Planck intermediate results: X. Physics of the hot gas in the Coma cluster

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; I. Bikmaev; H. Böhringer; A. Bonaldi; J. R. Bond; J. Borrill; F. R. Bouchet; H. Bourdin; M. L. Brown; S. D. Brown; R. Burenin; 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; J. Démoclès; 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; I. Khamitov; R. Kneissl; J. Knoche; L. Knox; M. Kunz; H. Kurki-Suonio; G. Lagache; A. Lähteenmäki; J. M. Lamarre; 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; D. Novikov; I. Novikov; 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; I. Ristorcelli; G. Rocha; M. Romen; C. Rosset; M. Rossetti; J. A. Rubiño-Martín; L. Rudnick; 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

doi:10.1051/0004-6361/201220247

Planck intermediate results: X. Physics of the hot gas in the Coma cluster

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, I. Bikmaev, H. Böhringer, A. Bonaldi, J. R. BondJ. Borrill, F. R. Bouchet, H. Bourdin, M. L. Brown, S. D. Brown, R. Burenin, 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, J. Démoclès, 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, I. Khamitov, R. Kneissl, J. Knoche, L. Knox, M. Kunz, H. Kurki-Suonio, G. Lagache, A. Lähteenmäki, J. M. Lamarre, 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, D. Novikov, I. Novikov, 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, I. Ristorcelli, G. Rocha, M. Romen, C. Rosset, M. Rossetti, J. A. Rubiño-Martín, L. Rudnick, 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

Physics

Research output: Contribution to journal › Article › peer-review

44 Scopus citations

Abstract

We present an analysis of Planck satellite data on the Coma cluster observed via the Sunyaev-Zeldovich effect. Thanks to its great sensitivity, Planck is able, for the first time, to detect SZ emission up to r ≈ 3 × R₅₀₀. We test previously proposed spherically symmetric models for the pressure distribution in clusters against the azimuthally averaged data. In particular, we find that the Arnaud et al. (2010, A&A, 517, A92) "universal" pressure profile does not fit Coma, and that their pressure profile for merging systems provides a reasonable fit to the data only at r < R₅₀₀; by r = 2 × R₅₀₀ it underestimates the observed y profile by a factor of â‰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 > R₅₀₀ than the mean pressure profile predicted by the simulations used to constrain the models. 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 as well as in the radio. Using Plancky profiles extracted from corresponding sectors we find pressure jumps of 4.9_-0.2^+0.4 and 5.0_-0.1 ^+1.3 in the west and south-east, respectively. Assuming Rankine-Hugoniot pressure jump conditions, we deduce that the shock waves should propagate with Mach number M_w = 2.03_-0.04^+0.09 and M_se = 2.05_-0.02^+0.25 in the west and south-east, 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.

Original language	English (US)
Article number	A140
Journal	Astronomy and Astrophysics
Volume	554
DOIs	https://doi.org/10.1051/0004-6361/201220247
State	Published - 2013

All Science Journal Classification (ASJC) codes

Astronomy and Astrophysics
Space and Planetary Science

Keywords

Cosmic background radiation
Cosmology: observations
Galaxies: clusters: general
Galaxies: clusters: individual: Coma cluster
Galaxies: clusters: intracluster medium
X-rays: galaxies: clusters

Access to Document

10.1051/0004-6361/201220247

Cite this

Ade, P. A. R., Aghanim, N., Arnaud, M., Ashdown, M., Atrio-Barandela, F., Aumont, J., Baccigalupi, C., Balbi, A., Banday, A. J., Barreiro, R. B., Bartlett, J. G., Battaner, E., Benabed, K., Benoît, A., Bernard, J. P., Bersanelli, M., Bikmaev, I., Böhringer, H., Bonaldi, A., ... Zonca, A. (2013). Planck intermediate results: X. Physics of the hot gas in the Coma cluster. Astronomy and Astrophysics, 554, [A140]. https://doi.org/10.1051/0004-6361/201220247

