Insights into gas heating and cooling in the disc of NGC 891 from Herschel far-infrared spectroscopy
Résumé
We present Herschel PACS and SPIRE spectroscopy of the most important
far-infrared cooling lines in the nearby, edge-on spiral galaxy, NGC 891: [Cii]
158 μm,
[Nii] 122, 205 μm, [Oi] 63, 145 μm, and [Oiii] 88
μm. We find
that the photoelectric heating efficiency of the gas, traced via the
([Cii]+[Oi]63)/FTIR ratio, varies from a mean of
3.5 × 10-3 in the
centre up to 8 ×
10-3 at increasing radial and vertical distances in the
disc. A decrease in ([Cii]+[Oi]63)/FTIR but
constant ([Cii]+[Oi]63)/FPAH with increasing FIR colour suggests
that polycyclic aromatic hydrocarbons (PAHs) may become important for gas heating in the
central regions. We compare the observed flux of the FIR cooling lines and total IR
emission with the predicted flux from a PDR model to determine the gas density, surface
temperature and the strength of the incident far-ultraviolet (FUV) radiation field,
G0. Resolving details on physical scales
of ~0.6 kpc, a
pixel-by-pixel analysis reveals that the majority of the PDRs in NGC 891’s disc have
hydrogen densities of 1 <
log (n/ cm-3) < 3.5 experiencing an
incident FUV radiation field with strengths of 1.7 < log G0< 3. Although these
values we derive for most of the disc are consistent with the gas properties found in PDRs
in the spiral arms and inter-arm regions of M 51, observed radial trends in
n and
G0 are shown to be sensitive to varying
optical thickness in the lines, demonstrating the importance of accurately accounting for
optical depth effects when interpreting observations of high inclination systems.
Increasing the coverage of our analysis by using an empirical relationship between the
MIPS 24 μm
and [Nii] 205 μm emission, we estimate an enhancement of the FUV
radiation field strength in the far north-eastern side of the disc relative to the rest of
the disc that coincides with the above-average star formation rate surface densities and
gas-to-dust ratios. However, an accurate interpretation remains difficult due to optical
depth effects, confusion along the line-of-sight and observational uncertainties.
Origine : Publication financée par une institution
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