a multi-wavelength view of rx j1347-1145 the interest of ... · overview of the talk introduction...

A multi-wavelength view of RX J1347-1145 &The interest of joint radio and mm cluster studies

Chiara Ferrari

in collaboration with:

H.T. Intema, E. Orrù, F. Govoni, M. Murgia, B. Mason, H. Bourdin, K.M. Asad, P. Mazzotta, M.W. Wise, T. Mroczkowski, J.H. Croston

Overview of the talk

Introduction

i. Diffuse intra-cluster radio sources

ii. Sunyaev-Zel’dovich effect and galaxy cluster studies

Multi-wavelength analysis of RX J1347-1145

i. Comparison of radio, X-ray & mm data

ii. Conclusions

Diffuse radio sources in galaxy clusters& electron acceleration

Halos: ICM turbulence due to cluster merging

Mini-halos: Cool core turbulence and gas sloshing

Relics: shocks due to cluster merging

X-ray images + radio contours

Halo Mini-halo Relics

Feretti+ 01 Gitti+ 07 van Weeren+ 09

CMB photons Inverse Compton effect

Thermal Sunyaev-Zel’dovich Effect

Carlstrom+ 02Bourdin+ 11

X-ray emission:thermal intracluster medium Thermal SZ effect

∆TSZE

TCMB= f(ν) y

y ∝�

neT dl

SZE: importance for cluster studies

Courtesy: M. Douspis & Planck collaboration

Carlstrom+ 02

∆TSZE

TCMB= f(ν) y

y ∝�

neT dl

Cluster detection

Cluster detection with X-ray and SZ observations

7

X-ray emissivity ∝�

n2eT

1/2dl

Fabian & Sanders 09

ICM density

∆TSZE

TCMB= f(ν) y

y ∝�

neT dl

Bagchi+ 11


Carlstrom+ 02

∆TSZE

TCMB= f(ν) y

y ∝�

neT dl

ICM shock detection

X-ray ImageSurface

brightness profile Density profile Temperature profile

Macario+ 11


Korngut+ 11

Carlstrom+ 02

∆TSZE

TCMB= f(ν) y

y ∝�

neT dl

ICM shock detection

Overview of the talk

Introduction

i. Diffuse intra-cluster radio sources

ii. Sunyaev-Zel’dovich effect and galaxy cluster studies


i. Comparison of radio, X-ray & mm data

ii. Conclusions

RX J1347-1145

XMMICM temperature map

X-ray contours

Gitti+ 04

ChandraRaw X-ray image

Allen+ 02

RX J1347-1145

Mason+ 10

MUSTANG90 GHz

res. 10’’

XMMICM temperature map

X-ray contours

Gitti+ 04

ChandraRaw X-ray image

Allen+ 02

Mason+ 10

MUSTANG SZE imageHST optical image

Surface mass density contours

Chandra X-ray imageMUSTANG SZE contours

Merging scenario

Previous radio results

Gitti, Ferrari+ 07

X-ray image (XMM)Radio contours (VLA @ 1.4 GHz)

New GMRT observations

100 kpc

13 47 2913 47 3013 47 3113 47 32

-11 45 30

-11 45 15

-11 45 00

-11 44 45

RIGHT ASCENSION (J2000)

DEC

LIN

ATIO

N (

J200

0)

Ferrari+ sub.

237 MHzres. 11.7’’× 9.3’’

rms = 2.7 mJy/b

614 MHzres. 4.8’’ × 3.5’’rms = 0.3 mJy/b

Mini-halo:S237 MHz = 131 ± 6 mJy

S614 MHz = 50 ± 2 mJy

SE excess:S614 MHz = 3.3 ± 0.3 mJy

Comparison with X-ray and mm data

0.01 0.02 0.03

Temperature map (XMM) 614 MHz contours (GMRT)

X-ray surface brightness contours (Chandra)

614 MHz map & contours (GMRT)SZE contours (MUSTANG - Mason+ 10)

8 9 10 11 12 13 14 15 16 17

Conclusions

Comparison of radio observations with SZE analyses for :

i. Cluster identification and mass

ii. Cluster physical properties


i. Discovery of the correspondence between intra-cluster radio emission and high-

pressure region detected through SZE

ii. Diffuse radio emission in this cluster ≡ “Mini-halo” + “Relic”

Conclusions

Comparison of radio observations with SZE analyses for :

i. Cluster identification and mass

ii. Cluster physical properties


i. Discovery of the correspondence between intra-cluster radio emission and high-

pressure region detected through SZE

ii. Diffuse radio emission in this cluster ≡ “Mini-halo” + “Relic”

Thanks !

a multi-wavelength view of rx j1347-1145 the interest of ... · overview of the talk introduction...

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