Properties of galaxies reproduced by a hydrodynamic simulation

Vogelsberger, Mark; Genel, Shy; Springel, Volker; Torrey, Paul; Sijacki, Debora; Xu, D.; Snyder, Gregory F.; Bird, Simeon; Nelson, Dylan; Hernquist, Lars

doi:10.1038/nature13316

Cited by 1,216 publications

(1,005 citation statements)

References 68 publications

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“…In preliminary work, we conducted a simple proof-of-concept to combine our Thin lightcone geometries with the spectral synthesis code Sunrise (Jonsson 2006;Jonsson et al 2010), and we will release these initial synthetic images to the community. For example, Vogelsberger et al (2014a) used these to compare the Illustris to the HST Ultra Deep Field. Similarly, Kaviraj et al (2016) presented a lightcone image from the Horizon-AGN simulation (e.g., Dubois et al 2014).…”

Section: Discussion and Summarymentioning

confidence: 99%

“…The three Wide fields together total ∼ 410 arcmin 2 , about half the area surveyed by CANDELS-Wide (Grogin et al 2011;Koekemoer et al 2011). Each Thin lightcone is ∼ 8 arcmin 2 , a little smaller than the Hubble Space Telescope Ultra Deep Field (11 arcmin 2 Beckwith et al 2006), and we used these to create the synthetic Deep Fields for Illustris (Vogelsberger et al 2014b). For our investigation into pair statistics in this Section, we use the Wide lightcones.…”

Section: Catalog Synthesis and Pair Countingmentioning

confidence: 99%

“…We define δ with a technique based on the three-dimensional distance to the fifth nearest tracer, similar to Vogelsberger et al (2014a). First, the density field is smoothed by a three-dimensional Gaussian function with σ equal to the distance to the 5th nearest tracer galaxy with r-band absolute magnitude mr −19.5.…”

Section: Local Environments Of Massive Pairsmentioning

confidence: 99%

“…The recent emergence of relatively large (∼ 100 Mpc) hydrodynamical simulations with moderate resolution (∼ 1 kpc) and accuracy offers an opportunity to refine our assumptions about galaxy merger observability timescales (e.g., Dubois et al 2014;Khandai et al 2015;Schaye et al 2014;Vogelsberger et al 2014a). Their cosmological sizes allow us to convert these simulations into mock catalogs in the same way as has been done for several years using semianalytic and semi-empirical models, for example by using the lightcone technique to create mock galaxy catalogs as a function of angular coordinates and redshift (e. Bernyk et al 2016;Overzier et al 2013;TaghizadehPopp et al 2015).…”

Section: Introductionmentioning

confidence: 99%

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Massive close pairs measure rapid galaxy assembly in mergers at high redshift

Snyder

Lotz

Rodríguez-Gómez

et al. 2017

Monthly Notices of the Royal Astronomical Society

136

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We compare mass-selected close pairs at z > 1 with the intrinsic galaxy merger rate in the Illustris Simulations. To do so, we construct three 140 arcmin 2 lightcone catalogs and measure pair fractions, finding that they change little or decrease with increasing redshift at z > 1. Consistent with current surveys, this trend requires a decrease in the merger-pair observability time, roughly as τ ∝ (1 + z) −2 , in order to measure the merger rates of the same galaxies. This implies that major mergers are more common at high redshift than implied by the simplest arguments assuming a constant observability time. Several effects contribute to this trend: (1) The fraction of massive, major (4:1) pairs which merge by today increases weakly from ∼ 0.5 at z = 1 to ∼ 0.8 at z = 3. (2) The median time elapsed between an observed pair and final remnant decreases by a factor of two from z ∼ 1 to z ∼ 3. (3) An increasing specific star formation rate (sSFR) decreases the time during which common stellarmass based pair selection criteria could identify the mergers. The average orbit of the pairs at observation time varies only weakly, suggesting that the dynamical time is not varying enough to account by itself for the pair fraction trends. Merging pairs reside in dense regions, having overdensity δ ∼ 10 to ∼ 100 times greater than the average massive galaxy. We forward model the pairs to reconstruct the merger remnant production rate, showing that it is consistent with a rapid increase in galaxy merger rates at z > 1.

