The Argo simulation – I. Quenching of massive galaxies at high redshift as a result of cosmological starvation

Feldmann, Robert; Mayer, Lucio

doi:10.1093/mnras/stu2207

Cited by 119 publications

(95 citation statements)

References 209 publications

(255 reference statements)

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“…While these are fundamental observations of galaxy evolution, a consensus has yet to be reached about the physical processes that dictate them. The anti-hierarchical quenching of galaxies and AGN might be partially caused by stable virial shocks and gravitational heating due to infalling galaxies (e.g., Feldmann & Mayer 2015), but most successful models invoke additional energy input, most likely from AGNs. In fact, strong quasar activity is known to launch rapid outflows of gas, and powerful radio jets are observed to play an important role in galaxy clusters, but the total energy released by these processes as a function of redshift and environment remains largely unknown.…”

Section: Discussionmentioning

confidence: 99%

Constraining Agn Feedback in Massive Ellipticals With South Pole Telescope Measurements of the Thermal Sunyaev–zel’dovich Effect

Spacek

Scannapieco

Cohen

et al. 2016

ApJ

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Energetic feedback due to active galactic nuclei (AGNs) is likely to play an important role in the observed antihierarchical trend in the evolution of galaxies, and yet the energy injected into the circumgalactic medium by this process is largely unknown. One promising approach to constrain this feedback is through measurements of spectral distortions in the cosmic microwave background due to the thermal Sunyaev-Zeldovich (tSZ) effect, whose magnitude is directly proportional to the energy input by AGNs. With current instruments, making such measurements requires stacking large numbers of objects to increase signal-to-noise. While one possible target for such stacks is AGNs themselves, these are relatively scarce sources that contain contaminating emission that complicates tSZ measurements. Here we adopt an alternative approach and co-add South Pole Telescope SZ (SPT-SZ) survey data around a large set of massive quiescent elliptical galaxies at  z 0.5, which are much more numerous and less contaminated than active AGNs, yet are subject to the same feedback processes from the AGNs they hosted in the past. We use data from the Blanco Cosmology Survey and VISTA Hemisphere Survey to create a large catalog of galaxies split up into two redshift bins: one with 3394 galaxies at   z 0.5 1.0 and one with 924 galaxies at   z 1.0 1.5, with typical stellar masses of´ M 1.5 10 . 11We then co-add the emission around these galaxies, resulting in a measured tSZ signal at s 2.2 significance for the lower redshift bin and a contaminating signal at s 1.1 for the higher redshift bin. To remove contamination due to dust emission, we use SPT-SZ source counts to model a contaminant source population in both the SPT-SZ bands and Planck highfrequency bands for a subset of 937 galaxies in the low-redshift bin and 240 galaxies in the high-redshift bin. This increases our detection to s 3.6 for low redshifts and s 0.9 for high redshifts. We find the mean angularly integrated Compton-y values to be- 60 erg, respectively. These numbers are higher than expected from simple theoretical models that do not include AGN feedback, and serve as constraints that can be applied to current simulations of massive galaxy formation.

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Section: Discussionmentioning

confidence: 99%

Constraining Agn Feedback in Massive Ellipticals With South Pole Telescope Measurements of the Thermal Sunyaev–zel’dovich Effect

Spacek

Scannapieco

Cohen

et al. 2016

ApJ

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“…Simple stability arguments predict that such gas-rich galaxies are also prone to stronger gravitational instabilities, and thus favor more rapid compaction, and hence quenching, processes. In such case, the downward tilt in Figure 7 could be due to gas starvation after an instabilityinduced starburst, i.e., a wet inflow that causes a peak in the SFR at the maximum gas density and declines progressively with the gas supply, while the core mass increases (see, e.g., Feldmann & Mayer 2015;Zolotov et al 2015in simulations and Ikarashi et al 2015and Barro et al 2016 for recent observations of compact nuclear starburst at z 2 ). The truncation of the gas DS (right) for all massive galaxies at z 0.5 3 < < , color-coded by the Sérsic index.…”

Section: A Redshift-independent Sequence Relating Galaxy Structure Anmentioning

confidence: 98%

Structural and Star-forming Relations since z ∼ 3: Connecting Compact Star-forming and Quiescent Galaxies

