An ALMA archival study of the clump mass function in the Large Magellanic Cloud. (arXiv:1811.07994v1 [astro-ph.GA])
<a href="http://arxiv.org/find/astro-ph/1/au:+Brunetti_N/0/1/0/all/0/1">Nathan Brunetti</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wilson_C/0/1/0/all/0/1">Christine D. Wilson</a>
We present 1.3 and 3.2 mm continuum maps of three star forming regions in the
Large Magellanic Cloud (LMC) observed with the Atacama Large
Millimeter/Submillimeter Array (ALMA). The data were taken as part of two
projects retrieved from the ALMA public archive plus one project observed
specifically for this work. We develop a technique to combine maps at these
wavelengths to estimate dust-only emission corrected for free-free emission
contamination. From these observations we identify 32 molecular clumps in the
LMC and estimate their total mass from their dust emission to range from 205 to
5740 M$_{odot}$. We derive a cumulative clump mass function ($N(geq M)
propto M^{alpha + 1}$) and fit it with a double power law to find
$alpha_{mathrm{low}} = -1.76^{+0.04}_{-0.05}$, $alpha_{mathrm{high}} = -3.3
pm 0.2$, and a break mass of 2500$^{+300}_{-200}$ M$_{odot}$. A comparison to
the 30 Doradus-10 mass function derived previously from CO (2-1) data reveals a
consistent range of clump masses and good agreement between the fitted slopes.
We also find that the low mass index of the LMC mass function agrees well with
the high mass index for core and clump mass functions from several star forming
regions in the Milky Way. This agreement may indicate an extension of the Milky
Way power law to higher masses than previously observed.
We present 1.3 and 3.2 mm continuum maps of three star forming regions in the
Large Magellanic Cloud (LMC) observed with the Atacama Large
Millimeter/Submillimeter Array (ALMA). The data were taken as part of two
projects retrieved from the ALMA public archive plus one project observed
specifically for this work. We develop a technique to combine maps at these
wavelengths to estimate dust-only emission corrected for free-free emission
contamination. From these observations we identify 32 molecular clumps in the
LMC and estimate their total mass from their dust emission to range from 205 to
5740 M$_{odot}$. We derive a cumulative clump mass function ($N(geq M)
propto M^{alpha + 1}$) and fit it with a double power law to find
$alpha_{mathrm{low}} = -1.76^{+0.04}_{-0.05}$, $alpha_{mathrm{high}} = -3.3
pm 0.2$, and a break mass of 2500$^{+300}_{-200}$ M$_{odot}$. A comparison to
the 30 Doradus-10 mass function derived previously from CO (2-1) data reveals a
consistent range of clump masses and good agreement between the fitted slopes.
We also find that the low mass index of the LMC mass function agrees well with
the high mass index for core and clump mass functions from several star forming
regions in the Milky Way. This agreement may indicate an extension of the Milky
Way power law to higher masses than previously observed.
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