Cosmological Simulations

Numerical CLONESThe Universe or at least part of it

In memory of Cécile Renault

You are somewhere therein!

Jenny Sorce Centre de Recherche Astrophysique de Lyon Webinar dark energy - May 11th 2021 Motivation : ΛCDM ? Current strategy

Observations Simulations ?

Directly Cosmological Observable Model Universe

Jenny Sorce (CRAL) CLONES 2021 2 Motivation : ΛCDM ? Current strategy

Observations Simulations ?

Directly Cosmological Observable Model Universe

If all goes well… it is a perfect match

Jenny Sorce (CRAL) CLONES 2021 3 Motivation : ΛCDM ? In practice

Observations Simulations ?

Directly Cosmological Observable Model Universe

Observations Simulations

Springel

Overall: ΛCDM

Jenny Sorce (CRAL) CLONES 2021 4 Motivation : ΛCDM ? Toward precision cosmology

Precision Era: ΛCDM checked on all scales 1-2% precision

Observational Dark matter only

Duffy 2014 Fosalba2017

Ned

Deeper and higher and higher larger surveys resolution simulations

Jenny Sorce (CRAL) CLONES 2021 5 Motivation : ΛCDM ? Toward precision cosmology

Precision Era: ΛCDM checked on all scales 1-2% precision

With baryons Dark matter only

Illustris TNG website Fosalba2017

Ned

higher and higher resolution simulations

Zoom Simulations to retain large scale effects

Jenny Sorce (CRAL) CLONES 2021 6 Motivation : ΛCDM ? Toward precision cosmology

Precision Era: What is in there? 1-2% precision

Thermal Energy

shocks

AGN tive ➝ B cooling Radia

supernova

Star formation

+ Cosmic Rays, etc

What more can we do wrt these typical simulations and why ?

Jenny Sorce (CRAL) CLONES 2021 7 Motivation : ΛCDM ? with more precision come some tensions !

Let’s start with why

Example: Equation of state of the dark energy

ΛCDM ObservationCamarena+2018

w= p/ρ tensions

hlocal

Jenny Sorce (CRAL) CLONES 2021 8 Motivation : ΛCDM ?

Precision is not accuracy !

Jenny Sorce (CRAL) CLONES 2021 9 Motivation : ΛCDM ? Precision is not accuracy: environmental biases?

Example: Equation of state of the dark energy

ΛCDM ObservationCamarena+2018

w= p/ρ tensions

hlocal

biases due to our environment?

Jenny Sorce (CRAL) CLONES 2021 10 Motivation : ΛCDM ? Both precision and accuracy are required!

Example: Equation of state of the dark energy

ΛCDM Camarena+2018 Without cosmic variance w=

p/ρ With cosmic variance

hlocal

Accuracy: 1% bias non-negligible

Jenny Sorce (CRAL) CLONES 2021 11 ΛCDM questioned? Precision cosmology

When observations challenge ΛCDM

Jenny Sorce (CRAL) CLONES 2021 12 ΛCDM questioned? Precision cosmology

A few examples

Small scales local scales Large scales

local / global H0 CMB Thin disks of satellites North/South Asymmetry

>3σ

Science Francis+2010 Observed… not simulated very unlikely…

Famaey+2013, Bullock+2017

Freedman+2017 e.g. Schwarz+2016

Jenny Sorce (CRAL) CLONES 2021 13 ΛCDM questioned? Precision cosmology

A few examples

Small scales local scales Large scales

local / global H0 CMB Thin disks of satellites North/South Asymmetry

>3σ

Science Francis+2010 Observed… not simulated very unlikely…

Famaey+2013, Bullock+2017 Freedman+2017

e.g. Schwarz+2016

Jenny Sorce (CRAL) CLONES 2021 14 ΛCDM questioned? Precision cosmology

A few examples

Small scales local scales Large scales

local / global H0 CMB Thin disks of satellites North/South Asymmetry

>3σ

Science Francis+2010 Observed… not simulated very unlikely…

Famaey+2013, Bullock+2017 Freedman+2017 e.g. Schwarz+2016

More examples: local void emptier with larger , CMB/ clusters σ8, lack of angular correlation at large scales local correlations slope and scatter, missing satellites, cold spot, etc

Jenny Sorce (CRAL) CLONES 2021 15 Local-induced biases ?

