The Preferential Tidal Stripping of Dark Matter Versus Stars in Galaxies

Smith, Rory; Choi, Hoseung; Lee, Jae-Hyun; Rhee, Jinsu; Sánchéz-Janssen, R.; Yi, Sukyoung K.

doi:10.3847/1538-4357/833/1/109

Cited by 108 publications

(133 citation statements)

References 67 publications

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“…The figure shows that galaxies that have lost < 90% of the maximum dark matter mass still retain > 90% of their maximum stellar mass. These results are broadly consistent with work by Smith et al (2016) who showed that galaxies around clusters that lose ∼ 80% of their dark matter mass only lose ∼ 10% of their stellar mass. Our results are not directly comparable since we do not follow the galaxies' particles from peak to z = 0 in the same way as Smith et al (2016).…”

Section: Radial Trajectoriessupporting

confidence: 92%

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The trajectories of galaxies in groups: mass-loss and preprocessing

Joshi

Parker

Wadsley

et al. 2018

Monthly Notices of the Royal Astronomical Society

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We present a study of environmental effects and preprocessing in a large galaxy group using a high-resolution, zoom-in simulation run with the gasoline2 hydrodynamics code. We categorize galaxies that were always in distinct haloes as unaccreted, galaxies that were distinct before accretion onto the main group as single, and galaxies that were in external sub-groups before accretion onto the main group as grouped.The unaccreted galaxy population experiences steady growth in dark matter, gas and stellar mass. Both single-and group-accreted galaxies begin to lose dark matter and gas after first accretion onto any host but continue to grow in stellar mass. Individual trajectories show that galaxies cease mass growth within roughly three virial radii of the main group. Single galaxies continue to form stars until the group virial radius is crossed, when they begin to lose both dark matter and gas. Grouped galaxies peak in mass when joining their external sub-group, indicating that they experience preprocessing. Most accreted galaxies retain their accumulated stellar mass. The total mass loss is dominated by tidal stripping, with evidence for additional gas stripping via ram pressure. Most accreted galaxies are quenched ∼(0.5-2.5) Gyr after accretion onto any group.These differing histories place unaccreted, single and grouped galaxies in distinct regions of the stellar mass-to-halo mass (SMHM) relation. This suggests that preprocessed galaxies are a key source of scatter in the SMHM relation for mixed galaxy populations.

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Section: Radial Trajectoriessupporting

confidence: 92%

“…Previous studies have suggested a strong correlation between the stellar mass and peak mass of galaxies (e.g. Peñarrubia et al 2008;Smith et al 2016). As we have found in this study, most of the single and grouped galaxies reach their peak total mass around the time they first became part of Figure 14.…”

Section: S7 S8mentioning

confidence: 98%

The trajectories of galaxies in groups: mass-loss and preprocessing

Joshi

Parker

Wadsley

et al. 2018

Monthly Notices of the Royal Astronomical Society

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“…Therefore we cannot directly measure the effect that tidal stripping might have on their baryonic component, which of course is the only component directly visible to us. However, as shown by Smith et al (2016), the relationship between dark matter tidal stripping and stellar tidal stripping in hydrodynamical cosmological simulations is actually quite well constrained: only halos that have lost more than ∼80% of their dark matter halo are likely to suffer any stellar stripping. Then, as the remaining ∼ 20% of the dark matter is stripped, the stellar fraction reduces rapidly towards 0%.…”

