Figure 7.
![Emission-line surface brightness profile for the nebula around HE 0238−1904. The [O ii] and [O iii] profiles are extracted over a velocity interval of −600 to $600 \, \rm km \, s^{-1}$, and are circularly averaged at different distances from the quasar centroid. The profile of [O ii] declines smoothly as a function of radius, while the [O iii] exhibits shallower drop due to the bright knots seen in the narrow-band images.](https://oup.silverchair-cdn.com/oup/backfile/Content_public/Journal/mnras/527/3/10.1093_mnras_stad3364/1/stad3364fig7.jpeg?Expires=1749753906&Signature=UtXVfiPsakiFNckx7BU3prttcsitrQklpygpijeEzRj2YqwG1TYplhB2oMA4gdHbXe573THWvJl2MxyJqXvRtlwohW~wO4zwFuKoRJnx6ei0NZ3qMit163SEnJ08nZTPCh4HYxvtdO6SEy3JSj4Gl96u-pn6XfzcsUWC2l7acY1GbCfF0eQnbJV4NX4pAe4tb40TF6qJMjdF39MkclJM9Ti5g1KkUKibApMXShnnfvdddAatDXweyQW7KSYItS~CJnOStah9a~FDJEAL1J5XpxEDeaV26EbAGpXMYpp1nD1oFCQm4bglumanti7OR89d8sD038Eb72unfHpwKpAvGg__&Key-Pair-Id=APKAIE5G5CRDK6RD3PGA)
Emission-line surface brightness profile for the nebula around HE 0238−1904. The [O ii] and [O iii] profiles are extracted over a velocity interval of −600 to |$600 \, \rm km \, s^{-1}$|, and are circularly averaged at different distances from the quasar centroid. The profile of [O ii] declines smoothly as a function of radius, while the [O iii] exhibits shallower drop due to the bright knots seen in the narrow-band images.
