Wilson, O. C. & Skumanich, A. 1964, ApJ, 140, 1401"]}

Published
2018
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112. Precise Properties Of Kepler Stars And Planets In The Gaia Era

Author

Berger, Travis, Huber, Daniel, Gaidos, Eric, van Saders, Jennifer, and Wolk, Scott

Subjects
techniques: photometric, Astrophysics::Instrumentation and Methods for Astrophysics, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Earth and Planetary Astrophysics, stars: fundamental parameters, planetary systems, Astrophysics::Galaxy Astrophysics, catalogs
Abstract

A major bottleneck for the exploitation of data from the Kepler mission for stellar astrophysics and exoplanet research has been the lack of precise radii and evolutionary states for most of the observed stars. We present revised radii of ~180,000 Kepler stars derived by combining parallaxes from the Gaia Data Release 2 with the DR25 Kepler Stellar Properties Catalog. The median radius precision is ≈8%, a typical improvement by a factor of 4–5 over previous estimates for typical Kepler stars. We find that ≈67% of all Kepler targets are main-sequence stars, ≈21% are subgiants, and ≈12% are red giants, demonstrating that subgiant contamination is less severe than some previous estimates and that Kepler targets are mostly main-sequence stars. Using the revised stellar radii, we recalculate the radii for > 4000 exoplanets. We confirm the presence of a gap in the radius distribution of small, close-in planets, and its location may be at a slightly larger radius when compared to previous results. Furthermore, we find several confirmed exoplanets occupying a previously described “hot super-Earth desert” at high irradiance, show the relation between a gas-giant planet’s radius and its incident flux, and establish a bona fide sample of 38 planets smaller than two earth radii in circumstellar habitable zones.The results presented here demonstrate the potential for transformative characterization of stellar and exoplanet populations using Gaia data.

Published
2018
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114. A Hot Saturn Orbiting an Oscillating Late Subgiant Discovered byTESS

Author

Huber, Daniel, primary, Chaplin, William J., additional, Chontos, Ashley, additional, Kjeldsen, Hans, additional, Christensen-Dalsgaard, Jørgen, additional, Bedding, Timothy R., additional, Ball, Warrick, additional, Brahm, Rafael, additional, Espinoza, Nestor, additional, Henning, Thomas, additional, Jordán, Andrés, additional, Sarkis, Paula, additional, Knudstrup, Emil, additional, Albrecht, Simon, additional, Grundahl, Frank, additional, Andersen, Mads Fredslund, additional, Pallé, Pere L., additional, Crossfield, Ian, additional, Fulton, Benjamin, additional, Howard, Andrew W., additional, Isaacson, Howard T., additional, Weiss, Lauren M., additional, Handberg, Rasmus, additional, Lund, Mikkel N., additional, Serenelli, Aldo M., additional, Rørsted Mosumgaard, Jakob, additional, Stokholm, Amalie, additional, Bieryla, Allyson, additional, Buchhave, Lars A., additional, Latham, David W., additional, Quinn, Samuel N., additional, Gaidos, Eric, additional, Hirano, Teruyuki, additional, Ricker, George R., additional, Vanderspek, Roland K., additional, Seager, Sara, additional, Jenkins, Jon M., additional, Winn, Joshua N., additional, Antia, H. M., additional, Appourchaux, Thierry, additional, Basu, Sarbani, additional, Bell, Keaton J., additional, Benomar, Othman, additional, Bonanno, Alfio, additional, Buzasi, Derek L., additional, Campante, Tiago L., additional, Çelik Orhan, Z., additional, Corsaro, Enrico, additional, Cunha, Margarida S., additional, Davies, Guy R., additional, Deheuvels, Sebastien, additional, Grunblatt, Samuel K., additional, Hasanzadeh, Amir, additional, Di Mauro, Maria Pia, additional, A. García, Rafael, additional, Gaulme, Patrick, additional, Girardi, Léo, additional, Guzik, Joyce A., additional, Hon, Marc, additional, Jiang, Chen, additional, Kallinger, Thomas, additional, Kawaler, Steven D., additional, Kuszlewicz, James S., additional, Lebreton, Yveline, additional, Li, Tanda, additional, Lucas, Miles, additional, Lundkvist, Mia S., additional, Mann, Andrew W., additional, Mathis, Stéphane, additional, Mathur, Savita, additional, Mazumdar, Anwesh, additional, Metcalfe, Travis S., additional, Miglio, Andrea, additional, F. G. Monteiro, Mário J. P., additional, Mosser, Benoit, additional, Noll, Anthony, additional, Nsamba, Benard, additional, Joel Ong, Jia Mian, additional, Örtel, S., additional, Pereira, Filipe, additional, Ranadive, Pritesh, additional, Régulo, Clara, additional, Rodrigues, Thaíse S., additional, Roxburgh, Ian W., additional, Aguirre, Victor Silva, additional, Smalley, Barry, additional, Schofield, Mathew, additional, Sousa, Sérgio G., additional, Stassun, Keivan G., additional, Stello, Dennis, additional, Tayar, Jamie, additional, White, Timothy R., additional, Verma, Kuldeep, additional, Vrard, Mathieu, additional, Yıldız, M., additional, Baker, David, additional, Bazot, Michaël, additional, Beichmann, Charles, additional, Bergmann, Christoph, additional, Bugnet, Lisa, additional, Cale, Bryson, additional, Carlino, Roberto, additional, Cartwright, Scott M., additional, Christiansen, Jessie L., additional, Ciardi, David R., additional, Creevey, Orlagh, additional, Dittmann, Jason A., additional, Nascimento, Jose-Dias Do, additional, Eylen, Vincent Van, additional, Fürész, Gabor, additional, Gagné, Jonathan, additional, Gao, Peter, additional, Gazeas, Kosmas, additional, Giddens, Frank, additional, Hall, Oliver J., additional, Hekker, Saskia, additional, Ireland, Michael J., additional, Latouf, Natasha, additional, LeBrun, Danny, additional, Levine, Alan M., additional, Matzko, William, additional, Natinsky, Eva, additional, Page, Emma, additional, Plavchan, Peter, additional, Mansouri-Samani, Masoud, additional, McCauliff, Sean, additional, Mullally, Susan E., additional, Orenstein, Brendan, additional, Soto, Aylin Garcia, additional, Paegert, Martin, additional, van Saders, Jennifer L., additional, Schnaible, Chloe, additional, Soderblom, David R., additional, Szabó, Róbert, additional, Tanner, Angelle, additional, Tinney, C. G., additional, Teske, Johanna, additional, Thomas, Alexandra, additional, Trampedach, Regner, additional, Wright, Duncan, additional, Yuan, Thomas T., additional, and Zohrabi, Farzaneh, additional