Barro

Faber

Koo

et al. 2017

ApJ

271

384

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We study the evolution of the scaling relations that compare the effective density ( r r , e e S < ) and core density ( r , 1 1 S < kpc) to the stellar masses of star-forming galaxies (SFGs) and quiescent galaxies. These relations have been fully in place since z 3 and have exhibited almost constant slope and scatter since that time. For SFGs, the zero points in e S and 1 S decline by only 2 . This fact plus the narrowness of the relations suggests that galaxies could evolve roughly along the scaling relations. Quiescent galaxies follow different scaling relations that are offset to higher densities at the same mass and redshift. Furthermore, the zero point of their core density has declined by only 2 since z 3 , while the zero point of the effective density declines by 10 . When galaxies quench, they move from the star-forming relations to the quiescent relations. This involves an increase in the core and effective densities, which suggests that SFGs could experience a phase of significant core growth relative to the average evolution along the structural relations. The distribution of massive galaxies relative to the SFR-M and the quiescent M  Srelations exhibits an L-shape that is independent of redshift. The knee of this relation consists of a subset of "compact" SFGs that are the most likely precursors of quiescent galaxies forming at later times. The compactness selection threshold in 1 S exhibits a small variation from z=3 to 0.5, M 0.65 log 10.5 9.6 9.3 1 * S --> -( ) M e kpc −2 , allowing the most efficient identification of compact SFGs and quiescent galaxies at every redshift.

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“…Conversely, even halos with low accretion rates are expected to contain significant hot gas components, which can in principle provide fuel for star formation. Hydrodynamic simulations are necessary to investigate whether low halo accretion rates can be a significant factor in the quenching of central galaxies over the redshift range where conformity is now known to exist; Feldmann & Mayer (2014) have recently demonstrated this at z 2 > , but their simulations do not extend to lower redshift.…”

Section: Physical Causes Of Conformitymentioning

confidence: 99%

SATELLITE QUENCHING AND GALACTIC CONFORMITY AT 0.3 < z < 2.5*

Kawinwanichakij

Quadri

Papovich

et al. 2016

ApJ

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We measure the evolution of the quiescent fraction and quenching efficiency of satellites around star-forming and quiescent central galaxies with stellar mass M M log 10.5. We combine imaging from three deep near-infrared-selected surveys (ZFOURGE/CANDELS, Ultra Deep Survey, and UltraVISTA), which allows us to select a stellar-mass complete sample of satellites with. Satellites for both starforming and quiescent central galaxies ("centrals") have higher quiescent fractions compared to field galaxies matched in stellar mass at all redshifts. We also observe "galactic conformity": satellites around quiescent centrals are more likely to be quenched compared to the satellites around star-forming centrals. In our sample, this conformity signal is significant at 3  s for z 0.6 1.6 < < , whereas it is only weakly significant at z 0.3 0.6 < < and z 1.6 2.5 < <. Therefore, conformity (and thus satellite quenching) has been present for a significant fraction of the age of the universe. The satellite quenching efficiency increases with increasing stellar mass of the central, but does not appear to depend on the stellar mass of the satellite to the mass limit of our sample. When we compare the satellite quenching efficiency of star-forming centrals with stellar masses 0.2 dex higher than quiescent centrals (which should account for any difference in halo mass), the conformity signal decreases, but remains statistically significant at z 0.6 0.9 < < . This is evidence that satellite quenching is connected to the star formation properties of the central galaxy as well as to the mass of the halo. We discuss physical effects that may contribute to galactic conformity, and emphasize that they must allow for continued star formation in the central galaxy even as the satellites are quenched.

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The Argo simulation – I. Quenching of massive galaxies at high redshift as a result of cosmological starvation

Cited by 119 publications

References 209 publications

Constraining Agn Feedback in Massive Ellipticals With South Pole Telescope Measurements of the Thermal Sunyaev–zel’dovich Effect

Constraining Agn Feedback in Massive Ellipticals With South Pole Telescope Measurements of the Thermal Sunyaev–zel’dovich Effect

Structural and Star-forming Relations since z ∼ 3: Connecting Compact Star-forming and Quiescent Galaxies

SATELLITE QUENCHING AND GALACTIC CONFORMITY AT 0.3 < z < 2.5*

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