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Section: Discussion and Summarymentioning

confidence: 99%

Section: Catalog Synthesis and Pair Countingmentioning

confidence: 99%

Section: Local Environments Of Massive Pairsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

Massive close pairs measure rapid galaxy assembly in mergers at high redshift

Snyder

Lotz

Rodríguez-Gómez

et al. 2017

Monthly Notices of the Royal Astronomical Society

136

View full text Add to dashboard Cite

show abstract

“…The formation of the stellar bulge and black hole are modelled quite independently in the Illustris simulation and hence relations between these two components may be taken as predictions rather than necessary consequences of the implementation, unlike in many semi-analytic models. Full details on the prescriptions for black hole growth in Illustris are given in Vogelsberger et al (2013Vogelsberger et al ( , 2014a. As with L-Galaxies, the radio mode AGN feedback prescription in Illustris leads to a quenching probability which is primarily a function of black hole mass, i.e.…”

Section: Details On Illustris and L-galaxiesmentioning

confidence: 99%

The impact of galactic properties and environment on the quenching of central and satellite galaxies: a comparison between SDSS, Illustris and L-Galaxies

Bluck

Mendel

Ellison

et al. 2016

Mon. Not. R. Astron. Soc.

135

226

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We quantify the impact that a variety of galactic and environmental properties have on the quenching of star formation. We collate a sample of ∼ 400,000 central and ∼ 100,000 satellite galaxies from the Sloan Digital Sky Survey Data Release 7 (SDSS DR7). Specifically, we consider central velocity dispersion (σ c ), stellar, halo, bulge and disk mass, local density, bulge-to-total ratio, group-centric distance and galaxy-halo mass ratio. We develop and apply a new statistical technique to quantify the impact on the quenched fraction (f Quench ) of varying one parameter, while keeping the remaining parameters fixed. For centrals, we find that the f Quench − σ c relationship is tighter and steeper than for any other variable considered. We compare to the Illustris hydrodynamical simulation and the Munich semi-analytic model (L-Galaxies), finding that our results for centrals are qualitatively consistent with their predictions for quenching via radio-mode AGN feedback, hinting at the viability of this process in explaining our observational trends. However, we also find evidence that quenching in L-Galaxies is too efficient and quenching in Illustris is not efficient enough, compared to observations. For satellites, we find strong evidence that environment affects their quenched fraction at fixed central velocity dispersion, particularly at lower masses. At higher masses, satellites behave identically to centrals in their quenching. Of the environmental parameters considered, local density affects the quenched fraction of satellites the most at fixed central velocity dispersion.

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Simulated X‐ray emission in galaxy clusters with feedback from active galactic nuclei

et al. 2021

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To investigate the effect of feedback from active galactic nuclei (AGN) on their surrounding medium, we study the diffuse X-ray emission from galaxy groups and clusters by coupling the Astrophysical Plasma Emission Code (APEC) with the cosmological hydrodynamic simulation involving AGN feedback. We construct a statistical sample of synthetic Chandra X-ray photon maps to observationally characterize the effect of AGN on the ambient medium. We show that AGN are effective in displacing the hot X-ray emitting gas from the centers of groups and clusters, and that these signatures remain evident in observations of the X-ray surface brightness profiles.

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Properties of galaxies reproduced by a hydrodynamic simulation

Cited by 1,216 publications

References 68 publications

Massive close pairs measure rapid galaxy assembly in mergers at high redshift

Massive close pairs measure rapid galaxy assembly in mergers at high redshift

The impact of galactic properties and environment on the quenching of central and satellite galaxies: a comparison between SDSS, Illustris and L-Galaxies

Simulated X‐ray emission in galaxy clusters with feedback from active galactic nuclei

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