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2014A&A...571A...6P - Astronomy and Astrophysics, volume 571A, 6-6 (2014/11-1)

Planck 2013 results. VI. High Frequency Instrument data processing.

PLANCK COLLABORATION, ADE P.A.R., AGHANIM N., ARMITAGE-CAPLAN C., ARNAUD M., ASHDOWN M., ATRIO-BARANDELA F., AUMONT J., BACCIGALUPI C., BANDAY A.J., BARREIRO R.B., BATTANER E., BENABED K., BENOIT A., BENOIT-LEVY A., BERNARD J.-P., BERSANELLI M., BIELEWICZ P., BOBIN J., BOCK J.J., BOND J.R., BORRILL J., BOUCHET F.R., BOULANGER F., BOWYER J.W., BRIDGES M., BUCHER M., BURIGANA C., CARDOSO J.-F., CATALANO A., CHAMBALLU A., CHARY R.-R., CHEN X., CHIANG H.C., CHIANG L.-Y, CHRISTENSEN P.R., CHURCH S., CLEMENTS D.L., COLOMBI S., COLOMBO L.P.L., COMBET C., COUCHOT F., COULAIS A., CRILL B.P., CURTO A., CUTTAIA F., DANESE L., DAVIES R.D., DAVIS R.J., DE BERNARDIS P., DE ROSA A., DE ZOTTI G., DELABROUILLE J., DELOUIS J.-M., DESERT F.-X., DICKINSON C., DIEGO J.M., DOLE H., DONZELLI S., DORE O., DOUSPIS M., DUNKLEY J., DUPAC X., EFSTATHIOU G., ENSSLIN T.A., ERIKSEN H.K., FINELLI F., FORNI O., FRAILIS M., FRAISSE A.A., FRANCESCHI E., GALEOTTA S., GANGA K., GIARD M., GIARDINO G., GIRARD D., GIRAUD-HERAUD Y., GONZALEZ-NUEVO J., GORSKI K.M., GRATTON S., GREGORIO A., GRUPPUSO A., GUDMUNDSSON J.E., HANSEN F.K., HANSON D., HARRISON D., HELOU G., HENROT-VERSILLE S., HERENT O., HERNANDEZ-MONTEAGUDO C., HERRANZ D., HILDEBRANDT S.R., HIVON E., HOBSON M., HOLMES W.A., HORNSTRUP A., HOU Z., HOVEST W., HUFFENBERGER K.M., HURIER G., JAFFE A.H., JAFFE T.R., JONES W.C., JUVELA M., KEIHAENEN E., KESKITALO R., KISNER T.S., KNEISSL R., KNOCHE J., KNOX L., KUNZ M., KURKI-SUONIO H., LAGACHE G., LAMARRE J.-M., LASENBY A., LAUREIJS R.J., LAWRENCE C.R., LE JEUNE M., LEONARDI R., LEROY C., LESGOURGUES J., LIGUORI M., LILJE P.B., LINDEN-VORNLE M., LOPEZ-CANIEGO M., LUBIN P.M., MACIAS-PEREZ J.F., MacTAVISH C.J., MAFFEI B., MANDOLESI N., MARIS M., MARLEAU F., MARSHALL D.J., MARTIN P.G., MARTINEZ-GONZALEZ E., MASI S., MASSARDI M., MATARRESE S., MATTHAI F., MAZZOTTA P., McGEHEE P., MEINHOLD P.R., MELCHIORRI A., MELOT F., MENDES L., MENNELLA A., MIGLIACCIO M., MITRA S., MIVILLE-DESCHENES M.-A., MONETI A., MONTIER L., MORGANTE G., MORTLOCK D., MOTTET S., MUNSHI D., MURPHY J.A., NASELSKY P., NATI F., NATOLI P., NETTERFIELD C.B., NORGAARD-NIELSEN H.U., NORTH C., NOVIELLO F., NOVIKOV D., NOVIKOV I., ORIEUX F., OSBORNE S., OXBORROW C.A., PACI F., PAGANO L., PAJOT F., PALADINI R., PAOLETTI D., PASIAN F., PATANCHON G., PERDEREAU O., PEROTTO L., PERROTTA F., PIACENTINI F., PIAT M., PIERPAOLI E., PIETROBON D., PLASZCZYNSKI S., POINTECOUTEAU E., POLENTA G., PONTHIEU N., POPA L., POUTANEN T., PRATT G.W., PREZEAU G., PRUNET S., PUGET J.-L., RACHEN J.P., RACINE B., REACH W.T., REBOLO R., REINECKE M., REMAZEILLES M., RENAULT C., RICCIARDI S., RILLER T., RISTORCELLI I., ROCHA G., ROSSET C., ROUDIER G., ROWAN-ROBINSON M., RUSHOLME B., SANSELME L., SANTOS D., SAUVE A., SAVINI G., SCOTT D., SHELLARD E.P.S., SPENCER L.D., STARCK J.-L., STOLYAROV V., STOMPOR R., SUDIWALA R., SUREAU F., SUTTON D., SUUR-USKI A.-S., SYGNET J.-F., TAUBER J.A., TAVAGNACCO D., TECHENE S., TERENZI L., TOMASI M., TRISTRAM M., TUCCI M., UMANA G., VALENZIANO L., VALIVIITA J., VAN TENT B., VIBERT L., VIELVA P., VILLA F., VITTORIO N., WADE L.A., WANDELT B.D., WHITE S.D.M., YVON D., ZACCHEI A. and ZONCA A.

Abstract (from CDS):

We describe the processing of the 531 billion raw data samples from the High Frequency Instrument (HFI), which we performed to produce six temperature maps from the first 473 days of Planck-HFI survey data. These maps provide an accurate rendition of the sky emission at 100, 143, 217, 353, 545, and 857GHz with an angular resolution ranging from 9.7' to 4.6'. The detector noise per (effective) beam solid angle is respectively, 10, 6, 12, and 39µK in the four lowest HFI frequency channels (100-353GHz) and 13 and 14kJy/sr in the 545 and 857GHz channels. Relative to the 143GHz channel, these two high frequency channels are calibrated to within 5% and the 353GHz channel to the percent level. The 100 and 217GHz channels, which together with the 143GHz channel determine the high-multipole part of the CMB power spectrum (50<l<2500), are calibrated relative to 143GHz to better than 0.2%.

Abstract Copyright:

Journal keyword(s): methods: data analysis - cosmic background radiation - cosmology: observations - surveys

Simbad objects: 7

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2019.09.21-18:10:15

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