J/A+A/622/A132ivo://CDS.VizieR/J/A+A/622/A132doi:10.26093/cds/vizier.36220132CDSMosenkov A.V.Baes M.Bianchi S.Casasola V.Cassara L.P.,Clark C.J.R.Davies J.De Looze I.De Vis P.Fritz J.Galametz M.,Galliano F.Jones A.P.Lianou S.Madden S. C.Nersesian A.,Smith M.W.L.Trcka A.Verstocken S.Viaene S.Vika M.Xilouris E.2026-01-20T12:11:13Z2019-02-07T09:51:50ZCDS support team

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

cds-question@unistra.frgalaxiesphotometryMost radiative transfer models assume that dust in spiral galaxies is distributed exponentially. In this paper our goal is to verify this assumption by analysing the two-dimensional large-scale distribution of dust in galaxies from the DustPedia sample. For this purpose, we have made use of Herschel imaging in five bands, from 100 to 500um, in which the cold dust constituent is primarily traced and makes up the bulk of the dust mass in spiral galaxies. For a subsample of 320 disc galaxies, we successfully performed a simultaneous fitting with a single Sersic model of the Herschel images in all five bands using the multi-band modelling code GALFITM. We report that the Sersic index n, which characterises the shape of the Sersic profile, lies systematically below 1 in all Herschel bands and is almost constant with wavelength. The average value at 250um is 0.67+/-0.37 (187 galaxies are fitted with n^250^<=0.75, 87 galaxies have 0.75<n^250^<=1.25, and 46 - with n^250^>1.25). Most observed profiles exhibit a depletion in the inner region (at r<0.3-0.4 of the optical radius r25) and are more or less exponential in the outer part. We also find breaks in the dust emission profiles at longer distances (0.5-0.6)r25 which are associated with the breaks in the optical and near-infrared. We assumed that the observed deficit of dust emission in the inner galaxy region is related to the depression in the radial profile of the HI surface density in the same region because the atomic gas reaches high enough surface densities there to be transformed into molecular gas. If a galaxy has a triggered star formation in the inner region (for example, because of a strong bar instability, which transfers the gas inwards to the centre, or a pseudobulge formation), no depletion or even an excess of dust emission in the centre is observed.2019A&A...622A.132Mhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/622/A132CatalogResearchIsServedByTAP VizieR generic servicerelated-toII/311 : WISE All-Sky Data Release (Cutri+ 2012)J/ApJS/219/4 : S4G pipeline 4: multi-component decompositions (Salo+, 2015)J/A+A/609/A37 : 875 nearby galaxies multiwavelength photometry (Clark+, 2018)J/A+A/623/A5 : DustPedia metallicities and HI masses (De Vis+, 2019)J/A+A/649/A18 : Nearby galaxy perspective on dust evolution (Galliano+, 2021)J/A+A/699/A346 : Gas and dust in DustPedia galaxies (Salvestrini+, 2025)J/A+A/620/A112 : Template SED of DustPedia galaxies (Bianchi+, 2018)http://dustpedia.astro.noa.gr : DustPedia Home Pagehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/622/A132https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/622/A132http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/622/A132https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/622/A132https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/622/A132http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/622/A132GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tap3.972892068905477e-22 6.513807192489934e-20defaultJ/A+A/622/A132/fitw1The fit results as derived