A simple and general method for solving detailed chemical evolution with delayed production of iron and other chemical elements

Vincenzo, Fiorenzo; Matteuccí, F.; Spitoni, E.

doi:10.1093/mnras/stw3369

Cited by 15 publications

(15 citation statements)

References 60 publications

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“…The yield for delayed metals is adopted to be y ∆ Z ≈ 2.7 × 10 −3 ; this has been computed taking into account that the occurrence of type-Ia SNe is around 2 × 10 −3 /M per stellar mass formed, and that 0.63 M of iron-group elements are produced on average per explosion (see Bell et al 2003;Maoz et al 2014); the outcome is also consistent with the normalization of the observed type-Ia SN delay time distribution (e.g., Vincenzo et al 2017).…”

Section: Yields and Other Imf-related Parameterssupporting

confidence: 65%

“…Finally, some specific issues related to the global evolution of the baryonic content in galaxies can be tackled with analytic models, i.e., models with analytic solutions (e.g., Schmidt 1963;Talbot & Arnett 1971;Tinsley 1974;Pagel & Patchett 1975;Hartwick 1976;Chiosi 1980;Matteucci & Greggio 1986;Edmunds 1990;Dwek 1998;Hirashita 2000, Hirashita et al 2015Chiappini et al 2001;Draine 2003Draine , 2011Inoue 2003;Greggio 2005;Naab & Ostriker 2006;Erb 2008;Zhukovska et al 2008;Valiante et al 2009;Bouché et al 2010;Dwek & Cherchneff 2011;Davé et al 2012;Asano et al 2013;Lilly et al 2013;De Benassutti et al 2014;Dekel & Mandelker 2014;Forbes et al 2014a;Pipino et al 2014;Feldmann 2015;Mancini et al 2015;Mollá et al 2015;Recchi & Kroupa 2015;Rodriguez-Puebla et al 2016;Andrews et al 2017;Gioannini et al 2017;Spitoni et al 2017;Weinberg et al 2017;Vincenzo et al 2017;Grisoni et al 2018;Imara et al 2018;…”

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confidence: 99%

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New Analytic Solutions for Galaxy Evolution: Gas, Stars, Metals, and Dust in Local ETGs and Their High-z Star-forming Progenitors

Pantoni

Lapi

Massardi

et al. 2019

ApJ

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We present a set of new analytic solutions aimed at self-consistently describing the spatially-averaged time evolution of the gas, stellar, metal, and dust content in an individual starforming galaxy hosted within a dark halo of given mass and formation redshift. Then, as an application, we show that our solutions, when coupled to specific prescriptions for parameter setting (inspired by in-situ galaxy-black hole coevolution scenarios) and merger rates (based on numerical simulations), can be exploited to reproduce the main statistical relationships followed by early-type galaxies and by their high-redshift starforming progenitors. Our analytic solutions allow to easily disentangle the diverse role of the main physical processes regulating galaxy formation, to quickly explore the related parameter space, and to make transparent predictions on spatially-averaged quantities. As such, our analytic solutions may provide a basis for improving the (subgrid) physical recipes presently implemented in theoretical approaches and numerical simulations, and can offer a benchmark for interpreting and forecasting current and future broadband observations of high-redshift starforming galaxies.2 PANTONI ET AL. evolution of the gas, stellar, metal, and dust content in an individual starforming galaxy hosted within a dark halo of given mass and formation redshift. Our basic framework pictures a galaxy as an open, one-zone system comprising three interlinked mass components: a reservoir of warm gas subject to cooling and condensation toward the central regions; cold gas fed by infall and depleted by star formation and stellar feedback (type-II supernovae [SNe] and stellar winds); stellar mass, partially restituted to the cold phase by stars during their evolution. Remarkably, the corresponding analytic solutions for the metal enrichment history of the cold gas and stellar mass are self-consistently derived using as input the solutions for the evolution of the mass components; the metal equations includes effects of feedback, astration, instantaneous production during star formation, and delayed production by type-Ia SNe, possibly following a specified delay time distribution. Finally, the dust mass evolution takes into account the formation of grain cores associated to star formation, and of the grain mantles due to accretion onto pre-existing cores; astration of dust by star formation and stellar feedback, and spallation by SN shockwaves are also included.We then apply our analytic solutions to describe the formation of spheroids/early-type galaxies (ETGs) and the evolution of their starforming progenitors. To this purpose, we couple our solutions to two additional ingredients: (i) specific prescriptions for parameter setting, inspired by in-situ galaxy-black hole coevolution scenarios of ETG formation; (ii) estimates of the halo and stellar mass growth by mergers, computed on the basis of the merger rates from state-of-the-art numerical simulations. We then derive and confront with available data a bunch of fundamental spatially-...

