Planck intermediate results: VIII. Filaments between interacting clusters

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; R. Bhatia; I. Bikmaev; H. Böhringer; A. Bonaldi; J. R. Bond; J. Borrill; F. R. Bouchet; H. Bourdin; R. Burenin; C. Burigana; P. Cabella; J. F. Cardoso; G. Castex; A. Catalano; L. Cayón; A. Chamballu; R. R. Chary; L. Y. Chiang; G. Chon; P. R. Christensen; D. L. Clements; S. Colafrancesco; L. P.L. Colombo; B. Comis; A. Coulais; B. P. Crill; F. Cuttaia; A. Da Silva; H. Dahle; L. Danese; R. J. Davis; P. De Bernardis; G. De Gasperis; G. De Zotti; J. Delabrouille; J. Démoclès; F. X. Désert; J. M. Diego; K. Dolag; H. Dole; S. Donzelli; O. Doré; U. Dörl; M. Douspis; X. Dupac; G. Efstathiou; 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; Y. Giraud-Héraud; J. González-Nuevo; K. M. Górski; A. Gregorio; A. Gruppuso; F. K. Hansen; D. Harrison; A. Hempel; S. Henrot-Versillé; C. Hernández-Monteagudo; D. Herranz; S. R. Hildebrandt; E. Hivon; M. Hobson; W. A. Holmes; W. Hovest; G. Hurier; T. R. Jaffe; A. H. Jaffe; T. Jagemann; W. C. Jones; M. Juvela; I. Khamitov; T. S. Kisner; R. Kneissl; J. Knoche; L. Knox; M. Kunz; H. Kurki-Suonio; G. Lagache; 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; G. Luzzi; J. F. MacÍas-Pérez; B. Maffei; D. Maino; N. Mandolesi; M. Maris; F. Marleau; D. J. Marshall; 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; F. Nati; P. Natoli; H. U. Nørgaard-Nielsen; F. Noviello; D. Novikov; I. Novikov; S. Osborne; F. Pajot; D. Paoletti; F. Pasian; G. Patanchon; O. Perdereau; L. Perotto; 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. Roman; C. Rosset; M. Rossetti; J. A. Rubiño-Martín; B. Rusholme; M. Sandri; G. Savini; B. M. Schaefer; D. Scott; G. F. Smoot; J. L. Starck; R. Sudiwala; R. Sunyaev; D. Sutton; A. S. Suur-Uski; J. F. Sygnet; J. A. Tauber; L. Terenzi; L. Toffolatti; M. Tomasi; M. Tristram; L. Valenziano; B. Van Tent; P. Vielva; F. Villa; N. Vittorio; L. A. Wade; B. D. Wandelt; N. Welikala; S. D.M. White; D. Yvon; A. Zacchei; A. Zonca

