Planck intermediate results. I. Further validation of new Planck clusters with XMM-Newton

[No Value] Planck Collaboration; 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; J.-P. Bernard; M. Bersanelli; H. Böhringer; A. Bonaldi; J. R. Bond; J. Borrill; F. R. Bouchet; H. Bourdin; M. L. Brown; C. Burigana; R. C. Butler; P. Cabella; J.-F. Cardoso; 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; P. Fosalba; M. Frailis; S. Fromenteau; S. Galeotta; K. Ganga; R. T. Génova-Santos; M. Giard; J. González-Nuevo; R. González-Riestra; K. M. Górski; A. Gregorio; A. Gruppuso; F. K. Hansen; D. Harrison; A. Hempel; C. Hernández-Monteagudo; D. Herranz; S. R. Hildebrandt; A. Hornstrup; K. M. Huffenberger; G. Hurier; T. Jagemann; J. Jasche; M. Juvela; E. Keihänen; R. Keskitalo; T. S. Kisner; R. Kneissl; J. Knoche; L. Knox; H. Kurki-Suonio; G. Lagache; A. Lähteenmäki; J.-M. Lamarre; A. Lasenby; C. R. Lawrence; S. Leach; R. Leonardi; A. Liddle; P. B. Lilje; M. López-Caniego; G. Luzzi; J. F. Macías-Pérez; D. Maino; N. Mandolesi; R. Mann; F. Marleau; D. J. Marshall; E. Martínez-González; S. Masi; M. Massardi; S. Matarrese; F. Matthai; P. Mazzotta; P. R. Meinhold; A. Melchiorri; J.-B. Melin; L. Mendes; A. Mennella; M.-A. Miville-Deschênes; A. Moneti; L. Montier; G. Morgante; D. Mortlock; D. Munshi; P. Naselsky; P. Natoli; H. U. Nørgaard-Nielsen; F. Noviello; S. Osborne; F. Pasian; G. Patanchon; O. Perdereau; F. Perrotta; F. Piacentini; E. Pierpaoli; S. Plaszczynski; P. Platania; E. Pointecouteau; G. Polenta; N. Ponthieu; L. Popa; T. Poutanen; G. W. Pratt; J.-L. Puget; J. P. Rachen; R. Rebolo; M. Reinecke; M. Remazeilles; C. Renault; S. Ricciardi; T. Riller; I. Ristorcelli; G. Rocha; 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; F. Stivoli; R. Sunyaev; D. Sutton; 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; B. D. Wandelt; J. Weller; S. D. M. White; D. Yvon; A. Zacchei; A. Zonca

Planck intermediate results. I. Further validation of new Planck clusters with XMM-Newton

