The baryon content of groups and clusters of galaxies in the FABLE simulations

Henden, Nicholas A.; Puchwein, Ewald; Sijacki, Debora

doi:10.48550/arxiv.1911.12367

Cited by 5 publications

(9 citation statements)

References 182 publications

(430 reference statements)

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“…From the figure we see that our simulations tend to have too massive BCGs with respect to observational data (a factor of 2 at M 500 = 3 × 10 14 M ), in line with the findings of other groups (e.g., Bahé et al 2017, Pillepich et al 2018, Henden et al 2019. Moreover, current simulations have more massive BCGs than the LR simulations from Ragone-Figueroa et al ( 2018) (orange line in the plot), being a factor of 2.3 more massive at M 500 = 3 × 10 14 M .…”

Section: Bcg − M 500 Correlationsupporting

confidence: 90%

“…The main difference is around 10 10 M , were simulations have too many galaxies. As noted by Henden et al (2019), larger values of the softening length numerically decrease the number of galaxies at these masses. However, an investigation of the stellar feedback will be needed to better describe the GSMF at our low mass end.…”

Section: Galaxy Stellar Mass Functionmentioning

confidence: 56%

“…Similar results are also found by other groups. Henden et al (2019) made a similar analysis considering all the clusters with M 200 > 10 14 M and computed the instantaneous SFR within a spherical aperture of 30 kpc at z = 0.2. Their results show that their BCGs form stars at a rate similar to ours when they do not have a null SFR (see their Fig.…”

Section: Star Formation Rate Of Bgcsmentioning

confidence: 99%

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The DIANOGA simulations of galaxy clusters: characterizing star formation in proto-clusters

Bassini,

Rasia,

Borgani

et al. 2020

Preprint

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Aims. We studied the star formation rate (SFR) in cosmological hydrodynamical simulations of galaxy (proto-)clusters in the redshift range 0 < z < 4, comparing them to recent observational studies; we also investigated the effect of varying the parameters of the star formation model on galaxy properties such as SFR, star-formation efficiency, and gas fraction. Methods. We analyze a set of zoom-in cosmological hydrodynamical simulations centred on twelve clusters. The simulations are carried out with the GADGET-3 TreePM/SPH code which includes various subgrid models to treat unresolved baryonic physics, including AGN feedback. Results. Simulations do not reproduce the high values of SFR observed within protoclusters cores, where the values of SFR are underpredicted by a factor 4 both at z ∼ 2 and z ∼ 4. The difference arises as simulations are unable to reproduce the observed starburst population and is worsened at z ∼ 2 because simulations underpredict the normalization of the main sequence of star forming galaxies (i.e., the correlation between stellar mass and SFR) by a factor of ∼ 3. As the low normalization of the main sequence seems to be driven by an underestimated gas fraction, it remains unclear whether numerical simulations miss starburst galaxies due to a too low predicted gas fractions or too low star formation efficiencies. Our results are stable against varying several parameters of the star formation subgrid model and do not depend on the details of the AGN feedback.Conclusions. The subgrid model for star formation (Springel & Hernquist 2003), introduced to reproduce the self-regulated evolution of quiescent galaxies, is not suitable to describe violent events like high-redshift starbursts. We find that this conclusion holds independently of the parameters choice of the star formation and AGN models. The increasing amount of multi-wavelength high-redshift observations will help improving the current star formation model, in order to fully recover the observed star formation history of galaxy clusters.

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Section: Bcg − M 500 Correlationsupporting

confidence: 90%

Section: Galaxy Stellar Mass Functionmentioning

confidence: 56%

Section: Star Formation Rate Of Bgcsmentioning

confidence: 99%

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The DIANOGA simulations of galaxy clusters: characterizing star formation in proto-clusters

Bassini,

Rasia,

Borgani

et al. 2020

Preprint

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“…The amplitude of the baryonic mass fraction between 10 13 M and 10 14 M is nearly flat, and consistent with cluster observations (Gonzalez et al 2013;Decker et al 2019; also see Figure 3 of Tremmel et al 2019), while some other simulations predict a slightly steeper slope (Davies et al 2019;Chisari et al 2018b) or a higher (M gas /M tot ) (Henden et al 2019) on cluster mass scales. Le Brun et al (2014), however, show a cluster gas fraction (see Figure 3 in their paper) where observational and simulated trends are roughly consistent with the HR5 results.…”

Section: Fractional Mass Of Halossupporting

confidence: 82%

The Horizon Run 5 Cosmological Hydrodynamic Simulation: Probing Galaxy Formation from Kilo- to Giga-parsec Scales