Can our local environment bias our ‘’perception’’ at the 1-2% level preventing us from reaching 1-2% accuracy…

Small scales Local scales Large scales

Are we comparing apple to apple? Are we a neutral observer? What about foreground effects? Do we understand enough?

A neutral environment? Photons travel a lot Correlation with environment Very unlikely… before reaching us…

and eventually decrease or increase tensions with ΛCDM ?

Jenny Sorce (CRAL) CLONES 2021 16 Local-induced biases ? on the small scales

Everything relies on the mass estimate of galaxy clusters

Planck

Dependence on the Pratt+2019 halo mass function estimate

Need to understand these physics laboratories before using them as cosmological probes Best known are closeby & Dependence on the environment !

Jenny Sorce (CRAL) CLONES 2021 17 Local-induced biases ? on the local scales

A simple example: if we live in a spherical underdensity

Hoscheit+2018 Hoscheit+2018 Keenan+2014 ΛCDM + KBC void

Observations

An example: Hint at a local underdensity up to z=0.07

Jenny Sorce (CRAL) CLONES 2021 18 Local-induced biases ? on the local scales

As many effect values as environments

Void

1.02

Wojtak+2013 Cluster

For an average environment: a 2% bias !

Jenny Sorce (CRAL) CLONES 2021 19 Local-induced biases ? on the large scales

Gravitational and the large scale surveys

photons photons Wojtak+2015 Void photons Void 10-3 uncertainty

photons

photons -0.001 Cluster future large scale surveys

Not bound overdensity l

As many effect values as environments

Wojtak +2015

Void Cluster Wojtak+2015

Value: [10-5 - 10-4] For an average environment: a 1-2% bias !

Jenny Sorce (CRAL) CLONES 2021 20 Local-induced biases ? on the large scales

Gravitational redshifts and the large scale surveys

photons photons Wojtak+2015 Void photons Void 10-3 uncertainty

photons

photons -0.001 Cluster future large scale surveys

Not bound overdensity l

As many effect values as environments

Wojtak +2015

Void Cluster Wojtak+2015

Value: [10-5 - 10-4] For an average environment: a 1-2% bias !

Jenny Sorce (CRAL) CLONES 2021 21 Local-induced biases ? on the large scales

Gravitational redshifts and the large scale surveys

photons photons Wojtak+2015 Void photons Void 10-3 uncertainty

photons

photons -0.001 Cluster future large scale surveys

Not bound overdensity l

As many effect values as environments

Wojtak +2015

Required Precision !

Void Cluster Wojtak+2015

Value: [10-5 - 10-4] For an average environment: a 1-2% bias !

Jenny Sorce (CRAL) CLONES 2021 22 Local-induced biases ? on the large scales

Gravitational redshifts and the large scale surveys

photons photons Wojtak+2015 Void photons Void 10-3 uncertainty

photons

photons -0.001 Cluster future large scale surveys

Not bound overdensity l

As many effect values as environments

Wojtak +2015

Void Cluster Wojtak+2015

Value: [10-5 - 10-4] For an average environment: a 1-2% bias !

Jenny Sorce (CRAL) CLONES 2021 23 Local-induced biases ? on the large scales

Gravitational redshifts and the CMB

Wojtak+2015 photons Void photons 10-3 uncertainty photons Void Integrated Sachs-Wolfe & Rees-Sciama photons -0.001 Cluster photons Effectsfuture large scale surveys

l Not bound overdensity Maturi+2007 As many effect values as environments increasing sensitivity increasing Wojtakprecision WMAP = reducing +2015error bars

Void Clusterlocal foreground effect = ‘noise/ Wojtak+2015 bias’ Value: [10-5 - 10-4] For an average environment: a 1-2% bias !

