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Sökning: WFRF:(Kovalev M.) > (2015-2019) > The Gaia-ESO Survey :

The Gaia-ESO Survey : Hydrogen lines in red giants directly trace stellar mass

Bergemann, Maria (författare)
Max Planck Inst Astron, D-69117 Heidelberg, Germany.,Max Planck Institute for Astronomy
Serenelli, Aldo (författare)
Campus UAB, ICE CSIC IEEC, Inst Ciencias Espacio, Carrer Can Magrans S-N, Bellaterra 08193, Spain.,Autonomous University of Barcelona
Schonrich, Ralph (författare)
Univ Oxford, Rudolf Peierls Ctr Theoret Phys, 1 Keble Rd, Oxford OX1 3NP, England.,University of Oxford
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Ruchti, Greg (författare)
Lund Observ, Box 43, S-22100 Lund, Sweden.
Korn, Andreas (författare)
Uppsala University,Uppsala universitet,Institutionen för fysik och astronomi,Uppsala Univ, Div Astron & Space Phys, Dept Phys & Astron, Angstrom Lab, Box 516, S-75120 Uppsala, Sweden.
Hekker, Saskia (författare)
Max Planck Inst Solar Syst Res, Justus von Liebig Weg 3, D-37077 Gttingen, Germany.,Max Planck Institute for Solar System Research,Aarhus University
Kovalev, Mikhail (författare)
Max Planck Inst Astron, D-69117 Heidelberg, Germany.,Max Planck Institute for Astronomy
Mashonkina, Lyudmila (författare)
P.N. Lebedev Physical Institute of the Russian Academy of Sciences
Gilmore, Gerry (författare)
Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England.,University of Cambridge
Randich, Sofia (författare)
INAF Osservatorio Astrofis Arcetri, Largo Fermi 5, I-50125 Florence, Italy.,INAF - Osservatorio Astrofisico di Arcetri
Asplund, Martin (författare)
Australian Natl Univ, Mt Stromlo Observ, Res Sch Astron & Astrophys, Weston, ACT 2611, Australia.,Australian National University
Rix, Hans-Walter (författare)
Max Planck Inst Astron, D-69117 Heidelberg, Germany.,Max Planck Institute for Astronomy
Casey, Andrew R. (författare)
Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England.,University of Cambridge
Jofre, Paula (författare)
Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England.,University of Cambridge
Pancino, Elena (författare)
INAF Osservatorio Astron, Via Ranzani 1, I-40127 Bologna, Italy.;ASI Sci Data Ctr, Via Politecn SNC, I-00133 Rome, Italy.,Italian Space Agency,INAF Osservatorio Astronomico di Bologna
Recio-Blanco, Alejandra (författare)
Univ Nice Sophia Antipolis, CNRS, Observ Cote Azur, Lab Lagrange, BP 4229, F-06304 Nice 4, France.,Université Nice Sophia Antipolis
de Laverny, Patrick (författare)
Univ Nice Sophia Antipolis, CNRS, Observ Cote Azur, Lab Lagrange, BP 4229, F-06304 Nice 4, France.,Université Nice Sophia Antipolis
Smiljanic, Rodolfo (författare)
Nicolaus Copernicus Astron Ctr, Dept Astrophys, Ul Rabianska 8, PL-87100 Torun, Poland. Aarhus Univ, Dept Phys & Astron, Stellar Astrophys Ctr, Ny Munckegade 120, DK-8000 Aarhus, Denmark.,Institute - Center for Molecular and Macromolecular Studies of the Polish Academy of Sciences
Tautvaisiene, Grazina (författare)
Vilnius Univ, Inst Theoret Phys & Astron, Gostauto 12, LT-01108 Vilnius, Lithuania.,Vilnius University
Bayo, Amelia (författare)
Inst Fis & Astron, Fac Ciencias, Gran Bretana 1111, Playa Ancha, Chile.,University of Valparaíso
Lewis, Jim (författare)
Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England.,University of Cambridge
Koposov, Sergey (författare)
Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England.,University of Cambridge
Hourihane, Anna (författare)
Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England.,University of Cambridge
Worley, Clare (författare)
Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England.,University of Cambridge
Morbidelli, Lorenzo (författare)
INAF Osservatorio Astrofis Arcetri, Largo Fermi 5, I-50125 Florence, Italy.,INAF - Osservatorio Astrofisico di Arcetri
Franciosini, Elena (författare)
