Colloque national CMB-France #5

4 déc. 2023, 09:00 → 5 déc. 2023, 18:40 Europe/Paris

IAP

L'initiative CMB-France vise à mettre en place une animation scientifique au niveau national autour des études CMB (cmb-france.cnrs.fr).

Le CMB-France #5 aura lieu les 4 et 5 Décembre 2023 à l'Institut d'Astrophysique de Paris (IAP, Paris).

 

L'inscription est gratuite mais obligatoire: ici.

 

CMB-France peut prendre en charge les missions (dans la limite des stocks disponibles). 

Renseignez-vous auprès de M. Tristram.

 

L’agenda est en cours de finalisation mais l’idée de ces colloques est de:

• présenter les nouveautés scientifiques et les nouveaux résultats dans le domaine
• donner un statut sur l’avancement des expériences ou des projets en cours
• permettre aux jeunes (post-doc, PhD) de présenter leur travail

 

Nous mettrons une place une connexion afin de suivre les présentations: zoom

 

Les informations de connexion seront envoyées par la mailing-liste cmb-france. Pensez à vous inscrire.

 

 Cette action est soutenue par le PNCG.

lundi 4 décembre

10:00 Bienvenu

Contributions

1 Cosmology with the final Planck data release (PR4)

We present constraints on cosmological parameters using maps from the last Planck data release (PR4). In particular, we detail an upgraded version of the cosmic microwave background likelihood, HiLLiPoP, based on angular power spectra and relying on a physical modelling of the foreground residuals in the spectral domain. This new version of the likelihood retains a larger sky fraction (up to 75 %) and uses an extended multipole range. Using this likelihood, along with low-l measurements from LoLLiPoP, we derive constraints on ΛCDM parameters that are in good agreement with previous Planck 2018 results, but with 10 % to 20 % smaller uncertainties. We demonstrate that the foregrounds can be accurately described in the spectral domain with only negligible impact on ΛCDM parameters. We also derive constraints on single-parameter extensions to ΛCDM including AL , ΩK , Neff , and P mν . Noteworthy results from this updated analysis include a lensing amplitude value of AL = 1.036 ± 0.051, which aligns more closely with theoretical expectations within the ΛCDM framework. Additionally, our curvature measurement, ΩK = −0.012 ± 0.010, now demonstrates complete consistency with a flat universe, and our measurement of S8 is closer to the measurements derived from large-scale structure surveys (at the 1.6 σ level).

Orateur: Matthieu Tristram (IJClab, CNRS, France)

Planck PR4 Cosmology.pdf

2 Tensor-to-scalar ratio and beyond with CMB and gravitational waves

In my recent publication (arXiv:2208.00188), I adopted a comprehensive approach to refine the constraints on the tensor-to-scalar ratio ($r$) and the tensor spectral index ($n_t$). This involved utilizing data from 10 datasets, including those from the BICEP/Keck Array 2015 and 2018, Planck releases 3 and 4, and the LIGO-Virgo-KAGRA collaboration. During this presentation, I will walk through the two distinct approaches I employed to probe the tensor sector, determining the most reliable method. Moreover, I will present the results of this work, which establish the strongest constraint on the tensor-to-scalar ratio in the current literature: $r < 0.028$ and $−1.37 < n_t < 0.42$ at a 95% confidence level. Additionally, I will share some insight into my ongoing efforts to enhance this analysis within the tensor sector of parameter space.

Orateur: Giacomo Galloni (University of Rome Tor Vergata)

CMB_France_Galloni.pdf

3 Planck CO maps revisited

Publicly available maps of Galactic CO emission form Planck are contaminated by noise and/or emission from other foregrounds (SZ clusters, IR and radio sources, Galactic dust). Using a modified version of GNILC, we post-process existing Planck CO maps to produce substantially cleaner full-sky maps for the first three rotational lines of Galactic CO.

Orateur: Jacques Delabrouille (IN2P3)

CO-revisited-final.pdf

4 New PR4 dust intensity and polarization maps

We present new dust intensity and polarization maps obtained from Planck PR4 frequency maps.
Those maps are obtained using a modified version of GNILC that allows for better angular resolution in the final dust maps.