doi:10.1051/0004-6361/201220194

Planck intermediate results: VIII. Filaments between interacting clusters

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, R. Bhatia, I. Bikmaev, H. Böhringer, A. BonaldiJ. R. Bond, J. Borrill, F. R. Bouchet, H. Bourdin, R. Burenin, C. Burigana, P. Cabella, J. F. Cardoso, G. Castex, A. Catalano, L. Cayón, A. Chamballu, R. R. Chary, L. Y. Chiang, G. Chon, P. R. Christensen, D. L. Clements, S. Colafrancesco, L. P.L. Colombo, B. Comis, A. Coulais, B. P. Crill, F. Cuttaia, A. Da Silva, H. Dahle, L. Danese, R. J. Davis, P. De Bernardis, G. De Gasperis, G. De Zotti, J. Delabrouille, J. Démoclès, F. X. Désert, J. M. Diego, K. Dolag, H. Dole, S. Donzelli, O. Doré, U. Dörl, M. Douspis, X. Dupac, G. Efstathiou, 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, Y. Giraud-Héraud, J. González-Nuevo, K. M. Górski, A. Gregorio, A. Gruppuso, F. K. Hansen, D. Harrison, A. Hempel, S. Henrot-Versillé, C. Hernández-Monteagudo, D. Herranz, S. R. Hildebrandt, E. Hivon, M. Hobson, W. A. Holmes, W. Hovest, G. Hurier, T. R. Jaffe, A. H. Jaffe, T. Jagemann, W. C. Jones, M. Juvela, I. Khamitov, T. S. Kisner, R. Kneissl, J. Knoche, L. Knox, M. Kunz, H. Kurki-Suonio, G. Lagache, 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, G. Luzzi, J. F. MacÍas-Pérez, B. Maffei, D. Maino, N. Mandolesi, M. Maris, F. Marleau, D. J. Marshall, 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, F. Nati, P. Natoli, H. U. Nørgaard-Nielsen, F. Noviello, D. Novikov, I. Novikov, S. Osborne, F. Pajot, D. Paoletti, F. Pasian, G. Patanchon, O. Perdereau, L. Perotto, 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. Roman, C. Rosset, M. Rossetti, J. A. Rubiño-Martín, B. Rusholme, M. Sandri, G. Savini, B. M. Schaefer, D. Scott, G. F. Smoot, J. L. Starck, R. Sudiwala, R. Sunyaev, D. Sutton, A. S. Suur-Uski, J. F. Sygnet, J. A. Tauber, L. Terenzi, L. Toffolatti, M. Tomasi, M. Tristram, L. Valenziano, B. Van Tent, P. Vielva, F. Villa, N. Vittorio, L. A. Wade, B. D. Wandelt, N. Welikala, S. D.M. White, D. Yvon, A. Zacchei, A. Zonca

Physics

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

31 Scopus citations

Abstract

Context. About half of the baryons of the Universe are expected to be in the form of filaments of hot and low-density intergalactic medium. Most of these baryons remain undetected even by the most advanced X-ray observatories, which are limited in sensitivity to the diffuse low-density medium. Aims. The Planck satellite has provided hundreds of detections of the hot gas in clusters of galaxies via the thermal Sunyaev-Zel'dovich (tSZ) effect and is an ideal instrument for studying extended low-density media through the tSZ effect. In this paper we use the Planck data to search for signatures of a fraction of these missing baryons between pairs of galaxy clusters. Methods. Cluster pairs are good candidates for searching for the hotter and denser phase of the intergalactic medium (which is more easily observed through the SZ effect). Using an X-ray catalogue of clusters and the Planck data, we selected physical pairs of clusters as candidates. Using the Planck data, we constructed a local map of the tSZ effect centred on each pair of galaxy clusters. ROSAT data were used to construct X-ray maps of these pairs. After modelling and subtracting the tSZ effect and X-ray emission for each cluster in the pair, we studied the residuals on both the SZ and X-ray maps. Results. For the merging cluster pair A399-A401 we observe a significant tSZ effect signal in the intercluster region beyond the virial radii of the clusters. A joint X-ray SZ analysis allows us to constrain the temperature and density of this intercluster medium. We obtain a temperature of kT = 7.1 ± 0.9 keV (consistent with previous estimates) and a baryon density of (3.7 ± 0.2) × 10^-4 cm ^-3. Conclusions. The Planck satellite mission has provided the first SZ detection of the hot and diffuse intercluster gas.

Original language	English (US)
Article number	A134
Journal	Astronomy and Astrophysics
Volume	550
DOIs	https://doi.org/10.1051/0004-6361/201220194
State	Published - 2013

All Science Journal Classification (ASJC) codes

Astronomy and Astrophysics
Space and Planetary Science

Keywords

Galaxies: clusters: general
Large-scale structure of Universe

Access to Document

10.1051/0004-6361/201220194

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., Bhatia, R., Bikmaev, I., Böhringer, H., ... Zonca, A. (2013). Planck intermediate results: VIII. Filaments between interacting clusters. Astronomy and Astrophysics, 550, Article A134. https://doi.org/10.1051/0004-6361/201220194