Jenny Sorce (CRAL) CLONES 2021 24 Accounting for the effects crude modeling

A crude modeling is a beginning…

but not nearly enough…

Jenny Sorce (CRAL) CLONES 2021 25 Accounting for the effects crude modeling

A few examples

Small scales Local scales Large scales

H0 local / global local global

Average broken North/South asymmetry Science ~2 Underdense

Publication year Francis+2010

Do we live in a filament that But correction from reproduces exactly that thin In what kind of density surveys only… plane? do we live exactly?

Jenny Sorce (CRAL) CLONES 2021 26 Accounting for the effects crude modeling

A few examples

Small scales Local scales Large scales

H0 local / global local global

Average broken North/South asymmetry Science ~2 Underdense

Publication year Francis+2010

Do we live in a filament that In what kind of density But correction from redshift reproduces exactly that thin do we live exactly? surveys only… plane?

Jenny Sorce (CRAL) CLONES 2021 27 Accounting for the effects crude modeling

A few examples

Small scales Local scales Large scales

H0 local / global local global

Average broken North/South asymmetry Science ~2 Underdense

Publication year Francis+2010

Do we live in a filament that In what kind of density But correction from redshift reproduces exactly that thin do we live exactly? surveys only… plane?

That concludes why we might want to do more

Jenny Sorce (CRAL) CLONES 2021 28 Accounting for the effects Summary

Let’s continue with what more wrt typical simulations can we do or reformulating how can we build a local modeling in order to account for the local-induced biases?

CLONES = Constrained LOcal & Nesting Environment Simulations

Jenny Sorce (CRAL) CLONES 2021 29 Local Universe’s initial conditions constrained initial conditions

Bayes1761 Wiener1942 Hoffman & Ribak 1991 Zaroubi+1995 van der Weijgaert & Bertshinger 1996

Jenny Sorce (CRAL) CLONES 2021 30 Local Universe’s initial conditions constrained initial conditions

Part of the Universe at 13.7 light-Gyr Photons received today have been emitted when it was ~380 000 yrs. old

Homogeneous and Isotropic Universe

Probability excess to have an object at a distance r from Gaussian white noise w(k) and power spectrum are another = autocorrelation of the density contrast = initial density sufcient to get a … Fourier transform of the power spectrum feld RANDOM realization = whatever part of the Universe

Constrained initial Applying local constraints conditions

Jenny Sorce (CRAL) CLONES 2021 31 Local Universe’s initial conditions constrained initial conditions

Baryons 3% Constraints Redshift surveys peculiar velocities peculiar velocities Work + density Kitaura2008,2012, ☑ constraints 2013 Hess+2013 Dark Lavaux2010, ☑ matter Jasche+2013-tdy Dark 27% Wang+2014-tdy ☑ Energy 70% Klypin+2003 ☑

Sorce+2014-tdy ☑

no luminosity bias • Account for the entire underlying gravitational field • Correlated on large scale • Highly linear e.g. Tully+(including Sorce)2013, Tully+(including Sorce)2016

Jenny Sorce (CRAL) CLONES 2021 32 Peculiar velocities catalog direct distance measurements

v radial pec =vobs- H0 x d

m-M ∝ log(d)

Jenny Sorce (CRAL) CLONES 2021 33 Method Sorce & Tempel 2017,2018

Radial peculiar velocity catalog vrad

Grouping + + Sorce 2015, 2018 Theoretical Observed Minimization of biases N

vrad Wiener filtering

Wiener1942 Doumler+2013 Sorce+2014

Reverse Zel’dovich Approximation Vrad Random field V 3D + + +

Constrained realization

Hoffman & Ribak 1991

Constrained initial conditions

Jenny Sorce (CRAL) CLONES 2021 34 Method Sorce & Tempel 2017,2018

Radial peculiar velocity catalog vrad

Grouping + + Sorce 2015, 2018 Theoretical distance catalog Observed Minimization of biases N

vrad Wiener filtering

Wiener1942 Doumler+2013 Sorce+2014

Reverse Zel’dovich Approximation Vrad Random field V 3D + + +

Constrained realization

Hoffman & Ribak 1991

Constrained initial conditions

Jenny Sorce (CRAL) CLONES 2021 35 Method Sorce & Tempel 2017,2018

Radial peculiar velocity catalog vrad

Grouping + + Sorce 2015, 2018 Theoretical Distance (modulus) of the groupObserved and its uncertainty Minimization of biases N

vrad Wiener filtering

Wiener1942 Doumler+2013 Sorce+2014 Peculiar velocity of the group and its uncertainty

