Show simple item record

dc.contributor.authorBanerjee, Arunima
dc.contributor.authorJog, Chanda J.
dc.contributor.authorBrinks, E.
dc.contributor.authorBagetakos, Ioannis
dc.date.accessioned2011-09-22T09:01:08Z
dc.date.available2011-09-22T09:01:08Z
dc.date.issued2011-07
dc.identifier.citationBanerjee , A , Jog , C J , Brinks , E & Bagetakos , I 2011 , ' Theoretical determination of HI vertical scale heights in the dwarf galaxies DDO 154, Ho II, IC 2574 and NGC 2366 ' , Monthly Notices of the Royal Astronomical Society , vol. 415 , no. 1 , pp. 687-694 . https://doi.org/10.1111/j.1365-2966.2011.18745.x
dc.identifier.issn0035-8711
dc.identifier.otherPURE: 367841
dc.identifier.otherPURE UUID: 97308d8a-0177-4d71-90f4-087807afaff9
dc.identifier.otherWOS: 000293755000076
dc.identifier.otherScopus: 79960125649
dc.identifier.otherORCID: /0000-0002-7758-9699/work/30407819
dc.identifier.urihttp://hdl.handle.net/2299/6463
dc.descriptionThe definitive version can be found at: http://onlinelibrary.wiley.com/ Copyright Royal Astronomical Society
dc.description.abstractIn this paper, we model dwarf galaxies as a two-component system of gravitationally coupled stars and atomic hydrogen gas in the external force field of a pseudo-isothermal dark matter halo, and numerically obtain the radial distribution of HI vertical scale heights. This is done for a group of four dwarf galaxies (DDO 154, Ho II, IC 2574 and NGC 2366) for which most necessary input parameters are available from observations. The formulation of the equations takes into account the rising rotation curves generally observed in dwarf galaxies. The inclusion of self-gravity of the gas into the model at par with that of the stars results in scale heights that are smaller than what was obtained by previous authors. This is important as the gas scale height is often used for deriving other physical quantities. The inclusion of gas self-gravity is particularly relevant in the case of dwarf galaxies where the gas cannot be considered a minor perturbation to the mass distribution of the stars. We find that three out of four galaxies studied show a flaring of their HI discs with increasing radius, by a factor of a few within several disc scale lengths. The fourth galaxy has a thick HI disc throughout. This flaring arises as a result of the gas velocity dispersion remaining constant or decreasing only slightly while the disc mass distribution declines exponentially as a function of radius.en
dc.format.extent8
dc.language.isoeng
dc.relation.ispartofMonthly Notices of the Royal Astronomical Society
dc.rightsEmbargoed
dc.subjectgalaxies: dwarf
dc.subjectgalaxies: individual: IC 2574
dc.subjectgalaxies: individual: DDO 154
dc.subjectgalaxies: irregular
dc.subjectgalaxies: ISM
dc.subjectgalaxies: kinematics and dynamics
dc.titleTheoretical determination of HI vertical scale heights in the dwarf galaxies DDO 154, Ho II, IC 2574 and NGC 2366en
dc.contributor.institutionSchool of Physics, Astronomy and Mathematics
dc.contributor.institutionScience & Technology Research Institute
dc.contributor.institutionCentre for Astrophysics Research
dc.description.statusPeer reviewed
dc.date.embargoedUntil2011-12-01
dc.relation.schoolSchool of Physics, Astronomy and Mathematics
dc.description.versiontypeFinal Accepted Version
dcterms.dateAccepted2011-07
rioxxterms.versionAM
rioxxterms.versionofrecordhttps://doi.org/10.1111/j.1365-2966.2011.18745.x
rioxxterms.licenseref.startdate2011-12-01
rioxxterms.typeJournal Article/Review
herts.preservation.rarelyaccessedtrue
herts.date.embargo2011-12-01
herts.rights.accesstypeEmbargoed


Files in this item

Thumbnail

This item appears in the following Collection(s)

Show simple item record