Published
2019
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115. The Largest M Dwarf Flares from ASAS-SN

Author

Schmidt, Sarah J., primary, Shappee, Benjamin J., additional, van Saders, Jennifer L., additional, Stanek, K. Z., additional, Brown, Jonathan S., additional, Kochanek, C. S., additional, Dong, Subo, additional, Drout, Maria R., additional, Frank, Stephan, additional, Holoien, T. W.-S., additional, Johnson, Sean, additional, Madore, Barry F., additional, Prieto, J. L., additional, Seibert, Mark, additional, Seidel, Marja K., additional, and Simonian, Gregory V. A., additional

Published
2019
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121. Star Clocks.

Author

van Saders, Jennifer

Subjects
*SOLAR magnetic fields, *OPEN clusters of stars, *STELLAR magnetic fields, *MAIN sequence (Astronomy), *AGE of stars
Published
2020

125. KELT-1b: A STRONGLY IRRADIATED, HIGHLY INFLATED, SHORT PERIOD, 27 JUPITER-MASS COMPANION TRANSITING A MID-F STAR

Author

Siverd, Robert J., primary, Beatty, Thomas G., additional, Pepper, Joshua, additional, Eastman, Jason D., additional, Collins, Karen, additional, Bieryla, Allyson, additional, Latham, David W., additional, Buchhave, Lars A., additional, Jensen, Eric L. N., additional, Crepp, Justin R., additional, Street, Rachel, additional, Stassun, Keivan G., additional, Scott Gaudi, B., additional, Berlind, Perry, additional, Calkins, Michael L., additional, DePoy, D. L., additional, Esquerdo, Gilbert A., additional, Fulton, Benjamin J., additional, Fűrész, Gábor, additional, Geary, John C., additional, Gould, Andrew, additional, Hebb, Leslie, additional, Kielkopf, John F., additional, Marshall, Jennifer L., additional, Pogge, Richard, additional, Stanek, K. Z., additional, Stefanik, Robert P., additional, Szentgyorgyi, Andrew H., additional, Trueblood, Mark, additional, Trueblood, Patricia, additional, Stutz, Amelia M., additional, and van Saders, Jennifer L., additional