@article{7ced539b8f5d41c48476fcd992a87e48,

title = "Planck intermediate results: X. Physics of the hot gas in the Coma cluster",

abstract = "We present an analysis of Planck satellite data on the Coma cluster observed via the Sunyaev-Zeldovich effect. Thanks to its great sensitivity, Planck is able, for the first time, to detect SZ emission up to r ≈ 3 × R500. We test previously proposed spherically symmetric models for the pressure distribution in clusters against the azimuthally averaged data. In particular, we find that the Arnaud et al. (2010, A&A, 517, A92) {"}universal{"} pressure profile does not fit Coma, and that their pressure profile for merging systems provides a reasonable fit to the data only at r < R500; by r = 2 × R500 it underestimates the observed y profile by a factor of {\^a}‰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 > R500 than the mean pressure profile predicted by the simulations used to constrain the models. 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 as well as in the radio. Using Plancky profiles extracted from corresponding sectors we find pressure jumps of 4.9-0.2+0.4 and 5.0-0.1 +1.3 in the west and south-east, respectively. Assuming Rankine-Hugoniot pressure jump conditions, we deduce that the shock waves should propagate with Mach number Mw = 2.03-0.04+0.09 and Mse = 2.05-0.02+0.25 in the west and south-east, 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.",

keywords = "Cosmic background radiation, Cosmology: observations, Galaxies: clusters: general, Galaxies: clusters: individual: Coma cluster, Galaxies: clusters: intracluster medium, X-rays: galaxies: clusters",

author = "Ade, {P. A.R.} and N. Aghanim and M. Arnaud and M. Ashdown and F. Atrio-Barandela and J. Aumont and C. Baccigalupi and A. Balbi and Banday, {A. J.} and Barreiro, {R. B.} and Bartlett, {J. G.} and E. Battaner and K. Benabed and A. Beno{\^i}t and Bernard, {J. P.} and M. Bersanelli and I. Bikmaev and H. B{\"o}hringer and A. Bonaldi and Bond, {J. R.} and J. Borrill and Bouchet, {F. R.} and H. Bourdin and Brown, {M. L.} and Brown, {S. D.} and R. Burenin and C. Burigana and P. Cabella and Cardoso, {J. F.} and P. Carvalho and A. Catalano and L. Cay{\'o}n and Chiang, {L. Y.} and G. Chon and Christensen, {P. R.} and E. Churazov and Clements, {D. L.} and S. Colafrancesco and Colombo, {L. P.L.} and A. Coulais and Crill, {B. P.} and F. Cuttaia and {Da Silva}, A. and H. Dahle and L. Danese and Davis, {R. J.} and {De Bernardis}, P. and {De Gasperis}, G. and {De Rosa}, A. and {De Zotti}, G. and J. Delabrouille and J. D{\'e}mocl{\`e}s and D{\'e}sert, {F. X.} and C. Dickinson and Diego, {J. M.} and K. Dolag and H. Dole and S. Donzelli and O. Dor{\'e} and U. D{\"o}rl and M. Douspis and X. Dupac and En{\ss}lin, {T. A.} and Eriksen, {H. K.} and F. Finelli and I. Flores-Cacho and O. Forni and M. Frailis and E. Franceschi and M. Frommert and S. Galeotta and K. Ganga and G{\'e}nova-Santos, {R. T.} and M. Giard and M. Gilfanov and J. Gonz{\'a}lez-Nuevo and G{\'o}rski, {K. M.} and A. Gregorio and A. Gruppuso and Hansen, {F. K.} and D. Harrison and S. Henrot-Versill{\'e} and C. Hern{\'a}ndez-Monteagudo and Hildebrandt, {S. R.} and E. Hivon and M. Hobson and Holmes, {W. A.} and A. Hornstrup and W. Hovest and Huffenberger, {K. M.} and G. Hurier and Jaffe, {T. R.} and T. Jagemann and Jones, {W. C.} and M. Juvela and E. Keih{\"a}nen and I. Khamitov and R. Kneissl and J. Knoche and L. Knox and M. Kunz and H. Kurki-Suonio and G. Lagache and A. L{\"a}hteenm{\"a}ki and Lamarre, {J. M.} and A. Lasenby and Lawrence, {C. R.} and {Le Jeune}, M. and R. Leonardi and Lilje, {P. B.} and M. Linden-V{\o}rnle and M. L{\'o}pez-Caniego and Lubin, {P. M.} and Mac{\'i}as-P{\'e}rez, {J. F.} and B. Maffei and D. Maino and N. Mandolesi and M. Maris and F. Marleau and E. Mart{\'i}nez-Gonz{\'a}lez and S. Masi and M. Massardi and S. Matarrese and F. Matthai and P. Mazzotta and S. Mei and A. Melchiorri and Melin, {J. B.} and L. Mendes and A. Mennella and S. Mitra and Miville-Desch{\^e}nes, {M. A.} and A. Moneti and L. Montier and G. Morgante and D. Munshi and Murphy, {J. A.} and P. Naselsky and P. Natoli and N{\o}rgaard-Nielsen, {H. U.} and F. Noviello and D. Novikov and I. Novikov and S. Osborne and F. Pajot and D. Paoletti and O. Perdereau and F. Perrotta and F. Piacentini and M. Piat and E. Pierpaoli and R. Piffaretti and S. Plaszczynski and E. Pointecouteau and G. Polenta and N. Ponthieu and L. Popa and T. Poutanen and Pratt, {G. W.} and S. Prunet and Puget, {J. L.} and Rachen, {J. P.} and R. Rebolo and M. Reinecke and M. Remazeilles and C. Renault and S. Ricciardi and T. Riller and I. Ristorcelli and G. Rocha and M. Romen and C. Rosset and M. Rossetti and Rubi{\~n}o-Mart{\'i}n, {J. A.} and L. Rudnick and B. Rusholme and M. Sandri and G. Savini and Schaefer, {B. M.} and D. Scott and Smoot, {G. F.} and F. Stivoli and R. Sudiwala and R. Sunyaev and D. Sutton and Suur-Uski, {A. S.} and Sygnet, {J. F.} and Tauber, {J. A.} and L. Terenzi and L. Toffolatti and M. Tomasi and M. Tristram and J. Tuovinen and M. T{\"u}rler and G. Umana and L. Valenziano and {Van Tent}, B. and J. Varis and P. Vielva and F. Villa and N. Vittorio and Wade, {L. A.} and Wandelt, {B. D.} and N. Welikala and White, {S. D.M.} and D. Yvon and A. Zacchei and S. Zaroubi and A. Zonca",

