Planck intermediate results. IV. The XMM-Newton validation programme for new Planck galaxy clusters
Articolo
Data di Pubblicazione:
2013
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&sun;. 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 2sigma 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&sun; 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.
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&sun;. 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 2sigma 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&sun; 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.
Tipologia CRIS:
1.1 Articolo in rivista
Keywords:
cosmology: observations; galaxies: clusters: general; galaxies: clusters: intracluster medium; cosmic background radiation; X-rays: galaxies: clusters
Elenco autori:
P., Collaboration; P. A., R.; 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., Beno�t; J., Bernard; M., Bersanelli; I., Bikmaev; H., B�hringer; 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., Cay�n; A., Chamballu; R., Chary; L., Chiang; G., Chon; P. R., Christensen; D. L., Clements; S., Colafrancesco; S., Colombi; A., Coulais; B. P., Crill; F., Cuttaia; A. D., Silva; H., Dahle; R. J., Davis; P. d., Bernardis; G. d., Gasperis; G. d., Zotti; J., Delabrouille; J., D�mocl�s; F., D�sert; J. M., Diego; K., Dolag; H., Dole; S., Donzelli; O., Dor�; M., Douspis; X., Dupac; T. A., En�lin; H. K., Eriksen; F., Finelli; I., Flores Cacho; O., Forni; M., Frailis; E., Franceschi; M., Frommert; S., Galeotta; K., Ganga; R. T., G�nova Santos; Y., Giraud H�raud; J., Gonz�lez Nuevo; R., Gonz�lez Riestra; K. M., G�rski; A., Gregorio; A., Gruppuso; F. K., Hansen; D., Harrison; A., Hempel; S., Henrot Versill�; C., Hern�ndez 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., Lamarre; A., Lasenby; C. R., Lawrence; M. L., Jeune; S., Leach; R., Leonardi; A., Liddle; P. B., Lilje; M., Linden V�rnle; M., L�pez Caniego; G., Luzzi; J. F., Mac�as P�rez; D., Maino; N., Mandolesi; R., Mann; M., Maris; F., Marleau; D. J., Marshall; E., Mart�nez Gonz�lez; S., Masi; M., Massardi; S., Matarrese; P., Mazzotta; S., Mei; P. R., Meinhold; A., Melchiorri; J., Melin; L., Mendes; A., Mennella; S., Mitra; M., Miville Desch�nes; A., Moneti; G., Morgante; D., Mortlock; D., Munshi; P., Naselsky; F., Nati; P., Natoli; H. U., N�rgaard 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., Puget; M., Reinecke; M., Remazeilles; C., Renault; S., Ricciardi; G., Rocha; C., Rosset; M., Rossetti; Mart�n, J. A. Rubi�o.; B., Rusholme; M., Sandri; G., Savini; D., Scott; G. F., Smoot; A., Stanford; F., Stivoli; R., Sudiwala; R., Sunyaev; D., Sutton; A., Suur Uski; J., Sygnet; J. A., Tauber; Terenzi, Luca; L., Toffolatti; M., Tomasi; M., Tristram; L., Valenziano; B. V., Tent; P., Vielva; F., Villa; N., Vittorio; L. A., Wade; B. D., Wandelt; N., Welikala; J., Weller; S. D., M.; D., Yvon; A., Zacchei; A., Zonca
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