Catalogue of High Protostellar Surface Density Regions in Nearby Embedded Clusters. (arXiv:1812.00556v1 [astro-ph.GA])
<a href="http://arxiv.org/find/astro-ph/1/au:+Li_J/0/1/0/all/0/1">Juan Li</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Myers_P/0/1/0/all/0/1">Philip C. Myers</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kirk_H/0/1/0/all/0/1">Helen Kirk</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gutermuth_R/0/1/0/all/0/1">Robert A. Gutermuth</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dunham_M/0/1/0/all/0/1">Michael M. Dunham</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pokhrel_R/0/1/0/all/0/1">Riwaj Pokhrel</a>
We analyze high-quality stellar catalogs for 24 young and nearby (within 1
kpc) embedded clusters and present a catalogue of 32 groups which have a high
concentration of protostars. The median effective radius of these groups is
0.17 pc. The median protostellar and pre-main sequence star surface densities
are 46 M_{odot} pc^{-2} and 11 M_{odot} pc^{-2}, respectively. We estimate
the age of these groups using a model of constant birthrate and random
accretion stopping and find a median value of 0.25 Myr. Some groups in Aquila
and Serpens, Corona Australia and Ophichus L1688 show high protostellar surface
density and high molecular gas surface density, which seem to be undergoing
vigorous star formation. These groups provide an excellent opportunity to study
initial conditions of clustered star formation. Comparison of protostellar and
pre-main-sequence stellar surface densities reveal continuous low-mass star
formation of these groups over several Myr in some clouds. For groups with
typical protostellar separations of less than 0.4 pc, we find that these
separations agree well with the thermal Jeans fragmentation scale. On the other
hand, for groups with typical protostellar separations larger than 0.4 pc,
these separations are always larger than the associated Jeans length.
We analyze high-quality stellar catalogs for 24 young and nearby (within 1
kpc) embedded clusters and present a catalogue of 32 groups which have a high
concentration of protostars. The median effective radius of these groups is
0.17 pc. The median protostellar and pre-main sequence star surface densities
are 46 M_{odot} pc^{-2} and 11 M_{odot} pc^{-2}, respectively. We estimate
the age of these groups using a model of constant birthrate and random
accretion stopping and find a median value of 0.25 Myr. Some groups in Aquila
and Serpens, Corona Australia and Ophichus L1688 show high protostellar surface
density and high molecular gas surface density, which seem to be undergoing
vigorous star formation. These groups provide an excellent opportunity to study
initial conditions of clustered star formation. Comparison of protostellar and
pre-main-sequence stellar surface densities reveal continuous low-mass star
formation of these groups over several Myr in some clouds. For groups with
typical protostellar separations of less than 0.4 pc, we find that these
separations agree well with the thermal Jeans fragmentation scale. On the other
hand, for groups with typical protostellar separations larger than 0.4 pc,
these separations are always larger than the associated Jeans length.
http://arxiv.org/icons/sfx.gif