note = "Funding Information: A description of the Planck Collaboration and a list of its members, indicating which technical or scientific activities they have been involved in, can be found at http://www.rssd.esa.int/Planck_Collaboration . The Planck Collaboration acknowledges the support of: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MICINN and JA (Spain); Tekes, AoF and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); and DEISA (EU). Partial support for this work for L. Rudnick comes from U.S. NSF Grant 09-08668 to the University of Minnesota. We would also like to acknowledge useful conversations with G. Brunetti.",

year = "2013",

doi = "10.1051/0004-6361/201220247",

language = "English (US)",

volume = "554",

journal = "Astronomy and Astrophysics",

issn = "0004-6361",

publisher = "EDP Sciences",

}

Ade, PAR, Aghanim, N, Arnaud, M, Ashdown, M, Atrio-Barandela, F, Aumont, J, Baccigalupi, C, Balbi, A, Banday, AJ, Barreiro, RB, Bartlett, JG, Battaner, E, Benabed, K, Benoît, A, Bernard, JP, Bersanelli, M, Bikmaev, I, Böhringer, H, Bonaldi, A, Bond, JR, Borrill, J, Bouchet, FR, Bourdin, H, Brown, ML, Brown, SD, Burenin, R, Burigana, C, Cabella, P, Cardoso, JF, Carvalho, P, Catalano, A, Cayón, L, Chiang, LY, Chon, G, Christensen, PR, Churazov, E, Clements, DL, Colafrancesco, S, Colombo, LPL, Coulais, A, Crill, BP, Cuttaia, F, Da Silva, A, Dahle, H, Danese, L, Davis, RJ, De Bernardis, P, De Gasperis, G, De Rosa, A, De Zotti, G, Delabrouille, J, Démoclès, J, Désert, FX, Dickinson, C, Diego, JM, Dolag, K, Dole, H, Donzelli, S, Doré, O, Dörl, U, Douspis, M, Dupac, X, Enßlin, TA, Eriksen, HK, Finelli, F, Flores-Cacho, I, Forni, O, Frailis, M, Franceschi, E, Frommert, M, Galeotta, S, Ganga, K, Génova-Santos, RT, Giard, M, Gilfanov, M, González-Nuevo, J, Górski, KM, Gregorio, A, Gruppuso, A, Hansen, FK, Harrison, D, Henrot-Versillé, S, Hernández-Monteagudo, C, Hildebrandt, SR, Hivon, E, Hobson, M, Holmes, WA, Hornstrup, A, Hovest, W, Huffenberger, KM, Hurier, G, Jaffe, TR, Jagemann, T, Jones, WC, Juvela, M, Keihänen, E, Khamitov, I, Kneissl, R, Knoche, J, Knox, L, Kunz, M, Kurki-Suonio, H, Lagache, G, Lähteenmäki, A, Lamarre, JM, Lasenby, A, Lawrence, CR, Le