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The 21-SPONGE H I Absorption Line Survey. I. The Temperature of Galactic H I
Citation
Murray, CE and Stanimirovic, S and Goss, WM and Heiles, C and Dickey, JM and Babler, B and Kim, CG, The 21-SPONGE H I Absorption Line Survey. I. The Temperature of Galactic H I, Astrophysical Journal Supplement Series, 238, (2) Article 14. ISSN 0067-0049 (2018) [Refereed Article]
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Copyright Statement
Copyright 2018 The American Astronomical Society
DOI: doi:10.3847/1538-4365/aad81a
Abstract
We present 21 cm Spectral Line Observations of Neutral Gas with the VLA (21-SPONGE), a Karl G. Jansky Very Large Array (VLA) large project (~600 hr) for measuring the physical properties of Galactic neutral hydrogen (H I). 21-SPONGE is distinguished among previous Galactic H I studies as a result of (1) its exceptional optical depth sensitivity (στ < 10-3 per 0.42 km s-1 channel over 57 lines of sight), (2) matching 21 cm emission spectra with the highest possible angular resolution (∼ 4') from the Arecibo Observatory, and (3) detailed comparisons with numerical simulations for assessing observational biases. We autonomously decompose 21 cm spectra and derive the physical properties (i.e., spin temperature, Ts, and column density) of the cold neutral medium (CNM; Ts < 250 K), thermally unstable medium (UNM; 250 K < Ts < 1000 K), and warm neutral medium (WNM; Ts > 1000 K) simultaneously. Of the total H I mass observed, 50% is detected in both absorption and emission. The CNM makes up the majority of the absorbing gas (56% ± 10%) and 28% of the total H I mass including gas detected only in emission. We find that 20% of the total H I mass is thermally unstable (41% ± 10% of H I detected in absorption), with no significant variation with Galactic latitude. Finally, although the WNM makes up 52% of the total H I mass, we detect little evidence for WNM absorption with 1000 K < Ts < 4000 K. Following spectral modeling, we detect a stacked residual absorption feature corresponding to WNM with Ts ∼ 104 K. We conclude that excitation in excess of collisions likely produces significantly higher WNM T s than predicted by steady-state models.
Item Details
| Item Type: | Refereed Article |
|---|---|
| Keywords: | clouds, structure, radio lines, radio astronomy |
| 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 |
| UTAS Author: | Dickey, JM (Professor John Dickey) |
| ID Code: | 133228 |
| Year Published: | 2018 |
| Web of Science® Times Cited: | 13 |
| Deposited By: | Mathematics and Physics |
| Deposited On: | 2019-06-19 |
| Last Modified: | 2019-08-08 |
| Downloads: | 4 View Download Statistics |
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