Challenges to the DGP model from horizon-scale growth and geometry
Open accessAbstract
We conduct a Markov Chain Monte Carlo study of the Dvali-Gabadadze-Porrati self-accelerating braneworld scenario given the cosmic microwave background (CMB) anisotropy, supernovae and Hubble constant data by implementing an effective dark energy prescription for modified gravity into a standard Einstein-Boltzmann code. We find no way to alleviate the tension between distance measures and horizon-scale growth in this model. Growth alterations due to perturbations propagating into the bulk appear as excess CMB anisotropy at the lowest multipoles. In a flat cosmology, the maximum likelihood Dvali-Gabadadze-Porrati model is nominally a $5.3\ensuremath{\sigma}$ poorer fit than $\ensuremath{\Lambda}\mathrm{CDM}$. Curvature can reduce the tension between distance measures but only at the expense of exacerbating the problem with growth leading to a $4.8\ensuremath{\sigma}$ result that is dominated by the low multipole CMB temperature spectrum. While changing the initial conditions to reduce large-scale power can flatten the temperature spectrum, this also suppresses the large angle polarization spectrum in violation of recent results from the five-year Wilkinson Microwave Anisotropy Probe. The failure of this model highlights the power of combining growth and distance measures in cosmology as a test of gravity on the largest scales.
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The detailed predictions of the self-accelerating branch were inconsistent with cosmological observations.
“Furthermore, the detailed predictions of the SA branch were inconsistent with cosmological observations [13].”
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Cites
Lewis, A., Challinor, A., & Lasenby, A. (2000) · The Astrophysical Journal · doi:10.1086/309179 · Cited by 4,920 · see citing works
Cosmological parameters from CMB and other data: A Monte Carlo approach
Lewis, A., & Bridle, S. (2002) · Physical Review D · doi:10.1103/physrevd.66.103511 · Cited by 3,495 · see citing works
Charmousis, C., Gregory, R., Kaloper, N., & Padilla, A. (2006) · Journal of High Energy Physics · doi:10.1088/1126-6708/2006/10/066 · Cited by 188 · see citing works
Flagged first, then by citations
Research works printed but not linked: 47
- G. R. Dvali, G. Gabadadze and M. Porrati, Phys. Lett. B 485, 208 (2000), [arXiv:hep-th/0005016]. · arXiv
- C. Deffayet, Phys. Lett. B 502, 199 (2001), [arXiv:hep- th/0010186].
- M. A. Luty, M. Porrati and R. Rattazzi, JHEP 09, 029 (2003), [arXiv:hep-th/0303116]. · arXiv
- A. Nicolis and R. Rattazzi, JHEP 06, 059 (2004), [arXiv:hep-th/0404159]. · arXiv
- K. Koyama, Phys. Rev. D 72, 123511 (2005), [arXiv:hep- th/0503191].
- D. Gorbunov, K. Koyama and S. Sibiryakov, Phys. Rev. D 73, 044016 (2006), [arXiv:hep-th/0512097]. · arXiv
- C. Charmousis, R. Gregory, N. Kaloper and A. Padilla, JHEP 10, 066 (2006), [arXiv:hep-th/0604086]. · arXiv
- C. Deffayet, G. Gabadadze and A. Iglesias, JCAP 0608, 012 (2006), [arXiv:hep-th/0607099]. · arXiv
- G. Dvali, New J. Phys. 8, 326 (2006), [arXiv:hep- th/0610013].
- K. Koyama and F. P. Silva, Phys. Rev. D 75, 084040 (2007), [arXiv:hep-th/0702169]. · arXiv
- M. Fairbairn and A. Goobar, Phys. Lett. B 642, 432 (2006), [arXiv:astro-ph/0511029]. · arXiv
- R. Maartens and E. Majerotto, Phys. Rev. D 74, 023004 (2006), [arXiv:astro-ph/0603353]. · arXiv
- Y.-S. Song, I. Sawicki and W. Hu, Phys. Rev. D 75, 064003 (2007), [arXiv:astro-ph/0606286]. · arXiv
- A. Lue, R. Scoccimarro and G. D. Starkman, Phys. Rev. D 69, 124015 (2004), [arXiv:astro-ph/0401515]. · arXiv
- K. Koyama and R. Maartens, JCAP 0601, 016 (2006), [arXiv:astro-ph/0511634]. · arXiv
- S. Wang, L. Hui, M. May and Z. Haiman, Phys. Rev. D 76, 063503 (2007), [arXiv:0705.0165]. · arXiv
- C. Deffayet, Phys. Rev. D 66, 103504 (2002), [arXiv:hep- th/0205084].
- I. Sawicki, Y.-S. Song and W. Hu, Phys. Rev. D 75, 064002 (2007), [arXiv:astro-ph/0606285]. · arXiv
- A. Cardoso, K. Koyama, S. S. Seahra and F. P. Silva, Phys. Rev. D 77, 083512 (2008), [arXiv:0711.2563]. · arXiv
- W. Hu, Phys. Rev. D 77, 103524 (2008), [arXiv:0801.2433]. · arXiv
- W. Hu and I. Sawicki, Phys. Rev. D 76, 104043 (2007), [arXiv:0708.1190]. · arXiv
- WMAP, M. R. Nolta et al., arXiv:0803.0593. · arXiv
- S. Bashinsky, arXiv:0707.0692. · arXiv
- M. Kunz and D. Sapone, Phys. Rev. Lett. 98, 121301 (2007), [arXiv:astro-ph/0612452]. · arXiv
- R. Caldwell, A. Cooray and A. Melchiorri, Phys. Rev. D 76, 023507 (2007), [arXiv:astro-ph/0703375]. · arXiv
- B. Jain and P. Zhang, arXiv:0709.2375. · arXiv
- E. Bertschinger and P. Zukin, arXiv:0801.2431. · arXiv
- C. Deffayet, S. J. Landau, J. Raux, M. Zaldarriaga and P. Astier, Phys. Rev. D 66, 024019 (2002), [arXiv:astro- ph/0201164].
