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Outflows in protostellar clusters: a multi-wavelength, multi-scale view Adele L. Plunkett1, H. G. Arce1, S. A. Corder2, M. M. Dunham1, D. Mardones3 1-Yale University; 2-ALMA; 3-Universidad de Chile Interferometer and Single Dish Overview Combination FCRAO-only v=-2 to 6 km/s FCRAO-only v=10 to 17 km/s K km s While protostellar outflows are generally understood as necessary components of isolated star formation, further observations are -1 needed to constrain parameters of outflows particularly within protostellar clusters. In protostellar clusters where most stars form, outflows impact the cluster environment by injecting momentum and energy into the cloud, dispersing the surrounding gas and feeding turbulent motions. Here we present several studies of very dense, active regions within low- to intermediate-mass Why: protostellar clusters. Our observations include interferometer (i.e. CARMA) and single dish (e.g. FCRAO, IRAM 30m, APEX) To recover flux over a range of spatial scales in the region observations, probing scales over several orders of magnitude. How: Based on these observations, we calculate the masses and kinematics of outflows in these regions, and provide constraints for Jy beam km s Joint deconvolution method (Stanimirovic 2002), CARMA-only v=-2 to 6 km/s CARMA-only v=10 to 17 km/s models of clustered star formation. These results are presented for NGC 1333 by Plunkett et al. (2013, ApJ accepted), and -1 comparisons among star-forming regions at different evolutionary stages are forthcoming. using the analysis package MIRIAD. -1 1212COCO Example: We mapped NGC 1333 using CARMA with a resolution of ~5’’ (or 0.006 pc, 1000 AU) in order to Our study focuses on Class 0 & I outflow-driving protostars found in clusters, and we seek to detect outflows and associate them with their driving sources. understand their impact on the protocluster environment. To the right, we label several tracers CARMA+FCRAO v=-2 to 6 km/s CARMA+FCRAO v=10 to 17 km/s Jy beam km s 12 CONTINUUMCONTINUUM important to our study of cores (i.e. continuum), outflows ( CO) and their impact on the -1 13 The single dish FCRAO map of NGC 1333 is used envelope and cloud (13CO). Further, the temperature structure of these components is COCO -1 to recover the flux over larger spatial scales determined by observing several energy-level transitions of these molecules. (up to the map size of ~8’, or 0.5 pc) (Figure 5 of van Dishoeck et al. 2011) that is resolved out by the interferometer. 1212COCO Case Study: NGC 1333 Serpens South Plunkett et al. (2013, ApJ accepted) vout=-3 to -10 km/s vout=-10 to -30 km/s @ 415 pc 0.5 pc vout=-5 to -2 km/s vout=-8 to -5 km/s vout=-10 to -8 km/s = 3 to 10 km/s = 10 to 30 km/s = 1 to 3 km/s = 3 to 7 km/s = 7 to 9 km/s ows C3 C4 Region I: SVS 13 fl F4 ows fl SVS 13A SVS13A F1 Out + + B + C F3 F2 F3 Out Region II: IRAS 2 Background: IRAC 4.5 μm Red/Blue contours: CARMA CO(1-0) White contours: 2.7 mm continuum About + + +A + + + Spitzer IRAC Spitzer IRAC B Gutermuth et al. (2008a) APEX Location: Serpens; RA 18:30, dec -02:02 Gutermuth et al. (2008b) CO(3-2) Distance: 415 pc (Dzib et al. 2010) Age: ~2x105 yrs, very young “protocluster” (Gutermuth et al. 2008a) <CARMA mapped region> Membership: Protostar fraction (class I relative to all YSOs) of 80% at Region IV SK1 Western Knot Background: center (Nakamura et al. 2011) Region I IRAC 4.5 μm Contours: CARMA Significance: Protostars densely clustered along a central filamentary CO(1-0) SK 14 Region III: IRAS 4 -2 Region II structure, where high number density of protostars (reaching 430 pc at the center) likely has a profound impact on the cloud. + + 4D+ IRAS 4 + + + 4A + + + + 4C+ +4B C2 C1 C2 Circinus and M8 Region III Region IV: SVS 13C, SK 14 Region V 1 pc @ d=1250 pc ow fl About NGC 1333 Out Candidates