point sources from the same images are also presented by Whitney et al. (2008), but Whitney et al. (2008) miss a significant fraction of point sources in the 30 Doradus region, as their study is motivated towards detecting reliable sources throughout the LMC via pipeline analysis. Gruendl & Chu (2009) detect objects in the dense and nebulous surroundings using detailed aperture photometry (see Section 6.3 of Gruendl & Chu (2009) for a comparison). Photometry in the fIR at 100 and 160$\mu$m, and 250 and 350$\mu$m of point-like and extended sources in the stapler nebula is given in Seale et al (2014), using images taken by the [*Herschel*]{} space telescope PACS (Photoconductor Array Camera and Spectrometer), and SPIRE (Spectral and Photometric Imaging Receiver) instruments respectively as part of the [*Hershel*]{} large program HERITAGE (HERschel Inventory of The Agents of Galaxy Evolution; Meixner et al. 2013). The FWHM for these images are 8$\arcsec$, 12$\arcsec$, 18$\arcsec$ and 25$\arcsec$ respectively. We utilize the photometry from Gruendl & Chu (2009) and Seale et al. (2014) in this study.

Molecular clouds
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Figure \[fig:CO\] shows the CO(2-1) integrated line emission over the velocity interval 235–270 kms$^{-1}$ as contours, superimposed on the HST composite $BVI$H$\alpha$ image. Strong 