Bias in the effective field theory of large scale structures
We study how to describe collapsed objects, such as galaxies, in the context of the Effective Field Theory of Large Scale Structures. The overdensity of galaxies at a given location and time is determined by the initial tidal tensor, velocity gradients and spatial derivatives of the regions of dark matter that, during the evolution of the universe, ended up at that given location. Similarly to what was recently done for dark matter, we show how this Lagrangian space description can be recovered by upgrading simpler Eulerian calculations. We describe the Eulerian theory. We show that it is perturbatively local in space, but non-local in time, and we explain the observational consequences of this fact. We give an argument for why to a certain degree of accuracy the theory can be considered as quasi time-local and explain what the operator structure is in this case. Furthermore, we describe renormalization of the bias coefficients so that, after this and after upgrading the Eulerian calculation to a Lagrangian one, the perturbative series for galaxies correlation functions results in a manifestly convergent expansion in powers of k/k NL and k/k M, where k is the wavenumber of interest, k NL is the wavenumber associatedmore »
- Authors:
-
[1]
- Stanford Univ., CA (United States). Stanford Inst. of Theoretical Physics (ITP); Kavli Institute for Particle Astrophysics and Cosmology, SLAC and Stanford Univ., Menlo Park, CA (United States)
- Publication Date:
- Report Number(s):
- SLAC-PUB-16640
Journal ID: ISSN 1475-7516; arXiv:1406.7843
- Grant/Contract Number:
- AC02-76SF00515
- Type:
- Accepted Manuscript
- Journal Name:
- Journal of Cosmology and Astroparticle Physics
- Additional Journal Information:
- Journal Volume: 2015; Journal Issue: 11; Journal ID: ISSN 1475-7516
- Publisher:
- Institute of Physics (IOP)
- Research Org:
- SLAC National Accelerator Lab., Menlo Park, CA (United States)
- Sponsoring Org:
- USDOE Office of Science (SC)
- Country of Publication:
- United States
- Language:
- English
- Subject:
- 79 ASTRONOMY AND ASTROPHYSICS; astrophysics; gravitation and cosmology; phenomenology-HEP; Theory-HEP; ASTRO; cosmological perturbation theory; power spectrum; cosmological parameters from LSS; baryon acoustic oscillations
- OSTI Identifier:
- 1263394
Senatore, Leonardo. Bias in the effective field theory of large scale structures. United States: N. p.,
Web. doi:10.1088/1475-7516/2015/11/007.
Senatore, Leonardo. Bias in the effective field theory of large scale structures. United States. doi:10.1088/1475-7516/2015/11/007.
Senatore, Leonardo. 2015.
"Bias in the effective field theory of large scale structures". United States.
doi:10.1088/1475-7516/2015/11/007. https://www.osti.gov/servlets/purl/1263394.
@article{osti_1263394,
title = {Bias in the effective field theory of large scale structures},
author = {Senatore, Leonardo},
abstractNote = {We study how to describe collapsed objects, such as galaxies, in the context of the Effective Field Theory of Large Scale Structures. The overdensity of galaxies at a given location and time is determined by the initial tidal tensor, velocity gradients and spatial derivatives of the regions of dark matter that, during the evolution of the universe, ended up at that given location. Similarly to what was recently done for dark matter, we show how this Lagrangian space description can be recovered by upgrading simpler Eulerian calculations. We describe the Eulerian theory. We show that it is perturbatively local in space, but non-local in time, and we explain the observational consequences of this fact. We give an argument for why to a certain degree of accuracy the theory can be considered as quasi time-local and explain what the operator structure is in this case. Furthermore, we describe renormalization of the bias coefficients so that, after this and after upgrading the Eulerian calculation to a Lagrangian one, the perturbative series for galaxies correlation functions results in a manifestly convergent expansion in powers of k/kNL and k/kM, where k is the wavenumber of interest, kNL is the wavenumber associated to the non-linear scale, and kM is the comoving wavenumber enclosing the mass of a galaxy.},
doi = {10.1088/1475-7516/2015/11/007},
journal = {Journal of Cosmology and Astroparticle Physics},
number = 11,
volume = 2015,
place = {United States},
year = {2015},
month = {11}
}
- Free Publicly Accessible Full Text
-
Accepted Manuscript (DOE)
- Publisher's Version of Record
- https://doi.org/10.1088/1475-7516/2015/11/007