(Proto-)Clusters of Galaxies @z>1.5: an X-ray view Stefano Ettori - - PowerPoint PPT Presentation

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(Proto-)Clusters of Galaxies @z>1.5: an X-ray view Stefano Ettori - - PowerPoint PPT Presentation

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(Proto-)Clusters of Galaxies @z>1.5: an X-ray view Stefano Ettori INAF-OA / INFN Bologna XLSSC122 @z1.99 (Mantz+16) (Proto-)Clusters of Galaxies @z>1.5: an X-ray view Two issues are relevant to the X-rays: Detection of the ICM

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Stefano Ettori

INAF-OA / INFN Bologna

(Proto-)Clusters of Galaxies @z>1.5: an X-ray view

XLSSC122 @z1.99 (Mantz+16)

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(Proto-)Clusters of Galaxies @z>1.5: an X-ray view

Two issues are relevant to the X-rays:

  • Detection of the ICM
  • Characterization of its properties

Entropy profile Pure gravitation With AGN and supernova heating

Radius (kpc)

1000 100 10 100 1000

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Chandra view of high-z clusters

Santos+08, 10

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An example: RXJ1252, z=1.235

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An example: RXJ1252, z=1.235

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z=0.81 z=0.81 z=1.26 z=1.26

Gas density from the deprojected Sb~int(ε dl)

Mtot(< r)∝−r Tgas(r) d ln(ngas Tgas) d ln r Mgas(< r) = µmu n

∫

gas(r) dV

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Gas temperature profiles @z>1

Amodeo+16

  • n the c-M-z relation

z=0.83-1.24

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The entropy of ICM:

K = Pρ-5/3 ∝ T ne

  • 2/3 (keV cm2)
  • Entropy distribution in ICM determines the

clusterʼs equilibrium structure

high-K gas floats, low-K gas sinks; ICM convects until its isentropic surface coincide with equipotential surface

  • f DM potential
  • Entropy distribution retains information about

clusterʼs thermodynamic history

  • Heating and cooling change K more than T
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Evolution of the K profile

Ghirardini+ in prep

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Evolution of the K profile

Ghirardini+ in prep.

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(Proto-)Clusters of Galaxies @z>1.5: an X-ray view

  • For a given mass, scaling relations in the LCDM

predict that the clusters formed at larger redshift are hotter / denser and therefore more luminous in X- rays than their local z~0 counterparts.

  • This effect overturns the decrease in the observable X-

ray flux so that it does not decrease at z>1, similar to the SZ signal.

  • Provided that scaling relations remain valid at larger

redshifts, X-ray surveys will not miss massive clusters at any redshift, no matter how far they are.

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Evolution of the X-ray scaling laws

ü In the absence of non-gravitational physical processes, ICM evolves in the DM potential following the (pseudo-; see Diemer+12) evolution of the associated overdensity:

M / R3 ~ <ρ> ~ Δ ρcr(z) ~ Hz

2

Hz ~ (1+z)1.4 (@z>1.5)

ü From virial theorem/HEE: M / R ≈ T & hz M ∝ T3/2 ü Assuming brehmsstrahlung emission & ρDM ≈ ngas, L ≈ ∫ ngas

2 Λ(T) dV ≈ ngas 2 T1/2 R3 ∝ fgas 2 T2 ∝ fgas 2 M4/3

hz

  • 1 L ∝ (hz M)4/3

hz

  • 1 L ∝ T2
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Dashed (solid) line: expected (best-fit) relation

Evolution of the X-ray scaling laws

Reichert et al. 11

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Dashed (solid) line: expected (best-fit) relation

Evolution of the X-ray scaling laws

Reichert et al. 11

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  • No evolution, apart from self-similar expectations, is
  • bserved in M-T & Mgas-T & L-Y

The normalization in M – T/YX for nearby systems is lower (by ~20%) than the one predicted from simulations including cooling & galaxy feedback.

