Characterising the intra-cluster light in The Three Hundred simulations

Contreras-Santos, A.; Knebe, A.; Cui, W.; Alonso Asensio, I.; Dalla Vecchia, C.; Cañas, R.; Haggar, R.; Mostoghiu Paun, R. A.; Pearce, F. R.; Rasia, E.

doi:10.1051/0004-6361/202348474

“…Despite the diversity (10%-30%) in ICL fractions among the GRT clusters, we find that the median ICL fraction for relaxed clusters (the solid red line) is higher compared to unrelaxed clusters (the solid blue line). This difference shows the possibility that the dynamical state of clusters can play a role in the ICL fraction of clusters, as suggested by both the observation and the theoretical studies (e.g., Da Rocha et al 2008;Montes & Trujillo 2018;Ragusa et al 2021Ragusa et al , 2023Contini et al 2023Contini et al , 2024Contreras-Santos et al 2024).…”

Section: Icl Detectionmentioning

confidence: 76%

Formation Channels of Diffuse Lights in Groups and Clusters over Time

Chun,

Shin,

Ko

et al. 2024

ApJ

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We explore the formation of the intragroup light and intracluster light, representing diffuse lights within groups and clusters, from the point that z = 1.5. For this, we perform multiresolution cosmological N-body simulations using the “galaxy replacement technique” and identify the progenitors in which the diffuse light stars existed when they fell into the groups or clusters. Our findings reveal that typical progenitors contributing to diffuse lights enter the host halo with massive galaxies containing a stellar mass of 10 < log M gal [ M ⊙ ] < 11 , regardless of the mass or dynamical state of the host halos at z = 0. In cases where the host halos are dynamically unrelaxed or more massive, diffuse lights from massive progenitors with log M gal [ M ⊙ ] > 11 are more prominent, with over half of them already preprocessed before entering the host halo. Additionally, we find that the main formation mechanism of diffuse lights is the stripping process of satellites, and a substantial fraction (40%–45%) of diffuse light stars are linked to the merger tree of the brightest cluster galaxy. Remarkably, all trends persist for groups and clusters at higher redshifts. The fraction of diffuse lights in the host halos with a similar mass decreases as the redshift increases, but they are already substantial at z = 1.5 (∼10%). However, it is crucial to acknowledge that detection limits related to the observable radius and faint-end surface brightness may obscure numerous diffuse light stars and even alter the main formation channel of diffuse lights.

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Characterizing tidal features around galaxies in cosmological simulations

Khalid,

Brough,

Martin

et al. 2024

Monthly Notices of the Royal Astronomical Society

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Tidal features provide signatures of recent mergers and offer a unique insight into the assembly history of galaxies. The Vera C. Rubin Observatory’s Legacy Survey of Space and Time (LSST) will enable an unprecedentedly large survey of tidal features around millions of galaxies. To decipher the contributions of mergers to galaxy evolution it will be necessary to compare the observed tidal features with theoretical predictions. Therefore, we use cosmological hydrodynamical simulations NewHorizon, eagle, IllustrisTNG, and Magneticum to produce LSST-like mock images of z ∼ 0 galaxies (z ∼ 0.2 for NewHorizon) with $M_{\scriptstyle \star ,\text{ 30 pkpc}}\ge 10^{9.5}$ M$_{\scriptstyle \odot }$. We perform a visual classification to identify tidal features and classify their morphology. We find broadly good agreement between the simulations regarding their overall tidal feature fractions: $f_{\small {\rm NEWHORIZON}}=0.40\pm 0.06$, $f_{\small {\rm EAGLE}}=0.37\pm 0.01$, $f_{\small {\rm TNG}}=0.32\pm 0.01$ and $f_{\small {\rm MAGNETICUM}}=0.32\pm 0.01$, and their specific tidal feature fractions. Furthermore, we find excellent agreement regarding the trends of tidal feature fraction with stellar and halo mass. All simulations agree in predicting that the majority of central galaxies of groups and clusters exhibit at least one tidal feature, while the satellite members rarely show such features. This agreement suggests that gravity is the primary driver of the occurrence of visually-identifiable tidal features in cosmological simulations, rather than subgrid physics or hydrodynamics. All predictions can be verified directly with LSST observations.

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Assembly of the intracluster light in the Horizon-AGN simulation

Brown,

Martin,

Pearce

et al. 2024

Monthly Notices of the Royal Astronomical Society

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The diffuse stellar component of galaxy clusters made up of intergalactic stars is termed the intracluster light (ICL). Although there is a developing understanding of the mechanisms by which the ICL is formed, no strong consensus has yet been reached on which objects the stars of the ICL are primarily sourced from. We investigate the assembly of the ICL starting approximately 10 Gyr before $z=0$ in 11 galaxy clusters (halo masses between $\sim 1\times 10^{14}$ and $\sim 7\times 10^{14}$ M$_{\odot }$ at $z\approx 0$) in the Horizon-AGN simulation. By tracking the stars of galaxies that fall into these clusters past cluster infall, we are able to link almost all of the $z\approx 0$ ICL back to progenitor objects. Satellite stripping, mergers, and pre-processing are all found to make significant contributions to the ICL, but any contribution from in situ star formation directly into the ICL appears negligible. Even after compensating for resolution effects, we find that approximately 90 per cent of the stacked ICL of the 11 clusters that is not pre-processed should come from galaxies infalling with stellar masses above $10^{9}$ M$_{\odot }$, with roughly half coming from infalling galaxies with stellar masses within half a dex of $10^{11}$ M$_{\odot }$. The fact that the ICL appears largely sourced from such massive objects suggests that the ICL assembly of any individual cluster may be principally stochastic.

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Characterising the intra-cluster light in The Three Hundred simulations

Cited by 5 publications

References 125 publications

Formation Channels of Diffuse Lights in Groups and Clusters over Time

Formation Channels of Diffuse Lights in Groups and Clusters over Time

Characterizing tidal features around galaxies in cosmological simulations

Assembly of the intracluster light in the Horizon-AGN simulation

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