Planck intermediate results: IV. the XMM-Newton validation programme for new Planck galaxy clusters

P. A.R. Ade, N. Aghanim, M. Arnaud, M. Ashdown, 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, S. BorganiJ. Borrill, F. R. Bouchet, M. L. Brown, C. Burigana, R. C. Butler, P. Cabella, P. Carvalho, A. Catalano, L. Cayón, A. Chamballu, R. R. Chary, L. Y. Chiang, G. Chon, P. R. Christensen, D. L. Clements, S. Colafrancesco, S. Colombi, A. Coulais, B. P. Crill, F. Cuttaia, A. Da Silva, H. Dahle, 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, 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, Y. Giraud-Héraud, J. González-Nuevo, R. González-Riestra, 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, A. Hornstrup, W. Hovest, K. M. Huffenberger, G. Hurier, A. H. Jaffe, T. Jagemann, W. C. Jones, M. Juvela, R. Kneissl, J. Knoche, L. Knox, M. Kunz, H. Kurki-Suonio, G. Lagache, J. M. Lamarre, A. Lasenby, C. R. Lawrence, M. Le Jeune, S. Leach, R. Leonardi, A. Liddle, P. B. Lilje, M. Linden-Vørnle, M. López-Caniego, G. Luzzi, J. F. MacÍas-Pérez, D. Maino, N. Mandolesi, R. Mann, M. Maris, F. Marleau, D. J. Marshall, E. Martínez-González, S. Masi, M. Massardi, S. Matarrese, P. Mazzotta, S. Mei, P. R. Meinhold, A. Melchiorri, J. B. Melin, L. Mendes, A. Mennella, S. Mitra, M. A. Miville-Deschênes, A. Moneti, G. Morgante, D. Mortlock, D. Munshi, P. Naselsky, F. Nati, 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, P. Platania, E. Pointecouteau, G. Polenta, L. Popa, T. Poutanen, G. W. Pratt, S. Prunet, J. L. Puget, M. Reinecke, M. Remazeilles, C. Renault, S. Ricciardi, G. Rocha, C. Rosset, M. Rossetti, J. A. Rubiño-Martín, B. Rusholme, M. Sandri, G. Savini, D. Scott, G. F. Smoot, A. Stanford, 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, L. Valenziano, B. Van Tent, P. Vielva, F. Villa, N. Vittorio, L. A. Wade, B. D. Wandelt, N. Welikala, J. Weller, S. D.M. White, D. Yvon, A. Zacchei, A. Zonca

Resultado de la investigación: Article

10 Citas (Scopus)

Resumen

We present the final results from the XMM-Newton validation follow-up of new Planck galaxy cluster candidates. We observed 15 new candidates, detected with signal-to-noise ratios between 4.0 and 6.1 in the 15.5-month nominal Planck survey. The candidates were selected using ancillary data flags derived from the ROSAT All Sky Survey (RASS) and Digitized Sky Survey all-sky maps, with the aim of pushing into the low SZ flux, high-z regime and testing RASS flags as indicators of candidate reliability. Fourteen new clusters were detected by XMM-Newton, ten single clusters and two double systems. Redshifts from X-ray spectroscopy lie in the range 0.2 to 0.9, with six clusters at z > 0.5. Estimated masses (M500) range from 2.5 × 1014 to 8 × 1014 M. We discuss our results in the context of the full XMM-Newton validation programme, in which 51 new clusters have been detected. This includes four double and two triple systems, some of which are chance projections on the sky of clusters at different redshifts. We find thatassociation with a source from the RASS-Bright Source Catalogue is a robust indicator of the reliability of a candidate, whereas association with a source from the RASS-Faint Source Catalogue does not guarantee that the SZ candidate is a bona fide cluster. Nevertheless, most Planck clusters appear in RASS maps, with a significance greater than 2σ being a good indication that the candidate is a real cluster. Candidate validation from association with SDSS galaxy overdensity at z > 0.5 is also discussed. The full sample gives a Planck sensitivity threshold of Y500 4 × 10-4 arcmin2, with indication for Malmquist bias in the Y X-Y500 relation below this threshold. The corresponding mass threshold depends on redshift. Systems with M500 > 5 × 1014 MM at z > 0.5 are easily detectable with Planck. The newly-detected clusters follow the YX-Y500 relation derived from X-ray selected samples. Compared to X-ray selected clusters, the new SZ clusters have a lower X-ray luminosity on average for their mass. There is no indication of departure from standard self-similar evolution in the X-ray versus SZ scaling properties. In particular, there is no significant evolution of the YX/Y500 ratio.

