J/A+A/695/A101ivo://CDS.VizieR/J/A+A/695/A101doi:10.26093/cds/vizier.36950101CDSRaycheva N.Haverkorn M.Ideguchi S.Stil J.M.Sun X.Han J.L.,Carretti E.Gao X.Y.Bracco A.Clark S.E.Dickey J.M.Gaensler B.M.,Hill A.Landecker T.Ordog A.Seta A.Tahani M.Wolleben M.2025-05-21T20:02:22Z2025-03-19T09:01:52ZCDS support team

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

cds-question@unistra.frinterstellar-mediummagnetic-fieldspolarimetryFaraday tomography of broadband radio polarization surveys enables us to study magnetic fields and their interaction with the interstellar medium (ISM). Such surveys include the Global Magneto-Ionic Medium Survey (GMIMS), which covers the northern and southern hemispheres at ~300-1800MHz. In this work, we used the GMIMS High Band South (1328-1768MHz), also named the Southern Twenty-centimeter All-sky Polarization Survey (STAPS), which observes the southern sky at a resolution of 18{deg}. To extract the key parameters of the magnetized ISM from STAPS, we computed the Faraday moments of the tomographic data cubes. These moments include the total polarized intensity, the mean Faraday depth weighted by the polarized intensity, the weighted dispersion of the Faraday spectrum, and its skewness. We compared the Faraday moments to those calculated over the same frequency range in the northern sky (using the Dominion Radio Astrophysical Observatory, DRAO), in a strip of 360{deg}x30{deg} that overlaps with STAPS coverage. We find that the total polarized intensity is generally dominated by diffuse emission that decreases at longitudes of l<=300{deg}. The Faraday moments reveal a variety of polarization structures. Low-intensity regions at high latitudes usually have a single Faraday depth component. Due to its insufficiently large frequency coverage, STAPS cannot detect Faraday thick structures. Comparing the Faraday depths from STAPS to total rotation measures from extragalactic sources suggests that STAPS frequencies are high enough that the intervening ISM causes depolarization to background emission at intermediate and high Galactic latitudes. Where they overlap, the STAPS and DRAO surveys exhibit broad correspondence but differ in polarized intensity by a factor of ~1.82025A&A...695A.101Rhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/695/A101CatalogResearchIsServedByTAP VizieR generic servicerelated-toJ/A+A/694/A169 : STAPS images (Sun+, 2025)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/695/A101https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/695/A101http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/695/A101https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/695/A101https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/695/A101http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/695/A101GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapAssociated datahttps://cdsarc.cds.unistra.fr/assocdata/?obs_collection=J/A+A/695/A101defaultJ/A+A/695/A101/listList of fits mapsrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNxNumber of pixels along X-axismeta.numberintNyNumber of pixels along Y-axismeta.numberintsizeSize of FITS fileKibytephys.size;meta.fitsintFileNameName of FITS file, in subdirectory fitsmeta.id;meta.fitscharTitleTitle of the FITS filemeta.title;meta.fitschar