Constraining DGP Gravity from Observational Data
Abstract
The accelerating expansion of our universe at present could be driven by an unknown energy component (Dark Energy) or a modification of general relativity (Modified Gravity). In this note we revisit the constraints on a phenomenological model which interpolates between the pure CDM model and the DvaliGabadadzePorrati (DGP) braneworld model with an additional parameter . Combining the cosmic microwave background (CMB), baryon acoustic oscillations (BAO) and type Ia supernovae (SNIa), as well as some highredshift observations, such as the gammaray bursts (GRB) and the measurements of linear growth factors (LGF), we obtain the tight constraint on the parameter ( C.L.), which implies that the flat DGP model is incompatible with the current observations, while the pure CDM model still fits the data very well. Finally, we simulate the future measurements with higher precisions and find that the constraint on can be improved by a factor two, when compared to the present constraints.
I Introduction
Current cosmological observations, such as the CMB measurements of temperature anisotropies and polarization at high redshift Komatsu:2008hk () and the redshiftdistance measurements of SNIa at Kowalski:2008ez (), have demonstrated that the universe is now undergoing an accelerated phase of expansion. The simplest explanation is that this behavior is driven by the cosmological constant or the dynamical dark energy models, which suffers from the severe coincidence and finetuning problems CCproblem (). On the other hand, this observed latetime acceleration of the expansion on the large scales could also be caused by some modifications of general relativity, such as the scalartensor ST () and theories fR (), and gravitational slip slip ().
One of the wellknown examples is the DGP braneworld model DGP (), in which the gravity leaks off the four dimensional brane into the five dimensional spacetime. On small scales gravity is bound to the four dimensional brane and the general relativity is recovered to a good approximation. In the framework of flat DGP model, the Friedmann equation will be modified as DGPCosmology ():
(1) 
where is the crossover scale. At early times, , the Friedmann equation of general relativity is recovered, while in the future, , the expansion is asymptotically de Sitter. Recently there have been a lot of interests in the phenomenological studies relevant to the DGP model in the literature Lue (); DGPRev ().
In this note we investigate an interesting phenomenological model, first introduced in Ref.mDGP (), which interpolates between the pure CDM model and the DGP model with an additional parameter and presents the tight constraints from the current observations and future measurements. The paper is organized as follows: In Sec. II we describe the general formalism of the modified gravity model. Sec. III contains the current observations we use, and Sec. IV includes our main global fitting results. In Sec. V we present the forecasts from the future measurements, while Sec. VI is dedicated the conclusions.
Ii General Formalism
In this phenomenological model, assuming the flatness of our universe, the Friedmann equation is modified as mDGP ():
(2) 
where . Thus, we can straightforwardly rewrite the above equation and obtain the expansion rate as following:
(3) 
where the last term denotes the modification of the Friedmann equation of general relativity:
(4) 
Furthermore, we can obtain the effective equation of state:
(5) 
where the prime denotes the derivative with respect to the redshift .
In Fig.1 we illustrate the evolutions of the effective energy density and for different values of parameter . During the matter dominated era, varies as , which corresponds to the effective equation of state: . In the future , with the matter density , we have and .
Besides the modification of the Friedmann equation, the flat DGP model also changes the growth function of density perturbation . Under assumptions of a quasistatic regime and subhorizon scales, the correct evolution of perturbation was found Lue (); Koyama1 ():
(6) 
where the dot denotes the derivative with respect to the cosmic time , and the factor is given by:
(7) 
However, this phenomenological model Eq.(2) is a parametrization, so the situation is more complicated. One of the possible methods was found by Ref.Koyama2 (). In order to obtain the growth function of density perturbation within a covariant theory, the authors introduced a correction term and assumed the structure of modified theory of gravity to determine this term. Based on those assumptions, it was consequently found that the factor was:
(8) 
In the following analysis, we will use Eq.(6) and Eq.(8) to calculate the growth of density perturbation.
Defined the normalized growth , the growth function Eq.(6) can be rewritten as:
(9)  
where the variable is the ratio of the matter density to the effective energy density . In Fig.2 we plot the linear growth factor as function of scale factor for different values of . One can see that the linear growth factor has been suppressed obviously as long as is larger than zero. Thus, in the literature the linear growth has been widely used to study the modified gravity models, especially the DGP model DGPGrowth ().
Furthermore, the growth factor can be parameterized as gamma ():
(10) 
where is the growth index. And then the growth function becomes:
(11)  
For the pure CDM model, the theoretical value of is , while in the flat DGP model gammavalue ().
