2011A&A...536A...9P


C.D.S. - SIMBAD4 rel 1.7 - 2020.08.10CEST03:05:08

2011A&A...536A...9P - Astronomy and Astrophysics, volume 536A, 9-9 (2011/12-1)

Planck early results. IX. XMM-Newton follow-up for validation of Planck cluster candidates.

PLANCK COLLABORATION, ADE P.A.R., AGHANIM N., ARNAUD M., ASHDOWN M., AUMONT J., BACCIGALUPI C., BAKER M., BALBI A., BANDAY A.J., BARREIRO R.B., BARTLETT J.G., BATTANER E., BENABED K., BENNETT K., BENOIT A., BERNARD J.-P., BERSANELLI M., BHATIA R., BOCK J.J., BONALDI A., BOND J.R., BORRILL J., BOUCHET F.R., BRADSHAW T., BREMER M., BUCHER M., BURIGANA C., BUTLER R.C., CABELLA P., CANTALUPO C.M., CAPPELLINI B., CARDOSO J.-F., CARR R., CASALE M., CATALANO A., CAYON L., CHALLINOR A., CHAMBALLU A., CHARRA J., CHARY R.-R., CHIANG L.-Y., CHIANG C., CHRISTENSEN P.R., CLEMENTS D.L., COLOMBI S., COUCHOT F., COULAIS A., CRILL B.P., CRONE G., CROOK M., CUTTAIA F., DANESE L., D'ARCANGELO O., DAVIES R.D., DAVIS R.J., DE BERNARDIS P., DE BRUIN J., DE GASPERIS G., DE ROSA A., DE ZOTTI G., DELABROUILLE J., DELOUIS J.-M., DESERT F.-X., DICK J., DICKINSON C., DOLAG K., DOLE H., DONZELLI S., DORE O., DOERL U., DOUSPIS M., DUPAC X., EFSTATHIOU G., ENSSLIN T.A., ERIKSEN H.K., FINELLI F., FOLEY S., FORNI O., FOSALBA P., FRAILIS M., FRANCESCHI E., FRESCHI M., GAIER T.C., GALEOTTA S., GALLEGOS J., GANDOLFO B., GANGA K., GIARD M., GIARDINO G., GIENGER G., GIRAUD-HERAUD Y., GONZALEZ J., GONZALEZ-NUEVO J., GORSKI K.M., GRATTON S., GREGORIO A., GRUPPUSO A., GUYOT G., HAISSINSKI J., HANSEN F.K., HARRISON D., HELOU G., HENROT-VERSILLE S., HERNANDEZ-MONTEAGUDO C., HERRANZ D., HILDEBRANDT S.R., HIVON E., HOBSON M., HOLMES W.A., HORNSTRUP A., HOVEST W., HOYLAND R.J., HUFFENBERGER K.M., JAFFE A.H., JAGEMANN T., JONES W.C., JUILLET J.J., JUVELA M., KANGASLAHTI P., KEIHAENEN E., KESKITALO R., KISNER T.S., KNEISSL R., KNOX L., KRASSENBURG M., KURKI-SUONIO H., LAGACHE G., LAEHTEENMAEKI A., LAMARRE J.-M., LANGE A.E., LASENBY A., LAUREIJS R.J., LAWRENCE C.R., LEACH S., LEAHY J.P., LEONARDI R., LEROY C., LILJE P.B., LINDEN-VORNLE M., LOPEZ-CANIEGO M., LOWE S., LUBIN P.M., MACIAS-PEREZ J.F., MACIASZEK T., MacTAVISH C.J., MAFFEI B., MAINO D., MANDOLESI N., MANN R., MARIS M., MARTINEZ-GONZALEZ E., MASI S., MASSARDI M., MATARRESE S., MATTHAI F., MAZZOTTA P., McDONALD A., McGEHEE P., MEINHOLD P.R., MELCHIORRI A., MELIN J.-B., MENDES L., MENNELLA A., MEVI C., MINISCALCO R., MITRA S., MIVILLE-DESCHENES M.-A., MONETI A., MONTIER L., MORGANTE G., MORISSET N., MORTLOCK D., MUNSHI D., MURPHY A., NASELSKY P., NATOLI P., NETTERFIELD C.B., NORGAARD-NIELSEN H.U., NOVIELLO F., NOVIKOV D., NOVIKOV I., O'DWYER I.J., ORTIZ I., OSBORNE S., OSUNA P., OXBORROW C.A., PAJOT F., PALADINI R., PARTRIDGE B., PASIAN F., PASSVOGEL T., PATANCHON G., PEARSON D., PEARSON T.J., PERDEREAU O., PEROTTO L., PERROTTA F., PIACENTINI F., PIAT M., PIERPAOLI E., PLASZCZYNSKI S., PLATANIA P., POINTECOUTEAU E., POLENTA G., PONTHIEU N., POPA L., POUTANEN T., PREZEAU G., PRUNET S., PUGET J.-L., RACHEN J.P., REACH W.T., REBOLO R., REINECKE M., REIX J.-M., RENAULT C., RICCIARDI S., RILLER T., RISTORCELLI I., ROCHA G., ROSSET C., ROWAN-ROBINSON M., RUBINO-MARTIN J.A., RUSHOLME B., SALERNO E., SANDRI M., SANTOS D., SAVINI G., SCHAEFER B.M., SCOTT D., SEIFFERT M.D., SHELLARD P., SIMONETTO A., SMOOT G.F., SOZZI C., STARCK J.-L., STERNBERG J., STIVOLI F., STOLYAROV V., STOMPOR R., STRINGHETTI L., SUDIWALA R., SUNYAEV R., SYGNET J.-F., TAPIADOR D., TAUBER J.A., TAVAGNACCO D., TAYLOR D., TERENZI L., TEXIER D., TOFFOLATTI L., TOMASI M., TORRE J.-P., TRISTRAM M., TUOVINEN J., TUERLER M., TUTTLEBEE M., UMANA G., VALENZIANO L., VALIVIITA J., VARIS J., VIBERT L., VIELVA P., VILLA F., VITTORIO N., WADE L.A., WANDELT B.D., WATSON C., WHITE S.D.M., WHITE M., WILKINSON A., YVON D., ZACCHEI A. and ZONCA A.

