On the spin bias of satellite galaxies in the local group-like environment

Lee, Jounghun; Lemson, Gerard

doi:10.1088/1475-7516/2013/05/022

Cited by 4 publications

(4 citation statements)

References 34 publications

(47 reference statements)

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“…The left panel shows the specific angular momentum as a function of the halo mass. Compared to halos without neighbors, those with neighbors have, on average, a slightly higher j core , and it is consistent with the previous findings (e.g., Lee & Lemson 2013;Johnson et al 2019). Although the increase in j core is statistically significant, the difference between the two subsamples is quite small.…”

Section: Linking Soa To Interaction With Neighborssupporting

confidence: 90%

Living with Neighbors. IV. Dissecting the Spin$-$Orbit Alignment of Dark Matter Halos: Interacting Neighbors and the Local Large-scale Structure

An,

Kim,

Moon

et al. 2021

Preprint

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Spin-orbit alignment (SOA; i.e., the vector alignment between the halo spin and the orbital angular momentum of neighboring halos) provides an important clue to how galactic angular momenta develop. For this study, we extract virial-radius-wise contact halo pairs with mass ratios between 1/10 and 10 from a set of cosmological N -body simulations. In the spin-orbit angle distribution, we find a significant SOA in that 52.7 % ± 0.2 % of neighbors are on the prograde orbit. The SOA of our sample is mainly driven by low-mass target halos (< 10 11.5 h −1 M ) with close merging neighbors, corroborating the notion that the tidal interaction is one of the physical origins of SOA. We also examine the correlation of SOA with the adjacent filament and find that halos closer to the filament show stronger SOA. Most interestingly, we discover for the first time that halos with the spin parallel to the filament experience most frequently the prograde-polar interaction (i.e., fairly perpendicular but still prograde interaction; spin-orbit angle ∼ 70 • ). This instantly invokes the spin-flip event and the prograde-polar interaction will soon flip the spin of the halo to align it with the neighbor's orbital angular momentum. We propose that the SOA originates from the local cosmic flow along the anisotropic large-scale structure, especially that along the filament, and grows further by interactions with neighbors.

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Section: Linking Soa To Interaction With Neighborssupporting

confidence: 90%

Living with Neighbors. IV. Dissecting the Spin$-$Orbit Alignment of Dark Matter Halos: Interacting Neighbors and the Local Large-scale Structure

An,

Kim,

Moon

et al. 2021

Preprint

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“…The mass resolution of BoxA (2.6 × 10 5 h −1 M per particle) is very close to that of the Aquarius-A simulation at level 4 (Springel et al 2008) which had a particle mass of 2.7 × 10 5 h −1 M in the high resolution region. This is roughly three times better mass resolution than the Millennium-II simulation (m p = 6.9 × 10 6 h −1 M ) used by Lee & Lemson (2013). The cosmology was chosen to be the same as in the Aquarius simulation, i.e.…”

Section: Simulation Datamentioning

confidence: 99%

“…Due to a lack of resolution in previous generations of large cosmological simulations, subhalo spins have not been thoroughly investigated so far, despite their application within current semi-analytic models (Guo et al 2011). Initial work by Lee & Lemson (2013) analyzed the spins of the two most massive substructures of Local Group like systems in the Millennium-II simulation (Boylan-Kolchin et al 2009) and revealed possible consequences for the application of subhalo spins to near-field cosmology. Onions et al (2013) investigated the spin distribution of subhaloes in two high resolution simulations of a Milky Waylike halo (the Aquarius simulation (Springel et al 2008) and the GHALO simulation (Stadel et al 2009)) analyzed by a variety of subhalo finders.…”

Section: Introductionmentioning

confidence: 99%

Solving the Puzzle of Subhalo Spins

Wang

Lin

Pearce

et al. 2015

ApJ

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Investigating the spin parameter distribution of subhaloes in two high resolution isolated halo simulations, recent work by Onions et al. suggested that typical subhalo spins are consistently lower than the spin distribution found for field haloes. To further examine this puzzle, we have analyzed simulations of a cosmological volume with sufficient resolution to resolve a significant subhalo population. We confirm the result of Onions et al. and show that the typical spin of a subhalo decreases with decreasing mass and increasing proximity to the host halo center. We interpret this as the growing influence of tidal stripping in removing the outer layers, and hence the higher angular momentum particles, of the subhaloes as they move within the host potential. Investigating the redshift dependence of this effect, we find that the typical subhalo spin is smaller with decreasing redshift. This indicates a temporal evolution as expected in the tidal stripping scenario.

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“…Their mass resolution is equivalent to the resolution of the Aquarius project simulations at level 5 and level 4, respectively (Springel et al 2008). The mass resolution of the Aquarius simulation at level 5 is roughly three times higher than that of the Millennium-II simulation (mp = 6.9 × 10 6 h −1 M ) used by Lee & Lemson (2013). The cosmology was chosen to be the same as in the Aquarius simulation, i.e.…”

Section: Convergence Studymentioning

confidence: 99%

Sussing merger trees: stability and convergence

Wang

Pearce

Knebe

et al. 2016

Mon. Not. R. Astron. Soc.

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Merger trees are routinely used to follow the growth and merging history of dark matter haloes and subhaloes in simulations of cosmic structure formation. Srisawat et al. (2013) compared a wide range of merger-tree-building codes. Here we test the influence of output strategies and mass resolution on tree-building. We find that, somewhat surprisingly, building the tree from more snapshots does not generally produce more complete trees; instead, it tends to shorten them. Significant improvements are seen for patching schemes which attempt to bridge over occasional dropouts in the underlying halo catalogues or schemes which combine the halofinding and tree-building steps seamlessly. The adopted output strategy does not affect the average number of branches (bushiness) of the resultant merger trees. However, mass resolution has an influence on both main branch length and the bushiness. As the resolution increases, a halo with the same mass can be traced back further in time and will encounter more small progenitors during its evolutionary history. Given these results, we recommend that, for simulations intended as precursors for galaxy formation models where of order 100 or more snapshots are analysed, the tree-building routine should be integrated with the halo finder, or at the very least be able to patch over multiple adjacent snapshots.

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On the spin bias of satellite galaxies in the local group-like environment

Cited by 4 publications

References 34 publications

Living with Neighbors. IV. Dissecting the Spin$-$Orbit Alignment of Dark Matter Halos: Interacting Neighbors and the Local Large-scale Structure

Living with Neighbors. IV. Dissecting the Spin$-$Orbit Alignment of Dark Matter Halos: Interacting Neighbors and the Local Large-scale Structure

Solving the Puzzle of Subhalo Spins

Sussing merger trees: stability and convergence

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