In the framework of this phenomenological model, we can easily see that the pure CDM model and flat DGP model can be recovered when and , respectively. In order to be consistent with the cosmological observations, the term should be very small in the early times, such as the Big Bang Nucleosynthesis (BBN) era (). This limit corresponds to the upper bound: mDGP (). On the other hand, when , the effective equation of state will become smaller than , which leads to the instability of linear growth of density perturbation due to the appearance of term Eq.(8).
At early times, such as the matter dominated era, we have and . Thus, Eq.(8) becomes
(12) 
since at . By contrast, at late times the matter energy density and the expansion is asymptotically de Sitter, . And then we have
(13) 
Based on Eq.(12) and Eq.(13), we can straightforwardly see that as long as , during the evolution of universe the value of should change the sign at one pivot redshift , which leads to and . In Fig.3 we have shown the evolution of when fixing . There is an obvious singularity at . Therefore, based on these discussions above, we use a tophat prior on as in our calculations.
Iii Method and Data
In our calculations we assume a flat space and use a uniform prior on the present matter density fraction of the universe: . Furthermore, we constrain the Hubble parameter to be uniformly in Hubble Space Telescope (HST) region: . The resulting plots are produced with CosmoloGUI^{1}^{1}1URL: http://www.sarahbridle.net/cosmologui/..
In this section we will list the cosmological observations used in our calculations: CMB, BAO and SNIa measurements, as well as some highredshift observations, such as the GRB and LGF data. We have taken the total likelihood to be the products of the separate likelihoods () of these cosmological probes. In other words, defining , we get:
(14)  
If the likelihood function is Gaussian, coincides with the usual definition of up to an additive constant corresponding to the logarithm of the normalization factor of .
iii.1 CMB Data
CMB measurement is sensitive to the distance to the decoupling epoch via the locations of peaks and troughs of the acoustic oscillations. Here we use the “WMAP distance information” obtained by the WMAP group Komatsu:2008hk (), which includes the “shift parameter” , the “acoustic scale” , and the photon decoupling epoch ^{2}^{2}2In the revised version of WMAP5 paper Komatsu:2008hk (), they also extend the baryon density into the WMAP distance information. But our calculations are not sensitive to and they also claim that this extension does not affect the constraints. Thus, we fix to be the best fit value obtained by the WMAP group.. and correspond to the ratio of angular diameter distance to the decoupling era over the Hubble horizon and the sound horizon at decoupling, respectively, given by:
(15)  
(16) 
where and denote the comoving distance to and the comoving sound horizon at , respectively. The decoupling epoch is given by zast ():
(17) 
where
(18) 
We calculate the likelihood of the WMAP distance information as follows:
(19) 
where is the parameter vector and is the inverse covariance matrix for the WMAP distance information shown in Table I.
Table I. Inverse covariance matrix for the WMAP distance information , and . The maximum likelihood values are , and , respectively.

iii.2 BAO Data
The BAO information has been already detected in the current galaxy redshift survey. The BAO can directly measure not only the angular diameter distance, , but also the expansion rate of the universe, . But current BAO data are not accurate enough for extracting the information of and separately Okumura:2007br (). Therefore, one can only determine the following effective distance Eisenstein:2005su ():
(20) 
In this note we use the gaussian priors on the distance ratios :
(21) 
with a correlation coefficient of , extracted from the SDSS and 2dFGRS surveys BAO (), where is the comoving sound horizon size and is the drag epoch at which baryons were released from photons given by zd ():
(22) 
where
(23) 
iii.3 SNIa Data
The SNIa data give the luminosity distance as a function of redshift
(24) 
The supernovae data we use in this paper are the recently released Union compilation (307 sample) from the Supernova Cosmology project Kowalski:2008ez (), which include the recent samples of SNIa from the SNLS and ESSENCE survey, as well as some older data sets, and span the redshift range . In the calculation of the likelihood from SNIa we have marginalized over the nuisance parameter, the absolute magnitude , as done in Ref.SNMethod ():
(25) 
where
(26) 
iii.4 GRB Data
GRBs can potentially be used to measure the luminosity distance out to higher redshift than SNIa. Recently, several empirical correlations between GRB observables were reported, and these findings have triggered intensive studies on the possibility of using GRBs as cosmological “standard” candles. However, due to the lack of lowredshift long GRBs data to calibrate these relations, in a cosmologyindependent way, the parameters of the reported correlations are given, assuming an input cosmology, and obviously they depend on the same cosmological parameters that we would like to constrain. Thus, applying such relations to constrain cosmological parameters leads to biased results. In Ref.xiagrb () the circular problem is naturally eliminated by marginalizing over the free parameters involved in the correlations; in addition, some results show that these correlations do not change significantly for a wide range of cosmological parameters Firmani (). Therefore, in this paper we use the 69 GRBs sample over a redshift range from published in Ref.Schaefer:2006pa () but we keep in mind the issues related to the “circular problem” that are more extensively discussed in Ref.xiagrb ().