Abstract (from CDS):

We present the XMM-Newton follow-up for confirmation of Planck cluster candidates. Twenty-five candidates have been observed to date using snapshot (∼10ks) exposures, ten as part of a pilot programme to sample a low range of signal-to-noise ratios (4<S/N<6), and a further 15 in a programme to observe a sample of S/N>5 candidates. The sensitivity and spatial resolution of XMM-Newton allows unambiguous discrimination between clusters and false candidates. The 4 false candidates have S/N≤4.1. A total of 21 candidates are confirmed as extended X-ray sources. Seventeen are single clusters, the majority of which are found to have highly irregular and disturbed morphologies (about ∼70%). The remaining four sources are multiple systems, including the unexpected discovery of a supercluster at z=0.45. For 20 sources we are able to derive a redshift estimate from the X-ray Fe K line (albeit of variable quality). The new clusters span the redshift range 0.09≲z≲0.54, with a median redshift of z∼0.37. A first determination is made of their X-ray properties including the characteristic size, which is used to improve the estimate of the SZ Compton parameter, Y500. The follow-up validation programme has helped to optimise the Planck candidate selection process. It has also provided a preview of the X-ray properties of these newly-discovered clusters, allowing comparison with their SZ properties, and to the X-ray and SZ properties of known clusters observed in the Planck survey. Our results suggest that Planck may have started to reveal a non-negligible population of massive dynamically perturbed objects that is under-represented in X-ray surveys. However, despite their particular properties, these new clusters appear to follow the Y500-YX relation established for X-ray selected objects, where YX is the product of the gas mass and temperature.

Abstract Copyright:

Journal keyword(s): cosmology: observations - galaxies: clusters: general - galaxies: clusters: intracluster medium - cosmic background radiation - X-rays: galaxies: clusters

Simbad objects: 29

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Number of rows : 29

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 PSZ1 G205.07-62.94 ClG 02 46 22 -20 31.6           ~ 12 0
2 PLCKESZ G277.75-51.73 ClG 02 54 23 -58 57.8           ~ 30 0
3 PSZ1 G171.96-40.64 ClG 03 12 55 +08 22.8           ~ 30 0
4 RX J0359.1-7205 X 03 59 06.0 -72 05 00           ~ 1 0
5 PSZ1 G286.27-38.39 ClG 03 59 12 -72 04.0           ~ 9 0
6 XMMXCS J043818.0-541917.5 ClG 04 38 17.70 -54 19 20.7           ~ 51 0
7 NAME LMC G 05 23 34.6 -69 45 22     0.4     ~ 14874 1
8 PSZ1 G286.60-31.23 ClG 05 31 22.3 -75 09 50           ~ 17 0
9 NAME LMC 2 Supergiant Shell sh 05 41 27 -69 22.4           ~ 169 0
10 PSZ1 G241.11-28.70 ClG 05 43 04 -36 01.3           ~ 7 0
11 SPT-CL J0549-6205 ClG 05 49 16 -62 05.2           ~ 26 0
12 PLCKESZ G226.1-16.9 ClG 06 12 33 -19 02.4           ~ 2 0
13 PSZ1 G284.97-23.69 ClG 07 23.2 -73 27           ~ 13 0
14 PSZ1 G285.62-17.23 ClG 08 43 49 -71 11.4           ~ 8 0
15 PLCKESZ G214.6+36.9 ClG 09 08 49 +14 38.5           ~ 4 0
16 PSZ1 G250.02+24.15 ClG 09 32 10 -17 38.8           ~ 8 0
17 PSZ1 G272.85+48.78 ClG 11 33 14 -09 28.7           ~ 8 0
18 PSZ1 G287.00+32.90 ClG 11 50 49.20 -28 04 36.5           ~ 54 0
19 PSZ1 G292.53+21.97 ClG 12 01 08.18 -39 54 33.0           ~ 9 0
20 PSZ1 G308.33-20.21 ClG 15 18 21 -81 31.4           ~ 13 0
21 PLCKESZ G018.7+23.6 ClG 17 02 13 -01 00.2           ~ 8 0
22 NGC 6752 GlC 19 10 52.11 -59 59 04.4   6.96 6.28     ~ 1811 0
23 PSZ1 G337.11-25.98 ClG 19 14 20 -59 30.8           ~ 6 0
24 PLCKESZ G004.5-19.5 ClG 19 16 54 -33 30.5           ~ 14 0
25 PLCKESZ G334.8-38.0 ClG 20 52 42 -61 12.1           ~ 3 0
26 PLCKESZ G343.4-43.4 ClG 21 20 35 -53 37.9           ~ 2 0
27 PLCKESZ G070.8-21.5 ClG 21 25 38 +19 56.5           ~ 2 0
28 PLCKESZ G100.2-30.4 ClG 23 22 21 +28 33.8           ~ 4 0
29 PLCKESZ G317.4-54.1 ClG 23 40 59 -61 02.3           ~ 2 0

    Equat.    Gal    SGal    Ecl

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2020.08.10-03:05:08

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