@article{cd9d9d111d884d3fb8bb5a3211ed2d2f,

title = "Planck intermediate results: VIII. Filaments between interacting clusters",

abstract = "Context. About half of the baryons of the Universe are expected to be in the form of filaments of hot and low-density intergalactic medium. Most of these baryons remain undetected even by the most advanced X-ray observatories, which are limited in sensitivity to the diffuse low-density medium. Aims. The Planck satellite has provided hundreds of detections of the hot gas in clusters of galaxies via the thermal Sunyaev-Zel'dovich (tSZ) effect and is an ideal instrument for studying extended low-density media through the tSZ effect. In this paper we use the Planck data to search for signatures of a fraction of these missing baryons between pairs of galaxy clusters. Methods. Cluster pairs are good candidates for searching for the hotter and denser phase of the intergalactic medium (which is more easily observed through the SZ effect). Using an X-ray catalogue of clusters and the Planck data, we selected physical pairs of clusters as candidates. Using the Planck data, we constructed a local map of the tSZ effect centred on each pair of galaxy clusters. ROSAT data were used to construct X-ray maps of these pairs. After modelling and subtracting the tSZ effect and X-ray emission for each cluster in the pair, we studied the residuals on both the SZ and X-ray maps. Results. For the merging cluster pair A399-A401 we observe a significant tSZ effect signal in the intercluster region beyond the virial radii of the clusters. A joint X-ray SZ analysis allows us to constrain the temperature and density of this intercluster medium. We obtain a temperature of kT = 7.1 ± 0.9 keV (consistent with previous estimates) and a baryon density of (3.7 ± 0.2) × 10-4 cm -3. Conclusions. The Planck satellite mission has provided the first SZ detection of the hot and diffuse intercluster gas.",

keywords = "Galaxies: clusters: general, Large-scale structure of Universe",

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 R. Bhatia 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 R. Burenin and C. Burigana and P. Cabella and Cardoso, {J. F.} and G. Castex and A. Catalano and L. Cay{\'o}n and A. Chamballu and Chary, {R. R.} and Chiang, {L. Y.} and G. Chon and Christensen, {P. R.} and Clements, {D. L.} and S. Colafrancesco and Colombo, {L. P.L.} and B. Comis 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 Zotti}, G. and J. Delabrouille and J. D{\'e}mocl{\`e}s and D{\'e}sert, {F. X.} 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 G. Efstathiou 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 Y. Giraud-H{\'e}raud 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 A. Hempel and S. Henrot-Versill{\'e} and C. Hern{\'a}ndez-Monteagudo and D. Herranz and Hildebrandt, {S. R.} and E. Hivon and M. Hobson and Holmes, {W. A.} and W. Hovest and G. Hurier and Jaffe, {T. R.} and Jaffe, {A. H.} and T. Jagemann and Jones, {W. C.} and M. Juvela and I. Khamitov and Kisner, {T. S.} and R. Kneissl and J. Knoche and L. Knox and M. Kunz and H. Kurki-Suonio and G. Lagache 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 G. Luzzi 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 Marshall, {D. J.} 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 F. Nati 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 F. Pasian and G. Patanchon and O. Perdereau and L. Perotto 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. Roman and C. Rosset and M. Rossetti and Rubi{\~n}o-Mart{\'i}n, {J. A.} and B. Rusholme and M. Sandri and G. Savini and Schaefer, {B. M.} and D. Scott and Smoot, {G. F.} and Starck, {J. L.} 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 L. Valenziano and {Van Tent}, B. 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 A. Zonca",

note = "Funding Information: Based on observations obtained with Planck ( http://www.esa.int/Planck ), an ESA science mission with instruments and contributions directly funded by ESA Member States, NASA, and Canada. The development of Planck has been supported by: 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 The development of Planck has been supported by: 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 PRACE (EU). We acknowledge the use of the Healpix software (G{\'o}rski et al. 2005) and SEXTRACTOR (Bertin & Arnouts 1996).",

