Origin of the Angular Momentum of Galaxies

Peebles, P. J. E.

doi:10.1086/149876

Cited by 999 publications

(1,017 citation statements)

References 0 publications

Supporting

Mentioning

977

Contrasting

Unclassified

Order By: Relevance

“…There has been much attention on measuring the alignment, if any, between the spin of halos within filaments and walls and the orientation of the filaments and walls themselves. This alignment is predicted by the tidal torque theory, by which galaxies acquire their angular momentum from the large scale tidal force field [62,63]. Tidal torque theory has been investigated in LCDM simulations (see, e.g., [23,[64][65][66][67]) and in observations [68], but results so far vary greatly and remain inconclusive.…”

Section: Halo Propertiesmentioning

confidence: 98%

The Vainshtein mechanism in the cosmic web

Falck

Koyama

Zhao

et al. 2014

J. Cosmol. Astropart. Phys.

View full text Add to dashboard Cite

We investigate the dependence of the Vainshtein screening mechanism on the cosmic web morphology of both dark matter particles and halos as determined by ORIGAMI. Unlike chameleon and symmetron screening, which come into effect in regions of high density, Vainshtein screening instead depends on the dimensionality of the system, and screened bodies can still feel external fields. ORIGAMI is well-suited to this problem because it defines morphologies according to the dimensionality of the collapsing structure and does not depend on a smoothing scale or density threshold parameter. We find that halo particles are screened while filament, wall, and void particles are unscreened, and this is independent of the particle density. However, after separating halos according to their large scale cosmic web environment, we find no difference in the screening properties of halos in filaments versus halos in clusters. We find that the fifth force enhancement of dark matter particles in halos is greatest well outside the virial radius. We confirm the theoretical expectation that even if the internal field is suppressed by the Vainshtein mechanism, the object still feels the fifth force generated by the external fields, by measuring peculiar velocities and velocity dispersions of halos. Finally, we investigate the morphology and gravity model dependence of halo spins, concentrations, and shapes.

show abstract

Section: Halo Propertiesmentioning

confidence: 98%

The Vainshtein mechanism in the cosmic web

Falck

Koyama

Zhao

et al. 2014

J. Cosmol. Astropart. Phys.

View full text Add to dashboard Cite

show abstract

“…We present results for both the Bullock spin parameter (Bullock et al 2001) and the Peebles spin parameter (Peebles 1969), defined as…”

Section: Spin Parametermentioning

confidence: 99%

Properties of dark matter haloes as a function of local environment density

Lee

Primack

Behroozi

et al. 2016

Mon. Not. R. Astron. Soc.

View full text Add to dashboard Cite

We study how properties of discrete dark matter halos depend on halo environment, characterized by the mass density around the halos on scales from 0.5 to 16 h −1 Mpc. We find that low mass halos (those less massive than the characteristic mass M C of halos collapsing at a given epoch) in high-density environments have lower accretion rates, lower spins, higher concentrations, and rounder shapes than halos in median density environments. Halos in median and low-density environments have similar accretion rates and concentrations, but halos in low density environments have lower spins and are more elongated. Halos of a given mass in high-density regions accrete material earlier than halos of the same mass in lower-density regions. All but the most massive halos in high-density regions are losing mass (i.e., being stripped) at low redshifts, which causes artificially lowered NFW scale radii and increased concentrations. Tidal effects are also responsible for the decreasing spins of low mass halos in high density regions at low redshifts z < 1, by preferentially removing higher angular momentum material from halos. Halos in low-density regions have lower than average spins because they lack nearby halos whose tidal fields can spin them up. We also show that the simulation density distribution is well fit by an Extreme Value Distribution, and that the density distribution becomes broader with cosmic time.

show abstract

“…The basic understanding of the origin of AM in galaxies is that, as the proto-galactic density perturbations grow, they acquire AM through the gravitational tidal torques exerted by neighboring perturbations (Hoyle 1951;Peebles 1969;Doroshkevich 1970). This has been clarified and put together by White (1984) as the standard linear tidal-torque theory (TTT).…”

Section: Introductionmentioning

confidence: 99%

“…The nature and origin of this messy region is not tion by Peebles (1969), λ = J|E| 1/2 G −1 M −5/2 (where E is the energy), in the case of a singular isothermal sphere truncated at Rv.…”

Section: Introductionmentioning

confidence: 99%

Four phases of angular-momentum buildup in high-z galaxies: from cosmic-web streams through an extended ring to disc and bulge

Danovich¹,

Dekel²,

Hahn³

et al. 2015

Monthly Notices of the Royal Astronomical Society

293

377

View full text Add to dashboard Cite

We study the angular-momentum (AM) buildup in high-z massive galaxies using highresolution cosmological simulations. The AM originates in co-planar streams of cold gas and merging galaxies tracing cosmic-web filaments, and it undergoes four phases of evolution. (I) Outside the halo virial radius (R v ∼ 100 kpc), the elongated streams gain AM by tidal torques with a specific AM (sAM) ∼ 1.7 times the dark-matter (DM) spin due to the gas' higher quadrupole moment. This AM is expressed as stream impact parameters, from ∼ 0.3R v to counter rotation. (II) In the outer halo, while the incoming DM mixes with the existing halo of lower sAM to a spin λ dm ∼ 0.04, the cold streams transport the AM to the inner halo such that their spin in the halo is ∼ 3λ dm . (III) Near pericenter, the streams dissipate into an irregular rotating ring extending to ∼ 0.3R v and tilted relative to the inner disc. Torques exerted partly by the disc make the ring gas lose AM, spiral in, and settle into the disc within one orbit. The ring is observable with 30% probability as a damped Lyman-α absorber. (IV) Within the disc, < 0.1R v , torques associated with violent disc instability drive AM out and baryons into a central bulge, while outflows remove low-spin gas, introducing certain sensitivity to feedback strength. Despite the different AM histories of gas and DM, the disc spin is comparable to the DM-halo spin. Counter rotation can strongly affect disc evolution.

show abstract

Origin of the Angular Momentum of Galaxies

Cited by 999 publications

References 0 publications

The Vainshtein mechanism in the cosmic web

The Vainshtein mechanism in the cosmic web

Properties of dark matter haloes as a function of local environment density

Four phases of angular-momentum buildup in high-z galaxies: from cosmic-web streams through an extended ring to disc and bulge

Contact Info

Product

Resources

About