Published
2012
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130. Using Modern Stellar Observables to Constrain Stellar Parameters and the Physics of the Stellar Interior

Author

van Saders, Jennifer Lynn

Subjects
Astrophysics, Astronomy, stars, stellar evolution, stellar rotation, asteroseismology, stellar structure
Abstract

The current state and future evolution of a star is, in principle, specified by a only a few physical quantities: the mass, age, hydrogen, helium, and metal abundance. These same fundamental quantities are crucial for reconstructing the history of stellar systems ranging in scale from planetary systems to galaxies. However, the fundamental parameters are rarely directly observable, and we are forced to use proxies that are not always sensitive or unique functions of the stellar parameters we wish to determine. Imprecise or inaccurate determinations of the fundamental parameters often limit our ability to draw inferences about a given system. As new technologies, instruments, and observing techniques become available, the list of viable stellar observables increases, and we can explore new links between the observables and fundamental quantities in an effort to better characterize stellar systems. In the era of missions such as Kepler, time-domain observables such as the stellar rotation period and stellar oscillations are now available for an unprecedented number of stars, and future missions promise to further expand the sample. Furthermore, despite the successes of stellar evolution models, the processes and detailed structure of the deep stellar interior remains uncertain. Even in the case of well-measured, well understood stellar observables, the link to the underlying parameters contains uncertainties due to our imperfect understanding of stellar interiors. Model uncertainties arise from sources such as the treatment of turbulent convection, transport of angular momentum and mixing, and assumptions about the physical conditions of stellar matter. By carefully examining the sensitivity of stellar observables to physical processes operating within the star and model assumptions, we can design observational tests for the theory of stellar interiors. I propose a series of tools based on new or revisited stellar observables that can be used both to constrain stellar parameters and the physics of the interior. I examine how the acoustic signature of the location of the base of stellar convective envelopes can be used as an absolute abundance indicator, and describe a novel 3He-burning instability in low mass stars along with the observational signatures of such a process. Finally, I examine the manner in which stellar rotation, observed in a population of objects, can be used as a means to distinguish between different evolutionary states, masses, and ages. I emphasize that rotation periods can be used as age indicators (as often discussed in the literature), but that the interpretation of rotation periods must be made within the context of the full stellar population to arrive at accurate results.

Published
2014

132. Prospects for Galactic and stellar astrophysics with asteroseismology of giant stars in the TESS continuous viewing zones and beyond

Author

Jennifer L. van Saders, Léo Girardi, Johanna Teske, Emma Willett, Dennis Stello, Tiago L. Campante, M. Vrard, William J. Chaplin, Marc H. Pinsonneault, Savita Mathur, Andreas Christ Sølvsten Jørgensen, Paul G. Beck, Andrea Miglio, Martin Bo Nielsen, B. Mosser, Aldo Serenelli, Thaíse S. Rodrigues, Rafael A. García, Maria Bergemann, Josefina Montalbán, Jamie Tayar, Oliver J. Hall, Sarbani Basu, Luca Casagrande, Domenico Nardiello, Yvonne Elsworth, Rachael L. Beaton, Saniya Khan, Warrick H. Ball, Christina Chiappini, Victor Silva Aguirre, J. Ted Mackereth, Diego Bossini, Government of Canada, University of Toronto, Ministerio de Ciencia, Innovación y Universidades (España), European Commission, Australian Research Council, Generalitat de Catalunya, National Aeronautics and Space Administration (US), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Mackereth, Ted, Miglio, Andrea, Elsworth, Yvonne, Mosser, Benoit, Mathur, Savita, Garcia, Rafael A, Nardiello, Domenico, Hall, Oliver J, Vrard, Mathieu, Ball, Warrick H, Basu, Sarbani, Beaton, Rachael L, Beck, Paul G, Bergemann, Maria, Bossini, Diego, Casagrande, Luca, Campante, Tiago L, Chaplin, William J, Chiappini, Cristina, Girardi, Léo, Jørgensen, Andreas Christ Sølvsten, Khan, Saniya, Montalbán, Josefina, Nielsen, Martin B, Pinsonneault, Marc H, Rodrigues, Thaíse S, Serenelli, Aldo, Silva Aguirre, Victor, Stello, Denni, Tayar, Jamie, Teske, Johanna, van Saders, Jennifer L, and Willett, Emma