Idioma originalEnglish
Número de artículoA130
PublicaciónAstronomy and Astrophysics
Volumen550
DOI
EstadoPublished - 18 feb 2013

Huella dactilar

XMM-Newton telescope
newton
galaxies
indication
x rays
catalogs
thresholds
sky
programme
signal-to-noise ratio
X-ray spectroscopy
pushing
signal to noise ratios
projection
luminosity
scaling

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science

Citar esto

Ade, P. A. R., Aghanim, N., Arnaud, M., Ashdown, M., Aumont, J., Baccigalupi, C., ... Zonca, A. (2013). Planck intermediate results: IV. the XMM-Newton validation programme for new Planck galaxy clusters. Astronomy and Astrophysics, 550, [A130]. https://doi.org/10.1051/0004-6361/201219519
Ade, P. A.R. ; Aghanim, N. ; Arnaud, M. ; Ashdown, M. ; 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. ; Bond, J. R. ; Borgani, S. ; Borrill, J. ; Bouchet, F. R. ; Brown, M. L. ; Burigana, C. ; Butler, R. C. ; Cabella, P. ; Carvalho, P. ; Catalano, A. ; Cayón, L. ; Chamballu, A. ; Chary, R. R. ; Chiang, L. Y. ; Chon, G. ; Christensen, P. R. ; Clements, D. L. ; Colafrancesco, S. ; Colombi, S. ; Coulais, A. ; Crill, B. P. ; Cuttaia, F. ; Da Silva, A. ; Dahle, H. ; 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. ; Douspis, M. ; Dupac, X. ; 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. ; Giraud-Héraud, Y. ; González-Nuevo, J. ; González-Riestra, R. ; 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. ; Hornstrup, A. ; Hovest, W. ; Huffenberger, K. M. ; Hurier, G. ; Jaffe, A. H. ; Jagemann, T. ; Jones, W. C. ; Juvela, M. ; Kneissl, R. ; Knoche, J. ; Knox, L. ; Kunz, M. ; Kurki-Suonio, H. ; Lagache, G. ; Lamarre, J. M. ; Lasenby, A. ; Lawrence, C. R. ; Le Jeune, M. ; Leach, S. ; Leonardi, R. ; Liddle, A. ; Lilje, P. B. ; Linden-Vørnle, M. ; López-Caniego, M. ; Luzzi, G. ; MacÍas-Pérez, J. F. ; Maino, D. ; Mandolesi, N. ; Mann, R. ; Maris, M. ; Marleau, F. ; Marshall, D. J. ; Martínez-González, E. ; Masi, S. ; Massardi, M. ; Matarrese, S. ; Mazzotta, P. ; Mei, S. ; Meinhold, P. R. ; Melchiorri, A. ; Melin, J. B. ; Mendes, L. ; Mennella, A. ; Mitra, S. ; Miville-Deschênes, M. A. ; Moneti, A. ; Morgante, G. ; Mortlock, D. ; Munshi, D. ; Naselsky, P. ; Nati, F. ; Natoli, P. ; Nørgaard-Nielsen, H. U. ; Noviello, F. ; Osborne, S. ; Pajot, F. ; Paoletti, D. ; Perdereau, O. ; Perrotta, F. ; Piacentini, F. ; Piat, M. ; Pierpaoli, E. ; Piffaretti, R. ; Plaszczynski, S. ; Platania, P. ; Pointecouteau, E. ; Polenta, G. ; Popa, L. ; Poutanen, T. ; Pratt, G. W. ; Prunet, S. ; Puget, J. L. ; Reinecke, M. ; Remazeilles, M. ; Renault, C. ; Ricciardi, S. ; Rocha, G. ; Rosset, C. ; Rossetti, M. ; Rubiño-Martín, J. A. ; Rusholme, B. ; Sandri, M. ; Savini, G. ; Scott, D. ; Smoot, G. F. ; Stanford, A. ; Stivoli, F. ; 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. ; Weller, J. ; White, S. D.M. ; Yvon, D. ; Zacchei, A. ; Zonca, A. / Planck intermediate results : IV. the XMM-Newton validation programme for new Planck galaxy clusters. En: Astronomy and Astrophysics. 2013 ; Vol. 550.
@article{eff127c7a3124741be35bb9c838312e0,
title = "Planck intermediate results: IV. the XMM-Newton validation programme for new Planck galaxy clusters",
abstract = "We present the final results from the XMM-Newton validation follow-up of new Planck galaxy cluster candidates. We observed 15 new candidates, detected with signal-to-noise ratios between 4.0 and 6.1 in the 15.5-month nominal Planck survey. The candidates were selected using ancillary data flags derived from the ROSAT All Sky Survey (RASS) and Digitized Sky Survey all-sky maps, with the aim of pushing into the low SZ flux, high-z regime and testing RASS flags as indicators of candidate reliability. Fourteen new clusters were detected by XMM-Newton, ten single clusters and two double systems. Redshifts from X-ray