iii.5 LGF Data
As we point out above, the linear growth factor will be suppressed in the modified gravity model. It will be helpful using the measurements of linear growth factor to constrain the modified gravity models. Therefore, in Table II we list linear growth factors data we use in our analysis: the linear growth rate from galaxy power spectrum at low redshifts Hawkins:2002sg (); Tegmark:2006az (); Ross:2006me (); Guzzo (); daAngela:2006mf () and lyman growth factor measurement obtained with the lyman power spectrum at McDonald:2004xn (). It is worth noting that the data points in Table II are obtained with assuming the CDM model, thus, one should use these data very carefully, especially for the points obtained from Refs.Tegmark:2006az (); Ross:2006me (); daAngela:2006mf (). The corresponding is simply given by:
(27) 
TABLE II. The currently available data for linear growth rates we use in our analysis.

Ref.  
0.15 
0.51  0.11  Hawkins:2002sg () 
0.35  0.70  0.18  Tegmark:2006az () 
0.55  0.75  0.18  Ross:2006me () 
0.77  0.91  0.36  Guzzo () 
1.40  0.90  0.24  daAngela:2006mf () 
3.00  1.46  0.29  McDonald:2004xn () 

Iv Numerical Results
TABLE III. Constraints on the parameters , and . Here we have shown the mean values and errors from the current observations and the standard derivations from the future measurements.



CMB+BAO+SN 

All Real Data  
Future  0.07  0.005  0.050 

In this section we present our main results of constraints on this phenomenological model from the current observational data, as shown in Table III.
In Fig.4 we illustrate the posterior distribution of from the current data. Firstly, we neglect the high redshift probes. The result shows that the current observations yield a strong constraint on the parameter:
(28) 
One can see that the pure CDM model () still fits data very well at uncertainty, which is consistent with the current status of global fitting results Komatsu:2008hk (); xiaglobal (). And the upper limit is , which implies that there is a significant tension between the flat DGP model () and the current observations, which is consistent with other works (e.g. Ref.ariel (); otherDGP ()). However, unlike other works ariel (), in our analysis we use the “WMAP distance information” which includes the “shift parameter” , the “acoustic scale” , and the photon decoupling epoch , instead of only, to constrain this phenomenological model. Recently, many results show that the “WMAP distance information” can give the similar constraints, when compared with the results from the full CMB power spectrum compare (). By contrast, could not be an accurate substitute for the full CMB data and may in principle give some misleading results shift ().
And then, we include some high redshift probes, such as GRB and LGF data sets. From Table III and Fig.4, we can find that the constraint on becomes slightly tighter:
(29) 
and at confidence level. As we have mentioned before, the effective equation of state of this phenomenological model will depart from the cosmological constant boundary at high redshifts. Therefore, these high redshift observations are helpful to improve the constraints on this phenomenological model.
These results (Eqs.(2829)) are not surprising. From Fig.1 we find that the effective equation of state of the flat DGP model, , will depart from the cosmological constant at highredshift universe significantly. But the current constraint on is closed to Komatsu:2008hk (); xiaglobal (), so we require the small value of to match the current observations. There is a small difference that our result slightly favors a nonzero value of , but not significantly, which needs more accurate measurements to verify it further.
In Fig.5 we plot the two dimensional constraint in the (,) panel. and are strongly anticorrelated. The reason of this degeneracy is that the constraint mainly comes from the luminosity and angular diameter distance information. From Eq.(3) and Eq.(4) we can see that when is increased, the contribution of last term to the expansion rate will become large, due to the positive . Consequently, must be decreased correspondingly in order to produce the same expansion rate. When combining those current observational data, the matter energy density has been constrained very stringent: , which is also consistent with the current status of global fitting results Komatsu:2008hk (); xiaglobal (). Naturally, the constraint on will also be improved, because of the tight constraint on the matter energy density.
Furthermore, we also investigate the limit on the growth index and obtain at confidence level. Obviously, the growth index of the pure CDM is consistent with this result. However, the theoretical value of growth index in the flat DGP model, , is disfavored.