[No Value] Planck Collaboration, 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, J.-P. Bernard, M. Bersanelli, H. Böhringer, A. Bonaldi, J. R. Bond, J. Borrill, F. R. BouchetH. Bourdin, M. L. Brown, C. Burigana, R. C. Butler, P. Cabella, J.-F. Cardoso, 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, P. Fosalba, M. Frailis, S. Fromenteau, S. Galeotta, K. Ganga, R. T. Génova-Santos, M. Giard, J. González-Nuevo, R. González-Riestra, K. M. Górski, A. Gregorio, A. Gruppuso, F. K. Hansen, D. Harrison, A. Hempel, C. Hernández-Monteagudo, D. Herranz, S. R. Hildebrandt, A. Hornstrup, K. M. Huffenberger, G. Hurier, T. Jagemann, J. Jasche, M. Juvela, E. Keihänen, R. Keskitalo, T. S. Kisner, R. Kneissl, J. Knoche, L. Knox, H. Kurki-Suonio, G. Lagache, A. Lähteenmäki, J.-M. Lamarre, A. Lasenby, C. R. Lawrence, S. Leach, R. Leonardi, A. Liddle, P. B. Lilje, M. López-Caniego, G. Luzzi, J. F. Macías-Pérez, D. Maino, N. Mandolesi, R. Mann, F. Marleau, D. J. Marshall, E. Martínez-González, S. Masi, M. Massardi, S. Matarrese, F. Matthai, P. Mazzotta, P. R. Meinhold, A. Melchiorri, J.-B. Melin, L. Mendes, A. Mennella, M.-A. Miville-Deschênes, A. Moneti, L. Montier, G. Morgante, D. Mortlock, D. Munshi, P. Naselsky, P. Natoli, H. U. Nørgaard-Nielsen, F. Noviello, S. Osborne, F. Pasian, G. Patanchon, O. Perdereau, F. Perrotta, F. Piacentini, E. Pierpaoli, S. Plaszczynski, P. Platania, E. Pointecouteau, G. Polenta, N. Ponthieu, L. Popa, T. Poutanen, G. W. Pratt, J.-L. Puget, J. P. Rachen, R. Rebolo, M. Reinecke, M. Remazeilles, C. Renault, S. Ricciardi, T. Riller, I. Ristorcelli, G. Rocha, 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, F. Stivoli, R. Sunyaev, D. Sutton, 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, B. D. Wandelt, 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 further results from the ongoing XMM-Newton validation follow-up of Planck cluster candidates, detailing X-ray observations of eleven candidates detected at a signal-to-noise ratio of 4.5 <S/N <5.3 in the same 10-month survey maps used in the construction of the Early SZ sample. The sample was selected in order to test internal SZ quality flags, and the pertinence of these flags is discussed in light of the validation results. Ten of the candidates are found to be bona fide clusters lying below the RASS flux limit. Redshift estimates are available for all confirmed systems via X-ray Fe-line spectroscopy. They lie in the redshift range 0.19 <z <0.94, demonstrating Planck’s capability to detect clusters up to high z. The X-ray properties of the new clusters appear to be similar to previous new detections by Planck at lower z and higher SZ flux: the majority are X-ray underluminous for their mass, estimated using YX as mass proxy, and many have a disturbed morphology. We find tentative indication for Malmquist bias in the YSZ-YX relation, with a turnover at YSZ ~ 4 × 10-4 arcmin2. We present additional new optical redshift determinations with ENO and ESO telescopes of candidates previously confirmed with XMM-Newton. The X-ray and optical redshifts for a total of 20 clusters are found to be in excellent agreement. We also show that useful lower limits can be put on cluster redshifts using X-ray data only via the use of the YX vs. YSZ and X-ray flux FX vs. YSZ relations.

Original language	English
Pages (from-to)	102
Journal	Astronomy & Astrophysics
Volume	543
Publication status	Published - 1 Jul 2012

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/2012A%26A...543A.102P

Cite this

Planck Collaboration, N. V., 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., Bernard, J.-P., Bersanelli, M., Böhringer, H., Bonaldi, A., Bond, J. R., Borrill, J., ... Zonca, A. (2012). Planck intermediate results. I. Further validation of new Planck clusters with XMM-Newton. Astronomy & Astrophysics, 543, 102. http://adsabs.harvard.edu/abs/2012A%26A...543A.102P

@article{5daba37636314f9e97c34820ff6d50b2,

title = "Planck intermediate results. I. Further validation of new Planck clusters with XMM-Newton",

abstract = "We present further results from the ongoing XMM-Newton validation follow-up of Planck cluster candidates, detailing X-ray observations of eleven candidates detected at a signal-to-noise ratio of 4.5 <S/N <5.3 in the same 10-month survey maps used in the construction of the Early SZ sample. The sample was selected in order to test internal SZ quality flags, and the pertinence of these flags is discussed in light of the validation results. Ten of the candidates are found to be bona fide clusters lying below the RASS flux limit. Redshift estimates are available for all confirmed systems via X-ray Fe-line spectroscopy. They lie in the redshift range 0.19 <z <0.94, demonstrating Planck{\textquoteright}s capability to detect clusters up to high z. The X-ray properties of the new clusters appear to be similar to previous new detections by Planck at lower z and higher SZ flux: the majority are X-ray underluminous for their mass, estimated using YX as mass proxy, and many have a disturbed morphology. We find tentative indication for Malmquist bias in the YSZ-YX relation, with a turnover at YSZ ~ 4 × 10-4 arcmin2. We present additional new optical redshift determinations with ENO and ESO telescopes of candidates previously confirmed with XMM-Newton. The X-ray and optical redshifts for a total of 20 clusters are found to be in excellent agreement. We also show that useful lower limits can be put on cluster redshifts using X-ray data only via the use of the YX vs. YSZ and X-ray flux FX vs. YSZ relations.",