Reverse Zel’dovich Approximation Vrad Random field V 3D + + +

Constrained realization

Hoffman & Ribak 1991

Constrained initial conditions

Jenny Sorce (CRAL) CLONES 2021 36 Method Sorce & Tempel 2017,2018

Radial peculiar velocity catalog vrad

Grouping + + Sorce 2015, 2018 Theoretical Distance (modulus) of the groupObserved and its uncertainty Minimization of biases N

vrad Wiener filtering

Wiener1942 Doumler+2013 Sorce+2014 Peculiar velocity of the group and its uncertainty Reverse Zel’dovich Approximation The difficulty is Vto determine properly the radgroups ! Random field V 3D + + +

Constrained realization

Hoffman & Ribak 1991

Constrained initial conditions

Jenny Sorce (CRAL) CLONES 2021 37 Method Sorce & Tempel 2017,2018

Radial peculiar velocity catalog vrad

Grouping + + Sorce 2015, 2018 Theoretical Observed Minimization of biases N

vrad Wiener filtering Corrected peculiar velocities Wiener1942 Doumler+2013 Sorce+2014

Reverse Zel’dovich Approximation Vrad Random field V 3D + + + Probability ∉ Gaussian Weighted uncertainty Constrained realization Final uncertainty ∝ d & nconstraints

Hoffman & Ribak 1991

Constrained initial conditions

Jenny Sorce (CRAL) CLONES 2021 38 Method Sorce & Tempel 2017,2018

Radial peculiar velocity catalog vrad

Grouping + + Sorce 2015, 2018 Theoretical Observed Minimization of biases N

vrad Wiener filtering

Wiener1942 Doumler+2013 Sorce+2014

Reverse Zel’dovich Approximation Vrad Linear minimum variance estimator Random field V 3D + + + Data = Model Constrained realization constraints

Hoffman & Ribak 1991 Correlation functions Constrained initial conditions

Jenny Sorce (CRAL) CLONES 2021 39 Method Sorce & Tempel 2017,2018

Radial peculiar velocity catalog vrad

Grouping + + Sorce 2015, 2018 Theoretical Observed Minimization of biases N

vrad Wiener filtering

Wiener1942 Doumler+2013 Sorce+2014

Reverse Zel’dovich Approximation Vrad Linear minimum variance estimator Random field V 3D + + + Data = power spectrum Model Constrained realization constraints

Hoffman & Ribak 1991 Correlation functions Constrained initial conditions

Jenny Sorce (CRAL) CLONES 2021 40 Method Sorce & Tempel 2017,2018

Radial peculiar velocity catalog vrad

Grouping + + Sorce 2015, 2018 Theoretical Observed Minimization of biases N

vrad Wiener filtering

Wiener1942 Doumler+2013 Sorce+2014

Reverse Zel’dovich Approximation Vrad Random field V 3D + + +

Constrained realization Position of the progenitors

Hoffman & Ribak 1991

Constrained initial conditions growth rate

Jenny Sorce (CRAL) CLONES 2021 41 Method Sorce & Tempel 2017,2018

Radial peculiar velocity catalog vrad

Grouping + + Sorce 2015, 2018 Constrained Realization: Estimate ofTheoretical the residual Observed Minimization of biases & N

Correlationvrad functions Wiener filtering depend only on the model

Wiener1942 Doumler+2013 Sorce+2014

Reverse Zel’dovich Approximation Vrad V Random field 3D + + +

Constrained realization

Hoffman & Ribak 1991

Constrained initial conditions

Jenny Sorce (CRAL) CLONES 2021 42 Method Sorce & Tempel 2017,2018

Radial peculiar velocity catalog vrad

Grouping + + Sorce 2015, 2018 Theoretical Observed Minimization of biases N

vrad Wiener filtering

Wiener1942 Doumler+2013 Sorce+2014

Reverse Zel’dovich Approximation Vrad V Random field 3D + + +

Constrained realization

Hoffman & Ribak 1991

Constrained initial conditions

Jenny Sorce (CRAL) CLONES 2021 43 Results: the local large scale CLONE z=0, large scale Sorce+2016

