Cosmographic constraints on a class of Palatini \mathbf{f(R)} gravity

Cosmographic constraints on a class of Palatini gravity

N.    J.    J. S. Departamento de Física, Universidade Federal do Rio G. do Norte, 59072-970 Natal - RN, Brasil Observatório Nacional, 20921-400 Rio de Janeiro - RJ, Brasil
July 16, 2019

Modified gravity, known as gravity, has presently been applied to Cosmology as a realistic alternative to dark energy. For this kind of gravity the expansion of the Universe may accelerate while containing only baryonic and cold dark matter. The aim of the present investigation is to place cosmographic constraints on the class of theories of the form within the Palatini approach. Although extensively discussed in recent literature and confronted with several observational data sets, cosmological tests are indeed inconclusive about the true signal of in this class of theories. This is particularly important to define which kind of corrections (infra-red or high-energy) to general relativity this class of theory indeed represent. We shed some light on this question by examining the evolution of the deceleration parameter for these theories. We find that for a large range of , models based on gravity in th e Palatini approach can only have positive values for , placing thus a broad restriction on this class of gravity.

cosmological parameters — modified gravity — Palatini approach

I Introduction

gravity examines the possibility of modifying Einstein’s general relativity (GR) by adding terms proportional to powers of the Ricci scalar to the Einstein-Hilbert Lagrangian Starobinsky (). The cosmological interest in these theories comes from the fact that they can naturally exhibit an accelerating expansion phase of the universe without introducing dark energy. However, the freedom in the choice of different functional forms of gives rise to the problem of how to constrain the many possible gravity theories on theoretical and/or observational grounds. In this regard, much efforts have been developed so far, mainly from the theoretical viewpoint Ferraris () (see also Refs. Francaviglia () for recent reviews). General principles such as the so-called energy conditions energy_conditions (), nonlocal causal structure RSantos (), have also been taken into account in order to clarify its subtleties. More recently, observational cons traints from several cosmological data sets have been explored for testing the viability of these theories Amarzguioui (); Tavakol (); Janilo (); Fabiocc (); Yang (); Li (); Koivisto (); Fairbairn ().

An important aspect that is worth emphasizing concerns the two different variational approaches that may be followed when one works with -gravity theories, namely, the metric and the Palatini formalisms (see, e.g., Francaviglia ()). In the metric formalism the connections are assumed to be the Christoffel symbols and the variation of the action is taken with respect to the metric, whereas in the Palatini variational approach the metric and the affine connections are treated as independent fields and the variation is taken with respect to both. In fact, these approaches are equivalents only in the context of GR, i.e., in the case of linear Hilbert action; for a general term in the action, they provide completely different theories, with almost no similarities and very distinct equations of motion444These differences also extend to the observational aspects of these approaches. For instance, we note that cosmological models based on a power-law function all form in the metric approach fail in reproducing the standard matter-dominated era followed by an acceleration phase Amendola (), whereas in the Palatini approach, analysis of a dynamical autonomous systems for the same Lagrangian density have shown that such theories admit the three post inflationary phases of the standard cosmological model Tavakol ()..

In this brief report we will restrict ourselves to the Palatini formalism. By discussing the deceleration/acceleration history of the Universe through the evolution of the deceleration parameter , we place stringent bounds on a class of theory given by . In particular, we find that the range of negative values of predicts a behavior that is grossly inconsistent with cosmological observations (e.g. CMB WMAP-7 ()), being therefore ruled out even if it is compatible with supernova, lensing statistics and local gravity constraints.

Ii Palatini cosmologies

cosmologies are based in the modified Einstein equations of motion derived from the dubbed gravity. The action that defines an gravity is given by


where , is the determinant of the metric tensor and is the standard action for the matter fields. Treating the metric and the connection as completely independent fields, variation of this action with respect to the metric provides the field equations


while variation with respect to the connection gives


In (2) is the matter energy-momentum tensor which, for a perfect-fluid, is given by , where is the energy density, is the fluid pressure and is the fluid four-velocity. Here, we adopt the notation and . The second equation (3) give us the connections , which are related with the Christoffel symbols of the metric by


Note that in (2), must be calculated in the usual way, i.e., in terms of the independent connection , given by (4) and its derivatives.

