Carbon and Oxygen Galactic Gradients: Observational Values from HII Region Recombination Lines

Details Carbon and Oxygen Galactic Gradients: Observational Values from HII Region Recombination Lines Carbon and Oxygen Galactic Gradients: Observational Values from HII Region Recombination Lines

2004-08-23

arxiv.org/abs/astro-ph/0408397v2

Astrophys.J. 618 (2004) L95-L98

Astronomy and Astrophysics

Astrophysics

13 pages, 2 tables, 2 figures. Published in ApJ Letters, 618, L95

Scientific paper

10.1086/426889

We present results of deep echelle spectrophotometry of eight Galactic HII regions located at Galactocentric distances between 6.3 and 10.4 kpc. The data have been taken with the Very Large Telescope (VLT) Ultraviolet Echelle Spectrograph (UVES) in the 3100 to 10360 A range. We have derived C++ and O++ abundances from recombination lines for all the objects, as well as O+ abundances from this kind of lines for three of the nebulae. The intensity of recombination lines is almost independent of the assumed electron temperature as well as of the possible presence of spatial temperature variations or fluctuations inside the nebulae. These data allow the determination of the gas-phase C and O abundance gradients of the Galactic disk, of paramount importance for chemical evolution models. This is the first time the C gradient is derived from such a large number of HII regions and for such a wide range of Galactocentric distances. Abundance gradients are found of the form $\Delta$log(O/H) = -0.044$\pm$0.010 dex kpc^-1, $\Delta$log(C/H) = -0.103$\pm$0.018 dex kpc^-1, and $\Delta$log(C/O) = -0.058$\pm$0.018 dex kpc^-1.

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