year = "2013",

doi = "10.1051/0004-6361/201220194",

language = "English (US)",

volume = "550",

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, Bhatia, R, Bikmaev, I, Böhringer, H, Bonaldi, A, Bond, JR, Borrill, J, Bouchet, FR, Bourdin, H, Burenin, R, Burigana, C, Cabella, P, Cardoso, JF, Castex, G, Catalano, A, Cayón, L, Chamballu, A, Chary, RR, Chiang, LY, Chon, G, Christensen, PR, Clements, DL, Colafrancesco, S, Colombo, LPL, Comis, B, Coulais, A, Crill, BP, Cuttaia, F, Da Silva, A, Dahle, H, Danese, L, Davis, RJ, De Bernardis, P, De Gasperis, G, De Zotti, G, Delabrouille, J, Démoclès, J, Désert, FX, Diego, JM, Dolag, K, Dole, H, Donzelli, S, Doré, O, Dörl, U, Douspis, M, Dupac, X, Efstathiou, G, 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, Giraud-Héraud, Y, González-Nuevo, J, Górski, KM, Gregorio, A, Gruppuso, A, Hansen, FK, Harrison, D, Hempel, A, Henrot-Versillé, S, Hernández-Monteagudo, C, Herranz, D, Hildebrandt, SR, Hivon, E, Hobson, M, Holmes, WA, Hovest, W, Hurier, G, Jaffe, TR, Jaffe, AH, Jagemann, T, Jones, WC, Juvela, M, Khamitov, I, Kisner, TS, Kneissl, R, Knoche, J, Knox, L, Kunz, M, Kurki-Suonio, H, Lagache, G, Lamarre, JM, Lasenby, A, Lawrence, CR, Le Jeune, M, Leonardi, R, Lilje, PB, Linden-Vørnle, M, López-Caniego, M, Lubin, PM, Luzzi, G, MacÍas-Pérez, JF, Maffei, B, Maino, D, Mandolesi, N, Maris, M, Marleau, F, Marshall, DJ, 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, Nati, F, Natoli, P, Nørgaard-Nielsen, HU, Noviello, F, Novikov, D, Novikov, I, Osborne, S, Pajot, F, Paoletti, D, Pasian, F, Patanchon, G, Perdereau, O, Perotto, L, 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, Roman, M, Rosset, C, Rossetti, M, Rubiño-Martín, JA, Rusholme, B, Sandri, M, Savini, G, Schaefer, BM, Scott, D, Smoot, GF, Starck, JL, Sudiwala, R, Sunyaev, R, Sutton, D, Suur-Uski, AS, Sygnet, JF, Tauber, JA, Terenzi, L, Toffolatti, L, Tomasi, M, Tristram, M, Valenziano, L, Van Tent, B, Vielva, P, Villa, F, Vittorio, N, Wade, LA, Wandelt, BD, Welikala, N, White, SDM, Yvon, D, Zacchei, A & Zonca, A 2013, 'Planck intermediate results: VIII. Filaments between interacting clusters', Astronomy and Astrophysics, vol. 550, A134. https://doi.org/10.1051/0004-6361/201220194

TY - JOUR

T1 - Planck intermediate results

T2 - VIII. Filaments between interacting clusters

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 - Bhatia, R.

AU - Bikmaev, I.

AU - Böhringer, H.

AU - Bonaldi, A.

AU - Bond, J. R.

AU - Borrill, J.

AU - Bouchet, F. R.

AU - Bourdin, H.

AU - Burenin, R.

AU - Burigana, C.

AU - Cabella, P.

AU - Cardoso, J. F.

AU - Castex, G.

AU - Catalano, A.

AU - Cayón, L.

AU - Chamballu, A.

AU - Chary, R. R.

AU - Chiang, L. Y.

AU - Chon, G.

AU - Christensen, P. R.

AU - Clements, D. L.

AU - Colafrancesco, S.

AU - Colombo, L. P.L.

AU - Comis, B.

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 Zotti, G.

AU - Delabrouille, J.

AU - Démoclès, J.

AU - Désert, F. X.

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 - Efstathiou, G.

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 - Giraud-Héraud, Y.

AU - González-Nuevo, J.

AU - Górski, K. M.

AU - Gregorio, A.

AU - Gruppuso, A.

AU - Hansen, F. K.

AU - Harrison, D.

AU - Hempel, A.

AU - Henrot-Versillé, S.

