2013A&A...554A.139P

Query : 2013A&A...554A.139P

2013A&A...554A.139P - Astronomy and Astrophysics, volume 554A139-139 (2013/6-1)

Planck intermediate results. IX. Detection of the Galactic haze with Planck.

PLANCK COLLABORATION, ADE P.A.R., AGHANIM N., ARNAUD M., ASHDOWN M., ATRIO-BARANDELA F., AUMONT J., BACCIGALUPI C., BALBI A., BANDAY A.J., BARREIRO R.B., BARTLETT J.G., BATTANER E., BENABED K., BENOIT A., BERNARD J.-P., BERSANELLI M., BONALDI A., BOND J.R., BORRILL J., BOUCHET F.R., BURIGANA C., CABELLA P., CARDOSO J.-F., CATALANO A., CAYON L., CHARY R.-R., CHIANG L.-Y., CHRISTENSEN P.R., CLEMENTS D.L., COLOMBO L.P.L., COULAIS A., CRILL B.P., CUTTAIA F., DANESE L., D'ARCANGELO O., DAVIS R.J., DE BERNARDIS P., DE GASPERIS G., DE ROSA A., DE ZOTTI G., DELABROUILLE J., DICKINSON C., DIEGO J.M., DOBLER G., DOLE H., DONZELLI S., DORE O., DOERL U., DOUSPIS M., DUPAC X., EFSTATHIOU G., ENSSLIN T.A., ERIKSEN H.K., FINELLI F., FORNI O., FRAILIS M., FRANCESCHI E., GALEOTTA S., GANGA K., GIARD M., GIARDINO G., GONZALEZ-NUEVO J., GORSKI K.M., GRATTON S., GREGORIO A., GRUPPUSO A., HANSEN F.K., HARRISON D., HELOU G., HENROT-VERSILLE S., HERNANDEZ-MONTEAGUDO C., HILDEBRANDT S.R., HIVON E., HOBSON M., HOLMES W.A., HORNSTRUP A., HOVEST W., HUFFENBERGER K.M., JAFFE T.R., JAGEMANN T., JEWELL J., JONES W.C., JUVELA M., KEIHAENEN E., KNOCHE J., KNOX L., 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., LOPEZ-CANIEGO 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., MATTHAI F., MAZZOTTA P., MEINHOLD P.R., MELCHIORRI A., MENDES L., MENNELLA A., MITRA S., MONETI A., MONTIER L., MORGANTE G., MUNSHI D., MURPHY J.A., NASELSKY P., NATOLI P., NORGAARD-NIELSEN H.U., NOVIELLO F., NOVIKOV D., NOVIKOV I., OSBORNE S., PAJOT F., PALADINI R., PAOLETTI D., PARTRIDGE B., PEARSON T.J., PERDEREAU O., 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., PRUNET S., PUGET J.-L., RACHEN J.P., REBOLO R., REINECKE M., RENAULT C., RICCIARDI S., RILLER T., RISTORCELLI I., ROCHA G., ROSSET C., RUBINO-MARTIN J.A., RUSHOLME B., SANDRI M., SAVINI G., SCHAEFER B.M., SCOTT D., SMOOT G.F., SPENCER L., STIVOLI F., SUDIWALA R., SUUR-USKI A.-S., SYGNET J.-F., TAUBER J.A., TERENZI L., TOFFOLATTI L., TOMASI M., TRISTRAM M., TUERLER M., UMANA G., VALENZIANO L., VAN TENT B., VIELVA P., VILLA F., VITTORIO N., WADE L.A., WANDELT B.D., WHITE M., YVON D., ZACCHEI A. and ZONCA A.

Abstract (from CDS):

Using precise full-sky observations from Planck, and applying several methods of component separation, we identify and characterise the emission from the Galactic ``haze'' at microwave wavelengths. The haze is a distinct component of diffuse Galactic emission, roughly centered on the Galactic centre, and extends to |b|∼35-50° in Galactic latitude and |l|∼15-20° in longitude. By combining the Planck data with observations from the Wilkinson Microwave Anisotropy Probe, we were able to determine the spectrum of this emission to high accuracy, unhindered by the strong systematic biases present in previous analyses. The derived spectrum is consistent with power-law emission with a spectral index of -2.56±0.05, thus excluding free-free emission as the source and instead favouring hard-spectrum synchrotron radiation from an electron population with a spectrum (number density per energy) dN/dE∝E–2.1. At Galactic latitudes |b|<30°, the microwave haze morphology is consistent with that of the Fermi gamma-ray ``haze'' or ``bubbles'', while at b~-50° we have identified an edge in the microwave haze that is spatially coincident with the edge in the gamma-ray bubbles. Taken together, this indicates that we have a multi-wavelength view of a distinct component of our Galaxy. Given both the very hard spectrum and the extended nature of the emission, it is highly unlikely that the haze electrons result from supernova shocks in the Galactic disk. Instead, a new astrophysical mechanism for cosmic-ray acceleration in the inner Galaxy is implied.

Abstract Copyright: ∼

Journal keyword(s): Galaxy: nucleus - ISM: structure - ISM: bubbles - radio continuum: ISM

Simbad objects: 11

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Number of rows : 11
N Identifier Otype ICRS (J2000)
RA 		ICRS (J2000)
DEC 		Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2026 		#notes
1 M 31 AGN 00 42 44.330 +41 16 07.50 4.86 4.36 3.44     ~ 13622 1
2 NAME Magellanic Clouds GrG 03 00 -71.0           ~ 7988 0
3 NAME Barnard's Loop HII 05 27.5 -03 58           ~ 131 1
4 NAME GUM Nebula ISM 07 43 -42.1           ~ 454 1
5 NAME Centaurus A BLL 13 25 27.61521044 -43 01 08.8050291   8.18 6.84 6.66   ~ 4774 3
6 NAME Loop I SR? 15 01 -38.7           ~ 414 2
7 NAME Ophiuchus Molecular Cloud SFR 16 28 06 -24 32.5           ~ 3969 1
8 NAME zet Oph Cloud Cld 16 37 09 -10 34.0           ~ 114 0
9 NAME Fermi Bubbles bub 17 45 -29.0           ~ 525 0
10 NAME Galactic Center reg 17 45 39.60213 -29 00 22.0000           ~ 16269 0
11 NAME Gould Belt PoG ~ ~           ~ 956 1

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