1 Introduction

Vacuum dynamics in the Universe versus a rigid const.111Invited review paper based on the invited plenary talk by J. Solà at the Conference on Cosmology, Gravitational Waves and Particles, NTU, Singapore, 2017. Some of the results and discussions presented here have been further updated and slightly expanded with respect to the published version.

Joan Solà, Adrià Gómez-Valent, and Javier de Cruz Pérez

Departament de Física Quàntica i Astrofísica, and Institute of Cosmos Sciences,

Universitat de Barcelona,

Av. Diagonal 647, E-08028 Barcelona, Catalonia, Spain

E-mails: sola@fqa.ub.edu, adriagova@fqa.ub.edu, decruz@fqa.ub.edu

Abstract. In this year, in which we celebrate 100 years of the cosmological term, , in Einstein’s gravitational field equations, we are still facing the crucial question whether is truly a fundamental constant or a mildly evolving dynamical variable. After many theoretical attempts to understand the meaning of , and in view of the enhanced accuracy of the cosmological observations, it seems now mandatory that this issue should be first settled empirically before further theoretical speculations on its ultimate nature. In this work, we summarize the situation of some of these studies. Devoted analyses made recently show that the const. hypothesis, despite being the simplest, may well not be the most favored one. The overall fit to the cosmological observables SNIa+BAO++LSS+CMB singles out the class RVM of the “running” vacuum models, in which is an affine power-law function of the Hubble rate. It turns out that the performance of the RVM as compared to the “concordance” CDM model (with const.) is much better. The evidence in support of the RVM may reach c.l., and is bolstered with Akaike and Bayesian criteria providing strong evidence in favor of the RVM option. We also address the implications of this framework on the tension between the CMB and local measurements of the current Hubble parameter.

1 Introduction

One hundred years ago, in mid-February 1917, the famous seminal paper in which Einstein introduced the cosmological term (actually denoted “” in it), as a part of the generally covariant gravitational field equations, was published [1]. Fourteen years later, the idea of as a fundamental piece of these equations was abandoned by Einstein himself [2]; and only one year later the Einstein-de Sitter model, modernly called the cold dark matter model (CDM), was proposed with no further use of the term for the description of the cosmological evolution [3]. The situation with did not stop here and it took an unexpected new turn when reappeared shortly afterwards in the works of Lemaître [4], wherein was associated to the concept of vacuum energy density through the expression – in which is Newton’s constant. This association is somehow natural if we take into account that the vacuum energy is thought of as being uniformly distributed in all corners of space, thus preserving the Cosmological Principle. The problem (not addressed by Lemaître) is to understand the origin of the vacuum energy in fundamental physics, namely in the quantum theory and more specifically in quantum field theory (QFT). Here is where the cosmological constant (CC) problem first pops up. It was first formulated in preliminary form by Zeldovich 50 years ago [5].

The CC problem [6, 7, 8] is the main source of headache for every theoretical cosmologist confronting his/her theories with the measured value of [9, 10, 11]. The purported discovery of the Higgs boson at the LHC has actually accentuated the CC problem greatly, certainly much more than is usually recognized [8]. Owing to the necessary spontaneous symmetry breaking (SSB) of the electroweak (EW) theory, there emerges an induced contribution to that must also be taken into account. These SSB effects are appallingly much larger (viz. ) than the tiny value GeV extracted from observations222Being a density, and hence a dimensionful quantity, “tiny” value means only within the particle physics standards, of course. . So the world-wide celebrated “success” of the Higgs finding in particle physics actually became a cosmological fiasco, since it automatically detonated the “modern CC problem”, i.e. the confirmed size of the EW vacuum, which should be deemed as literally “real” (in contrast to other alleged – ultralarge – contributions from QFT) or “unreal” as the Higgs boson itself! One cannot exist without the other. Such uncomfortable situation of the Higgs boson with cosmology might be telling us that the found Higgs boson is not a fundamental particle, as in such a case the EW vacuum could not be counted as a fundamental SSB contribution to the vacuum energy of the universe. We refer the reader to some review papers [6, 7], including [8, 12], for a more detailed presentation of the CC problem. Setting aside the “impossible” task of predicting the value itself – unless it is understood as a “primordial renormalization” [13] – we will focus here on a special class of models in which appears neither as a rigid constant nor as a scalar field (quintessence and the like) [7], but as a “running” quantity in QFT in curved spacetime. This is a natural option for an expanding universe. As we will show, such kind of dynamical vacuum models are phenomenologically quite successful; in fact so successful that they are currently challenging the CDM [14, 15, 16, 17, 18], see specially the most recent works [19, 20, 21, 22, 23], in which the most significant signs of vacuum dynamics have been found. Potential time variation of the fundamental constants associated to these models has also been explored in [24, 25, 26, 27, 28, 29], and can be used as complementary experimental signatures for them.