from the single Sersic fitting of the WISE 3.4um data (fitw1) and supplementary data (fitw1s)recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNameGalaxy namemeta.id;meta.maincharprimarymtot[5.55/17.66]? Model magnitude WISE 3.4ummagphot.mag;meta.modelledfloatnullablere[0.01/5606.11]? Effective radiusarcsecphys.angSizefloatnullablen[0.02/20.0]? Sersic indexstat.fit.paramfloatnullableq[0.01/1.0]? Axis ratiophys.size.axisRatiofloatnullablePA[-89.8/90.0]? Position angledegpos.posAngfloatnullableHerindicates fit results as derived from the multiband single Sersic fitting of the Herschel 100-500um data in fithermeta.ref.urlcharmap[5.75/21.81]? Aperture magnitude WISE 3.4um (1)magphot.mag;em.IR.3-4umfloatnullablelogLum[1.49/10.8]? Log total luminosity (2)log(solLum)phys.luminosityfloatnullablelogMass[2.7/12.01]? Log stellar mass (3)log(solMass)phys.massfloatnullablei[0.0/90.0]? Galaxy inclination (4)degsrcfloatnullableT[-5.0/10.0]? Morphological type (5)src.morph.typefloatnullablee_T[0.1/7.1]? Uncertainty of morphological type (5)stat.errorfloatnullableSimbadNameSimbad column added by the CDSmeta.idcharJ/A+A/622/A132/fitherThe fit results as derived from the multiband single Sersic fitting of the Herschel 100-500um datarecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNameGalaxy namemeta.id;meta.maincharF100[0.26/666.3]? Model flux in PACS 100um bandJyphot.flux.density;em.IR.60-100umdoublenullablere100[0.02/338.46]? Effective radius in PACS 100um bandarcsecpos.posAngfloatnullablen100[0.01/45.21]? Sersic index in PACS 100um bandstat.fit.paramfloatnullableq100[0.07/0.98]? Axis ratio in PACS 100um bandphys.size.axisRatiofloatnullablePA100[-89.1/90.0]? Position angle in PACS 100um banddegpos.posAngfloatnullableF160[0.36/853.58]? Model flux in PACS 160um bandJyphot.flux.density;em.mm.1500-3000GHzdoublenullablere160[0.05/4740.01]? Effective radius in PACS 160um bandarcsecpos.posAngfloatnullablen160[0.01/33.55]? Sersic index in PACS 160um bandstat.fit.paramfloatnullableq160[0.07/0.98]? Axis ratio in PACS 160um bandphys.size.axisRatiofloatnullablePA160[-89.1/90.0]? Position angle in PACS 160um banddegpos.posAngfloatnullableF250[0.26/401.81]? Model flux in SPIRE 250um bandJyphot.flux.density;em.mm.750-1500GHzdoublenullablere250[0.05/381.04]? Effective radius in SPIRE 250um bandarcsecphys.angSize;em.mm.750-1500GHzfloatnullablen250[0.02/20.0]? Sersic index in SPIRE 250um bandstat.fit.paramfloatnullableq250[0.07/0.98]? Axis ratio in SPIRE 250um bandphys.size.axisRatiofloatnullablePA250[-89.1/90.0]? Position angle in SPIRE 250um banddegpos.posAngfloatnullableF350[0.195/188.08]? Model flux in SPIRE 350um bandJyphot.flux.density;em.mm.750-1500GHzdoublenullablere350[0.48/1758.74]? Effective radius in SPIRE 350um bandarcsecphys.angSize;em.mm.750-1500GHzfloatnullablen350[0.01/20.0]? Sersic index in SPIRE 350um bandstat.fit.paramfloatnullableq350[0.07/0.98]? Axis ratio in SPIRE 350um bandphys.size.axisRatiofloatnullablePA350[-89.1/90.0]? Position angle in SPIRE 350um banddegpos.posAngfloatnullableF500[0.09/72.83]? Model flux in SPIRE 500um bandJyphot.flux.density;em.mm.400-750GHzdoublenullablere500[0.03/3679.21]? Effective radius in SPIRE 500um bandarcsecphys.angSize;em.mm.400-750GHzfloatnullablen500[0.01/37.21]? Sersic index in SPIRE 500um bandstat.fit.paramfloatnullableq500[0.07/0.98]? Axis ratio in SPIRE 500um bandphys.size.axisRatiofloatnullablePA500[-89.1/90.0]? Position angle in SPIRE 500um banddegpos.posAngfloatnullablechi2nu[0.71/106.364]? Reduced chi2stat.fit.chi2floatnullable