The evolution of the mass-metallicity relation in galaxies of different morphological types

Calura, F.; Pipino, A.; Chiappini, Cristina; Matteuccí, F.; Maiolino, R.

doi:10.1051/0004-6361/200911756

Cited by 133 publications

(161 citation statements)

References 87 publications

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“…Without energy injection from supernovae to regulate the star formation, gas that remains in galaxies rapidly cools, forms stars, and increases its metallicity too early, producing a M − Z relation too flat compared to observations. However, Calura et al (2009) reproduced the M − Z relation with chemical evolution models for ellipticals, spirals and irregular galaxies, by means of an increasing efficiency of star formation with mass in galaxies of all morphological types, without the need for outflows favoring the loss of metals in the less massive galaxies. A recent study that supports this result for massive galaxies is that of Vale Asari et al (2009), modelling the time evolution of stellar metallicity using a closed-box chemical evolution model.…”

Section: Effect Of the Mass And Luminosity-metallicity Relationsmentioning

confidence: 81%

Study of star-forming galaxies in SDSS up to redshift 0.4

Lara-López¹,

Cepa

Bongiovanni³

et al. 2009

A&A

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Context. The chemical composition of the gas in galaxies over cosmic time provides a very important tool for understanding galaxy evolution. Although there are many studies at high redshift, they are rather scarce at lower redshifts. However, low redshift studies can provide important clues about the evolution of galaxies, furnishing the required link between the local and high redshift universe. In this work, we focus on the metallicity of the gas of star-forming galaxies at low redshift, looking for signs of chemical evolution.Aims. We aim to analyze the metallicity contents star-forming galaxies of similar luminosities and masses at different redshifts. With this purpose, we present a study of the metallicity of relatively massive (log(M star /M ) 10.5) star forming galaxies from SDSS-DR5 (Sloan Digital Sky Survey-data release 5), using different redshift intervals from 0.04 to 0.4. Methods. We used data processed with the STARLIGHT spectral synthesis code, correcting the fluxes for dust extinction, estimating metallicities using the R 23 method, and segregating the samples with respect to the value of the [N ii] λ6583/[O ii] λ3727 line ratio in order to break the R 23 degeneracy selecting the upper branch. We analyze the luminosity and mass-metallicity relations, and the effect of the Sloan fiber diameter looking for possible biases. Results. By dividing our redshift samples in intervals of similar magnitude and comparing them, significant signs of metallicity evolution are found. Metallicity correlates inversely with redshift: from redshift 0 to 0.4 a decrement of ∼0.1 dex in 12 + log(O/H) is found.

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Section: Effect Of the Mass And Luminosity-metallicity Relationsmentioning

confidence: 81%

Study of star-forming galaxies in SDSS up to redshift 0.4

Lara-López¹,

Cepa

Bongiovanni³

et al. 2009

A&A

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“…Besides, less efficient star formation in low-mass galaxies could also cause the lower chemical enrichment of smaller galaxies and explain the origin of the MZR (e.g. Brooks et al 2007; Mouhcine et al 2008;Calura et al 2009). The evolution of the MZR could also be affected by the different SF histories associated with galaxies with different morphologies (see e.g.…”

Section: Introductionmentioning

confidence: 99%

“…The evolution of the MZR could also be affected by the different SF histories associated with galaxies with different morphologies (see e.g. Calura et al 2009). In addition, the infall of metal-poor gas on to the outer parts of galaxies or inflows triggered by mergers with other systems could play an important role (e.g.…”

Section: Introductionmentioning

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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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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“…The second one is the correlation between the metallicity and kinematics (Wolfe & Prochaska 1998;Ledoux et al 2006;Prochaska, Hennawi, & Herbert-Fort 2008;Neeleman et al 2013), which is largely due to the underlying massmetallicity relation that has been well-established in galaxies at high and low redshifts (Tremonti et al 2004;Savaglio et al 2005;Erb et al 2006;Maiolino et al 2008;Møller et al 2013;Neeleman et al 2013). The correlations between metallicity and other fundamental parameters such as stellar mass and star formation rate are key to understanding various galaxy populations (Calura et al 2009;Mannucci et al 2010).…”

Section: Introductionmentioning

confidence: 99%

Quasar 2175 Å dust absorbers – II. Correlation analysis and relationship with other absorption line systems

Prochaska

et al. 2017

Monthly Notices of the Royal Astronomical Society

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We present the cold neutral content (H i and C i gas) of 13 quasar 2175Å dust absorbers (2DAs) at z = 1.6 -2.5 to investigate the correlation between the presence of the UV extinction bump with other physical characteristics. These 2DAs were initially selected from the Sloan Digital Sky Surveys I -III and followed up with the Keck-II telescope and the Multiple Mirror Telescope as detailed in our Paper I. We perform a correlation analysis between metallicity, redshift, depletion level, velocity width, and explore relationships between 2DAs and other absorption line systems. The 2DAs on average have higher metallicity, higher depletion levels, and larger velocity widths than Damped Lyman-α absorbers (DLAs) or subDLAs. The correlation between [Zn/H] and [Fe/Zn] or [Zn/H] and log∆V 90 can be used as alternative stellar mass estimators based on the well-established mass-metallicity relation. The estimated stellar masses of the 2DAs in this sample are in the range of ∼ 10 9 to ∼2 × 10 11 M ⊙ with a median value of ∼2 × 10 10 M ⊙ . The relationship with other quasar absorption line systems can be described as (1) 2DAs are a subset of Mg ii and Fe ii absorbers, (2) 2DAs are preferentially metal-strong DLAs/subDLAs, (3) More importantly, all of the 2DAs show C i detections with logN(C i) > 14.0 cm −2 , (4) 2DAs can be used as molecular gas tracers. Their host galaxies are likely to be chemically enriched, evolved, massive (more massive than typical DLA/subDLA galaxies), and presumably star-forming galaxies.

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The evolution of the mass-metallicity relation in galaxies of different morphological types

Cited by 133 publications

References 87 publications

Study of star-forming galaxies in SDSS up to redshift 0.4

Study of star-forming galaxies in SDSS up to redshift 0.4

Galaxy metallicity scaling relations in the EAGLE simulations

Quasar 2175 Å dust absorbers – II. Correlation analysis and relationship with other absorption line systems

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