Jeune, M, Leonardi, R, Lilje, PB, Linden-Vørnle, M, López-Caniego, M, Lubin, PM, Macías-Pérez, JF, Maffei, B, Maino, D, Mandolesi, N, Maris, M, Marleau, F, Martínez-González, E, Masi, S, Massardi, M, Matarrese, S, Matthai, F, Mazzotta, P, Mei, S, Melchiorri, A, Melin, JB, Mendes, L, Mennella, A, Mitra, S, Miville-Deschênes, MA, Moneti, A, Montier, L, Morgante, G, Munshi, D, Murphy, JA, Naselsky, P, Natoli, P, Nørgaard-Nielsen, HU, Noviello, F, Novikov, D, Novikov, I, Osborne, S, Pajot, F, Paoletti, D, Perdereau, O, Perrotta, F, Piacentini, F, Piat, M, Pierpaoli, E, Piffaretti, R, Plaszczynski, S, Pointecouteau, E, Polenta, G, Ponthieu, N, Popa, L, Poutanen, T, Pratt, GW, Prunet, S, Puget, JL, Rachen, JP, Rebolo, R, Reinecke, M, Remazeilles, M, Renault, C, Ricciardi, S, Riller, T, Ristorcelli, I, Rocha, G, Romen, M, Rosset, C, Rossetti, M, Rubiño-Martín, JA, Rudnick, L, Rusholme, B, Sandri, M, Savini, G, Schaefer, BM, Scott, D, Smoot, GF, Stivoli, F, Sudiwala, R, Sunyaev, R, Sutton, D, Suur-Uski, AS, Sygnet, JF, Tauber, JA, Terenzi, L, Toffolatti, L, Tomasi, M, Tristram, M, Tuovinen, J, Türler, M, Umana, G, Valenziano, L, Van Tent, B, Varis, J, Vielva, P, Villa, F, Vittorio, N, Wade, LA, Wandelt, BD, Welikala, N, White, SDM, Yvon, D, Zacchei, A, Zaroubi, S & Zonca, A 2013, 'Planck intermediate results: X. Physics of the hot gas in the Coma cluster', Astronomy and Astrophysics, vol. 554, A140. https://doi.org/10.1051/0004-6361/201220247

TY - JOUR

T1 - Planck intermediate results

T2 - X. Physics of the hot gas in the Coma cluster

AU - Ade, P. A.R.

AU - Aghanim, N.

AU - Arnaud, M.

AU - Ashdown, M.

AU - Atrio-Barandela, F.

AU - Aumont, J.

AU - Baccigalupi, C.

AU - Balbi, A.

AU - Banday, A. J.

AU - Barreiro, R. B.

AU - Bartlett, J. G.

AU - Battaner, E.

AU - Benabed, K.

AU - Benoît, A.

AU - Bernard, J. P.

AU - Bersanelli, M.

AU - Bikmaev, I.

AU - Böhringer, H.

AU - Bonaldi, A.

AU - Bond, J. R.

AU - Borrill, J.

AU - Bouchet, F. R.

AU - Bourdin, H.

AU - Brown, M. L.

AU - Brown, S. D.

AU - Burenin, R.

AU - Burigana, C.

AU - Cabella, P.

AU - Cardoso, J. F.

AU - Carvalho, P.

AU - Catalano, A.

AU - Cayón, L.

AU - Chiang, L. Y.

AU - Chon, G.

AU - Christensen, P. R.

AU - Churazov, E.

AU - Clements, D. L.

AU - Colafrancesco, S.

AU - Colombo, L. P.L.

AU - Coulais, A.

AU - Crill, B. P.

AU - Cuttaia, F.

AU - Da Silva, A.

AU - Dahle, H.

AU - Danese, L.

AU - Davis, R. J.

AU - De Bernardis, P.

AU - De Gasperis, G.

AU - De Rosa, A.

AU - De Zotti, G.

AU - Delabrouille, J.

AU - Démoclès, J.

AU - Désert, F. X.

AU - Dickinson, C.

AU - Diego, J. M.

AU - Dolag, K.

