Red Supergiants as Cosmic Abundance Probes: Massive Star Clusters in M83 and the Mass–Metallicity Relation of Nearby Galaxies

Davies, Ben; Kudritzki, Rolf‐Peter; Lardo, C.; Bergemann, M.; Beasor, Emma R.; Plez, B.; Evans, C. J.; Bastian, N.; Patrick, L. R.

doi:10.3847/1538-4357/aa89ed

Cited by 45 publications

(48 citation statements)

References 56 publications

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“…In the last decade, new techniques have been developed to study the chemical contents of nearby galaxies using blue supergiants (BSGs) as well as red supergiants (RSGs). It has been shown extensively that accurate metallicities can be obtained in agreement with measurements inferred using the T e -based method using either BSGs or RSGs (Kudritzki et al 2012(Kudritzki et al , 2013Hosek et al 2014;Davies et al 2010;Gazak et al 2014;Davies et al 2015;Gazak et al 2015;Davies et al 2017). The agreement between the nebular and stellar abundances is of the order of ∼0.1 dex.…”

Section: Introductionmentioning

confidence: 75%

The First Metallicity Study of M83 Using the Integrated UV Light of Star Clusters^*

Hernández

Larsen

Aloisi

et al. 2019

ApJ

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Stellar populations are powerful tools for investigating the evolution of extragalactic environments. We present the first UV integrated-light spectroscopic observations for 15 young star clusters in the starburst M83 with a special focus on metallicity measurements. The data were obtained with the Cosmic Origins Spectrograph (COS) onboard the Hubble Space Telescope. We analyse the data applying an abundance technique previously used to study an optical set of star clusters. We estimate a central metallicity of [Z] = +0.20 ± 0.15 dex in agreement with those obtained through independent methods, i.e. J-band and blue supergiants. We estimate a UV metallicity gradient of −0.041 ± 0.022 dex kpc −1 consistent with the optical metallicity gradient of −0.040 ± 0.032 dex kpc −1 for R/R 25 < 0.5. Combining our stellar metallicities, UV and optical, with those from H II regions (strongline abundances based on empirical calibrations) we identify two possible breaks in the gradient of M83 at galactocentric distances of R ∼ 0.5 and 1.0 R 25 . If the abundance breaks are genuine, the metallicity gradient of this galaxy follows a steep-shallow-steep trend, a scenario predicted by three-dimensional (3D) numerical simulations of disc galaxies. The first break is located near the corotation radius. This first steep gradient may have originated by recent star formation episodes and a relatively young bar (<1 Gyr). In the numerical simulations the shallow gradient is created by the effects of dilution by outflow where low-metallicity material is mixed with enriched gas. And finally, the second break and last steep gradient mark the farthest galactocentric distances where the outward flow has penetrated.

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Section: Introductionmentioning

confidence: 75%

The First Metallicity Study of M83 Using the Integrated UV Light of Star Clusters^*

Hernández

Larsen

Aloisi

et al. 2019

ApJ

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“…Similarly to Tremonti et al (2004), the calibrations adopted in the latter works provide oxygen abundances based on the predictions of different grids of photoionisation models. More precisely, for Maiolino et al (2008) In addition, we plot the oxygen abundance measurements derived for nearby galaxies in the local Universe (including the Milky Way) which exploits stellar spectroscopy of young (∼ 10 − 50 Myr) red and blue supergiants (RSG, BSG) to probe the chemical enrichment level Davies et al 2015;Bresolin et al 2016;Kudritzki et al 2016); the data points are taken from the compilation presented in Table 3 of Davies et al (2017)(see also references therein). Metallicity measurements from blue supergiants are plotted as blue crosses, while abundances measured from red supergiants are plotted as red stars; a few galaxies in the sample have both measurements, which always agree within 0.1 dex.…”

Section: Comparison With Different Mzr From the Literaturementioning

confidence: 99%

“…In particular, theKewley & Dopita 2002;Tremonti et al 2004;Mannucci et al 2010 curves are anchored to abundance scale defined by different grids of photoionization models, while theAndrews & Martini 2013, Pettini & Pagel 2004and Yates et al 2019 curve are based on the T e -based abundance scale. Red stars and blue crosses represent the abundances derived in nearby galaxies from stellar spectroscopy of red an blue supergiants respectively, as collected byDavies et al 2017.…”

mentioning

confidence: 99%

The mass–metallicity and the fundamental metallicity relation revisited on a fully Te-based abundance scale for galaxies

Curti

Mannucci

Cresci

et al. 2019

Monthly Notices of the Royal Astronomical Society

249

440

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The relationships between stellar mass, gas-phase metallicity and star formation rate (i.e. the Mass-Metallicity, MZR, and the Fundamental Metallcity Relation, FMR) in the local Universe are revisited by fully anchoring the metallicity determination for SDSS galaxies on the T e abundance scale defined exploiting the strong-line metallicity calibrations presented in Curti et al. (2017). Self-consistent metallicity measurements allow a more unbiased assessment of the scaling relations involving M, Z and SFR, which provide powerful constraints for the chemical evolution models. We parametrise the MZR with a new functional form which allows us to better characterise the turnover mass. The slope and saturation metallicity are in good agreement with previous determinations of the MZR based on the Te method, while showing significantly lower normalisation compared to those based on photoionisation models. The Z-SFR dependence at fixed stellar mass is also investigated, being particularly evident for highly star forming galaxies, where the scatter in metallicity is reduced up to a factor of ∼ 30%. A new parametrisation of the FMR is given by explicitly introducing the SFR-dependence of the turnover mass into the MZR. The residual scatter in metallicity for the global galaxy population around the new FMR is 0.054 dex. The new FMR presented in this work represents a useful local benchmark to compare theoretical predictions and observational studies (of both local and high-redshift galaxies) whose metallicity measurements are tied to the abundance scale defined by the T e method, hence allowing to properly assess its evolution with cosmic time.