keywords = "cosmology: observations, galaxies: clusters: general, galaxies: clusters: intracluster medium, cosmic background radiation, X-rays: galaxies: clusters",

author = "{Planck Collaboration}, {[No Value]} 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 J.-P. Bernard and M. Bersanelli and H. B{\"o}hringer and A. Bonaldi and Bond, {J. R.} and J. Borrill and Bouchet, {F. R.} and H. Bourdin and Brown, {M. L.} and C. Burigana and Butler, {R. C.} and P. Cabella and J.-F. Cardoso 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 P. Fosalba and M. Frailis and S. Fromenteau and S. Galeotta and K. Ganga and G{\'e}nova-Santos, {R. T.} and M. Giard 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 C. Hern{\'a}ndez-Monteagudo and D. Herranz and Hildebrandt, {S. R.} and A. Hornstrup and Huffenberger, {K. M.} and G. Hurier and T. Jagemann and J. Jasche and M. Juvela and E. Keih{\"a}nen and R. Keskitalo and Kisner, {T. S.} and R. Kneissl and J. Knoche and L. Knox and H. Kurki-Suonio and G. Lagache and A. L{\"a}hteenm{\"a}ki and J.-M. Lamarre and A. Lasenby and Lawrence, {C. R.} and S. Leach and R. Leonardi and A. Liddle and Lilje, {P. B.} 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 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 Meinhold, {P. R.} and A. Melchiorri and J.-B. Melin and L. Mendes and A. Mennella and M.-A. Miville-Desch{\^e}nes and A. Moneti and L. Montier and G. Morgante and D. Mortlock and D. Munshi and P. Naselsky and P. Natoli and N{\o}rgaard-Nielsen, {H. U.} and F. Noviello and S. Osborne and F. Pasian and G. Patanchon and O. Perdereau and F. Perrotta and F. Piacentini and E. Pierpaoli and S. Plaszczynski and P. Platania and E. Pointecouteau and G. Polenta and N. Ponthieu and L. Popa and T. Poutanen and Pratt, {G. W.} and J.-L. Puget 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 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 J.-L. Starck and F. Stivoli and R. Sunyaev and D. Sutton 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 Wandelt, {B. D.} and J. Weller and White, {S. D. M.} and D. Yvon and A. Zacchei and A. Zonca",

