II number ratio, $R_{\mathrm{I:II}}$, both constructed using the method described in @Ybarra:2013kh.

For the $R_{\mathrm{II:III}}$ map we limited the source candidates to a de-reddened brightness $H$=13.5 mag. This brightness cut avoids biasing the number counts from incompleteness due to patchy extinction. We used the Bayesian estimator described in @Ybarra:2013kh to calculate the ratios within circular projected regions with radius 3$^\prime$. The map only shows ratios for regions with sufficient number counts such that $N_{1}+N_{2}+1 <  0.25(N_{1}+1)(N_{2}-1)$, where $N_{1}$ is the number count of the numerator, and $N_{2}$ is the number count of the denominator.

We found that the whole complex has $R_{\mathrm{II:III}} \ge 1.0$ which suggests star formation was ubiquitous throughout the complex $\sim$ 2-3 Myr ago. We can also trace the most recent star formation by using the $R_{\mathrm{I:II}}$ ratio (Fig. \[fig:ratiomaps\], right). Regions with significant $R_{\mathrm{I:II}}$ are expected to have been actively forming stars within the last Myr. We found that the regions of high $R_{\mathrm{I:II}}$ appear to form an oblong ring around IC 1795. This mirrors the distribution of Class I/0 sources which also appear to surround IC 1795 (see Fig. \[fig:gather\]). Interestingly, the high $R_{\mathrm{II:III}}$ in IC 1795 suggests that stars were forming there up to 