V Future Constraints
Since the present data clearly do not give very stringent constraint on the parameter , it is worthwhile to discuss whether future data could determine conclusively. For that purpose we have performed an analysis and chosen the fiducial model as the mean values of Table III obtained from the current constraints.
The projected satellite SNAP (Supernova / Acceleration Probe) would be a space based telescope with a one square degree field of view with pixels. It aims to increase the discovery rate for SNIa to about per year in the redshift range . In this paper we simulate about SNIa according to the forecast distribution of the SNAP Kim:2003mq (). For the error, we follow the Ref.Kim:2003mq () which takes the magnitude dispersion and the systematic error . The whole error for each data is given by:
(30) 
where is the number of supernovae of the th redshift bin. Furthermore, we add as an external data set a mock dataset of 400 GRBs, in the redshift range with an intrinsic dispersion in the distance modulus of and with a redshift distribution very similar to that of Figure 1 of Ref.Hooper:2005xx ().
For the linear growth factors data, we simulate the mock data from the fiducial model with the error bars reduced by a factor of two. This is probably reasonable given the larger amounts of galaxy power spectrum and lyman forest power spectrum data that will become available soon as long with a better control of systematic errors in the next generated large scale structure survey. In addition we also assume a Gaussian prior on the matter energy density as , which is close to future Planck constraints Planck ().
From Table III it is clear that the future measurements with higher precision could improve the constraints dramatically. The standard derivation of is reduced by a factor two. Assuming the mean value remains unchanged in the future, the nonzero value of will be confirmed around confidence level by the future measurements. In addition we also illustrate the two dimensional contour of parameters and in Fig.6. Comparing with the contour in Fig.5, the allowed parameter region has been shrunk significantly. The future measurements could have enough ability to distinguish between the modified gravity model and the pure CDM model.
Vi Conclusions
As an alternative approach to generate the latetime acceleration of the expansion of our universe, models of modifications of gravity have attracted a lot of interests in the phenomenological studies recently. In this note we investigate an interesting phenomenological model which interpolates between the pure CDM model and the flat DGP braneworld model with an additional parameter .
Firstly, we find that when is less than zero, the growth function of density perturbation will appear an apparent singularity. This is because the variable will change the sign during the evolution of our universe. And then the term caused by the modified gravity model will be divergent at some redshift .
From the current CMB, BAO and SNIa data, we obtain a tight constraint on the parameter , which implies that the flat DGP model () is incompatible with the current observations, while the pure CDM model still fits the data very well. When adding the highredshift GRB and LGF data, the constraint is more stringent , which means that these high redshift observations are helpful to improve the constraints on this phenomenological model.
Finally, we simulate the future measurements with higher precisions to limit this phenomenological model. And we find that these accurate probes will be helpful to improve the constraints on the parameters of the model and could distinguish between the modified gravity model and the pure CDM model.
References
 (1) E. Komatsu, et al., arXiv:0803.0547.
 (2) M. Kowalski et al., arXiv:0804.4142.
 (3) S. Weinberg, Rev. Mod. Phys. 61, 1 (1989); I. Zlatev, L. M. Wang and P. J. Steinhardt, Phys. Rev. Lett. 82, 896 (1999).
 (4) S. M. Carroll, V. Duvvuri, M. Trodden, and M. S. Turner, Phys. Rev. D 70, 043528 (2004); C. Schimd, J. P. Uzan and A. Riazuelo, Phys. Rev. D 71, 083512 (2005).
 (5) See e.g. V. Acquaviva, C. Baccigalupi and F. Perrotta, Phys. Rev. D 70, 023515 (2004); P. Zhang, Phys. Rev. D 73, 123504 (2006); Y. S. Song, H. Peiris and W. Hu, Phys. Rev. D 76, 063517 (2007); E. Bertschinger and P. Zukin, Phys. Rev. D 78, 024015 (2008); and references therein.
 (6) S. F. Daniel, R. R. Caldwell, A. Cooray and A. Melchiorri, Phys. Rev. D 77, 103513 (2008); S. F. Daniel, R. R. Caldwell, A. Cooray, P. Serra and A. Melchiorri, arXiv:0901.0919.
 (7) G. R. Dvali, G. Gabadadze and M. Porrati, Phys. Lett. B 485, 208 (2000).
 (8) C. Deffayet, Phys. Lett. B 502, 199 (2001).
 (9) A. Lue, Phys. Rept. 423, 1 (2006).
 (10) C. Deffayet, Int. J. Mod. Phys. D 16 (2008) 2023; R. Durrer and R. Maartens, arXiv:0811.4132; and references therein.
 (11) G. Dvali and M. S. Turner, arXiv:astroph/0301510.