We assume a homogeneous and isotropic Friedmann-Lemaître-Robertson-Walker universe whose metric is , where is the cosmological scale factor. The generalized Friedmann equation, obtained from (2), can be written in terms of the redshift parameter and the density parameter as


where is the matter density today. In terms of these quantities, the trace of Eq. (2) provides an important relation:


Iii Cosmographic constraints

Cosmographic parameters linked to geometry play a key role in cosmology. In particular, the deceleration parameter, defined as , can be written in terms of and its derivative as


In what follows we use (5) and (7) to place constraints on the free parameters () of one of the most extensively discussed theory, i.e.,


Note that positive values of provide IR modifications of GR while negative ones correspond to high-energy corrections. For this kind of gravity reduces to Einstein’s general relativity plus a cosmological constant, . It is worth noting that, for a theory like (8), Eq. (6) evaluated at imposes the following relation between and the pair ()


where is the value of the Ricci scalar today. Note also that can be determined from the algebraic equation resulting from equating (5) and (6) for . Hence, specifying the values of two of these parameters the third is automatically fixed. In other words, in the Palatini approach, one of the two free parameters and can be eliminated by the constraint (9).

Test Ref.
SNe Ia (Gold)555+ CMB + BAO Amarzguioui () [-0.3,0.3] [-6.8,-2.2]
SNe Ia (SNLS) Tavakol () [-0.23,0.42] [2.73,10.6]
SNe Ia (Union) Janilo () [-0.3,0.1] [1.3,5.5]
Fabiocc () [-0.25,0.35] [2.3,7.1]
Strong lensing Yang () [-0.202,0.078] [2.89,4.67]
SNLS + WMAP + SDSS666 + BAO + matter power spectrum + TT CMB spectrum Li ()  [-5.98,-2.12]
SDSS777+ CMB + matter power spectrum Koivisto ()  [-2.321,1.329]
Table 1: Current constraints on and for a gravity given by (8). The CDM model corresponds to and ).

Recently, the observational viability of the functional form (8) have been discussed by several groups. Constraints from distance measurements to type-Ia Supernova (SNe Ia) Amarzguioui (); Tavakol (); Janilo (), determinations by differential age method Fabiocc (), strong lensing statistics Yang (), matter power spectra Li (), Baryon Acoustic Oscillation peak (BAO) and CMB shift parameter have been derived providing the following intervals and , at (C.L.) (see Table 1).

However, a glance through Table 1 shows that cosmological tests are indeed inconclusive about the true signal of . This in turn gives rise to the following question: what kind of corrections to GR do theories like (8) indeed represent? The answer to this question surely depends of the signal of the parameter . In what follows, we show that some light can be shed on this discussion just by examining the signal of , as given by (7) and taking into account (5)–(6).

Figure 1: Cosmic deceleration/acceleration history as a function of redshift for the gravity theory given by (8). Several cases are shown for selected values of and . While positive values of provides a evolution very similar to the standard CDM model, negative values of predict either an always accelerating universe or two periods of acceleration separated by a deceleration phase.

In Fig. 1 we show the evolution of the deceleration parameter with for several values of and , which corresponds to the best-fit value found from a joint analysis involving SNe Ia + BAO + CMB + data Janilo (); Fabiocc (). As can be seen from Fig. 1, for positive values of , approaches the standard CDM evolution at intermediary redshifts and the Universe has only one recent transition toward an accelerating universe. In this case, the transition redshift does not vary considerably with .

On the other hand, negative values of have great influence on the evolution. In particular, we find that models given by (8) with predicts an always accelerating universe, which is clearly incompatible with a past dark matter-dominated epoch (and the standard law), whose existence is fundamental for the structure formation process to take place888This value of is slightly dependent on the matter density parameter in the [0.1, 0.3].. Note that for these modified scenarios predict two recent periods of acceleration separated by a deceleration phase.

Fig. 2 shows the first transition redshift as a function of . We find that the first epoch of acceleration is pushed to higher redshifts as approaches zero from negative values and that such an effect is extremely sensitive to this parameter. For instance, for the first transition happens at very high () whereas for it occurs during the matter epoch (). It is also worth mentioning that, although we have plotted Figs. 1 and 2 for a single value of (= 0.26), we have indeed repeated our analysis for a larger interval (). We found that the behavior of and is very similar to the one shown in both figures, which means that for the current allowed range of the matter density parameter, negative values of are incompatible with a past matter-dominated epoch. This means that to be consistent with cosm ological observations from LSS and CMB data the only correction to GR from a -gravity like (8) is a IR modification (). Note that an exception to this conclusion is the limit (from negative values), which for all practical purposes is equivalent to the late-time evolution of the standard CDM scenario.

Figure 2: The first transition redshift () as a function of . Note that as the epoch of the first acceleration phase is pushed to higher .

Iv Concluding Remarks

Cosmological models based on gravity may exhibit a natural acceleration mechanism without introducing a dark energy component. However, in order to provide a realistic alternative describing the late-time dynamics of the Universe, it is qualitatively well accepted (since the current observational data are inconclusive to this respect – see Table I) that such theories must provide only an IR correction to GR. In this paper, we have discussed quantitatively this question by studying the evolution of the deceleration parameter with and imposing the existence of a past matter-dominated epoch. For the class of gravity given by (8), we have shown that negative values of (high-energy correction) predict either an always accelerating universe (which is inconsistent with the past structure formation process) or two periods of acceleration separated by a deceleration phase. These results show that even passing the background tests (such as supernova ) and escaping from local gravity constraints practically the entire branch of negative values of is ruled out by the cosmographic bounds discussed here.

