An observed correlation between galaxy spins and initial conditions

Motloch, Pavel; Yu, Hao-Ran; Pen, Ue-Li; Xie, Yuanbo

doi:10.1038/s41550-020-01262-3

Cited by 42 publications

(62 citation statements)

References 47 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…In Lagrangian space, by using the E-mode reconstructed density fields [7] we are able to construct a scale dependent spin mode, and successfully predict the spins of dark matter halos [8]. By applying this method to the ELUCID reconstruction of the local universe [9] and a first spin catalog of observed galaxies, [10] for the first time confirmed the correlation between galaxy spins and initial conditions of the Universe. These studies open the path of using galaxy spins to constrain the primordial state of the universe, including primordial non-Gaussianity, gravity waves, parity violation [8], and neutrino mass [11].…”

Section: Introductionmentioning

confidence: 69%

“…The spins of disk galaxies are observable and we have discovered a positive correlation signal between disk galaxies and their halos and the reconstructed initial density field of the local universe [10]. This observed correlation is a result of many facts: the observability of galaxy spiral arms indicating their spin directions; the underlying galaxyhalo spin correlation, confirmed by many galaxy formation simulations; the Lagrangian-Eulerian spin correlation; the tidal torque theory and spin mode reconstruction linking the primordial density field with protohalo spins; and the density reconstruction given galaxy positions.…”

Section: Discussionmentioning

confidence: 87%

“…We have confirmed that L TT is a reconstructed spin field as a reliable proxy of j L , j E of dark matter halos in N-body simulations [8], of j E of simulated galaxies in galaxy formation simulations (Liao et al in prep. ), and of j E of observed disk galaxies [10].…”

Section: Spin Conservation and Reconstructionmentioning

confidence: 98%

“…as the proxies of λ K , where β IT optimizes the measurement of anisotropies and misalignment between two tensors I and T, whereas tidal environment parameter β TT measures the anisotropy and twist of T on physical scale r. A schematic interpretation of β TT is discussed in the Fig. 1 of [10].…”

Section: Spin Parameters In Lagrangian Spacementioning

confidence: 99%

See 3 more Smart Citations

Spin mode reconstruction in Lagrangian space

Liao

et al. 2021

Phys. Rev. D

Self Cite

View full text Add to dashboard Cite

Galaxy angular momentum directions (spins) are observable, well described by the Lagrangian tidal torque theory, and proposed to probe the primordial universe. They trace the spins of dark matter halos, and are indicators of protohalos properties in Lagrangian space. We define a Lagrangian spin parameter and tidal twist parameters and quantify their influence on the spin conservation and predictability in the spin mode reconstruction in N-body simulations. We conclude that protohalos in more tidal twisting environments are preferentially more rotation-supported, and more likely to conserve their spin direction through the cosmic evolution. These tidal environments and spin magnitudes are predictable by a density reconstruction in Lagrangian space, and such predictions can improve the correlation between galaxy spins and the initial conditions in the study of constraining the primordial universe by spin mode reconstruction.

show abstract

Section: Introductionmentioning

confidence: 69%

Section: Discussionmentioning

confidence: 87%

Section: Spin Conservation and Reconstructionmentioning

confidence: 98%

Section: Spin Parameters In Lagrangian Spacementioning

confidence: 99%

See 2 more Smart Citations

Spin mode reconstruction in Lagrangian space

Liao

et al. 2021

Phys. Rev. D

Self Cite

View full text Add to dashboard Cite

show abstract

“…As a collapsing region reaches turnaround, tidal torques cease to be effective and the final angular momentum of a collapsed region is far from what tidal torque theory would predict [9][10][11] . Although one recent study 12 has demonstrated that galaxy spin direction (that is, clockwise versus anticlockwise) can be predicted from initial conditions, revealing a critical clue to the nonlinear acquisition of angular momentum, our understanding of spin magnitude, direction and history remains in its infancy. Regions that are still in the linear or quasilinear phase of collapse could provide a better stage for the application of tidal torque theory.…”

mentioning

confidence: 99%

Possible observational evidence for cosmic filament spin

et al. 2021

View full text Add to dashboard Cite

Although structures in the Universe form on a wide variety of scales, from small dwarf galaxies to large super clusters, the generation of angular momentum across these scales is poorly understood. Here we investigate the possibility that filaments of galaxies-cylindrical tendrils of matter hundreds of millions of light years across-are themselves spinning. By stacking thousands of filaments together and examining the velocity of galaxies perpendicular to the filament's axis (via their redshift and blueshift), we find that these objects too display vortical motion consistent with rotation, making them the largest objects known to have angular momentum. The strength of the rotation signal is directly dependent on the viewing angle and the dynamical state of the filament. Filament rotation is more clearly detected when viewed edge-on. In addition, the more massive the haloes that sit at either end of the filaments, the more rotation is detected. These results signify that angular momentum can be generated on unexpectedly large scales.

show abstract

Large‐scale asymmetry in galaxy spin directions: Analysis of galaxies with spectra in DES, SDSS, and DESI Legacy Survey

Shamir

2022

Astron Nachr

View full text Add to dashboard Cite

Multiple previous studies using several different probes have shown considerable evidence for the existence of cosmological‐scale anisotropy and a Hubble‐scale axis. One of the probes that show such evidence is the distribution of the directions toward which galaxies spin. The advantage of the analysis of the distribution of galaxy spin directions compared to the cosmic microwave background anisotropy is that the ratio of galaxy spin directions is a relative measurement, and therefore less sensitive to background contamination such as Milky Way obstruction. Another advantage is that many spiral galaxies have spectra, and therefore allow to analyze the location of such axis relative to Earth. This paper shows an analysis of the distribution of the spin directions of over 90K galaxies with spectra. That analysis is also compared to previous analyses using the Earth‐based Sloan Digital Sky Survey, Panoramic Survey Telescope and Rapid Response System, and Dark Energy Spectroscopic Instrument Legacy Survey, as well as space‐based data collected by Hubble Space Telescope. The results show very good agreement between the distribution patterns observed with the different telescopes. The dipole or quadrupole axes formed by the spin directions of the galaxies with spectra do not necessarily go directly through Earth.

show abstract

An observed correlation between galaxy spins and initial conditions

Cited by 42 publications

References 47 publications

Spin mode reconstruction in Lagrangian space

Spin mode reconstruction in Lagrangian space

Possible observational evidence for cosmic filament spin

Large‐scale asymmetry in galaxy spin directions: Analysis of galaxies with spectra in DES, SDSS, and DESI Legacy Survey

Contact Info

Product

Resources

About