http://arxiv.org/abs/1905.06935
We present a method for deriving the electron density of ionized gas using the ratio of the intensity of the [NII] 205um line to that of a Hydrogen radio recombination line (RRL). We use this method to derive electron densities of 21 velocity components in 11 lines of sight, including the Galactic center. We observed, at high–spectral resolution, the [NII] 205um with the Herschel/HIFI and SOFIA/GREAT instruments and the radio recombination lines with the Green Bank Telescope and the NASA Deep Space Network Deep Space Station 43 (DSS-43) telescope. We find typical electron densities between 6 to 170 cm^{-3}, which are consistent with those derived at low spectral resolution using the [NII] 205um/122um ratio with Herschel/PACS on a larger sample of sight lines in the Galactic plane. By matching the electron densities derived from the [NII] 205um/RRL intensity ratio and the [NII] 122um/205um intensity ratio, we derive the nitrogen fractional abundance for our velocity components. We investigate the dependence of the N/H ratio with Galactocentric distance in the inner Galaxy (R_gal<6kpc), which is inaccessible in optical studies due to dust extinction. We find that the distribution of nitrogen abundances in the inner galaxy derived from our data has a slope that is consistent to that found in the outer Galaxy in optical studies. This result is inconsistent with some suggestions of a flatter distribution of the nitrogen abundance in the inner galaxy.
J. Pineda, S. Horiuchi, L. Anderson, et. al.
Fri, 17 May 19
21/59
Comments: 18 pages, 9 figures, to be submitted to ApJ, comments welcome
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