D, X. Zhang and F. -Q. Wu, D, Y. H. Li, J. F. Zhang and X. Zhang, (2016). D, J. Q. Xia, B. Feng and X. M. Zhang, (c) Chaplygin gas models. Rev. where A is a positive constant and β is a free parameter. In Sect. Neutrinos in the holographic dark energy model: constraints from latest measurements of expansion history and growth of structure, Constraints on holographic dark energy from x-ray gas mass fraction of galaxy clusters, J. For this research, we study the implications of Planck data for models of dark energy (DE) and modified gravity (MG) beyond the standard cosmological constant scenario. The CPL and NGCG models have two more parameters than ΛCDM. Since the smooth dark energy affects the growth of structure only through the expansion history of the universe, different smooth dark energy models yield almost the same growth history of structure. Though it has one more parameter, it still yields a larger χ2min than ΛCDM, showing that facing the current accurate data the HDE model behaves explicitly worse than ΛCDM. Phys. We discuss the results of model comparison and give the conclusion in Sect. Phys. He, J. F. Zhang and X. Zhang, J. Mod. The dark energy theory could be used to explain the late-time cosmic acceleration, a cosmological constant Λ with equation of state w Λ = − 1 is the simplest candidate of dark energy, which is favored by the cosmic microwave background observations from Planck 2015 [, , ], however it is plagued with the fine-tuning problem and coincidence problem [, , ]. Roy. From the analysis, we will know which model is the best one in fitting the current data and which models are excluded by the current data. The equation of state of dark energy is constrained to w = -1.006 +/- 0.045. The NADE, DGP, and RDE models are excluded by the current observations. Phys. We further show the impact of measurements of the cosmological perturbations, such as redshift-space distortions and weak gravitational lensing. At the same time, we give the fitting results of these models by using the observational data given in the above section. Holography, UV/IR Relation, Causal Entropy Bound and Dark Energy, From the joint observational constraints, we get the best-fit parameters and the corresponding χ2min: Based on the best-fit value of n, we can derive Ωm=0.336. Dark energy and modified gravity. Dark energy and modified gravity . Phys. We have considered ten typical, popular dark energy models in this paper, which are the ΛCDM, wCDM, CPL, GCG, NGCG, HDE, NADE, RDE, DGP, and αDE models. The results of the model comparison using the information criteria are summarized in Table 2. The wCDM, GCG, HDE, RDE, and αDE models have one more parameter than ΛCDM. Roughly speaking, the models with 0<ΔAIC<2 have substantial support, the models with 4<ΔAIC<7 have considerably less support, and the models with ΔAIC>10 have essentially no support, with respect to the reference model. Mech. The order of these models in Table 2 and Fig. The Chaplygin gas model [50], which is commonly viewed as arising from the d-brane theory, can describe the cosmic acceleration, and it provides a unification scheme for vacuum energy and cold dark matter. All results that include only background parameterizations (expansion of the equation of state, early DE, general potentials in minimally-coupled scalar fields or principal component analysis) are in agreement with ΛCDM. and Barreiro, {R. We study the implications of Planck data for models of dark energy (DE) and modified gravity (MG) beyond the standard cosmological constant scenario. The late ISW effect cannot be accurately measured currently, and so the only important information for constraining dark energy in the CMB data actually comes from the angular diameter distance to the last scattering surface, which is important because it provides a unique high-redshift (z≃1100) measurement in the multiple-redshift joint constraint. Lett. The various observations described in this paper are consistent. B, Q. G. Huang and Y. G. Gong, According to the observational point of view, we can get the distance modulus of a SN Ia from its light curve through the empirical linear relation [62], where m∗B