Observational constraints on dark matter-dark energy scattering cross section

In this letter, we report precise and robust observational constraints on dark matter-dark energy scattering cross section, using the latest data from cosmic microwave background (CMB) Planck temperature and polarization, baryon acoustic oscillations (BAO) measurements and weak gravitational lensing data from Canada-France-Hawaii Telescope Lensing Survey (CFHTLenS). The scattering scenario consists of a pure momentum exchange between the dark components, and we find $\sigma_d<10^{-29} \, {\rm cm^2}$ at 95\% CL from the joint analysis (CMB + BAO + CFHTLenS), for typical dark matter particle mass of the order 1-10 ${\rm GeV}/c^2$. We notice that the scattering among the dark components may influence the growth of large scale structure in the Universe, leaving the background cosmology unaltered.


I. INTRODUCTION
Cosmological observations reveal that approximately 95% of the energy content of our Universe is unknown, and this matter/energy content is usually termed the dark sector of the Universe. Constraints from Planck team [1] show that 25% of this content is in the form of a non-relativistic matter called dark matter (DM). The other part of this dark sector is in the form of an exotic component, dubbed dark energy (DE), with negative pressure responsible for accelerated expansion of the Universe at late times [2,3]. The particle physics experiments are yet to discover suitable particle candidates for the two dark components, and it is one of the greatest challenges in the contemporary physics. The popular candidate of DE is a positive cosmological constant [4][5][6] that suffers from theoretical inconsistencies, and consequently several alternative models have been proposed in the literature to explain the late time accelerated expansion of the Universe [7].
Models with energy exchange modify the cosmology at background level (expansion history) and perturbative level (growth of structures). A scenario with a pure momentum exchange between the dark components is presented in [35], where the energy exchange between the dark components is negligible. Thus, the expansion history is the same as for a non-interacting scenario. This class of interaction considers an elastic scattering of the DM particles with DE. For, the DE presents a low density (∼ 10 −47 GeV 4 ), and DM particles exhibit nonrelativistic velocities dispersion, that is, DM is cold, or at least a considerable part of the DM is cold. Therefore, an elastic scattering appears as a natural modeling of the dark sector physics. On the other hand, elastic scattering is the most abundant process at the energy scales of interest. The model is independent of the microphysics involved in the scattering process, or the DE nature. Consequences of the elastic scattering interaction between the dark components on the growth of large scale structure are presented in [35] while its effects on linear and nonlinear structure formation via N-body simulations are investigated in [36,37]. In the next section, we present more details about this interaction model. The aim of this paper is to constrain the DM-DE scattering cross section (as well as the equation of state parameter of DE in this context) with precision and robustness using the latest observational data from CMB Planck temperature and polarization, BAO measurements and CFHTLenS data. In next section, we introduce the model with the elastic scattering between DM and DE. We present the results and the related discussion of our analysis in Section III. In the final section, we summarize the findings of our study with future perspectives. The interaction between particles can be quantified by the cross section (the likelihood within an area transverse to their relative motions) within which the particles must meet in order to scatter from each other, implying a transfer of momentum and/or energy, or lead to the creation of new particles. At low energies the cross section can be well described by a process of elastic scattering. For instance, the photon-baryons fluid (essentially photon-electrons) in the early Universe is given in terms of the Thomson cross section, σ T 10 −25 cm 2 . In general, the drag force can be written as where v is the velocity of the particle traversing the fluid, and γ is the Lorentz factor. For instance, the photonelectron coupling (w = 1/3) is given by Considering the drag force 1 as the only nongravitational force between DE and DM, the linear perturbation theory equations (in conformal newtonian gauge) for DE-DM interaction fluids are given by [35,38] and where n dm is the proper number density of DM particles, σ d is the scattering cross section between DE and DM. The velocity perturbation above exhibits a new drag term It represents the DE fraction which is subject to scattering per unit time. In this scenario, the equation of continuity, δ i=dm,de = δρ i=dm,de /ρ i=dm,de , remains unchanged and follows the standard evolution. As already commented above, this scenario assumes that the dark components are not coupled at background level. Here, the interaction in the dark sector is quantified by the drag term S, and only acts via the velocity perturbation equations.
Once that ρ dm = m dm n dm for DM particles, where m dm stands for the mass of a typical DM particle. Then, eq. (4) can be rewritten as where we have defined with dimensions/units of barn · c 2 /GeV, as the characteristic parameter of the drag term.

III. RESULTS
In order to constrain the cross section of elastic scattering between DE and DM, we consider the following data sets (briefly described) sensitive at the perturbations level.
CMB: We use the full Planck 2015 data [1] comprised of temperature (TT), polarization (EE) and the cross correlation of temperature and polarization (TE) together with the CMB lensing power spectrum.

