<scp>L-GALAXIES</scp> 2020: The evolution of radial metallicity profiles and global metallicities in disc galaxies

Yates, Robert M.; Henriques, Bruno M. B.; Fu, Jiang; Kauffmann, Guinevere; Thomas, P.; Guo, Qi; White, Simon D. M.; Schady, P.

doi:10.1093/mnras/stab741

Cited by 47 publications

(42 citation statements)

References 178 publications

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“…2). This trend is in agreement with previous works on the evolution of the metallicity gradients in individual galaxies, which reported large scatter and rapid variation of the gasphase metallicity gradients for higher redshift (see also Ma et al 2017b;Yates et al 2021). Here, our goal is to trace the evolution of ∇ (O/H) for individual galaxies along their merger trees, while keeping a statistical approach.…”

Section: Evolution Of the Metallicity Gradients Of Individual Galaxiessupporting

confidence: 89%

“…This contributes to enhance the chemical content in the ISM, modifying the metallicity gradient gradually towards a shallower one. Hence, when galaxies with different formation histories are combined together, the correlation is likely to be suppressed or weakened due to the large variety of evolutionary tracks (Tissera et al 2016b), even if it exists for individual galaxies (Ma et al 2017a;Yates et al 2021).…”

Section: Ssfr Dependence Of the Metallicity Gradientsmentioning

confidence: 99%

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The evolution of the oxygen abundance gradients in star-forming galaxies in the EAGLE simulations

Tissera,

Rosas-Guevara,

Sillero

et al. 2021

Preprint

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We analyse the evolution of the oxygen abundance gradient of star-forming galaxies with stellar mass M * ≥ 10 9 M in the simulation over the redshift range 𝑧 = [0, 2.5]. We find that the median metallicity gradient of the simulated galaxies is close to zero at all 𝑧, whereas the scatter around the median increases with 𝑧. The metallicity gradients of individual galaxies can evolve from strong to weak and vice-versa, since mostly low-metallicity gas accretes onto the galaxy, resulting in enhanced star formation and ejection of metal enriched gas by energy feedback. Such episodes of enhanced accretion, mainly dominated by major mergers, are more common at higher 𝑧, and hence contribute to increasing the diversity of gradients. For galaxies with negative metallicity gradients, we find a redshift evolution of ∼ −0.03 dex kpc −1 /𝛿z. A positive mass dependence is found at 𝑧 ≤ 0.5, which becomes slightly stronger for higher redshifts and, mainly, for M * < 10 9.5 M . Only galaxies with negative metallicity gradients define a correlation with galaxy size, consistent with an inside-out formation scenario. Our findings suggest that major mergers and/or significant gas accretion can drive strong negative or positive metallicity gradients. The first ones are preferentially associated with disc-dominated galaxies, and the second ones with dispersion-dominated systems. The comparison with forthcoming observations at high redshift will allow a better understanding of the potential role of metallicity gradients as a chemical probe of galaxy formation.

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Section: Evolution Of the Metallicity Gradients Of Individual Galaxiessupporting

confidence: 89%

Section: Ssfr Dependence Of the Metallicity Gradientsmentioning

confidence: 99%

The evolution of the oxygen abundance gradients in star-forming galaxies in the EAGLE simulations

Tissera,

Rosas-Guevara,

Sillero

et al. 2021

Preprint

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“…A more self-consistent (although still approximate) estimate of the dust mass produced by Type I SLSNe at high redshift can be obtained from cosmological galaxy evolution simulations. For example, the cosmic dust production rate density (DD) from SLSNe can be calculated from the L-Galaxies 2020 semi-analytic model (Henriques et al 2020;Yates et al 2021). We assume that (a) Type I SLSNe only form in galaxies with gas-phase metallicity ≤ 0.5 Z , (b) the initial mass function (IMF) is fixed over time and space, (c) SLSNe produce 10 times as much dust per event as CCSNe, and (d) the shape of the DD evolution from SNe follows that of the cosmic star formation rate density (SFRD).…”

