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Recovering interstellar gas properties with Hi spectral lines: a comparison between synthetic spectra and 21-SPONGE

Citation

Murray, CE and Stanimirovic, S and Kim, C-G and Ostriker, EC and Lindner, RR and Heiles, C and Dickey, JM and Babler, B, Recovering interstellar gas properties with Hi spectral lines: a comparison between synthetic spectra and 21-SPONGE, Astrophysical Journal, 837, (1) Article 55. ISSN 0004-637X (2017) [Refereed Article]


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DOI: doi:10.3847/1538-4357/aa5d12

Abstract

We analyze synthetic neutral hydrogen (H i) absorption and emission spectral lines from a high-resolution, three-dimensional hydrodynamical simulation to quantify how well observational methods recover the physical properties of interstellar gas. We present a new method for uniformly decomposing H i spectral lines and estimating the properties of associated gas using the Autonomous Gaussian Decomposition (AGD) algorithm. We find that H i spectral lines recover physical structures in the simulation with excellent completeness at high Galactic latitude, and this completeness declines with decreasing latitude due to strong velocity-blending of spectral lines. The temperature and column density inferred from our decomposition and radiative transfer method agree with the simulated values within a factor of $\lt 2$ for the majority of gas structures. We next compare synthetic spectra with observations from the 21-SPONGE survey at the Karl G. Jansky Very Large Array using AGD. We find more components per line of sight in 21-SPONGE than in synthetic spectra, which reflects insufficient simulated gas scale heights and the limitations of local box simulations. In addition, we find a significant population of low-optical depth, broad absorption components in the synthetic data which are not seen in 21-SPONGE. This population is not obvious in integrated or per-channel diagnostics, and reflects the benefit of studying velocity-resolved components. The discrepant components correspond to the highest spin temperatures ($1000\lt {T}_{s}\lt 4000\,{\rm{K}}$), which are not seen in 21-SPONGE despite sufficient observational sensitivity. We demonstrate that our analysis method is a powerful tool for diagnosing neutral interstellar medium conditions, and future work is needed to improve observational statistics and implementation of simulated physics.

Item Details

Item Type:Refereed Article
Keywords:radio astronomy, galactic structure, interstellar medium
Research Division:Physical Sciences
Research Group:Astronomical and Space Sciences
Research Field:Galactic Astronomy
Objective Division:Expanding Knowledge
Objective Group:Expanding Knowledge
Objective Field:Expanding Knowledge in the Physical Sciences
Author:Dickey, JM (Professor John Dickey)
ID Code:122648
Year Published:2017
Funding Support:Australian Research Council (DP110104101)
Deposited By:Office of the School of Physical Sciences
Deposited On:2017-11-21
Last Modified:2017-11-22
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