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Spherical collapse and the halo model in braneworld gravity

Schmidt, Fabian and Hu, Wayne and Lima, Marcos (2010) Spherical collapse and the halo model in braneworld gravity. Physical Review D, 81 (6). Art. No. 063005. ISSN 0556-2821. http://resolver.caltech.edu/CaltechAUTHORS:20100517-101855245

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Abstract

We present a detailed study of the collapse of a spherical perturbation in Dvali-Gabadadze-Porrati (DGP) braneworld gravity for the purpose of modeling simulation results for the halo mass function, bias, and matter power spectrum. The presence of evolving modifications to the gravitational force in the form of the scalar brane-bending mode leads to qualitative differences to the collapse in ordinary gravity. In particular, differences in the energetics of the collapse necessitate a new, generalized method for defining the virial radius which does not rely on strict energy conservation. These differences and techniques apply to smooth dark energy models with w ≠ -1 as well. We also discuss the impact of the exterior of the perturbation on collapse quantities due to the lack of a Birkhoff theorem in DGP. The resulting predictions for the mass function, halo bias, and power spectrum are in good overall agreement with DGP N-body simulations on both the self-accelerating and normal branch. In particular, the impact of the Vainshtein mechanism as measured in the full simulations is matched well. The model and techniques introduced here can serve as practical tools for placing consistent constraints on braneworld models using observations of large-scale structure.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://dx.doi.org/10.1103/PhysRevD.81.063005 DOIArticle
http://prd.aps.org/abstract/PRD/v81/i6/e063005PublisherArticle
Additional Information:© 2010 The American Physical Society. Received 30 November 2009; published 15 March 2010. The simulations used in this work have been performed on the Joint Fermilab—KICP Supercomputing Cluster, supported by grants from Fermilab, Kavli Institute for Cosmological Physics, and the University of Chicago. F. S. acknowledges support from the Gordon and Betty Moore Foundation at Caltech. This work was supported by the Kavli Institute for Cosmological Physics at the University of Chicago through NSF Grants No. PHY- 0114422 and No. PHY-0551142. W.H. was additionally supported by DOE Contract No. DE-FG02-90ER-40560 and the Lucile and David Packard Foundation. M. L. was supported by an NSF-PIRE grant.
Group:Moore Center for Theoretical Cosmology and Physics
Funders:
Funding AgencyGrant Number
Gordon and Betty Moore Foundation UNSPECIFIED
NSFPHY-0114422
NSFPHY-0551142
Department of Energy (DOE)DE-FG02-90ER-40560
Lucile and David Packard FoundationUNSPECIFIED
NSF Partnerships for International Research and Education (PIRE)UNSPECIFIED
Classification Code:PACS: 95.30.Sf, 95.36.+x, 98.80.-k, 98.80.Jk.
Record Number:CaltechAUTHORS:20100517-101855245
Persistent URL:http://resolver.caltech.edu/CaltechAUTHORS:20100517-101855245
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:18323
Collection:CaltechAUTHORS
Deposited By: Tony Diaz
Deposited On:19 May 2010 16:14
Last Modified:20 Jan 2015 17:58

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