[CII] Emission and Star Formation in Late-Type Galaxies |
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| Authors: | D Pierini KJ Leech RJ Tuffs HJ Völk |
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| Institution: | (1) Max-Planck-Institut für Kernphysik, Heidelberg, Germany;(2) ESA Astrophysics Division, ISO Data Centre, Villafranca del Castillo, Spain |
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| Abstract: | A linear correlation between the ratio of theCII( $^{\text{2}}$ P A linear correlation between the ratio of theCII(
P
→
P
)] line intensity to the
CO(J:1 →0)] line emission, I
/I
and the
equivalent width (EW) is found, over the range 2–71 ? in
EW, for a sample of 21late-Type= galaxies. The latter is comprised of an optically selected sample of 12 normal Virgo Cluster
spiral galaxies with CII] detections obtained by us with ISOLWS, plus nine late-Type= galaxies with higher star formation
rates (SFRs), for which CII] data and, especially,
EW data are available in the literature. As a result we infer I
/I
to be a reliable tracer of the current mass-normalized global SFR for non-starburst spiral galaxies. Moreover, the ratio
of the CII] line to the total far-infrared (FIR) continuum intensity, I
/I
, is found to decrease from ∼0.5% to ∼0.1% with decreasing SFR which we propose is due to a `CII]-quiet' component of I
from dust heated by the general interstellar radiation field (ISRF). The more `quiescent' galaxies in the sample have values
of I
/I
different from those observed in `compact' Galactic interstellar regions. Their CII]-emission is interpreted to be dominated
by diffuse regions of the interstellar medium (ISM). For normal `star-forming' galaxies the diffuse component of the CII]
emission is estimated to account for at least 50% of the total.
This revised version was published online in July 2006 with corrections to the Cover Date. |
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| Keywords: | |
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