{'fraction_non_alphanumeric': 0.037825059101654845, 'fraction_numerical': 0.04964539007092199, 'mean_word_length': 4.578947368421052, '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}}
The Late Appearance of He I in V445 Puppis

We present a 0.9–2.5 μm spectrum of V445 Puppis obtained about 3 years after maximum brightness. The spectrum shows thermal continuum emission and two narrow, structured emission lines: He I 1.0830 μm and 2.0581 μm. We interpret this to be emission from a hydrogen-deficient, helium-rich, low-temperature nebula surrounded by an optically thick dust shell, probably carbonaceous.