spectroscopy lie in the range 0.2 to 0.9, with six clusters at z > 0.5. Estimated masses (M500) range from 2.5 × 1014 to 8 × 1014 MM·. We discuss our results in the context of the full XMM-Newton validation programme, in which 51 new clusters have been detected. This includes four double and two triple systems, some of which are chance projections on the sky of clusters at different redshifts. We find thatassociation with a source from the RASS-Bright Source Catalogue is a robust indicator of the reliability of a candidate, whereas association with a source from the RASS-Faint Source Catalogue does not guarantee that the SZ candidate is a bona fide cluster. Nevertheless, most Planck clusters appear in RASS maps, with a significance greater than 2σ being a good indication that the candidate is a real cluster. Candidate validation from association with SDSS galaxy overdensity at z > 0.5 is also discussed. The full sample gives a Planck sensitivity threshold of Y500 4 × 10-4 arcmin2, with indication for Malmquist bias in the Y X-Y500 relation below this threshold. The corresponding mass threshold depends on redshift. Systems with M500 > 5 × 1014 MM at z > 0.5 are easily detectable with Planck. The newly-detected clusters follow the YX-Y500 relation derived from X-ray selected samples. Compared to X-ray selected clusters, the new SZ clusters have a lower X-ray luminosity on average for their mass. There is no indication of departure from standard self-similar evolution in the X-ray versus SZ scaling properties. In particular, there is no significant evolution of the YX/Y500 ratio.",
keywords = "Cosmic background radiation, Cosmology: observations, Galaxies: clusters: general, Galaxies: clusters: intracluster medium, X-rays: galaxies: clusters",
author = "Ade, {P. A.R.} and N. Aghanim and M. Arnaud and M. Ashdown 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 S. Borgani and J. Borrill and Bouchet, {F. R.} and Brown, {M. L.} and C. Burigana and Butler, {R. C.} and P. Cabella and P. Carvalho 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 S. Colombi and A. Coulais and Crill, {B. P.} and F. Cuttaia and {Da Silva}, A. and H. Dahle 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 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 Y. Giraud-H{\'e}raud and J. Gonz{\'a}lez-Nuevo and R. Gonz{\'a}lez-Riestra 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 A. Hornstrup and W. Hovest and Huffenberger, {K. M.} and G. Hurier and Jaffe, {A. H.} and T. Jagemann and Jones, {W. C.} and M. Juvela 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 S. Leach and R. Leonardi and A. Liddle and Lilje, {P. B.} and M. Linden-V{\o}rnle and M. L{\'o}pez-Caniego and G. Luzzi and Mac{\'I}as-P{\'e}rez, {J. F.} and D. Maino and N. Mandolesi and R. Mann 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 P. Mazzotta and S. Mei and Meinhold, {P. R.} 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 G. Morgante and D. Mortlock and D. Munshi and P. Naselsky and F. Nati and P. Natoli and N{\o}rgaard-Nielsen, {H. U.} and F. Noviello 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 P. Platania and E. Pointecouteau and G. Polenta and L. Popa and T. Poutanen and Pratt, {G. W.} and S. Prunet and Puget, {J. L.} and M. Reinecke and M. Remazeilles and C. Renault and S. Ricciardi and G. Rocha 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 D. Scott and Smoot, {G. F.} and A. Stanford 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 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 J. Weller and White, {S. D.M.} and D. Yvon and A. Zacchei and A. Zonca",
year = "2013",
month = "2",
day = "18",
doi = "10.1051/0004-6361/201219519",
language = "English",
volume = "550",
journal = "Astronomy and Astrophysics",
issn = "0004-6361",
publisher = "EDP Sciences",

