High-z clusters: prospectives with SKA and its precursors Chiara - - PowerPoint PPT Presentation

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High-z clusters: prospectives with SKA and its precursors Chiara - - PowerPoint PPT Presentation

Feb 03, 2023 239 likes •617 views

High-z clusters: prospectives with SKA and its precursors Chiara Ferrari (OCA, Lagrange) Image courtesy: www.skatelescope.org SKA1: 2018-2023 with cost-cap 650 M SKA1-LOW (AUS) SKA1-MID (SA) 130,000 dipoles 133 15m dishes +

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Image courtesy: www.skatelescope.org

High-z clusters: prospectives with SKA and its precursors

Chiara Ferrari

(OCA, Lagrange)

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SLIDE 2

SKA1: 2018-2023 with cost-cap 650 M€

SKA1-LOW (AUS)

  • 130,000 dipoles
  • Frequency coverage: 50 - 350 MHz
  • Max baseline: 80 km

SKA1-MID (SA)

  • 133 15m dishes + MeerKAT
  • Frequency coverage: 0.350 - 1.8 GHz & 4.6 - 13.8 GHz
  • Max baseline: 150 km
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SLIDE 3

The precursors

  • Location: Australia
  • Max baseline: 3 km
  • Frequency coverage: 80 - 300 MHz
  • Number of stations: 128
  • Antennas per station: 16
  • Fully operational since 2012

MWA

  • Location: South Africa
  • Max baseline: 8 km
  • Frequency coverage: 0.5 - 10 GHz
  • Number of antennas: 64
  • Diameter of antennas: 13.5 m
  • Fully operational from 2017

MeerKAT

  • Location: Australia
  • Max baseline: 6 km
  • Frequency coverage: 0.7 - 8 GHz
  • Number of antennas: 36
  • Diameter of antennas: 12 m
  • Fully operational from 2016

ASKAP

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SLIDE 4

Detection of high-z clusters FRI / FRII Diffuse radio emission ICM physics Feedback Non-thermal component Galaxy evolution

Importance of radio observations for high-z cluster studies

Castignani+ 14

20.0 18.0 16.0 14.0 12.0 9:47:10.0 08.0 06.0 04.0 40.0 35.0 30.0 25.0 20.0 15.0 10.0 05.0 76:23:00.0 55.0

50 kpc

Gitti+ 15 Miley+ 06

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SLIDE 5

Importance of radio observations for high-z cluster studies

Castignani+ 14

Detection of high-z clusters FRI / FRII Diffuse radio emission ICM physics Feedback Non-thermal component Galaxy evolution

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SLIDE 6

Detection of high-z clusters

  • FRI and FRII as beacons -

FRI: ~70% in clusters (from low to high-z) FRII: ~20-25% in intermediate/ rich groups (low-z) ~20-50% (high-z)

e.g. Zirbel 97; Galametz+12 e.g. Zirbel 97; Castignani+14

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SLIDE 7

Detection of high-z clusters

  • FRI and FRII as beacons -

FRI: ~70% in clusters (from low to high-z) FRII: ~20-25% in intermediate/ rich groups (low-z) ~20-50% (high-z)

NVSS J111921−363139: z=2.769

−10 −5 5 10 Arcminutes −10 −5 5 10 Arcminutes

MP J1758−6738: z=2.026

−10 −5 5 10 Arcminutes −10 −5 5 10 Arcminutes

Rigby+ 14 e.g. Zirbel 97; Galametz+12 e.g. Zirbel 97; Castignani+14

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SLIDE 8

Detection of high-z clusters

  • FRI and FRII as beacons -

FRI: ~70% in clusters (from low to high-z) FRII: ~20-25% in intermediate/ rich groups (low-z) ~20-50% (high-z)

NVSS J111921−363139: z=2.769

−10 −5 5 10 Arcminutes −10 −5 5 10 Arcminutes

MP J1758−6738: z=2.026

−10 −5 5 10 Arcminutes −10 −5 5 10 Arcminutes

Rigby+ 14 e.g. Zirbel 97; Galametz+12 e.g. Zirbel 97; Castignani+14 Castignani+ 14 z~0.9-2.9

