tokens: timing solution in NGC 6624 (pulsars D, E, F, and H), as well as to validate the timing position derived for the new eccentric binary MSP (pulsar G). With the observing setup used for the two TRAPUM observations of this cluster (obs. ids 10L-trapum and 12L-trapum) reported in Section 2 , the individual beams making up the tiling have elliptic shapes with semi-axes in the range of ∼8–11 arcsec at half power, with the exact values depending on the elevation and other factors. We assume these values as the maximum uncertainty for the positions that we derive for these pulsars. The results are summarized in Table 5 , where we list the beams in which each pulsar was detected with highest S/N, and their boresight coordinates. The same is shown graphically in Fig. 9 , where the beams with localized pulsars are higlighted in grey. As can be seen, pulsars D and H are found to be the closest to the cluster centre. The eclipsing redback F and the isolated pulsar E are found at the much larger distances of ∼0.42 and ∼0.79 arcmin from the cluster centre, respectively, putting the former near the edge of, and the latter well outside, the half-power of the tied-array beam of the MeerTime observations (which used only the 1-km core antennas) of NGC 6624. This explains why NGC 6624F and E are detected with significantly lower S/N than expected in the MeerTime data as compared to the TRAPUM data, even after accounting for the different number of antennas used. Finally, the eccentric binary pulsar NGC 6624G showed up with highest S/N in beam #002. This had boresight coordinates of α = 18 h 23 m 41150 and δ = −30°21 ′ 3850. This is just ∼6.2 arcsec away from, and therefore consistent with, the corresponding timing-derived position of G. Figure 9. Tiling of the first TRAPUM observation (obs. id 10L-trapum) of NGC 6624. 60 dishes were used to synthesize 288 beams, with an overlap fraction of 80 per cent, around the nominal centre position of the cluster. The light-grey ellipses show the contours of the TRAPUM beams at their 84 per cent level of the power of their boresights, at 1284 MHz. We highlight in solid grey those beams where some of the pulsars show up with the highest S/N: the name of such pulsars are shown next to the beam number. The red ellipses show, for comparison, the L -band beam (at half power for top, centre, and bottom of the band) of one of the MeerTime observations of NGC 6624, which used only 42 antennas of the 1-km core of the array. Table 5. List of the NGC 6624 pulsars without a known position and corresponding beams where they were detected with highest S/N in the first TRAPUM observation of the cluster (id 10L-trapum). θ ⊥ is the angular distance between the beam boresight and the nominal cluster centre. 4.2.3 L-band detection of the transitional pulsar M28I M28I (also known as PSR J1824−2452I) is a redback system in M28 beloging to the rare class of transitional MSPs (see Jaodand, Hessels Archibald 2018 ; Papitto de Martino 2020 for
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