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Sökning: WFRF:(Jönsson A C) > (2020-2024) > Oxygen, sulfur, and...

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FältnamnIndikatorerMetadata
00009902naa a2200673 4500
001oai:DiVA.org:mau-64218
003SwePub
008231211s2023 | |||||||||||000 ||eng|
0247 a https://urn.kb.se/resolve?urn=urn:nbn:se:mau:diva-642182 URI
0247 a https://doi.org/10.1051/0004-6361/2023469822 DOI
040 a (SwePub)mau
041 a engb eng
042 9 SwePub
072 7a ref2 swepub-contenttype
072 7a art2 swepub-publicationtype
1001 a da Silva, R.u Inaf -Osservatorio Astronomico di Roma, via Frascati 33, Monte Porzio Catone, 00078, Italy; Agenzia Spaziale Italiana, Space Science Data Center, via del Politecnico snc, Rome, 00133, Italy4 aut
2451 0a Oxygen, sulfur, and iron radial abundance gradients of classical Cepheids across the Galactic thin disk
264 1b EDP Sciences,c 2023
338 a electronic2 rdacarrier
520 a Context. Classical Cepheids (CCs) are solid distance indicators and tracers of young stellar populations. Dating back to the beginning of the 20th century, they have been safely adopted to trace the rotation, kinematics, and chemical enrichment history of the Galactic thin disk.Aims. The main aim of this investigation is to provide iron, oxygen, and sulfur abundances for the largest and most homogeneous sample of Galactic CCs analyzed so far (1118 spectra of 356 objects). The current sample, containing 70 CCs for which spectroscopic metal abundances are provided for the first time, covers a wide range in galactocentric distances, pulsation modes, and pulsation periods.Methods. Optical high-resolution spectra with a high signal-to-noise ratio that were collected with different spectrographs were adopted to provide homogeneous estimates of the atmospheric parameters (effective temperature, surface gravity, and microturbulent velocity) that are required to determine the abundance. Individual distances were based either on trigonometric parallaxes by the Gaia Data Release 3 (Gaia DR3) or on distances based on near-infrared period-luminosity relations.Results. We found that iron and α-element radial gradients based on CCs display a well-defined change in the slope for galactocentric distances larger than ~12 kpc. We also found that logarithmic regressions account for the variation in [X/H] abundances from the inner to the outer disk. Radial gradients for the same elements, but based on open clusters covering a wide range in cluster ages, display similar trends. This means that the flattening in the outer disk is an intrinsic feature of the radial gradients because it is independent of age. Empirical evidence indicates that the S radial gradient is steeper than the Fe radial gradient. The difference in the slope is a factor of two in the linear fit (−0.081 vs. −0.041 dex kpc−1) and changes from −1.62 to −0.91 in the logarithmic distance. Moreover, we found that S (explosive nucleosynthesis) is underabundant on average when compared with O (hydrostatic nucleosynthesis). The difference becomes clearer in the metal-poor regime and for the [O/Fe] and [S/Fe] abundance ratios. We performed a detailed comparison with Galactic chemical evolution models and found that a constant star formation efficiency for galactocentric distances larger than 12 kpc accounts for the flattening observed in both iron and α-elements. To further constrain the impact of the predicted S yields for massive stars on radial gradients, we adopted a toy model and found that the flattening in the outermost regions requires a decrease of a factor of four in the current S predictions.Conclusions. CCs are solid beacons for tracing the recent chemical enrichment of young stellar populations. Sulfur photospheric abundances, when compared with other α-elements, have the key advantage of being a volatile element. Therefore, stellar S abundances can be directly compared with nebular sulfur abundances in external galaxies.
650 7a NATURVETENSKAPx Fysikx Astronomi, astrofysik och kosmologi0 (SwePub)103052 hsv//swe
650 7a NATURAL SCIENCESx Physical Sciencesx Astronomy, Astrophysics and Cosmology0 (SwePub)103052 hsv//eng
653 a Galaxy: disk
653 a stars: abundances
653 a stars: fundamental parameters
653 a stars: variables: Cepheids
7001 a D’Orazi, V.u Department of Physics, University of Rome Tor Vergata, via della Ricerca Scientifica 1, Rome, 00133, Italy; Inaf -Osservatorio Astronomico di Padova, vicolo dell'Osservatorio 5, Padova, 35122, Italy4 aut
7001 a Palla, M.u Sterrenkundig Observatorium, Ghent University, Krijgslaan 281 - S9, Gent, 9000, Belgium; Inaf -Osservatorio Astronomico di Bologna, via Gobetti 93/3, Bologna, 40129, Italy4 aut
7001 a Bono, G.u Inaf -Osservatorio Astronomico di Roma, via Frascati 33, Monte Porzio Catone, 00078, Italy; Department of Physics, University of Rome Tor Vergata, via della Ricerca Scientifica 1, Rome, 00133, Italy4 aut
