Probing the formation of intermediate- to high-mass stars in protoclusters II. Comparison between millimeter interferometric observations of NGC 2264-C and SPH simulations of a collapsing clump

TL;DR

This study combines millimeter interferometric observations and SPH simulations to investigate the early collapse and fragmentation of a massive star-forming clump in NGC 2264-C, revealing insights into initial conditions and dynamical processes.

Contribution

It provides the first detailed comparison between high-resolution observations and hydrodynamic simulations of a collapsing protocluster, supporting gravity-driven collapse with specific initial conditions.

Findings

Detection of a new compact source near the central protostar.

Collapse and fragmentation along the clump's long axis supported by simulations.

Collapse phase is short-lived, less than 10^5 years, with low turbulence influence.

Abstract

The earliest phases of massive star formation in clusters are still poorly understood. Here, we test the hypothesis for high-mass star formation proposed in our earlier paper (Peretto et al. 2006). In order to confirm the physical validity of this hypothesis, we carried out IRAM Plateau de Bure interferometer observations of NGC 2264-C and performed SPH numerical simulations of the collapse of a Jeans-unstable, prolate dense clump. Our Plateau de Bure observations reveal the presence of a new compact source (C-MM13) located only \~ 10000 AU away, but separated by ~ 1.1 km/s in (projected) velocity, from the most massive Class 0 object (C-MM3) lying at the very center of NGC 2264-C. Detailed comparison with our numerical SPH simulations supports the view that NGC 2264-C is an elongated cluster-forming clump in the process of collapsing and fragmenting along its long axis, leading to a strong dynamical interaction and possible protostar merger in the central region of the clump. The present study also sets several quantitative constraints on the initial conditions of large-scale collapse in NGC 2264-C. Our hydrodynamic simulations indicate that the observed velocity pattern characterizes an early phase of protocluster collapse which survives for an only short period of time (i.e., < 10^5 yr). To provide a good match to the observations the simulations require an initial ratio of turbulent to gravitational energy of only ~ 5 %, which strongly suggests that the NGC 2264-C clump is structured primarily by gravity rather than turbulence. The required "cold'' initial conditions may result from rapid compression by an external trigger.