500 Mpc/h, 1024^3 particles, DM only, Planck cosmology

Note the fingers of gods

Jenny Sorce (CRAL) CLONES 2021 44 Results: the local large scale CLONE z=0, large scale Sorce+2016

500 Mpc/h, 1024^3 particles, DM only, Planck cosmology

Note the fingers of gods

Jenny Sorce (CRAL) CLONES 2021 45 Results: the local large scale CLONE z=0, large scale Sorce+2016

500 Mpc/h, 1024^3 particles, DM only, Planck cosmology

Note the fingers of gods

Jenny Sorce (CRAL) CLONES 2021 46 Results: the local large scale CLONE z=0, large scale Sorce+2016

Average variance between pairs of random fields of 300 Mpc/h aside

Random 0.6 Constrained different RR 1.0 Constrained same RR 0.5 N(>d)/N 0.4

σ 0.3 Reduced 0.5 cosmic variance tot 0.2 Average variance between 0.1 pairs of constrained fields of 400 Mpc/h aside 0.0 0.0 0 100 200 300 400 500 Size of the sub-box (h-1 Mpc)

Jenny Sorce (CRAL) CLONES 2021 47 ! Virgo ! Centaurus ! Virgo! Hy!draVirgo! Cen! ta!VuriurPgseor!seuCsen! taVu! riruHgsoy!dra!CenCtoamu! rauHsy!draC! enPtearu!sreuuHssydra! Per!seuH!syCdroam! aPerseu!s Com! aPerseu!s Coma ! Coma 100 ! 100 ! 100 ! 100 ! ! 100 ! ! ! ! ! ! ! ! ! ! ! ! ! ! ! Results: the local clusters CLONES z=0, cluster scale Sorce 2018 u u u u u 80 ! 80 ! 80 ! 80 ! ! 80 ! ! ! ! ! ! ! ! ! ! ! ! ! ! ! m m m m m ! ! ! ! ! ! ! ! ! ! ! ! ! ! ! ! i i i i ! ! ! ! i s s s s s 60 ! 60 ! 60 ! 60 ! ! 60 ! ! ! ! ! ! ! ! ! ! ! ! ! ! ! ! ! ! ! ! % % % % % 40 ! 40 ! 40 ! 40 ! ! 40 ! ! ! ! ! ! ! ! ! ! ! ! ! ! ! Dark matter halos = counterparts of observed local clusters 20 ! 20 ! 20 ! 20 ! ! 20 ! ! ! ! ! ! ! ! ! ! ! ! ! ! ! 0 ! 0 ! 0 ! 0 ! ! 0 ! ! ! ! ! ! ! ! ! ! ! ! ! ! ! 12 Virgo ! Centaurus12 Virgo! H1y2draVirgo! C1e2nta!VuriurPgseor!seuC1se2ntaVirgoVu! riruHgs o yCentaurus!dra!CenCtoamu! r a uHydraHsy!dr aC! e nPComatearu!sreuuHssydra! Per!seuH!syCdroam! aPerseu!s Com! aPerseu!s Coma ! Coma ) ) ) ) ) ! ! ! ! ! ! ! ! ! ! ! ! !! ! ! ! ! ! ! ! ! ! ! ! ! ! ! ! ! ! ! ! ! ! ! ! ! ! ! ! ! ! ! ! ! ! ! ! ! ! ! ! ! ! ! ! ! ! ! o o o o . o . . . . 10 ! ! 1! 0 ! 1! 0 ! ! 1! 0 ! ! ! 1!0 ! ! ! ! !! ! ! ! ! ! ! ! ! ! ! ! ! ! ! ! ! ! ! ! ! ! ! ! ! ! ! ! M M M M M 1 1 1 1 1 ? ? ? ? ? 8 ! 8 ! 8 ! 8 ! ! 8 ! ! ! ! ! ! ! ! ! ! ! ! ! ! ! h h h h h ! ! ! ! ! ! ! ! ! ! ! ! ! ! ! ! ! ! ! ! ! ! ! ! ! 4 4 4 4 4 1 1 1 1 1 6 ! 6 ! 6 ! 6 ! ! 6 ! ! ! ! ! ! ! ! ! ! ! ! ! ! ! 0 0 0 0 0 1 1 1 1 1 ( ( ( ( ( ! ! ! ! ! 4 ! 4 ! 4 ! 4 ! ! 4 ! ! ! ! ! ! ! ! ! ! ! ! ! ! ! M M M M M 2 ! 2 ! 2 ! 2 ! ! 2 ! ! ! ! ! ! ! ! ! ! ! ! ! ! ! 0 ! 0 ! 0 ! 0 ! ! 0 ! ! ! ! ! ! ! ! ! ! ! ! ! ! ! ! 1st 2nd 3rd ! 1st 2nd ! 3rd1st ! 2nd1!st3rd21nsdt ! 23nrdd1!st3!rd21nsdt1!st23nrdd21!nsdt3!rd231nrsddt 1!st23n!rdd21nsdt31!rsdt23nrdd21!nsdt3!rd231nrsddt 1!st23nrdd21nsdt3!rd23nrdd1!st3!rd21nsdt 1!st23nrdd21nsdt3!rd23nrd1!st3rd21nsdt ! 23nrdd1st3rd2nd ! 3rd1st 2nd 3rd Generation Generation GeneraGtioenneGraetnioenraGtioeneGraeGtnioeennraeGtriaoetnioeGnraeincreasingGtnioernaeGtriaoeGtn idistanceoenraeGtriaoetnioeGnraeGtnioernaeGtriaoetnioernaGtioeneGraeGtnioenraeGtriaoetnioernaGtioeneGraetnioenraGtioeneration Generation