Section: Discussionmentioning

confidence: 99%

SN 2018bsz: significant dust formation in a nearby superluminous supernova

-W.¹,

Brennan²,

Wesson³

et al. 2021

Preprint

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We investigate the thermal emission and extinction from dust associated with the nearby superluminous supernova (SLSN) 2018bsz. Our dataset has daily cadence and simultaneous optical and near-infrared coverage up to ∼100 days, together with late time (+1.7 yr) MIR observations. At 230 days after light curve peak the SN is not detected in the optical, but shows a surprisingly strong near-infrared excess, with r − J > 3 mag and r − K s > 5 mag. The time evolution of the infrared light curve enables us to investigate if the mid-infrared emission is from newly formed dust inside the SN ejecta, from a pre-existing circumstellar envelope, or interstellar material heated by the radiation from the SN. We find the latter two scenarios can be ruled out, and a scenario where new dust is forming in the SN ejecta at epochs > 200 days can self-consistently reproduce the evolution of the SN flux. We can fit the spectral energy distribution well at +230 d with 5 × 10 −4 M of carbon dust, increasing over the following several hundred days to 10 −2 M by +535 d. SN 2018bsz is the first SLSN showing evidence for dust formation within the SN ejecta, and appears to form ten times more dust than normal core-collapse SNe at similar epochs. Together with their preference for low mass, low metallicity host galaxies, we suggest that SLSNe may be a significant contributor to dust formation in the early Universe.

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“…When analysing the chemical evolution of galaxies in L-G 2020, Yates et al (2021a) found that the default version of the model, which allows 70 per cent of the material ejected by SNe to directly enrich the ambient ISM, returned stellar and ISM metallicities that were too high compared to the latest global and spatially-resolved observational data (e.g. Zahid et al 2017;Belfiore et al 2017;Yates et al 2020).…”

Section: Parameter Changesmentioning

confidence: 99%

L-GALAXIES 2020: The formation and chemical evolution of stellar haloes in Milky Way Analogues and galaxy clusters

Murphy,

Yates,

Mohamed

2021

Preprint

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We present an analysis of the formation and chemical evolution of stellar haloes around (a) Milky Way Analogue (MWA) galaxies and (b) galaxy clusters in the L-G 2020 semi-analytic model of galaxy evolution. Observed stellar halo properties are better reproduced when assuming a gradual stripping model for the removal of cold gas and stars from satellites, compared to an instantaneous stripping model. The slope of the stellar mass -metallicity relation for MWA stellar haloes is in good agreement with that observed in the local Universe. This extends the good agreement between L-G 2020 and metallicity observations from the gas and stars inside galaxies to those outside. Halo stars contribute on average only ∼ 0.1 per cent of the total circumgalactic medium (CGM) enrichment by 𝑧 = 0 in MWAs, ejecting predominantly carbon produced by AGB stars. Around a quarter of MWAs have a single 'significant progenitor' with a mean mass of ∼ 2.3 × 10 9 M , similar to that measured for Gaia Enceladus. For galaxy clusters, L-G 2020 shows good correspondence with observations of stellar halo mass fractions, but slightly over-predicts stellar masses. Assuming a Navarro-Frenk-White profile for the stellar halo mass distribution provides the best agreement. On average, the intracluster stellar component (ICS) is responsible for 5.4 per cent of the total intracluster medium (ICM) iron enrichment, exceeding the contribution from the brightest cluster galaxy (BCG) by 𝑧 = 0. We find that considering gradual stripping of satellites and realistic radial profiles is crucial for accurately modelling stellar halo formation on all scales in semi-analytic models.

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L-GALAXIES 2020: The evolution of radial metallicity profiles and global metallicities in disc galaxies

Cited by 47 publications

References 178 publications

The evolution of the oxygen abundance gradients in star-forming galaxies in the EAGLE simulations

The evolution of the oxygen abundance gradients in star-forming galaxies in the EAGLE simulations

SN 2018bsz: significant dust formation in a nearby superluminous supernova

L-GALAXIES 2020: The formation and chemical evolution of stellar haloes in Milky Way Analogues and galaxy clusters

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