{'fraction_non_alphanumeric': 0.03684210526315789, 'fraction_numerical': 0.03984962406015038, 'mean_word_length': 4.302788844621514, 'pattern_counts': {'":': 0, '<': 0, '<?xml version=': 0, '>': 0, '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}}
A Catalog of Molecular Clumps and Cores with Infall Signatures

The research of infall motion is a common means to study molecular cloud dynamics and the early process of star formation. Many works had been done in-depth research on infall. We searched the literature related to infall study of molecular cloud since 1994, summarized the infall sources identified by the authors. A total of 456 infall sources are cataloged. We classify them into high-mass and low-mass sources, in which the high-mass sources are divided into three evolutionary stages: prestellar, protostellar and H ii region. We divide the sources into clumps and cores according to their sizes. The H2 column density values range from 1.21 × 1021 to 9.75 × 1024 cm−2, with a median value of 4.17 × 1022 cm−2. The H2 column densities of high-mass and low-mass sources are significantly separated. The median value of infall velocity for high-mass clumps is 1.12 km s−1, and the infall velocities of low-mass cores are virtually all less than 0.5 km s−1. There is no obvious difference between different stages of evolution. The mass infall rates of low-mass cores are between 10−7 and 10−4 M ⊙yr−1, and those of high-mass clumps are between 10−4 and 10−1 M ⊙yr−1 with only one exception. We do not find that the mass infall rates vary with evolutionary stages.