}

Ade, PAR, Aghanim, N, Arnaud, M, Ashdown, M, 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, Borgani, S, Borrill, J, Bouchet, FR, Brown, ML, Burigana, C, Butler, RC, Cabella, P, Carvalho, P, Catalano, A, Cayón, L, Chamballu, A, Chary, RR, Chiang, LY, Chon, G, Christensen, PR, Clements, DL, Colafrancesco, S, Colombi, S, Coulais, A, Crill, BP, Cuttaia, F, Da Silva, A, Dahle, H, 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, 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, Giraud-Héraud, Y, González-Nuevo, J, González-Riestra, R, 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, Hornstrup, A, Hovest, W, Huffenberger, KM, Hurier, G, Jaffe, AH, Jagemann, T, Jones, WC, Juvela, M, Kneissl, R, Knoche, J, Knox, L, Kunz, M, Kurki-Suonio, H, Lagache, G, Lamarre, JM, Lasenby, A, Lawrence, CR, Le Jeune, M, Leach, S, Leonardi, R, Liddle, A, Lilje, PB, Linden-Vørnle, M, López-Caniego, M, Luzzi, G, MacÍas-Pérez, JF, Maino, D, Mandolesi, N, Mann, R, Maris, M, Marleau, F, Marshall, DJ, Martínez-González, E, Masi, S, Massardi, M, Matarrese, S, Mazzotta, P, Mei, S, Meinhold, PR, Melchiorri, A, Melin, JB, Mendes, L, Mennella, A, Mitra, S, Miville-Deschênes, MA, Moneti, A, Morgante, G, Mortlock, D, Munshi, D, Naselsky, P, Nati, F, Natoli, P, Nørgaard-Nielsen, HU, Noviello, F, Osborne, S, Pajot, F, Paoletti, D, Perdereau, O, Perrotta, F, Piacentini, F, Piat, M, Pierpaoli, E, Piffaretti, R, Plaszczynski, S, Platania, P, Pointecouteau, E, Polenta, G, Popa, L, Poutanen, T, Pratt, GW, Prunet, S, Puget, JL, Reinecke, M, Remazeilles, M, Renault, C, Ricciardi, S, Rocha, G, Rosset, C, Rossetti, M, Rubiño-Martín, JA, Rusholme, B, Sandri, M, Savini, G, Scott, D, Smoot, GF, Stanford, A, Stivoli, F, 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, Weller, J, White, SDM, Yvon, D, Zacchei, A & Zonca, A 2013, 'Planck intermediate results: IV. the XMM-Newton validation programme for new Planck galaxy clusters', Astronomy and Astrophysics, vol. 550, A130. https://doi.org/10.1051/0004-6361/201219519

Planck intermediate results : IV. the XMM-Newton validation programme for new Planck galaxy clusters. / Ade, P. A.R.; Aghanim, N.; Arnaud, M.; Ashdown, M.; 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.; Bond, J. R.; Borgani, S.; Borrill, J.; Bouchet, F. R.; Brown, M. L.; Burigana, C.; Butler, R. C.; Cabella, P.; Carvalho, P.; Catalano, A.; Cayón, L.; Chamballu, A.; Chary, R. R.; Chiang, L. Y.; Chon, G.; Christensen, P. R.; Clements, D. L.; Colafrancesco, S.; Colombi, S.; Coulais, A.; Crill, B. P.; Cuttaia, F.; Da Silva, A.; Dahle, H.; 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.; Douspis, M.; Dupac, X.; 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.; Giraud-Héraud, Y.; González-Nuevo, J.; González-Riestra, R.; 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.; Hornstrup, A.; Hovest, W.; Huffenberger, K. M.; Hurier, G.; Jaffe, A. H.; Jagemann, T.; Jones, W. C.; Juvela, M.; Kneissl, R.; Knoche, J.; Knox, L.; Kunz, M.; Kurki-Suonio, H.; Lagache, G.; Lamarre, J. M.; Lasenby, A.; Lawrence, C. R.; Le Jeune, M.; Leach, S.; Leonardi, R.; Liddle, A.; Lilje, P. B.; Linden-Vørnle, M.; López-Caniego, M.; Luzzi, G.; MacÍas-Pérez, J. F.; Maino, D.; Mandolesi, N.; Mann, R.; Maris, M.; Marleau, F.; Marshall, D. J.; Martínez-González, E.; Masi, S.; Massardi, M.; Matarrese, S.; Mazzotta, P.; Mei, S.; Meinhold, P. R.; Melchiorri, A.; Melin, J. B.; Mendes, L.; Mennella, A.; Mitra, S.; Miville-Deschênes, M. A.; Moneti, A.; Morgante, G.; Mortlock, D.; Munshi, D.; Naselsky, P.; Nati, F.; Natoli, P.; Nørgaard-Nielsen, H. U.; Noviello, F.; Osborne, S.; Pajot, F.; Paoletti, D.; Perdereau, O.; Perrotta, F.; Piacentini, F.; Piat, M.; Pierpaoli, E.; Piffaretti, R.; Plaszczynski, S.; Platania, P.; Pointecouteau, E.; Polenta, G.; Popa, L.; Poutanen, T.; Pratt, G. W.; Prunet, S.; Puget, J. L.; Reinecke, M.; Remazeilles, M.; Renault, C.; Ricciardi, S.; Rocha, G.; Rosset, C.; Rossetti, M.; Rubiño-Martín, J. A.; Rusholme, B.; Sandri, M.; Savini, G.; Scott, D.; Smoot, G. F.; Stanford, A.; Stivoli, F.; 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.; Weller, J.; White, S. D.M.; Yvon, D.; Zacchei, A.; Zonca, A.

