A BUDGET AND ACCOUNTING OF METALS AT<i>z</i>∼ 0: RESULTS FROM THE COS-HALOS SURVEY

Peeples, Molly S.; Werk, Jessica K.; Tumlinson, Jason; Oppenheimer, Benjamin D.; Prochaska, J. Xavier; Katz, Neal; Weinberg, David H.

doi:10.1088/0004-637x/786/1/54

Cited by 336 publications

(441 citation statements)

References 151 publications

(215 reference statements)

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“…Naab et al 2014;Peeples et al 2014;Hirschmann et al 2013) and show passive evolution from z = 2. We find that 3 out of 9 BCGs in our sample have old central ages (> 12 Gyr), in agreement with this prediction.…”

Section: Stellar Agesmentioning

confidence: 99%

The accretion histories of brightest cluster galaxies from their stellar population gradients

Oliva-Altamirano

Brough

Jimmy

et al. 2015

Monthly Notices of the Royal Astronomical Society

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We analyse the spatially-resolved stellar populations of 9 local (z < 0.1) Brightest Cluster Galaxies (BCGs) observed with VIMOS in IFU mode. Our sample is composed of 7 slowrotating and 2 fast-rotating BCGs. We do not find a connection between stellar kinematics and stellar populations in this small sample. The BCGs have shallow metallicity gradients (medianand a wide range of central ages (from 5 to 15 Gyr). We propose that the reason for this is diverse evolutionary paths in BCGs. 67 per cent of the sample (6/9) show ∼ 7 Gyr old central ages, which reflects an active accretion history, and 33 per cent of the sample (3/9) have central ages older than 11 Gyr, which suggest no star formation since z = 2. The BCGs show similar central stellar populations and stellar population gradients to early-type galaxies of similar mass (M dyn > 10 11.3 M ) from the ATLAS 3D survey (median [Z/H] = 0.04 ± 0.07, ∆[Z/H] = −0.19 ± 0.1). However, massive early-type galaxies from ATLAS 3D have consistently old ages (median Age = 12.0 ± 3.8 Gyr). We also analyse the close massive companion galaxies of two of the BCGs. These galaxies have similar stellar populations to their respective BCGs.

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Section: Stellar Agesmentioning

confidence: 99%

The accretion histories of brightest cluster galaxies from their stellar population gradients

Oliva-Altamirano

Brough

Jimmy

et al. 2015

Monthly Notices of the Royal Astronomical Society

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“…Figure 10 shows that the density of dust in the hot halo and ejected reservoir is always higher than the density of dust in the cold gas, especially at redshifts z < 1.5. These predictions suggest that a large fraction of the dust (and metals) ever formed may be stored outside galaxies (Peeples et al 2014;Peek, Ménard & Corrales 2015). If we can quantify these reservoirs observationally (for instance through reddening studies around galaxies or by looking at absorbers along quasar lines of sight) , this will provide unique additional constraints for the ejective feedback recipes in galaxy formation models.…”

Section: Dust In the Hot Halo And Ejected Reservoirmentioning

confidence: 99%

“…Dust contributes significantly to the metals in the circumgalactic medium (CGM) and can be an additional cooling channel for gas (e.g. Ostriker & Silk 1973;Ménard et al 2010;Peeples et al 2014;Peek, Ménard & Corrales 2015).…”

Section: Introductionmentioning

confidence: 99%

The dust content of galaxies from z = 0 to z = 9

Popping

Somerville

Galametz

2017

Monthly Notices of the Royal Astronomical Society

237

326

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We study the dust content of galaxies from z = 0 to z = 9 in semi-analytic models of galaxy formation that include new recipes to track the production and destruction of dust. We include condensation of dust in stellar ejecta, the growth of dust in the interstellar medium (ISM), the destruction of dust by supernovae and in the hot halo, and dusty winds and inflows. The rate of dust growth in the ISM depends on the metallicity and density of molecular clouds. Our fiducial model reproduces the relation between dust mass and stellar mass from z = 0 to z = 7, the number density of galaxies with dust masses less than 10 8.3 M , and the cosmic density of dust at z = 0. The model accounts for the double power-law trend between dust-togas (DTG) ratio and gas-phase metallicity of local galaxies and the relation between DTG ratio and stellar mass. The dominant mode of dust formation is dust growth in the ISM, except for galaxies with M * < 10 7 M , where condensation of dust in supernova ejecta dominates. The dust-to-metal ratio of galaxies depends on the gasphase metallicity, unlike what is typically assumed in cosmological simulations. Model variants including higher condensation efficiencies, a fixed timescale for dust growth in the ISM, or no growth at all reproduce some of the observed constraints, but fail to simultaneously reproduce the shape of dust scaling relations and the dust mass of high-redshift galaxies.

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“…At z = 2, only about 50% of the metals produced by galaxies have been found in the galaxies themselves (Bouché et al 2006). At z = 0, a similarly small fraction of the metals produced by stars is accounted for within the ISM and stars alone (Peeples et al 2014) (hereafter P14). This is known as the galactic "missing metals problem".…”

Section: Introductionmentioning

confidence: 99%

Metal flows of the circumgalactic medium, and the metal budget in galactic haloes

Muratov

Kereš

Faucher-Giguère

et al. 2017

Monthly Notices of the Royal Astronomical Society

173

161

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We present an analysis of the flow of metals through the circumgalactic medium (CGM) in the Feedback in Realistic Environments (FIRE) simulations of galaxy formation, ranging from isolated dwarfs to L * galaxies. We find that nearly all metals produced in high-redshift galaxies are carried out in winds that reach 0.25R vir . When measured at 0.25R vir the metallicity of outflows is slightly higher than the interstellar medium (ISM) metallicity. Many metals thus reside in the CGM. Cooling and recycling from this reservoir determine the metal budget in the ISM. The outflowing metal flux decreases by a factor of ∼ 2 − 5 between 0.25R vir and R vir . Furthermore, outflow metallicity is typically lower at R vir owing to dilution of the remaining outflow by metal-poor material swept up from the CGM. The inflow metallicity at R vir is generally low, but outflow and inflow metallicities are similar in the inner halo. At low redshift, massive galaxies no longer generate outflows that reach the CGM, causing a divergence in CGM and ISM metallicity. Dwarf galaxies continue to generate outflows, although they preferentially retain metal ejecta. In all but the least massive galaxy considered, a majority of the metals are within the halo at z = 0. We measure the fraction of metals in CGM, ISM and stars, and quantify the thermal state of CGM metals in each halo. The total amount of metals in the low-redshift CGM of two simulated L * galaxies is consistent with estimates from the COS halos survey, while for the other two it appears to be lower.

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A BUDGET AND ACCOUNTING OF METALS ATz∼ 0: RESULTS FROM THE COS-HALOS SURVEY

Cited by 336 publications

References 151 publications

The accretion histories of brightest cluster galaxies from their stellar population gradients

The accretion histories of brightest cluster galaxies from their stellar population gradients

The dust content of galaxies from z = 0 to z = 9

Metal flows of the circumgalactic medium, and the metal budget in galactic haloes

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