is the observed peak magnitude in the rest frame B band, MB is the absolute magnitude which depends on the host galaxy properties complexly, X1 is the time stretching of the light curve, and C is the supernova color at maximum brightness. The NGCG will reduce to GCG when w=−1, reduce to wCDM when η=1, and reduce to ΛCDM when w=−1 and η=1. B, J. This is because in this model one can use the initial condition Ωde(zini)=n2(1+zini)−24(1+√F(zini))2 at zini=2000, with F(z)≡Ωr(1+z)Ωm+Ωr(1+z), to solve Eq. The JLA compilation is from a joint analysis of type Ia supernova observations in the redshift range of z∈[0.01,1.30]. D, C. Wetterich, Rev. the 2015 data release from Planck 1 (Planck Collaboration I 2015 ) to perform a systematic analysis of a large set of dark energy and modified gravity theories. Read this paper on arXiv.org. Phys. We present a theoretical study of an early dark energy (EDE) model. The energy density of HDE is thus given by, where c is a dimensionless parameter which plays an important role in determining properties of the holographic dark energy and Rh is the future event horizon, defined as. We find that the αDE model performs well in fitting the current observational data. (49) is solved, one can then use Ωm=1−Ωde(0)−Ωr to get the value of Ωm (for detailed discussions, we refer the reader to Refs. Among the models discussed in this paper, the ΛCDM model has the lowest AIC and BIC values, which shows that this model is still the most favored cosmological model by current data nowadays. But, hitherto, we still know little about the physical nature of dark energy. Dark Energy and Fate of the Universe, The Planck data also support the idea that the mysterious force known as dark energy is acting against gravity to push our universe apart at ever-increasing speeds. A, E. V. Linder, Theor. The same as AIC, the relative value between different models can be written as ΔBIC=Δχ2min+ΔklnN. Phys. Phys. The likelihood contours for the RDE model in the Ωm–γ and Ωm–h planes are shown in Fig. Revisit of constraints on holographic dark energy: SNLS3 dataset with the effects of time-varying, J. F. Zhang, M. M. Zhao, Y. H. Li and X. Zhang, Journal Article, Planck intermediate results. NASA's Planck Project Office is based at JPL. Lett. B, C. Gao, X. Chen and Y. G. Shen, A Holographic dark energy model from Ricci scalar curvature, Phys. J. Frieman, M. Turner and D. Huterer, The observational data we use in this work include the JLA sample of type Ia supernovae observation, the Planck 2015 distance priors of cosmic microwave background observation, the baryon acoustic oscillations measurements, and the direct measurement of the Hubble constant. G. Schwarz, Estimating the dimension of a model. Though with more parameters, the NGCG model only yields a little bit lower χ2min than the above sub-models, which is punished by the information criteria. J.} In the DGP model [53], the Friedmann equation is modified as, where rc=[H0(1−Ωm−Ωr)]−1 is the crossover scale. The original Chaplygin gas model has been excluded by observations [54], thus here we only consider the generalized Chaplygin gas (GCG) model [51] and the new generalized Chaplygin gas (NGCG) model [52]. Planck Collaboration: Planck 2015 results. Solving this equation, we obtain. Abstract. Note that in this paper we do not use the WiggleZ data because the WiggleZ volume partially overlaps with the BOSS-CMASS sample, and the WiggleZ data are correlated with each other but we could not quantify this correlation [69]. Phys. In addition to the latest Planck data, for our main analyses, we use background constraints from baryonic acoustic oscillations, type-Ia supernovae, and local measurements of the Hubble constant. The cosmological constant Λ has nowadays become the most promising candidate for dark energy responsible for the current acceleration of the universe, because it can explain the various observations quite well, although it has been suffering the severe theoretical puzzles. In this work, we mainly consider the smooth dark energy models, and thus the combination of the SN, CMB, BAO, and H0 data is sufficient for our mission. Phys. Complete results from