Evolution of the radial ISM metallicity gradient in the Milky Way disk since redshift $\approx 3$ Article Swipe
Bridget Ratcliffe
,
Sergey Khoperskov
,
Ivan Minchev
,
Nathan De Lee
,
Tobias Buck
,
L. Marques
,
Lucy Lu
,
M. Steinmetz
·
YOU?
·
· 2024
· Open Access
·
· DOI: https://doi.org/10.48550/arxiv.2410.17326
YOU?
·
· 2024
· Open Access
·
· DOI: https://doi.org/10.48550/arxiv.2410.17326
Recent works identified a way to recover the time evolution of a galaxy's disk metallicity gradient from the shape of its age--metallicity relation. However, the success of the method is dependent on how the width of the star-forming region evolves over time, which in turn is dependent on a galaxy's present-day bar strength. In this paper, we account for the time variation in the width of the star-forming region when deriving the interstellar medium (ISM) metallicity gradient evolution over time ($\rm \nabla [Fe/H](τ)$), which provides more realistic birth radii estimates of Milky Way (MW) disk stars. Using MW/Andromeda analogues from the TNG50 simulation, we quantified the disk growth of newly born stars as a function of present-day bar strength to provide a correction that improves recovery of $\rm \nabla [Fe/H](τ)$. In TNG50, we find that our correction reduces the median absolute error in recovering $\rm \nabla [Fe/H] (τ)$ by over 30%. To confirm its universality, we test our correction on two galaxies from NIHAO-UHD and find the median absolute error is over 3 times smaller even in the presence of observational uncertainties for the barred, MW-like galaxy. Applying our correction to APOGEE DR17 red giant MW disk stars suggests the effects of merger events on $\rm \nabla [Fe/H](τ)$ are less significant than originally found, and the corresponding estimated birth radii expose epochs when different migration mechanisms dominated. Our correction to account for the growth of the star-forming region in the disk allows for better recovery of the evolution of the MW disk's ISM metallicity gradient and, thus, more meaningful stellar birth radii estimates. With our results, we are able to suggest the evolution of not only the ISM gradient, but also the total stellar disk radial metallicity gradient, providing key constraints to select MW analogues across redshift.
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- Type
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- Language
- en
- Landing Page
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- https://arxiv.org/pdf/2410.17326
- OA Status
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- Related Works
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- OpenAlex ID
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All OpenAlex metadata
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- DOI
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https://doi.org/10.48550/arxiv.2410.17326Digital Object Identifier
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Evolution of the radial ISM metallicity gradient in the Milky Way disk since redshift $\approx 3$Work title
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preprintOpenAlex work type
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enPrimary language
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2024Year of publication
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2024-10-22Full publication date if available
- Authors
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Bridget Ratcliffe, Sergey Khoperskov, Ivan Minchev, Nathan De Lee, Tobias Buck, L. Marques, Lucy Lu, M. SteinmetzList of authors in order
- Landing page
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https://arxiv.org/abs/2410.17326Publisher landing page
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https://arxiv.org/pdf/2410.17326Direct link to full text PDF
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YesWhether a free full text is available
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greenOpen access status per OpenAlex
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https://arxiv.org/pdf/2410.17326Direct OA link when available
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| abstract_inverted_index.expose | 220 |
| abstract_inverted_index.found, | 213 |
| abstract_inverted_index.growth | 107, 233 |
| abstract_inverted_index.median | 139, 167 |
| abstract_inverted_index.medium | 73 |
| abstract_inverted_index.merger | 202 |
| abstract_inverted_index.method | 28 |
| abstract_inverted_index.paper, | 55 |
| abstract_inverted_index.radial | 285 |
| abstract_inverted_index.region | 38, 68, 237 |
| abstract_inverted_index.select | 292 |
| abstract_inverted_index.stars. | 95 |
| abstract_inverted_index.MW-like | 185 |
| abstract_inverted_index.account | 57, 230 |
| abstract_inverted_index.barred, | 184 |
| abstract_inverted_index.confirm | 152 |
| abstract_inverted_index.effects | 200 |
| abstract_inverted_index.evolves | 39 |
| abstract_inverted_index.galaxy. | 186 |
| abstract_inverted_index.provide | 120 |
| abstract_inverted_index.recover | 6 |
| abstract_inverted_index.reduces | 137 |
| abstract_inverted_index.smaller | 174 |
| abstract_inverted_index.stellar | 259, 283 |
| abstract_inverted_index.success | 25 |
| abstract_inverted_index.suggest | 270 |
| abstract_inverted_index.Applying | 187 |
| abstract_inverted_index.However, | 23 |
| abstract_inverted_index.absolute | 140, 168 |
| abstract_inverted_index.deriving | 70 |
| abstract_inverted_index.function | 114 |
| abstract_inverted_index.galaxies | 161 |
| abstract_inverted_index.galaxy's | 12, 49 |
| abstract_inverted_index.gradient | 15, 76, 254 |
| abstract_inverted_index.improves | 124 |
| abstract_inverted_index.presence | 178 |
| abstract_inverted_index.provides | 84 |
| abstract_inverted_index.recovery | 125, 244 |
| abstract_inverted_index.results, | 265 |
| abstract_inverted_index.strength | 118 |
| abstract_inverted_index.suggests | 198 |
| abstract_inverted_index.NIHAO-UHD | 163 |
| abstract_inverted_index.analogues | 98, 294 |
| abstract_inverted_index.dependent | 30, 46 |
| abstract_inverted_index.different | 223 |
| abstract_inverted_index.estimated | 217 |
| abstract_inverted_index.estimates | 89 |
| abstract_inverted_index.evolution | 9, 77, 247, 272 |
| abstract_inverted_index.gradient, | 278, 287 |
| abstract_inverted_index.migration | 224 |
| abstract_inverted_index.providing | 288 |
| abstract_inverted_index.realistic | 86 |
| abstract_inverted_index.redshift. | 296 |
| abstract_inverted_index.relation. | 22 |
| abstract_inverted_index.strength. | 52 |
| abstract_inverted_index.variation | 61 |
| abstract_inverted_index.correction | 122, 136, 158, 189, 228 |
| abstract_inverted_index.dominated. | 226 |
| abstract_inverted_index.estimates. | 262 |
| abstract_inverted_index.identified | 2 |
| abstract_inverted_index.meaningful | 258 |
| abstract_inverted_index.mechanisms | 225 |
| abstract_inverted_index.originally | 212 |
| abstract_inverted_index.quantified | 104 |
| abstract_inverted_index.recovering | 143 |
| abstract_inverted_index.[Fe/H](τ)$ | 207 |
| abstract_inverted_index.constraints | 290 |
| abstract_inverted_index.metallicity | 14, 75, 253, 286 |
| abstract_inverted_index.present-day | 50, 116 |
| abstract_inverted_index.significant | 210 |
| abstract_inverted_index.simulation, | 102 |
| abstract_inverted_index.MW/Andromeda | 97 |
| abstract_inverted_index.[Fe/H](τ)$. | 129 |
| abstract_inverted_index.interstellar | 72 |
| abstract_inverted_index.star-forming | 37, 67, 236 |
| abstract_inverted_index.[Fe/H](τ)$), | 82 |
| abstract_inverted_index.corresponding | 216 |
| abstract_inverted_index.observational | 180 |
| abstract_inverted_index.uncertainties | 181 |
| abstract_inverted_index.universality, | 154 |
| abstract_inverted_index.age--metallicity | 21 |
| cited_by_percentile_year | |
| countries_distinct_count | 0 |
| institutions_distinct_count | 8 |
| citation_normalized_percentile |