2 Running vacuum as the next-to-minimal step beyond the Cdm

The “concordance” or CDM model, i.e. the standard model of cosmology is based on the assumption of the existence of dark matter (DM) and the spatial flatness of the Friedmann-Lemaître-Robertson-Walker (FLRW) metric. At the same time the model is based on the existence of a nonvanishing but rigid (and positive) cosmological constant term: const. The model was first proposed as having the minimal ingredients for a possible successful phenomenological description of the data by Peebles in 1984 [30]. Nowadays we know it is consistent with a large body of observations, and in particular with the high precision data from the cosmic microwave background (CMB) anisotropies [9].

The rigid const. term in the concordance CDM model is the simplest (perhaps too simple) possibility. The running vacuum models (RVMs) (cf. [8, 12] and references therein) build upon the idea that the cosmological term , and the corresponding vacuum energy density, , should be time dependent quantities in cosmology. It is difficult to conceive an expanding universe with a strictly constant vacuum energy density that has remained immutable since the origin of time. Rather, a smoothly evolving DE density that inherits its time-dependence from cosmological variables, such as the Hubble rate , or the scale factor , is not only a qualitatively more plausible and intuitive idea, but is also suggested by fundamental physics, in particular by QFT in curved spacetime. We denote it in general by . Despite its time evolution, it may still have the vacuum equation of state (EoS) , or a more general one , or even a dynamical effective EoS . The main standpoint of the RVM class of dynamical DE models is that “runs” because the effective action receives quantum effects from the matter fields. The leading effects may generically be captured from a renormalization group equation (RGE) of the form [8]


The running scale is typically identified with or related variables. The RVM ansatz is that because will be naturally associated to the Hubble parameter at a given epoch , and hence should evolve with the rate of expansion . Notice that can involve only even powers of the Hubble rate (because of the covariance of the effective action) [8]. The coefficients , , … are dimensionless, and the are the masses of the particles in the loops. Because can be in general a linear combination of the homogeneous terms and , it is obvious that upon integration of the above RGE we expect the following general type of (appropriately normalized) RVM density [8, 12, 13]:


where and are dimensionless parameters, but has dimension (energy squared) in natural units. We emphasize that so as to insure a smooth CDM limit when the dimensionless coefficients and are set to zero 333It is important to make clear that models with (for any and ) are ruled out by the observations, as shown in [14, 15, 16]. This conclusion also applies to all DE models of the form , with a linear term admitted only on phenomenological grounds [14, 15]. In particular, the model is strongly ruled out, see [15] (and the discussion in its Appendix).. The interesting possibility that and/or are nonvanishing may induce a time evolution of the vacuum energy density. These dimensionless coefficients can be computed in QFT from the ratios squared of the masses to the Planck mass [31], and are therefore small as expected from their interpretation as -function coefficients of the RGE (1). Since some of the masses inhabit the GUT scale GeV, the values of need not be very small, typically at most upon accounting for the large multiplicities that are typical in a GUT – see Ref.[31] for a concrete estimate.

Finally, we note that the -terms in (2) are irrelevant for the study of the current universe, but are essential for the correct account of the inflationary epoch in this context and to explain the graceful exit and entropy problems [12, 13]. The RVM (2) is therefore capable of providing a unified dynamical vacuum picture for the entire cosmic evolution [32, 33, 34].

Concerning the parameters and , they must be determined phenomenologically by confronting the model to the wealth of observations. It is remarkable that the aforementioned theoretical estimate [31], leading to , is of the order of magnitude of the phenomenological determination [19, 14, 15, 16, 17, 18]. For the current presentation, however, we will assume hereafter and will focus on the implications for the current universe of the canonical RVM:


