2013A&A...557A..53P

Query : 2013A&A...557A..53P

2013A&A...557A..53P - Astronomy and Astrophysics, volume 557A, 53-53 (2013/9-1)

Planck intermediate results. XII: diffuse Galactic components in the Gould Belt system.

PLANCK COLLABORATION, ADE P.A.R., AGHANIM N., ALVES M.I.R., ARNAUD M., ASHDOWN M., ATRIO-BARANDELA F., AUMONT J., BACCIGALUPI C., BALBI A., BANDAY A.J., BARREIRO R.B., BARTLETT J.G., BATTANER E., BEDINI L., BENABED K., BENOIT A., BERNARD J.-P., BERSANELLI M., BONALDI A., BOND J.R., BORRILL J., BOUCHET F.R., BOULANGER F., BURIGANA C., BUTLER R.C., CABELLA P., CARDOSO J.-F., CHEN X., CHIANG L.-Y., CHRISTENSEN P.R., CLEMENTS D.L., COLOMBI S., COLOMBO L.P.L., COULAIS A., CUTTAIA F., DAVIES R.D., DAVIS R.J., DE BERNARDIS P., DE GASPERIS G., DE ZOTTI G., DELABROUILLE J., DICKINSON C., DIEGO J.M., DOBLER G., DOLE H., DONZELLI S., DORE O., DOUSPIS M., DUPAC X., ENSSLIN T.A., FINELLI F., FORNI O., FRAILIS M., FRANCESCHI E., GALEOTTA S., GANGA K., GENOVA-SANTOS R.T., GHOSH T., GIARD M., GIARDINO G., GIRAUD-HERAUD Y., GONZALEZ-NUEVO J., GORSKI K.M., GREGORIO A., GRUPPUSO A., HANSEN F.K., HARRISON D., HERNANDEZ-MONTEAGUDO C., HILDEBRANDT S.R., HIVON E., HOBSON M., HOLMES W.A., HORNSTRUP A., HOVEST W., HUFFENBERGER K.M., JAFFE T.R., JAFFE A.H., JUVELA M., KEIHAENEN E., KESKITALO R., KISNER T.S., KNOCHE J., KUNZ M., KURKI-SUONIO H., LAGACHE G., LAEHTEENMAEKI A., LAMARRE J.-M., LASENBY A., LAWRENCE C.R., LEACH S., LEONARDI R., LILJE P.B., LINDEN-VORNLE M., LUBIN P.M., MACIAS-PEREZ J.F., MAFFEI B., MAINO D., MANDOLESI N., MARIS M., MARSHALL D.J., MARTIN P.G., MARTINEZ-GONZALEZ E., MASI S., MASSARDI M., MATARRESE S., MAZZOTTA P., MELCHIORRI A., MENNELLA A., MITRA S., MIVILLE-DESCHENES M.-A., MONETI A., MONTIER L., MORGANTE G., MORTLOCK D., MUNSHI D., MURPHY J.A., NASELSKY P., NATI F., NATOLI P., NORGAARD-NIELSEN H.U., NOVIELLO F., NOVIKOV D., NOVIKOV I., OSBORNE S., OXBORROW C.A., PAJOT F., PALADINI R., PAOLETTI D., PEEL M., PEROTTO L., PERROTTA F., PIACENTINI F., PIAT M., PIERPAOLI E., PIETROBON D., PLASZCZYNSKI S., POINTECOUTEAU E., POLENTA G., POPA L., POUTANEN T., PRATT G.W., PRUNET S., PUGET J.-L., RACHEN J.P., REACH W.T., REBOLO R., REINECKE M., RENAULT C., RICCIARDI S., RISTORCELLI I., ROCHA G., ROSSET C., RUBINO-MARTIN J.A., RUSHOLME B., SALERNO E., SANDRI M., SAVINI G., SCOTT D., SPENCER L., STOLYAROV V., SUDIWALA R., SUUR-USKI A.-S., SYGNET J.-F., TAUBER J.A., TERENZI L., TIBBS C.T., TOFFOLATTI L., TOMASI M., TRISTRAM M., VALENZIANO L., VAN TENT B., VARIS J., VIELVA P., VILLA F., VITTORIO N., WADE L.A., WANDELT B.D., YSARD N., YVON D., ZACCHEI A. and ZONCA A.

Abstract (from CDS):

We perform an analysis of the diffuse low-frequency Galactic components in the southern part of the Gould Belt system (130°≤l≤230° and -50°≤b≤-10°). Strong ultra-violet flux coming from the Gould Belt super-association is responsible for bright diffuse foregrounds that we observe from our position inside the system and that can help us improve our knowledge of the Galactic emission. Free-free emission and anomalous microwave emission (AME) are the dominant components at low frequencies (ν<40GHz), while synchrotron emission is very smooth and faint. We separated diffuse free-free emission and AME from synchrotron emission and thermal dust emission by using Planck data, complemented by ancillary data, using the correlated component analysis (CCA) component-separation method and we compared our results with the results of cross-correlation of foreground templates with the frequency maps. We estimated the electron temperature Te from Hα and free-free emission using two methods (temperature-temperature plot and cross-correlation) and obtained Te ranging from 3100 to 5200K for an effective fraction of absorbing dust along the line of sight of 30% (fd=0.3). We estimated the frequency spectrum of the diffuse AME and recovered a peak frequency (in flux density units) of 25.5±1.5GHz. We verified the reliability of this result with realistic simulations that include biases in the spectral model for the AME and in the free-free template. By combining physical models for vibrational and rotational dust emission and adding the constraints from the thermal dust spectrum from Planck and IRAS, we are able to present a good description of the AME frequency spectrum for plausible values of the local density and radiation field.

Abstract Copyright: ∼

Journal keyword(s): Galaxy: general - radio continuum: ISM - radiation mechanisms: general

Simbad objects: 9

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Number of rows : 9
N Identifier Otype ICRS (J2000)
RA 		ICRS (J2000)
DEC 		Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2024 		#notes
1 NAME NCP reg 00 00 00 +90 00.0           ~ 186 0
2 NAME Eridanus Shell sh 02 17 31 +07 49.6           ~ 50 0
3 ACO 426 ClG 03 19 47.2 +41 30 47           ~ 2257 1
4 NAME Taurus Complex SFR 04 41.0 +25 52           ~ 4415 0
5 NAME Barnard's Loop HII 05 27.5 -03 58           ~ 125 1
6 NAME Ori Complex Cld 05 35.3 -05 23           ~ 441 0
7 NAME Ophiuchus Molecular Cloud SFR 16 28 06 -24 32.5           ~ 3630 1
8 NAME Galactic Center reg 17 45 39.60213 -29 00 22.0000           ~ 14410 0
9 NAME Gould Belt PoG ~ ~           ~ 873 1

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