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Summary plot for radio surveys

Prandoni & Seymour 15

Bulk of AGN population down to L~1022 W/Hz, z~0.5 (Wide), z~2 (Deep), z~4 (Ultra Deep) 0.5'' resolution at ~1 GHz

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Summary plot for radio surveys

Prandoni & Seymour 15 Pre-2010 Pre-SKA SKA

Bulk of AGN population down to L~1022 W/Hz, z~0.5 (Wide), z~2 (Deep), z~4 (Ultra Deep) 0.5'' resolution at ~1 GHz

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SLIDE 11

SKA survey speed

SKA1 Science Requirements Braun+ (SKAO)

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Polarisation studies

RM ∝

  • ne

B · d l χ = χ0 + RM × λ2

Coma-like cluster

200 400 600 800 1000 1200 distance [kpc] 100 200 300 400 |RM| rad/m

2

SKA1-SUR VLA observations

Figure 1: SKA1-SUR predictions for the RM for Coma-lik

Bonafede+ 15

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SLIDE 13

Polarisation studies

Broderick+ 07

RM ∝

  • ne

B · d l χ = χ0 + RM × λ2

Coma-like cluster

200 400 600 800 1000 1200 distance [kpc] 100 200 300 400 |RM| rad/m

2

SKA1-SUR VLA observations

Figure 1: SKA1-SUR predictions for the RM for Coma-lik

Bonafede+ 15

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SLIDE 14

Polarisation studies

Broderick+ 07 Taylor+ 01

RM ∝

  • ne

B · d l

Fabian & Sanders 09

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SLIDE 15

Diffuse radio emission in clusters

The Coma cluster observed at 352 MHz with WSRT Brown & Rudnick 11 Correlation between X-ray and radio cluster luminosities Cassano+ 13

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SLIDE 16

Detection of clusters through their diffuse radio emission

Macario+ 14 de Gasperin+ 16

MACSJ0520.7-1328 1WGA J0521.0-1333

1 Mpc

Companion of MACS J0520.7-1328 (z=0.3)

X-ray images Radio contours

Companion of A3527 (z=0.2)

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Detection of diffuse radio emission at high-z : a challenging task

Pizzo & de Bruyn 09

Radio image at 25 cm of A2255

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Radio galaxies + Radio halo (P1.4 GHz ~ 1 × 1024 W/Hz) @ z ≥ 0.5

Cassano+ 13 Feretti+ 12

Diffuse radio emission from galaxy clusters with SKA1

Relativistic electron population + Magnetic field model Faraday tool (Murgia+ 04)

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Radio galaxies + Radio halo (P1.4 GHz ~ 1 × 1024 W/Hz) @ z ≥ 0.5 Relativistic electron population + Magnetic field model Faraday tool (Murgia+ 04) Simulations of SKA1 MID & SUR

  • bservations

MeqTrees tool (Noordam & Smirnov 10) 8 hours observations 60 sec integration time 50 MHz BW starting @ 1415 MHz

Diffuse radio emission from galaxy clusters with SKA1

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Radio maps before deconvolution from the instrument PSF 1 arcsec resolution SKA1 MID (Zoom in)

Simulated SKA1-MID observations

Ferrari+ 15

MORESANE algorithm : new deconvolution method based on sparse representations developed @ OCA, Nice (FR)

Dabbech+ 12; Dabbech+ 15

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Up to which z can we detect this cluster with SKA1 MID?

