2020
DOI: 10.3847/1538-4357/ab92a3
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Kinematics of the Magellanic Stream and Implications for Its Ionization*

Abstract: The Magellanic Stream and the Leading Arm form a massive, filamentary system of gas clouds surrounding the Large and Small Magellanic Clouds. Here we present a new component-level analysis of their ultraviolet (UV) kinematic properties using a sample of 31 sightlines through the Magellanic System observed with the Hubble Space Telescope/Cosmic Origins Spectrograph. Using Voigt-profile fits to UV metal-line absorption, we quantify the kinematic differences between the low-ion ( … Show more

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Cited by 25 publications
(25 citation statements)
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“…However, this increased radiation still cannot explain the extremely high Hα emission seen in the region of the Stream under the South Galactic Pole, which may indicate a recent Seyfert flare from the Galactic Center (Bland-Hawthorn et al 2019). The enhanced radiation field intensity at d=20 kpc would also affect the ionization level inferred from UV metal-line studies of the Stream (Fox et al 2014(Fox et al , 2020; however, the ionized/neutral ratio of ∼3:1 is distance-independent since both the neutral and ionized masses scale as d 2 .…”
Section: Resultsmentioning
confidence: 95%
“…However, this increased radiation still cannot explain the extremely high Hα emission seen in the region of the Stream under the South Galactic Pole, which may indicate a recent Seyfert flare from the Galactic Center (Bland-Hawthorn et al 2019). The enhanced radiation field intensity at d=20 kpc would also affect the ionization level inferred from UV metal-line studies of the Stream (Fox et al 2014(Fox et al , 2020; however, the ionized/neutral ratio of ∼3:1 is distance-independent since both the neutral and ionized masses scale as d 2 .…”
Section: Resultsmentioning
confidence: 95%
“…The most plausible explanation for this, so far, is recent ac-tivity from the Galactic Center. A bipolar, radiative ionization cone from a Seyfert nucleus associated with SGR A* can not only explain the elevated Hα emission but also higher hydrogen ionization fraction, higher C IV/ CII and Si IV/ Si II ratios, and high C IV and Si IV column densities along that segment of the Stream (Bland-Hawthorn et al 2013Fox et al 2020).…”
Section: Hα Emissionmentioning
confidence: 99%
“…Due to this parameter degeneracy, the predicted gas temperature within the Fermi bubbles should be considered uncertain as it depends on the amount of injected thermal energy assumed in the model. Additional observational constraints such as X-ray, UV, and radio emission/absorption lines 33,34,46,47 may be used to break the parameter degeneracy.…”
Section: Simulation Setup and Parametersmentioning
confidence: 99%