The open cluster King 1 in the second quadrant

Carrera, R.; Espinosa, Loreto Rodríguez; Casamiquela, L.; Nunez, L. Balaguer; Jordi, C.; Prieto, C. Allende; Stetson, P. B.

doi:10.1093/mnras/stx1526

Cited by 10 publications

(7 citation statements)

References 48 publications

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“…For its super-solar metallicity of [Fe/H] = +0.3, a younger age of 2.8 Gyr and a larger absorption of 2 mag present a better fit. This age is in good agreement with previous dedicated studies of this cluster (2.8 ± 0.3 Gyr Carrera et al 2017).…”

Section: Agessupporting

confidence: 93%

Abundance–age relations with red clump stars in open clusters

Casamiquela

Soubiran

Jofré

et al. 2021

A&A

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Context. Precise chemical abundances coupled with reliable ages are key ingredients to understanding the chemical history of our Galaxy. Open clusters (OCs) are useful for this purpose because they provide ages with good precision. Aims. The aim of this work is to investigate the relation between different chemical abundance ratios and age traced by red clump (RC) stars in OCs. Methods. We analyzed a large sample of 209 reliable members in 47 OCs with available high-resolution spectroscopy. We applied a differential line-by-line analysis, performing a comprehensive chemical study of 25 chemical species. This sample is among the largest samples of OCs homogeneously characterized in terms of atmospheric parameters, detailed chemistry, and age. Results. In our metallicity range (−0.2 < [M/H] < +0.2) we find that while most Fe-peak and α elements show a flat dependence on age, the s-process elements show a decreasing trend with increasing age with a remarkable knee at 1 Gyr. For Ba, Ce, Y, Mo, and Zr, we find a plateau at young ages (< 1 Gyr). We investigate the relations between all possible combinations among the computed chemical species and age. We find 19 combinations with significant slopes, including [Y/Mg] and [Y/Al]. The ratio [Ba/α] shows the most significant correlation. Conclusions. We find that the [Y/Mg] relation found in the literature using solar twins is compatible with the one found here in the solar neighborhood. The age–abundance relations in clusters at large distances(d > 1 kpc) show larger scatter than those in clusters in the solar neighborhood, particularly in the outer disk. We conclude that, in addition to pure nucleosynthetic arguments, the complexity of the chemical space introduced by the Galactic dynamics must be taken into account in order to understand these relations, especially outside of the local bubble.

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Section: Agessupporting

confidence: 93%

Abundance–age relations with red clump stars in open clusters

Casamiquela

Soubiran

Jofré

et al. 2021

A&A

Self Cite

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show abstract

“…For its super-solar metallicity of [Fe/H] = +0.3, a younger age of 2.8 Gyr and a larger absorption of 2 mag present a better fit. This age has a good agreement with previous dedicated studies of this cluster (2.8 ± 0.3 Gyr Carrera et al 2017). -NGC 6791: CG20 quotes an age of 6.76 Gyr and A V = 0.67 mag.…”

Section: Agessupporting

confidence: 92%

Abundance-age relations with red clump stars in open clusters

Casamiquela,

Soubiran,

Jofré

et al. 2021

Preprint

View full text Add to dashboard Cite

Context. Precise chemical abundances coupled with reliable ages are key ingredients to understand the chemical history of our Galaxy. Open Clusters (OCs) are useful for this purpose because they provide ages with good precision. Aims. The aim of this work is to investigate the relations of different chemical abundance ratios vs age traced by red clump (RC) stars in OCs. Methods. We analyze a large sample of 209 reliable members in 47 OCs with available high-resolution spectroscopy. We applied a differential line-by-line analysis to provide a comprehensive chemical study of 25 chemical species. This sample is among the largest samples of OCs homogeneously characterized in terms of atmospheric parameters, detailed chemistry, and ages. Results. In our metallicity range (−0.2 < [M/H] < +0.2) we find that while most Fe-peak and α elements have flat dependence with age, the s-process elements show decreasing trends with increasing age with a remarkable knee at 1 Gyr. For Ba, Ce, Y, Mo and Zr we find a plateau at young ages (< 1 Gyr). We investigate the relations of all possible combinations among the computed chemical species with age. We find 19 combinations with significant slopes, including [Y/Mg] and [Y/Al]. The ratio [Ba/α] is the one with the most significant correlations found. Conclusions. We find that the [Y/Mg] relation found in the literature using Solar twins is compatible with the one found here in the Solar neighbourhood. The age-abundance relations show larger scatter for clusters at large distances (d > 1 kpc) than for the Solar neighbourhood, particularly in the outer disk. We conclude that these relations need to be understood also in terms of the complexity of the chemical space introduced by the Galactic dynamics, on top of pure nucleosynthetic arguments, especially out of the local bubble.

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“…In all the models, the height above the plane and the dispersion of the eccentricity increases in accordance with age. The sky emissions, both continuum and lines, were removed following the procedure described by Carrera et al (2017). For each order, the sky and object spectra are separated into two components: continuum and lines.…”

Section: Discussionmentioning

confidence: 99%

Occaso

Carrera

Casamiquela

Carbajo-Hijarrubia

et al. 2022

A&A

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Context. Open clusters (OCs) are widely used as test particles to investigate a variety of astrophysical phenomena, from stellar evolution to Galactic evolution. Gaia and the complementary massive spectroscopic surveys are providing an unprecedented wealth of information about these systems. Aims. The Open Cluster Chemical Abundances from Spanish Observatories (OCCASO) survey aims to complement all this work by determining OCs' accurate radial velocities and chemical abundances from high-resolution, R≥60 000, spectra. Methods. Radial velocities were obtained by cross-correlating the observed spectra with a library of synthetic spectra that covers early M to A spectral types. Results. We provide radial velocities for 336 stars including several Gaia benchmark stars and objects belonging to 51 open clusters. The internal uncertainties of the derived radial velocities go from 10 m s −1 to 21 m s −1 as a function of the instrumental configuration used. The derived radial velocities, together with the Gaia proper motions, were used to investigate the cluster membership of the observed stars. After this careful membership analysis, we obtained average velocities for 47 open clusters. To our knowledge, this is the first radial velocity determination for five of these clusters. Finally, the radial velocities, proper motions, distances and ages were used to investigate the kinematics of the observed clusters and in the integration of their orbits.

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The open cluster King 1 in the second quadrant

Cited by 10 publications

References 48 publications

Abundance–age relations with red clump stars in open clusters

Abundance–age relations with red clump stars in open clusters

Abundance-age relations with red clump stars in open clusters

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