Jenny Sorce (CRAL) CLONES 2021 48 Results: the Local Group CLONES = HESTIA z=0, group scale

induced by the local environment, not directly constrained (non-linear scales)

Salomon Sohn+2012 +2016

An example of application: in favor of a higher tangential velocity

Carlesi,Sorce+2016 Carlesi,Hoffman,Sorce+2016 Carlesi,Hoffman,Sorce+2017 Libeskind+(including Sorce)2020

Jenny Sorce (CRAL) CLONES 2021 49 The Virgo CLONE Simulated Virgo & Random clusters

Small residual cosmic variance

Rhapsody (Hahn +2017)

500 Mpc/h, 20483 particles effective (20 Mpc/h zoom), 3.8 kpc/h, DM only, Planck cosmology

Jenny Sorce (CRAL) CLONES 2021 50 The Virgo galaxy cluster CLONE

Overall agreement with observations

Sorce, Blaizot, Dubois 2019

Jenny Sorce (CRAL) CLONES 2021 51 The Virgo galaxy cluster CLONE

Velocity

Spin

➙ Environment

Sorce, Blaizot, Dubois 2019

Jenny Sorce (CRAL) CLONES 2021 52 The Virgo galaxy cluster CLONE

Number of substructures

Center of mass offset wrt spherical center

➙ History

Sorce, Blaizot, Dubois 2019

Jenny Sorce (CRAL) CLONES 2021 53 The Virgo galaxy cluster CLONE

Selection: No mass bias!

Sorce, Blaizot, Dubois 2019

Jenny Sorce (CRAL) CLONES 2021 54 The Virgo galaxy cluster CLONE

Selection: No mass bias!

➙ History

➙ Environment

Different from an average random cluster

Sorce, Blaizot, Dubois 2019

Jenny Sorce (CRAL) CLONES 2021 55 The Virgo galaxy cluster CLONE Sorce+2021 Simulated & Observed Virgo clusters

−1 −1 -1-1 -1-1 Hubble law with H0 = 67.77 km s Mpc Hubble law with H0 == 67.7767.77 kmkm ss MpcMpc Running Median (1.5 Mpc) Running Median (1.5 Mpc) 2000 Fit 2000 Fit