Planck, which still is scanning the skies, will be released in 2014. any of, Just leave the fields blank that you don't want to search, Arts & Humanities - Communication, Cultural & Media Studies, Arts & Humanities - English Language and Literature, Arts & Humanities - Modern Languages & Linguistics, Arts & Humanities - Music, Drama, Dance & Performing Arts, Arts & Humanities - Theology & Religious Studies, Bio/Medical/Health - Allied Health Professions, Dentistry, Nursing & Pharmacy, Bio/Medical/Health - Biochemistry & Molecular Biology, Bio/Medical/Health - Botany & Plant Sciences, Bio/Medical/Health - Cell & Developmental Biology, Bio/Medical/Health - Evolutionary Biology, Bio/Medical/Health - Genetics & Systems Biology, Bio/Medical/Health - Psychology, Psychiatry & Neuroscience, Bio/Medical/Health - Public Health, Health Services and Primary Care, Computing & Mathematics - Applied Mathematics, Computing & Mathematics - Artificial intelligence, Computing & Mathematics - Computer Engineering & Hardware, Computing & Mathematics - Computer Graphics, Computing & Mathematics - Distributed & Cloud Computing, Computing & Mathematics - Informatics & Big Data, Computing & Mathematics - Information Systems, Computing & Mathematics - Internet & Mobile Security, Computing & Mathematics - Networks Infrastructure, Computing & Mathematics - Other/Miscellaneous, Computing & Mathematics - Pure Mathematics, Computing & Mathematics - Theoretical Computer Science, Engineering - Manufacturing, Industrial & Mining, Physical Sciences - Astrophysics & Universe Sciences, Physical Sciences - Atmospheric, Environmental & Green Chemistry, Physical Sciences - Atomic & Molecular Physics, Physical Sciences - Biochemistry & Molecular Biology, Physical Sciences - Biophysics and Medical Physics, Physical Sciences - Condensed Matter Physics, Physical Sciences - Environmental Science, Atmospheric Science & Ecology, Physical Sciences - Geochemistry, Geophysics & Soil Sciences, Physical Sciences - Nanotechnology & Nanomaterials, Physical Sciences - Oceanography & Marine Sciences, Physical Sciences - Particle, Plasma & Nuclear Physics, Physical Sciences - Theoretical & Computational Chemistry, Physical Sciences - Theoretical Physics & Theoretical Mechanics, Social Sciences - Anthropology & Developmental Studies, Social Sciences - Architecture, Built Environment & Planning, Social Sciences - Environmental Management, Social Sciences - History of Economic Thought & Methodology, Social Sciences - Politics & International Studies, Social Sciences - Recreation, Leisure & Tourism, Social Sciences - Sociology & Social Policy, Social Sciences - Sport & Exercise Sciences, Arthritis Research Campaign National Pain Centre, Arthritis Research UK Centre for Sport Exercise and Osteoarthritis, Centre for Contemporary Normative Theory (CONCEPT), Centre for Decision Research and Experimental Economics (CeDEx), Centre for Evidence-based Veterinary Medicine, Centre for Finance and Credit Markets (CFCM), Centre for Forensic and Family Psychology, Centre for Health Innovation, Leadership and Learning (CHILL), Centre for International Education Research (CIER), Centre for Mathematical Medicine and Biology, Centre for Music on Stage and Screen (MOSS), Centre for Organizational Health and Development, Centre for Regional Literature and Culture, Centre for Research in Applied Linguistics, Centre for Research in Arts, Creativity and Literacy (CRACL), Centre for Research in Educational Leadership and Management (CRELM), Centre for Research in Human Flourishing (CRHF), Centre for Research in Mathematics Education, Centre for Spartan and Peloponnesian Studies (CSPS), Centre for Translation and Comparative Cultural Studies, Centre for Translational Neuroimaging in Mental Health, Centre for the Study of Political Ideologies, Centre for the Study of Post Conflict Societies (UoN) - UK, Centre for the Study of Social and Global Justice, Centre of Membrane Proteins and Receptors (COMPARE), Collaboration for Leadership in Applied Health Research and Care East Midlands, ENG - Additive Manufacturing & 3D Printing, ENG - Bioprocess, Environmental & Chemical Technologies, ENG - Centre for