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The 21-sponge H ɪ absorption survey. I. Techniques and initial results


Murray, CE and Stanimirovic, S and Goss, WM and Dickey, JM and Heiles, C and Lindner, RR and Babler, B and Pingel, NM and Lawrence, A and Jencson, J and Hennebelle, P, The 21-sponge H ɪ absorption survey. I. Techniques and initial results, The Astrophysical Journal, 804, (2) Article 89. ISSN 0004-637X (2015) [Refereed Article]


Copyright Statement

Copyright 2015 The American Astronomical Society

DOI: doi:10.1088/0004-637X/804/2/89


We present methods and results from "21 cm Spectral Line Observations of Neutral Gas with the EVLA" (21-SPONGE), a large survey for Galactic neutral hydrogen (H ɪ) absorption with the Karl G. Jansky Very Large Array (VLA). With the upgraded capabilities of the VLA, we reach median rms noise in optical depth of σT = 9 10-4 per 0.42 km s-1 channel for the 31 sources presented here. Upon completion, 21-SPONGE will be the largest H ɪ absorption survey with this high sensitivity. We discuss the observations and data reduction strategies, as well as line fitting techniques. We prove that the VLA bandpass (BP) is stable enough to detect broad, shallow lines associated with warm H ɪ, and we show that BP observations can be combined in time to reduce spectral noise. In combination with matching H ɪ emission profiles from the Arecibo Observatory (~3′.5 angular resolution), we estimate excitation (or spin) temperatures (Ts) and column densities for Gaussian components fitted to sightlines along which we detect H ɪ absorption (30/31). We measure temperatures up to Ts ~ 1500 K for individual lines, showing that we can probe the thermally unstable interstellar medium (ISM) directly. However, we detect fewer of these thermally unstable components than expected from previous observational studies. We probe a wide range in column density between ~1016 and >1021 cm-2 for individual H ɪ clouds. In addition, we reproduce the trend between cold gas fraction and average Ts found by the Kim et al. synthetic observations of a hydrodynamic ISM simulation. Finally, we compare methods for estimating Ts using H ɪ observations.

Item Details

Item Type:Refereed Article
Keywords:interstellar medium, galactic structure, radio spectroscopy, ISM: clouds, ISM: structure, radiolines: ISM
Research Division:Physical Sciences
Research Group:Astronomical sciences
Research Field:Galactic astronomy
Objective Division:Expanding Knowledge
Objective Group:Expanding knowledge
Objective Field:Expanding knowledge in the physical sciences
UTAS Author:Dickey, JM (Professor John Dickey)
ID Code:102294
Year Published:2015
Funding Support:Australian Research Council (DP110104101)
Web of Science® Times Cited:53
Deposited By:Mathematics and Physics
Deposited On:2015-08-11
Last Modified:2017-11-06
Downloads:183 View Download Statistics

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