Constraining the baryon–dark matter relative velocity with the large-scale three-point correlation function of the SDSS BOSS DR12 CMASS galaxies

Slepian, Zachary; Eisenstein, Daniel J.; Blazek, Jonathan; Brownstein, Joel R.; Chuang, Chia-Hsun; Gil-Marín, Héctor; Ho, Shirley; Kitaura, Francisco-Shu; McEwen, Joseph E.; Percival, Will J.; Ross, Ashley J.; Rossi, Graziano; Seo, Hee-Jong; Slosar, Anže; Vargas-Magaña, Mariana

doi:10.1093/mnras/stx2723

Cited by 36 publications

(17 citation statements)

References 43 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…These baryonic effects can be added to the biasing description, considering them as an additional species adding to the full set of symmetry allowed terms for the galaxy overdensity [79,80], starting from additional relativedensity δ bc and relative-velocity θ bc perturbation. In addition to these effects we have also higher order contributions starting from the relative velocity effects [79][80][81][82], though these terms have also been recently studied and constrained to be a rather small effect [83,84] relative to the rest of the terms. We also note that similar effects described by the general formalism presented in [79,80] could also be adapted to describe effects of cosmic neutrinos or fluctuating dark energy models [85] on mildly-nonlinear scales.…”

Section: Discussionmentioning

confidence: 99%

Modeling CMB lensing cross correlations with CLEFT

Modi

White

Vlah

2017

J. Cosmol. Astropart. Phys.

View full text Add to dashboard Cite

Abstract.A new generation of surveys will soon map large fractions of sky to ever greater depths and their science goals can be enhanced by exploiting cross correlations between them. In this paper we study cross correlations between the lensing of the CMB and biased tracers of large-scale structure at high z. We motivate the need for more sophisticated bias models for modeling increasingly biased tracers at these redshifts and propose the use of perturbation theories, specifically Convolution Lagrangian Effective Field Theory (CLEFT). Since such signals reside at large scales and redshifts, they can be well described by perturbative approaches. We compare our model with the current approach of using scale independent bias coupled with fitting functions for non-linear matter power spectra, showing that the latter will not be sufficient for upcoming surveys. We illustrate our ideas by estimating σ 8 from the auto-and cross-spectra of mock surveys, finding that CLEFT returns accurate and unbiased results at high z. We discuss uncertainties due to the redshift distribution of the tracers, and several avenues for future development.

show abstract

Section: Discussionmentioning

confidence: 99%

Modeling CMB lensing cross correlations with CLEFT

Modi

White

Vlah

2017

J. Cosmol. Astropart. Phys.

View full text Add to dashboard Cite

show abstract

“…In general this method is regarded as highly robust as it probes very large scales which are largely unaffected by astrophysical processes. However, relative component contributions to the two-point function also occur on very large scales and their oscillatory features, although arising from the same physical process of the standard BAO features in the matter density power spectrum, could bias our estimates of the distance scale if not properly taken into account [22][23][24]. Indeed, as shown in the left panel of Fig.…”

Section: Degeneracies and Bias To Baomentioning

confidence: 96%

Biased tracers of two fluids in the Lagrangian picture

Chen

Castorina

White

2019

J. Cosmol. Astropart. Phys.

View full text Add to dashboard Cite

We explore Lagrangian perturbation theory (LPT) for biased tracers in the presence of two fluids, focusing on the case of cold dark matter (CDM) and baryons. The presence of two fluids induces corrections to the Lagrangian bias expansion and tracer advection, both of which we formulate as expansions in the three linear modes of the Lagrangian equations of motion. We compute the linear-order two-fluid corrections in the Zeldovich approximation, finding that modifications to the bias expansion and tracer advection both enter as percentlevel corrections over a large range of wavenumbers at low redshift and draw parallels with the Eulerian formalism. We then discuss nonlinear corrections in the two-fluid picture, and calculate contributions from the relative velocity effect (∝ v 2 r ) at one loop order. Finally, we conduct an exploratory Fisher analysis to assess the impact of two-fluid corrections on baryon acoustic oscillations (BAO) measurements, finding that while modest values of the relative bias parameters can introduce systematic biases in the measured BAO scale of up to 0.5 σ, fitting for these effects as additional parameters increases the error bar by less than 30% across a wide range of bias values. Linear Equations of Motion in Lagrangian SpaceIn the Lagrangian picture, fluid dynamics is encoded in the displacements Ψ σ (q) of fluid elements of each species, σ, originally situated at Lagrangian positions q, such that their Eulerian positions at conformal time τ (dτ = a −1 dt) are given by [28,37,38] x σ (q, τ ) = q + Ψ σ (q, τ ).(2.1)The subscript σ = {c, b} denotes the species, either cold dark matter (CDM) or baryons, respectively, whose motion we are tracking. Assuming that initial displacements are infinitesimally small compared to those at the redshifts of interest, the overdensity, δ σ , of each species at Eulerian

show abstract

“…A number of recent analyses have included the simplest non-Gaussian statistic; the 3-Point Correlation Function (3PCF) [14,15], or bispectrum [16][17][18][19][20]. This has been facilitated by fast algorithms for computing such statistics [e.g., [21][22][23][24][25][26][27][28][29], as well as the development of theory models for the galaxy 3PCF [30] and bispectrum [e.g., [31][32][33][34][35][36][37], though the latter is still in its infancy.…”

Section: Introductionmentioning

confidence: 99%

A First Detection of the Connected 4-Point Correlation Function of Galaxies Using the BOSS CMASS Sample

Philcox,

Hou,

Slepian

2021

Preprint

Self Cite

View full text Add to dashboard Cite

We present an 8.1σ detection of the non-Gaussian 4-Point Correlation Function (4PCF) using a sample of Ng ≈ 8 × 10 5 galaxies from the BOSS CMASS dataset. Our measurement uses the O(N 2 g ) NPCF estimator of , including a new modification to subtract the disconnected 4PCF contribution (arising from the product of two 2PCFs) at the estimator level. This approach is unlike previous work and ensures that our signal is a robust detection of gravitationally-induced non-Gaussianity. The estimator is validated with a suite of lognormal simulations, and the analytic form of the disconnected contribution is discussed. Due to the high dimensionality of the 4PCF, data compression is required; we use a signal-to-noise-based scheme calibrated from theoretical covariance matrices to restrict to ∼ 100 basis vectors. The compression has minimal impact on the detection significance and facilitates traditional χ 2 -like analyses using a suite of mock catalogs. The significance is stable with respect to different treatments of noise in the sample covariance (arising from the limited number of mocks), but decreases to 4.7σ when a minimum galaxy separation of 14 h −1 Mpc is enforced on the 4PCF tetrahedra (such that the statistic can be modelled more easily). The detectability of the 4PCF in the quasi-linear regime implies that it will become a useful tool in constraining cosmological and galaxy formation parameters from upcoming spectroscopic surveys.

show abstract

Constraining the baryon–dark matter relative velocity with the large-scale three-point correlation function of the SDSS BOSS DR12 CMASS galaxies

Cited by 36 publications

References 43 publications

Modeling CMB lensing cross correlations with CLEFT

Modeling CMB lensing cross correlations with CLEFT

Biased tracers of two fluids in the Lagrangian picture

A First Detection of the Connected 4-Point Correlation Function of Galaxies Using the BOSS CMASS Sample

Contact Info

Product

Resources

About