The cosmic evolution of metallicity from the SDSS fossil record

Panter, Ben; Jiménez, Raúl; Heavens, Alan; Charlot, S.

doi:10.1111/j.1365-2966.2008.13981.x

Cited by 202 publications

(283 citation statements)

References 41 publications

(77 reference statements)

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“…On the other hand, the approach used by Panter et al (2008) yields a mass fraction weighted metallicity. From Fig.…”

Section: The M * -Z * R E L At I O Nmentioning

confidence: 99%

“…The number of galaxies per mass bin is N bin 10 at all considered z. Observational data at z ∼ 0 from Gallazzi et al (2005) are represented as black circles with error bars, which indicate the median relation together with the 16th and 84th percentiles. The fitted relation to SDSS data given in Panter et al (2008) is shown with a dotted green line. We also show findings by Gallazzi et al (2014) at z = 0.7 as green asterisks with error bars, depicting the median relation together with the 16th and 84th percentiles.…”

Section: The M * -Z * R E L At I O Nmentioning

confidence: 99%

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Galaxy metallicity scaling relations in the EAGLE simulations

Rossi

Bower

Font

et al. 2017

Monthly Notices of the Royal Astronomical Society

144

136

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Citation for published item:he ossiD w r¡ % imili nd fowerD i h rd qF nd pontD endree F nd h yeD toop nd heunsD om @PHIUA 9q l xy met lli ity s ling rel tions in the ieqvi simul tionsF9D wonthly noti es of the oy l estronomi l o ietyFD RUP @QAF ppF QQSREQQUUF Further information on publisher's website: Use policyThe full-text may be used and/or reproduced, and given to third parties in any format or medium, without prior permission or charge, for personal research or study, educational, or not-for-pro t purposes provided that:• a full bibliographic reference is made to the original source • a link is made to the metadata record in DRO • the full-text is not changed in any way The full-text must not be sold in any format or medium without the formal permission of the copyright holders.Please consult the full DRO policy for further details. ABSTRACTWe quantify the correlations between gas-phase and stellar metallicities and global properties of galaxies, such as stellar mass, halo mass, age and gas fraction, in the Evolution and Assembly of GaLaxies and their Environments suite of cosmological hydrodynamical simulations. The slope of the correlation between stellar mass and metallicity of star-forming (SF) gas (M * -Z SF,gas relation) depends somewhat on resolution, with the higher resolution run reproducing a steeper slope. This simulation predicts a non-zero metallicity evolution, increasing by ≈0.5 dex at ∼10 9 M since z = 3. The simulated relation between stellar mass, metallicity and star formation rate at z 5 agrees remarkably well with the observed fundamental metallicity relation. At M * 10 10.3 M and fixed stellar mass, higher metallicities are associated with lower specific star formation rates, lower gas fractions and older stellar populations. On the other hand, at higher M * , there is a hint of an inversion of the dependence of metallicity on these parameters. The fundamental parameter that best correlates with the metal content, in the simulations, is the gas fraction. The simulated gas fraction-metallicity relation exhibits small scatter and does not evolve significantly since z = 3. In order to better understand the origin of these correlations, we analyse a set of lower resolution simulations in which feedback parameters are varied. We find that the slope of the simulated M * -Z SF,gas relation is mostly determined by stellar feedback at low stellar masses (M * 10 10 M ), and at high masses (M * 10 10 M ) by the feedback from active galactic nuclei.

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“…On the other hand, the approach used by Panter et al (2008) yields a mass fraction weighted metallicity. From Fig.…”

Section: The M * -Z * R E L At I O Nmentioning

confidence: 99%

Section: The M * -Z * R E L At I O Nmentioning

confidence: 99%

Galaxy metallicity scaling relations in the EAGLE simulations

Rossi

Bower

Font

et al. 2017

Monthly Notices of the Royal Astronomical Society

144

136

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show abstract

“…Disk-dominated galaxies contain <25%, while both types of galaxies contribute similarly to the total stellar mass density. 338 E. K. Grebel Panter et al (2008) derived the mass-fraction-weighted galaxian metallicity as a function of present-day stellar mass based on the analysis of > 300, 000 galaxies from the SDSS. Panter et al find a flat relation with little scatter (∼0.15 dex) around ∼1.1 Z for galaxies with masses 10 10.5 M .…”

Section: Mass-metallicity Relationsmentioning

confidence: 99%

“…Galaxies in high-density regions are generally found to have higher metallicities than those in low-density regions (see, e.g., Panter et al 2008). Sheth et al (2006) find that galaxies with above-average star formation rates and high metallicities at high redshifts are situated mainly in galaxy clusters in the present-day Universe.…”

Section: Environmental Trendsmentioning

confidence: 99%

Observational Comparison of Star Formation in Different Galaxy Types

Grebel

2010

Proc. IAU

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Abstract. Galaxies cover a wide range of masses and star formation histories. In this review, I summarize some of the evolutionary key features of common galaxy types. At the high-mass end, very rapid, efficient early star formation is observed, accompanied by strong enrichment and later quiescence, well-described by downsizing scenarios. In the intermediate-mass regime, early-type galaxies may still show activity in low-mass environments or when being rejuvenated by wet mergers. In late-type galaxies, we find continuous, though variable star formation over a Hubble time. In the dwarf regime, a wide range of properties from bursty activity to quiescence is observed. Generally, stochasticity dominates here, and star formation rates and efficiencies tend to be low. Morphological types and their star formation properties correlate with environment.

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“…For example, Trager & Somerville (2009) demonstrate a potentially important difference between the type of luminosity-weighting that we use and an SSP-weighting, which is more relevant for the Gallazzi et al (2005) spectral index calibrations (see also Panter et al 2008). Moreover, aperture bias, particularly for galaxies with both bulge and disk components, is partially responsible for the flattening of the mass-stellar metallicity relation in the SDSS measurements (Kauffmann et al 2003), and the choice of model metallicity grids (Koleva et al 2008) may also have a subtle effect.…”

Section: Uncertainties In the Model-data Comparisonmentioning

confidence: 99%

A framework for empirical galaxy phenomenology: the scatter in galaxy ages and stellar metallicities

Muñoz

Peeples

2015

Monthly Notices of the Royal Astronomical Society

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We develop a theoretical framework that extracts a deeper understanding of galaxy formation from empirically-derived relations among galaxy properties by extending the main-sequence integration method for computing galaxy star formation histories. We properly account for scatter in the stellar mass-star formation rate relation and the evolving fraction of passive systems and find that the latter effect is almost solely responsible for the age distributions among z ∼ 0 galaxies with stellar masses above ∼ 10 10 M ⊙ . However, while we qualitatively agree with the observed median stellar metallicity as a function of stellar mass, we attribute our inability to reproduce the distribution in detail largely to a combination of imperfect gas-phase metallicity and α/Fe ratio calibrations. Our formalism will benefit from new observational constraints and, in turn, improve interpretations of future data by providing self-consistent star formation histories for population synthesis modeling.

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The cosmic evolution of metallicity from the SDSS fossil record

Abstract: 11.02.13 KB. Accepted version ok to add to Spiral. RAS/Wiley/OU

Cited by 202 publications

References 41 publications

Galaxy metallicity scaling relations in the EAGLE simulations

Galaxy metallicity scaling relations in the EAGLE simulations

Observational Comparison of Star Formation in Different Galaxy Types

A framework for empirical galaxy phenomenology: the scatter in galaxy ages and stellar metallicities

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