- W. Hu and D. J. Eisenstein, Phys. Rev. D 59, 083509 (1999), [arXiv:astro-ph/9809368]. · arXiv
- E. Bertschinger, Astrophys. J. 648, 797 (2006), [arXiv:astro-ph/0604485]. · arXiv
- A. Lewis, A. Challinor and A. Lasenby, Astrophys. J. 538, 473 (2000), [arXiv:astro-ph/9911177]. · arXiv
- The SNLS, P. Astier et al., Astron. Astrophys. 447, 31 (2006), [arXiv:astro-ph/0510447]. · arXiv
- WMAP, J. Dunkley et al., arXiv:0803.0586, see also http://lambda.gsfc.nasa.gov. · arXiv
- HST, W. L. Freedman et al., Astrophys. J. 553, 47 (2001), [arXiv:astro-ph/0012376]. · arXiv
- A. Lewis and S. Bridle, Phys. Rev. D 66, 103511 (2002), [arXiv:astro-ph/0205436], the code and de- scription of its features are available on the Web site: http://cosmologist.info/cosmomc. · arXiv
- N. Metropolis, A. W. Rosenbluth, M. N. Rosenbluth, A. H. Teller and E. Teller, The Journal of Chemical Physics 21, 1087 (1953).
- W. K. Hastings, Biometrika 57, 97 (1970).
- A. Gelman and D. B. Rubin, Statistical Science 7, 457 (1992).
- WMAP, E. Komatsu et al., arXiv:0803.0547. · arXiv
- D. J. Eisenstein et al., Astrophys. J. 633, 560 (2005), [arXiv:arXiv:astro-ph/0501171]. · arXiv
- G. Hütsi, Astron. Astrophys. 459, 375 (2006), [arXiv:arXiv:astro-ph/0604129]. · arXiv
- W. J. Percival et al., Mon. Not. Roy. Astron. Soc. 381, 1053 (2007), [arXiv:arXiv:0705.3323]. · arXiv
- E. Gaztanaga, A. Cabre and L. Hui, ArXiv e-prints (2008), [arXiv:0807.3551]. · arXiv
- M. J. Mortonson and W. Hu, arXiv:0804.2631. · arXiv
- T. Giannantonio, Y.-S. Song and K. Koyama, arXiv:0803.2238. · arXiv
- M. Zaldarriaga, U. Seljak and E. Bertschinger, Astro- phys. J. 494, 491 (1998), [arXiv:astro-ph/9704265]. · arXiv
- J. Zhang, L. Hui and A. Stebbins, Astrophys. J. 635, 806 (2005), [arXiv:arXiv:astro-ph/0312348]. · arXiv
Cited by
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Testing general relativity in cosmology
Ishak, M. (2019) · Living Reviews in Relativity · doi:10.1007/s41114-018-0017-4 · Cited by 449 · see citing works
Current constraints on the cosmic growth history
Bean, R., & Tangmatitham, M. (2010) · Physical Review D · doi:10.1103/physrevd.81.083534 · Cited by 184 · see citing works
Out of the White Hole: A Holographic Origin for the Big Bang
Pourhasan, R., Afshordi, N., & Mann, R. B. (2014) · Journal of Cosmology and Astroparticle Physics · doi:10.1088/1475-7516/2014/04/005 · Cited by 32 · see citing works
- Authors
- Fang, W., Wang, S., Hu, W., Haiman, Z., Hui, L., & May, M.
- Affiliations
- Columbia University (US)
- University of Chicago (US)
- Brookhaven National Laboratory (US)
- Venue
- Physical Review D
- Publisher
- American Physical Society (APS)
- Published
- 2008-11-10
- Volume
- 78
- Issue
- 10
- ISSN
- 0556-2821 (ISSN-L)
- 1550-7998
- 1550-2368
- OpenAlex
- W2133186943
- Cited by
- 147
- References
- 3
- Citations by year
- 2026: 3 · 2025: 4 · 2024: 3 · 2023: 7 · 2022: 5 · 2021: 8 · 2020: 1 · 2019: 7 · 2018: 9 · 2017: 4 · 2016: 5 · 2015: 6 · 2014: 16 · 2013: 15 · 2012: 12
- FWCI
- 7.77
- Type
- journal article
- Language
- en
- Open access
- green
- arxiv.org
- Locations
- Physical review. D. Particles, fields, gravitation, and cosmology/Physical review. D. Particles and fields (publishedVersion)
- arXiv (Cornell University) (submittedVersion)
- arXiv (Cornell University)
- Funders
- National Science Foundation (0114422, DE-AC02-98CH10886)
- U.S. Department of Energy (DEAC-02-98CH10886, -AC02-98 CH 10886)
- Nemzeti Kutatási és Technológiai Hivatal
- Kavli Institute for Cosmological Physics, University of Chicago
- Fermilab
- Topics
- Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Cosmology and Gravitation Theories
- Physical Sciences › Physics and Astronomy › Statistical and Nonlinear Physics › Noncommutative and Quantum Gravity Theories
- Physical Sciences › Physics and Astronomy › Nuclear and High Energy Physics › Black Holes and Theoretical Physics
- Keywords
- Dvali-Gabadadze-Porrati model, brane cosmology, modified gravity, dark energy, cosmic microwave background anisotropies, large-scale structure growth, Hubble tension, distance measures, curvature, initial conditions, CMB polarization
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