The brightest observed emission line in many star-forming galaxies is the [C II} 158 μm line, making it detectable up to z ∼ 7. In order to better understand and quantify the [C II] emission as a tracer of star formation, the theoretical ratio between the [N II] 158 μm emission has been employed to empirically determine the fraction of [C II] emission that originates from the ionized and neutral phases of the interstellar medium (ISM). Sub-kiloparsec measurements of the [C II] 158 μm and [N II] 205 μm lines in nearby galaxies have recently become available as part of the Key Insights in Nearby Galaxies: A Far Infrared Survey with Herschel (KINGFISH) and Beyond the Peak programs. With the information from these two far-infrared lines along with the multi-wavelength suite of KINGFISH data, a calibration of the [C II] emission line as a star formation rate (SFR) indicator and a better understanding of the [C II] deficit are pursued. [C II] emission is also compared to polycyclic aromatic hydrocarbon (PAH) emission in these regions to compare photoelectric heating from PAH molecules to cooling by [C II]in the neutral and ionized phases of the ISM. We find that the[C II] emission originating in the neutral phase of the ISM does not exhibit a deficit with respect to the infrared luminosity and is therefore preferred over the emission originating in the ionized phase of the ISM as an SFR indicator for the normal star-forming galaxies included in this sample.
|Original language||English (US)|
|State||Published - Nov 20 2019|
All Science Journal Classification (ASJC) codes
- Astronomy and Astrophysics
- Space and Planetary Science