Orateur: Elisa Russier

CMB France conference propre.pdf

5 Revisiting the CMB anomalies at large scale: The impact of the Local universe.

Precise measurements of the CMB temperature fluctuations have highlighted the presence of unexpectedly strong anomalies on the largest scales. Among the possible explanations of these deviations, the role of the local large-scale structure (LSS), which contributes to the CMB signal via secondary anisotropies on these large scales, needs to be fully investigated.

In this talk, I will present our study of the thermal and kinetic Sunyaev-Zeldovich (tSZ and kSZ) signal from the local LSS, based on the constrained hydrodynamical simulation SLOW (Simulating the Local Web) reproducing the local Universe up to 350 Mpc. I will characterise the tSZ and kSZ maps of the local universe and I will show their impact on the standard statistics used to describe the CMB large-scale anomalies, with comparisons to their values in the latest Planck data.

Orateur: Gabriel Jung (IAS Orsay)

2023_12_04_slides.pdf

6 A Unified Framework for Mitigating Foregrounds and Systematic Effects for Tensor-to-Scalar Ratio and Birefringence Angle Measurements

Precise measurements of the faint primordial B-modes originating from cosmological inflation (parameterized by r), or from EB correlations coming from parity-violating mechanisms in the Universe (parameterized by the isotropic cosmic birefringence angle, β), require meticulous attention to the removal of Galactic foregrounds and the mitigation of systematic effects, as well as the interplay between the two.
In Jost et al. 2023 (PRD), we address this interplay by developing a map-based parametric component separation approach that considers polarization angle miscalibration and incorporates calibration priors. This framework propagates statistical and systematic errors from spectral and instrumental parameters to estimate r and β. In this talk I will show new applications of this approach. First, its utility in ground-based experiments for polarization angle calibration requirements and E-to-B leakage mitigation in the search for r. Secondly, this framework is used as one of the forecasting pipelines assessing LiteBIRD’s capabilities in measuring β under varying levels of foregrounds and systematic complexity. I will provide a brief overview of the other methodologies employed in this study and explain how this framework complements the diverse approaches utilized.

Orateur: Baptiste Jost (IPMU)

Baptiste Jost CMB France Dec 2023.pdf

Experiments

7 BICEP and CMB plans at the South Pole

Orateur: Dr Clem Pryke

20231204_paris_edit.pdf

8 CMB-S4

place holder for S4

Orateur: Jacques Delabrouille (IN2P3)

Delabrouille-CMBFrance-CMBS4-final.pdf

9 IN2P3 activities and developments for CMB-S4

CMB-S4 is the next generation CMB instrument, led by the US. It will observe the sky from Chile and the South Pole with 500000 detectors. The large scale of the project gives rise to numerous challenges in terms of instrument design, hardware production, data management and data analysis. Several IN2P3 laboratories are involved in this project, both from the data management/analysis and instrumental point of view. In this presentation I will give an overview of these activities, which are being consolidated into a cooperative research and development agreement. In particular, I will describe the contributions to the warm analog front-end electronics of the instrument and the proposed contributions in data management, which include data movement, metadata infrastructure, data simulation and data reduction.

Orateur: Manuel Gonzalez (Astroparticule et Cosmologie)

CMB-S4-IN2P3 CMB-France.pdf

10 Road to first light, an overview of Simons Observatory in 2024

The Simons Observatory (SO) is a new cosmic microwave background experiment being built on Cerro Toco in Chile, due to begin observations in the early 2024. SO will measure the temperature and polarization anisotropies of the cosmic microwave background in six frequency bands, from 27 to 280 GHz. The initial configuration of SO will have three small-aperture 0.5-m telescopes (SATs) and one large-aperture 6-m telescope (LAT), with a total of 60,000 cryogenic bolometers. The detector count, both on SATs and LAT, will double in 2028.

Our key science goals are to characterize the primordial perturbations, measure the number of relativistic species and the mass of neutrinos, test for deviations from a cosmological constant, improve our understanding of galaxy evolution, and constrain the duration of reionization. The SATs will target the largest angular scales observable from Chile, mapping ~10% of the sky to a white noise level of 2 μK-arcmin in combined 93 and 145 GHz bands, to measure the primordial tensor-to-scalar ratio, r, at a target level of σ(r)=0.003. The LAT will map ~40% of the sky at arcminute angular resolution to an expected white noise level of 6 μK-arcmin in combined 93 and 145 GHz bands, overlapping with the majority of the LSST sky region and partially with DESI.

