Astrophys. J., 826, 175-175 (2016/August-1)
The ionized gas in nearby galaxies as traced by the [N II] 122 and 205 µm transitions.
HERRERA-CAMUS R., BOLATTO A., SMITH J.D., DRAINE B., PELLEGRINI E., WOLFIRE M., CROXALL K., DE LOOZE I., CALZETTI D., KENNICUTT R., CROCKER A., ARMUS L., VAN DER WERF P., SANDSTROM K., GALAMETZ M., BRANDL B., GROVES B., RIGOPOULOU D., WALTER F., LEROY A., BOQUIEN M., TABATABAEI F.S. and BEIRAO P.
Abstract (from CDS):
The [N ii] 122 and 205 µm transitions are powerful tracers of the ionized gas in the interstellar medium. By combining data from 21 galaxies selected from the Herschel KINGFISH and Beyond the Peak surveys, we have compiled 141 spatially resolved regions with a typical size of ∼1 kpc, with observations of both [N ii] far-infrared lines. We measure [N ii] 122/205 line ratios in the ∼0.6-6 range, which corresponds to electron gas densities of ne ∼ 1-300/cm3, with a median value of ne=30/cm3. Variations in the electron density within individual galaxies can be as high as a factor of ∼50, frequently with strong radial gradients. We find that ne increases as a function of infrared color, dust-weighted mean starlight intensity, and star-formation rate (SFR) surface density (ΣSFR). As the intensity of the [N ii] transitions is related to the ionizing photon flux, we investigate their reliability as tracers of the SFR. We derive relations between the [N ii] emission and SFR in the low-density limit and in the case of a log-normal distribution of densities. The scatter in the correlation between [N ii] surface brightness and ΣSFR can be understood as a property of the ne distribution. For regions with ne close to or higher than the [N ii] line critical densities, the low-density limit [N ii]-based SFR calibration systematically underestimates the SFR because the [N ii] emission is collisionally quenched. Finally, we investigate the relation between [N ii] emission, SFR, and ne by comparing our observations to predictions from the MAPPINGS-III code.
© 2016. The American Astronomical Society. All rights reserved.
galaxies: ISM - galaxies: star formation - ISM: structure
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