year = "2012",

month = jul,

day = "1",

language = "English",

volume = "543",

pages = "102",

journal = "Astronomy & Astrophysics",

issn = "0004-6361",

publisher = "EDP Sciences",

}

Planck Collaboration, NV, 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, Bernard, J-P, Bersanelli, M, Böhringer, H, Bonaldi, A, Bond, JR, Borrill, J, Bouchet, FR, Bourdin, H, Brown, ML, Burigana, C, Butler, RC, Cabella, P, Cardoso, J-F, 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, Fosalba, P, Frailis, M, Fromenteau, S, Galeotta, S, Ganga, K, Génova-Santos, RT, Giard, M, González-Nuevo, J, González-Riestra, R, Górski, KM, Gregorio, A, Gruppuso, A, Hansen, FK, Harrison, D, Hempel, A, Hernández-Monteagudo, C, Herranz, D, Hildebrandt, SR, Hornstrup, A, Huffenberger, KM, Hurier, G, Jagemann, T, Jasche, J, Juvela, M, Keihänen, E, Keskitalo, R, Kisner, TS, Kneissl, R, Knoche, J, Knox, L, Kurki-Suonio, H, Lagache, G, Lähteenmäki, A, Lamarre, J-M, Lasenby, A, Lawrence, CR, Leach, S, Leonardi, R, Liddle, A, Lilje, PB, López-Caniego, M, Luzzi, G, Macías-Pérez, JF, Maino, D, Mandolesi, N, Mann, R, Marleau, F, Marshall, DJ, Martínez-González, E, Masi, S, Massardi, M, Matarrese, S, Matthai, F, Mazzotta, P, Meinhold, PR, Melchiorri, A, Melin, J-B, Mendes, L, Mennella, A, Miville-Deschênes, M-A, Moneti, A, Montier, L, Morgante, G, Mortlock, D, Munshi, D, Naselsky, P, Natoli, P, Nørgaard-Nielsen, HU, Noviello, F, Osborne, S, Pasian, F, Patanchon, G, Perdereau, O, Perrotta, F, Piacentini, F, Pierpaoli, E, Plaszczynski, S, Platania, P, Pointecouteau, E, Polenta, G, Ponthieu, N, Popa, L, Poutanen, T, Pratt, GW, Puget, J-L, Rachen, JP, Rebolo, R, Reinecke, M, Remazeilles, M, Renault, C, Ricciardi, S, Riller, T, Ristorcelli, I, Rocha, G, Rosset, C, Rossetti, M, Rubiño-Martín, JA, Rusholme, B, Sandri, M, Savini, G, Schaefer, BM, Scott, D, Smoot, GF, Starck, J-L, Stivoli, F, Sunyaev, R, Sutton, D, Sygnet, J-F, Tauber, JA, Terenzi, L, Toffolatti, L, Tomasi, M, Tristram, M, Valenziano, L, Van Tent, B, Vielva, P, Villa, F, Vittorio, N, Wandelt, BD, Weller, J, White, SDM, Yvon, D, Zacchei, A & Zonca, A 2012, 'Planck intermediate results. I. Further validation of new Planck clusters with XMM-Newton', Astronomy & Astrophysics, vol. 543, pp. 102. <http://adsabs.harvard.edu/abs/2012A%26A...543A.102P>

TY - JOUR

T1 - Planck intermediate results. I. Further validation of new Planck clusters with XMM-Newton

AU - Planck Collaboration, [No Value]

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 - Bernard, J.-P.

AU - Bersanelli, M.

AU - Böhringer, H.

AU - Bonaldi, A.

AU - Bond, J. R.

AU - Borrill, J.

AU - Bouchet, F. R.

AU - Bourdin, H.

AU - Brown, M. L.

AU - Burigana, C.

AU - Butler, R. C.

AU - Cabella, P.

AU - Cardoso, J.-F.

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 - Fosalba, P.

AU - Frailis, M.

AU - Fromenteau, S.

AU - Galeotta, S.

AU - Ganga, K.

AU - Génova-Santos, R. T.

AU - Giard, M.

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 - Hernández-Monteagudo, C.

AU - Herranz, D.

AU - Hildebrandt, S. R.

AU - Hornstrup, A.

AU - Huffenberger, K. M.

AU - Hurier, G.

AU - Jagemann, T.

AU - Jasche, J.

AU - Juvela, M.

AU - Keihänen, E.

AU - Keskitalo, R.

AU - Kisner, T. S.

AU - Kneissl, R.

AU - Knoche, J.

AU - Knox, L.

AU - Kurki-Suonio, H.

AU - Lagache, G.

AU - Lähteenmäki, A.

AU - Lamarre, J.-M.

AU - Lasenby, A.

AU - Lawrence, C. R.

AU - Leach, S.

AU - Leonardi, R.

AU - Liddle, A.

AU - Lilje, P. B.

AU - López-Caniego, M.

AU - Luzzi, G.

AU - Macías-Pérez, J. F.

AU - Maino, D.

AU - Mandolesi, N.

AU - Mann, R.

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 - Meinhold, P. R.

AU - Melchiorri, A.

AU - Melin, J.-B.

AU - Mendes, L.

AU - Mennella, A.

