[CI](1-0) and [CI](2-1) in resolved local galaxies
  We present resolved [CI] line intensities of 18 nearby galaxies observed with
the SPIRE FTS spectrometer on the Herschel Space Observatory. We use these data
along with resolved CO line intensities from $J_\mathrm{up} = 1$ to 7 to
interpret what phase of the interstellar medium the [CI] lines trace within
typical local galaxies. A tight, linear relation is found between the
intensities of the CO(4-3) and [CI](2-1) lines; we hypothesize this is due to
the similar upper level temperature of these two lines. We modeled the [CI] and
CO line emission using large velocity gradient models combined with an
empirical template. According to this modeling, the [CI](1-0) line is clearly
dominated by the low-excitation component. We determine [CI] to molecular mass
conversion factors for both the [CI](1-0) and [CI](2-1) lines, with mean values
of $\alpha_{\mathrm{[CI](1-0)}} = 7.3$ M$_{\mathrm{sun}}$ K$^{-1}$ km$^{-1}$ s
pc$^{-2}$ and $\alpha_{\mathrm{[CI](2-1)}} = 34 $ M$_{\mathrm{sun}}$ K$^{-1}$
km$^{-1}$ s pc$^{-2}$ with logarithmic root-mean-square spreads of 0.20 and
0.32 dex, respectively. The similar spread of $\alpha_{\mathrm{[CI](1-0)}}$ to
$\alpha_{\mathrm{CO}}$ (derived using the CO(2-1) line) suggests that [CI](1-0)
may be just as good a tracer of cold molecular gas as CO(2-1) in galaxies of
this type. On the other hand, the wider spread of $\alpha_{\mathrm{[CI](2-1)}}$
and the tight relation found between [CI](2-1) and CO(4-3) suggest that much of
the [CI](2-1) emission may originate in warmer molecular gas.
