Top: The Hidden Cooling flow Rates (HCR upper points) and the lower SFRs from (McDonald et al. 2018) plotted against the Imaging Cooling flow rates (IMR). Note that for many objects the HCR and IMR are about a factor of 20 above the SFR. Bottom: The ratio of imaging to hidden mass cooling rates (IMR/HCR) plotted against imaging rates. When |${\rm IMR}\lt 10{{\rm \, {\rm M}_{\odot }}{\rm \, yr}^{-1}\, }$| the two rates are mostly comparable, but above that value the |${\rm IMR} \gt {\rm HCR}$| by up to a factor of 10 or more. This zone in parameter space is coloured pink. The difference between IMR and HCR rates, which cover different size regions (the imaging cooling region being much larger than the hidden cooling one) is presumably made up by AGN feedback heating and offsetting cooling of outer gas. Objects from left to right and where relevant top to bottom are M84, NGC1600, NGC4472, NGC5846, NGC5813, HGC62, A262, Cen, M87, NGC3581, A2052, A2199, A496, NGC5044, A85, A3112, Hydra A, Cyg A, A1068, 2A0335, S159, A2597, Per (upper limit), ZW3146, R1931, R1532, A1835 (upper limit), and RXJ1504.he text/caption for Fig. X currently contains reference to colour used within the figure. For accessibility purposes, reference to colour should be avoided. If possible, please update the wording for the figure caption to remove reference to colour. Make any changes directly in the text.