Faint emission lines in the Galactic H II regions M16, M20 and NGC 3603

Details Faint emission lines in the Galactic H II regions M16, M20 and NGC 3603 Faint emission lines in the Galactic H II regions M16, M20 and NGC 3603

2006-01-26

arxiv.org/abs/astro-ph/0601595v1

Mon.Not.Roy.Astron.Soc. 368 (2006) 253-279

Astronomy and Astrophysics

Astrophysics

22 pages, 13 Tables, 7 Figures. Accepted for publication by MNRAS

Scientific paper

10.1111/j.1365-2966.2006.10105.x

We present deep echelle spectrophotometry of the Galactic {\hii} regions M16, M20 and NGC 3603. The data have been taken with the Very Large Telescope Ultraviolet-Visual Echelle Spectrograph in the 3100 to 10400 \AA range. We have detected more than 200 emission lines in each region. Physical conditions have been derived using different continuum and line intensity ratios. We have derived He$^{+}$, C$^{++}$ and O$^{++}$ abundances from pure recombination lines as well as abundances from collisionally excited lines for a large number of ions of different elements. We have obtained consistent estimations of the temperature fluctuation parameter, {\ts}, using different methods. We also report the detection of deuterium Balmer lines up to D$\delta$ (M16) and to D$\gamma$ (M20) in the blue wings of the hydrogen lines, which excitation mechanism seems to be continuum fluorescence. The temperature fluctuations paradigm agree with the results obtained from optical CELs and the more uncertain ones from far IR fine structure CELs in NGC 3603, although, more observations covering the same volume of the nebula are necessary to obtain solid conclusions.

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