  We present multi-wavelength imagery of the merger remnant galaxy NGC 1316
with an objective to study the content of dust and its association with the
other phases of the ISM. Color-index maps as well as extinction maps derived
for this galaxy reveal an intricate and complex dust morphology in NGC 1316,
i.e., in the inner part it exists in the form of a prominent lane while at
about 6--7\,kpc it apparently takes an arc-like pattern extended along the
North-East direction. In addition to this, several other dust clumps and knots
are also evident in this galaxy. Dust emission mapped using \textit{Spitzer}
data at 8 $\mu$m indicates even more complex morphological structures of the
dust in NGC1316. The extinction curve derived over the optical to near-IR bands
closely follows the standard Galactic curve suggesting similar properties of
the dust grains. The dust content of NGC 1316 estimated from optical extinction
is $\sim$ 2.13$\times\, 10^5$ \Msun. This is a lower limit compared to that
estimated using the IRAS flux densities $\sim$ 5.17$\times\, 10^6$ \Msun\, and
flux densities at 24$\mu$m, 70$\mu$m and 160 $\mu$m from MIPS $\sim$
3.2$\times\, 10^7$ \Msun. High resolution \textit{Chandra} observations of this
merger remnant system have provided with an unprecedented view of the complex
nature of hot gas distribution in NGC 1316 which closely matches the morphology
of ionized gas and to some extent with the dust also. X-ray color-color plot
for the resolved sources within optical D$_{25}$ extent of NGC 1316 has enabled
us to separate them in different classes.
