Studies of the distinct regions due to CO selective dissociation in the Aquila molecular cloud (2010.16118v2)

Abstract: Aims. We investigate the role of selective dissociation in the process of star formation by comparing the physical parameters of protostellar-prestellar cores and the distinct regions with the CO isotope distributions in photodissociation regions. We seek to understand whether there is a better connection between the evolutionary age of star forming regions and the effect of selective dissociation Methods. Wide-field observations of the $\rm ^{12}CO$, $\rm ^{13}CO$, and $\rm C^{18}O$ ( J = 1 - 0) emission lines are used to study the ongoing star formation activity in the Aquila molecular region, and the 70 $\mu$m and 250 $\mu$m data are used to describe the heating of the surrounding material and as an indicator of the evolutionary age of the core. Results. The protostellar-prestellar cores are found at locations with the highest $\rm C^{18}O$ column densities and their increasing evolutionary age would relate to an increasing 70$\mu$m/250$\mu$m emission ratio at their location. An evolutionary age of the cores may also follow from the $\rm ^{13}CO$ versus $\rm C^{18}O$ abundance ratio, which decreases with increasing $\rm C^{18}O$ column densities. The original mass has been estimated for nine representative star formation regions and the original mass of the region correlated well with the integrated 70 $\mu$m flux density. Similarly, the $ X_{\rm ^{13}CO}$/$X_{\rm C^{18}O}$ implying the dissociation rate for these regions correlates with the 70$\mu$m/250$\mu$m flux density ratio and reflects the evolutionary age of the star formation activity.