Carma Observations of Protostellar Outflows in NGC 1333

Abstract

We present observations of outflows in the star-forming region NGC 1333 using the Combined Array for Research in Millimeter-Wave Astronomy (CARMA). We combined the 12 CO and 13 CO (1-0) CARMA mosaics with data from the 14-m Five College Radio Astronomy Observatory (FCRAO) to probe the central, most dense and active region of this protostellar cluster at scales from 5 to 7 (or 1000 AU to 0.5 pc at a distance of 235 pc). We map and identify 12 CO outflows, and along with 13 CO data we estimate their mass, momentum and energy. Within the 7 × 7 map, the 5 resolution allows for a detailed study of morphology and kinematics of outflows and outflow candidates, some of which were previously confused with other outflow emission in the region. In total, we identify 22 outflow lobes, as well as 9 dense circumstellar envelopes marked by continuum emission, of which 6 drive outflows. We calculate a total outflow mass, momentum and energy within the mapped region of 6 M , 19 M km s −1 , and 7 ×10 44 erg, respectively. Within this same region, we compare outflow kinematics with turbulence and gravitational energy, and we suggest that outflows are likely important agents for the maintenance of turbulence in this region. In the earliest stages of star formation, outflows do not yet contribute enough energy to totally disrupt the clustered region where most star formation is happening, but have the potential to do so as the protostellar sources evolve. Our results can be used to constrain outflow properties, such as outflow strength, in numerical simulations of outflow-driven turbulence in clusters.

Do siblings always form and evolve simultaneously? Testing the coevality of multiple protostellar systems through SEDs

“…One of the components in SVS13A is expected to be the driving source of HH 7-11 (Rodríguez et al 1997;Looney et al 2000). SVS13A is observed to have a prominent molecular outflow in the SE-NW direction with a moderate inclination angle and wide opening angles (Plunkett et al 2013). These outflow characteristics together with the presence of a centimeter source and being the exciting source for HH 7-11 (Rodríguez et al 1997) suggest that SVS13A is a Class 0/I transition object.…”

“…NGC 1333 SVS13A shows molecular outflow lobes that are wide and shell-like, while SVS13C exhibits a collimated outflow with indications of being in the plane of the sky, meaning that the disk is seen edge-on (Plunkett et al 2013;Lee et al 2016). This possible inclination misalignment might be the reason that this system appears to be non-coeval based on the SEDs.…”

The Link Between Turbulence, Magnetic Fields, Filaments, and Star Formation in the Central Molecular Zone Cloud G0.253+0.016

“…In general, potential driving mechanisms include supernova explosions and expanding radiation fronts and shells induced by high-mass stellar feedback (McKee 1989;Balsara et al 2004;Krumholz et al 2006;Breitschwerdt et al 2009;Goldbaum et al 2011;Peters et al 2011;Lee et al 2012), winds , gravitational collapse and accretion of material (Vazquez-Semadeni et al 1998;Elmegreen & Burkert 2010;Klessen & Hennebelle 2010;Vázquez-Semadeni et al 2010;Federrath et al 2011b;Robertson & Goldreich 2012;Lee et al 2015), and Galactic spiral-arm compressions of H I clouds turning them into molecular clouds (Dobbs & Bonnell 2008;, as well as magnetorotational instability (MRI) and shear (Piontek & Ostriker 2007;Tamburro et al 2009). Jets and outflows from young stars and their accretion disks have also been suggested to drive turbulence (Norman & Silk 1980;Matzner & McKee 2000;Banerjee et al 2007;Nakamura & Li 2008;Cunningham et al 2009Cunningham et al , 2011Carroll et al 2010;Wang et al 2010;Plunkett et al 2013Plunkett et al , 2015Federrath et al 2014;Offner & Arce 2014). While different drivers may play a role in different environments (such as in spiral-arm clouds), Kruijssen et al (2014) found that most of these drivers are not sufficient to explain the turbulent velocity dispersions in the CMZ.…”

First results from the CALYPSO IRAM-PdBI survey

“…SiO, CH 3 OH), revealing two perpendicular outflows, directed NE-SW (PA 25 • ; hereafter called N-S for sake of clarity) and SE-NW (PA 105 • ; hereafter E-W), both originating to within a few arcseconds from IRAS2A (e.g. Bachiller et al 1998;Knee & Sandell 2000;Jørgensen et al 2004aJørgensen et al ,b, 2009Wakelam et al 2005;Persson et al 2012;Plunkett et al 2013). These outflows seem intrinsically different, the E-W outflow being more collimated and chemically richer than the N-S one, supporting the possibility that IRAS2A is an unresolved proto-binary.…”