J/A+A/565/A103ivo://CDS.VizieR/J/A+A/565/A103doi:10.26093/cds/vizier.35650103CDSPlanck CollaborationAde P.A.R.Aghanim N.Alves M.I.R.Arnaud M.,Atrio-Barandela F.Aumont J.Baccigalupi C.Banday A.J.Barreiro R.B.,Battaner E.Benabed K.Benoit-Levy A.Bernard J.-P.Bersanelli M.,Bielewicz P.Bobin J.Bonaldi A.Bond J.R.Borrill J.Bouchet F.R.,Boulanger F.Burigana C.Cardoso J.-F.Casassus S.Catalano A.,Chamballu A.Chen X.Chiang H.C.Chiang L.-Y.Christensen P.R.,Clements D.L.Colombi S.Colombo L.P.L.Couchot F.Crill B.P.,Cuttaia F.Danese L.Davies R.D.Davis R.J.De Bernardis P.,De Rosa A.De Zotti G.Delabrouille J.Desert F.-X.Dickinson C.,Diego J.M.Donzelli S.Dore O.Dupac X.Ensslin T.A.Eriksen H.K.,Finelli F.Forni O.Franceschi E.Galeotta S.Ganga K.,Genova-Santos R.T.Ghosh T.Giard M.Gonzalez-Nuevo J.Gorski K.M.,Gregorio A.Gruppuso A.Hansen F.K.Harrison D.L.Helou G.,Hernandez-Monteagudo C.Hildebrandt S.R.Hivon E.Hobson M.,Hornstrup A.Jaffe A.H.Jaffe T.R.Jones W.C.Keihaenen E.,Keskitalo R.Kneissl R.Knoche J.Kunz M.Kurki-Suonio H.,Laehteenmaeki A.Lamarre J.-M.Lasenby A.Lawrence C.R.Leonardi R.,Liguori M.Lilje P.B.Linden-Vornle M.Lopez-Caniego M.,Macias-Perez J.F.Maffei B.Maino D.Mandolesi N.Marshall D.J.,Martin P.G.Martinez-Gonzalez E.Masi S.Massardi M.Matarrese S.,Mazzotta P.Meinhold P.R.Melchiorri A.Mendes L.Mennella A.,Migliaccio M.Miville-Deschenes M.-A.Moneti A.Montier L.Morgante G.,Mortlock D.Munshi D.Naselsky P.Nati F.Natoli P.,Norgaard-Nielsen H.U.Noviello F.Novikov D.Novikov I.Oxborrow C.A.,Pagano L.Pajot F.Paladini R.Paoletti D.Patanchon G.Pearson T.J.,Peel M.Perdereau O.Perrotta F.Piacentini F.Piat M.Pierpaoli E.,Pietrobon D.Plaszczynski S.Pointecouteau E.Polenta G.Ponthieu N.,Popa L.Pratt G.W.Prunet S.Puget J.-L.Rachen J.P.Rebolo R.,Reich W.Reinecke M.Remazeilles M.Renault C.Ricciardi S.Riller T.,Ristorcelli I.Rocha G.Rosset C.Roudier G.Rubino-Martin J.A.,Rusholme B.Sandri M.Savini G.Scott D.Spencer L.D.Stolyarov V.,Sutton D.Suur-Uski A.-S.Sygnet J.-F.Tauber J.A.Tavagnacco D.,Terenzi L.Tibbs C.T.Toffolatti L.Tomasi M.Tristram M.Tucci M.,Valenziano L.Valiviita J.Van Tent B.Varis J.Verstraete L.,Vielva P.Villa F.Wandelt B.D.Watson R.Wilkinson A.Ysard N.,Yvon D.Zacchei A.Zonca A.2014-09-24T13:26:20Z2014-09-09T11:57:05ZCDS support team

CDS, Observatoire de Strasbourg, 11 rue de l'Universite, F-67000 Strasbourg, France

cds-question@unistra.frh-ii-regionsradio-continuum-emissionAnomalous microwave emission (AME) is believed to be due to electric dipole radiation from small spinning dust grains. The aim of this paper is a statistical study of the basic properties of AME regions and the environment in which they emit. We used WMAP and Planck maps, combined with ancillary radio and IR data, to construct a sample of 98 candidate AME sources, assembling SEDs for each source using aperture photometry on 1{deg}-smoothed maps from 0.408GHz up to 3000GHz. Each spectrum is fitted with a simple model of free-free, synchrotron (where necessary), cosmic microwave background (CMB), thermal dust, and spinning dust components. We find that 42 of the 98 sources have significant (>5{sigma}) excess emission at frequencies between 20 and 60GHz. An analysis of the potential contribution of optically thick free-free emission from ultra-compact HII regions, using IR colour criteria, reduces the significant AME sample to 27 regions. The spectrum of the AME is consistent with model spectra of spinning dust. Peak frequencies are in the range 20-35GHz except for the California nebula (NGC1499), which appears to have a high spinning dust peak frequency of (50+/-17)GHz. The AME regions tend to be more spatially extended than regions with little or no AME. The AME intensity is strongly correlated with the sub-millimetre/IR flux densities and comparable to previous AME detections in the literature. AME emissivity, defined as the ratio of AME to dust optical depth, varies by an order of magnitude for the AME regions. The AME regions tend to be associated with cooler dust in the range 14-20K and an average emissivity index, {beta}_d_, of +1.8, while the non-AME regions are typically warmer, at 