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 | |
| 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
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Planck intermediate results : VIII. Filaments between interacting clusters. / 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.; Bonaldi, A.; Bond, J. R.; Borrill, J.; Bouchet, F. R.; Bourdin, H.; Burenin, R.; Burigana, C.; Cabella, P.; Cardoso, J. F.; Castex, G.; Catalano, A.; Cayón, L.; Chamballu, A.; Chary, R. R.; Chiang, L. Y.; Chon, G.; Christensen, P. R.; Clements, D. L.; Colafrancesco, S.; Colombo, L. P.L.; Comis, B.; Coulais, A.; Crill, B. P.; Cuttaia, F.; Da Silva, A.; Dahle, H.; Danese, L.; Davis, R. J.; De Bernardis, P.; De Gasperis, G.; De Zotti, G.; Delabrouille, J.; Démoclès, J.; Désert, F. X.; Diego, J. M.; Dolag, K.; Dole, H.; Donzelli, S.; Doré, O.; Dörl, U.; Douspis, M.; Dupac, X.; Efstathiou, G.; Enßlin, T. A.; Eriksen, H. K.; Finelli, F.; Flores-Cacho, I.; Forni, O.; Frailis, M.; Franceschi, E.; Frommert, M.; Galeotta, S.; Ganga, K.; Génova-Santos, R. T.; Giard, M.; Gilfanov, M.; Giraud-Héraud, Y.; González-Nuevo, J.; Górski, K. M.; Gregorio, A.; Gruppuso, A.; Hansen, F. K.; Harrison, D.; Hempel, A.; Henrot-Versillé, S.; Hernández-Monteagudo, C.; Herranz, D.; Hildebrandt, S. R.; Hivon, E.; Hobson, M.; Holmes, W. A.; Hovest, W.; Hurier, G.; Jaffe, T. R.; Jaffe, A. H.; Jagemann, T.; Jones, W. C.; Juvela, M.; Khamitov, I.; Kisner, T. S.; Kneissl, R.; Knoche, J.; Knox, L.; Kunz, M.; Kurki-Suonio, H.; Lagache, G.; Lamarre, J. M.; Lasenby, A.; Lawrence, C. R.; Le Jeune, M.; Leonardi, R.; Lilje, P. B.; Linden-Vørnle, M.; López-Caniego, M.; Lubin, P. M.; Luzzi, G.; MacÍas-Pérez, J. F.; Maffei, B.; Maino, D.; Mandolesi, N.; Maris, M.; Marleau, F.; Marshall, D. J.; Martínez-González, E.; Masi, S.; Massardi, M.; Matarrese, S.; Matthai, F.; Mazzotta, P.; Mei, S.; Melchiorri, A.; Melin, J. B.; Mendes, L.; Mennella, A.; Mitra, S.; Miville-Deschênes, M. A.; Moneti, A.; Montier, L.; Morgante, G.; Munshi, D.; Murphy, J. A.; Naselsky, P.; Nati, F.; Natoli, P.; Nørgaard-Nielsen, H. U.; 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, G. W.; Prunet, S.; Puget, J. L.; Rachen, J. P.; Rebolo, R.; Reinecke, M.; Remazeilles, M.; Renault, C.; Ricciardi, S.; Riller, T.; Ristorcelli, I.; Rocha, G.; Roman, M.; Rosset, C.; Rossetti, M.; Rubiño-Martín, J. A.; Rusholme, B.; Sandri, M.; Savini, G.; Schaefer, B. M.; Scott, D.; Smoot, G. F.; Starck, J. L.; Sudiwala, R.; Sunyaev, R.; Sutton, D.; Suur-Uski, A. S.; Sygnet, J. F.; Tauber, J. A.; Terenzi, L.; Toffolatti, L.; Tomasi, M.; Tristram, M.; Valenziano, L.; Van Tent, B.; Vielva, P.; Villa, F.; Vittorio, N.; Wade, L. A.; Wandelt, B. D.; Welikala, N.; White, S. D.M.; Yvon, D.; Zacchei, A.; Zonca, A.
In: Astronomy and Astrophysics, Vol. 550, A134, 2013.Research output: Contribution to journal › Article › peer-review
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
VL - 550
JO - Astronomy and Astrophysics
JF - Astronomy and Astrophysics
SN - 0004-6361
M1 - A134
ER -