Closing the feedback loop With the improved calibration of the ALMA observation we are able to trace in the detailed morphology and kinematics of the filaments of cold molecular gas of and the CND in the central regions of NGC 1275. The data clearly show how kpc-sized filaments flow towards the CND and how they are accreting onto the CND, building it up in mass. This on-going formation of the CND is further confirmed by the non-regular kinematics of the outer regions of the CND which suggest that the gas there is not in a kinetically relaxed state due to the arrival of new filaments. This allows us to complete the picture of the gas cycle in NGC 1275. Several authors have suggested that in NGC 1275 we observe a mixture of heating and cooling processes in the gaseous medium driven by the AGN, and how these processes could be connected to AGN fuelling (Salomé et al. 2006; Lim et al.2008; Scharwächter et al. 2013). Multi-phase outflows driven by the jets, cool as they rise, leading to formation of colder gas filaments (Qiu et al. 2020). Earlier studies have proposed these filaments may fall back and accrete onto the CND and eventually fuel the AGN (Salomé et al. 2006; Lim et al 2008), similar as in models of AGN-driven accretion models (Gaspari et al. 2017). This would close the feedback and fuelling loop of the AGN. Our results from ALMA provide the observational evidence that this process is indeed occurring. Molecular gas feeding 3C 84 Past observations with a resolution of about 1 kpc of the cold molecular gas in the regions of NGC 1275 hosting the radio-loud AGN 3C 84, have shown that it is primarily concentrated in three radial filaments aligned in the east-west direction that could be radially in-falling gas and feeding a CND (Lim et al. 2008; Ho et al. 2009). However, the relatively low spatial resolution does not allow to separate these large filaments from the CND and to establish whether the filaments are actually accreting onto the CND. Using the much better resolution of ALMA (∼50 pc), Nagai et al. (2019) were able to identify a rotating CND of cold molecular gas in NGC 1275. However, due to bandpass calibration issues due to the strong flux of 3C 84, their data cube suffers from strong imaging artefacts which prevent investigating the possible connection between the filaments and the CND. Here we present results from re-processing these ALMA observations, using a different bandpass calibration scheme which resulted in much improved image quality (see Fig. 5). This has allowed us to clearly detect, with 50 pc resolution, the detailed distribution and kinematics of the molecular gas in the central kpc region of NGC 1275. The main results are shown in Figs 1, 2 and 3 where we present the integrated line emission and the velocity field of the CO(2-1). They show that the distribution and the kinematics of the molecular gas are much more complex than perceived from the Lim et al. and Ho et al. data. Furthermore, they separate the filaments and the CND for the first time and allow us to study the connection between the CND and the molecular gas in the central regions of NGC 1275, and how the large filaments are feeding the CND. Closing the feedback-feeding loop of the radio galaxy 3C 84 Tom Oosterloo1,2, Raffaella Morganti1,2 & Suma Murthy3 1ASTRON, the Netherlands Institute for Radio Astronomy, Oude Hoogeveensedijk 4, 7991 PD Dwingeloo, The Netherlands. 2Kapteyn Astronomical Institute, University of Groningen, Postbus 800, 9700 AV Groningen, The Netherlands 3Joint Institute for VLBI ERIC, Oude Hoogeveensedijk 4, 7991 PD Dwingeloo, The Netherlands. Gas accretion by a galaxy’s central super massive black hole (SMBH) and the resultant energetic feedback by the accreting active galactic nucleus (AGN) on the gas in and around a galaxy, are two tightly intertwined but competing processes that play a crucial role in the evolution of galaxies. Observations of galaxy clusters have shown how the plasma jets emitted by the AGN heat