En: Astronomy and Astrophysics, Vol. 550, A130, 18.02.2013.

Resultado de la investigación: Article

TY - JOUR

T1 - Planck intermediate results

T2 - IV. the XMM-Newton validation programme for new Planck galaxy clusters

AU - Ade, P. A.R.

AU - Aghanim, N.

AU - Arnaud, M.

AU - Ashdown, M.

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 - Borgani, S.

AU - Borrill, J.

AU - Bouchet, F. R.

AU - Brown, M. L.

AU - Burigana, C.

AU - Butler, R. C.

AU - Cabella, P.

AU - Carvalho, P.

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 - Colombi, S.

AU - Coulais, A.

AU - Crill, B. P.

AU - Cuttaia, F.

AU - Da Silva, A.

AU - Dahle, H.

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 - 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 - Giraud-Héraud, Y.

AU - González-Nuevo, J.

AU - González-Riestra, R.

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 - Hornstrup, A.

AU - Hovest, W.

AU - Huffenberger, K. M.

AU - Hurier, G.

AU - Jaffe, A. H.

AU - Jagemann, T.

AU - Jones, W. C.

AU - Juvela, M.

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 - Leach, S.

AU - Leonardi, R.

AU - Liddle, A.

AU - Lilje, P. B.

AU - Linden-Vørnle, M.

AU - López-Caniego, M.

AU - Luzzi, G.

AU - MacÍas-Pérez, J. F.

AU - Maino, D.

AU - Mandolesi, N.

AU - Mann, R.

AU - Maris, M.

AU - Marleau, F.

AU - Marshall, D. J.

AU - Martínez-González, E.

AU - Masi, S.

AU - Massardi, M.

AU - Matarrese, S.

AU - Mazzotta, P.

AU - Mei, S.

AU - Meinhold, P. R.

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 - Morgante, G.

AU - Mortlock, D.

AU - Munshi, D.

AU - Naselsky, P.

AU - Nati, F.

AU - Natoli, P.

AU - Nørgaard-Nielsen, H. U.

AU - Noviello, F.

AU - Osborne, S.

AU - Pajot, F.

AU - Paoletti, D.

AU - Perdereau, O.

AU - Perrotta, F.

AU - Piacentini, F.

AU - Piat, M.

AU - Pierpaoli, E.

AU - Piffaretti, R.

AU - Plaszczynski, S.

AU - Platania, P.

AU - Pointecouteau, E.

AU - Polenta, G.

AU - Popa, L.

AU - Poutanen, T.

AU - Pratt, G. W.

AU - Prunet, S.

AU - Puget, J. L.

AU - Reinecke, M.

AU - Remazeilles, M.

AU - Renault, C.

AU - Ricciardi, S.

AU - Rocha, G.

AU - Rosset, C.

AU - Rossetti, M.

AU - Rubiño-Martín, J. A.

AU - Rusholme, B.

AU - Sandri, M.

AU - Savini, G.

AU - Scott, D.

AU - Smoot, G. F.

AU - Stanford, A.

AU - Stivoli, F.

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 - Weller, J.

AU - White, S. D.M.

AU - Yvon, D.

AU - Zacchei, A.

AU - Zonca, A.

