instrument, [@McFadden1987] derived the water production rates from OH (3090 Å) emission. [@Fink1996] derived the water production rates from the \[OI\]($^1$D) forbidden line doublet using a correlation between the water production rates and the total photon luminosity. [@Faggi2019] and [@Roth2020] measured directly the water production rates from near-infrared spectra. TRAPPIST and UVES data points are from this work (see section \[water-production-rate\] and \[uves-water-production-rate\]). The maximum in the last four apparitions was reached about one month before perihelion and does not change over all apparitions, but we observe a clear systematic difference between the narrow band and spectroscopic methods in the optical on one hand and the measurements made from the space observations of the H Ly-$\alpha$ emission in the UV on the other hand. The maximum of the water production we measured was on August 17, 24 days before the perihelion, and it reached (3.72$\pm$0.07)$\times$10$^{28}$ molec/s in good agreement with [@Schleicher2018] measurement of 4.20$\times$10$^{28}$ molec/s at the heliocentric distance 1.07 au. Using the same technique for the 1985 apparition, [@Schleicher1987] reported Q(H$_2$O)=4.85$\times$10$^{28}$ molec/s when the comet was at 1.05 au from the Sun. Using high resolution infrared spectroscopy, [@Weaver1999] measured $\sim$2–3$\times$10$^{28}$ molec/s at r$_h$=1.10 au in 1998. For the 2005 