ar X iv : a st ro - p h / 06 09 17 6 v 1 6 S ep 2 00 6 Two Bipolar Outflows and Magnetic Fields in a Multiple Protostar System , L 1448 IRS 3

We performed spectral line observations of CO J = 2 → 1, CO J = 1 → 0, and CO J = 1 → 0 and polarimetric observations in the λ = 1.3 mm continuum and CO J = 2 → 1 toward a multiple protostar system, L1448 IRS 3, in the Perseus molecular complex at a distance of ∼ 250 pc, using the BIMA array. In the λ = 1.3 mm continuum, two sources (IRS 3A and 3B) were clearly detected with estimated envelope masses of 0.21 and 1.15 M⊙, and one source (IRS 3C) was marginally detected with an upper mass limit of 0.03 M⊙. In CO J = 2 → 1, we revealed two outflows originating from IRS 3A and 3B. The masses, mean number densities, momentums, and kinetic energies of outflow lobes were estimated. Based on those estimates and outflow features, we concluded that the two outflows are interacting and that the IRS 3A outflow is nearly perpendicular to the line of sight. In addition, we estimated the velocity, inclination, and opening of the IRS 3B outflow using Bayesian statistics. When the opening angle is ∼ 20, we constrain the velocity to ∼ 45 km s and the inclination angle to ∼ 57. Linear polarization was detected in both the λ = 1.3 mm continuum and CO J = 2 → 1. The linear polarization in the continuum shows a magnetic field at the central source (IRS 3B) perpendicular to the outflow direction, and the linear polarization in the CO J = 2 → 1 was detected in the outflow regions, parallel or perpendicular to the outflow direction. Moreover, we comprehensively discuss whether the binary system of IRS 3A and 3B is gravitationally bound, based on the velocity differences detected in CO J = 1 → 0 and CO J = 1 → 0 observations and on the outflow features. The specific angular momentum of the system was estimated as ∼ 3 × 10 cm s, comparable to the values obtained from previous studies on binaries and molecular clouds in Taurus. Additionally at National Center for Supercomputing Applications Currently at Department of Physics and Astronomy, Cardiff University