7001 a Braga, V. F.u Inaf -Osservatorio Astronomico di Roma, via Frascati 33, Monte Porzio Catone, 00078, Italy; Agenzia Spaziale Italiana, Space Science Data Center, via del Politecnico snc, Rome, 00133, Italy4 aut
7001 a Fabrizio, M.u Inaf -Osservatorio Astronomico di Roma, via Frascati 33, Monte Porzio Catone, 00078, Italy; Agenzia Spaziale Italiana, Space Science Data Center, via del Politecnico snc, Rome, 00133, Italy4 aut
7001 a Lemasle, B.u Astronomisches Rechen-Institut, Zah, Universität Heidelberg, Mönchhofstr. 12-14, Heidelberg, 69120, Germany4 aut
7001 a Spitoni, E.u Inaf, Osservatorio Astronomico di Trieste, via G. B. Tiepolo 11, Trieste, 34131, Italy4 aut
7001 a Matteucci, F.u Inaf, Osservatorio Astronomico di Trieste, via G. B. Tiepolo 11, Trieste, 34131, Italy; Dipartimento di Fisica, Sezione di Astronomia, Università Degli Studi di Trieste, via G. B. Tiepolo 11, Trieste, 34131, Italy; Infn, Sezione di Trieste, via A. Valerio 2, Trieste, 34100, Italy4 aut
7001 a Jönsson, H.u Malmö universitet,Institutionen för materialvetenskap och tillämpad matematik (MTM)4 aut0 (Swepub:mau)ak0675
7001 a Kovtyukh, V.u Astronomical Observatory, Odessa National University, Shevchenko Park, Odessa, 65014, Ukraine4 aut
7001 a Magrini, L.u Inaf -Osservatorio Astrofisico di Arcetri, Largo E. Fermi 5, Firenze, Italy4 aut
7001 a Bergemann, M.u Max Planck Institute for Astronomy, Heidelberg, 69117, Germany; Niels Bohr International Academy, Niels Bohr Institute, Blegdamsvej 17, Copenhagen, 2100, Denmark4 aut
7001 a Dall’Ora, M.u Inaf -Osservatorio Astronomico di Capodimonte, Salita Moiariello 16, Napoli, 80131, Italy4 aut
7001 a Ferraro, I.u Inaf -Osservatorio Astronomico di Roma, via Frascati 33, Monte Porzio Catone, 00078, Italy4 aut
7001 a Fiorentino, G.u Inaf -Osservatorio Astronomico di Roma, via Frascati 33, Monte Porzio Catone, 00078, Italy4 aut
7001 a François, P.u Gepi, Observatoire de Paris, Psl Research University, Cnrs, 61 avenue de l'Observatoire, Paris, 75014, France; Upjv, Université de Picardie Jules Verne, 33 rue St Leu, Amiens, 80080, France4 aut
7001 a Iannicola, G.u Inaf -Osservatorio Astronomico di Roma, via Frascati 33, Monte Porzio Catone, 00078, Italy4 aut
7001 a Inno, L.u Science and Technology Department, Parthenope University of Naples, Naples, Italy4 aut
7001 a Kudritzki, R.-P.u Lmu München, Universitätssternwarte, Scheinerstr. 1, München, 81679, Germany; Institute for Astronomy, University of Hawaii at Manoa, 2680 Woodlawn Drive, Honolulu, 96822, HI, United States4 aut
7001 a Matsunaga, N.u Department of Astronomy, School of Science, The University of Tokyo, 7-3-1, Hongo, Bunkyo-ku, Tokyo, 113-0033, Japan; Laboratory of Infrared High-Resolution Spectroscopy (LiH), Koyama Astronomical Observatory, Kyoto Sangyo University, Motoyama, Kamigamo, Kita-ku, Kyoto, 603-8555, Japan4 aut
7001 a Monelli, M.u Inaf -Osservatorio Astronomico di Roma, via Frascati 33, Monte Porzio Catone, 00078, Italy; Instituto de Astrofísica de Canarias (IAC), C. Vía Láctea s/n, La Laguna, 38205, Spain; Departamento de Astrofísica, Universidad de la Laguna (ULL), Laguna, 38200 La, Spain4 aut
7001 a Nonino, M.u Inaf, Osservatorio Astronomico di Trieste, via G. B. Tiepolo 11, Trieste, 34131, Italy4 aut
7001 a Sneden, C.u Department of Astronomy and McDonald Observatory, The University of Texas, Austin, 78712, TX, United States4 aut
7001 a Storm, J.u Leibniz-Institut für Astrophysik Potsdam (AIP), An der Sternwarte 16, Potsdam, 14482, Germany4 aut
7001 a Thévénin, F.u Université Côte d'Azur, Observatoire de la Côte d'Azur, Cnrs, Lagrange Umr 7293, Cs 34229 Cedex, Nice, 06304-4, France4 aut
7001 a Tsujimoto, T.u National Astronomical Observatory of Japan, Mitaka, Tokyo, 1818588, Japan4 aut
7001 a Zocchi, A.u Department of Astrophysics, University of Vienna, Türkenschanzstraße 17, Vienna, 1180, Austria4 aut
7102 a Inaf -Osservatorio Astronomico di Roma, via Frascati 33, Monte Porzio Catone, 00078, Italy; Agenzia Spaziale Italiana, Space Science Data Center, via del Politecnico snc, Rome, 00133, Italyb Department of Physics, University of Rome Tor Vergata, via della Ricerca Scientifica 1, Rome, 00133, Italy; Inaf -Osservatorio Astronomico di Padova, vicolo dell'Osservatorio 5, Padova, 35122, Italy4 org
7730 t Astronomy and Astrophysicsd : EDP Sciencesg 678, s. A195-A195q 678<A195-A195x 0004-6361x 1432-0746
8564 u https://doi.org/10.1051/0004-6361/202346982y Fulltext
8564 u https://mau.diva-portal.org/smash/get/diva2:1818519/FULLTEXT01.pdfx primaryx Raw objecty fulltext:print
8564 8u https://urn.kb.se/resolve?urn=urn:nbn:se:mau:diva-64218
8564 8u https://doi.org/10.1051/0004-6361/202346982

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