model fits. Right: Distribution of Class 0/I candidate sources disk accretion rate estimates from SED model fits.[]{data-label="fig:C1disks"}](f6a.pdf "fig:"){width="2.5in"} ![Left: Distribution of Class 0/I candidate sources mass estimates from SED model fits. Right: Distribution of Class 0/I candidate sources disk accretion rate estimates from SED model fits.[]{data-label="fig:C1disks"}](f6b.pdf "fig:"){width="2.5in"}

The Star Formation History of DR15 \[analysis:sfh\]
---------------------------------------------------

### Identification of the main stellar groups in DR15 {#analysis:sfh:clusterid}

To further investigate the stellar formation history in the DR15 region we attempted to identify the individual stellar clusters present in our field of study. Two clusters are easy to identify, namely the cluster at the center of the field and the cluster embedded in the IRDC at the north. However, the map of Figure \[fig:ysodist\] shows a good number of sources located around the molecular gas filaments, which may or may not be part of previously formed stellar clusters or groups.

In order to identify significant overdensities of stars in the DR15 region, we constructed surface density maps using the `Gather` algorithm of @Gladwin:1999id. This algorithm is based in turn on the *nearest neighbor* method, which assigns individual surface density values to points on a two-dimensional map based on the equivalent circular area defined 