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We present our investigation of the Extended Ultraviolet (XUV) disk galaxy,NGC 3344, conducted as part of Deciphering the Interplay between theInterstellar medium, Stars, and the Circumgalactic medium (DIISC) survey. Weuse surface and aperture photometry of individual young stellar complexes tostudy star formation and its effect on the physical properties of theinterstellar medium. We measure the specific star-formation rate (sSFR) andfind 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 forinside-out disk growth. If these sSFRs are maintained, the XUV disk stellarmass can double in $\sim$0.5 Gyr, suggesting a burst of star formation. The XUVdisk will continue forming stars for a long time due to the high gas depletiontimes ($\tau_{dep}$). The stellar complexes in the XUV disk havehigh-$\Sigma_{HI}$ and low-$\Sigma_{SFR}$ with $\tau_{dep}\sim$10 Gyrs, markingthe onset of a deviation from the traditional Kennicutt-Schmidt law. We findthat both far-ultraviolet (FUV) and a combination of FUV and 24$\mu$meffectively trace star formation in the XUV disk. H$\alpha$ is weaker ingeneral and prone to stochasticities in the formation of massive stars.Investigation of the circumgalactic medium at 29.5 kpc resulted in thedetection of two absorbing systems with metal-line species: the strongerabsorption component is consistent with gas flows around the disk, most likelytracing inflow, while the weaker component is likely tracing corotatingcircumgalactic gas.

DIISC-II: Unveiling the Connections between Star Formation and ISM in the Extended Ultraviolet Disk of NGC 3344