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Section: Yields and Other Imf-related Parameterssupporting

confidence: 65%

mentioning

confidence: 99%

New Analytic Solutions for Galaxy Evolution: Gas, Stars, Metals, and Dust in Local ETGs and Their High-z Star-forming Progenitors

Pantoni

Lapi

Massardi

et al. 2019

ApJ

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“…This is due to the fact that Type II SNe trace the SFR. If the SFR peaks at early time (e.g., τ D1 =0.1), at t max = 4.3 Gyr the iron produced by Type Ia SNe with a time delay will dominate the ISM pollution (Matteucci et al 2009;Bonaparte et al 2013;Vincenzo et al 2017). When the SFR is more extended in time (e.g., τ D1 =2), a smaller [α/Fe] abundance ratio is therefore expected.…”

Section: Model Results Taking Into Account the Observational Errorsmentioning

confidence: 99%

Galactic Archaeology with asteroseismic ages: Evidence for delayed gas infall in the formation of the Milky Way disc

Spitoni

Aguirre

Matteuccí

et al. 2019

A&A

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183

239

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Context. Precise stellar ages from asteroseismology have become available and can help setting stronger constraints on the evolution of the Galactic disc components. Recently, asteroseismology has confirmed a clear age difference in the solar annulus between two distinct sequences in the [α/Fe] versus [Fe/H] abundance ratios relation: the high-α and low-α stellar populations. Aims. We aim at reproducing these new data with chemical evolution models including different assumptions for the history and number of accretion events. Methods. We tested two different approaches: a revised version of the "two-infall" model where the high-α phase forms by a fast gas accretion episode and the low-α sequence follows later from a slower gas infall rate, and the parallel formation scenario where the two disc sequences form coevally and independently. Results. The revised "two-infall" model including uncertainties in age and metallicity is capable of reproducing: i) the [α/Fe] vs. [Fe/H] abundance relation at different Galactic epochs, ii) the age−metallicity relation and the time evolution [α/Fe]; iii) the age distribution of the high-α and low-α stellar populations, iv) the metallicity distribution function. The parallel approach is not capable of properly reproduce the stellar age distribution, in particular at old ages. Conclusions. The best chemical evolution model is the revised "two-infall" one, where a consistent delay of ∼4.3 Gyr in the beginning of the second gas accretion episode is a crucial assumption to reproduce stellar abundances and ages.

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“…Côté et al (2017) and Andrews et al (2017) both assume a linear Schmidt law n Schmidt = 1 (same as this work), whereas Chiappini et al (2001) use n Schmidt = 1.5 together with a gas density threshold. See Vincenzo et al (2017) for a detailed comparison between linear and non-linear Schmidt law. …”

Section: Stellar Physics Parametersmentioning

confidence: 99%

Chempy: A flexible chemical evolution model for abundance fitting

Rybizki

Just

Rix

2017

A&A

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Elemental abundances of stars are the result of the complex enrichment history of their galaxy. Interpretation of observed abundances requires flexible modeling tools to explore and quantify the information about Galactic chemical evolution (GCE) stored in such data. Here we present Chempy, a newly developed code for GCE modeling, representing a parametrized open one-zone model within a Bayesian framework. A Chempy model is specified by a set of five to ten parameters that describe the effective galaxy evolution along with the stellar and star-formation physics: for example, the star-formation history (SFH), the feedback efficiency, the stellar initial mass function (IMF), and the incidence of supernova of type Ia (SN Ia). Unlike established approaches, Chempy can sample the posterior probability distribution in the full model parameter space and test data-model matches for different nucleosynthetic yield sets. It is essentially a chemical evolution fitting tool. We straightforwardly extend Chempy to a multi-zone scheme. As an illustrative application, we show that interesting parameter constraints result from only the ages and elemental abundances of the Sun, Arcturus, and the present-day interstellar medium (ISM). For the first time, we use such information to infer the IMF parameter via GCE modeling, where we properly marginalize over nuisance parameters and account for different yield sets. We find that 11.6 +2.1 −1.6 % of the IMF explodes as core-collapse supernova (CC-SN), compatible with Salpeter (1955, ApJ, 121, 161). We also constrain the incidence of SN Ia per 10 3 M to 0.5−1.4. At the same time, this Chempy application shows persistent discrepancies between predicted and observed abundances for some elements, irrespective of the chosen yield set. These cannot be remedied by any variations of Chempy's parameters and could be an indication of missing nucleosynthetic channels. Chempy could be a powerful tool to confront predictions from stellar nucleosynthesis with far more complex abundance data sets and to refine the physical processes governing the chemical evolution of stellar systems.

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A simple and general method for solving detailed chemical evolution with delayed production of iron and other chemical elements

Cited by 15 publications

References 60 publications

New Analytic Solutions for Galaxy Evolution: Gas, Stars, Metals, and Dust in Local ETGs and Their High-z Star-forming Progenitors

New Analytic Solutions for Galaxy Evolution: Gas, Stars, Metals, and Dust in Local ETGs and Their High-z Star-forming Progenitors

Galactic Archaeology with asteroseismic ages: Evidence for delayed gas infall in the formation of the Milky Way disc

Chempy: A flexible chemical evolution model for abundance fitting

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