BAO:
We use the BAO measurements from the Six Degree Field Galaxy Survey (6dF) [39], the Main Galaxy Sample of Data Release 7 of Sloan Digital Sky Survey (SDSS-MGS) [40], the LOWZ and CMASS galaxy samples of the Baryon Oscillation Spectroscopic Survey (BOSS-LOWZ and BOSS-CMASS, respectively) [41], and the distribution of the LymanForest in BOSS (BOSS-Ly) [42]. These data points are summarized in Table I of [43].
CFHTLenS: We consider the full likelihood of the weak gravitational lensing data from blue galaxy sample compiled in [44].
The base parameters set for the DM-DE scattering model, to be constrained, is given by where the first six parameters are the base parameters for the standard ΛCDM model (see [1] for more details) while the remaining two parameters correspond to its extension in the present study.
For DE properties, we assume that its equation of state parameter is constant (w de = constant) and we have taken c 2 s = δp de /δρ de = 1 (c 2 s is in units of the speed of light). This necessarily implies that DE is a very light scalar field, as a typical canonical scalar field model with mass H 0 . Also, in order to avoid the unphysical sound speed, usually we take c 2 s = 1. We consider suitable uniform priors on the parameters of the model under consideration. In particular, we choose ξ ∈ [10 −9 , 10 −3 ]. We take 10 −3 as an upper bound, since values greater than that return surreal values to σ 8 . On the other hand, it is reasonable to expect that ξ << 1.
We modified the publicly available CLASS [45] and Monte Python [46] codes for the DM-DE scattering   Table I summarizes the main results of the statistical analysis carried out using three different combinations of data sets: CMB alone, CMB + BAO and CMB + BAO + CFHTLenS. The one-dimensional marginalized distribution of ξ is shown in Fig. 1 while one-dimensional marginalized distribution, two-dimensional 1σ and 2σ confidence contours for some selected parameters are displayed in Fig. 2.
In all the three cases, we note that ξ 10 −4 . From eq. One-dimensional marginalized distribution, twodimensional 1σ and 2σ confidence contours for some selected parameters. as or in terms of the Thomson cross section value, σ T 10 −25 cm 2 , as  Table I.
The typical DM particle mass (as weakly interacting massive particle (WIMP) candidate) can be taken in the range 1 -1000 GeV/c 2 . Recently, the best upper limits for WIMP masses are found as 10 GeV/c 2 , 40 GeV/c 2 , and 50 GeV/c 2 from the experiments XENON1T [48], PandaX-II [49], and LUX [50], respectively. In order to qualitatively discuss our results, taking m dm = 10 GeV/c 2 , we expect to have σ d 10 −3 σ T cm 2 at 95% CL. As expected, we can note that the interaction (nongravitational) between the dark components is too small, at least three orders of magnitude lower than the photonelectron interaction.
The constraints obtained by using CMB data alone show a small preference for a phantom dynamics, i.e., w de −1. Such a constraint on w de from CMB has also been observed in [51][52][53]. In the present study, we may infer that the DM particles undergo elastic scattering with scalar fields having negative kinetic term. It is well known that these fields suffer from instabilities at the classical and quantum levels [54,55] that casts doubts about their existence. Nevertheless, observationally such fields cannot be discarded, as we have also observed here.
From Table I and Fig. 2, it is clear that the combined data set CMB + BAO + CFHTLenS yields the most tight constraints on the model parameters. In order to observe/show the quantitative effects of ξ on the power spectrum P (k) of matter at z = 0, and CMB TT power spectrum in contrast with the base line Planck 2015 ΛCDM model [1], we select some particular values of ξ from its 95% confidence region given by the combined data set CMB + BAO + CFHTLenS.  Table I. We see that relative deviation of CMB TT power spectrum varies from the percent level to 8%. On  Table I. the other hand, significant relative deviation of matter power spectrum can be observed for the different values of ξ in Fig. 4. It is clear that the larger values of ξ tend to cause significant effects on the two power spectra.

IV. CONCLUSION AND PERSPECTIVES
In this study, we have considered an elastic scattering between DM and DE to constrain the cross section between the dark components. This elastic scattering for DM-DE is analogous to the Thomson scattering for baryons and photons. We find σ d 10 −29 cm 2 at 95% CL from our joint analysis (CMB + BAO + CFHTLenS), for typical DM mass of the order 1-10 GeV/c 2 . This quantifies a very small interaction among the dark components. We find that the combined data set CMB + BAO + CFHTLenS puts the most tight constraints on the model parameters when compared with the other two cases considered in this study, and some possible values of ξ can cause significant changes in the matter power spectrum P (k).
It may be noted that the DM-DE scattering model studied here reduces to the standard ΛCDM model with ξ = 0 and w de = −1. The constraints in Table I for the combined data set do not differ considerably from the ones obtained in [1] for the base line Planck 2015 ΛCDM model. Therefore, the presence of the non-zero parameter ξ does not yield significant changes in the background cosmological dynamics. However, as pointed out in [35], the elastic scattering among dark components may influence the growth of large scale structure in the Universe (see Figures 3 and 4). The precise and robust constraints obtained in the present study may be utilized for studying the linear and nonlinear structure formation in the DM-DE elastic scattering model via N-body simulations (see [36,37]). On the other hand, one can generalize the DM-DE elastic scattering scenario investigated here by considering an energy exchange between DM and DE, beyond the pure momentum exchange, that is, a modified model with cosmological effects at background level (expansion history) and perturbative level (growth of structures) using a general parametrization of DE coupled to DM. Also, it could be worthwhile to investigate an elastic scattering between DE and massive neutrinos (and/or dark radiation). Progress in this direction will be reported in a forthcoming paper.