In this talk we will present the science goals of SO as well as the status of it deployment as we approach first light. We will also summarise the recently approved plans to upgrade the current design (SO:UK, SO:JP and Advanced SO).

Orateur: Benjamin Beringue (APC, CNRS)

CMB-France_beringue.pdf

11 An additional High Frequencies KID French SAT for SO

In recent months, several discussions have taken place at different levels on the possibility of participating in the SO collaboration by adding a 20k-pixels KID-based SAT observing between 200 and 400 GHz.
Hardware participation will allow us to demonstrate 100 % French technology and to consolidate the scientific impact of the French community in one of the reference CMB projects for the next years.
We will give an overview of the proposed instrumental setup and present the scientific drivers.

Orateur: M. Andrea Catalano (LPSC - Grenoble)

CMB_France_20231204_r.pdf

16:15 Café

Contributions

12 Updated Constraints on Hubble Tension Solutions with Recent SH0ES and SPT-3G data

Since its appearance almost a decade ago, the Hubble Tension received a great deal of proposals to solve it, with none being completely successful. However, new state of the art data improve our assessment of these models and better constrain their parameters.
In this talk, an evaluation of eleven cosmological models is presented. These models consist of five classical extensions of ΛCDM, Early Dark Energy, the Majoron and the varying electron mass models, along with three of the latter’s extensions. This evaluation, previously performed using Planck, ACT and SDSS data, is now updated with recent SPT-3G and SH0ES data.
Using a set of tension metrics, these models are ranked based on which one is now out of the competition, and which requires further study before potentially becoming the new concordance model of Cosmology.

Orateur: Dr Ali Rida Khalife (IAP)

H0 Olympics with SPT3G II.pdf

13 A Differentiable Likelihood for CMB Analysis

CMB power spectrum measurements from ground-based experiments are expected to match and surpass Planck-precision on cosmological parameters in the immediate future. With this constraining power comes great responsibility; the potential of detecting physics beyond the standard model demands a demonstrably robust analysis.
In this talk, I present a differentiable likelihood for CMB analysis designed for this level of scrutiny. The likelihood code is written in python and can be interfaced with widely available analysis software. The software is designed to leverage the power of the JAX-library, such that when paired with a differentiable theory code it provides a fully differentiable analysis framework from cosmological parameters to the chi-squared value. I showcase the basic use of the likelihood and highlight several applications of a fully differentiable pipeline. I emphasise the scope of robustness tests and analysis optimisation exercises made feasible in the differentiable framework.

Orateur: Lennart Balkenhol (Institut d'Astrophysique de Paris)

cmbfrance_nov23.pdf

14 CMB Spectral Distortions Measurement Prospects

In the 1990s, the COBE/FIRAS mission measured the Cosmic Microwave Background (CMB) spectrum and showed that the CMB spectral energy distribution is close to a perfect blackbody. However, the CMB spectrum contains tiny departures from a perfect blackbody to $\Delta I/I \simeq 10^{-5}$. These are referred to as spectral distortions.
The two main types of CMB spectral distortions are the Compton $y$-distortion from energy release in the optically thin regime at redshifts $z < 5 \times 10^{4}$, and chemical potential or $\mu$-distortion from the optically thick regime imprinted at $z > 5 \times 10^{4}$. Measuring those faint signals is challenging but allows us to access information about the thermal history of the Universe, from the present to the very early Universe, that cannot be extracted in any other way.

High-precision spectroscopy of the CMB is one of the three themes that have been selected by the ESA Voyage 2050 program. Several dedicated space missions such as PIXIE, PRISTINE, and FOSSIL have been proposed since 2011. Additionally, balloon-borne missions, such as BISOU, have also been considered as a pathfinder of a future space mission dedicated to CMB spectral distortions.

I will present an effort undertaken to define future missions and instruments dedicated to measuring the CMB spectral distortions. Sensitivity estimates that could be reached by such projects are calculated by combining two newly developed models. The first is a versatile photometric model based on key instrument subsystem choices together with their parameters. The second is a sky emission model taking into account spatially varying foregrounds at frequencies relevant to CMB spectral distortions.
Optimizing both instrument concept and mission parameters (scanning strategy, mission duration, ...) can be achieved by combining the outputs of those models. This would be applied here in the case of future missions dedicated to CMB spectral distortion measurement such as FOSSIL, a space mission proposed to answer the recent ESA M7 proposal, and BISOU, a CNES Phase 0 study for a balloon-borne mission.

