Early-type Galaxy Spin Evolution in the Horizon-AGN Simulation

Choi, Hoseung; Yi, Sukyoung K.; Dubois, Yohan; Kimm, Taysun; Devriendt, Julien; Pichon, Christophe

doi:10.3847/1538-4357/aab08f

Cited by 39 publications

(39 citation statements)

References 69 publications

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“…Most galaxies, regardless of their stellar mass, show a decrease in V θ /σ after infall, as also demonstrated in Gnedin (2003b), Choi & Yi (2017) and Choi et al (2018). At a given mass, galaxies with higher Φ/∆t have V θ /σ smaller than those with lower Φ/∆t at both z = 0 and z infall .…”

Section: Stability Of Spin Vectors and V θ /σsupporting

confidence: 58%

Wobbling Galaxy Spin Axes in Dense Environments

Lee

Kim

Jeong

et al. 2018

ApJ

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The orientation of galaxy spin vectors within the large scale structure has been considered an important test of our understanding of structure formation. We investigate the angular changes of galaxy spin vectors in clusters -denser environments than are normally focused upon, using hydrodynamic zoomed simulations of 17 clusters YZiCS and a set of complementary controlled simulations. The magnitude by which galaxies change their spin vector is found to be a function of their rotational support with larger cumulative angular changes of spin vectors when they have initially lower V θ /σ. We find that both mergers and tidal perturbations can significantly swing spin vectors, with larger changes in spin vector for smaller pericentre distances. Strong tidal perturbations are also correlated with the changes in stellar mass and specific angular momentum of satellite galaxies. However, changes in spin vector can often result in a canceling out of previous changes. As a result, the integrated angular change is always much larger than the angular change measured at any instant. Also, overall the majority of satellite galaxies do not undergo mergers or sufficiently strong tidal perturbation after infall into clusters, and thus they end up suffering little change to their spin vectors. Taken as a whole, these results suggest that any signatures of spin alignment from the large scale structure will be preserved in the cluster environment for many gigayears.

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Section: Stability Of Spin Vectors and V θ /σsupporting

confidence: 58%

Wobbling Galaxy Spin Axes in Dense Environments

Lee

Kim

Jeong

et al. 2018

ApJ

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“…However, tidal interactions (or fly bys) between galaxies can produce similar effects to that due to actual mergers (e.g. Martin et al 2018a;Choi et al 2018). To explore the effect of tidal interactions on LSBGs and HSBGs, we employ a perturbation index (PI) which quantifies the environmental tidal field due to objects in the vicinity of the galaxy in question.…”

Section: Perturbations Due To the Ambient Tidal Field -A Key Driver Omentioning

confidence: 99%

The formation and evolution of low-surface-brightness galaxies

Martin

Kaviraj

Laigle

et al. 2019

Monthly Notices of the Royal Astronomical Society

119

123

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Our statistical understanding of galaxy evolution is fundamentally driven by objects that lie above the surface-brightness limits of current wide-area surveys (µ ∼ 23 mag arcsec −2 ). While both theory and small, deep surveys have hinted at a rich population of lowsurface-brightness galaxies (LSBGs) fainter than these limits, their formation remains poorly understood. We use Horizon-AGN, a cosmological hydrodynamical simulation to study how LSBGs, and in particular the population of ultra-diffuse galaxies (UDGs; µ > 24.5 mag arcsec −2 ), form and evolve over time. For M * >10 8 M , LSBGs contribute 47, 7 and 6 per cent of the local number, mass and luminosity densities respectively (∼85/11/10 per cent for M * >10 7 M ). Today's LSBGs have similar dark-matter fractions and angular momenta to high-surface-brightness galaxies (HSBGs; µ < 23 mag arcsec −2 ), but larger effective radii (×2.5 for UDGs) and lower fractions of dense, star-forming gas (more than ×6 less in UDGs than HSBGs). LSBGs originate from the same progenitors as HSBGs at z > 2. However, LSBG progenitors form stars more rapidly at early epochs. The higher resultant rate of supernova-energy injection flattens their gas-density profiles, which, in turn, creates shallower stellar profiles that are more susceptible to tidal processes. After z ∼ 1, tidal perturbations broaden LSBG stellar distributions and heat their cold gas, creating the diffuse, largely gas-poor LSBGs seen today. In clusters, ram-pressure stripping provides an additional mechanism that assists in gas removal in LSBG progenitors. Our results offer insights into the formation of a galaxy population that is central to a complete understanding of galaxy evolution, and which will be a key topic of research using new and forthcoming deep-wide surveys.