 (12) K. Koyama and R. Maartens, JCAP 0601, 16 (2006).
 (13) K. Koyama, JCAP 0603, 17 (2006).
 (14) E. V. Linder, Phys. Rev. D 72, 043529 (2005); D. Huterer and E. V. Linder, Phys. Rev. D 75, 023519 (2007); D. Polarski, arXiv:astroph/0605532; S. A. Thomas, F. B. Abdalla and J. Weller, arXiv:0810.4863.
 (15) P. J. E. Peebles, LargeScale Structure of the Universe, Princeton Univ. Press, 1980; P. J. E. Peebles, Astrophys. J. 284, 439 (1984); O. Lahav, P. B. Lilje, J. R. Primack and M. J. Rees, Mon. Not. R. Astron. Soc. 251, 128 (1991).
 (16) E. V. Linder and R. N. Cahn, Astropart. Phys. 28, 481 (2007).
 (17) W. Hu and N. Sugiyama, Astrophys. J. 471, 542 (1996).
 (18) T. Okumura, T. Matsubara, D. J. Eisenstein, I. Kayo, C. Hikage, A. S. Szalay and D. P. Schneider, Astrophys. J. 677, 889 (2008).
 (19) D. J. Eisenstein et al. Astrophys. J. 633, 560 (2005).
 (20) W. J. Percival, et al., Mon. Not. Roy. Astron. Soc. 381, 1053 (2007).
 (21) D. Eisenstein and W. Hu, Astrophys. J. 496, 605 (1998).
 (22) E. Di Pietro and J. F. Claeskens, Mon. Not. Roy. Astron. Soc. 341, 1299 (2003).
 (23) H. Li, J. Q. Xia, J. Liu, G. B. Zhao, Z. H. Fan and X. Zhang, Astrophys. J. 680, 92 (2008).
 (24) C. Firmani, V. AvilaReese, G. Ghisellini and G. Ghirlanda, Rev. Mex. Astron. Astrofis. 43, 203 (2007).
 (25) B. E. Schaefer, Astrophys. J. 660, 16 (2007).
 (26) E. Hawkins et al., Mon. Not. Roy. Astron. Soc. 346, 78 (2003); L. Verde et al., Mon. Not. Roy. Astron. Soc. 335, 432 (2002).
 (27) M. Tegmark et al., Phys. Rev. D 74, 123507 (2006).
 (28) N. P. Ross et al., arXiv:astroph/0612400.
 (29) L. Guzzo et al., Nature 451, 541 (2008).
 (30) J. da Angela et al., arXiv:astroph/0612401.
 (31) P. McDonald et al. Astrophys. J. 635, 761 (2005).
 (32) J. Q. Xia, H. Li, G. B. Zhao and X. Zhang, Phys. Rev. D 78, 083524 (2008).
 (33) M. Fairbairn and A. Goobar, Phys. Lett. B 642, 432 (2006); Z. K. Guo, Z. H. Zhu, J. S. Alcaniz and Y. Z. Zhang, Astrophys. J. 646, 1 (2006); S. Rydbeck, M. Fairbairn and A. Goobar, JCAP 0705, 003 (2007); T. M. Davis et al., Astrophys. J. 666, 716 (2007); M. S. Movahed, M. Farhang and S. Rahvar, Int. J. Theor. Phys. 48, 1203 (2009).
 (34) Y. S. Song, Phys. Rev. D 71, 024026 (2005); Y. S. Song, I. Sawicki and W. Hu, Phys. Rev. D 75, 064003 (2007); W. Fang, S. Wang, W. Hu, Z. Haiman, L. Hui and M. May, Phys. Rev. D 78, 103509 (2008); Z. H. Zhu and M. Sereno, arXiv:0804.2917; S. A. Thomas, F. B. Abdalla and J. Weller, arXiv:0810.4863; and references therein.
 (35) P. S. Corasaniti and A. Melchiorri, Phys. Rev. D 77, 103507 (2008); H. Li, J. Q. Xia, G. B. Zhao, Z. H. Fan and X. Zhang, Astrophys. J. 683, L1 (2008).
 (36) O. Elgaroy and T. Multamaki, Astron. Astrophys. 471, 65 (2007).
 (37) A. G. Kim, E. V. Linder, R. Miquel and N. Mostek, Mon. Not. Roy. Astron. Soc. 347, 909 (2004).
 (38) D. Hooper and S. Dodelson, Astropart. Phys. 27, 113 (2007).
 (39) Planck Collaboration, arXiv:astroph/0604069.