Spin Alignment of Dark Matter Halos in Filaments and Walls

Aragón-Calvo, M. A.; Weygaert, Rien van de; Jones, Bernard J. T.; Hulst, van der Thijs

doi:10.1086/511633

Cited by 268 publications

(368 citation statements)

References 30 publications

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“…On the other hand, the spin axes of bright spirals have a weak tendency to be aligned along the filament's spine. This spinflip was found in numerical simulations as well (Aragón-Calvo et al 2007;Codis et al 2012;Libeskind et al 2013) and found to be mass and environment dependent. Below a certain mass, haloes spin parallel to filaments, above a certain mass they spin perpendicular to them.…”

Section: Introductionsupporting

confidence: 55%

“…Methods to quantify the cosmic web abound (Stoica et al 2005;Shen et al 2006;Aragón-Calvo et al 2007;Hahn et al 2007;Sousbie et al 2008;Forero-Romero et al 2009;Hoffman et al 2012;Libeskind et al 2012Libeskind et al , 2013Tempel et al 2014a) depending on the data and problem at hand. In general, the methods based on simulations rely on a more complete knowledge of the cosmic fluid than what is usually available in observations.…”

Section: Introductionmentioning

confidence: 99%

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The alignment of galaxy spin with the shear field in observations

Pahwa

Libeskind

Tempel

et al. 2016

Mon. Not. R. Astron. Soc.

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Tidal torque theory suggests that galaxies gain angular momentum in the linear stage of structure formation. Such a theory predicts alignments between the spin of haloes and tidal shear field. However, non-linear evolution and angular momentum acquisition may alter this prediction significantly. In this paper, we use a reconstruction of the cosmic shear field from observed peculiar velocities combined with spin axes extracted from galaxies within 115 Mpc (∼ 8000 kms −1 ) from 2MRS catalog, to test whether or not galaxies appear aligned with principal axes of shear field. Although linear reconstructions of the tidal field have looked at similar issues, this is the first such study to examine galaxy alignments with velocity-shear field. Ellipticals in the 2MRS sample, show a statistically significant alignment with two of the principal axes of the shear field. In general, elliptical galaxies have their short axis aligned with the axis of greatest compression and perpendicular to the axis of slowest compression. Spiral galaxies show no signal. Such an alignment is significantly strengthened when considering only those galaxies that are used in velocity field reconstruction. When examining such a subsample, a weak alignment with the axis of greatest compression emerges for spiral galaxies as well. This result indicates that although velocity field reconstructions still rely on fairly noisy and sparse data, the underlying alignment with shear field is strong enough to be visible even when small numbers of galaxies are considered -especially if those galaxies are used as constraints in the reconstruction.

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Section: Introductionsupporting

confidence: 55%

Section: Introductionmentioning

confidence: 99%

The alignment of galaxy spin with the shear field in observations

Pahwa

Libeskind

Tempel

et al. 2016

Mon. Not. R. Astron. Soc.

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“…Aragón-Calvo et al 2007;Libeskind et al 2013;Laigle et al 2015). Another application of our method is to more reliably measure the "effective field" properties of dark matter (e.g.…”

Section: Discussionmentioning

confidence: 99%

The properties of cosmic velocity fields

Hahn¹,

Angulo²,

Abel³

2015

Mon. Not. R. Astron. Soc.

125

170

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Understanding the velocity field is very important for modern cosmology: it gives insights to structure formation in general, and also its properties are crucial ingredients in modelling redshift-space distortions and in interpreting measurements of the kinetic Sunyaev-Zeldovich effect. Unfortunately, characterising the velocity field in cosmological N -body simulations is inherently complicated by two facts: i) The velocity field becomes manifestly multi-valued after shell-crossing and has discontinuities at caustics. This is due to the collisionless nature of dark matter. ii) N -body simulations sample the velocity field only at a set of discrete locations, with poor resolution in low-density regions. In this paper, we discuss how the associated problems can be circumvented by using a phase-space interpolation technique. This method provides extremely accurate estimates of the cosmic velocity fields and its derivatives, which can be properly defined without the need of the arbitrary "coarse-graining" procedure commonly used. We explore in detail the configuration-space properties of the cosmic velocity field on very large scales and in the highly nonlinear regime. In particular, we characterise the divergence and curl of the velocity field, present their one-point statistics, analyse the Fourier-space properties and provide fitting formulae for the velocity divergence bias relative to the non-linear matter power spectrum. We furthermore contrast some of the interesting differences in the velocity fields of warm and cold dark matter models. We anticipate that the high-precision measurements carried out here will help to understand in detail the dynamics of dark matter and the structures it forms.

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“…The former has been seen by a number of previous studies (e.g., Bordoloi et al 2011) but is an unlikely scenario for explaining the Mg II absorbers found around LRGs due to the observed low SFR. At the same time, it has been shown both in simulations and in observations that elliptical galaxies preferentially have their major axes aligned with the filamentary structures (e.g., Aragón-Calvo et al 2007;Tempel et al 2013), where accretion of intergalactic gas and satellites originates (e.g., Faucher-Giguère & Kereš 2011;Fumagalli et al 2011;Tempel et al 2015).…”

Section: Incidence and Covering Fraction Of Mg II Absorbers In Lrg Halosmentioning

confidence: 97%

Characterizing the chemically enriched circumgalactic medium of ∼38 000 luminous red galaxies in SDSS DR12

Huang

Chen

Johnson

et al. 2015

Monthly Notices of the Royal Astronomical Society

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We report a definitive detection of chemically-enriched cool gas around massive, quiescent galaxies at z ≈ 0.4 − 0.7. The result is based on a survey of 37621 luminous red galaxy (LRG)-QSO pairs in SDSS DR12 with projected distance d < 500 kpc. LRGs at d < 50 kpc, provides important insights into the origin of the observed chemically-enriched cool gas in LRG halos. We consider different scenarios and conclude that the observed Mg II absorbers around LRGs are best-explained by a combination of cool clouds formed in thermally unstable LRG halos and satellite accretion through filaments.

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Spin Alignment of Dark Matter Halos in Filaments and Walls

Cited by 268 publications

References 30 publications

The alignment of galaxy spin with the shear field in observations

The alignment of galaxy spin with the shear field in observations

The properties of cosmic velocity fields

Characterizing the chemically enriched circumgalactic medium of ∼38 000 luminous red galaxies in SDSS DR12

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