Orateur: Xavier COULON (IAS)

CMB_France.pdf

15 Spectral Imaging and Bolometric Interferometry: a new path for CMB polarimetry and foreground contamination mitigation

Spectral Imaging relies on the interferometric nature of a bolometric interferometer: the combination of fringes at the focal plane formed by the aperture array in the pupil plane results in a point spread function for the instrument that exhibits multiple peaks, each with a width corresponding to the angular resolution of the instrument. The angular distance separating the peaks is proportional to wavelength, exactly as in grism spectroscopy. This PSF is known as the synthesized beam.
The signal in each detector is therefore a linear combination of signals from different regions of the sky and different wavelength, in a manner that is perfectly known for an ideal instrument, and can be precisely calibrated through usual calibration, or even further with the interferometry-specific "self-calibration". A Bolometric Interferometer therefore has spectral information encoded in the detector signal, in contrast with a classical imager where this information is averaged out in the bandwidth.
A number of consequences follow that I will describe in this presentation:

• Ability to perform mapmaking into sub-bands within the physical bandwidth, resulting in a higher spectral resolution which allows for precise removal of foreground contamination (foregrounds with spectral features)
• Ability to perform foreground component map-making directly from Time-Ordered-Data with a number of advantages: simpler and more accurate noise modeling, direct account for systematics, better ability to reconstruct emission line foregrounds (eg. CO)
• The possibility of Ultra-Wide-Band focal planes, covering from 90-280 GHz with all detectors receiving photons from all frequencies, therefore increasing throughput by a significant factor with respect to classical imagers where the focal needs to be split into the distinct frequencies.

These feature will soon be tested with QUBIC and, if confirmed, could represent a significant breakthrough in CMB polarimetry.

Orateur: Mathias Regnier (APC)

Spectral-imaging with QUBIC

16 Accounting for the beams in the parametric component separation

Performing an efficient and reliable component separation is of fundamental importance for the data analysis of the current CMB experiments targeting primordial B-modes. In this talk I will present an extension of the parametric maximum likelihood-based component separation technique, where in the likelihood implementation it is allowed to go back and forth from the pixel to the harmonic domain. This, together with the implementation of a preconditioned conjugate gradient solver, allows us to reliably perform the component separation on more complex input frequency maps.
In particular, I will show how this method allows us to rigorously deal with beam-convolved input frequency maps. The approach used to date to account for the beams is to convolve all the frequency maps to a common resolution and then perform the component separation. In the alternative, more rigorous, method that I present we apply the beam deconvolution / convolution operations within the component separation step. These are performed in the harmonic domain, but the method still remains as much as possible in the pixel domain to exploit the advantages of pixel-based parametric component separation (e.g. dealing with the spatial variability of the foregrounds).

Orateur: Arianna Rizzieri (APC)

Rizzieri_CMB-France_2023.pdf

19:30 Diner

https://www.felicie.info/

mardi 5 décembre

Cross-correlations

17 More than the sum of its parts: joint analysis of LSS and CMB experiments

Through weak lensing and galaxy clustering measurements, future large-scale galaxy surveys will provide unprecedented constraints on the late Universe. On the other hand, high-quality CMB observations (Planck and future CMB experiments) can -- and already do -- put tight constraints on the early Universe. In this talk, I will show that combining these two sources of cosmological information can yield a significant lever arm and improve tremendously the constraints on our cosmological model. Moreover, I will also address the cross-correlation of those two types of signals, which can yield additional and significant constraints especially on extensions to the standard cosmological model. As a part of my talk, I will present in particular forecasts of the future Euclid x CMB cross-correlation constraints, performed by the CMB-cross correlations Science Working Group of the Euclid Collaboration.

Orateur: Stéphane Ilic (IJCLab)

Ilic_CMB_France_2023.pdf

18 Cosmology from weak lensing, galaxy clustering, CMB lensing and tSZ

Orateur: Karim Benabed

19 Cosmology from cross-correlations of unWISE galaxies and ACT DR6 CMB lensing

Orateur: Gerrit Farren

20 Opening-up a new window with projected-field cross-correlations

We present new methods and analyses of hybrid bispectra between large-scale-structure tracers projected on the sphere. Such cross-correlations have been recently measured for kSZ x galaxies (Kusiak et al 2021) and galaxies x CMB lensing (Farren et al 2023) and can be modeled using the halo-model formalism (Bolliet et al 2022). They will allow us to break degeneracies between parameters measured from 2-point analyses and should enable a significant increase in constraining power on the galaxy-halo connections, halo properties and galaxy biases, especially with the new wealth of forthcoming high-resolution and large-volume Stage 4 era data.