Lee,

Shin,

Snaith

et al. 2020

Preprint

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Horizon Run 5 (HR5) is a cosmological hydrodynamics simulation which captures the properties of the Universe on a Gpc scale while achieving a resolution of 1 kpc. This enormous dynamic range allows us to simultaneously capture the physics of the cosmic web on very large scales and account for the formation and evolution of dwarf galaxies on much smaller scales. Inside the simulation box we zoom-in on a high-resolution cuboid region with a volume of 1049×114×114 Mpc 3 . The sub-grid physics chosen to model galaxy formation includes radiative heating/cooling, reionization, star formation, supernova feedback, chemical evolution tracking the enrichment of oxygen and iron, the growth of supermassive black holes and active galactic nuclei (AGN) feedback in the form of a dual jet-heating mode. For this simulation we implemented a hybrid MPI-OpenMP version of the RAMSES code, specifically targeted for modern many-core many thread parallel architectures. For the post-processing, we extended the Friends-of-Friend (FoF) algorithm and developed a new galaxy finder to analyse the large outputs of HR5. The simulation successfully reproduces many observations, such as the cosmic star formation history, connectivity of galaxy distribution and stellar mass functions. The simulation also indicates that hydrodynamical effects on small scales impact galaxy clustering up to very large scales near and beyond the baryonic acoustic oscillation (BAO) scale. Hence, caution should be taken when using that scale as a cosmic standard ruler: one should carefully understand the corresponding biases. The simulation is expected to be an invaluable asset for the interpretation of upcoming deep surveys of the Universe.

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“…Clusters of galaxies are expected to grow over time by accreting smaller groups. During the infall process, the material stripped from the galaxy outskirts builds up the intra-cluster light (ICL; see Napolitano et al 2003;Contini et al 2014;Cui et al 2014;Pillepich et al 2018;DeMaio et al 2018;Contini et al 2019;Henden et al 2019). The ICL is the fossil record of all past interactions and mergers.…”

Section: Introductionmentioning

confidence: 99%

The Fornax Deep Survey with VST. VIII. Connecting the accretion history with the cluster density

Spavone,

Iodice,

van de Ven

et al. 2020

Preprint

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Context. This work is based on deep multi-band (g, r, i) data from the Fornax Deep Survey (FDS) with the VLT Survey Telescope (VST). We analyse the surface brightness profiles of the 19 bright Early Type Galaxies (m B ≤ 15 mag) inside the virial radius of the Fornax cluster (R vir ∼ 0.7 Mpc), in the mass range 8 × 10 8 ≤ M * ≤ 1.2 × 10 11 M . Aims. The main aim of this work is to identify signatures of accretion onto galaxies by studying the presence of outer stellar halos, and understand their nature and occurrence. Our analysis also provides a new and accurate estimate of the intra-cluster light inside the virial radius of Fornax. Methods. We performed multi-component fits to the azimuthally averaged surface brightness profiles available for all sample galaxies. This allows to quantify the relative weight of all components in the galaxy structure that contribute to the total light. In addition, we derived the average g − i colours in each component identified by the fit, as well as the azimuthally averaged g − i colour profiles, to correlate them with the stellar mass of each galaxy and the location inside the cluster. Results. We find that in the most massive (10 10 ≤ M ≤ 10 11 M ) and reddest ETGs the fraction of light in, probably accreted, halos (50%-90%) is much larger than in the other galaxies. All of them are located in the high-density region of the cluster (≤ 0.4R vir ∼ 0.3 Mpc), belonging to the north-south clump. Less-massive galaxies (10 9 ≤ M ≤ 10 10 M ) have an accreted mass fraction lower than 30%, bluer colours and reside in the low-density regions of the cluster. The colour profiles of the ETGs with the largest accreted mass fraction tend to flatten in the galaxy's outskirts, i.e. beyond the transition radius from the central in-situ to the ex-situ accreted component. Inside the virial radius of the cluster (∼ 0.7 Mpc), the total luminosity of the intra-cluster light, compared with the total luminosity of all cluster members (bright galaxies as well as dwarfs), is about 34%. Conclusions. Inside the Fornax cluster there is a clear correlation between the amount of accreted material in the stellar halos of galaxies and the density of the environment in which those galaxies reside. By comparing this quantity with theoretical predictions and previous observational estimates, there is a clear indication that the driving factor for the accretion process is the total stellar mass of the galaxy, in agreement with the hierarchical accretion scenario. Massive galaxies in the north-south clump, with the largest accreted mass fractions, went through pre-processing in a group environment before this group merged with the main cluster early on. At the present epoch of the Fornax assembly history, they are the major contribution to the stellar density in the core of the cluster.

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The baryon content of groups and clusters of galaxies in the FABLE simulations

Cited by 5 publications

References 182 publications

The DIANOGA simulations of galaxy clusters: characterizing star formation in proto-clusters

The DIANOGA simulations of galaxy clusters: characterizing star formation in proto-clusters

The Horizon Run 5 Cosmological Hydrodynamic Simulation: Probing Galaxy Formation from Kilo- to Giga-parsec Scales

The Fornax Deep Survey with VST. VIII. Connecting the accretion history with the cluster density

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