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“…Maier et al (2016) derived two metallicity calibrations for galaxies on the star-forming sequence based on equations 3. and 4. of Kewley et al (2013). The calibration as a function of the line ratio [OIII]/Hβ is very useful as a metallicity indicator for highredshifted galaxies which do not have measurements of the [NII] and Hα ELs, and it can be expressed as follows: (Bresolin et al (2016)) and red supergiants (Davies et al (2017)) have, however, demonstrated that the metallicity calibration based on strong emission line ratios, yielding the most accurate, absolute metallicities is the O3N2 calibration, and we have chosen to use this calibration throughout this study, when all 4 ELs of interest were present. The values for the (O/H)s of the R2248 cluster galaxies are listed in in Table 1.…”

Section: Oxygen Abundancesmentioning

confidence: 99%

“…al (2019) have demonstrated, that both the shape and the overall normalisation of the gas-phase MZR depend on the metallicity calibration used. Studies of blue (Bresolin et al (2016)) and red supergiants (Davies et al (2017)) have shown that the EL metallicity calibration, yielding absolute metallicities, is the O3N2 calibration, the one used throughout this work (cf. Fig.…”

Section: The Fundamental Metallicity Relation Z(msfr) For Thementioning

confidence: 99%

CLASH-VLT: Enhancement of (O/H) in z = 0.35 RX J2248−4431 cluster galaxies

Ciocan

Maier

Ziegler

et al. 2020

A&A

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Aims. Gas-phase metallicities offer insight into the chemical evolution of galaxies, as they reflect the recycling of gas through star formation, galactic inflows and outflows. Environmental effects such as star-formation quenching mechanisms play an important role in shaping the evolution of galaxies. Clusters of galaxies at z < 0.5 are expected to be the sites where environmental effects can be clearly observed with present-day telescopes. Methods. We explore the Frontier Fields cluster RXJ2248-443 at z = 0.348 with VIMOS/VLT spectroscopy from CLASH-VLT, which covers a central region corresponding to almost 2 virial radii. The fluxes of [OII] λ3727, Hβ, [OIII] λ5007, Hα and [NII] λ6584 emission lines were measured allowing the derivation of (O/H) gas metallicities, star formation rates based on extinction-corrected Hα fluxes and active galactic nuclei (AGN) contamination. We compare our sample of cluster galaxies to a population of field galaxies at similar redshifts. Results. We use the location of galaxies in projected phase-space to distinguish between cluster and field galaxies. Both populations follow the star-forming-sequence in the diagnostic diagrams, which allow disentangling between the ionising sources in a galaxy, with only a low number of galaxies classified as Seyfert II. Both field and cluster galaxies follow the "Main-Sequence" of star forming galaxies, with no substantial difference observed between the two populations. In the Mass -Metallicity (MZ) plane, both high mass field and cluster galaxies show comparable (O/H)s to the local SDSS MZ relation, with an offset of low mass galaxies (log(M/M ) < 9.2) towards higher metallicities. While both the metallicities of "accreted" (R < R 500 ) and "infalling" (R > R 500 ) cluster members are comparable at all masses, the cluster galaxies from the intermediate, mass complete bin (9.2 < log(M/M ) < 10.2) show more enhanced metallicities than their field counterparts, by a factor of 0.065 dex, with a ∼ 1.8σ significance. The intermediate mass field galaxies are in accordance with the expected (O/H)s from the Fundamental Metallicity relation, while the cluster members deviate strongly from the model predictions, by a factor of ∼ 0.12 dex. The results of this work are in accordance with studies of other clusters at z < 0.5 and favour the scenario in which the hot halo gas of low and intermediate mass cluster galaxies is removed due to ram pressure stripping, leading to an increase in their gas-phase metallicity.

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Red Supergiants as Cosmic Abundance Probes: Massive Star Clusters in M83 and the Mass–Metallicity Relation of Nearby Galaxies

Cited by 45 publications

References 56 publications

The First Metallicity Study of M83 Using the Integrated UV Light of Star Clusters^*

The First Metallicity Study of M83 Using the Integrated UV Light of Star Clusters^*

The mass–metallicity and the fundamental metallicity relation revisited on a fully Te-based abundance scale for galaxies

CLASH-VLT: Enhancement of (O/H) in z = 0.35 RX J2248−4431 cluster galaxies

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Red Supergiants as Cosmic Abundance Probes: Massive Star Clusters in M83 and the Mass–Metallicity Relation of Nearby Galaxies

Cited by 45 publications

References 56 publications

The First Metallicity Study of M83 Using the Integrated UV Light of Star Clusters*

The First Metallicity Study of M83 Using the Integrated UV Light of Star Clusters*

The mass–metallicity and the fundamental metallicity relation revisited on a fully Te-based abundance scale for galaxies

CLASH-VLT: Enhancement of (O/H) in z = 0.35 RX J2248−4431 cluster galaxies

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Resources

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The First Metallicity Study of M83 Using the Integrated UV Light of Star Clusters^*

The First Metallicity Study of M83 Using the Integrated UV Light of Star Clusters^*