Orateur: Boris Bolliet (Cambridge)

BOLLIET

21 Constraining cosmology with Quaia quasars and CMB lensing

Quaia is a new full-sky high-redshift quasar catalog containing 1.5 million objects with estimated redshift derived from the Gaia DR3 quasar candidates. I will first present the work that went into the creation of the catalog using unWISE, SDSS data and a machine learning approach, as well as its decontamination from stars and dust extinction. I will then present the recent cosmological results based on the cross-correlation of QUaia and CMB lensing measurements of Planck. I will focus on the implication of these results for the S8 tension and local primordial non-Gaussianities. I will conclude discussing ongoing work to constrain the star formation history and the growth rate of LSS across cosmic time using Quaia

Orateur: Giulio Fabbian (Cardiff University)

11:00 Café

Experiments

22 LiteBIRD Status

While the LiteBIRD satellite mission is about to enter a new phase, both at the Japanese and European levels, I will make the status of the recent progress made and the perspectives for the next months and years.

Orateur: Ludovic Montier (IRAP)

23 Updates from SPT-3G

In this talk, I will review the current status of the SPT-3G project, present recent papers and highlight perspectives.

Orateur: Etienne Camphuis (Institut d'Astrophysique de Paris)

20231204_cmbfrance.pdf

Contributions

24 Constraining cosmic reionisation by combining the kinetic Sunyaev-Zel'dovich effect and the 21cm signal

During the Epoch of Reionisation (EoR), neutral hydrogen in the intergalactic medium can emit radiation through the 21cm hyperfine transition. The 21cm signal is a direct probe of this epoch, but a notoriously difficult observation to make.
On the other hand, the kinetic Sunyaev-Zel'dovich effect (pkSZ) is induced by the scattering of CMB photons with a medium of free electrons that possess a non-zero bulk velocity. These scatterings alter the small-scale CMB temperature anisotropies, which correlate with the growth of ionising regions during reionization.
So far, only upper limits have been set on both observables. We propose to leverage the information content enclosed in both power spectra to make the most of current observations.
We write both the 21cm and the pkSZ power spectra in terms of a simple parametric model of reionisation. This equation allows us to simultaneously use both data set to constrain the history and morphology of reionisation.
Through an MCMC analysis, we discover that these two observables exhibit complementary characteristics, leading to significantly improved constraints on reionisation compared to analysing each data set separately. We present how future measurements of the 21cm power spectrum with the SKA and the pkSZ power spectrum measurement are combined to constrain models of cosmic reionisation. Our findings demonstrate that a few well-informed measurements of the 21cm power spectrum and pkSZ data can precisely determine the reionisation history of the Universe.

Orateur: Adélie Gorce (McGill University)

CMBFrance Adélie Gorce.pdf

25 Toward the first public release of the NIKA2 data within the Sunyaev-Zeldovich Large Program

The Sunyaev-Zeldovich effect offers a powerful probe of the large-scale structures up to high redshifts. SZ-based cosmology, however, requires a precise characterization of cosmological tools such as a mass-observable scaling relation and a mean electronic pressure profile. Systematic effects, in particular at high redshift, have an impact on these tools and are currently the main limitation of cluster-based cosmology.

NIKA2, a millimeter camera installed at the IRAM 30-m telescope is a major experiment to extend our understanding of galaxy clusters. Combining sub-arcminute (17.6’’ at 150 GHz) angular resolution and a 6.5’ field-of-view diameter, NIKA2 can resolve and map the Sunyaev-Zel'dovich (SZ) effect towards clusters up to high redshifts. Combined with X-ray data from the XMM-Newton satellite, we can infer with high precision the thermodynamical properties and the hydrostatic masses of such objects within the NIKA2 SZ Large Program (LPSZ), which covers a representative sample of about 38 galaxy clusters at 0.5<z<0.9.

In this talk I will present the method selected for the public release preparation of the NIKA2 data, going from the Time-Ordered Data quality assessment in map-making to obtaining electronic pressure and mass profiles of individual clusters. Then, I will discuss a new method to combine all individual estimates while accounting for their intrinsic scatter, to infer the mean pressure profile of clusters.

