RECORD
Chemical evolution of disc galaxies from cosmological simulations
Astrophysics of Galaxies · Submitted 15 Feb 2019
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim We find that a Kroupa et al. (1993) IMF has to be preferred when modelling late-type galaxies in the local universe.
The compiled record
The paper's own sentences, arranged. Each label is drawn from a closed vocabulary; the number beside it is the probability the classifier gave that label. Numbers in the tables are the authors', checked by code. No sentence in this record was written by a model.
Open the compiled record
The abstract, sentence by sentence
We perform a suite of cosmological hydrodynamical simulations of disc galaxies, with zoomed-in initial conditions leading to the formation of a halo of mass $M_{\rm halo, \, DM} \simeq 2 \cdot 10^{12}$ M$_{\odot}$ at redshift $z=0$. These simulations aim at investigating the chemical evolution and the distribution of metals in a disc galaxy, and at quantifying the effect of $(i)$ the assumed IMF, $(ii)$ the adopted stellar yields, and $(iii)$ the impact of binary systems originating SNe Ia on the process of chemical enrichment. We consider either a Kroupa et al. (1993) or a more top-heavy Kroupa (2001) IMF, two sets of stellar yields and different values for the fraction of binary systems suitable to give rise to SNe Ia. We investigate stellar ages, SN rates, stellar and gas metallicity gradients, and stellar $\alpha$-enhancement in simulations, and compare predictions with observations. We find that a Kroupa et al. (1993) IMF has to be preferred when modelling late-type galaxies in the local universe. On the other hand, the comparison of stellar metallicity profiles and $\alpha$-enhancement trends with observations of Milky Way stars shows a better agreement when a Kroupa (2001) IMF is assumed. Comparing the predicted SN rates and stellar $\alpha$-enhancement with observations supports a value for the fraction of binary systems producing SNe Ia of $0.03$, at least for late-type galaxies and for the considered IMFs. Adopted stellar yields are crucial in regulating cooling and star formation, and in determining patterns of chemical enrichment for stars, especially for those located in the galaxy bulge.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | We perform a suite of cosmological hydrodynamical simulations of disc galaxies, with zoomed-in initial conditions leading to the formation of a halo of mass $M_{\rm halo, \, DM} \simeq 2 \cdot 10^{12}$ M$_{\odot}$ at redshift $z=0$. | method 0.93 | 0.96 | 0.02 | asserted 0.99 |
| s1 | These simulations aim at investigating the chemical evolution and the distribution of metals in a disc galaxy, and at quantifying the effect of $(i)$ the assumed IMF, $(ii)$ the adopted stellar yields, and $(iii)$ the impact of binary systems originating SNe Ia on the process of chemical enrichment. | contribution 0.91 | 0.40 | 0.03 | asserted 0.76 |
| s2 | We consider either a Kroupa et al. (1993) or a more top-heavy Kroupa (2001) IMF, two sets of stellar yields and different values for the fraction of binary systems suitable to give rise to SNe Ia. | method 0.98 | 0.83 | 0.02 | asserted 0.89 |
| s3 | We investigate stellar ages, SN rates, stellar and gas metallicity gradients, and stellar $\alpha$-enhancement in simulations, and compare predictions with observations. | method 0.50 | 0.95 | 0.03 | asserted 0.88 |
| s4 | We find that a Kroupa et al. (1993) IMF has to be preferred when modelling late-type galaxies in the local universe. | result 0.93 | 0.95 | 0.29 | asserted 1.00 |
| s5 | On the other hand, the comparison of stellar metallicity profiles and $\alpha$-enhancement trends with observations of Milky Way stars shows a better agreement when a Kroupa (2001) IMF is assumed. | result 0.99 | 0.89 | 0.14 | asserted 0.95 |
| s6 | Comparing the predicted SN rates and stellar $\alpha$-enhancement with observations supports a value for the fraction of binary systems producing SNe Ia of $0.03$, at least for late-type galaxies and for the considered IMFs. | result 1.00 | 0.92 | 0.17 | asserted 0.62 |
