Marco Baldi & Kazuya Koyama Brief summary of the conference “The Quest for Dark Energy: when theory meets simulations” @ Ringberg Castle, Germany
Cosmological models beyond the standard Λ CDM are attracting more and more attention lately (maybe also because of Euclid?) Several conferences and meetings devoted to non-standard cosmologies are taking place... Just to give an idea, my personal agenda of the last month has been: June 18-20, Paris: 17th Itzykson meeting “Heart of Darkness: Dark Energy and Modified Gravity” June 24-29, Ringberg: International conference “The quest for Dark Energy: when theory meets simulations” July 2-6, Sesto: International conference “Beyond Λ CDM: from dark matter halos to large-scale structures”
Cosmological models beyond the standard Λ CDM are attracting more and more attention lately (maybe also because of Euclid?) Several conferences and meetings devoted to non-standard cosmologies are taking place... Just to give an idea, my personal agenda of the last month has been: June 18-20, Paris: 17th Itzykson meeting “Heart of Darkness: Dark Energy and Modified Gravity” June 24-29, Ringberg: International conference “The quest for Dark Energy: when theory meets simulations” July 2-6, Sesto: International conference “Beyond Λ CDM: from dark matter halos to large-scale structures”
The conference website
The conference venue 45 participants, 8 talks sessions: 3 on theory, 3 on simulations, 2 on observations
Topics within the simulations sessions Overview on Dark Energy and Modified Gravity simulations M. Baldi Simulations of quintessence models: P . S. Corasaniti (The DEUS Full Universe Run) L. Casarini (shear spectra from simulations) Baryonic effects in simulations A. Maccio’ (supernova feedback) J. Schaye (AGN feedback) Simulations of interacting dark energy and modified gravity Y. Ayaita (simulations of growing neutrinos) B. Li (the modified gravity code ecosmog ) E. Puchwein (The modified gravity code mg-gadget ) F. Schmidt (a modified gravity code for Vainshtein screenings) H. Winther (voids in modified gravity) C. Llinares (cluster shapes in modified gravity) G. B. Zhao (environmental effects in modified gravity) E. Jennings (redshift-space distortions in modified gravity)
M. Baldi: overview on N-body & DE spatial time evolution interactions fluctuations ✘ ✘ ✘ Λ Dynamical DE ✔ ✘ ✘ (quintessence, a dynamical (scalar) no clustering at minimally-coupled to k-essence, EDE) degree of freedom sub-horizon scales matter fields ✔ ✔ ✘ Clustering DE a dynamical (scalar) small sound speed, minimally (“cold” DE models) degree of freedom clustering at sub-H coupled to matter Interacting DE ✔ ✔ ✔ (Coupled and Extended a dynamical (scalar) fluctuations sourced non-minimally Quintessence, degree of freedom by the interaction coupled to matter Modified Gravity) Marco Baldi - Dark Energy Simulations - Ringberg, 25 VI 2012
M. Baldi: overview on N-body & DE Summary of the results obtained in the last 10 years on DE observational features from N-body simulations Marco Baldi - Dark Energy Simulations - Ringberg, 25 VI 2012
M. Baldi: overview on N-body & DE Summary of the results obtained in the last 10 years on DE observational features from N-body simulations gadget (TreePM) MB 2011 Variable couplings can produce opposite effects with respect to constant couplings on the nonlinear matter power spectrum, the density profiles, and the c-M relation Marco Baldi - Dark Energy Simulations - Ringberg, 25 VI 2012
M. Baldi: overview on N-body & DE Summary of the results obtained in the last 10 years on DE observational features from N-body simulations MB & Pettorino 2011; MB 2012 gadget (TreePM) gadget (TreePM) MB 2011 CMB normalization!!! cDE can increase the Variable couplings can number of high-z massive produce opposite clusters even for CMB effects with respect to normalization, and for the constant couplings on case of a SUGRA potential, the nonlinear matter even for a simultaneous power spectrum, the CMB and z=0 normalization density profiles, and the c-M relation Marco Baldi - Dark Energy Simulations - Ringberg, 25 VI 2012
