Detection of baryon acoustic oscillation features in the large-scale three-point correlation function of SDSS BOSS DR12 CMASS galaxies

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

doi:10.1093/mnras/stx488

Cited by 133 publications

(113 citation statements)

References 78 publications

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“…The BAO has also been detected in the higher order statistics of the 3-point correlation function (Slepian et al 2017) and bispectrum (Pearson & Samushia 2018) for the BOSS CMASS sample. The BAO feature has been measured using voids as the clustering tracer (Kitaura et al 2016a;Liang et al 2016), also in BOSS.…”

Section: Introductionmentioning

confidence: 88%

“…The formalism used to calculate Eq. 2 using fast Fourier transforms (FFTs) is described in Hand et al (2017b), and builds upon the ideas of Bianchi et al (2015); Scoccimarro (2015) and Slepian & Eisenstein (2015).…”

Section: Power Spectrum Multipolesmentioning

confidence: 99%

“…Removal of these shifts can reduce the damping of the BAO and increase the S/N of this feature. This increased S/N results from information that was absorbed into higher order statistics being moved back into linear fluctuations (Schmittfull et al 2015;Slepian et al 2017). Density field reconstruction has been applied in analyses of the 6dFGS (Carter et al 2018), SDSS (Padmanabhan et al 2012;Ross et al 2015), WiggleZ (Kazin et al 2014) and throughout BOSS (Alam et al 2017).…”

Section: Introductionmentioning

confidence: 99%

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The impact of the fiducial cosmology assumption on BAO distance scale measurements

Carter

Beutler

Percival

et al. 2020

Monthly Notices of the Royal Astronomical Society

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Standard analysis pipelines for measurements of Baryon Acoustic Oscillations (BAO) in galaxy surveys make use of a fiducial cosmological model to guide the data compression required to transform from observed redshifts and angles to the measured angular and radial BAO peak positions. In order to remove any dependence on the fiducial cosmology from the results, all models compared to the data should mimic the compression and its dependence on the fiducial model. In practice, approximations are made when testing models: (1) There is assumed to be no residual dependence on the fiducial cosmology after reconstruction, (2) differences in the distance-redshift relationship are assumed to match a linear scaling, and (3) differences in clustering between true and fiducial models are assumed to be removed by the free parameters used to null the non-BAO signal. We test these approximations using the current standard measurement procedure with a set of halo catalogs from the Aemulus suite of N-body simulations, which span a range of wCDM cosmological models. We focus on reconstruction of the primordial BAO and locating the BAO. For the range of wCDM cosmologies covered by the Aemulus suite, we find no evidence for systematic errors in the measured BAO shift parameters α and α ⊥ to < 0.1%. However, the measured errors σ α and σ α ⊥ show a notable absolute increase by up to +0.001 and +0.002 respectively in the case that the fiducial cosmology does not match the truth. These effects on the inferred BAO scale will be important given the precision of measurements expected from future surveys including DESI, Euclid, and WFIRST.

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Section: Introductionmentioning

confidence: 88%

Section: Power Spectrum Multipolesmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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The impact of the fiducial cosmology assumption on BAO distance scale measurements

Carter

Beutler

Percival

et al. 2020

Monthly Notices of the Royal Astronomical Society

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“…These characteristics make LRGs particularly interesting to study the physics of the baryon cycle because they extend the mass scale to >L* (the COS-Halos survey is ∼L*), and their passivity ensures we are characterizing the CGM around galaxies that are at the end of their star-forming life cycle. Given their importance for cosmological studies (e.g., Eisenstein et al 2005;Xu et al 2013;Slepian et al 2017), there are large samples of LRGs with both SDSS photometry and spectroscopy (Dawson et al 2013(Dawson et al , 2016Prakash et al 2016;Albareti et al 2017). Due to these SDSS surveys, the general characteristics of LRGs are well-understood.…”

Section: Introductionmentioning

confidence: 99%

The Red Dead Redemption Survey of Circumgalactic Gas about Massive Galaxies. I. Mass and Metallicity of the Cool Phase