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“…Thus we have the ability to unveil new and important shortcomings of the simulations. Ellipticity has been explored in combination with V/σ and λ R (e.g., Naab et al 2014;Penoyre et al 2017;Choi et al 2018;Lagos et al 2018b;Schulze et al 2018), but here we have taken an additional step of comparing ellipticity distributions using massmatched samples. The offset towards thicker disks in eagle was also noticed by Trayford et al (2017) who found that the optical extinction is much smaller than observed for edge-on galaxies, but consistent for face-on objects.…”

Section: Comparing Observations and Simulations With Eagle Horizon-amentioning

confidence: 99%

“…The success of such an approach has already been demonstrated by Naab et al (2014), Welker et al (2017), Remus et al (2017), Penoyre et al (2017), Choi & Yi (2017), Choi et al (2018), Lagos et al (2018a,b), and Martin et al (2018). Naab et al (2014) use cosmological hydrodynamical zoom-in simulations of 44 individual central galaxies, and link the assembly history of these galaxies to their stellar dynamical features.…”

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confidence: 99%

The SAMI Galaxy Survey: comparing 3D spectroscopic observations with galaxies from cosmological hydrodynamical simulations

Sande

Lagos

Welker

et al. 2018

Monthly Notices of the Royal Astronomical Society

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Cosmological hydrodynamical simulations are rich tools to understand the build-up of stellar mass and angular momentum in galaxies, but require some level of calibration to observations. We compare predictions at z ∼ 0 from the eagle, hydrangea, horizon-agn, and magneticum simulations with integral field spectroscopic (IFS) data from the SAMI Galaxy Survey, ATLAS 3D , CALIFA and MASSIVE surveys. The main goal of this work is to simultaneously compare structural, dynamical, and stellar population measurements in order to identify key areas of success and tension. We have taken great care to ensure that our simulated measurement methods match the observational methods as closely as possible, and we construct samples that match the observed stellar mass distribution for the combined IFS sample. We find that the eagle and hydrangea simulations reproduce many galaxy relations but with some offsets at high stellar masses. There are moderate mismatches in R e (+), (−), σ e (−), and mean stellar age (+), where a plus sign indicates that quantities are too high on average, and minus sign too low. The horizon-agn simulations qualitatively reproduce several galaxy relations, but there are a number of properties where we find a quantitative offset to observations. Massive galaxies are better matched to observations than galaxies at low and intermediate masses. Overall, we find mismatches in R e (+), (−), σ e (−) and (V/σ) e (−). magneticum matches observations well: this is the only simulation where we find ellipticities typical for disk galaxies, but there are moderate differences in σ e (−), (V/σ) e (−) and mean stellar age (+). Our comparison between simulations and observational data has highlighted several areas for improvement, such as the need for improved modelling resulting in a better vertical disk structure, yet our results demonstrate the vast improvement of cosmological simulations in recent years.

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Early-type Galaxy Spin Evolution in the Horizon-AGN Simulation

Cited by 39 publications

References 69 publications

Wobbling Galaxy Spin Axes in Dense Environments

Wobbling Galaxy Spin Axes in Dense Environments

The formation and evolution of low-surface-brightness galaxies

The SAMI Galaxy Survey: comparing 3D spectroscopic observations with galaxies from cosmological hydrodynamical simulations

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