Orateur: Corentin Hanser (UGA)

CMBFrance23_Hanser.pdf

26 A joint Planck and SPT-SZ measurement of CMB lensing cluster masses

We present the first CMB-lensing galaxy cluster mass measurement using a combination of ground and space-based surveys (SPT-SZ and Planck). We measure the signal at 4.8 sigma, a significant gain with respect to measurements performed on the two individual datasets. In particular, we show that we take advantage of correlations between the scales observed by SPT-SZ and the scales observed by Planck to improve the constraints on the lensing potential. This result demonstrates that Planck data will remain a key element in CMB-lensing cluster studies for decades to come.

Orateur: M. Alexandre Huchet (CEA Saclay)

HUCHET_Alexandre-CMB_France_2023.pdf

27 Cosmology with Planck-detected clusters: a new multi-wavelength analysis

Galaxy clusters are a powerful cosmological probe: they track the latest evolution of large scale structure and are therefore fundamental for testing the cosmological model in the recent Universe.
CMB experiments represent a great opportunity for cosmology with galaxy clusters: due to the inverse Compton scattering of CMB photons by the hot gas of clusters, they are signal-limited, full-sky (or at least large area) surveys of clusters.
To compare the observations of galaxy clusters with the theoretical prediction and thus constrain the cosmological parameters of the underlying model, a precise knowledge of clusters’ masses and redshift is required.
Scaling relations relating the mass with a given cluster observable (like the richness in optical wavelength, $Y_{SZ}$ in the mm-band or $Y_X$ in X-rays) are usually used to compute the mass of clusters.
We provide a new scaling relation using a large and representative sample of clusters from the Planck Early Sunyaev-Zeldovich catalogue that was observed in X-rays by Chandra, and compare it to the results of the Planck collaboration obtained from XMM-Newton observations.
We calibrate a new mass bias using weak-lensing data, obtain cosmological constraints from the Planck cosmological cluster sample and discuss the link between mass calibration and cosmological tensions.

Orateur: Gaspard Aymerich (Institut d'Astrophysique Spatiale, Université Paris-Saclay)

Pres_CMB_France.pdf

28 Characterising galaxy clusters' completeness function in Planck with hydrodynamical simulations

Galaxy cluster number counts are an important probe to constrain cosmological parameters. One of the main ingredients of the analysis, along with accurate estimates of the clusters' masses, is the selection function, and in particular the completeness, associated to the cluster sample one is considering. Incorrectly characterising this function can lead to biases in the cosmological constraints.
We study here the completeness of the Planck cluster catalog, whose clusters are detected at mm-wavelenghts via the Sunyaev-Zel’dovich effect by the Planck satellite. We estimate the completeness in the case in which the cluster model assumed in the detection method differs from the shapes and pressure profiles of true galaxy clusters, using mock cluster images from hydrodynamical simulations. We find that the shape of the cluster pressure profile has a significant effect on the completeness, while cluster morphologies have generally a small impact.

Orateur: Stefano Gallo

CMBFrance_Gallo_20231205.pdf

29 A comparison of the tSZ properties in the Horizon and Magneticum suite of hydrodynamical simulations

The distribution of matter in the Universe is a powerful probe of cosmology. Measuring the efficiency with which gravity produces clusters against expanding Universe is the key to understanding, e.g. the equation of state of dark energy. Numerous projects aim at measuring the matter distribution across time in the Universe but no observable gives the perfect figure of this distribution (because of instrumental limitation, astrophysical limitation, or because they probe different redshifts). Cross-correlation of different probes is a powerful way to lift these limitations. My work focuses on the construction of a robust halo model for the thermal Sunyaev-Zeldovich power spectrum (one such tracer of the LSS) and to cross-correlate it with different probes of the distribution of matter (lensing, CMB lensing, galaxy count,…). To do so, I work with an analytical halo model of this power spectrum and I measure different profiles and power spectrums in the Horizon and Magneticum suite of hydrodynamical simulations to compare both and to test hypotheses of the model, such as the pressure profiles in halos and their link with feedback. In this talk, I will present and comment my results on these comparisons.

Orateur: Emma Ayçoberry (IAP)

Aycoberry_CMB_france.pdf

16:00 Conclusions