We will use the above expression to study the RVM background cosmology and the corresponding perturbations equations. We can compare with the concordance CDM cosmology by just setting in the obtained results. The background cosmological equations for the RVM take on the same form as in the CDM by simply replacing the rigid cosmological term with the dynamical vacuum energy density (3). In this way we obtain the generalized Friedmann’s and acceleration equations, which read as follows:


where and are the EoS parameters of the matter fluid and of the DE, respectively. It is well known that for relativistic and nonrelativistic matter, respectively. Then, for simplicity, we will denote the EoS of the DE component simply as . The explicit solution will depend of course on whether we assume that the DE is canonical vacuum energy (), in which case can be properly denoted as , or dynamical DE with . In some cases can also be a function of time or of some cosmic variable, but we shall not consider this possibility here – see, however, Ref. [14] in which such situation would be mandatory. The solution of the cosmological equations may also depend on whether the gravitational coupling is constant or also running with the expansion, (as itself). And, finally, it may depend on whether we assume that there exists an interaction of the DE with the matter (mainly DM). Whatever it be the nature of our assumptions on these important details, they must be of course consistent with the Bianchi identity, which is tantamount to saying with the local covariant conservation laws. In fact, these possibilities have all been carefully studied in the literature and the complete solution of the cosmological equations has been provided in each case [20, 21, 23, 19, 22, 14, 15, 16, 17, 18]. In what follows we report only on some of the solutions for the densities of matter and DE in the case when there is an interaction between the DE and matter at fixed . At the same time we will compare the result when the EoS of the DE is (which means that we will leave this parameter also free in the fit) and when (the strict vacuum case).

3 Canonical RVM with conserved baryon and radiation densities

The total matter density can be split into the contribution from baryons and cold DM, namely . In the following we assume that the DM density is the only one that carries the anomaly, whereas radiation and baryons are self-conserved, so that their energy densities evolve in the standard way and . On the other hand the dynamical evolution of the vacuum is given by Eq. (3). Since it is only the DM that exchanges energy with the vacuum, the local conservation law reads as follows:


The source function is a calculable expression from (3) and Friedmann’s equation in (4). We find: . It can be useful to compare the canonical RVM with two alternative dynamical vacuum models (DVMs) with different forms of the interaction sources. Let us therefore list the three models under comparison, which we denote RVM, and according to the structure of the interaction source, or also for convenience just I, II and III:


Each model has a characteristic (dimensionless) parameter as a part of the interaction source, which must be fitted to the observational data. Notice that the three model names are preceded by to recall that, in the general case, the equation of state (EoS) is very near to the vacuum one (, with ). For this reason these dynamical quasi-vacuum models are also denoted as DVMs. In the particular case (i.e. ) the DVMs become just the canonical DVMs. As an example, let us provide the matter and vacuum energy densities for the RVM:




For the corresponding expressions of the other models, see [22, 23]. Models II and III were previously studied in different approximations e.g. in [35, 37, 36]. As can be easily checked, for we recover the corresponding results for the CDM, as it should. The Hubble function can be immediately obtained from these formulas after inserting them in Friedmann’s equation, together with the conservation laws for radiation and baryons, and .

4 The XCDM and CPL parametrizations

In Section 6, when we compare the DVMs to the CDM, it is also convenient to fit the data to the simple XCDM parametrization of the dynamical DE [38]. Since both matter and DE are self-conserved (i.e., they are not interacting) in the XCDM, the DE energy density as a function of the scale factor is simply given by , with , where is the (constant) equation of state (EoS) parameter of the generic DE entity in this parametrization. The normalized Hubble function is:


For it boils down to that of the CDM with rigid CC term. Use of the XCDM parametrization becomes useful so as to roughly mimic a (noninteractive) DE scalar field with constant EoS. For the XCDM mimics quintessence, whereas for it mimics phantom DE.

A slightly more sophisticated parametrization to the behavior of a noninteractive scalar field playing the role of dynamical DE is furnished by the CPL parametrization [39], in which one assumes that the generic DE entity has a slowly varying EoS of the form


The CPL parametrization, in contrast to the XCDM one, gives room for a time evolution of the dark energy EoS owing to the presence of the additional parameter , which satisfies , with or . The corresponding normalized Hubble function for the CPL can be easily computed:


Both the XCDM and the CPL parametrizations can be thought of as a kind of baseline frameworks to be referred to in the study of dynamical DE. They can be used as fiducial models to which we can compare other, more sophisticated, models for the dynamical DE, such as the DVMs under study. The XCDM, however, is more appropriate for a fairer comparison with the DVMs, since they have one single vacuum parameter . For this reason we present the main fitting results with the XCDM, along with the other models, in Table 1. The numerical fitting results for the CPL parametrization are given in [22]. Owing to the presence of an extra parameter the errors in the fitting values of and are bigger than the error in the single parameter of the XCDM parametrization. For this presentation, we limit ourselves to report on the latter, together with the rest of the models.

