Investigating the [CII]-PAHs relation in a large sample of local galaxies

Details Investigating the [CII]-PAHs relation in a large sample of local galaxies Investigating the [CII]-PAHs relation in a large sample of local galaxies

Feb 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003esasp.511..279c&link_type=abstract

Exploiting the ISO Data Archive. Infrared Astronomy in the Internet Age, held in Siguenza, Spain 24-27 June, 2002. Edited by

Astronomy and Astrophysics

Astronomy

2

Scientific paper

We present preliminary results about the linear correlation existing between the Mid Infrared (MIR) Aromatic Features seen in emission (AFEs) and the emission of the main cooling line of the neutral atomic medium, [CII] at 158 μm, for a sample of 140 galaxies. A similar analysis on a smaller sample of normal galaxies only, has been already published by Helou et al. (2001ApJ...548L..73H). The final aim of the work presented here is to further investigate the physical origin and implications of such a relation and to see if the same results hold for a much wider variety of galaxy types and activities. When only spiral galaxies are considered, we confirm the results already obtained in previous works by Malhotra et al. (Malhotra et al. 2001ApJ...561..766M) and Helou et al. (2001ApJ...548L..73H): there exists a difference between the behavior of the [CII]/FIR and [CII]/AFE ratios as a function of the 60 μm 100 μm IRAS colors: while [CII]/FIR decreases with the IRAS color, the [CII]/AFE ratio stays constant. The same result seems to hold also for early-type and irregular galaxies although they show a much higher dispersion in the [CII]/AFE ratio. As first step of the analysis, we concentrate on understanding the origin of the dispersion in order to separate intrinsic physical behavior from errors in the ISOCAM photometry. There exist few outsiders with a [CII]/AFE ratio lower than the main trend outlined from late spiral and irregular galaxies, although, at this preliminary stage of the analysis, we are not yet able to explain the physical origin.

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