FN Archimer Export Format PT J TI Planck intermediate results: LV. Reliability and thermal properties of high-frequency sources in the Second Planck Catalogue of Compact Sources BT AF AKRAMI, Y. ASHDOWN, M. AUMONT, J. BACCIGALUPI, C. BALLARDINI, M. BANDAY, A. J. BARREIRO, R. B. BARTOLO, N. BASAK, S. BENABED, K. BERNARD, J-P BERSANELLI, M. BIELEWICZ, P. BOND, J. R. BORRILL, J. BOUCHET, F. R. BURIGANA, C. CALABRESE, E. CARVALHO, P. CHIANG, H. C. CRILL, B. P. CUTTAIA, F. DE ROSA, A. DE ZOTTI, G. DELABROUILLE, J. DELOUIS, Jean Marc DI VALENTINO, E. DIEGO, J. M. DUPAC, X. DUSINI, S. EFSTATHIOU, G. ELSNER, F. ENSSLIN, T. A. ERIKSEN, H. K. FERNANDEZ-COBOS, R. FINELLI, F. FRAISSE, A. A. FRANCESCHI, E. FROLOV, A. GALEOTTA, S. GANGA, K. GERBINO, M. GONZALEZ-NUEVO, J. GORSKI, K. M. GRATTON, S. GRUPPUSO, A. GUDMUNDSSON, J. E. HANDLEY, W. HANSEN, F. K. HERRANZ, D. HIVON, E. HOBSON, M. HUANG, Z. JONES, W. C. KEIHANEN, E. KESKITALO, R. KIM, J. KISNER, T. S. KRACHMALNICOFF, N. KUNZ, M. KURKI-SUONIO, H. LAMARRE, J-M LASENBY, A. LATTANZI, M. LAWRENCE, C. R. LE JEUNE, M LEVRIER, F. LILJE, P. B. LINDHOLM, V LOPEZ-CANIEGO, M. MA, Y-Z MACIAS-PEREZ, J. F. MAGGIO, G. MANDOLESI, N. MARCOS-CABALLERO, A. MARIS, M. MARTIN, PG MARTINEZ-GONZALEZ, E. MATARRESE, S. MAURI, N. MCEWEN, J. D. MIGLIACCIO, M. MOLINARI, D. MONETI, A. MONTIER, L. MORGANTE, G. NATOLI, P. PAOLETTI, D. PARTRIDGE, B. PERROTTA, F. PETTORINO, V PIACENTINI, F. POLENTA, G. PUGET, J-L RACHEN, J. P. REINECKE, M. REMAZEILLES, M. RENZI, A. ROCHA, G. ROUDIER, G. RUIZ-GRANADOS, B. SAVELAINEN, M. SCOTT, D. SIRRI, G. SPENCER, L. D. SUUR-USKI, A-S TAUBER, J. A. TAVAGNACCO, D. TENTI, M. TOFFOLATTI, L. TOMASI, M. TROMBETTI, T. VALIVIITA, J. VAN TENT, B. VIELVA, P. VILLA, F. WEHUS, I. K. ZACCHEI, A. ZONCA, A. AS 1:12,43,44;2:4,51;3:75;4:63;5:17,32;6:8,75;7:47;8:20,48;9:68;10:42,70;11:8,75;12:23,36;13:61,63;14:6;15:10,73;16:42,70;17:21,35,38;18:66;19:7;20:5,19;21:9,49;22:32;23:32;24:33;25:2;26:52;27:50;28:47;29:26;30:48;31:44,51;32:58;33:58;34:45;35:47;36:32,38;37:19;38:32;39:69;40:34;41:2;42:29;43:14;44:49,76;45:44,51;46:32,38;47:19,74;48:4,51;49:45;50:47;51:42,70;52:4;53:67;54:19;55:18;56:10;57:58;58:56;59:63;60:3,11,41;61:18,31;62:71;63:4,51;64:21,39;65:49;66:2;67:71;68:45;69:18,31;70:26;71:60,62,65;72:53;73:34;74:21,32;75:47;76:34;77:6;78:47;79:20,28,48;80:38;81:59;82:25,40;83:21,32,39;84:42,70;85:8,75;86:32;87:21,39,72;88:32,38;89:30;90:63;91:1;92:22;93:72;94:41,42;95:15;96:58;97:50;98:48;99:9,49;100:2,49,71;101:13,46;102:18,31,57;103:16;104:38;105:66;106:18,31;107:27;108:24,34;109:37;110:14,32;111:23,36;112:35,39;113:18,31;114:54,55;115:47;116:32;117:45;118:34;119:64; FF 1:;2:;3:;4:;5:;6:;7:;8:;9:;10:;11:;12:;13:;14:;15:;16:;17:;18:;19:;20:;21:;22:;23:;24:;25:;26:;27:;28:;29:;30:;31:;32:;33:;34:;35:;36:;37:;38:;39:;40:;41:;42:;43:;44:;45:;46:;47:;48:;49:;50:;51:;52:;53:;54:;55:;56:;57:;58:;59:;60:;61:;62:;63:;64:;65:;66:;67:;68:;69:;70:;71:;72:;73:;74:;75:;76:;77:;78:;79:;80:;81:;82:;83:;84:;85:;86:;87:;88:;89:;90:;91:;92:;93:;94:;95:;96:;97:;98:;99:;100:;101:;102:;103:;104:;105:;106:;107:;108:;109:;110:;111:;112:;113:;114:;115:;116:;117:;118:;119:; C1 Univ Paris Diderot, Univ Paris Saclay, Sorbonne Paris Cite, CNRS,AIM,CEA, F-91191 Gif Sur Yvette, France. 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C2 UNIV PARIS 07, FRANCE UNIV PARIS 07, FRANCE AFRICAN INST MATH SCI, SOUTH AFRICA UNIV CAMBRIDGE, UK UNIV KWAZULU NATAL, SOUTH AFRICA UNIV TORONTO, CANADA CMDLABS, UK CNRS, FRANCE CALTECH, USA LAWRENCE BERKELEY NATL LAB, USA UNIV GENEVA, SWITZERLAND ENS, FRANCE UNIV LA LAGUNA ULL, SPAIN UNIV OVIEDO, SPAIN UNIV RADBOUD NIJMEGEN, NETHERLANDS UNIV BRITISH COLUMBIA, CANADA UNIV WESTERN CAPE, SOUTH AFRICA UNIV HELSINKI, FINLAND UNIV PRINCETON, USA UNIV PADUA, ITALY UNIV FERRARA, ITALY UNIV ROMA LA SAPIENZA, ITALY UNIV MILAN, ITALY