PY - 2013/2/18

Y1 - 2013/2/18

N2 - We present the final results from the XMM-Newton validation follow-up of new Planck galaxy cluster candidates. We observed 15 new candidates, detected with signal-to-noise ratios between 4.0 and 6.1 in the 15.5-month nominal Planck survey. The candidates were selected using ancillary data flags derived from the ROSAT All Sky Survey (RASS) and Digitized Sky Survey all-sky maps, with the aim of pushing into the low SZ flux, high-z regime and testing RASS flags as indicators of candidate reliability. Fourteen new clusters were detected by XMM-Newton, ten single clusters and two double systems. Redshifts from X-ray spectroscopy lie in the range 0.2 to 0.9, with six clusters at z > 0.5. Estimated masses (M500) range from 2.5 × 1014 to 8 × 1014 MM·. We discuss our results in the context of the full XMM-Newton validation programme, in which 51 new clusters have been detected. This includes four double and two triple systems, some of which are chance projections on the sky of clusters at different redshifts. We find thatassociation with a source from the RASS-Bright Source Catalogue is a robust indicator of the reliability of a candidate, whereas association with a source from the RASS-Faint Source Catalogue does not guarantee that the SZ candidate is a bona fide cluster. Nevertheless, most Planck clusters appear in RASS maps, with a significance greater than 2σ being a good indication that the candidate is a real cluster. Candidate validation from association with SDSS galaxy overdensity at z > 0.5 is also discussed. The full sample gives a Planck sensitivity threshold of Y500 4 × 10-4 arcmin2, with indication for Malmquist bias in the Y X-Y500 relation below this threshold. The corresponding mass threshold depends on redshift. Systems with M500 > 5 × 1014 MM at z > 0.5 are easily detectable with Planck. The newly-detected clusters follow the YX-Y500 relation derived from X-ray selected samples. Compared to X-ray selected clusters, the new SZ clusters have a lower X-ray luminosity on average for their mass. There is no indication of departure from standard self-similar evolution in the X-ray versus SZ scaling properties. In particular, there is no significant evolution of the YX/Y500 ratio.

AB - We present the final results from the XMM-Newton validation follow-up of new Planck galaxy cluster candidates. We observed 15 new candidates, detected with signal-to-noise ratios between 4.0 and 6.1 in the 15.5-month nominal Planck survey. The candidates were selected using ancillary data flags derived from the ROSAT All Sky Survey (RASS) and Digitized Sky Survey all-sky maps, with the aim of pushing into the low SZ flux, high-z regime and testing RASS flags as indicators of candidate reliability. Fourteen new clusters were detected by XMM-Newton, ten single clusters and two double systems. Redshifts from X-ray spectroscopy lie in the range 0.2 to 0.9, with six clusters at z > 0.5. Estimated masses (M500) range from 2.5 × 1014 to 8 × 1014 MM·. We discuss our results in the context of the full XMM-Newton validation programme, in which 51 new clusters have been detected. This includes four double and two triple systems, some of which are chance projections on the sky of clusters at different redshifts. We find thatassociation with a source from the RASS-Bright Source Catalogue is a robust indicator of the reliability of a candidate, whereas association with a source from the RASS-Faint Source Catalogue does not guarantee that the SZ candidate is a bona fide cluster. Nevertheless, most Planck clusters appear in RASS maps, with a significance greater than 2σ being a good indication that the candidate is a real cluster. Candidate validation from association with SDSS galaxy overdensity at z > 0.5 is also discussed. The full sample gives a Planck sensitivity threshold of Y500 4 × 10-4 arcmin2, with indication for Malmquist bias in the Y X-Y500 relation below this threshold. The corresponding mass threshold depends on redshift. Systems with M500 > 5 × 1014 MM at z > 0.5 are easily detectable with Planck. The newly-detected clusters follow the YX-Y500 relation derived from X-ray selected samples. Compared to X-ray selected clusters, the new SZ clusters have a lower X-ray luminosity on average for their mass. There is no indication of departure from standard self-similar evolution in the X-ray versus SZ scaling properties. In particular, there is no significant evolution of the YX/Y500 ratio.

KW - Cosmic background radiation

KW - Cosmology: observations

KW - Galaxies: clusters: general

KW - Galaxies: clusters: intracluster medium

KW - X-rays: galaxies: clusters

UR - http://www.scopus.com/inward/record.url?scp=84873682329&partnerID=8YFLogxK

U2 - 10.1051/0004-6361/201219519

DO - 10.1051/0004-6361/201219519

M3 - Article

AN - SCOPUS:84873682329

VL - 550

JO - Astronomy and Astrophysics

JF - Astronomy and Astrophysics

SN - 0004-6361

M1 - A130

ER -