5 Structure formation under vacuum dynamics

The DVMs and DVMs are characterized by a dynamical vacuum/quasi-vacuum energy density. Therefore, in order to correctly fit these models to the data, a generalized treatment of the linear structure formation beyond the CDM is of course mandatory. At the (subhorizon) scales under consideration we will neglect the perturbations of the vacuum energy density in front of the perturbations of the matter field. This has been verified for various related cases, see e.g. [40] and [14] . For a recent detailed study directly involving the DVMs under consideration, see [41]. In the presence of dynamical vacuum energy the matter density contrast obeys the following differential equation (cf.  [22, 23] for details):


where the prime denotes differentiation with respect to the scale factor. The functions and can be determined after a straightforward application of the general perturbation equations in the presence of dynamical vacuum (cf. [40]), with the result:


Here and . For we have , and after some calculations one can easily show that (14) can be brought back to the common form for the XCDM and CDM. The (vacuum-matter) interaction source for each DVM is given by (6)-(8). For const. and for the XCDM there is no such an interaction, therefore , and Eq. (14) reduces to the CDM form:


Recalling that in the CDM, the growing mode solution of this equation can be solved by quadrature:


One can easily check that in the matter-dominated epoch (, ), the above equation yields , as expected. However, being there is an effective suppression of the form with [42]. The last feature is also true in the presence of dynamical vacuum. However, the generalized perturbations equation (14) cannot be solved analytically and one has to proceed numerically. The first thing to do is to fix the initial conditions analytically. This is possible because at high redshift, namely when nonrelativistic matter dominates over radiation and DE, functions (15) and (16) are then approximately constant and Eq. (14) admits power-law solutions . The values for the power can be computed for each model. For example, for the RVM it can be shown that . Notice that for and near . Using the appropriate initial conditions for each model, the numerical solution of (14) can be obtained – see [22, 23] for more details.

Armed with these equations, the linear LSS regime is usually analyzed with the help of the weighted linear growth , where is the growth rate and is the rms mass fluctuation on Mpc scales. It is computed as follows (see e.g. [22]):


where is a top-hat smoothing function and the transfer function [22]. The fitting parameters for each model are contained in . Following the above mentioned references, we define as fiducial model the CDM at fixed parameter values from the Planck 2015 TT,TE,EE+lowP+lensing data [9]. These fiducial values are collected in . The theoretical calculation of and of the product for each model is essential to compare with the LSS formation data. The calculation is possible after obtaining the fitting results for the parameters, as indicated in Tables 1 and 2 and Fig. 1. The result for is plotted in Fig. 2, together with the observational points. In Sect.7 we will further discuss these results. In the next section we discuss some basic facts of the fit analysis.

CDM - - 84.40/85 - -
XCDM - 76.80/84 5.35 3.11
RVM - 68.67/84 13.48 11.24
- 69.13/84 13.02 10.78
- 76.30/84 5.85 3.61
RVM 68.15/83 11.70 7.27
68.22/83 11.63 7.20
68.24/83 11.61 7.18
Table 1: Best-fit values for the free parameters of the CDM, XCDM, the three dynamical vacuum models (DVMs) and the three dynamical quasi-vacuum models (DVMs), including their statistical significance (i.e. the values of the -test and the difference of the values of the Akaike and Bayesian information criteria, AIC and BIC, with respect to the CDM). For a detailed description of the data and a full list of observational references, see [20, 22]. The quoted number of degrees of freedom () is equal to the number of data points minus the number of independent fitting parameters ( for the CDM, 5 for the XCDM and the DVMs, and 6 for the DVMs). For the CMB data we have used the marginalized mean values and covariance matrix for the parameters of the compressed likelihood for Planck 2015 TT,TE,EE + lowP+ lensing as in [23]. Each best-fit value and the associated uncertainties have been obtained by marginalizing over the remaining parameters.

6 Fitting the DVMs to observations

In this section, we put the dynamical vacuum models (DVMs) discussed above to the test, see  [19, 20, 21, 22, 23] for more details. It proves useful to study them altogether in a comparative way, and of course we compare them to the CDM.