UNIV TRIESTE, ITALY UNIV ROMA TOR VERGATA, ITALY ESA, SPAIN ESTEC, NETHERLANDS INFN, ITALY ARGONNE NATL LAB, USA HAVERFORD COLL, USA UNIV HELSINKI, FINLAND CNR, ITALY INAF, ITALY INAF, ITALY INAF, ITALY INAF IASF MILANO, ITALY INFN CNAF, ITALY INFN, ITALY INFN, ITALY UNIV ROMA TOR VERGATA, ITALY UNIV PARIS SACLAY, FRANCE INST ASTROPHYS PARIS, FRANCE UNIV LEIDEN, NETHERLANDS UNIV CAMBRIDGE, UK UNIV OSLO, NORWAY INST ASTROFIS CANARIAS, SPAIN UNIV CANTABRIA, SPAIN INFN, ITALY CALTECH, USA UNIV MANCHESTER, UK KAVLI INST COSMOL CAMBRIDGE, UK CNRS, FRANCE UNIV GRENOBLE ALPES, FRANCE UNIV PARIS SUD 11, FRANCE CNRS, FRANCE LAWRENCE BERKELEY NATL LAB, USA UNIV AALTO, FINLAND MAX PLANCK INST ASTROPHYS, GERMANY UNIV COLL LONDON, UK UNIV KWAZULU NATAL, SOUTH AFRICA NATL CTR NUCL RES, POLAND PURPLE MT OBSERV, CHINA SISSA, ITALY UNIV CALIF SAN DIEGO, USA UNIV KWAZULU NATAL, SOUTH AFRICA UNIV CARDIFF, UK UNIV SUN YAT SEN, CHINA IISER, INDIA UNIV SIMON FRASER, CANADA UNIV PARIS 06, FRANCE UNIV PARIS 06, FRANCE AGENZIA SPAZIALE ITALIANA, ITALY UNIV CALIF BERKELEY, USA UNIV STOCKHOLM, SWEDEN UNIV TOULOUSE, FRANCE UNIV WARSAW OBSERV, POLAND UM LOPS IN WOS Cotutelle UMR copubli-france copubli-europe copubli-univ-france copubli-int-hors-europe copubli-sud IF 5.802 TC 1 UR https://archimer.ifremer.fr/doc/00666/77840/80013.pdf LA English DT Article DE ;catalogs;cosmology: observations;submillimeter: general AB We describe an extension of the most recent version of the Planck Catalogue of Compact Sources (PCCS2), produced using a new multi-band Bayesian Extraction and Estimation Package (BeeP). BeeP assumes that the compact sources present in PCCS2 at 857 GHz have a dust-like spectral energy distribution (SED), which leads to emission at both lower and higher frequencies, and adjusts the parameters of the source and its SED to fit the emission observed in Planck's three highest frequency channels at 353, 545, and 857 GHz, as well as the IRIS map at 3000 GHz. In order to reduce confusion regarding diffuse cirrus emission, BeeP's data model includes a description of the background emission surrounding each source, and it adjusts the confidence in the source parameter extraction based on the statistical properties of the spatial distribution of the background emission. BeeP produces the following three new sets of parameters for each source: (a) fits to a modified blackbody (MBB) thermal emission model of the source; (b) SED-independent source flux densities at each frequency considered; and (c) fits to an MBB model of the background in which the source is embedded. BeeP also calculates, for each source, a reliability parameter, which takes into account confusion due to the surrounding cirrus. This parameter can be used to extract sub-samples of high-frequency sources with statistically well-understood properties. We define a high-reliability subset (BeeP/base), containing 26 083 sources (54.1% of the total PCCS2 catalogue), the majority of which have no information on reliability in the PCCS2. We describe the characteristics of this specific high-quality subset of PCCS2 and its validation against other data sets, specifically for: the sub-sample of PCCS2 located in low-cirrus areas; the Planck Catalogue of Galactic Cold Clumps; the Herschel GAMA15-field catalogue; and the temperature- and spectral-index-reconstructed dust maps obtained with Planck's Generalized Needlet Internal Linear Combination method. The results of the BeeP extension of PCCS2, which are made publicly available via the Planck Legacy Archive, will enable the study of the thermal properties of well-defined samples of compact Galactic and extragalactic dusty sources. PY 2020 PD DEC SO Astronomy & Astrophysics SN 0004-6361 PU Edp Sciences S A VL 644 IS A99 UT 000599932200001 DI 10.1051/0004-6361/201936794 ID 77840 ER EF