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

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

doi:10.1051/0004-6361/201118731

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

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. BourdinM. 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

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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'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 Y X as mass proxy, and many have a disturbed morphology. We find tentative indication for Malmquist bias in the Y SZ-Y X relation, with a turnover at Y SZ ~ 4 × 10 -4 arcmin 2. 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 Y X vs. Y SZ and X-ray flux F X vs. Y SZ relations. © 2012 ESO.

Original language	English
Article number	A102
Journal	Astronomy and Astrophysics
Volume	543
DOIs	https://doi.org/10.1051/0004-6361/201118731
Publication status	Published - 10 Jul 2012

Keywords

Cosmic background radiation
Cosmology: observations
Galaxies: clusters: general
Galaxies: clusters: intracluster medium
X-rays: galaxies: clusters

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10.1051/0004-6361/201118731

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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., Bouchet, F. R., ... Lilje, P. B. (2012). Planck intermediate results: I. Further validation of new Planck clusters with XMM-Newton. Astronomy and Astrophysics, 543, [A102]. https://doi.org/10.1051/0004-6361/201118731

@article{5922ebdcf52e4c8fa0b39a2f84a265c2,

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'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 Y X as mass proxy, and many have a disturbed morphology. We find tentative indication for Malmquist bias in the Y SZ-Y X relation, with a turnover at Y SZ ~ 4 × 10 -4 arcmin 2. 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 Y X vs. Y SZ and X-ray flux F X vs. Y SZ relations. {\textcopyright} 2012 ESO.",

keywords = "Cosmic background radiation, Cosmology: observations, Galaxies: clusters: general, Galaxies: clusters: intracluster medium, X-rays: galaxies: clusters",

author = "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 Bernard, {J. P.} 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 Cardoso, {J. F.} 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 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 Lamarre, {J. M.} and A. Lasenby and Lawrence, {C. R.} and S. Leach and R. Leonardi and A. Liddle and Lilje, {P. B.}",

year = "2012",

month = jul,

day = "10",

doi = "10.1051/0004-6361/201118731",

language = "English",

volume = "543",

journal = "Astronomy and Astrophysics",

issn = "0004-6361",

}

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, JP, Bersanelli, M, Böhringer, H, Bonaldi, A, Bond, JR, Borrill, J, Bouchet, FR, Bourdin, H, Brown, ML, Burigana, C, Butler, RC, Cabella, P, Cardoso, JF, 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, 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, JM, Lasenby, A, Lawrence, CR, Leach, S, Leonardi, R, Liddle, A & Lilje, PB 2012, 'Planck intermediate results: I. Further validation of new Planck clusters with XMM-Newton', Astronomy and Astrophysics, vol. 543, A102. https://doi.org/10.1051/0004-6361/201118731

TY - JOUR

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

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.

PY - 2012/7/10

Y1 - 2012/7/10

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 Y X as mass proxy, and many have a disturbed morphology. We find tentative indication for Malmquist bias in the Y SZ-Y X relation, with a turnover at Y SZ ~ 4 × 10 -4 arcmin 2. 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 Y X vs. Y SZ and X-ray flux F X vs. Y SZ relations. © 2012 ESO.

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 Y X as mass proxy, and many have a disturbed morphology. We find tentative indication for Malmquist bias in the Y SZ-Y X relation, with a turnover at Y SZ ~ 4 × 10 -4 arcmin 2. 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 Y X vs. Y SZ and X-ray flux F X vs. Y SZ relations. © 2012 ESO.

KW - Cosmic background radiation

KW - Cosmology: observations

KW - Galaxies: clusters: general

KW - Galaxies: clusters: intracluster medium

KW - X-rays: galaxies: clusters

U2 - 10.1051/0004-6361/201118731

DO - 10.1051/0004-6361/201118731

M3 - Article

VL - 543

JO - Astronomy and Astrophysics

JF - Astronomy and Astrophysics

SN - 0004-6361

M1 - A102

ER -

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

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Keywords

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