1000 1000 ) ) ) 1 -1 -1 − (km s (km s (km s c c c 0 0 v v v 400 400

200 200 ) ) ) 1 -1 − -1 0 0 (km s (km s (km s c c −1000 -1000 c v v v

−200 -200

−400 -400 2.95 4.425 5.9 7.375 8.85 2.95 4.425 5.9 7.375 8.858.85 Rc (Mpc) R (Mpc)(Mpc) −2000 -2000 cc R R R R 0 vir 2.95 ZV 5.9 8.85 11.8 14.75 17.7 20.65 0 vir 2.95 ZV 5.9 8.85 11.8 14.75 17.7 20.65 Rc (Mpc) Rc (Mpc)

500 Mpc/h, 8192^3 particles effective (20 Mpc/h zoom), 0.24 kpc/h hydrodynamics: SN and AGN feedback, Planck cosmology

Overall agreement with observations

Jenny Sorce (CRAL) CLONES 2021 56 The Virgo galaxy cluster CLONE Sorce+2021

* log(M /MO •) 14 12 10 8 6

Boselli+2016 Boselli+2016 - Schechter fit Simulation 1.8 r 1000 Simulation 1.8 rvir, simulated 1000 Simulation 2.5 rvir, observed vir, simulated Simulation - Schechter fit )

100 100 -1 ) -1 N (mag N ((0.5 dex)

10 10

Ferrarese+2016 Ferrarese+2016 - Schechter fit Simulation r=0.15 Mpc Simulation r=0.12 Mpc Simulation r=0.17 Mpc 1 1 -20 -18 -16 -14 -12 NUV (AB mag)

Overall agreement with observations

Jenny Sorce (CRAL) CLONES 2021 57 The Virgo galaxy cluster CLONE Sorce+2016

Boselli+2008,2014: from observation, only small mergers within the past few Gyrs

From simulation

Quieter merging history = no major merger

Sorce+2016

500 Mpc/h, 5123 particles, DM only, Planck cosmology

Agreement with observational predictions

Jenny Sorce (CRAL) CLONES 2021 58 The Virgo galaxy cluster CLONE Sorce+2016

West & Blakeslee 2000 : from observation, formation along a filament

From simulation

Preferential direction of infall = filament

500 Mpc/h, 5123 particles, DM only, Planck cosmology Agreement with observational predictions

Jenny Sorce (CRAL) CLONES 2021 59 The Virgo galaxy cluster CLONE

Lisker+2018: from observation, remnant of a group of ~10% mcluster that infall 2-3 Gyr ago

From simulation

Olchanski & Sorce 2018 only one merger of ~10% mcluster within the past 4 Gyr

Small group that merged within the Sorce+2021 500 Mpc/h, 5123 particles, DM only, Planck cosmology last few Gyrs

500 Mpc/h, 8192^3 particles effective (20 Mpc/h zoom), 0.24 kpc/h - Hydrodynamics: SN and AGN feedback, Planck cosmology Agreement with observational predictions Jenny Sorce (CRAL) CLONES 2021 60 The Virgo galaxy cluster CLONE

Observation 2000 Lisker+ 2018

1000

) virial radius -1 (km s 0 relc, hel v -1000

-2000 0.0 0.75 1.50 2.25 d from center (Mpc)

/ centre line-of-sight Group of galaxies that fell Sorce, Dubois, Blaizot+ in prep. within the line-of-sight?

Jenny Sorce (CRAL) CLONES 2021 61 The Virgo galaxy cluster CLONE

Observation Simulation - Perfect alignment Obs - M87 - MG 2000 2000 Lisker+ 2018

1000 1000 ) ) -1 -1 (km s 0 (km s 0 relc, hel relc, hel v v -1000 -1000

-2000 -2000 0.0 0.75 1.50 2.25 0.0 0.75 1.50 2.25 d from center (Mpc) d from center (Mpc)

Group of galaxies that fell Sorce+2021 within the line-of-sight?

