eCite Digital Repository

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]


Preview
PDF
3Mb
  

Copyright Statement

Copyright 2017 The American Astronomical Society

DOI: doi:10.3847/1538-4357/aa5d12

Abstract

We analyze synthetic neutral hydrogen (HI) 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 HI spectral lines and estimating the properties of associated gas using the Autonomous Gaussian Decomposition (AGD) algorithm. We find that HI 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 <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 < Ts < 4000 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, ISM clouds, ISM structure, radio lines
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)
Web of Science® Times Cited:3
Deposited By:Mathematics and Physics
Deposited On:2017-11-21
Last Modified:2018-04-27
Downloads:39 View Download Statistics

Repository Staff Only: item control page