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Ultraviolet and optical spectra of interstellar gas along the lines of sightto nearby stars have been interpreted by Redfield & Linsky (2008) and previousstudies as a set of discrete warm, partially ionized clouds each with adifferent flow vector, temperature, and metal depletion. Recently, Gry &Jenkins (2014) have proposed a fundamentally different model consisting of asingle cloud with nonrigid flows filling space out to 9 parsecs from the Sunthat they propose better describes the local ISM. Here we test thesefundamentally different morphological models against the spatially unbiasedMalamut et al. (2014) spectroscopic data set, and find that the multiple cloudmorphology model provides a better fit to both the new and old data sets. Thedetection of three or more velocity components along the lines of sight to manynearby stars, the presence of nearby scattering screens, the observed thinelongated structures of warm interstellar gas, and the likely presence ofstrong interstellar magnetic fields also support the multiple cloud model. Thedetection and identification of intercloud gas and the measurement of neutralhydrogen density in clouds beyond the Local Interstellar Cloud could providefuture morphological tests.

Evaluating the Morphology of the Local Interstellar Medium: Using New Data to Distinguish Between Multiple Discrete Clouds and a Continuous Medium