16

Simulated cluster MORESANE source model MORESANE residuals MS-CLEAN residuals MS-CLEAN source model

z=0.5 Res ~ 1” z=1.0 Res ~ 1”

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Primary cosmic rays protons (CRPs) & electrons (CREs)

Intra-cluster primary cosmic rays

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Primary cosmic rays protons (CRPs) & electrons (CREs) External processes

CRs acceleration driven by the assembly of clusters

  • accretion shocks (M ~ 103)
  • merging shocks (M ~ 3-10)
  • ICM turbulence

Courtesy: Vazza

Intra-cluster primary cosmic rays

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Primary cosmic rays protons (CRPs) & electrons (CREs) Internal processes

CRs accelerated inside cluster galaxies and then injected

  • SNae driven galactic winds
  • AGNs

Shull 09 Courtesy: Koekemoer

External processes

CRs acceleration driven by the assembly of clusters

  • accretion shocks (M ~ 103)
  • merging shocks (M ~ 3-10)
  • ICM turbulence

Courtesy: Vazza

Intra-cluster primary cosmic rays

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SLIDE 25

Not only non-thermal emission with SKA

Simulated 1h observation with SKA1-MID (Band 5) SZ signal from a cluster with M200 = 4x1014MSun at z=1.83

Grainge+ 15

SKA1 Baseline Designe

SKAO

‐ ‐ ‐ ‐ ‐

‐

‐ ‐

‐ ‐ ‐ ‐ ‐ ‐ ‐ ‐ ‐ ‐ ‐

5 10 15 20 25 30 35 40 45 50 100 1000 10000

log Tb (K) log (f) MHz Sky Noise: 350 MHz to 25 GHz & SKA1‐mid Receiver Bands

SKA1‐mid Band 1 Band 2 Band 3 Band 4 Band 5+

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Importance of radio observations for high-z cluster studies

20.0 18.0 16.0 14.0 12.0 9:47:10.0 08.0 06.0 04.0 40.0 35.0 30.0 25.0 20.0 15.0 10.0 05.0 76:23:00.0 55.0

50 kpc

Gitti+ 15

Detection of high-z clusters FRI / FRII Diffuse radio emission ICM physics Feedback Non-thermal component Galaxy evolution

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SLIDE 27

Radio feedback in cool-core clusters

McNamara+ 09 FRI radio galaxies in ≿70% of cD galaxies of cool-core clusters Bubbles of relativistic plasma excavating cavities in the ICM distribution

Radio X-rays

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SLIDE 28

Santos+ 12

Radio feedback in cool-core clusters at high-z

Santos+ 10 WARPJ1415.1+3612 at z =1 Chandra image + VLA contours Residual Chandra image VLA image NVSS limit @ z=1

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SLIDE 29

Santos+ 12

Radio feedback in cool-core clusters at high-z

Santos+ 10 Gitti+ 15 WARPJ1415.1+3612 at z =1 Chandra image + VLA contours Residual Chandra image VLA image

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the galaxy cluster radio “zoo”

Feretti+ 01

Several Mpc Few hundreds kpc Several tens kpc

Scale

Ferrari+ 11

Mini-halo

de Gasperin+ 12

M87 Radio halo

20 kpc Feretti+ 01

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A global view of non-thermal emission and feedback activity

20.0 18.0 16.0 14.0 12.0 9:47:10.0 08.0 06.0 04.0 40.0 35.0 30.0 25.0 20.0 15.0 10.0 05.0 76:23:00.0 55.0

50 kpc

Gitti+ 15

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Importance of radio observations for high-z cluster studies

Miley+ 06

Detection of high-z clusters FRI / FRII Diffuse radio emission ICM physics Feedback Non-thermal component Galaxy evolution

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Nuclear and star-formation activity in high-z cluster galaxies

b

Wang+ 16

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Nuclear and star-formation activity in high-z cluster galaxies

b

Wang+ 16 Murphy+ 15

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Nuclear and star-formation activity in high-z cluster galaxies

b

Wang+ 16 Murphy+ 15 Murphy+ 15 z=2 for νobs=10 GHz

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Detection of high-z clusters FRI / FRII Diffuse radio emission ICM physics Feedback Non-thermal component Galaxy evolution

The SKA will be an important instrument for the identification and physical characterisation of high-z clusters Thanks!