Evolution of groups and clusters since z=1.5 in cosmological - PowerPoint PPT Presentation

Evolution of groups and clusters since z=1.5 in cosmological simulations Amandine M. C. Le Brun CEA Saclay DRF/IRFU Service d’Astrophysique Collaborators: Monique Arnaud (CEA Saclay), Iacopo Bartalucci (CEA Saclay), Ian McCarthy (LJMU), Jean-Baptiste Melin (CEA Saclay), Trevor Ponman (Birmingham), Gabriel Pratt (CEA Saclay), Joop Schaye (Leiden),… High-redshift Cluster Workshop, Paris, October 05 th -07 th 2016 1

cosmo-OverWhelmingly Large Simulations • WMAP7 & Planck 2013 cosmology • 2.15 billion particles in 400 Mpc/h boxes with 4 kpc/h gravitational softening run using modified version of GADGET3 (Springel 2005) • Resorts to subgrid modeling for unresolved small scale physics and varying it: 1. metal-dependent radiative cooling (Wiersma et al. 2009a) 2. chemodynamics and stellar evolution (Wiersma et al. 2009b) 3. star formation (Schaye & Dalla Vecchia 2008) 4. kinetic supernova feedback (Dalla Vecchia & Schaye 2008) 5. AGN feedback (Booth & Schaye 2009). 13 M ⊙ at z=0 in Planck • More than 14,000 groups and clusters with M 500 >10 cosmology. 2

Le Brun et al. 2014 X-ray observations Data: Pratt09, Vikhlinin09, Sun09 and Osmond04 • Need feedback of some sort to solve overcooling problem • AGN 8.0 model broadly reproduces relation over two orders of magnitude in mass • Increased heating temperatures result in under-luminous systems at all masses 3

Le Brun et al. 2014 X-ray observations Lin12, Maughan08 and Sun09 Data: REXCESS, Vikhlinin06, • Observed trend and scatter reproduced extremely well by AGN 8.0 • Achieved primarily by ejection of gas from high-redshift progenitors • Increased heating temperatures result in too much gas being ejected • REF also yields reasonable f gas but relation is flatter than observed. Here, low f gas are achieved by overly efficient SF. 4

Le Brun et al. 2014 Entropy profiles Data: Sun09, Johnson09 Data: Pratt10, Vikhlinin06 • All radiative models yield profiles that are similar to the observed ones in the central regions of groups but in clusters only AGN 8.0 provides an adequate match. • At larger radii, the AGN models with increased heating temperatures have too large entropies due to ejection of too much gas from progenitors. 5

Le Brun et al. 2014 Demographics of cluster cores Data: Croston08 • AGN 8.0 has a distribution which is remarkably similar to the observed one. • No strong evidence of bi-modality in both simulations and observations but does not necessarily imply that entropy is not bi-modal. 6

Le Brun et al. 2015 An aside: Non-universal pressure profile • Shape of pressure profile is quite strongly mass-dependent • Need to make two of the GNFW coefficients (normalisation and concentration) mass-dependent to obtain a reasonable fit (red line) over the whole radial and halo mass range when AGN feedback is included 7

Le Brun et al. 2014 Sunyaev-Zel’dovich properties Intermediate Results IV, Sun09 Data: Vikhlinin06, Planck Y X is in fact sensitive to ICM physics as arbitrarily large amounts of gas ejection cannot be compensated by T increase as T forced to be always close to T vir by HSE 8

Le Brun et al. 2014 Sunyaev-Zel’dovich properties Data: Planck Early Results and Intermediate Results • Integrated SZ signal clearly sensitive to ICM physics • AGN 8.0 works best of the radiative models in Planck cosmology 9

Le Brun et al. 2014 Optical properties Data: Sanderson13, Gonzalez13 and Data: Rasmussen09 and Lin04 Budzynski14 • Only AGN feedback can yield the high observed total mass-to-light ratios • REF is a factor of three to five too low and yields BCGs which are too dominant • All the AGN models yield similar stellar fractions in the BCG 10

