J/A+A/652/A108ivo://CDS.VizieR/J/A+A/652/A108doi:10.26093/cds/vizier.36520108CDSSaponara J.Kamphuis P.Koribalski B.S.Benaglia P.2022-10-14T13:11:47Z2021-08-19T08:30:04ZCDS support team

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

cds-question@unistra.frgalaxiesh-i-line-emissionStudies of the stellar and the HI gas kinematics in dwarf and Low Surface Brightness (LSB) galaxies are essential for deriving constraints on their dark matter distribution. Moreover, a key component to unveil in the evolution of LSBs is why some of them can be classified as superthin. We aim to investigate the nature of the proto-typical superthin galaxy Fourcade-Figueroa (FF), to understand the role played by the dark matter halo in forming its superthin shape and to investigate the mechanism that explains the observed disruption in the approaching side of the galaxy. Combining new HI 21-cm observations obtained with the Giant Metrewave Radio Telescope with archival data from the Australia Telescope Compact Array we were able to obtain sensitive HI observations of the FF galaxy. These data were modeled with a 3D tilted ring model in order to derive the rotation curve and surface brightness density of the neutral hydrogen. We subsequently used this model, combined with a stellar profile from the literature, to derive the radial distribution of the dark matter in the FF galaxy. Additionally, we used a more direct measurement of the vertical HI gas distribution as a function of the galactocentric radius to determine the flaring of the gas disk. For the FF galaxy the Navarro-Frenk-White dark matter distribution provides the best fit to the observed rotation curve. However, the differences with a pseudo-isothermal halo are small. Both models indicate that the core of the dark matter halo is compact. Even though the FF galaxy classifies as superthin, the gas thickness about the galactic centre exhibits a steep flaring of the gas which is in agreement with the edge of the stellar disk. Besides, FF is clearly disrupted towards its north-west-side, clearly observed at both, optical and HI wavelengths. As suggested previously in the literature, the compact dark matter halo might be the main responsible for the superthin structure of the stellar disk in FF. This idea is strengthened through the detection of the mentioned disruption; the fact that the galaxy is disturbed also seems to support the idea that it is not isolation that cause its superthin structure.2021A&A...652A.108Shttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/652/A108CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/652/A108https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/652/A108http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/652/A108https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/652/A108https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/652/A108http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/652/A108GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/652/A108/list (Information on fits datacube)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/652/A108/list?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/652/A108/list?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/652/A108/list?GETtext/xml+votable180.050000true203.70472-45.526670.0055555555555555566/43231https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/652/A108?format=asciiRadiodefaultJ/A+A/652/A108/listInformation on fits datacuberecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintRAJ2000Right Ascension of center (J2000)degpos.eq.ra;meta.mainDEJ2000Declination of center (J2000)degpos.eq.dec;meta.mainNxNumber of pixels along X-axismeta.numberintNyNumber of pixels along Y-axismeta.numberintNzNumber of slicesmeta.numberintObs.dateObservation datestime.epoch;obsnullablebVELO-HELLower value of heliocentric velocity intervalkm/sphys.veloc;pos.heliocentricintBVELO-HELUpper value of heliocentric velocity intervalkm/sphys.veloc;pos.heliocentricintdVELO-HELHeliocentric velocity resolutionkm/sspect.resolutionintsizeSize of FITS fileKibytephys.size;meta.fitsintFileNameName of FITS file, in subdirectory fitsmeta.id;meta.fitscharTitleTitle of the FITS filemeta.title;meta.fitschar