Berg

Howk

Lehner

et al. 2019

ApJ

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We present a search for H I in the circumgalactic medium (CGM) of 21 massive ( log M ∼ 11.4), luminous red galaxies (LRGs) at z ∼ 0.5. Using UV spectroscopy of QSO sightlines projected within 500 kpc (∼R vir ) of these galaxies, we detect H I absorption in 11/21 sightlines, including two partial Lyman limit systems and two Lyman limit systems. The covering factor of log N (H I) ≥ 16.0 gas within the virial radius of these LRGs is f c (ρ ≤ R vir ) = 0.27 +0.11 −0.10 , while for optically-thick gas (log N (−0.07 . Combining this sample of massive galaxies with previous galaxy-selected CGM studies, we find no strong dependence of the H I covering factor on galaxy mass, although star-forming galaxies show marginally higher covering factors. There is no evidence for a critical mass above which dense, cold (T ∼ 10 4 K) gas is suppressed in the CGM of galaxies (spanning stellar masses 9.5 log M 11.8). The metallicity distribution in LRGs is indistinguishable from those found about lower-mass star-forming galaxies, and we find low-metallicity gas with [X/H] ≈ −1.8 (1.5% solar) and below about massive galaxies. About half the cases show super-solar [Fe II/Mg II] abundances as seen previously in cool gas near massive galaxies. While the high-metallicity cold gas seen in LRGs could plausibly result from condensation from a corona, the low-metallicity gas is inconsistent with this interpretation.

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“…On larger scales, observations, simulations, and perturbation theory suggests that galaxies do not strictly show a constant Q but exhibit scale and shape dependence (Jing & Börner 1998;Scoccimarro et al 1998;Takada & Jain 2003;McBride et al 2011;Hoffmann et al 2018). The BAO feature has been detected in the 3PCF measurements of BOSS galaxies (Slepian et al 2017), while other studies focus on the galaxy bispectrum (e.g., Tellarini et al 2016;Desjacques et al 2018;Gualdi et al 2019).…”

Section: Introductionmentioning

confidence: 98%

UV background fluctuations and three-point correlations in the large-scale clustering of the Lyman α forest

Tie

Weinberg

Martini

et al. 2019

Monthly Notices of the Royal Astronomical Society

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Using the Lyα mass assignment scheme (LyMAS), we make theoretical predictions for the 3-dimensional 3-point correlation function (3PCF) of the Lyα forest at redshift z = 2.3. We bootstrap results from the (100 h −1 Mpc) 3 Horizon hydrodynamic simulation to a (1 h −1 Gpc) 3 N -body simulation, considering both a uniform UV background (UVB) and a fluctuating UVB sourced by quasars with a comoving n q ≈ 10 −5 h 3 Mpc −3 placed either in massive halos or randomly. On scales of 10 − 30 h −1 Mpc, the flux 3PCF displays hierarchical scaling with the square of the 2PCF, but with an unusual value of Q ≡ ζ 123 /(ξ 12 ξ 13 + ξ 12 ξ 23 + ξ 13 ξ 23 ) ≈ −4.5 that reflects the low bias of the Lyα forest and the anti-correlation between mass density and transmitted flux. For halo-based quasars and an ionizing photon mean free path of λ = 300 h −1 Mpc comoving, UVB fluctuations moderately depress the 2PCF and 3PCF, with cancelling effects on Q. For λ = 100 h −1 Mpc or 50 h −1 Mpc, UVB fluctuations substantially boost the 2PCF and 3PCF on large scales, shifting the hierarchical ratio to Q ≈ −3. We scale our simulation results to derive rough estimate of the detectability of the 3PCF in current and future observational data sets for the redshift range z = 2.1−2.6. At r = 10 h −1 Mpc and 20 h −1 Mpc, we predict a signal-to-noise (SNR) of ∼ 9 and ∼ 7, respectively, for both BOSS and eBOSS, and ∼ 37 and ∼ 25 for DESI. At r = 40 h −1 Mpc the predicted SNR is lower by a factor of ∼ 3−5. Measuring the flux 3PCF would provide a novel test of the conventional paradigm of the Lyα forest and help separate the contributions of UVB fluctuations and density fluctuations to Lyα forest clustering, thereby solidifying its foundation as a tool of precision cosmology.

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Detection of baryon acoustic oscillation features in the large-scale three-point correlation function of SDSS BOSS DR12 CMASS galaxies

Cited by 133 publications

References 78 publications

The impact of the fiducial cosmology assumption on BAO distance scale measurements

The impact of the fiducial cosmology assumption on BAO distance scale measurements

The Red Dead Redemption Survey of Circumgalactic Gas about Massive Galaxies. I. Mass and Metallicity of the Cool Phase

UV background fluctuations and three-point correlations in the large-scale clustering of the Lyman α forest

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