We confront all these models to the main set of cosmological observations compiled to date, namely we fit the models to the following wealth of data (cf. Ref. [20, 21, 22] for a complete list of references): i) the data from distant type Ia supernovae (SNIa); ii) the data on baryonic acoustic oscillations (BAO’s); iii) the known values of the Hubble parameter at different redshift points, ; iv) the large scale structure (LSS) formation data encoded in the weighted linear growth rate ; v) the CMB distance priors from Planck 2015. Thus, we use the essential observational data represented by the cosmological observables SNIa+BAO++LSS+CMB. For the analysis we have defined a joint likelihood function from the product of the likelihoods for all the data sets discussed above. For Gaussian errors, the total to be minimized reads:


Each one of these terms is defined in the standard way, including the covariance matrices for each sector 444See the details in the appendix of [22].. The fitting results for models (6)-(8) are displayed in terms of contour plots in Fig. 1.

Figure 1: Likelihood contours in the -plane for the three DVMs I, II and III (we are restricting here to the vacuum case in all cases) defined in (6)-(8). Shown are the regions corresponding to , , , (corresponding to 1, 2, 3, 4 and 5 c.l.) after marginalizing over the rest of the fitting parameters indicated in Table 1. The elliptical shapes have been obtained applying the standard Fisher approach. We estimate that for the RVM, (resp. ) of the 4 (resp. 5) area is in the region. The CDM () appears disfavored at c.l. in the RVM and , and at c.l. for . For more details, see [22].

For the numerical fitting details, cf. Table 1. In such table we assess also the comparison of the various models in terms of the time-honored Akaike and Bayesian information criteria, AIC and BIC [43, 44]. These information criteria are extremely useful for comparing different models in competition. The reason is obvious: the models having more parameters have a larger capability to adjust the observations, and for this reason they should be penalized accordingly. It means that the minimum value of should be appropriately corrected so as to take into account this feature. This is achieved through the AIC and BIC estimators, which can be thought of as a modern quantitative formulation of Occam’s razor. They are defined as follows [43, 44, 45, 46]:




Here is the number of independent fitting parameters and the number of data points. The larger are the differences AIC (BIC) with respect to the model that carries smaller value of AIC (BIC) – the DVMs here – the higher is the evidence against the model with larger value of AIC (BIC) – the CDM. For AIC and/or BIC in the range we can speak of “strong evidence” against the CDM, and hence in favor of the DVMs. Above 10, we are entitled to claim “very strong evidence” [43, 44, 45, 46] in favor of the DVMs.

From Table 1 we can read off the results: for Models I and II we find AIC and BIC simultaneously. The results from both are consistent with the fact that these models yield a nonvanishing value for with the largest significance (). It means that the DVMs I and II fit better the overall data than the CDM at such confidence level. Model III (i.e. ) also fits better the observations than the CDM, but with a lesser c.l. Indeed, in this case AIC and BIC, and the parameter is nonvanishing at near . Thus, the three DVMs are definitely more favored than the CDM, and the most conspicuous one is the RVM, Eq.  (3).

We conclude that the wealth of cosmological data at our disposal currently suggests that the hypothesis const. despite being the simplest may well not be the most favored one. The absence of vacuum dynamics is excluded at nearly c.l. as compared to the best DVM considered here (the RVM). The strength of this statement is riveted with the firm verdict of Akaike and Bayesian criteria. Overall we have collected a fairly strong statistical support of the conclusion that the SNIa+BAO++LSS+CMB cosmological data do favor a mild dynamical vacuum evolution.

CDM - - 90.59/86 - -
XCDM - 87.38/85 0.97 -1.29
RVM - 78.96/85 9.39 7.13
- 79.17/85 9.18 6.92
- 82.48/85 5.87 3.61
RVM 78.93/84 7.11 2.66
79.17/84 6.88 2.42
78.98/84 7.07 2.61
Table 2: Best-fit values for the free parameters of the CDM, XCDM, the three dynamical vacuum models (DVMs) and the three dynamical quasi-vacuum models (DVMs), including their statistical significance (the values of the -test and the difference of the Akaike and Bayesian information criteria AIC and BIC with respect to the CDM), i.e. the same as in Table 1 but now adding the local measurement, as indicated in Eq. (23).

7 Dynamical vacuum and the tension. A case study.

The framework outlined in the previous sections suggest that owing to a possible small interaction with matter, the vacuum energy density might be evolving with the cosmic expansion. This opens new vistas for a possible understanding of the well known discrepancy between the CMB measurements of [9, 11], suggesting a value below km/s/Mpc, and the local determinations emphasizing a higher range clearly above km/s/Mpc [47].