20-27K. In agreement with previous studies, the AME emissivity appears to decrease with increasing column density. This supports the idea of AME originating from small grains that are known to be depleted in dense regions, probably due to coagulation onto larger grains. We also find a correlation between the AME emissivity (and to a lesser degree the spinning dust peak frequency) and the intensity of the interstellar radiation field, G_0_. Modelling of this trend suggests that both radiative and collisional excitation are important for the spinning dust emission. The most significant AME regions tend to have relatively less ionized gas (free-free emission), although this could be a selection effect. The infrared excess, a measure of the heating of dust associated with HII regions, is typically >4 for AME sources, indicating that the dust is not primarily heated by hot OB stars. The AME regions are associated with known dark nebulae and have higher 12{mu}m/25{mu}m ratios. The emerging picture is that the bulk of the AME is coming from the polycyclic aromatic hydrocarbons and small dust grains from the colder neutral interstellar medium phase.2014A&A...565A.103Phttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/565/A103CatalogResearchIsServedByTAP VizieR generic servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/565/A103https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/565/A103http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/565/A103https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/565/A103https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/565/A103http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/565/A103GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tap1.8818037326910254e-23 1.8818037326910254e-23RadiodefaultJ/A+A/565/A103/table3*List of 98 candidate anomalous microwave emission (AME) regionsrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNameRegion name (GLLL.ll+BB.bb)meta.id;obs.fieldcharf_Name[*] * for regions that show significant (>5{sigma}) AME, except for those with a high potential UCHII contribution (fmax>0.25)meta.codecharn_Name[abc ] Detection method (1)meta.notecharl_thetaLimit flag on thetameta.code.error;pos.posAngcharthetaFWHM deconvolved size {theta}degphys.angSizefloate_theta? rms uncertainty on thetadegstat.error;pos.posAngfloatnullableEMffEffective emission measure integrated over the aperturepc.cm**-6phys.angSize;instr.fovfloate_EMffrms uncertainty on EMffpc.cm**-6stat.errorfloattau250[0/47] Dust optical depth at 250{mu}m (4)phys.absorption.opticalDepthfloate_tau250rms uncertainty on tau250stat.errorfloatTd[13/27] Dust temperature (4)Kphys.temperaturefloate_Tdrms uncertainty on TdKstat.errorfloatbetad[1.3/2.4] Dust emissivity index {beta}_d_ (4)stat.fit.paramfloate_betadrms uncertainty on betadstat.errorfloatDTcmbCMB fluctuation temperature {Delta}T_CMB_uKstat.fit.paraminte_DTcmbrms uncertainty on DTcmbuKstat.errorintAspAnomalous microwave emission (AME) amplitude1e+20cm**-2phot.flux;arith.ratiofloate_Asp? rms uncertainty on Asp1e+20cm**-2stat.errorfloatnullablen_Asp[+] + when Asp fixed at zero (see Sect. 3.5)meta.notecharsigma[0.2/30]? AME significance ({sigma}_AME_)stat.fit.goodnessfloatnullablenusp? Dust peak frequency {nu}_sp_ (2)GHzem.freqfloatnullablee_nusp? rms uncertainty on nusp (2)GHzstat.errorfloatnullablefmax[0/6]? Ultra-Compact HII region contribution f_max_(UCHII)(=S_max_(UCHII)/S_resid_(28.4))stat.fit.paramfloatnullableG0[0.2/11.2] G_0_, relative strength of the Interstellar Radiation Field (IRSF) (G_0_=1 corresponds to 1.2{mu}W/m^2^)stat.fit.paramfloate_G0rms uncertainty on G0stat.errorfloatS28.4AME residual flux density at 28.4GHz (S_resid_(28.4))Jyphot.flux.density;em.IR.15-30umfloate_S28.4rms uncertainty on S28.4Jystat.errorfloatRatioRatio of AME flux density at 28.4GHz to 100um (3THz) flux density (S_resid_^24.8^/S_100um_)phot.flux;arith.ratiofloate_Ratiorms uncertainty on Ratiostat.error;arith.ratiofloatchi2r[0/2.6] Reduced {chi}^2^stat.fit.chi2floatNotesMolecular cloud name and notesmeta.notecharr_NotesReference for Notes (3)meta.ref;pos.framechar