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

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High-redshift Cluster Workshop, Paris, October 05th-07th 2016

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),…

Evolution of groups and clusters since z=1.5 in cosmological simulations

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).
• More than 14,000 groups and clusters with M500>10

13 M⊙ at z=0 in Planck

cosmology.

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X-ray observations

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Le Brun et al. 2014

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

X-ray observations

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Le Brun et al. 2014

Data: REXCESS, Vikhlinin06, Lin12, Maughan08 and Sun09

• 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 fgas but relation is flatter than observed.

Here, low fgas are achieved by overly efficient SF.

Entropy profiles

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Le Brun et al. 2014

• 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. Data: Sun09, Johnson09 Data: Pratt10, Vikhlinin06

Demographics of cluster cores

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Le Brun et al. 2014

• AGN 8.0 has a distribution which is remarkably similar to the observed
• ne.
• No strong evidence of bi-modality in both simulations and observations

but does not necessarily imply that entropy is not bi-modal.

Data: Croston08

An aside: Non-universal pressure profile

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• 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)

• ver the whole radial and halo

mass range when AGN feedback is included

Le Brun et al. 2015

Sunyaev-Zel’dovich properties

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Le Brun et al. 2014

Data: Vikhlinin06, Planck Intermediate Results IV, Sun09

YX 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 Tvir by HSE

Sunyaev-Zel’dovich properties

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Le Brun et al. 2014

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

Optical properties

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Le Brun et al. 2014

• 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

Data: Sanderson13, Gonzalez13 and Budzynski14 Data: Rasmussen09 and Lin04

Fitting of relations

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Le Brun et al. 2016a submitted (arXiv: 1606.04545)

Fit evolving (broken) power- laws to the median scaling relation and log-normal scatter Blue: evolving power-law Green: evolving broken power-law Red: evolving broken power-law with redshift- dependent low- mass mass slope Necessary to break the power-law and to make the low- mass mass slope redshift- dependent as leads to a decrease in 𝞇2 (e.g. for Mgas- M, it decreases from 0.322 to 0.056 in the case of the AGN 8.0 simulation)

Evolution of K/T

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• K/T increases with redshift at fixed mass
• AGN feedback notably increases kinetic motions in groups regime

➡ reversal of mass trend

Le Brun et al. 2016a submitted (arXiv: 1606.04545)

Evolution of mass slope

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• Mass-

temperature slightly shallower than self-similar (SS) for all models.

• Mgas-M500

steeper than SS for all the radiative models.

• Deviations from

SS increase with increasing feedback intensity.

Self-similar expectation for the slope

Le Brun et al. 2016a submitted (arXiv: 1606.04545)

Evolution of normalisation

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Self-similar expectation for the evolution

Le Brun et al. 2016a submitted (arXiv: 1606.04545)

Scatter

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All but one of the hot gas proxies examined here have a similar scatter at fixed total mass of about 10 per cent. The X-ray luminosity has a significantly larger scatter at fixed total mass (about three times higher).

Le Brun et al. 2016a submitted (arXiv: 1606.04545)

Scatter

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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.

Le Brun et al. 2016a submitted (arXiv: 1606.04545)

Evolution of HSE bias

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Le Brun et al. 2016a submitted (arXiv: 1606.04545)

Evolution of HSE bias

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Le Brun et al. 2016a submitted (arXiv: 1606.04545)

z=1 sample

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Bartalucci et al. 2016a submitted

Density profiles

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Bartalucci et al. 2016a submitted

Pressure profiles

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Bartalucci et al. 2016a submitted

Entropy profiles

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Bartalucci et al. 2016a submitted

Evolution of cluster dark matter profiles as a test of ΛCDM

• Goal: test ΛCDM using the evolution of the DM

profiles of the most massive clusters in the Universe

• Compare XMM observations of Planck detected

clusters with simulations

➡ Simulate 50-200 clusters with M500≥ 5 x1014 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

with 20483 DM particles) DM only simulations and (ii) zooming at high resolution (a few kpc) on 50-200 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).

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Dark Matter Gas 20 Mpc/h 100 Mpc/h

Conclusions

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• 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 in physical properties over approximately two decades in mass (10

13 M⊙ ≤ M500 ≤ 10 15

M⊙) and 1.5 decades in radius (0.05 ≤ r/r500 ≤ 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.