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• W1762062008 abstract "We report FUSE far-UV spectroscopy of the prototypical dwarf starburst galaxy NGC 1705. These data allow us for the first time to directly probe the coronal-phase (T = a few times 105 K) gas that may dominate the radiative cooling of the supernova-heated interstellar medium (ISM) and thereby determine the dynamical evolution of the starburst-driven outflows in dwarf galaxies. We detect a broad (~100 km s-1 FWHM) and blueshifted (Δv = 77 km s-1) O VI λ1032 absorption line arising in the previously known galactic outflow. The mass and kinetic energy in the outflow we detect is dominated by the warm (T ~ 104 K) photoionized gas which is also seen through its optical line emission. The kinematics of this warm gas are compatible with a simple model of the adiabatic expansion of a superbubble driven by the collective effect of the kinetic energy supplied by supernovae in the starburst. However, the observed properties of the O VI absorption in NGC 1705 are not consistent with the simple superbubble model, in which the O VI would arise in a conductive interface inside the superbubble's outer shell. The relative outflow speed of the O VI is too high and the observed column density (log N = 14.3) is much too large. We argue that the superbubble has begun to blow out of the ISM of NGC 1705. During this blowout phase the superbubble shell accelerates and fragments. The resulting hydrodynamical interaction as hot outrushing gas flows between the cool shell fragments will create intermediate-temperature coronal gas that can produce the observed O VI absorption. For the observed flow speed of ~102 km s-1, the observed O VI column density is just what is expected for gas that has been heated and which then cools radiatively. Assuming that the coronal-phase gas is in rough pressure balance with the warm photoionized gas, we estimate a cooling rate of order ~0.1 M☉ yr-1 and ~1039 ergs s-1 in the coronal gas. The latter represents less than 10% of the supernova heating rate. Independent of the assumed pressure, the lack of observed redshifted O VI emission from the back side of the outflow leads to upper limits on the cooling rate of ≤20% of the supernova heating rate. Since the X-ray luminosity of NGC 1705 is negligible, we conclude that radiative losses are insignificant in the outflow. The outflow should therefore be able to fully blow out of the ISM of NGC 1705 and vent its metals and kinetic energy. This process has potentially important implications for the evolution of dwarf galaxies and the intergalactic medium." @default.
• W1762062008 created "2016-06-24" @default.
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• W1762062008 date "2001-06-20" @default.
• W1762062008 modified "2023-10-14" @default.
• W1762062008 title "<i>FUSE</i>Observations of Outflowing O<scp>vi</scp>in the Dwarf Starburst Galaxy NGC 1705" @default.
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• W1762062008 cites W1617597187 @default.
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• W1762062008 cites W1968547533 @default.
• W1762062008 cites W1972568206 @default.
• W1762062008 cites W1973196718 @default.
• W1762062008 cites W1975349204 @default.
• W1762062008 cites W1977209901 @default.
• W1762062008 cites W1977457396 @default.
• W1762062008 cites W1979387394 @default.
• W1762062008 cites W1982220186 @default.
• W1762062008 cites W1985321813 @default.
• W1762062008 cites W1987635305 @default.
• W1762062008 cites W1991183958 @default.
• W1762062008 cites W1992704468 @default.
• W1762062008 cites W1997083858 @default.
• W1762062008 cites W1997340230 @default.
• W1762062008 cites W1997342342 @default.
• W1762062008 cites W2004952599 @default.
• W1762062008 cites W2009802717 @default.
• W1762062008 cites W2012220297 @default.
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• W1762062008 cites W2026818795 @default.
• W1762062008 cites W2032806516 @default.
• W1762062008 cites W2035467611 @default.
• W1762062008 cites W2039241537 @default.
• W1762062008 cites W2045603377 @default.
• W1762062008 cites W2051989818 @default.
• W1762062008 cites W2054872331 @default.
• W1762062008 cites W2059037849 @default.
• W1762062008 cites W2060049590 @default.
• W1762062008 cites W2063361568 @default.
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• W1762062008 doi "https://doi.org/10.1086/321422" @default.
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