PROSAC: A Submillimeter Array Survey of Low-Mass Protostars. I. Overview of Program: Envelopes, Disks, Outflows, and Hot Cores

By J. Jørgensen, T. Bourke, P. Myers, J. di Francesco, E. V. van Dishoeck, Chin-Fei Lee, N. Ohashi, F. Schoeier, S. Takakuwa, D. Wilner and 1 more. 2007

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This paper presents a large spectral line and continuum survey of eight deeply embedded, low-mass protostellar cores using the SMA. High-excitation line emission from 11 molecular species originating in warm and dense gas has been imaged at high angular resolution (1''-3'', typically 200-600 AU) together with continuum emission at 230 GHz (1.3 mm) and 345 GHz (0.8 mm). Compact continuum emission is observed for all sources, which likely originates in marginally optically thick circumstellar disks, with typical lower limits to their masses of 0.1 M☉ (1%-10% of the masses of their envelopes) and a dust opacity law, κν ∝ νβ, with β ≈ 1. Prominent collimated outflows are present in CO 2-1 observations in all sources. The most diffuse outflows are found in the sources with the lowest ratios of disk to envelope mass, and it is suggested that these sources are in a phase where accretion of matter from the envelope has almost finished and the remainder of the envelope material is being dispersed by the outflows. Other characteristic dynamical signatures are inverse P Cygni profiles indicative of infalling motions seen in the 13CO 2-1 lines toward NGC 1333 IRAS 4A and NGC 1333 IRAS 4B. Outflow-induced shocks are present on all scales in the protostellar environments and are most clearly traced by the emission of CH3OH in NGC 1333 IRAS 4A and NGC 1333 IRAS 4B. These observations suggest that the emission of CH3OH and H2CO from these proposed ``hot corinos'' is related to the shocks caused by the protostellar outflows. Only one source, NGC 1333 IRAS 2A, has evidence for hot, compact CH3OH emission coincident with the embedded protostar.

Subfields: Astronomy and Astrophysics, Atmospheric Science, Spectroscopy

View Paper: https://www.semanticscholar.org/paper/f8eb3c43dd43f5f1b7fc3a0471929ed87400ad17

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Citations in the corpus

Protoplanetary Disks and Their Evolution (2011, background): “Multi-wavelength observations of Class 0 cores by Jørgensen et al. (2007) and Kwon et al. (2009) show opacity indices, β ≈ 1, also shallower than the diffuse interstellar medium but not quite as steep as in protoplanetary disks.”
THE VLA NASCENT DISK AND MULTIPLICITY SURVEY OF PERSEUS PROTOSTARS (VANDAM). II. MULTIPLICITY OF PROTOSTARS IN THE PERSEUS MOLECULAR CLOUD (2016, methodology): “NGC 1333 IRAS4A was observed by Looney et al. (2000) and Jørgensen et al. (2007) at 2.7 mm and 1.3 mm, respectively.”
Complex Molecules in the L1157 Molecular Outflow (2008, background): “…clearly demonstrated by multi-molecular line observations reflecting enhanced molecular abundances either in shocks associated with the outflows or in the outflow cavity walls in the protostellar envelopes (e.g., Garay et al. 1998; Bachiller et al. 2001; Arce & Sargent 2006; Jørgensen et al. 2007).”
Water in star-forming regions with Herschel (WISH). II. Evolution of 557 GHz 110-101 emission in low-mass protostars (2012, background): “Furthermore, these objects have been the targets of numerous physical and chemical surveys (e.g., Hogerheijde et al. 1999; Shirley et al. 2000; Jørgensen et al. 2002, 2004b, 2007; Emprechtinger et al. 2009; Kristensen et al. 2010a,b).”
TADPOL: A 1.3 mm SURVEY OF DUST POLARIZATION IN STAR-FORMING CORES AND REGIONS (2013, background): “Its bipolar outflow is oriented in the east-west direction and is nearly in the plane of the sky, which makes the object an ideal target for studying the disk and outflow structure at the earliest stage of low mass star formation (e.g., Jørgensen et al. 2007).”
PROSAC: a submillimeter array survey of low-mass protostars - II. The mass evolution of envelopes, disks, and stars from the class 0 through I stages (2009, methodology): “That something like this may be going on is hinted by the observation that the compact components around the Class 0 sources show spectral slopes,α, of the emissionFν ∝ να, at 230 and 345 GHz in the range 2– 3 (Jørgensen et al., 2007a).”
Our astrochemical heritage (2012, methodology): “[246]; [336]), also found soon after protostellar birth, in Class 0 objects ([228]; [253]; [103]).”
Water in Star-forming Regions with the Herschel Space Observatory (WISH). I. Overview of Key Program and First Results (2010, background): “All sources have d < 450 pc and are well characterized with a variety of other single-dish submillimeter telescopes and interferometers (Jørgensen et al. 2004, 2007).”
Protostellar disk formation and transport of angular momentum during magnetized core collapse (2012, unknown): “Although as stressed by these authors, these estimates depend on the assumptions made regarding the envelope (Jørgensen et al. 2007, 2009; Enoch et al. 2009, 2011).”
The chemical history of molecules in circumstellar disks - I. Ices (2009, background): “However, the lack of widespread red-shifted absorption seen in interferometric observations suggests that the infall may stop already at an earlier time (Jørgensen et al. 2007).”