The authors acknowledge financial support from Conselho Nacional de Desenvolvimento Científico e Tecnológico (CNPq - Brazil) and Instituto Nacional de Estudos do Espaço (INEspaço). NP and JS also thank FAPERN for the grants under which this work was carried out.


  • (1) A. A. Starobinsky, Phys. Lett. B 91, 99 (1980); R. Kerner, Gen. Relativ. Gravit. 14, 453 (1982); J. D. Barrow and A. C. Ottewill, J. Phys. A: Math. Gen. 16, 2757 (1983); J. D. Barrow and S. Cotsakis, Phys. Lett. B 214, 515 (1988); B. Li and J. D. Barrow, Phys. Rev. D 75, 084010 (2007).
  • (2) M. Ferraris, M. Francaviglia and I. Volovich, Class. Quantum Grav. 11, 1505 (1994); A.D. Dolgov and M. Kawasaki, Phys. Lett. B 573, 1 (2003); É. É. Flanagan, Phys. Rev. Lett. 92, 071101 (2004); G. J. Olmo, Phys. Rev. D 72, 083505 (2005); Phys. Rev. D 75, 023511 (2007); Phys. Rev. Lett. 98, 061101 (2007); S. Capozziello, S. Nojiri, S.D. Odintsov and A. Troisi, Phys. Lett. B 639, 135 (2006); A. W. Brookfield, C. van de Bruck and L.M.H. Hall, Phys. Rev. D 74, 064028 (2006); T. Multamäki and I. Vilja, Phys. Rev. D 73, 024018 (2006); N. J. Poplawski, Phys. Rev. D 74, 084032 (2006); A. de la Cruz-Dombriz and A. Dobado, Phys. Rev. D 74, 087501 (2006); L. Amendola, R. Gannouji, D. Polarski and S. Tsujikawa, Phys. Rev. D 75, 083504 (2007); L. Amendola, D. Polarski and S. Tsujikawa, Int. J. Mod. Phys. D 16, 1555 (2007); W. Hu and I. Sawicki, Phys. Rev. D 76, 064004 (2007); Y.-S. Song, W. Hu and I. Sawicki, Phys. Rev. D 75, 044004 (2007); O. Bertolami, C.G. Böhmer, T. Harko and F.S.N. Lobo, Phys. Rev. D 75, 104016 (2007); B. Li, J.D. Barrow and D.F. Mota, Phys. Rev. D 76, 104047 (2007); I. Navarro and K. Van Acoleyen, JCAP 0702, 022 (2007); S. Baghram, M. Farhang and S. Rahvar, Phys. Rev. D 75, 044024 (2007); T. P. Sotiriou, Phys. Lett. B 645, 389 (2007); C.G. Böhmer, T. Harko and F.S.N. Lobo, JCAP 0803, 024 (2008); S.A. Appleby and R.A. Battye, JCAP 0805, 019 (2008); E. Barausse, T.P. Sotiriou and J.C. Miller, Class. Quantum Grav. 25, 105008 (2008); G. Cognola, E. Elizalde, S. Nojiri, S.D. Odintsov, L. Sebastiani and S.Zerbini, Phys. Rev. D 77, 046009 (2008); S. Nojiri and S.D. Odintsov, Phys. Rev. D 77, 026007 (2008); T. P. Sotiriou, S. Liberati and V. Faraoni, Int. J. Mod. Phys. D 17, 399 (2008); S. Nojiri and S.D. Odintsov, Phys. Rev. D 78, 046006 (2008); T.P. Sotiriou, Phys. Lett. B 664, 225-228 (2008); C.S.J. Pun, Z. Kovács and T. Harko, Phys. Rev. D 78, 024043 (2008); V. Faraoni, Phys. Lett. B 665, 135-138 (2008); S. DeDeo and D. Psaltis, Phys. Rev. D 78, 064013 (2008); S.H. Pereira, C.H. Bessa and J.A.S. Lima, arXiv:0911.0622 [astro-ph.CO]; G. Cognola, E. Elizalde, S. Nojiri, S.D. Odintsov, P. Tretyakov and S.Zerbini, Phys. Rev. D 79, 044001 (2009); V. Faraoni, Phys. Rev. D 81, 044002 (2010); T. Harko, Phys. Rev. D 81, 044021 (2010); T. Narikawa and K. Yamamoto, Phys. Rev. D 81, 043528 (2010); T. Multamäki, J. Vainio and I. Vilja, Phys. Rev. D 81, 064025 (2010); J. Kluson̆, Phys. Rev. D 81, 064028 (2010); E. Santos, Phys. Rev. D 81, 064030 (2010).
  • (3) S. Capozziello and M. Francaviglia, Gen. Relativ. Gravit. 40, 357 (2008); T. P. Sotiriou and V. Faraoni, Rev. Mod. Phys. 82, 451 (2010); A. De Felice and S. Tsujikawa, arXiv:1002.4928 [gr-qc].
