Figure 5.
![The predicted JWST spectrum of a low-redshift cooling flow and a variety of lowest flow temperatures. The upper panel shows the wavelength range detected by NIRSpec ($0.6\!-\!5\,\mu$m) while the lower panel shows MIRI ($5\!-\!28\,\mu$m). Very low ionization [Fe ii] and [N i] lines are strong in flows that cool down to $\sim 10^3$ K but are absent in flows that are reheated at higher temperatures. The spectrum is normalized to a cooling flow of 1 ${{\rm \, {\rm M}_{\odot }}{\rm \, yr}^{-1}\, }$ at the distance of the Centaurus cluster $z=0.0104$. The results in Fig. 1 suggest that the flow is about $14 {{\rm \, {\rm M}_{\odot }}{\rm \, yr}^{-1}\, }$.](https://oup.silverchair-cdn.com/oup/backfile/Content_public/Journal/mnras/535/3/10.1093_mnras_stae2414/3/stae2414fig5.jpeg?Expires=1749787600&Signature=CcjJwIvxkKciuOsR8Cj32MxMZZa0kde2iYY3ikUXsXl7BJoYeBmSPoHfy66XeACIWIgb1cvjW8JoChsvvIoxCwhas2Osr87iuR8mgd-P9tWmy0bLJ68Y8tdpZQeWvKC9l2cZLlTxRex~CVzA1ilhWH8PZvQMt3NDXVAG14ZaTKPHNcN2nAzqCn6lEgUDJ8t~8siPDU7afXrUUIlkizB3hG6VYskdBWvaV7QNpgi-hET~yqsDWARHEzBZV1FujZyNvx3X5ZHaHalcIOmDlollp~hAiq4ywSD6MT85vMRqoIb5D1xqqYFwG--rTrYZNTIzVOvGZgVwxORLzpJJ5r~IpA__&Key-Pair-Id=APKAIE5G5CRDK6RD3PGA)
The predicted JWST spectrum of a low-redshift cooling flow and a variety of lowest flow temperatures. The upper panel shows the wavelength range detected by NIRSpec (|$0.6\!-\!5\,\mu$|m) while the lower panel shows MIRI (|$5\!-\!28\,\mu$|m). Very low ionization [Fe ii] and [N i] lines are strong in flows that cool down to |$\sim 10^3$| K but are absent in flows that are reheated at higher temperatures. The spectrum is normalized to a cooling flow of 1 |${{\rm \, {\rm M}_{\odot }}{\rm \, yr}^{-1}\, }$| at the distance of the Centaurus cluster |$z=0.0104$|. The results in Fig. 1 suggest that the flow is about |$14 {{\rm \, {\rm M}_{\odot }}{\rm \, yr}^{-1}\, }$|.