Section: Discussionmentioning

confidence: 99%

Leavers and remainers: galaxies split by group-exit

Choque-Challapa

Smith

Candlish

et al. 2019

Monthly Notices of the Royal Astronomical Society

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The disruption of substructure in galaxy clusters likely plays an important role in shaping the cluster population as a significant fraction of cluster galaxies today have spent time in a previous host system, and thus may have been pre-processed. Once inside the cluster, group galaxies face the combined environmental effects from group and cluster -so called 'post-processing'. We investigate these concepts, by tracking the evolution of satellites and their hosts after entering the cluster and find that tidal forces during their first pericentric passage are very efficient at breaking up groups, preferentially removing satellites at larger distances from their hosts. 92.2% of satellites whose host has passed pericentre will leave their host by z = 0, typically no later than half a Gyr after pericentric passage. We find satellites leave with high velocities, and quickly separate to large distances from their hosts, making their identification within the cluster population challenging. Those few satellites (∼ 7.8%) that remain bound to their hosts after a pericentric passage are typically found close to their host centres. This implies that substructure seen in clusters today is very likely on first infall into the cluster, and yet to pass pericentre. This is even more likely if the substructure is extended, with satellites beyond R 200 of their host. We find the cluster dominates the tidal mass loss and destruction of satellites, and is responsible for rapidly halting the accretion of new satellites onto hosts once they reach 0.6-0.8 R 200 radii from the cluster.

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“…In Smith et al (2016), the authors study the stripping of stellar and dark matter in galaxies during their infall into simulated clusters, and found that 18% of the galaxies were undergoing important star formation during accretion, with an increase in stellar mass higher than 15%. We test the influence of strongly star forming galaxies by removing all galaxies that increase their stellar mass by more that 50% during their infall, which represent 10% of the total number of satellite galaxies in our sample.…”

Section: Evolution Of Mass Vs R Satmentioning

confidence: 99%

“…Conversely, subhaloes will be subject to destructive influence from their host, and their dark matter will be gradually stripped by tidal forces. This effect has been highlighted in a number of analyses of N-body simulations for host haloes ranging from the size of the Milky Way (Hayashi et al 2003a;Kravtsov et al 2004;Diemand et al 2007;Buck et al 2019) to that of the most massive galaxy clusters (Ghigna et al 1998;Gao et al 2004;Tormen et al 2004;van den Bosch et al 2005;Giocoli et al 2008;Xie & Gao 2015;Smith et al 2016;Rhee et al 2017), where subhalo mass loss is well described by analytical models of tidal stripping (Mamon 2000;Gan et al 2010;Han et al 2016;Hiroshima et al 2018).…”

mentioning

confidence: 99%

Dark matter stripping in galaxy clusters: a look at the stellar-to-halo mass relation in the Illustris simulation

Niemiec

Jullo

Giocoli

et al. 2019

Monthly Notices of the Royal Astronomical Society

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Satellite galaxies in galaxy clusters represent a significant fraction of the global galaxy population. Because of the unusual dense environment of clusters, their evolution is driven by different mechanisms than the ones affecting field or central galaxies. Understanding the different interactions they are subject to, and how they are influenced by them, is therefore an important step towards explaining the global picture of galaxy evolution. In this paper, we use the publicly-available high resolution hydrodynamical simulation Illustris-1 to study satellite galaxies in the three most massive host haloes (with masses M 200 > 10 14 h −1 M ) at z = 0. We measure the Stellar-to-Halo Mass Relation (hereafter SHMR) of the galaxies, and find that for satellites it is shifted towards lower halo masses compared to the SHMR of central galaxies. We provide simple fitting functions for both the central and satellite SHMR. To explain the shift between the two, we follow the satellite galaxies since their time of accretion into the clusters, and quantify the impact of dark matter stripping and star formation. We find that subhaloes start losing their dark matter as soon as they get closer than ∼ 1.5 × R vir to the centre of their host, and that up to 80% of their dark matter content gets stripped during infall. On the other hand, star formation quenching appears to be delayed, and galaxies continue to form stars for a few Gyr after accretion. The combination of these two effects impacts the ratio of stellar to dark matter mass which varies drastically during infall, from 0.03 to 0.3.

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The Preferential Tidal Stripping of Dark Matter Versus Stars in Galaxies

Cited by 108 publications

References 67 publications

The trajectories of galaxies in groups: mass-loss and preprocessing

The trajectories of galaxies in groups: mass-loss and preprocessing

Leavers and remainers: galaxies split by group-exit

Dark matter stripping in galaxy clusters: a look at the stellar-to-halo mass relation in the Illustris simulation

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