eCite Digital Repository

Calibrating the HISA temperature: Measuring the temperature of the Riegel-Crutcher cloud

Citation

Denes, H and McClure-Griffiths, NM and Dickey, JM and Dawson, JR and Murray, CE, Calibrating the HISA temperature: Measuring the temperature of the Riegel-Crutcher cloud, Monthly Notices of the Royal Astronomical Society, 479, (2) pp. 1465-1490. ISSN 0035-8711 (2018) [Refereed Article]


Preview
PDF
8Mb
  

Copyright Statement

Copyright 2018 The Authors. This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society : 2018 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved.

DOI: doi:10.1093/mnras/sty1384

Abstract

H I self-absorption (HISA) clouds are clumps of cold neutral hydrogen (H I) visible in front of warm background gas, which makes them ideal places to study the properties of the cold atomic component of the interstellar medium. The Riegel-Crutcher (R-C) cloud is the most striking HISA feature in the Galaxy. It is one of the closest HISA clouds to us and is located in the direction of the Galactic Centre, which provides a bright background. High-resolution interferometric measurements have revealed the filamentary structure of this cloud; however, it is difficult to accurately determine the temperature and the density of the gas without optical depth measurements. In this paper, we present new H I absorption observations with the Australia Telescope Compact Array against 46 continuum sources behind the R-C cloud to directly measure the optical depth of the cloud. We decompose the complex H I absorption spectra into Gaussian components using an automated machine learning algorithm. We find 300 Gaussian components, from which 67 are associated with the R-C cloud (0 < vLSR < 10 km s-1,  full width at half maximum < 10 km s-1). Combining the new H I absorption data with H I emission data from previous surveys, we calculate the spin temperature and find it to be between 20 and 80 K. Our measurements uncover a temperature gradient across the cloud with spin temperatures decreasing towards positive Galactic latitudes. We also find three new OH absorption lines associated with the cloud, which support the presence of molecular gas.

Item Details

Item Type:Refereed Article
Keywords:galaxy, local interstellar matter, 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:133229
Year Published:2018
Web of Science® Times Cited:8
Deposited By:Mathematics and Physics
Deposited On:2019-06-19
Last Modified:2019-07-23
Downloads:3 View Download Statistics

Repository Staff Only: item control page