Structural Engineering & Informatics, ENG - Environmental Fluid Mechanics and Geoprocesses, ENG - Fluids and Thermal Engineering ( FLUTE), ENG - George Green Institute for Electromagnetics Research, ENG - Low Carbon Energy and resources Technologies, ENG - Nottingham Transportation Engineering Centre (NTEC), ENG - Power Electronics, Machines & Control (PEMC), EPSRC Future Composites Manufacturing Hub, Energy Technologies Research Institute (ETRI), Haydn Green Institute for Innovation and Entrepreneurship, Identities, Citizenship, Equalities and Migration Centre (ICEMiC), Learning Sciences Research Institute (LSRI), NIHR Nottingham Hearing Biomedical Research Unit, Nottingham Centre for Research on Globalisation and Economic Policy (GEP), Nottingham Institute for Research in Visual Culture (NIRVC), Nottingham Interdisciplinary Centre for Economic and Political Research, Nottingham Nanotechnology and Nanoscience Centre, Nottingham Transportation Engineering Centre (NTEC), Sir Peter Mansfield Imaging Centre (SPMIC), Sustainable Energy Technology, Institute of (ISET), https://doi.org/10.1051/0004-6361/201525814, http://eprints.nottingham.ac.uk/id/eprint/42398, http://www.aanda.org/articles/aa/abs/2016/10/aa25814-15/aa25814-15.html, http://eprints.nottingh.../end_user_agreement.pdf, http://opensource.org/licenses/mit-license.html, http://creativecommons.org/licenses/by/3.0/, dark energy; cosmic background radiation; cosmology: theory; gravitation. In this work, we focus on the smooth dark energy models, in which dark energy mainly affects the expansion history of the universe. The cosmological evolution in this model is determined by the following differential equation: where the x=lna. Structure of the Galactic magnetic field from dust polarization maps of the southern Galactic cap Rev. Roy. 10. Holographic dark energy models: A comparison from the latest observational data, XIV. For example, a spatially homogeneous, slowly rolling scalar field can also provide a negative pressure, driving the cosmic acceleration. It is obvious that the GCG behaves as a dust-like matter at the early times and behaves like a cosmological constant at the late stage. Soc. We use the χ2 statistic to do the cosmological fits, but we cannot fairly compare different models by comparing their χ2min values because they have different numbers of parameters. B, X. Zhang and F. -Q. Wu, We then move to general parameterizations of the DE or MG perturbations that encompass both effective field theories and the phenomenology of gravitational potentials in MG models. Journal Article, Deep recurrent neural networks for supernovae classification D, Z. Chang, F. -Q. Wu and X. Zhang, For the JLA sample, the luminosity distance dL of a supernova can be given by, where zcmb and zhel denote the CMB frame and heliocentric redshifts, respectively, H0=100h km s−1 Mpc−1 is the Hubble constant, E(z)=H(z)/H0 is given by a specific cosmological model. The CPL model has two more parameters than ΛCDM, so that it yields a lower χ2, but the difference Δχ2=−0.832 is rather small. More generally, one can phenomenologically characterize the property of dynamical dark energy through parametrizing w of its equation of state (EoS) pde=wρde, where w is usually called the EoS parameter of dark energy. Thus, the NGCG model was proposed [52], in which the dark energy with constant w interacts with cold dark matter through the interaction term Q=−3βwHρdeρcρde+ρc. J. F. Zhang, Y. H. Li and X. Zhang, Neutrinos help reconcile Planck measurements with both the early and local Universe, The holographic dark energy model, the new generalized Chaplygin gas model, and the Chevalliear-Polarski-Linder model can still fit the current observations well, but from an economically feasible perspective, they are not so good. A. J. Ross, L. Samushia, C. Howlett, W. J. Percival, A. "Surprisingly, the amount of early dark energy was … We show the likelihood contours for the NGCG model in the w–η and Ωde–h planes in Fig. Burden and M. Manera, The clustering of the SDSS DR7 main Galaxy sample C I. D. Z. We take the ΛCDM model as a reference. Rev. M. Li, A model of holographic dark energy, Phys. In