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

[No Value] Planck Collaboration; 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. Borgani; J. 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

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

[No Value] Planck Collaboration, 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. BondS. Borgani, J. 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

School of Physics and Astronomy

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

Abstract / Description of output

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 YX-Y500 relation below this threshold. The corresponding mass threshold depends on redshift. Systems with M500 > 5 × 1014 M⊙ 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.

Original language	English
Pages (from-to)	130
Journal	Astronomy & Astrophysics
Volume	550
Publication status	Published - 1 Feb 2013

Keywords / Materials (for Non-textual outputs)

cosmology: observations
galaxies: clusters: general
galaxies: clusters: intracluster medium
cosmic background radiation
X-rays: galaxies: clusters

Access to Document

http://adsabs.harvard.edu/abs/2013A%26A...550A.130P

Cite this

Planck Collaboration, N. V., 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., ... Zonca, A. (2013). Planck intermediate results. IV. The XMM-Newton validation programme for new Planck galaxy clusters. Astronomy & Astrophysics, 550, 130. http://adsabs.harvard.edu/abs/2013A%26A...550A.130P

@article{4f1005f6b7854b41854e6352c04f70f1,

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 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 YX-Y500 relation below this threshold. The corresponding mass threshold depends on redshift. Systems with M500 > 5 × 1014 M⊙ 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 = "cosmology: observations, galaxies: clusters: general, galaxies: clusters: intracluster medium, cosmic background radiation, X-rays: galaxies: clusters",

author = "{Planck Collaboration}, {[No Value]} and 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 J.-P. Bernard 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 R.-R. Chary and L.-Y. Chiang 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 F.-X. D{\'e}sert 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 J.-M. Lamarre 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 J.-B. Melin and L. Mendes and A. Mennella and S. Mitra and M.-A. Miville-Desch{\^e}nes 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 J.-L. Puget 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 A.-S. Suur-Uski and J.-F. Sygnet 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 = feb,

day = "1",

language = "English",

volume = "550",

pages = "130",

journal = "Astronomy & Astrophysics",

issn = "0004-6361",

publisher = "EDP Sciences",

}

Planck Collaboration, NV, 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, J-P, 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, R-R, Chiang, L-Y, 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, F-X, 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, J-M, 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, 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, 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, J-L, 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, A-S, Sygnet, J-F, 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 & Astrophysics, vol. 550, pp. 130. <http://adsabs.harvard.edu/abs/2013A%26A...550A.130P>

TY - JOUR

T1 - Planck intermediate results. IV. The XMM-Newton validation programme for new Planck galaxy clusters

AU - Planck Collaboration, [No Value]

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 - 2013/2/1

Y1 - 2013/2/1

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 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 YX-Y500 relation below this threshold. The corresponding mass threshold depends on redshift. Systems with M500 > 5 × 1014 M⊙ 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 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 YX-Y500 relation below this threshold. The corresponding mass threshold depends on redshift. Systems with M500 > 5 × 1014 M⊙ 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 - cosmology: observations

KW - galaxies: clusters: general

KW - galaxies: clusters: intracluster medium

KW - cosmic background radiation

KW - X-rays: galaxies: clusters

M3 - Article

SN - 0004-6361

VL - 550

SP - 130

JO - Astronomy & Astrophysics

JF - Astronomy & Astrophysics

ER -

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

Abstract / Description of output

Keywords / Materials (for Non-textual outputs)

Access to Document

Fingerprint

Cite this