Galactic chemical evolution and chemical tagging with open clusters

Reddy, Arumalla B. S.; Giridhar, Sunetra; Lambert, David L.

doi:10.1007/s12036-020-09658-3

Cited by 6 publications

(4 citation statements)

References 34 publications

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“…In addition to our fiducial measure of the total radial gradient, we fit a two-component piecewise linear function to the abundance profile. We generally find that the inner region of the disk is steeper than the outer region, in contrast to some observations (for example Hayden et al 2014;Maciel & Andrievsky 2019), but in agreement with other observations (for example Netopil et al 2016;Reddy et al 2020). Exact comparisons with observations are difficult, because observations typically measure the radial gradient for all stars, rather than measuring for mono-age stellar populations.…”

Section: Discussionsupporting

confidence: 82%

3D elemental abundances of stars at formation across the histories of Milky Way-mass galaxies in the FIRE simulations

Bellardini,

Wetzel,

Loebman

et al. 2022

Preprint

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We characterize the 3-D spatial variations of [Fe/H], [Mg/H], and [Mg/Fe] in stars at the time of their formation, across 11 simulated Milky Way (MW)-and M31-mass galaxies in the FIRE-2 simulations, to inform initial conditions for chemical tagging. The overall scatter in [Fe/H] within a galaxy decreased with time until ≈ 7 Gyr ago, after which it increased to today: this arises from a competition between a reduction of azimuthal scatter and a steepening of the radial gradient in abundance over time. The radial gradient is generally negative, and it steepened over time from an initially flat gradient 12 Gyr ago. The strength of the present-day abundance gradient does not correlate with when the disk 'settled'; instead, it best correlates with the radial velocity dispersion within the galaxy. The strength of azimuthal variation is nearly independent of radius, and the 360 degree scatter decreased over time, from 0.17 dex at t lb = 11.6 Gyr to ∼ 0.04 dex at present day. Consequently, stars at t lb 8 Gyr formed in a disk with primarily azimuthal scatter in abundances. All stars formed in a vertically homogeneous disk, ∆[Fe/H]≤ 0.02 dex within 1 kpc of the galactic midplane, with the exception of the young stars in the inner ≈ 4 kpc at z ∼ 0. These results generally agree with our previous analysis of gas-phase elemental abundances, which reinforces the importance of cosmological disk evolution and azimuthal scatter in the context of stellar chemical tagging. We provide analytic fits to our results for use in chemical-tagging analyses.

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Section: Discussionsupporting

confidence: 82%

3D elemental abundances of stars at formation across the histories of Milky Way-mass galaxies in the FIRE simulations

Bellardini,

Wetzel,

Loebman

et al. 2022

Preprint

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“…It should also be noted that a significant variation in the slope and the turn-off point in the radial metallicity gradient among different studies comes from the choice of the cluster sample, selected range of R GC , and unequal vertical heights. Overall, our radial metallicity gradient estimates agree with most of the recent studies (Reddy et al 2020;Zhang et al 2021;Myers et al 2022a).…”

Section: Discussionsupporting

confidence: 92%

A study on the metallicity gradients in the galactic disk using open clusters

Joshi,

Deepak,

Malhotra

2024

Front. Astron. Space Sci.

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We study the metallicity distribution and evolution in the galactic disk based on the largest sample of open star clusters in the galaxy. From the catalog of 1,879 open clusters in the range of galactocentric distance (RGC) from 4 to 20 kpc, we investigate the variation in metallicity in the galactic disk as functions of RGC, vertical distance (Z), and ages of the clusters. In the direction perpendicular to the galactic plane, the variation in metallicity is found to follow a stepped linear relation. We estimate a vertical metallicity gradient d[Fe/H]d|Z| of −0.545 ± 0.046 dex kpc−1 for |Z| < 0.487 kpc and −0.075 ± 0.093 dex kpc−1 for 0.487 < |Z| < 1.8 kpc. On average, metallicity variations above and below the galactic plane are found to change at similar rates. The change in metallicity in the radial direction is also found to follow a two-function linear relation. We obtain a radial metallicity gradient d[Fe/H]dRGC of −0.070 ± 0.002 dex kpc−1 for 4.0 ≲ RGC ≲ 12.8 kpc and −0.005 ± 0.018 dex kpc−1 for 12.8 ≲ RGC ≲ 20.5 kpc, which clearly shows a strong variation in the metallicity gradient when moving from the inner to the outer galactic disk. The age–metallicity relation (AMR) is found to follow a steeper negative slope of −0.031 ± 0.006 dex Gyr−1 for clusters older than 240 Myr; however, there is some hint of positive metallicity age gradient for younger clusters.

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“…Moreover, to complicate the picture further, the yields of s-process elements are highly dependent on metallicity, in a non-monotonic way (see. e.g., [7,54,55]), and thus varied behaviours are expected at different Galactocentric regions, characterised by diverse star formation history and metallicity, as reflected by the presence of the radial metallicity gradient [56][57][58].…”

Section: Age Effects In the Abundances Of The S-process Elementsmentioning

confidence: 99%

The Abundance of S-Process Elements: Temporal and Spatial Trends from Open Cluster Observations

et al. 2022

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Spectroscopic observations of stars belonging to open clusters, with well-determined ages and distances, are a unique tool for constraining stellar evolution, nucleosynthesis, mixing processes, and, ultimately, Galactic chemical evolution. Abundances of slow (s) process neutron capture elements in stars that retain their initial surface composition open a window into the processes that generated them. In particular, they give us information on their main site of production, i.e., the low- and intermediate-mass Asymptotic Giant Branch (AGB) stars. In the present work, we review some observational results obtained during the last decade that contributed to a better understanding of the AGB phase: the growth of s-process abundances at recent epochs, i.e., in the youngest stellar populations; the different relations between age and [s/Fe] in distinct regions of the disc; and finally the use of s-process abundances combined with those of α elements, [s/α], to estimate stellar ages. We revise some implications that these observations had both on stellar and Galactic evolution, and on our ability to infer stellar ages.

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Galactic chemical evolution and chemical tagging with open clusters

Cited by 6 publications

References 34 publications

3D elemental abundances of stars at formation across the histories of Milky Way-mass galaxies in the FIRE simulations

3D elemental abundances of stars at formation across the histories of Milky Way-mass galaxies in the FIRE simulations

A study on the metallicity gradients in the galactic disk using open clusters

The Abundance of S-Process Elements: Temporal and Spatial Trends from Open Cluster Observations

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