7.1 A little of history

Such tension is reminiscent of the prediction by the famous astronomer A. Sandage in the sixties, who asserted [48] that the main task of future observational cosmology would be the search for two parameters: the Hubble constant and the deceleration parameter . The first of these parameters defines the most important distance (and time) scale in cosmology prior to any other cosmological quantity. Sandage’s last published value with Tammann (in 2010) is km/s/Mpc [49] – a value that was slightly revised in Ref. [50] as km/s/Mpc after due account of the high-weight TRGB (tip of the red-giant branch) calibration of SNIa.

Figure 2: The large scale structure (LSS) formation data () and the theoretical predictions for models I, II and III in the case (i.e. the DVMs). The computed values of for each model are also indicated. The curves for the cases Ia, IIIa and IIIb correspond to special scenarios for Models I and III, in which only the BAO and CMB data are used (not the LSS). Despite the agreement of the CMB measurement with the Riess et al. local value can be better for these special scenarios, the price to enforce such “agreement” is that the concordance with the LSS data is now spoiled (the curves for Ia and IIIa are higher). Case IIIb is our theoretical calculation of the impact on the LSS data for the scenario proposed in [63], aimed at optimally relaxing the tension with . Unfortunately it is in severe disagreement with the LSS data. The last three scenarios lead to phantom-like DE and are all disfavored (at different degrees) by the LSS data [23].

As for the deceleration parameter, , its measurement is equivalent to determining in the context of the concordance model. As indicated in the introduction, on fundamental grounds understanding the value of may not just be a matter of observation; in actual fact it embodies one of the most important and unsolved conundrums of theoretical physics and cosmology of all times: the cosmological constant problem [6]555There is a famous saying by Allan Sandage: ‘…it is not a matter of debate, it is a matter of observation’ [50], which we may as well apply here. The CC problem is a mater of debate, no doubt about it, but once more we should concur with him that it is above all a matter of observation; for observing if is a rigid parameter or a dynamical variable can also greatly help in the way we should finally tackle the CC problem! It may actually lead to the clue for its understanding. Is this not, after all, how real physics works? It is time for less formal theory and more observations!. It is our contention that a better understanding of is related to a deeper knowledge of the nature of , in particular whether the rigid option const. could be superseded by the more flexible notion of dynamical vacuum energy density. Obviously this has an implication on the value of , as shown in Table 1.

The actual value of has a long and tortuous history, and the tension among the different measurements is inherent to it. Let us only recall that after Baade’s revision (by a factor of one half [51]) of the exceedingly large value km/s/Mpc originally estimated by Hubble (implying a universe of barely two billion years old only), the Hubble parameter was further lowered to km/s/Mpc and finally was captured in the range km/s/Mpc, where it remained for 20 years (until 1995), mainly under the influence of Sandage’s devoted observations [52]. See nevertheless [53] for an alternative historical point of view, in which a higher range of values is advocated. Subsequently, with the first historical observations of the accelerated expansion of the universe, suggesting a positive value of [54, 55], the typical range for moved upwards to km/s/Mpc. In the meantime, a wealth of observational values of have piled up in the literature using different methods (see e.g. the median statistical analysis of measurements considered in [56, 57]).

Figure 3: Contour plots in the -plane for the RVM (blue) and RVM (orange) up to , together with those for the CDM (black) up to , corresponding to the situation when the local value of Riess et al. [47] is included as a data point in the fit (cf. Table 2)  [23].

7.2 The documented tension

As mentioned above, two kinds of precision (few percent level) measurements of have generated considerable perplexity in the recent literature, specifically between the latest Planck values () obtained from the CMB anisotropies, and the local HST measurement (based on distance estimates from Cepheids). The latter, obtained by Riess et al. [47], is


whereas the CMB value, depending on the kind of data used, reads[9]




In both cases there is a tension above c.l. (viz. and , respectively) with respect to the local measurement 666It is suggestive to see that the late local measurements of obtained by Sandage and Tammann [49], based on Cepheids and SNIa, are closer to the current CMB measurements than to the recent Riess et al. local measurements based on similar techniques. It makes one think if the current local measurement is actually an outlier.. We will refer the Planck measurement collectively as since the tension with the local measurement (23) is essentially the same. This situation, and in general a certain level of tension with some independent observations in intermediate cosmological scales, has stimulated a number of discussions and possible solutions in the literature, see e.g. [58, 59, 60, 61, 62, 63].