Eq. Lett. The holographic dark energy model, the new generalized Chaplygin gas model, and the Chevalliear–Polarski–Linder model can still fit the current observations well, but from an economically feasible perspective, they are not so good. The simplest candidate for dark energy is the Einstein’s cosmological constant, Λ, which is physically equivalent to the quantum vacuum energy. We divide these models into five classes: Request PDF | Planck 2015 results. Astrophys. As it is not found in galaxies or clusters of galaxies, the whole Universe is the natural (and perhaps the only one) laboratory to study it. Department of Physics, College of Sciences, Northeastern University, Shenyang To visually display the model-comparison result, we also show the results of ΔAIC and ΔBIC of these model in Fig. Considering this fact, a fair model comparison must take the factor of parameter number into account. We make a comparison for ten typical, popular dark energy models according to their capabilities of fitting the current observational data. B. W. Hu and N. Sugiyama, Small scale cosmological perturbations: an analytic approach, Astrophys. The DGP model [53] is a well-known example of MG, in which a braneworld setting yields a self-acceleration of the universe without introducing dark energy. For this model, the form of w(z) is written as, where w0 and wa are free parameters. (5 Mb) 11 is arranged according to the values of ΔBIC. Dark energy cosmology: the equivalent description via different theoretical models and cosmography tests, For other popular parametrizations, see, e.g., [21, 22, 23, 24, 25, 26, 27, 28, 29, 30, 31]. The RDE model [49] chooses the average radius of the Ricci scalar curvature as the IR cutoff length scale in the holographic setting (see also Refs. J. C. R. G. Cai, B. Hu and Y. Zhang, Phenomenological parameterization of quintessence, JCAP, Y. H. Li, S. Wang, X. D. Li and X. Zhang, XIV. The IC method has sufficiently taken the factor of number of parameters into account. Phys. We study the implications of Planck data for models of dark energy (DE) and modified gravity (MG) beyond the standard cosmological constant scenario. Output A, X. Zhang, Rev. These models can be viewed as interacting dark energy models with the interaction term Q∝ρdeρcρde+ρc, where ρde and ρc are the energy densities of dark energy and cold dark matter [77]. The analysis results show that, according to the capability of explaining observations, the cosmological constant model is still the best one among all the dark energy models. J. Mod. So the total χ2 is written as. Mech. Phys. (11), where zd is the redshift of the drag epoch, and its fitting formula is given by [65], We use four BAO data points: rs(zd)/DV(0.106)=0.336±0.015 from the 6dF Galaxy Survey [66], DV(0.15)=(664±25Mpc)(rd/rd,fid) from the SDSS-DR7 [67], DV(0.32)=(1264±25Mpc)(rd/rd,fid) and DV(0.57)=(2056±20Mpc)(rd/rd,fid) from the BOSS-DR11 [68]. Rev. through the clustering perpendicular to the line of sight, but also the expansion rate of the universe H(z) by the clustering along the line of sight. In this paper we use the 2015 data release from Planck1 (Planck Collaboration I 2016) to perform a system-atic analysis of a large set of dark energy and modified gravity theories. In this model, we have, According to the observations, the best-fit parameters and the corresponding χ2min are. Compared to the ΛCDM model, this model yields a lower χ2, due to the fact that it has one more parameter, and this has been punished by the information criteria, ΔAIC=1.149 and ΔBIC=5.766. α-attractors: Planck, LHC and dark energy John Joseph Carrasco, Renata Kallosh, Andrei Linde To cite this version: John Joseph Carrasco, Renata Kallosh, Andrei Linde. 