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dc.contributor.authorOh, S.H.
dc.contributor.authorBrook, C.
dc.contributor.authorGovernato, F.
dc.contributor.authorBrinks, E.
dc.contributor.authorMayer, L.
dc.contributor.authorde Blok, W.J.G.
dc.contributor.authorBrooks, A.
dc.contributor.authorWalter, F.
dc.date.accessioned2016-03-03T10:04:50Z
dc.date.available2016-03-03T10:04:50Z
dc.date.issued2011
dc.identifier.citationOh , S H , Brook , C , Governato , F , Brinks , E , Mayer , L , de Blok , W J G , Brooks , A & Walter , F 2011 , ' The central slope of dark matter cores in dwarf galaxies : simulations versus THINGS ' , The Astronomical Journal , vol. 142 , no. 1 , 24 . https://doi.org/10.1088/0004-6256/142/1/24
dc.identifier.issn0004-6256
dc.identifier.otherdspace: 2299/6043
dc.identifier.otherORCID: /0000-0002-7758-9699/work/30407823
dc.identifier.urihttp://hdl.handle.net/2299/16592
dc.description‘In these times, during the rise in the popularity of institutional repositories, the Society does not forbid authors from depositing their work in such repositories. However, the AAS regards the deposit of scholarly work in such repositories to be a decision of the individual scholar, as long as the individual's actions respect the diligence of the journals and their reviewers.’ Original article can be found at : http://iopscience.iop.org/ Copyright American Astronomical Society
dc.description.abstractWe make a direct comparison of the derived dark matter (DM) distributions between hydrodynamical simulations of dwarf galaxies assuming ACDM cosmology and the observed dwarf galaxies sample from the THINGS survey in terms of (1) the rotation curve shape and (2) the logarithmic inner density slope a of mass density profiles. The simulations, which include the effect of baryonic feedback processes, such as gas cooling, star formation, cosmic UV background heating, and most importantly, physically motivated gas outflows driven by supernovae, form bulgeless galaxies with DM cores. We show that the stellar and baryonic mass is similar to that inferred from photometric and kinematic methods for galaxies of similar circular velocity. Analyzing the simulations in exactly the same way as the observational sample allows us to address directly the so-called cusp/core problem in the ACDM model. We show that the rotation curves of the simulated dwarf galaxies rise less steeply than cold dark matter rotation curves and are consistent with those of the THINGS dwarf galaxies. The mean value of the logarithmic inner density slopes alpha of the simulated galaxies' DM density profiles is similar to-0.4 +/- 0.1, which shows good agreement with alpha = -0.29 +/- 0.07 of the THINGS dwarf galaxies. The effect of non-circular motions is not significant enough to affect the results. This confirms that the baryonic feedback processes included in the simulations are efficiently able to make the initial cusps with alpha similar to-1.0 to -1.5 predicted by DM-only simulations shallower and induce DM halos with a central mass distribution similar to that observed in nearby dwarf galaxies.en
dc.format.extent670595
dc.language.isoeng
dc.relation.ispartofThe Astronomical Journal
dc.subjectdark matter
dc.subjectgalaxies : dwarf
dc.subjectgalaxies : halos
dc.subjectgalaxies : kinematics and dynamics
dc.titleThe central slope of dark matter cores in dwarf galaxies : simulations versus THINGSen
dc.contributor.institutionSchool of Physics, Astronomy and Mathematics
dc.contributor.institutionCentre for Astrophysics Research
dc.description.statusPeer reviewed
dc.identifier.urlhttp://www.scopus.com/inward/record.url?scp=79959981100&partnerID=8YFLogxK
rioxxterms.versionofrecord10.1088/0004-6256/142/1/24
rioxxterms.typeJournal Article/Review
herts.preservation.rarelyaccessedtrue


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