Phillips, J. P.; White, Glenn J.; Richardson, K. J. and Williams, P. M.
|Google Scholar:||Look up in Google Scholar|
Spectra were obtained of W51-IRS2 in the wavelength ranges 2.95-3.5 μm, and 3.99-4.1 μm. These show the presence of the Pf epsilon and Br alpha recombination lines of HI, and the 3.28 μm narrow band emission feature. Sampling of Br alpha and the 3.28 μm feature northwards of IRS-2 shows emission to be in both cases extended over radial distances 20 arc seconds. In the case of Br alpha, we interpret this to arise in a blister region of density or approximately 103 cm-3. For the 3.28 μm feature, we demonstrate that observed band strengths are consistent with the Dweck et al. (1980) hypothesis of thermal excitation, providing that the oscillators responsible for this emissions are located within one extinction optical depth of the HI/HII interface.
|Item Type:||Conference Item|
|Copyright Holders:||1982 Not known|
|Keywords:||emission spectra; excitation; galactic evolution; high resolution; infrared spectroscopy; oscillators; brightness temperature; dust; interstellar extinction; kinematics; spatial distribution|
|Academic Unit/School:||Faculty of Science, Technology, Engineering and Mathematics (STEM) > Physical Sciences
Faculty of Science, Technology, Engineering and Mathematics (STEM)
|Interdisciplinary Research Centre:||Centre for Earth, Planetary, Space and Astronomical Research (CEPSAR)|
|Depositing User:||G. J. White|
|Date Deposited:||07 Jun 2012 08:13|
|Last Modified:||28 Nov 2016 14:16|
|Share this page:|