rotation of the nucleus. We chose the exposure time of the different filters depending on the brightness of the comet. We used exposure times between 60 s and 240 s for the broad-band filters and between 600 s and 1500 s for the narrow-band filters. Observational circumstances and number of sets of each filter are summarized in Table \[circ\] in the appendix. We started to collect data three months before perihelion to four months after perihelion. The comet reached perihelion on September 10, 2018 at a heliocentric distance of 1.01 au and a geocentric distance of 0.39 au. In total the comet was observed on 50 different nights with both telescopes, 13 nights before perihelion and 37 after. We used the same procedures described in our previous papers (e.g, [@Opitom2015a; @Moulane2018] and references therein) to reduce the data and to perform the flux calibration. To compute the production rates, we converted the flux of different gas species to column densities and we adjusted their profiles with a Haser model [@Haser1957]. This simple model, but widely used, is based on a number of assumptions. Outgassing is assumed to be isotropic and the gas has a constant radial velocity of 1 km/s. 