INAF Osservatorio Astrofis Arcetri, Largo Fermi 5, I-50125 Florence, Italy.,INAF - Osservatorio Astrofisico di Arcetri
Sacco, Germano (författare)
INAF Osservatorio Astrofis Arcetri, Largo Fermi 5, I-50125 Florence, Italy.,INAF - Osservatorio Astrofisico di Arcetri
Magrini, Laura (författare)
INAF Osservatorio Astrofis Arcetri, Largo Fermi 5, I-50125 Florence, Italy.,INAF - Osservatorio Astrofisico di Arcetri
Damiani, Francesco (författare)
INAF Osservatorio Astron Palermo, Piazza Parlamento 1, I-90134 Palermo, Italy. Russian Acad Sci, Inst Astron, Pyatnitskaya St 48, Moscow 119017, Russia.,National Institute for Astrophysics
Bestenlehner, Joachim M. (författare)
Max Planck Institute for Astronomy
Ruchti, Gregory (författare)
Lund University,Lunds universitet,Astronomi - Genomgår omorganisation,Institutionen för astronomi och teoretisk fysik - Genomgår omorganisation,Naturvetenskapliga fakulteten,Lund Observatory - Undergoing reorganization,Department of Astronomy and Theoretical Physics - Undergoing reorganization,Faculty of Science
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Max Planck Inst Astron, D-69117 Heidelberg, Germany Max Planck Institute for Astronomy (creator_code:org_t)
2016-10-20
2016
Engelska.
Ingår i: Astronomy and Astrophysics. - : EDP Sciences. - 0004-6361 .- 1432-0746. ; 594
Relaterad länk:
https://www.aanda.or...
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http://dx.doi.org/10...
https://urn.kb.se/re...
https://doi.org/10.1...
https://lup.lub.lu.s...
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  • Tidskriftsartikel (refereegranskat)
Abstract Ämnesord
Stäng  
  • Red giant stars are perhaps the most important type of stars for Galactic and extra-galactic archaeology: they are luminous, occur in all stellar populations, and their surface temperatures allow precise abundance determinations for many different chemical elements. Yet, the full star formation and enrichment history of a galaxy can be traced directly only if two key observables can be determined for large stellar samples: age and chemical composition. While spectroscopy is a powerful method to analyse the detailed abundances of stars, stellar ages are the missing link in the chain, since they are not a direct observable. However, spectroscopy should be able to estimate stellar masses, which for red giants directly infer ages provided their chemical composition is known. Here we establish a new empirical relation between the shape of the hydrogen line in the observed spectra of red giants and stellar mass determined from asteroseismology. The relation allows determining stellar masses and ages with an accuracy of 10-15%. The method can be used with confidence for stars in the following range of stellar parameters: 4000 < T-eff < 5000 K, 0.5 < log g < 3.5, -2.0 < [ Fe/H] < 0.3, and luminosities log L/L-Sun < 2.5. Our analysis provides observational evidence that the H-alpha spectral characteristics of red giant stars are tightly correlated with their mass and therefore their age. We also show that the method samples well all stellar populations with ages above 1 Gyr. Targeting bright giants, the method allows obtaining simultaneous age and chemical abundance information far deeper than would be possible with asteroseismology, extending the possible survey volume to remote regions of the Milky Way and even to neighbouring galaxies such as Andromeda or the Magellanic Clouds even with current instrumentation, such as the VLT and Keck facilities.

Ämnesord

NATURVETENSKAP  -- Fysik -- Astronomi, astrofysik och kosmologi (hsv//swe)
NATURAL SCIENCES  -- Physical Sciences -- Astronomy, Astrophysics and Cosmology (hsv//eng)

Nyckelord

techniques: spectroscopic
stars: fundamental parameters
stars: late-type
Galaxy: stellar content
Galaxy: stellar content
Stars: fundamental parameters
Stars: late-type
Techniques: spectroscopic

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