{'fraction_non_alphanumeric': 0.03726169844020797, 'fraction_numerical': 0.022530329289428077, 'mean_word_length': 4.552884615384615, '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}}
[Ne V] Imaging of the Cygnus Loop

We present continuum-subtracted images of a 20′ × 20′ region of the eastern Cygnus Loop (NGC 6995) in the 3425 Å forbidden line of Ne V. The images reveal bright linear filaments which are associated with, but not positionally coincident with, bright features seen in Hα, [O III], and other narrowband images. In some areas, the [Ne V] filaments define the edge of X-ray-emitting regions. The filaments exhibit a peak surface brightness of 1.2 × 10-4 photons cm-2 s-1 arcsec-2 at the top of the atmosphere in images with typical detection limits of ~10-5 photons cm-2 s-1 arcsec-2. We present arguments that these structures are produced by radiative shock waves and discuss implications for the shock velocities and the three-dimensional structure of this section of the Cygnus Loop. We place limits on the importance of thermal conduction-driven evaporation as a contribution to the mass of X-ray-emitting gas. Lack of evidence of [Ne V] emission resulting from thermal evaporation may have significance for supernova remnants and interstellar medium models that rely heavily on the importance of thermal evaporation.