Dynamical histories of the IC348 and NGC1333 star-forming regions in Perseus

Abstract

We present analyses of the spatial distributions of stars in the young (1 - 3 Myr) star-forming regions IC348 and NGC1333 in the Perseus Giant Molecular Cloud. We quantify the spatial structure using the $\mathcal{Q}$-parameter and find that both IC348 and NGC1333 are smooth and centrally concentrated with $\mathcal{Q}$-parameters of 0.98 and 0.89 respectively. Neither region exhibits mass segregation (${\Lambda }_{\mathrm{MSR}}=1.1_{-0.3}^{+0.2}$ for IC348 and ${\Lambda }_{\mathrm{MSR}}=1.2_{-0.3}^{+0.4}$ for NGC1333, where ${\Lambda }_{\mathrm{MSR}}\sim 1$ corresponds to no mass segregation), nor do the most massive stars reside in areas of enhanced stellar surface density compared to the average surface density, according to the ${\Sigma }_{\mathrm{LDR}}$ method. We then constrain the dynamical histories and hence initial conditions of both regions by comparing the observed values to $N$-body simulations at appropriate ages. Stars in both regions likely formed with sub-virial velocities which contributed to merging of substructure and the formation of smooth clusters. The initial stellar densities were no higher than $\rho \sim 100-500$M${}_{\odot }$pc${}^{-3}$ for IC348 and $\rho \sim 500-2000$M${}_{\odot }$pc${}^{-3}$ for NGC1333. These initial densities, in particular that of NGC1333, are high enough to facilitate dynamical interactions which would likely affect $\sim$10 per cent of protoplanetary discs and binary stars.

13 pages, 9 figures, accepted for publication in MNRAS (23.03.2017)

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