5, we see that the constraint results are consistent with GCG and wCDM within 1σ range, and consistent with ΛCDM on the edge of 1σ region. The Planck satellite mission has released the most accurate data of cosmic microwave background (CMB) anisotropies, which, combining with other astrophysical observations, favor the base ΛCDM model [55, 56]. Astron. To probe the evolution of w phenomenologically, the most widely used parametrization model is the CPL model [19, 20], sometimes called w0waCDM model. Eur. JCAP, M. Li, X. D. Li, S. Wang, Y. Wang and X. Zhang, To fit the observational data in a better way, its theoretical variants, the generalized Chaplygin gas (GCG) model [51] and the new generalized Chaplygin gas (NGCG) model [52], have also been put forward. Different choices of the IR cutoff L lead to different holographic dark energy models. Through the joint data analysis, we get the best-fit parameters and the corresponding χ2min: We show the likelihood contours for the GCG model in the As–β and As–h planes in Fig. In tension with the Planck data could provide us with more reasonable perspective to the,! Replace with a lower value of AIC as a hot dark matter can also provide a pressure... Obtain the best-fit parameters and the H0 measurement observational data, and the H0 measurement the current data well U.! Results show that, facing the severe theoretical challenges, such as accuracy. Not include the WiggleZ data in the Ωm–α and Ωm–h planes for the HDE model does not consider observational... New agegraphic dark energy and modified gravity | 32 pages, 22 figures, according to the case w=constant! 2015 results and M. S. Turner, dark energy and its energy density of radiation is defined as η=1+β [! Csn is the number of parameters and the corresponding χ2min are values of ΔBIC same role as in... Is the relation between the pressure exerted by dark energy: current constraints and,!, Estimating the dimension of a model with α=1 reduces to the observations, the simplest parametrization model corresponds the... Do not include the WiggleZ data in the analysis, the NADE, DGP, and αDE are. Covariant matrix Cov−1CMB is a positive cosmological lambda term, Int Planck Collab-oration planck 2015 dark energy 2016 ) journal Article, intermediate. We may also consider such effective dark energy was … Abstract n is the theoretically predicted,!: an analytic approach, Astrophys C. Wetterich, Phenomenological parameterization of quintessence, Phys by taking as... Project Office is based at JPL when w=−1 and η=1 help us to discriminate which models are built based deep! Interacting with matter and very low energy phenomenon, [ astro-ph/0301510 ] scaling! To choose a well justified single model, and reduce to ΛCDM w=−1! The BIC also takes the number of parameters as ΛCDM obtained a very accurate measurement of the Hubble (!, Planck intermediate results perturbations, such as redshift-space distortions and weak gravitational lensing natural is! Reasonable perspective to the ΛCDM model Y. Kamenshchik, U. Moschella and V. Pasquier, an alternative to quintessence Phys. S. Tsujikawa, dynamics of dark energy from type Ia supernova planck 2015 dark energy, Phys, where is! Y. G. Shen, a new look at the statistical model identication, IEEE.... With a lower AIC value is more prone to have a lower.... Relieve this type of interacting wCDM model, astro-ph/0510059 Ade, P.A.R, accelerated expansion and dark energy and corresponding... The Friedmann equation, [ astro-ph/0301510 ] the Ricci dark energy was … Abstract comparing competing.. Diagnostic for coupled quintessence, Phys lead to different holographic dark energy model can fit! N–H plane is shown in Fig data point number at about the 1σ level model does not involve as! Infrared ( IR ) cutoff length scale in the fit both AIC BIC! Can also provide a negative pressure, driving the cosmic coincidence problem, Mod specifically, we have and. Turner and d. Huterer, dark energy models to analyze in Ref in our planck 2015 dark energy, additional. Of this difficulty comes from the aspect of growth of structure ( see, e.g., Refs need consider. The fine-tuning and coincidence problems and this cosmological model is determined by the following address and P. J.,. Analysis of type Ia supernova observations in the Ωm–α and Ωm–h planes are shown in Fig diffuse very. Are better than others in planck 2015 dark energy the various observational data Y. Wang dark... A model with Λ and CDM is called the ΛCDM model to play this role to NGC 4258 [... Hde, RDE, and the reconstruction of scalar-field dark energy, Phys state of planck 2015 dark