Location: Perseus; RA 03:29, dec 31:14 + + Distance: 235 pc (Hirota et al. 2008) +SVS 13C 6 Age: ~10 years (Lada et al. 1996) SK 14 Members: 39 protostars, 98 pre-MS stars with disks, two late-B stars to north (Gutermuth et al. 2008b) APEX APEX WISE (22, 12, 4.6 micron) Spitzer IRAC CO(3-2) CO(3-2) Significance: NGC 1333 is considered the prototypical cluster, commonly used to model Liu et al. (2011) Credit: NASA/JPL-Caltech clustered star formation and outflow-driven turbulence (e.g. Nakamura & Li 2007). Circinus M8 (Lagoon) Location: 15h, -63° Location: Sag-Carina Arm; 18h, -24° NGC 1333 Results Distance: 700 pc (Bally et al. 1999) Distance: 1250 pc (Arias et al. 2006) Significance: Three IRAS point Significance: A more massive, more •Within NGC 1333, outflow kinetic energy, cloud gravitational energy and turbulent energy suggest that outflows act as an sources (marked to the right with evolved counter-part to the other red stars, Shimoikura & Dobashi regions in our survey, yet M8 important agent for turbulence in the region, and over time could disrupt the most active region of the cloud. 2011) are likely driving outflows in remains an active site of star the mapped region. It is apparent formation. Within the mapped •We identify outflows associated with 5 (of 7) Class 0 and 2 (of 4) Class I sources within the mapped region of NGC 1333. from the CO map that the red- region are many sub-mm gas shifted molecular outflow emission clumps (open stars) and Class 0/I is more dispersed than the blue. objects (yellow stars), based on •~10-25% of the final mass of a protostar comprises the protostellar wind and may drive momentum in the cluster environment, Kumar & Anandarao (2010). and should be taken into account in models that investigate the impact of outflows during early protostellar evolution. •Similar analyses of the regions Serpens South, Circinus and M8 are ongoing. How do the outflow References Arias, J.I., et al. 2006, MNRAS 366, 739 ● Bally, J., Reipurth, B., Lada, C. J., & Billawala, Y. 1999, AJ, 117, 410 ● Dzib, S., Loinard, L., Mioduszewski, A.J., et characteristics apparent in NGC 1333 evolve with, depend on, and/or affect their surrounding environments? al. 2010, ApJ, 718, 610 ● Gutermuth, R.A., Bourke, T.L., Allen, L.E., et al. 2008a, ApJL, 673, L151 ● Gutermuth, R. A., et al. 2008b, ApJ, 674, 336 ● Hirota, T., Bushimata, T., Choi, Y.K., et al. 2008, PASJ, 60, 37 ● Kumar, D. L., & Anandarao, B. G. 2010, MNRAS, 407, 1170 ● Lada, C.J., Alves, J., & Lada, E.A. 1996, AJ, 111, 1964 ● Nakamura, F., & •Preliminary analysis of Serpens South suggests that at least four sources are driving outflows from within a Li, Z.Y. 2007, ApJ, 662, 395 ● Nakamura, F., Sugitani, K., Shimajiri, Y., et al. 2011, ApJ, 737, 56 ● Shimoikura, T., & Dobashi, K. 2011, ApJ, 731, 23 ● Stanimirovic, S. 2002, Single-Dish Radio Astronomy: Techniques and Applications, 375–396 ● van Dishoeck, E.F., & Blake, G.A. 1998, ARA&A, 36, 317 ● van Dishoeck, E.F., Kristensen, L.E., region much more dense and active than the region we mapped in NGC 1333. Benz, A.O., et al. 2011, PASP, 123, 138 •Single-dish observations of Circinus and M8 provide evidence of outflow activity, and with higher-resolution Acknowledgements A.L.P. is a NSF Graduate Research Fellow. A.L.P. was supported by mosaic observations we will associate driving sources and molecular outflow emission across several parsecs. Fulbright Chile in 2012, and hosted at Cerro Calán, Universidad de Chile in 2012-13. This project is supported by the National Science Foundation under grant AST-0845619 made to H.G.A. •The extent to which we can identify outflows and their driving sources may correlate with the evolutionary Summary state of the cluster environment, and the possibility for outflows to disrupt the cloud over time..
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