1997/10/21 by Sangeeta Malhotra, S. Malhotra, G. Helou +34
Chemistry · Engineering · Physics and Astronomy · #Astrophysics (astro-ph) #Astrophysics and Star Formation Studies #FOS: Physical sciences #Semiconductor Lasers and Optical Devices #Spectroscopy and Laser Applications #astro-ph
paper · pdf · doi:10.48550/arxiv.astro-ph/9710220
Accepted for publication in ApJ Letters. Uses aastex. 11 pages with figures. Shortened abstract
arxiv created 1997/10/21 · openalex publication_date 1997/10/21 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/28
We report measurements of the [CII] fine structure line at 157.714 micron in 30 normal star-forming galaxies with the Long Wavelength Spectrometer (LWS) on the Infrared Space Observatory (ISO). The ratio of the line to total far-infrared luminosity, [CII]/FIR, measures the ratio of the cooling of gas to that of dust; and thus the efficiency of the grain photoelectric heating process. This ratio varies by a factor of 40 in the current sample. About two-thirds of the galaxies have [CII]/FIR = 2-7 x 10-3. The other one-third show trends of decreasing [CII]/FIR with increasing dust temperature, indicated by the ratio of infrared emission at 60 and 100 microns; and with increasing star-formation activity, measured by the ratio of far-infrared and blue band luminosity. We find three FIR bright galaxies with undetected [CII] line at 3-sigma upper limits of [CII]/FIR < 0.5-2 x 10-4. The trend in the [CII]/FIR ratio with the temperature of dust and with star-formation activity may be due to decreased efficiency of photoelectric heating of gas at high UV radiation intensity as dust grains become positively charged, decreasing the yield and the energy of the photoelectrons. The three galaxies with no observed PDR lines have among the highest ratios of FIR to Blue luminosity and the ratio of 60 and 100 micron emission. Their lack of [CII] lines may be due to a continuing trend of decreasing [CII]/FIR with increasing star-formation activity and dust temperature seen in one-third of the sample with warm IRAS colors. In that case the upper limits on [CII]/FIR imply a ratio of UV flux to gas density G0/n > 10 cm3. The low [CII]/FIR could also be due to either weak [CII] because of self-absorption or strong FIR continuum from regions weak in [CII], such as dense HII regions or plasma ionized by hard radiation of AGNs.