Subjects
Red giant, Star (game theory), Milky Way, oscillations [Stars], FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, Asteroseismology, fundamental parameters [Stars], 0103 physical sciences, Stars: oscillations, Astrophysics::Solar and Stellar Astrophysics, Asymptotic giant branch, stellar content [Galaxy], 010303 astronomy & astrophysics, Galaxy: structure, Astrophysics::Galaxy Astrophysics, Stars: fundamental parameters, Physics, Galaxy: stellar content, stars: oscillation, 010308 nuclear & particles physics, Star formation, Galaxy: fundamental parameter, fundamental parameters [Galaxy], Astronomy and Astrophysics, stars: fundamental parameter, Galaxy: fundamental parameters, kinematics and dynamics [Galaxy], Giant star, Astrophysics - Astrophysics of Galaxies, Stars, Space and Planetary Science, [SDU]Sciences of the Universe [physics], Astrophysics of Galaxies (astro-ph.GA), Galaxy: kinematics and dynamic, Astrophysics::Earth and Planetary Astrophysics, Galaxy: kinematics and dynamics, structure [Galaxy]
Abstract

Mackereth, J. Ted, et al., The NASA Transiting Exoplanet Survey Satellite (NASA-TESS) mission presents a treasure trove for understanding the stars it observes and the Milky Way, in which they reside. We present a first look at the prospects for Galactic and stellar astrophysics by performing initial asteroseismic analyses of bright (G < 11) red giant stars in the TESS southern continuous viewing zone (SCVZ). Using three independent pipelines, we detect νmax and Δν in 41 per cent of the 15 405 star parent sample (6388 stars), with consistency at a level of ∼2 per cent in νmax and ∼5 per cent in Δν. Based on this, we predict that seismology will be attainable for ∼3 × 105 giants across the whole sky and at least 104 giants with ≥1 yr of observations in the TESS-CVZs, subject to improvements in analysis and data reduction techniques. The best quality TESS-CVZ data, for 5574 stars where pipelines returned consistent results, provide high-quality power spectra across a number of stellar evolutionary states. This makes possible studies of, for example, the asymptotic giant branch bump. Furthermore, we demonstrate that mixed ℓ = 1 modes and rotational splitting are cleanly observed in the 1-yr data set. By combining TESS-CVZ data with TESS-HERMES, SkyMapper, APOGEE, and Gaia, we demonstrate its strong potential for Galactic archaeology studies, providing good age precision and accuracy that reproduces well the age of high [α/Fe] stars and relationships between mass and kinematics from previous studies based on e.g. Kepler. Better quality astrometry and simpler target selection than the Kepler sample makes this data ideal for studies of the local star formation history and evolution of the Galactic disc. These results provide a strong case for detailed spectroscopic follow-up in the CVZs to complement that which has been (or will be) collected by current surveys., JTM and AM acknowledge support from the ERC Consolidator Grant funding scheme (project ASTEROCHRONOMETRY, G.A. n. 772293). JTM acknowledges support from the Banting Postdoctoral Fellowship programme administered by the Government of Canada, and a CITA/Dunlap Institute fellowship. The Dunlap Institute is funded through an endowment established by the David Dunlap family and the University of Toronto. SM acknowledges support from the Spanish Ministry with the Ramon y Cajal fellowship number RYC-2015-17697. RAG acknowledges the support from the PLATO CNES grant. DB acknowledges supported by FCT through the research grants UIDB/04434/2020, UIDP/04434/2020, and PTDC/FIS-AST/30389/2017, and by FEDER – Fundo Europeu de Desenvolvimento Regional through COMPETE2020 – Programa Operacional Competitividade e Internacionalização (grant: POCI-01-0145-FEDER-030389). LC acknowledges support from the Australian Research Council grant FT160100402. TC acknowledges support from the European Union’s Horizon 2020 research and innovation programme under the Marie Skłodowska-Curie grant agreement no. 792848 (PULSATION). AS is partially supported by grants ESP2017-82674-R (Spanish Government) and 2017-SGR-1131 (Generalitat de Catalunya). MHP and MV acknowledge support from NASA grant 80NSSC18K1582.

Published
2021
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