AU - Hernández-Monteagudo, C.

AU - Herranz, D.

AU - Hildebrandt, S. R.

AU - Hivon, E.

AU - Hobson, M.

AU - Holmes, W. A.

AU - Hovest, W.

AU - Hurier, G.

AU - Jaffe, T. R.

AU - Jaffe, A. H.

AU - Jagemann, T.

AU - Jones, W. C.

AU - Juvela, M.

AU - Khamitov, I.

AU - Kisner, T. S.

AU - Kneissl, R.

AU - Knoche, J.

AU - Knox, L.

AU - Kunz, M.

AU - Kurki-Suonio, H.

AU - Lagache, G.

AU - Lamarre, J. M.

AU - Lasenby, A.

AU - Lawrence, C. R.

AU - Le Jeune, M.

AU - Leonardi, R.

AU - Lilje, P. B.

AU - Linden-Vørnle, M.

AU - López-Caniego, M.

AU - Lubin, P. M.

AU - Luzzi, G.

AU - MacÍas-Pérez, J. F.

AU - Maffei, B.

AU - Maino, D.

AU - Mandolesi, N.

AU - Maris, M.

AU - Marleau, F.

AU - Marshall, D. J.

AU - Martínez-González, E.

AU - Masi, S.

AU - Massardi, M.

AU - Matarrese, S.

AU - Matthai, F.

AU - Mazzotta, P.

AU - Mei, S.

AU - Melchiorri, A.

AU - Melin, J. B.

AU - Mendes, L.

AU - Mennella, A.

AU - Mitra, S.

AU - Miville-Deschênes, M. A.

AU - Moneti, A.

AU - Montier, L.

AU - Morgante, G.

AU - Munshi, D.

AU - Murphy, J. A.

AU - Naselsky, P.

AU - Nati, F.

AU - Natoli, P.

AU - Nørgaard-Nielsen, H. U.

AU - Noviello, F.

AU - Novikov, D.

AU - Novikov, I.

AU - Osborne, S.

AU - Pajot, F.

AU - Paoletti, D.

AU - Pasian, F.

AU - Patanchon, G.

AU - Perdereau, O.

AU - Perotto, L.

AU - Perrotta, F.

AU - Piacentini, F.

AU - Piat, M.

AU - Pierpaoli, E.

AU - Piffaretti, R.

AU - Plaszczynski, S.

AU - Pointecouteau, E.

AU - Polenta, G.

AU - Ponthieu, N.

AU - Popa, L.

AU - Poutanen, T.

AU - Pratt, G. W.

AU - Prunet, S.

AU - Puget, J. L.

AU - Rachen, J. P.

AU - Rebolo, R.

AU - Reinecke, M.

AU - Remazeilles, M.

AU - Renault, C.

AU - Ricciardi, S.

AU - Riller, T.

AU - Ristorcelli, I.

AU - Rocha, G.

AU - Roman, M.

AU - Rosset, C.

AU - Rossetti, M.

AU - Rubiño-Martín, J. A.

AU - Rusholme, B.

AU - Sandri, M.

AU - Savini, G.

AU - Schaefer, B. M.

AU - Scott, D.

AU - Smoot, G. F.

AU - Starck, J. L.

AU - Sudiwala, R.

AU - Sunyaev, R.

AU - Sutton, D.

AU - Suur-Uski, A. S.

AU - Sygnet, J. F.

AU - Tauber, J. A.

AU - Terenzi, L.

AU - Toffolatti, L.

AU - Tomasi, M.

AU - Tristram, M.

AU - Valenziano, L.

AU - Van Tent, B.

AU - Vielva, P.

AU - Villa, F.

AU - Vittorio, N.

AU - Wade, L. A.

AU - Wandelt, B. D.

AU - Welikala, N.

AU - White, S. D.M.

AU - Yvon, D.

AU - Zacchei, A.

AU - Zonca, A.

N1 - Funding Information: Based on observations obtained with Planck ( http://www.esa.int/Planck ), an ESA science mission with instruments and contributions directly funded by ESA Member States, NASA, and Canada. The development of Planck has been supported by: 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 The development of Planck has been supported by: 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 PRACE (EU). We acknowledge the use of the Healpix software (Górski et al. 2005) and SEXTRACTOR (Bertin & Arnouts 1996).

