{ "id": "1610.01001", "version": "v1", "published": "2016-10-04T14:03:57.000Z", "updated": "2016-10-04T14:03:57.000Z", "title": "The distribution and kinematics of interstellar O~{\\small VI} in the Milky Way}", "authors": [ "Rathin Sarma", "Amit Pathak", "Jayanta Murthy", "Jayanta K. Sarma" ], "comment": "6 figures, 3 tables, accepted for publication in MNRAS", "categories": [ "astro-ph.GA" ], "abstract": "We present the results of a survey of interstellar O~{\\small VI} absorption in the Milky Way (MW) towards {69} stars in the Large Magellanic Cloud (LMC) obtained with the \\textit{Far Ultraviolet Spectroscopic Explorer (FUSE)}. The integrated MW O~{\\small VI} column densities log N(O~{\\small VI}) are in the range from 13.68 to 14.73 with a mean of {14.26$_{-0.09}^{+0.07}$} atoms cm$^{-2}$. The O~{\\small VI} exponential scale height is found to be {2.28$\\pm$1.06} kpc. The O~{\\small VI} column density correlates with the Doppler parameter $\\it b$. The O~{\\small VI} velocity dispersion ranges from {14.0 to 91.6 with an average value of 62.7 km s$^{-1}$}. These high values of velocity dispersion reveal the effect of turbulence, multiple velocity components and collision on broad O~{\\small VI} profiles. There is a significant variation of O~{\\small VI} column density on all scales studied {(0.0025$\\degr$ - 6.35$\\degr$)}. The smallest scale for which O~{\\small VI} column density variations has been found is {$\\bigtriangleup \\theta$ $\\sim$~9$\\arcsec$}. Comparison of the O~{\\small VI} velocity profiles with Fe~{\\small II} indicates the presence of intermediate velocity cloud (IVC) and/or high velocity cloud (HVC) components in the O~{\\small VI} absorption.", "revisions": [ { "version": "v1", "updated": "2016-10-04T14:03:57.000Z" } ], "analyses": { "keywords": [ "milky way", "interstellar", "distribution", "kinematics", "ultraviolet spectroscopic explorer" ], "note": { "typesetting": "TeX", "pages": 0, "language": "en", "license": "arXiv", "status": "editable" } } }