7.3 Refiting the overall data in the presence of

We wish to reexamine here the tension, but not as an isolated conflict between two particular sources of observations, but rather in light of the overall fit to the current cosmological SNIa+BAO++LSS+CMB data. In other words, it is worthwhile to reconsider the fitting results of Table 1 when we introduce as an explicit data point in the fit. The result is recorded in Table 2.

Figure 4: Contour lines for the CDM (black) and RVM (blue) up to in the -plane. We present in the left plot the case when the local value of Riess et al.[47] is included in the fit (cf. Table 2), whereas in the right plot the case when that local value is not included (cf. Table 1). See [23] for more details.

In Fig. 2 we plot for the various models I, II and III for the case with constant using the fitted values of Table 2 and some other special situations described in the caption. The case is not plotted in Fig. 2 because it is visually undistinguishable from the case near . The numerical differences in the fitting results, however, are not negligible as can be see on comparing Tables 1 and 2.

In Fig. 3 we display the contour plots in the -plane for the RVM (blue) and RVM (orange) up to , together with those for the CDM (black) up to , corresponding to the situation when the local value of Riess et al. [47] is included as a data point in the fit (cf. Table 2)  [23]. One can see that when all data sources SNIa+BAO++LSS+CMB are used, the price for reaching the vicinity of is a too small value of around and requires extended contours beyond c.l. The figure also shows that both the RVM and RVM intersect much better (already at ) the range than the CDM. The latter requires also contours to reach , and near . In other words, when the local value enters the fit, the CDM is in a rather uncomfortable position, as it is almost far-equidistant from both the and domains!

Finally, in Fig.  4 we show once more the difficulty of reaching the neighborhood, as it enforces to extend the contours beyond the c.l., what would imply a too low value of in both cases (cf. Fig. 3) and, in addition, would result in a too large value of for the RVM. Interestingly, and are positively correlated in the RVM (i.e. decreases when decreases), whilst they are anticorrelated in the CDM ( increases when decreases, and vice versa). It is this opposite correlation feature with respect to the CDM what allows the RVM to improve the LSS fit in the region where both and are smaller than the respective CDM values (cf. Fig. 4). This explains why the Planck range for is clearly preferred by the RVM, as it allows a much better description of the LSS data.

While we must still remain open to the possibility that the and/or measurements are affected by some kind of (unknown) systematic errors, some of these possibilities may be on the way of being ruled out by recent works. In [64] the authors study the systematic errors in Planck’s data by comparing them with the South Pole Telescope data. They conclude that there is no evidence of systematic errors in Planck’s results. Let us also mention the “blinded” determination km/s/Mpc from [65], based on a reanalysis of the SNIa and Cepheid variables data from the older work by Riess et al., where it was found km/s/Mpc [66]. The tension with diminishes, compare with Eq. (23), since the central value decreased and the uncertainty has grown significantly by more than .

On the other hand, in [67] it is shown that by combining the latest BAO results with WMAP, Atacama Cosmology Telescope (ACT), or South Pole Telescope (SPT) CMB data produces values of that are lower than the distance ladder, independent of Planck. These authors conclude from their analysis that it is not possible to explain the disagreement solely with a systematic error specific to the Planck data. In another vein the work [68] excludes systematic bias or uncertainty in the Cepheid calibration step of the distance ladder measurement by [47]. Finally, we mention the recent study [69], in which the authors run a new (dis)cordance test based on using a recently introduced index of inconsistency capable of dissecting inconsistencies between two or more data sets. After comparing the constraints on from different methods and observing the decreasing behavior of such index when the local -measurement is removed they conclude that such local measurement is an outlier compared to the others, what would favor a systematics-based explanation. This is compatible with the observed improvement in the statistical quality of our analysis when the local -measurement is removed from our overall fit.

The search for a final solution to the tension is, of course, still work in progress. The class of the RVMs studied here offers a viable solution to both the and existing tensions in the data, which are both unaccountable within the CDM. Thus, within our dynamical vacuum framework the CMB-based Planck value of is definitely favored and is compatible with a smaller value of , whereas the local measurement of is considered an outlier, namely a value which seems to be irreconcilable with a simultaneous solution of the other CDM tensions.

8 Conclusions

In this work, we have reviewed the status of the dynamical vacuum models (DVMs) in their ability to compete with the CDM model (namely the standard or concordance model of cosmology) to fit the overall SNIa+BAO++LSS+CMB cosmological observations. We find that the the current cosmological data disfavors the CDM, and hence the const. hypothesis, in a very significant way. The best fit value to the overall data is provided by the running vacuum model (RVM), at a confidence level of roughly as compared to the CDM. Even a simple XCDM parametrization yields roughly . These results are consistent with our most recent studies [19, 20, 21, 22].

