  We present our investigation of the Extended Ultraviolet (XUV) disk galaxy,
NGC 3344, conducted as part of Deciphering the Interplay between the
Interstellar medium, Stars, and the Circumgalactic medium (DIISC) survey. We
use surface and aperture photometry of individual young stellar complexes to
study star formation and its effect on the physical properties of the
interstellar medium. We measure the specific star-formation rate (sSFR) and
find it to increase from $\rm10^{-10} yr^{-1}$ in the inner disk to
$\rm>10^{-8} yr^{-1}$ in the extended disk. This provides evidence for
inside-out disk growth. If these sSFRs are maintained, the XUV disk stellar
mass can double in $\sim$0.5 Gyr, suggesting a burst of star formation. The XUV
disk will continue forming stars for a long time due to the high gas depletion
times ($\tau_{dep}$). The stellar complexes in the XUV disk have
high-$\Sigma_{HI}$ and low-$\Sigma_{SFR}$ with $\tau_{dep}\sim$10 Gyrs, marking
the onset of a deviation from the traditional Kennicutt-Schmidt law. We find
that both far-ultraviolet (FUV) and a combination of FUV and 24$\mu$m
effectively trace star formation in the XUV disk. H$\alpha$ is weaker in
general and prone to stochasticities in the formation of massive stars.
Investigation of the circumgalactic medium at 29.5 kpc resulted in the
detection of two absorbing systems with metal-line species: the stronger
absorption component is consistent with gas flows around the disk, most likely
tracing inflow, while the weaker component is likely tracing corotating
circumgalactic gas.
