Volume 375, Number 2, August IV 2001
|Page(s)||566 - 578|
|Published online||15 August 2001|
Global physical conditions of the interstellar medium in nearby galaxies*
Department of Astronomy, School of Science, University of Tokyo, 7-3-1 Hongo, Bunkyo-ku, Tokyo 113-0033, Japan
2 MS245-6, NASA Ames Research Center, Moffett Field, CA94035-1000, USA
Corresponding author: T. Onaka, email@example.com
Accepted: 1 June 2001
Far-infrared spectra (43-197 μm) of 34 nearby galaxies obtained by the Long Wavelength Spectrometer (LWS) aboard the Infrared Space Observatory (ISO) were analyzed to investigate the general properties of interstellar matter in galaxies. The present sample includes not only normal galaxies but also starbursts and active galactic nuclei (AGNs). Far-infrared forbidden lines, such as [Cii]158 μm, [Oi]63 μm, [Nii]122 μm, and [Oiii]88 μm, were detected in most of the sample galaxies. [Oi]145 μm line was detected in 13 galaxies. The line fluxes of [Cii]158 μm and [Nii]122 μm relative to the total far-infrared flux (FIR) decrease as the far-infrared color becomes bluer, while the ratio of the [Oi]63 μm flux to FIR does not show a systematic trend with the color. The [Oiii]88 μm to FIR ratio shows a large scatter with a weak trend of increase with the color. AGNs do not show any distinguishable trend from normal and starburst galaxies in the far-infrared spectra, suggesting that the far-infrared emission is mainly driven by star-formation activities even in AGNs. We estimate the physical conditions of photodissociation regions (PDRs) in the sample galaxies, such as the far-ultraviolet radiation field intensity and the gas density n by assuming that all the observed [Oi]63 μm and far-infrared continuum emissions come from PDRs. Comparison with PDR models indicates that ranges from 102-104 and -. The present results also suggest that n varies proportionally with . The ratio of [Cii] 158 μm to CO (-0) line emission supports the linear increase in n with . We estimate that about a half of [Cii]158 μm emission originates from PDRs and attribute the rest to the emission as coming from low-density diffuse ionized gas. The estimated intensity of [Cii]158 μm from the ionized gas is compatible with the observed intensity of [Nii]122 μm if both lines come from the same diffuse ionized gas. The present analysis suggests that the decrease in [Cii]158 μm with the far-infrared color may not be accounted for by the decrease in the photoelectric heating efficiency owing to the increase in positive charges of dust grains because a measure of the efficiency, , is found to stay constant with the far-infrared color. Instead the decrease can be interpreted in terms of either the increase in the collisional de-excitation of the [Cii] transition due to the increase in the gas density or the decrease in the ionized component relative to the far-infrared intensity suggested by the decrease in [Nii]122 μm. Based on the present analysis, we derive average relations of the far-infrared color with and n in galaxies, which can be applied to the investigation of interstellar matter in distant galaxies.
Key words: galaxies: ISM / infrared: ISM / ISM: lines and bands / radiation mechanisms: thermal
© ESO, 2001
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