AU - Dole, H.

AU - Donzelli, S.

AU - Doré, O.

AU - Dörl, U.

AU - Douspis, M.

AU - Dupac, X.

AU - Enßlin, T. A.

AU - Eriksen, H. K.

AU - Finelli, F.

AU - Flores-Cacho, I.

AU - Forni, O.

AU - Frailis, M.

AU - Franceschi, E.

AU - Frommert, M.

AU - Galeotta, S.

AU - Ganga, K.

AU - Génova-Santos, R. T.

AU - Giard, M.

AU - Gilfanov, M.

AU - González-Nuevo, J.

AU - Górski, K. M.

AU - Gregorio, A.

AU - Gruppuso, A.

AU - Hansen, F. K.

AU - Harrison, D.

AU - Henrot-Versillé, S.

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N1 - Funding Information: A description of the Planck Collaboration and a list of its members, indicating which technical or scientific activities they have been involved in, can be found at http://www.rssd.esa.int/Planck_Collaboration . The Planck Collaboration acknowledges the support of: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MICINN and JA (Spain); Tekes, AoF and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); and DEISA (EU). Partial support for this work for L. Rudnick comes from U.S. NSF Grant 09-08668 to the University of Minnesota. We would also like to acknowledge useful conversations with G. Brunetti.

PY - 2013

Y1 - 2013

N2 - We present an analysis of Planck satellite data on the Coma cluster observed via the Sunyaev-Zeldovich effect. Thanks to its great sensitivity, Planck is able, for the first time, to detect SZ emission up to r ≈ 3 × R500. We test previously proposed spherically symmetric models for the pressure distribution in clusters against the azimuthally averaged data. In particular, we find that the Arnaud et al. (2010, A&A, 517, A92) "universal" pressure profile does not fit Coma, and that their pressure profile for merging systems provides a reasonable fit to the data only at r < R500; by r = 2 × R500 it underestimates the observed y profile by a factor of â‰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 > R500 than the mean pressure profile predicted by the simulations used to constrain the models. 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 as well as in the radio. Using Plancky profiles extracted from corresponding sectors we find pressure jumps of 4.9-0.2+0.4 and 5.0-0.1 +1.3 in the west and south-east, respectively. Assuming Rankine-Hugoniot pressure jump conditions, we deduce that the shock waves should propagate with Mach number Mw = 2.03-0.04+0.09 and Mse = 2.05-0.02+0.25 in the west and south-east, 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.

AB - We present an analysis of Planck satellite data on the Coma cluster observed via the Sunyaev-Zeldovich effect. Thanks to its great sensitivity, Planck is able, for the first time, to detect SZ emission up to r ≈ 3 × R500. We test previously proposed spherically symmetric models for the pressure distribution in clusters against the azimuthally averaged data. In particular, we find that the Arnaud et al. (2010, A&A, 517, A92) "universal" pressure profile does not fit Coma, and that their pressure profile for merging systems provides a reasonable fit to the data only at r < R500; by r = 2 × R500 it underestimates the observed y profile by a factor of â‰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 > R500 than the mean pressure profile predicted by the simulations used to constrain the models. 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 as well as in the radio. Using Plancky profiles extracted from corresponding sectors we find pressure jumps of 4.9-0.2+0.4 and 5.0-0.1 +1.3 in the west and south-east, respectively. Assuming Rankine-Hugoniot pressure jump conditions, we deduce that the shock waves should propagate with Mach number Mw = 2.03-0.04+0.09 and Mse = 2.05-0.02+0.25 in the west and south-east, 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.

KW - Cosmic background radiation

KW - Cosmology: observations

KW - Galaxies: clusters: general

KW - Galaxies: clusters: individual: Coma cluster

KW - Galaxies: clusters: intracluster medium

KW - X-rays: galaxies: clusters

UR - http://www.scopus.com/inward/record.url?scp=84879209116&partnerID=8YFLogxK

UR - http://www.scopus.com/inward/citedby.url?scp=84879209116&partnerID=8YFLogxK

U2 - 10.1051/0004-6361/201220247

DO - 10.1051/0004-6361/201220247

M3 - Article

AN - SCOPUS:84879209116

SN - 0004-6361

VL - 554

JO - Astronomy and Astrophysics

JF - Astronomy and Astrophysics

M1 - A140

ER -

Planck intermediate results: X. Physics of the hot gas in the Coma cluster

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