PY - 2013

Y1 - 2013

N2 - Context. About half of the baryons of the Universe are expected to be in the form of filaments of hot and low-density intergalactic medium. Most of these baryons remain undetected even by the most advanced X-ray observatories, which are limited in sensitivity to the diffuse low-density medium. Aims. The Planck satellite has provided hundreds of detections of the hot gas in clusters of galaxies via the thermal Sunyaev-Zel'dovich (tSZ) effect and is an ideal instrument for studying extended low-density media through the tSZ effect. In this paper we use the Planck data to search for signatures of a fraction of these missing baryons between pairs of galaxy clusters. Methods. Cluster pairs are good candidates for searching for the hotter and denser phase of the intergalactic medium (which is more easily observed through the SZ effect). Using an X-ray catalogue of clusters and the Planck data, we selected physical pairs of clusters as candidates. Using the Planck data, we constructed a local map of the tSZ effect centred on each pair of galaxy clusters. ROSAT data were used to construct X-ray maps of these pairs. After modelling and subtracting the tSZ effect and X-ray emission for each cluster in the pair, we studied the residuals on both the SZ and X-ray maps. Results. For the merging cluster pair A399-A401 we observe a significant tSZ effect signal in the intercluster region beyond the virial radii of the clusters. A joint X-ray SZ analysis allows us to constrain the temperature and density of this intercluster medium. We obtain a temperature of kT = 7.1 ± 0.9 keV (consistent with previous estimates) and a baryon density of (3.7 ± 0.2) × 10-4 cm -3. Conclusions. The Planck satellite mission has provided the first SZ detection of the hot and diffuse intercluster gas.

AB - Context. About half of the baryons of the Universe are expected to be in the form of filaments of hot and low-density intergalactic medium. Most of these baryons remain undetected even by the most advanced X-ray observatories, which are limited in sensitivity to the diffuse low-density medium. Aims. The Planck satellite has provided hundreds of detections of the hot gas in clusters of galaxies via the thermal Sunyaev-Zel'dovich (tSZ) effect and is an ideal instrument for studying extended low-density media through the tSZ effect. In this paper we use the Planck data to search for signatures of a fraction of these missing baryons between pairs of galaxy clusters. Methods. Cluster pairs are good candidates for searching for the hotter and denser phase of the intergalactic medium (which is more easily observed through the SZ effect). Using an X-ray catalogue of clusters and the Planck data, we selected physical pairs of clusters as candidates. Using the Planck data, we constructed a local map of the tSZ effect centred on each pair of galaxy clusters. ROSAT data were used to construct X-ray maps of these pairs. After modelling and subtracting the tSZ effect and X-ray emission for each cluster in the pair, we studied the residuals on both the SZ and X-ray maps. Results. For the merging cluster pair A399-A401 we observe a significant tSZ effect signal in the intercluster region beyond the virial radii of the clusters. A joint X-ray SZ analysis allows us to constrain the temperature and density of this intercluster medium. We obtain a temperature of kT = 7.1 ± 0.9 keV (consistent with previous estimates) and a baryon density of (3.7 ± 0.2) × 10-4 cm -3. Conclusions. The Planck satellite mission has provided the first SZ detection of the hot and diffuse intercluster gas.

KW - Galaxies: clusters: general

KW - Large-scale structure of Universe

UR - http://www.scopus.com/inward/record.url?scp=84873921479&partnerID=8YFLogxK

UR - http://www.scopus.com/inward/citedby.url?scp=84873921479&partnerID=8YFLogxK

U2 - 10.1051/0004-6361/201220194

DO - 10.1051/0004-6361/201220194

M3 - Article

AN - SCOPUS:84873921479

SN - 0004-6361

VL - 550

JO - Astronomy and Astrophysics

JF - Astronomy and Astrophysics

M1 - A134

ER -

Planck intermediate results: VIII. Filaments between interacting clusters

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