ALMA Observations of Two Massive and Dense MALT90 Clumps

Abstract

We report Atacama Large Millimeter Array observations of 3 mm dust continuum emission and line emission, in HCO + , H 13 CO + , N 2 H + , and CH 3 CN, toward two massive and dense clumps (MDCs) in early but distinct evolutionary phases (prestellar and protostellar), made with the goal of investigating their fragmentation characteristics at angular scales of ∼1″. Toward the prestellar clump we detected 10 compact structures (cores), with radii from 1200–4500 au and masses from 1.6–20  M ⊙ . Half of these cores exhibit inverse P Cygni profiles in HCO + and are subvirialized indicating that they are undergoing collapse. Toward the protostellar clump we detected a massive (119 M ⊙ ) central core, with a strong mass infall rate, and nine less massive cores, with masses from 1.7–27  M ⊙ and radii from 1000–4300 au. CH 3 CN rotational temperatures were derived for eight cores in the protostellar clump and three cores in the prestellar clump. Cores within the prestellar clump have smaller line widths and lower temperatures than cores within the protostellar clump. The fraction of total mass in cores to clump mass is smaller in the prestellar clump (∼6%) than in the protostellar clump (∼23%). We conclude that we are witnessing the evolution of the dense gas in globally collapsing MDCs; the prestellar clump illustrating the initial stage of fragmentation, harboring cores that are individually collapsing, and the protostellar clump reflecting a later stage in which a considerable fraction of the gas has been gravitationally focused into the central region.