High-z preheating+cooling

  • Negative evolution in L-T:

i.e. a slight decrease in L for given T at higher z is observed (when cores are not excised; the entropy at 0.1 R200 is measured higher in systems at higher redshift)

  • eROSITA needs SLs to connect 105

(only 2% with T; ~100 @z>1.5) X-ray detected GCs to their mass ¡

SN/AGN feedback from SAM Gravitational heat only

Evolution of the X-ray scaling laws

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Cluster Surveys: eROSITA

(Merloni+12, Pillepich+12, Borm+14)

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The Athena Observatory

L2 orbit Ariane V Mass < 5100 kg Power 2500 W 5 year mission X-ray Integral Field Unit: ΔE: 2.5 eV Field of View: 5 arcmin Operating temp: 50 mk Wide Field Imager: ΔE: 125 eV Field of View: 40 arcmin High countrate capability Silicon Pore Optics: 2 m2 at 1 keV 5 arcsec HEW Focal length: 12 m Sensitivity: 3 10-17 erg cm-2 s-1

Rau et al. 2013 arXiv1307.1709 Barret et al., 2013 arXiv:1308.6784 Willingale et al, 2013 arXiv1308.6785

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100 ¡x ¡ASTRO-­‑H ¡

The first Deep Universe X-ray Observatory

Athena+ has vastly improved capabilities compared to current or planned facilities, and will provide transformational science on virtually all areas of astrophysics

Athena+ XIFU ASTRO-H SXS Chandra HETG XMM-Newton RGS

Effective area (cm2) 1 10 100 1000 10000 Energy (keV) 1 10

XMM-Newton EPIC PN Athena+ WFI

x ~15

Effective area (cm2) 1000 10000 Energy (keV) 1 10

XMM-pn eROSITA Athena+ Athena+ (goal) Chandra ACIS-I ROSAT PSPC NuSTAR Swift XRT Suzaku XIS Astro-H SXI Grasp (m2 deg2) 0.001 0.01 0.1 1 Half Energy Width (arcsec) 1 10 100

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Role of Athena

By 2030s, the cosmological parameters describing the evolution

  • f the Universe as a whole will likely be tightly constrained

(thanks to Euclid & eROSITA). Progress will have been made in understanding how structure formation works via the study of the galaxy distribution and evolution (Euclid, LSST). However, major astrophysical questions related to the formation and the evolution of galaxy clusters will still remain:

  • Interplay btw central BH / galaxy / gas
  • Processes driving metal & energy enrichment of the ICM
  • How & when first collapsed groups appear
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The formation and evolution of clusters and groups of galaxies

How and when was the energy contained in the hot intra-cluster medium generated?

How does ordinary matter assemble into the large-scale structures that we see today?

Ettori+15

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Pure gravitation With AGN and supernova heating Entropy profile

Radius (kpc)

1000 100 10 100 1000

The formation and evolution of clusters and groups of galaxies

How and when was the energy contained in the hot intra-cluster medium generated?

z=1

Entropy profile Pure gravitation With AGN and supernova heating

Radius (kpc)

1000 100 10 100 1000

z=2

Entropy

Athena+ Simulation

Pointecouteau, Reiprich et al., 2013 arXiv1306.2319

How does ordinary matter assemble into the large-scale structures that we see today?

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The most massive clusters at high-z

There are ~50 clusters with M>1015 M¤ in the observable Universe (using Tinker+08

mass function; Churazov+16)

Number of objects with M500/M¤ > 5e13 (solid;

>1e14 dashed): 1900 (WMAP9; 5000 using Planck13) are expected

at z>2.5 (full sky; 1 per 22

deg2; Reiprich+)

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The most massive clusters at high-z

Accretion history from Van den Bosch+14

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How does it appear a z~2.5

  • bject with M500~5e13 Msun?

Reiprich et al,

supporting paper to Athena’s WP

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How does it appear a z~2.5

  • bject with M500~5e13 Msun?

Reiprich et al,

supporting paper to Athena’s WP

For the planned multi-tiered survey (4*1 Ms +20*300ks +75*100ks +250*30ks ~78 deg2 over 5 years) ~50 (5) groups @z>2 (2.5)

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Properties of a object with M500~5e13 Msun

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Properties of a object with M500~5e13 Msun

@z=2.5, 1 Msec XIFU εT~10%

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Properties of a object with M500~5e13 Msun

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Properties of a object with M500~5e13 Msun

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(Proto-)Clusters of Galaxies @z>1.5: an X-ray view

  • For a given mass, scaling relations in the LCDM

predict that the clusters formed at larger redshift are hotter / denser and therefore more luminous in X- rays than their local z~0 counterparts.

  • Provided that scaling relations remain valid at larger

redshifts, X-ray surveys will not miss massive clusters at any redshift, no matter how far they are.

  • Athena will resolve ICM properties up to z~2, detecting

the first collapsed structure at z~2.5