# A relativistic signature in large-scale structure

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**A relativistic signature in large-scale structure.** / Bartolo, Nicola; Bertacca, Daniele; Bruni, Marco; Koyama, Kazuya; Maartens, Roy; Matarrese, Sabino; Sasaki, Misao; Verde, Licia; Wands, David.

Research output: Contribution to journal › Article › peer-review

### Harvard

*Physics of the Dark Universe*, vol. 13, pp. 30-34. https://doi.org/10.1016/j.dark.2016.04.002

### APA

*Physics of the Dark Universe*,

*13*, 30-34. https://doi.org/10.1016/j.dark.2016.04.002

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### Bibtex

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### RIS

TY - JOUR

T1 - A relativistic signature in large-scale structure

AU - Bartolo, Nicola

AU - Bertacca, Daniele

AU - Bruni, Marco

AU - Koyama, Kazuya

AU - Maartens, Roy

AU - Matarrese, Sabino

AU - Sasaki, Misao

AU - Verde, Licia

AU - Wands, David

N1 - 8 pages, 2 figures. The original claim on galaxy bias for simple inflation models has been corrected; intrinsic non-Gaussianity in the matter density from GR effects is real, but observables that encode this remain to be found. Version accepted by Physics of the Dark Universe, Volume 13, September 2016, Pages 30-34

PY - 2016/9

Y1 - 2016/9

N2 - In General Relativity, the constraint equation relating metric and density perturbations is inherently nonlinear, leading to an effective non-Gaussianity in the dark matter density field on large scales - even if the primordial metric perturbation is Gaussian. Intrinsic non-Gaussianity in the large-scale dark matter overdensity in GR is real and physical. However, the variance smoothed on a local physical scale is not correlated with the large-scale curvature perturbation, so that there is no relativistic signature in the galaxy bias when using the simplest model of bias. It is an open question whether the observable mass proxies such as luminosity or weak lensing correspond directly to the physical mass in the simple halo bias model. If not, there may be observables that encode this relativistic signature.

AB - In General Relativity, the constraint equation relating metric and density perturbations is inherently nonlinear, leading to an effective non-Gaussianity in the dark matter density field on large scales - even if the primordial metric perturbation is Gaussian. Intrinsic non-Gaussianity in the large-scale dark matter overdensity in GR is real and physical. However, the variance smoothed on a local physical scale is not correlated with the large-scale curvature perturbation, so that there is no relativistic signature in the galaxy bias when using the simplest model of bias. It is an open question whether the observable mass proxies such as luminosity or weak lensing correspond directly to the physical mass in the simple halo bias model. If not, there may be observables that encode this relativistic signature.

KW - astro-ph.CO

KW - gr-qc

KW - RCUK

KW - STFC

KW - ST/K00090X/1

KW - ST/L005573/1

KW - General Relativity

KW - Large-scale perturbations

KW - Non-Gaussianity

U2 - 10.1016/j.dark.2016.04.002

DO - 10.1016/j.dark.2016.04.002

M3 - Article

VL - 13

SP - 30

EP - 34

JO - Physics of the Dark Universe

JF - Physics of the Dark Universe

SN - 2212-6864

ER -

ID: 3919555