M. Baldi: overview on N-body & DE Summary of the results obtained in the last 10 years on DE observational features from N-body simulations MB & Pettorino 2011; MB 2012 gadget Large N-body (TreePM) gadget simulations of several (TreePM) MB 2011 different cDE models CMB are now publicly normalization!!! available through the CoDECS Project gadget (TreePM) cDE can increase the Variable couplings can number of high-z massive produce opposite clusters even for CMB effects with respect to normalization, and for the constant couplings on case of a SUGRA potential, the nonlinear matter even for a simultaneous power spectrum, the CMB and z=0 normalization density profiles, and http://www.usm.lmu.de/~mbaldi/CoDECS the c-M relation Marco Baldi - Dark Energy Simulations - Ringberg, 25 VI 2012
Y . Ayaita: simulations of growing ν The formation of large-scale neutrino lumps including relativistic corrections, mass perturbations, and the backreaction effect
Y . Ayaita: simulations of growing ν The formation of large-scale neutrino lumps including relativistic corrections, mass perturbations, and the backreaction effect
B. Li: the MG code ECOSMOG
B. Li: the MG code ECOSMOG status of simulations: codes
工欲善其事，必先利其器 B. Li: the MG code ECOSMOG status of simulations: codes one who wants to get things well done must first have tools well prepared extended quintessence G chameleon ECOSMOG G symmetron f(R) gravity coupled quintessence G dilaton
B. Li: the MG code ECOSMOG status of simulations: runs models box size N particle N mesh N realisation 32Mpc/h 128^3 128^3 20 f(R) w/ f R0 = 1e-5 64Mpc/h 256^3 256^3 10 f(R) w/ f R0 = 1e-5 100Mpc/h 256^3 256^3 5 f(R) w/ f R0 = 1e-6/5/4 128Mpc/h 512^3 512^3 5 f(R) w/ f R0 = 1e-6/5/4 250Mpc/h 512^3 512^3 1 f(R) w/ f R0 = 1e-6/5/4 250Mpc/h 1024^3 1024^3 1 f(R) w/ f R0 = 1e-6/5/4 500Mpc/h 512^3 512^3 1 f(R) w/ f R0 = 1e-6/5/4 1.0Gpc/h 1024^3 1024^3 1 f(R) w/ f R0 = 1e-6/5/4 1.5Gpc/h 1024^3 1024^3 6 f(R) w/ f R0 = 1e-6/5/4 128Mpc/h 256^3 256^3 10 X 5 generalised chameleon 128Mpc/h 256^3 256^3 10 X 5 generalised symmetron 128Mpc/h 256^3 256^3 12 X 5 generalised dilaton
B. Li: the MG code ECOSMOG a general evolution path HS f(R) model HS f(R) model HS f(R) model f R0 = 1e-6 f R0 = 1e-5 f R0 = 1e-4 stage b end of stage ci well into stage cii
E. Puchwein: the MG code MG-GADGET A version of Gadget suitable for modified gravity models. The nonlinear Poisson solver is based on “adaptive tree refinement”
E. Puchwein: the MG code MG-GADGET A version of Gadget suitable for modified gravity models. The nonlinear Poisson solver is based on “adaptive tree refinement” mg-gadget ecosmog Puchwein, MB & Springel, in prep.
F . Schmidt: simulating Vainshtein N-body solver for modified gravity theories with Vainshtein screening mechanism
F . Schmidt: simulating Vainshtein N-body solver for modified gravity theories with Vainshtein screening mechanism
F . Schmidt: simulating Vainshtein N-body solver for modified gravity theories with Vainshtein screening mechanism
H. Winther: voids in modified gravity Statistics and density profiles of voids from the Symmetron N-body simulations by Davis et al. 1108.3081
H. Winther: voids in modified gravity Statistics and density profiles of voids from the Symmetron N-body simulations by Davis et al. 1108.3081
H. Winther: voids in modified gravity Statistics and density profiles of voids from the Symmetron N-body simulations by Davis et al. 1108.3081
G.B. Zhao: environmental dependence Mass difference between dynamical and lensing mass due to environmental dependent screening as appearing in simulations
G.B. Zhao: environmental dependence Mass difference between dynamical and lensing mass due to environmental dependent screening as appearing in simulations
E. Jennings: RSD in modified gravity Density and velocity power spectra extracted from large N-body simulations of f(R) models
E. Jennings: RSD in modified gravity Density and velocity power spectra extracted from large N-body simulations of f(R) models
Conclusions The Ringberg conference brought together experts in theoretical modeling and numerical simulations of non-standard DE scenarios General agreement that DE and MG should be treated as a single phenomenon The simulations sessions have shown that an impressive number of independent efforts towards simulating DE/MG models are being pursued in the community Multiple independent codes based on different basic algorithms have been developed, and could now be tested against each other Some first post-processing tools are also being developed and start providing results on possible specific diagnostics about the nature of gravity and DE
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