Does the stellar distribution flare? A comparison of stellar scale heights with LAB H I data
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TL;DR: In this paper, the authors discuss recent observational evidence for stellar flaring and compare it with H I data from the Leiden/Argentine/Bonn survey and find a good agreement between both.
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Abstract: The question of whether the stellar populations in the Milky Way take part in the flaring of scale heights as observed for the H I gas is a matter of debate. Standard mass models for the Milky Way assume a constant scale height for each of the different stellar distributions. However, there is mounting evidence that at least some of the stellar distributions reach, at large galactocentric distances, high altitudes, which are incompatible with a constant scale height. We discuss recent observational evidence for stellar flaring and compare it with H I data from the Leiden/Argentine/Bonn survey. Within the systemic and statistical uncertainties we find a good agreement between both.
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Citations
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TL;DR: In this paper, the authors used positions, abundances and ages for 31 244 red giant branch stars from the Sloan Digital Sky Survey (SDSS)-APOGEE survey, spanning 3 < Rgc < 15 kpc, to dissect the disc into mono-age and mono-[Fe/H] populations at low and high [α/Fe].
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TL;DR: In this article, the authors studied two different suites of simulated galactic disks formed in the cosmological context and showed that the scale-heights of coeval populations always increase with radius.
On the formation of galactic thick disks
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TL;DR: In this article, the authors studied two different suites of simulated galactic disks formed in the cosmological context and showed that the scale-heights of coeval populations always increase with radius.
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References
Vertical distribution and support of galactic H I
TL;DR: The shape of high-latitude 21 cm H I emission profiles suggests that the local neutral interstellar medium is supported in the Galactic gravitational potential primarily by turbulence, that is, by the motion of individual clouds as mentioned in this paper.
Galaxy Disks
TL;DR: The formation and evolution of galactic disks is particularly important for understanding how galaxies form and evolve, and the cause of the variety in which they appear to us Ongoing large surveys, made possible by new instrumentation at wavelengths from the ultraviolet (GALEX), via optical (HST and large ground-based telescopes) and infrared (Spitzer) to the radio are providing much new information about disk galaxies over a wide range of redshift Although progress has been made, the dynamics and structure of stellar disks including their truncations, are still not well understood.
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TL;DR: In this article, the authors present simple analytical approximations that allow for an efficient search through the vastness of parameter space, and apply this approximation to investigate the consequences of the uncertain gaseous velocity dispersion (σg) on the constraints imposed by the thickness of the Milky Way's gas layer.
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TL;DR: In this paper, the authors used the star count model of Ortiz & Lepine to perform an unprecedented exploration of the most important Galactic parameters comparing the predicted counts with the observed star counts in the J, H, and KS bands for a grid of positions covering the whole sky.
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