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Planck Intermediate Results. X. Physics of the hot gas in the Coma cluster | | Planck Collaboration
; P. A. R. Ade
; N. Aghanim
; M. Arnaud
; M. Ashdown
; F. Atrio-Barandela
; J. Aumont
; C. Baccigalupi
; A. Balbi
; A. J. Banday
; R. B. Barreiro
; J. G. Bartlett
; E. Battaner
; K. Benabed
; A. Benoît
; J.-P. Bernard
; M. Bersanelli
; A. Bonaldi
; J. R. Bond
; J. Borrill
; F. R. Bouchet
; H. Bourdin
; M. L. Brown
; C. Burigana
; P. Cabella
; J.-F. Cardoso
; P. Carvalho
; A. Catalano
; L. Cayón
; L.-Y Chiang
; G. Chon
; P. R. Christensen
; E. Churazov
; D. L. Clements
; S. Colafrancesco
; L. P. L. Colombo
; A. Coulais
; B. P. Crill
; F. Cuttaia
; A. Da Silva
; H. Dahle
; L. Danese
; R. J. Davis
; P. de Bernardis
; G. de Gasperis
; A. de Rosa
; G. de Zotti
; J. Delabrouille
; F.-X. Désert
; C. Dickinson
; J. M. Diego
; K. Dolag
; H. Dole
; S. Donzelli
; O. Doré
; U. Dörl
; M. Douspis
; X. Dupac
; T. A. Enßlin
; H. K. Eriksen
; F. Finelli
; I. Flores-Cacho
; O. Forni
; M. Frailis
; E. Franceschi
; M. Frommert
; S. Galeotta
; K. Ganga
; R. T. Génova-Santos
; M. Giard
; M. Gilfanov
; J. González-Nuevo
; K. M. Górski
; A. Gregorio
; A. Gruppuso
; F. K. Hansen
; D. Harrison
; S. Henrot-Versillé
; C. Hernández-Monteagudo
; S. R. Hildebrandt
; E. Hivon
; M. Hobson
; W. A. Holmes
; A. Hornstrup
; W. Hovest
; K. M. Huffenberger
; G. Hurier
; T. R. Jaffe
; T. Jagemann
; W. C. Jones
; M. Juvela
; E. Keihänen
; R. Kneissl
; J. Knoche
; L. Knox
; M. Kunz
; H. Kurki-Suonio
; G. Lagache
; A. Lähteenmäki
; A. Lasenby
; C. R. Lawrence
; M. Le Jeune
; R. Leonardi
; P. B. Lilje
; M. Linden-Vørnle
; M. López-Caniego
; P. M. Lubin
; J. F. Macías-Pérez
; B. Maffei
; D. Maino
; N. Mandolesi
; M. Maris
; F. Marleau
; E. Martínez-González
; S. Masi
; M. Massardi
; S. Matarrese
; F. Matthai
; P. Mazzotta
; S. Mei
; A. Melchiorri
; J.-B. Melin
; L. Mendes
; A. Mennella
; S. Mitra
; M.-A. Miville-Deschênes
; A. Moneti
; L. Montier
; G. Morgante
; D. Munshi
; J. A. Murphy
; P. Naselsky
; P. Natoli
; H. U. Nørgaard-Nielsen
; F. Noviello
; S. Osborne
; F. Pajot
; D. Paoletti
; O. Perdereau
; F. Perrotta
; F. Piacentini
; M. Piat
; E. Pierpaoli
; R. Piffaretti
; S. Plaszczynski
; E. Pointecouteau
; G. Polenta
; N. Ponthieu
; L. Popa
; T. Poutanen
; G. W. Pratt
; S. Prunet
; J.-L. Puget
; J. P. Rachen
; R. Rebolo
; M. Reinecke
; M. Remazeilles
; C. Renault
; S. Ricciardi
; T. Riller
; G. Rocha
; M. Roman
; C. Rosset
; M. Rossetti
; J. A. Rubiño-Martín
; B. Rusholme
; M. Sandri
; G. Savini
; B. M. Schaefer
; D. Scott
; G. F. Smoot
; F. Stivoli
; R. Sudiwala
; R. Sunyaev
; D. Sutton
; A.-S. Suur-Uski
; J.-F. Sygnet
; J. A. Tauber
; L. Terenzi
; L. Toffolatti
; M. Tomasi
; M. Tristram
; J. Tuovinen
; M. Türler
; G. Umana
; L. Valenziano
; B. Van Tent
; J. Varis
; P. Vielva
; F. Villa
; N. Vittorio
; L. A. Wade
; B. D. Wandelt
; N. Welikala
; S. D. M. White
; D. Yvon
; A. Zacchei
; S. Zaroubi
; A. Zonca
; | | Date: |
17 Aug 2012 | | Abstract: | We present an analysis of Planck satellite data on the Coma Cluster observed
via the Sunyaev-Zeldovich effect. Planck is able, for the first time, to detect
SZ emission up to r ~ 3 X R_500. We test previously proposed models for the
pressure distribution in clusters against the azimuthally averaged data. We
find that the Arnaud et al. universal pressure profile does not fit Coma, and
that their pressure profile for merging systems provides a good fit of the data
only at r<R_500: by r=2XR_500 it underestimates the observed y profile by a
factor of ~2. This may indicate that at these larger radii either i) the
cluster SZ emission is contaminated by unresolved SZ sources along the line of
sight or ii) the pressure profile of Coma is higher at r>R_500 than the mean
pressure profile predicted by the simulations. The Planck image shows
significant local steepening of the y profile in two regions about half a
degree to the west and to the south-east of the cluster centre. These features
are consistent with the presence of shock fronts at these radii, and indeed the
western feature was previously noticed in the ROSAT PSPC mosaic by Markevitch
(2000) as well as in the radio. Using Planck y profiles extracted from
corresponding sectors we find pressure jumps of 4.5+2.5-0.1 and 4.9+0.7-0.2 in
the west and southeast, respectively. Assuming Rankine-Hugoniot pressure jump
conditions, we deduce that the shock waves should propagate with Mach number
M_w=1.95+0.45-0.02 and M_se=2.03+0.14-0.04 in the West and Southeast,
respectively. Finally, we find that the y and radio-synchrotron signals are
quasi-linearly correlated on Mpc scales with small intrinsic scatter. This
implies either that the energy density of cosmic-ray electrons is relatively
constant throughout the cluster, or that the magnetic fields fall off much more
slowly with radius than previously thought. | | Source: | arXiv, 1208.3611 | | Services: | Forum | Review | PDF | Favorites | |
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