Le Brun et al. Fitting of relations 2016a submitted (arXiv: 1606.04545) Fit evolving (broken) power- laws to the median Necessary to break scaling relation the power-law and and log-normal to make the low- scatter mass mass slope redshift- dependent as Blue : evolving leads to a decrease power-law in 𝞇 2 (e.g. for M gas - Green : evolving M, it decreases broken power-law from 0.322 to 0.056 Red : evolving in the case of the broken power-law AGN 8.0 simulation) with redshift- dependent low- mass mass slope 11

Le Brun et al. Evolution of K/T 2016a submitted (arXiv: 1606.04545) • K/T increases with redshift at fixed mass • AGN feedback notably increases kinetic motions in groups regime ➡ reversal of mass trend 12

Le Brun et al. Self-similar Evolution of mass slope 2016a submitted expectation for (arXiv: 1606.04545) the slope • Mass- temperature slightly shallower than self-similar (SS) for all models. • M gas -M 500 steeper than SS for all the radiative models . • Deviations from SS increase with increasing feedback intensity . 13

Le Brun et al. Self-similar Evolution of normalisation 2016a submitted expectation for (arXiv: 1606.04545) the evolution 14

Le Brun et al. Scatter 2016a submitted (arXiv: 1606.04545) All but one of the The X-ray hot gas proxies luminosity has a examined here significantly larger have a similar scatter at fixed scatter at fixed total mass (about total mass of three times about 10 per cent . higher ). 15

Le Brun et al. Scatter 2016a submitted (arXiv: 1606.04545) Due to the uncertain non- gravitational physics of galaxy formation. The unphysical non- radiative model (NOCOOL) was excluded from its computation. • X-ray temperature is the ‘best’ mass proxy among considered hot gas properties • X-ray luminosity is the poorest one. 16

Le Brun et al. Evolution of HSE bias 2016a submitted (arXiv: 1606.04545) 17

Le Brun et al. Evolution of HSE bias 2016a submitted (arXiv: 1606.04545) 18

Bartalucci et al. z=1 sample 2016a submitted 19

Bartalucci et al. Density profiles 2016a submitted 20

Bartalucci et al. Pressure profiles 2016a submitted 21

Bartalucci et al. Entropy profiles 2016a submitted 22

Evolution of cluster dark matter profiles as a test of Λ CDM • Goal: test Λ CDM using the evolution of the DM Dark Matter profiles of the most massive clusters in the Universe 100 Mpc/h • Compare XMM observations of Planck detected clusters with simulations ➡ Simulate 50-200 clusters with M 500 ≥ 5 x10 14 M ⦿ in several redshift bins up to redshift 1 with a high-spatial resolution (a few kpc) • In practice: (i) doing three large (1 Gpc/h on a side Gas with 2048 3 DM particles) DM only simulations and (ii) zooming at high resolution (a few kpc) on 50-200 20 Mpc/h galaxy clusters in each of the bins which will progressively include the relevant galaxy formation physics • All the simulations are done with the AMR code RAMSES (Teyssier 2002) on the OCCIGEN supercomputer at CINES in Montpellier using a large French computing time-allocation (>13 million CPU hours over 2015-2016; PI Le Brun). 23

Conclusions • Some AGN feedback models can produce a realistic population of galaxy groups and clusters, broadly reproducing both the median trend and, for the first time, the scatter 13 M ⊙ ≤ M 500 ≤ 10 15 in physical properties over approximately two decades in mass (10 M ⊙ ) and 1.5 decades in radius (0.05 ≤ r/r 500 ≤ 1.5). • The median relations and the scatter about them are reasonably well modelled by evolving broken power-laws with redshift dependent low-mass power-law indices . • The predictions of the self-similar model break down when efficient feedback is included , for both mass slope and evolution. But deviations from self-similarity do not necessarily mean effects of non-gravitational physics . • The log-normal scatter varies only mildly with mass and non-gravitational physics but displays a relatively strong redshift dependency (decreasing with increasing redshift). • X-ray temperature is the ‘ best ’ overall mass proxy while X-ray luminosity is the poorest . • The shape and scatter of the pressure and entropy profiles of a z=1 SZ-selected massive cluster sample is reasonably well reproduced by the simulations. 24