000202409 001__ 202409
000202409 005__ 20181203023632.0
000202409 0247_ $$2doi$$a10.1093/mnras/stu1028
000202409 022__ $$a0035-8711
000202409 02470 $$2ISI$$a000339924900003
000202409 037__ $$aARTICLE
000202409 245__ $$aThe Smith Cloud and its dark matter halo: survival of a Galactic disc passage
000202409 260__ $$bWiley-Blackwell$$c2014$$aOxford
000202409 269__ $$a2014
000202409 300__ $$a9
000202409 336__ $$aJournal Articles
000202409 520__ $$aUnder conservative assumptions about the Galaxy, the derived velocity of the Smith Cloud indicates that it will have undergone at least one passage of the Galactic disc. Using hydrodynamic simulations, we examine the present-day structure of the Smith Cloud and find that a dark matter supported cloud is able to reproduce the observed present-day neutral hydrogen mass, column density distribution and morphology. In this case, the dark matter halo becomes elongated owing to the tidal interaction with the Galactic disc. Clouds in models neglecting dark matter confinement are destroyed upon disc passage, unless the initial cloud mass is well in excess of what is observed today. We then determine integrated flux upper limits to the gamma-ray emission around such a hypothesized dark matter core in the Smith Cloud. No statistically significant core or extended gamma-ray emission are detected down to a 95 per cent confidence level upper limit of 1.4 x 10(-10) ph cm(-2) s(-1) in the 1-300 GeV energy range. For the derived distance of 12.4 kpc, the Fermi upper limits set the first tentative constraints on the dark matter cross-sections annihilating into tau(+)tau(-) and b (b) over bar for a high-velocity cloud.
000202409 6531_ $$aISM: clouds
000202409 6531_ $$aISM: individual objects: Smith Cloud
000202409 6531_ $$aGalaxy: halo
000202409 6531_ $$adark matter
000202409 6531_ $$agamma-rays: general
000202409 700__ $$0246983$$g229902$$uObserv Sauverny, EPFL, Astrophys Lab, CH-1290 Versoix, Switzerland$$aNichols, Matthew
000202409 700__ $$uUniv Complutense Madrid, Dept Fis Atom Mol & Nucl, E-28040 Madrid, Spain$$aMirabal, Nestor
000202409 700__ $$uUniv Surrey, Dept Phys, Guildford GU2 7XH, Surrey, England$$aAgertz, Oscar
000202409 700__ $$uNatl Radio Astron Observ, Green Bank, WV 24944 USA$$aLockman, Felix J.
000202409 700__ $$aBland-Hawthorn, Joss
000202409 773__ $$j442$$tMonthly Notices Of The Royal Astronomical Society$$k4$$q2883-2891
000202409 909C0 $$xU10933$$0252365$$pLASTRO
000202409 909CO $$pSB$$particle$$ooai:infoscience.tind.io:202409
000202409 917Z8 $$x103317
000202409 937__ $$aEPFL-ARTICLE-202409
000202409 973__ $$rREVIEWED$$sPUBLISHED$$aEPFL
000202409 980__ $$aARTICLE