COLD-MODE ACCRETION: DRIVING THE FUNDAMENTAL MASS–METALLICITY RELATION AT z ∼ 2

Kacprzak, Glenn G.; Voort, Freeke van de; Glazebrook, Karl; Tran, Kim‐Vy H.; Yuan, Tiantian; Nanayakkara, Themiya; Allen, Rebecca J.; Alcorn, Leo Y.; Cowley, Michael J.; Labbé, Ivo; Spitler, Lee R.; Straatman, Caroline; Tomczak, Adam

doi:10.3847/2041-8205/826/1/l11

Cited by 60 publications

(67 citation statements)

References 52 publications

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“…They also find that satellite galaxies have higher metallicity for the same stellar mass, as it is indeed observed (Pasquali et al, 2012). Kacprzak et al (2016) find galaxies at redshift around 2 following the FMR. They show that the gas masses and metallicities required to reproduce the observed FMR are consistent with cold-accretion predictions obtained from their hydrodynamical simulations.…”

Section: Figsupporting

confidence: 66%

Gas Accretion and Star Formation Rates

Alméida

2017

Gas Accretion Onto Galaxies

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Cosmological numerical simulations of galaxy evolution show that accretion of metal-poor gas from the cosmic web drives the star formation in galaxy disks. Unfortunately, the observational support for this theoretical prediction is still indirect, and modeling and analysis are required to identify hints as actual signs of star-formation feeding from metal-poor gas accretion. Thus, a meticulous interpretation of the observations is crucial, and this observational review begins with a simple theoretical description of the physical process and the key ingredients it involves, including the properties of the accreted gas and of the star-formation that it induces. A number of observations pointing out the connection between metalpoor gas accretion and star-formation are analyzed, specifically, the short gas consumption time-scale compared to the age of the stellar populations, the fundamental metallicity relationship, the relationship between disk morphology and gas metallicity, the existence of metallicity drops in starbursts of star-forming galaxies, the socalled G dwarf problem, the existence of a minimum metallicity for the star-forming gas in the local universe, the origin of the α-enhanced gas forming stars in the local universe, the metallicity of the quiescent BCDs, and the direct measurements of gas accretion onto galaxies. A final section discusses intrinsic difficulties to obtain direct observational evidence, and points out alternative observational pathways to further consolidate the current ideas.

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Section: Figsupporting

confidence: 66%

Gas Accretion and Star Formation Rates

Alméida

2017

Gas Accretion Onto Galaxies

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“…These studies have been extended at different z by many authors in recent years (e.g. Cresci et al 2012;Hunt et al 2012;Henry et al 2013;LaraLópez, López-Sánchez & Hopkins 2013;Stott et al 2013;Cullen et al 2014;Maier et al 2014;Nakajima & Ouchi 2014;Zahid et al 2014a;Bothwell et al 2016a;Kacprzak et al 2016) but, as in the case of the MZR, the large uncertainties and diverse observational techniques involved in observational works prevent convergence towards a clear determination of these FMRs of galaxies, as discussed by Telford et al (2016).…”

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 mass of this halo is comparable to the gas mass of the galaxy itself (i.e., the ISM; Thom et al 2011;Tumlinson et al 2011;Werk et al 2013) and hence plays an important role in the evolution of galaxies. Models of the CGM indicate that gas can flow in and out of this reservoir, which in turn controls the star formation rate of the galaxy and the metallicity of stars formed from this gas (Oppenheimer & Davé 2008;Lilly et al 2013;Kacprzak et al 2016). While a more concrete model of how this gas drives isolated galaxy evolution is being built, we are still only just beginning to study the effects an interaction or merger can have on the CGM.…”

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confidence: 99%

The Impact of the Group Environment on the O vi Circumgalactic Medium

Pointon

Nielsen

Kacprzak

et al. 2017

ApJ

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We present a study comparing O VI λλ1031, 1037 doublet absorption found towards group galaxy environments with that of isolated galaxies. The O VI absorption in the circumgalactic medium (CGM) of isolated galaxies has been studied previously by the "Multiphase Galaxy Halos" survey, where the kinematics and absorption properties of the CGM have been investigated. We extend these studies to group environments. We define a galaxy group to have two or more galaxies having a line-of-sight velocity difference of no more than 1000 km s −1 and located within 350 kpc (projected) of a background quasar sightline. We identified a total of six galaxy groups associated with O VI absorption W r > 0.06 Å that have a median redshift of z gal = 0.1669 and a median impact parameter of D = 134.1 kpc. An additional 12 non-absorbing groups were identified with a median redshift of z gal = 0.2690 and a median impact parameter of D = 274.0 kpc. We find the average equivalent width to be smaller for group galaxies than for isolated galaxies (3σ). However, the covering fractions are consistent with both samples. We used the pixel-velocity two-point correlation function method and find that the velocity spread of O VI in the CGM of group galaxies is significantly narrower than that of isolated galaxies (10σ). We suggest that the warm/hot CGM does not exist as a superposition of halos, instead, the virial temperature of the halo is hot enough for O VI to be further ionised. The remaining O VI likely exists at the interface between hot, diffuse gas and cooler regions of the CGM.

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COLD-MODE ACCRETION: DRIVING THE FUNDAMENTAL MASS–METALLICITY RELATION AT z ∼ 2

Cited by 60 publications

References 52 publications

Gas Accretion and Star Formation Rates

Gas Accretion and Star Formation Rates

Galaxy metallicity scaling relations in the EAGLE simulations

The Impact of the Group Environment on the O vi Circumgalactic Medium

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