  • (4) J.H. Kung, Phys. Rev. D 53, 3017 (1996); S.E.P. Bergliaffa, Phys. Lett. B 642, 311 (2006); J. Santos, J.S. Alcaniz, M.J. Rebouças and F.C. Carvalho, Phys. Rev. D 76, 083513 (2007); K. Atazadeh, A. Khaleghi, H. R. Sepangi and Y. Tavakoli, Int. J. Mod. Phys. D 18, 1101 (2009); O. Bertolami and M.C. Sequeira, Phys. Rev. D 79, 104010 (2009); J. Santos, M.J. Rebouças and J.S. Alcaniz, arXiv:0807.2443 [astro-ph].
  • (5) T. Clifton and J. D. Barrow, Phys. Rev. D 72, 123003 (2005). M.J. Rebouças and J. Santos, Phys. Rev. D 80, 063009 (2009); J. Santos, M.J. Rebouças and T.B.R.F. Oliveira, arXiv:1004.2501 [astro-ph.CO].
  • (6) M. Amarzguioui, Ø. Elgarøy, D.F. Mota and T. Multamäki, Astron. Astrophys. 454, 707 (2006).
  • (7) S. Fay, R. Tavakol and S. Tsujikawa, Phys. Rev. D 75, 063509 (2007).
  • (8) J. Santos, J. S. Alcaniz, F. C. Carvalho, N. Pires, Phys. Lett. B 669, 14 (2008).
  • (9) F.C. Carvalho, E.M. Santos, J.S. Alcaniz and J. Santos, J. Cosmology Astroparticle Phys.: JCAP 09, 008 (2008);
  • (10) X.-J. Yang and Da-M. Chen, Mon. Not. R. Astron. Soc. 394, 1449 (2009).
  • (11) B. Li, K. C. Chan and M.-C. Chu, Phys. Rev. D 76, 024002 (2007).
  • (12) T. Koivisto, Phys. Rev. D 73, 083517 (2006).
  • (13) A. Borowiec, W. Godłowski and M. Szydłowski, Phys. Rev. D 74, 043502 (2006); B. Li and M.-C. Chu, Phys. Rev. D 74, 104010 (2006); M. Fairbairn and S. Rydbeck, JCAP 0712, 005 (2007); M. S. Movahed, S. Baghram and S. Rahvar, Phys. Rev. D 76, 044008 (2007); T. Koivisto, Phys. Rev. D 76, 043527 (2007); H. Oyaizu, M. Lima and W. Hu, Phys. Rev. D 78, 123524 (2008); C.-B. Li, Z.-Z. Liu and C.-G. Shao, Phys. Rev. D 79, 083536 (2009); K.W. Masui, F. Schmidt, Ue-L. Pen and P. McDonald, Phys. Rev. D 81, 062001 (2010).
  • (14) L. Amendola, D. Polarski and S. Tsujikawa, Phys. Rev. Lett. 98, 131302 (2007).
  • (15) E. Komatsu et al., Seven-year Wilkinson microwave anisotropy probe (WMAP) observations: Cosmological interpretation, arxiv:1001.4538 [astro-ph.CO].
  • (16) R. Jimenez and A. Loeb, Astrophys. J. 573, 37 (2002).
  • (17) S.M. Carroll, V. Duvvuri, M. Trodden and M.S. Turner, Phys. Rev. D 70, 043528 (2004).
Comments 0
Request Comment
You are adding the first comment!
How to quickly get a good reply:
  • Give credit where it’s due by listing out the positive aspects of a paper before getting into which changes should be made.
  • Be specific in your critique, and provide supporting evidence with appropriate references to substantiate general statements.
  • Your comment should inspire ideas to flow and help the author improves the paper.

The better we are at sharing our knowledge with each other, the faster we move forward.
The feedback must be of minimum 40 characters and the title a minimum of 5 characters
Add comment
Loading ...
This is a comment super asjknd jkasnjk adsnkj
The feedback must be of minumum 40 characters
The feedback must be of minumum 40 characters

You are asking your first question!
How to quickly get a good answer:
  • Keep your question short and to the point
  • Check for grammar or spelling errors.
  • Phrase it like a question
Test description