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

Query : 2011A&A...536A...9P

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-Y_X relation established for X-ray selected objects, where Y_X 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

Full paper

View the references in ADS

Number of rows : 29

N	Identifier	Otype	ICRS (J2000) RA	ICRS (J2000) DEC	Mag V	Sp type	#ref 1850 - 2023	#notes
1	ACT-CL J0246.4-2033	ClG	02 46 24.9	-20 33 27		~	18	0
2	ACT-CL J0254.3-5857	ClG	02 54 17.7	-58 57 11		~	42	0
3	PLCKESZ G171.9-40.7	ClG	03 12 55	+08 22.8		~	44	0
4	RX J0359.1-7205	X	03 59 06.0	-72 05 00		~	1	0
5	PLCKESZ G286.3-38.4	ClG	03 59 12	-72 04.0		~	10	0
6	ACT-CL J0438.2-5419	ClG	04 38 17.70	-54 19 20.7		~	63	0
7	NAME LMC	G	05 23 34.6	-69 45 22	0.4	~	16993	1
8	PLCKESZ G286.6-31.3	ClG	05 31 22.3	-75 09 50		~	20	0
9	NAME LMC 2 Supergiant Shell	sh	05 41 27	-69 22.4		~	190	0
10	PLCKESZ G241.2-28.7	ClG	05 43 04	-36 01.3		~	11	0
11	PLCKESZ G271.2-31.0	ClG	05 49 16	-62 05.2		~	34	0
12	PLCKESZ G226.1-16.9	ClG	06 12 33	-19 02.4		~	2	0
13	SMACS J0723.3-7327	ClG	07 23 13.3	-73 27 25		~	99	0
14	PLCKESZ G285.6-17.2	ClG	08 43 49	-71 11.4		~	9	0
15	PLCKESZ G214.6+37.0	ClG	09 08 49	+14 38.5		~	16	0
16	PSZ1 G250.02+24.15	ClG	09 32 10	-17 38.8		~	8	0
17	PLCKESZ G272.9+48.8	ClG	11 33 14	-09 28.7		~	9	0
18	PLCKESZ G287.0+32.9	ClG	11 50 49.20	-28 04 36.5		~	70	0
19	PSZ1 G292.53+21.97	ClG	12 01 08.18	-39 54 33.0		~	9	0
20	PLCKESZ G308.3-20.2	ClG	15 18 21	-81 31.4		~	19	0
21	PLCKESZ G018.7+23.6	ClG	17 02 13	-01 00.2		~	13	0
22	NGC 6752	GlC	19 10 52.11	-59 59 04.4		~	1966	0
23	PLCKESZ G337.1-26.0	ClG	19 14 20	-59 30.8		~	7	0
24	PLCKESZ G004.5-19.5	ClG	19 16 54	-33 30.5		~	24	0
25	PLCKESZ G334.8-38.0	ClG	20 52 42	-61 12.1		~	4	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

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