| s7 | Adopted stellar yields are crucial in regulating cooling and star formation, and in determining patterns of chemical enrichment for stars, especially for those located in the galaxy bulge. | result 0.85 | 0.77 | 0.08 | asserted 1.00 |
What was examined, and what was not
- arXiv listing abstract v1
- full text
- figures and tables
- references and citing sentences
- relations to other papers
- P abstract
- S sections
- T body sentences
- C citations
- R cross-paper relations
The paper
Original abstract
We perform a suite of cosmological hydrodynamical simulations of disc galaxies, with zoomed-in initial conditions leading to the formation of a halo of mass $M_{\rm halo, \, DM} \simeq 2 \cdot 10^{12}$ M$_{\odot}$ at redshift $z=0$. These simulations aim at investigating the chemical evolution and the distribution of metals in a disc galaxy, and at quantifying the effect of $(i)$ the assumed IMF, $(ii)$ the adopted stellar yields, and $(iii)$ the impact of binary systems originating SNe Ia on the process of chemical enrichment. We consider either a Kroupa et al. (1993) or a more top-heavy Kroupa (2001) IMF, two sets of stellar yields and different values for the fraction of binary systems suitable to give rise to SNe Ia. We investigate stellar ages, SN rates, stellar and gas metallicity gradients, and stellar $\alpha$-enhancement in simulations, and compare predictions with observations. We find that a Kroupa et al. (1993) IMF has to be preferred when modelling late-type galaxies in the local universe. On the other hand, the comparison of stellar metallicity profiles and $\alpha$-enhancement trends with observations of Milky Way stars shows a better agreement when a Kroupa (2001) IMF is assumed. Comparing the predicted SN rates and stellar $\alpha$-enhancement with observations supports a value for the fraction of binary systems producing SNe Ia of $0.03$, at least for late-type galaxies and for the considered IMFs. Adopted stellar yields are crucial in regulating cooling and star formation, and in determining patterns of chemical enrichment for stars, especially for those located in the galaxy bulge.
Human review
References
How the literature uses it
1 arXiv paper cite this in 1 sentence
What it cites · 7 sentences without a confident label
Contests 1 paper
-
At variance with our aformentioned recalibration, [ref] did not tune the stellar feedback efficiency accounting for the different number of stars produced by the adopted metallicity-dependent IMF, with a consequent overproduction of stellar mass resulting from a modified star formation history.
Simulating a metallicity-dependent initial mass function: Consequences for feedback and chemical abundances · Impact of IMF on the number of massive stars · contest 0.81
Cites as background 4 papers
-
The impact that the variation of the IMF slopes has on star formation rates, galaxy morphology, chemical properties of stars and timing of chemical enrichment has been investigated also in simulations, where different shapes of the IMF have been considered, either assuming a global IMF [ref] or one depending on gas density and metallicity [ref] .
Simulating a metallicity-dependent initial mass function: Consequences for feedback and chemical abundances · Introduction · 0.93
-
The impact that the variation of the IMF slopes has on star formation rates, galaxy morphology, chemical properties of stars and timing of chemical enrichment has been investigated also in simulations, where different shapes of the IMF have been considered, either assuming a global IMF [ref] or one depending on gas density and metallicity [ref] .
Calibrated, cosmological hydrodynamical simulations with variable IMFs I: Method and effect on global galaxy scaling relations · Introduction · 0.93
-
Some light on the origin and fate of metals in different systems have been shed by analysing the chemical properties of the ISM, CGM, IGM (intergalactic medium) and ICM (intra-cluster medium) in simulations, and comparing them with observations [ref] .
The multiphase circumgalactic medium traced by low metal ions in EAGLE zoom simulations · Introduction · 0.91
Discussion
Know something about this paper? Leave a comment, or highlight any passage above to comment on it.