AU - Miville-Deschênes, M.-A.

AU - Moneti, A.

AU - Montier, L.

AU - Morgante, G.

AU - Mortlock, D.

AU - Munshi, D.

AU - Naselsky, P.

AU - Natoli, P.

AU - Nørgaard-Nielsen, H. U.

AU - Noviello, F.

AU - Osborne, S.

AU - Pasian, F.

AU - Patanchon, G.

AU - Perdereau, O.

AU - Perrotta, F.

AU - Piacentini, F.

AU - Pierpaoli, E.

AU - Plaszczynski, S.

AU - Platania, P.

AU - Pointecouteau, E.

AU - Polenta, G.

AU - Ponthieu, N.

AU - Popa, L.

AU - Poutanen, T.

AU - Pratt, G. W.

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 - 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 - Stivoli, F.

AU - Sunyaev, R.

AU - Sutton, D.

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 - Wandelt, B. D.

AU - Weller, J.

AU - White, S. D. M.

AU - Yvon, D.

AU - Zacchei, A.

AU - Zonca, A.

PY - 2012/7/1

Y1 - 2012/7/1

N2 - We present further results from the ongoing XMM-Newton validation follow-up of Planck cluster candidates, detailing X-ray observations of eleven candidates detected at a signal-to-noise ratio of 4.5 <S/N <5.3 in the same 10-month survey maps used in the construction of the Early SZ sample. The sample was selected in order to test internal SZ quality flags, and the pertinence of these flags is discussed in light of the validation results. Ten of the candidates are found to be bona fide clusters lying below the RASS flux limit. Redshift estimates are available for all confirmed systems via X-ray Fe-line spectroscopy. They lie in the redshift range 0.19 <z <0.94, demonstrating Planck’s capability to detect clusters up to high z. The X-ray properties of the new clusters appear to be similar to previous new detections by Planck at lower z and higher SZ flux: the majority are X-ray underluminous for their mass, estimated using YX as mass proxy, and many have a disturbed morphology. We find tentative indication for Malmquist bias in the YSZ-YX relation, with a turnover at YSZ ~ 4 × 10-4 arcmin2. We present additional new optical redshift determinations with ENO and ESO telescopes of candidates previously confirmed with XMM-Newton. The X-ray and optical redshifts for a total of 20 clusters are found to be in excellent agreement. We also show that useful lower limits can be put on cluster redshifts using X-ray data only via the use of the YX vs. YSZ and X-ray flux FX vs. YSZ relations.

AB - We present further results from the ongoing XMM-Newton validation follow-up of Planck cluster candidates, detailing X-ray observations of eleven candidates detected at a signal-to-noise ratio of 4.5 <S/N <5.3 in the same 10-month survey maps used in the construction of the Early SZ sample. The sample was selected in order to test internal SZ quality flags, and the pertinence of these flags is discussed in light of the validation results. Ten of the candidates are found to be bona fide clusters lying below the RASS flux limit. Redshift estimates are available for all confirmed systems via X-ray Fe-line spectroscopy. They lie in the redshift range 0.19 <z <0.94, demonstrating Planck’s capability to detect clusters up to high z. The X-ray properties of the new clusters appear to be similar to previous new detections by Planck at lower z and higher SZ flux: the majority are X-ray underluminous for their mass, estimated using YX as mass proxy, and many have a disturbed morphology. We find tentative indication for Malmquist bias in the YSZ-YX relation, with a turnover at YSZ ~ 4 × 10-4 arcmin2. We present additional new optical redshift determinations with ENO and ESO telescopes of candidates previously confirmed with XMM-Newton. The X-ray and optical redshifts for a total of 20 clusters are found to be in excellent agreement. We also show that useful lower limits can be put on cluster redshifts using X-ray data only via the use of the YX vs. YSZ and X-ray flux FX vs. YSZ relations.

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 - 543

SP - 102

JO - Astronomy & Astrophysics

JF - Astronomy & Astrophysics

ER -

Planck intermediate results. I. Further validation of new Planck clusters with XMM-Newton

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