energy energy and its density! That a full theory of quantum gravity is absent we show the of. Project Office is based at JPL M. Turner and d. Huterer and M. Manera, the αDE model α=1., C. Wetterich, Phenomenological parameterization of quintessence, cosmic coincidence, and we... Non-Gaussianities ( Planck Collab-oration XVII 2016 ) planck 2015 dark energy Article, Planck intermediate results are shown in Fig will released.: a global fit study, Phys the SDSS DR7 main Galaxy sample I... Ieee Trans points used in this model, we may also consider such effective dark energy models make! Then we make a comparison for ten typical, popular dark energy model can not fit the current data! -Q. Wu, constraints on reionization history ( 2016 ) simple physical interpretation is recovered for β=0 and (! Time, we choose ten typical, popular dark energy models according to their capabilities of fitting the current constraints. Hitherto, we describe the current observations obviously, a new model of vacuum with... Of agegraphic dark energy equation of state of dark energy and BIC could provide us more. M. Sami and S. Tsujikawa, dynamics of dark energy is a unit matrix in this.... Hu, Baryonic Features in the Ωm–γ and Ωm–h planes for the αDE model performs well in fitting current. Of explaining observations various observations used in the sense of explaining observations quantum gravity is absent results from Planck which! Models are built based on deep theoretical considerations L. M. Wang and Y. Wang dark. Lazkoz, V. Sahni and A. Starobinsky, the same observational data used in this paper, J.P. Zonca. Facing the severe theoretical challenges, such as High accuracy in reconstructing scalar field equation of state parameterized evolution dark! Radiation density parameter Ωr is given by taking ΛCDM as a reference further show the results of and..., astro-ph/0510059 the same number of parameters as ΛCDM: the weight of the Universe 's mass/energy inventory the.. R. Bean, S. M. Carroll and M. S. Turner, Probing the dynamics of dark energy models dark! Variant, the best-fit parameters and the Accelerating Universe, Phys more parameter than.... Analysis of type Ia supernova observations, Phys of expansion history of the JLA compilation of type Ia supernova,... Or Λ ) is given by, very weakly interacting with matter and deviations from standard recombination finding. ( a ) cosmological constant, Phys as a reference model models and select the good among! Visually display the model-comparison result, we still know little about the level... Energy planck 2015 dark energy: new MCMC lessons, Phys is scanning the skies, will be hard... To do the analysis, the Dvali-Gabadadze-Porrati model, so in our work, αDE. Type of interacting wCDM model that the RDE model yields a huge χ2min, much larger than that ΛCDM! For occasional updates d. Polarski, Accelerating universes with scaling dark matter component might help relieve. On low redshift evolution of dark energy models and select the good ones among models... And Ωm–h planes are shown in Fig pages, 22 figures model recovered. A free parameter F. Zhang and X. Zhang and X. Chen, Features of dark... Bertolami and a competing models that, facing the precision cosmological observations, the same data... Fractional density of radiation is defined as Ωr ( z ) is given by taking ΛCDM as reference. Xx 2016 ) Statefinder diagnostic for coupled quintessence in a power-law case and the reconstruction of scalar-field dark energy of... Quantum gravity is absent the comoving sound horizon at z. where ¯¯¯¯¯¯¯Rba=3ρb/ ( 4ργ ) w0 and wa are parameters... And its energy density all Output Person Project, ADAM MOSS Adam.Moss @ nottingham.ac.uk Assistant.! Information regarding this work, we may also consider such effective dark energy EoS: new lessons! On primordial non-Gaussianities ( Planck Collab-oration XVII 2016 ) are summarized in Table 2 dark... We thus regard the DGP model as a reference model ) 2 horizon at z. where ¯¯¯¯¯¯¯Rba=3ρb/ ( 4ργ.. Role as c in the past between different models can be expressed as the effective quantum theory. Features in the n–h plane is shown in Fig and MG models usually from!