J/MNRAS/485/2825ivo://CDS.VizieR/J/MNRAS/485/2825doi:10.26093/cds/vizier.74852825CDSAlina D.Ristorcelli I.Montier L.Abdikamalov E.Juvela M.,Ferriere K.Bernard J.-P.Micelotta E.R.2025-05-22T20:15:34Z2023-10-10T15:20:58ZCDS support team

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

cds-question@unistra.frpolarimetryinterstellar-mediumextinctionradio-sourcesWe present a statistical study of the relative orientation in the plane of the sky between interstellar magnetic fields and filaments hosting cold clumps. For the first time, we consider both the density of the environment and the density contrast between the filaments and their environment. Moreover, we geometrically distinguish between the clumps and the remaining portions of the filaments. We infer the magnetic field orientations in the filaments and in their environment from the Stokes parameters, assuming optically thin conditions. Thus, we analyse the relative orientations between filaments, embedded clumps, internal and background magnetic fields, depending on their environment and evolutionary stages. We recover the previously observed trend for filaments in low column density environments to be aligned parallel to the background magnetic field; however, we find that this trend is significant only for low-contrast filaments, whereas high-contrast filaments tend to be randomly orientated with respect to the background magnetic field. Filaments in high column density environments do not globally show any preferential orientation, although low-contrast filaments alone tend to have perpendicular relative orientation with respect to the background magnetic field. For a subsample of nearby filaments, for which volume densities can be derived, we find a clear transition in the relative orientation with increasing density, at n_H_~10^3^cm^-3^, changing from mostly parallel to mostly perpendicular in the off-clump portions of filaments and from even to bimodal in clumps. Our results confirm a strong interplay between interstellar magnetic fields and filaments during their formation and evolution.2019MNRAS.485.2825Ahttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/MNRAS/485/2825CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toJ/A+A/594/A28 : Planck Catalogue of Galactic cold clumps (PGCC) (Planck+, 2016)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/MNRAS/485/2825https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/MNRAS/485/2825http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/MNRAS/485/2825https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/MNRAS/485/2825https://vizier.iucaa.in/viz-bin/votable?-source=J/MNRAS/485/2825http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/MNRAS/485/2825GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/MNRAS/485/2825/tablea1 (Characteristics of the filaments used in the study)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/MNRAS/485/2825/tablea1?https://vizier.iucaa.in/viz-bin/conesearch/J/MNRAS/485/2825/tablea1?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/MNRAS/485/2825/tablea1?GETtext/xml+votable180.050000true248.67248-15.775590.0055555555555555566/252 597 855 862 876 1067-1068 1074 1080 1082 1091 1145 1151 1167 1243 1312 1321 1344 1473 1499 1582 1612 1636 1653 1694 1812 1814 1959 1964 2807 2927 2957 2969 2972 3229 3344 3364 3386 3459 3645 3973 4037 7402 13050 13593 13665 13786 14052 14147 14350 14822 15408 15667 15685 15818 15825 15842 15955 15985 16071 16201 16217 16332 19885 20113 20204 20799 20857 20983 21308 21311 21329 21430 21440 22020 22137 22873 23167 23561 23590 23810 24014 24169 24202 24457 28863 28962 29247 29267 29317 29339 29442 29682 29884 30266 30343 30346 30733 30798 30820 30832 32121 33088 37126 37183 37234 37857 37864 37970 38573 39392 39918 41024 41031 41046 41059 41076 41128 41515 41518 41613 41644 41851 41879 41904 42564 42586 42972 43150 43339 45234 48875https://cdsarc.cds.unistra.fr/viz-bin/moc/J/MNRAS/485/2825?format=asciiRadiodefaultJ/MNRAS/485/2825/tablea1Characteristics of the filaments used in the study_RA.icrsRight ascension (ICRS) (computed by VizieR, not part of the original data. The format may include more digits than the original data because of internal accuracy requirements in VizieR and across other CDS services)degpos.eq.raindexed_DE.icrsDeclination (ICRS) (computed by VizieR, not part of the original data. The format may include more digits than the original data because of internal accuracy requirements in VizieR and across other CDS services)degpos.eq.decindexedrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintIDObject number in the Planck Galactic cold clump (PGCC) catalogue (Cat. J/A+A/594/A28/)meta.id;meta.mainintGLONGalactic longitudedegpos.galactic.lonGLATGalactic latitudedegpos.galactic.latsFilament lengtharcminsrc.morph.scLengthfloatwFilament widtharcminphys.angSizefloatPAfil2Average position angle given by the SupRHT method using Gaussian fitdegpos.posAng;meta.modelled;stat.meanfloate_PAfil2Error on PAfil2degstat.errorfloatNHtotAverage column density over the filament1e+20cm**-2phys.columnDensity;stat.meanfloate_NHtotError on NHtot1e+20cm**-2stat.errorfloatNHfilAverage column density over the filament excluding clumps areas1e+20cm**-2phys.columnDensity;stat.meanfloate_NHfilError on NHfil1e+20cm**-2stat.errorfloatNHbkgAverage column density over the background region1e+20cm**-2phys.columnDensity;obs.field;stat.meanfloate_NHbkgError on NHbkg1e+20cm**-2stat.errorfloatpsi2? Average magnetic field angle over the filament using Gaussian fitdegphys.magField;pos.angDistancefloatnullablepsi1? Average magnetic field angle over the filament using circular statisticsdegphys.magField;pos.posAngfloatnullablee_psi1? Error on psi1degstat.errorfloatnullableSimbadNameSimbad column added by the CDSmeta.idcharnullable