High resolution LAsMA $^{12}$CO and $^{13}$CO observation of the G305 giant molecular cloud complex : II. Effect of feedback on clump properties. (arXiv:2109.09615v1 [astro-ph.GA])

High resolution LAsMA $^{12}$CO and $^{13}$CO observation of the G305 giant molecular cloud complex : II. Effect of feedback on clump properties. (arXiv:2109.09615v1 [astro-ph.GA])
<a href="http://arxiv.org/find/astro-ph/1/au:+Mazumdar_P/0/1/0/all/0/1">P. Mazumdar</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wyrowski_F/0/1/0/all/0/1">F. Wyrowski</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Urquhart_J/0/1/0/all/0/1">J. S. Urquhart</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Colombo_D/0/1/0/all/0/1">D. Colombo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Menten_K/0/1/0/all/0/1">K. M. Menten</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Neupane_S/0/1/0/all/0/1">S. Neupane</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Thompson_M/0/1/0/all/0/1">M. A. Thompson</a>

G305 star-forming complex was observed in the 3-2 lines of 12 & 13CO to
investigate the effect of feedback from the central OB stars on the complex.
The region was decomposed into clumps using dendrogram analysis. A catalog of
the clump properties was created. The surface mass densities of the clumps were
plotted as a function of the incident 8um flux. A mask of the region with 8um
flux >100 MJy/sr was created and clumps were categorized based on the extent of
overlap with the mask into “mostly inside” , “partly inside'”, & “outside”. The
surface mass density distribution of each of these populations were plotted.
This was followed by comparing the G305 clumps with the Galactic average taken
from the ATLASGAL and CHIMPS clumps. Finally, the cumulative distribution
functions (CDF) of the clump masses in G305 and their L/M ratios were compared
to that of the Galactic sample. The surface mass densities of clumps showed a
positive correlation with the incident 8um flux. The data did not have
sufficient velocity resolution to discern the effects of feedback on the
linewidths of the clumps. The sub-sample of clumps named “mostly inside” had
the highest surface mass densities followed by “partly inside” and “outside”
sub-samples. These differences between the three sub-samples were shown to be
statistically significant using the KS test. The “mostly inside” sample also
showed the highest level of fragmentation compared to the other two. These
prove that the clumps inside the G305 region are triggered. The G305 clump
population is also statistically different from the Galactic average population
rejecting redistribution as a likely consequence of feedback. The CDFs of clump
masses and their L/M ratios are both flatter than the Galactic average,
indicating that feedback in G305 has triggered star formation. The collect and
collapse method is the dominant mechanism at play in G305.

G305 star-forming complex was observed in the 3-2 lines of 12 & 13CO to
investigate the effect of feedback from the central OB stars on the complex.
The region was decomposed into clumps using dendrogram analysis. A catalog of
the clump properties was created. The surface mass densities of the clumps were
plotted as a function of the incident 8um flux. A mask of the region with 8um
flux >100 MJy/sr was created and clumps were categorized based on the extent of
overlap with the mask into “mostly inside” , “partly inside'”, & “outside”. The
surface mass density distribution of each of these populations were plotted.
This was followed by comparing the G305 clumps with the Galactic average taken
from the ATLASGAL and CHIMPS clumps. Finally, the cumulative distribution
functions (CDF) of the clump masses in G305 and their L/M ratios were compared
to that of the Galactic sample. The surface mass densities of clumps showed a
positive correlation with the incident 8um flux. The data did not have
sufficient velocity resolution to discern the effects of feedback on the
linewidths of the clumps. The sub-sample of clumps named “mostly inside” had
the highest surface mass densities followed by “partly inside” and “outside”
sub-samples. These differences between the three sub-samples were shown to be
statistically significant using the KS test. The “mostly inside” sample also
showed the highest level of fragmentation compared to the other two. These
prove that the clumps inside the G305 region are triggered. The G305 clump
population is also statistically different from the Galactic average population
rejecting redistribution as a likely consequence of feedback. The CDFs of clump
masses and their L/M ratios are both flatter than the Galactic average,
indicating that feedback in G305 has triggered star formation. The collect and
collapse method is the dominant mechanism at play in G305.

http://arxiv.org/icons/sfx.gif