The bias of weighted dark matter haloes from peak theory

Verde, Licia; Jiménez, Raúl; Simpson, Fergus; Álvarez‐Gaumé, Luis; Heavens, Alan; Matarrese, S.

doi:10.1093/mnras/stu1164

Cited by 13 publications

(7 citation statements)

References 78 publications

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“…Without these two complications, we can indeed derive a closed form expression for signed critical points. A similar calculation was performed in [72], where the determinant weight in Eq. (3) was dropped altogether, by weighting with 1=j det Hj.…”

Section: A Signed Critical Pointsmentioning

confidence: 99%

Nonperturbative halo clustering from cosmological density peaks

Baldauf

Codis

Desjacques³

2021

Phys. Rev. D

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Associating the formation sites of haloes with the maxima of the smoothed linear density field, we present nonperturbative predictions for the Lagrangian and evolved halo correlation functions that are valid at all separations. In Lagrangian space, we find significant deviations from the perturbative bias calculation at small scales, in particular, a pronounced exclusion region where ξ ¼ −1 for maxima of unequal height. Our predictions are in good agreement with the Lagrangian clustering of dark matter proto-haloes reconstructed from N-body simulations. Our predictions for the mean infall and velocity dispersion of haloes, which differ from the local bias expansion, show a similar level of agreement with simulations. Finally, we displace the initial density peaks according to the Zeldovich approximation in order to predict the late-time clustering of dark matter haloes. While we are able to reproduce the early evolution of this conserved set of tracers, our approximation fails at the collapse epoch (z ¼ 0) on nonlinear scales r ≲ 10h −1 Mpc, emphasizing the need for a nonperturbative treatment of the halo displacement field.

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Section: A Signed Critical Pointsmentioning

confidence: 99%

Nonperturbative halo clustering from cosmological density peaks

Baldauf

Codis

Desjacques³

2021

Phys. Rev. D

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“…We refer the interested reader to ref. [79], where the authors investigate the effects of the smoothing procedure on dark matter halos bias.…”

Section: Jcap11(2018)043mentioning

confidence: 99%

Measuring the energy scale of inflation with large scale structures

Bellomo

Bartolo

Jiménez

et al. 2018

J. Cosmol. Astropart. Phys.

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“…Another approach is based on the peak theory (Bardeen et al 1986). Recently Verde et al (2014) calculated the Lagrangian (formation) bias for a Gaussian density field. The matter density field can be approximated more reliable using a logarithmic transformation (Falck et al 2012) which could serve as an improved starting point for such a bias calculation.…”

Section: Discussionmentioning

confidence: 99%

Spatial range of conformity

Kerscher

2018

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Context. Properties of galaxies like their absolute magnitude and their stellar mass content are correlated. These correlations are tighter for close pairs of galaxies, which is called galactic conformity. In hierarchical structure formation scenarios, galaxies form within dark matter halos. To explain the amplitude and the spatial range of galactic conformity two-halo terms or assembly bias become important. Aims. With the scale dependent correlation coefficients the amplitude and the spatial range of conformity are determined from galaxy and halo samples. Methods. The scale dependent correlation coefficients are introduced as a new descriptive statistic to quantify the correlations between properties of galaxies or halos, depending on the distances to other galaxies or halos. These scale dependent correlation coefficients can be applied to the galaxy distribution directly. Neither a splitting of the sample into subsamples, nor an a priori clustering is needed.Results. This new descriptive statistic is applied to galaxy catalogues derived from the Sloan Digital Sky Survey III and to halo catalogues from the MultiDark simulations. In the galaxy sample the correlations between absolute Magnitude, velocity dispersion, ellipticity, and stellar mass content are investigated. The correlations of mass, spin, and ellipticity are explored in the halo samples. Both for galaxies and halos a scale dependent conformity is confirmed. Moreover the scale dependent correlation coefficients reveal a signal of conformity out to 40 Mpc and beyond. The halo and galaxy samples show a differing amplitude and range of conformity.M 2 M r,1 , e 1 , M r,2 , e 2 | r = 2 (x 1 , M r,1 , e 1 ), (x 2 , M r,2 , e 2 ) 2 (1 + ξ 2 (r)) .( 3) M 2 M r,1 , e 1 , M r,2 , e 2 | r is the probability density of the absolute magnitudes M r,1 , M r,2 , and ellipticities e 1 , e 2 under the condition that this pair of galaxies is separated by r = |x 1 − x 2 |. We speak of mark-independent clustering, if M 2 M r,1 , e 1 , M r,2 , e 2 | r = M(M r,1 , e 1 )M(M r,2 , e 2 ) factorises and does not depend on the pair separation r. In such a case the absolute magnitudes and the ellipticities of galaxy pairs with a separation r are not different from any other pair of galaxies. On the contrary, markdependent clustering or mark segregation implies that the marks on certain galaxy pairs show deviations from the global mark distribution. The conditional probability density M 2 M r,1 , e 1 , M r,2 , e 2 | r is used to calculate the scale-dependent correlation coefficient:cor (M r , e | r) = M r,1 ,e 1 ,M r,2 ,e 2 M 2 M r,1 , e 1 , M r,2 , e 2 | r M r,1 − M r (e 1 − e)with the abbreviation M r,1 ,e 1 ,M r,2 ,e 2 := dM r,1 de 1 dM r,2 de 2 .

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The bias of weighted dark matter haloes from peak theory

Cited by 13 publications

References 78 publications

Nonperturbative halo clustering from cosmological density peaks

Nonperturbative halo clustering from cosmological density peaks

Measuring the energy scale of inflation with large scale structures

Spatial range of conformity

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