{'fraction_non_alphanumeric': 0.05189732142857143, 'fraction_numerical': 0.05915178571428571, 'mean_word_length': 4.258064516129032, 'pattern_counts': {'":': 0, '<': 0, '<?xml version=': 0, '>': 1, 'https://': 0, 'lorem ipsum': 0, 'www.': 0, 'xml': 0}, 'pii_count': 0, 'substrings_counts': 0, 'word_list_counts': {'cursed_substrings.json': 0, 'profanity_word_list.json': 0, 'sexual_word_list.json': 0, 'zh_pornsignals.json': 0}}
MOLECULAR OUTFLOWS IN B 335 AND

1) B335 B335 is well studied as a typical bipolar outflow source. The high-resolution singledish maps of CO(J=1-0) (Hirano et al. 1988; Moriarty-Schieven & Snell 1989) reveal that the outflow is of biconical shape and is centered at the cold IRAS source, 19347+0727. B335 is the most suitable object to study the detailed structure of the outflow in the close vicinity of its driving source, because the outflow axis has a small inclination angle (-10°) to the plane of the sky. In Figure 1 we present the distribution of the blueshifted emission (VL S R = 7.84 km s-1; solid contours), the redshifted emission (VLSR = 9.46 km s-1; dashed contours), and the 2.6 mm continuum emission (gray scale). The blueshifted and redshifted CO emission shows distinct biconical structure. Two prominent peaks are separated by 10" (= 2400 AU) in blueshifted component and 15" (= 3600 AU) in redshifted one. The north-south extent of the outflow at its center is less than 8" (= 2000 AU), indicating that the outflow is focused within ~ 1000 AU of its origin. The 2.6 mm continuum peak whose flux is ~ 80 mJy is located within 4" of the outflow center. The 2.6 mm continuum flux combined with the previous far-infrared and submillimeter measurements (Keene et al. 1983; Gee et al. 1985; Chandler et al. 1990; IRAS Point Source Catalog, Version 2, 1988) suggest that the very dense (> 108 cm-3) and massive (1.7 2.9 M®) core is surrounding the young stellar object; such high density material may be responsible for collimating the outflow. In the vicinity of the origin, the flow velocity shows a sudden increase away from the center (see Figure 3 of Hirano et al. 1992). A simple dynamical model of the expanding "snowplowing" shell can explain the velocity field of B335.