Jenny Sorce (CRAL) CLONES 2021 62 The Virgo galaxy cluster CLONE

Observation Simulation - Align.: Obs - M87 - 2/3 MG-M60 vector 2000 2000 Lisker+ 2018

1000 1000 ) ) -1 -1 (km s 0 (km s 0 relc, hel relc, hel v v -1000 -1000

-2000 -2000 0.0 0.75 1.50 2.25 0.0 0.75 1.50 2.25 d from center (Mpc) d from center (Mpc)

Group of galaxies that fell Sorce+2021 quasi within the line-of-sight

Agreement with observational predictions

Jenny Sorce (CRAL) CLONES 2021 63 The Virgo galaxy cluster CLONE Sorce+2021

Small group quasi in the 80 13.5 Gyrs line of sight 60 ) (Lisker+2018) o 40 80 20 15 11.9 Gyrs DEC ( 60 0 )

10 o 40 -20 20 260 220 180 DEC ( o 0 RA ( ) 80 9.98 Gyrs -20 60

) 260 220 180 o 40 RA (o) 20 DEC ( Slower accretion rate, 0 -20 only small galaxies 260 220 180 (Boselli+2017) RA (o) 80 80 ) 7.45 Gyrs 13.0 Gyrs

• O 60 60 ) ) o 40 o 40 20 20 DEC ( 80 DEC ( 0 10.9 Gyrs 0 60 )

-20 o -20 40 260 220 180 260 220 180 RA (o) 20 RA (o) DEC ( Mass (M 0 -20 14 80 260 220 180 9.08 Gyrs o 10 60 RA ( ) ) o 40 Main filament of infall 20

DEC ( (West & Blakeslee 2000) 0 -20 260 220 180 o 80 5.74 Gyrs RA ( ) 60 ) o 40 20 DEC ( 0 -20 260 220 180 RA (o)

4 6 8 10 12 14 Universe Age (Gyrs) Agreement with observational predictions

Jenny Sorce (CRAL) CLONES 2021 64 The CLONE Sorce+2017

Puppis-3 Cluster Cygnus A Cluster Chamaraux & Masnoux 2004 Ebeling+2002

ΛCDM challenges hidden in the Zone of Avoidance?

- number of

- longest structures

Vela Kraan-Korteweg+2017

Jenny Sorce (CRAL) CLONES 2021 65 The Zone of Avoidance CLONE Sorce+2017

Puppis-3 Cluster Cygnus A Cluster Chamaraux & Masnoux 2004 Ebeling+2002

ΛCDM challenges hidden in the Zone of Avoidance?

- number of superclusters

- longest structures

Vela Supercluster Kraan-Korteweg+2017

Jenny Sorce (CRAL) CLONES 2021 66 Some other examples: …

and more…

SLOW : local galaxies (Sorce, Dolag +) Cosmic Rays in the local Universe (Hackstein+2018)

Reionization of the local Universe (CoDa) Coma connectivity (Ocvirk+2020, Lewis+2020, etc) (Malavi, Aghanim, Sorce+)

Jenny Sorce (CRAL) CLONES 2021 67 Take home message Tensions = Do we need a new cosmological model?

To answer, nowadays : comparisons between typical cosmological simulations and observations

Small scales Local scales Large scales

Simulations of local estimates of cosmological CMB high sensitivity Galaxy formation & parameters experiment and large evolution scale surveys Biased Precision Cosmology

Jenny Sorce (CRAL) CLONES 2021 68 Take home message Tensions = Do we need a new cosmological model?

CLONES initial conditions for numerical specialists, theorists and observers

Small scales Local scales Large scales

4∗LU=3?

Simulations of unbiased local estimates of CMB high sensitivity Galaxy formation & cosmological parameters experiment and large evolution: scale surveys : foreground - reproduction effect correction - calibration Accurate Precision Cosmology

Jenny Sorce (CRAL) CLONES 2021 69 Thank you, Merci, Grazie, Gracias, Danke, спаси́ бо, Mahalo, , , ,Obrigada, Dank u ,תודה Tak, Cảm ơn, Dziękuję, Kiitos, Aitäh, diolch, dankewol, ಧನ#$ದಗ', …*

* Missing your ‘thanks’ spelling? It means I did not get the chance yet to visit your country but I am looking forward to do so ! (exceptions in red: I have not been but I have had the opportunity to learn how to say it)

Jenny Sorce (CRAL) CLONES 2021 70