We have also used these models to reanalyze the tension between the Riess et al. local measurement and the value obtained in the CMB measurements from the Planck satellite, , which is smaller. We find that the fit quality to the overall SNIa+BAO++LSS+CMB cosmological data increases to the maximum level only when the local measurement is not taken into account. In other words, the CMB determination of is clearly preferred. We demonstrate that not only the CMB and BAO, but also the LSS data, are essential to grant these results.

We have also comparatively considered the performance of the DVMs (i.e. the dynamical quasi-vacuum models with ), and we have found that they are also able to improve the CDM fit, although to a lesser extent than the best DVMs. However, the extra degree of freedom associated to the free parameter in these models can be used to try to enforce a minimal tension. What we find is that if the LSS data are not considered in the fit analysis, the tension can indeed be diminished, but only at the expense of a phantom-like dynamical behavior of the DE, namely turns out to satisfy .

But the main problem is that this implies a serious disagreement with the structure formation data. Such disagreement disappears when the LSS data are restored, and in fact a good fit quality to the overall observations (better than the CDM at c.l.) can be achieved, with no trace of phantom dynamical DE energy. In the absence of the local measurement, the fit quality in favor of the main dynamical vacuum models further increases up to c.l. In general the vacuum dynamics tends to favor the CMB determination of against the local measurement , but this measurement can still be accommodated in the fit without seriously spoiling the capacity of the RVM to improve the CDM fit.

These results are bolstered by outstanding marks of the information criteria (yielding values AIC and BIC) in favor of the main DVMs and against the concordance model. To summarize, we claim that significant signs of dynamical vacuum energy density are sitting in the current cosmological data, which the concordance CDM model is unable to accommodate.

9 Acknowledgments

J. Solà is thankful to Prof. Harald Fritzsch for the kind invitation to this stimulating conference on Cosmology, Gravitational Waves and Particles. He would also like to thank Prof. K. K. Phua for inviting him to present this contribution in the review section of IJMPA. We have been supported by MINECO FPA2016-76005-C2-1-P, Consolider CSD2007-00042, 2014-SGR-104 (Generalitat de Catalunya) and MDM- 2014-0369 (ICCUB). J. Solà is also particularly grateful for the support received from the Institute for Advanced Study of the Nanyang Technological University in Singapore, where part of this work was performed.

Note Added:
Since the first version of this work appeared, new analyses of the cosmological data have been published, in particular the one-year results by the DES collaboration (DES Y1 for short) [70]. The Bayes factor indicates that the DES Y1 and Planck data sets are consistent with each other in the context of CDM and therefore both are insensitive to any effect on dynamical DE. In the case of DES Y1 they do not use direct data on LSS structure formation despite they recognize that smaller values of than those predicted by the CDM are necessary to solve the tension between the concordance model and the LSS observations.

Another recent work that does not find any sign of dynamical DE is [71]. As we have explained in  [22], we attribute this lack of sensitivity once more to the fact of not using large scale structure formation data and BAO. The latter is indeed not used in that paper e.g. for the analysis of DE in terms of the XCDM parametrization, and they do not use data on anywhere in their analysis. We contend that by restricting to CMB and lensing data is not sufficient to be sensitive to a possible evolution of the DE.

This is also the reason why Planck did not report any such evidence. In previous works of us– see in particular  [20, 22] – we have explored quantitatively in detail why is so. For instance, in [9] the Planck team did not use LSS (RSD) data at all, and in [10] they used a rather restricted set of BAO and LSS points. In our previous works  [20, 22] we have explicitly demonstrated that under the same limited conditions used by Planck (not different from those of DES Y1 in this respect) we do recover their negative results on dynamical DE.

However, when we use the full data string, which involves not only CMB but also the rich BAO+LSS data set that has been described in  [20, 22], then we obtain substantially positive indications of dynamical DE at a confidence level in between . While incontestable evidence requires of course c.l. at least, these results are already quite encouraging. In fact, they are actually consistent with the recent analysis by Gong-Bo Zhao et al. [72], who reported on a signal of dynamical DE at c.l using similar data ingredients as in our analysis. See also the complementary comments on these results provided in [73], where it is suggested that they seem to point to a “crack in the current cosmological paradigm”.


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