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Table 2.

Properties of the five bursts that have a peak flux at least 4 times the quiescent emission levels of ∼0.5 mJy in Stokes V.

Central Duration Central phase τvar Rmax log 10 ( T b min ) $ \log_{10}(T_{b}^{\min}) $ L Drift V/I Type
time (UT) (minutes) 1, Φ2) (s) (R) (K) (1023 erg s−1) (Mhz/s) (%)
21/01-09:50 ∼45 0.40, 0.96 300 179.1 6.5 9.1 Irregular ∼87 F, G?
21/01-12:15 ∼30 0.78, 0.93 240 142.9 6.3 4.1 Irregular ∼81 G?
21/01-13:01 ∼10 0.88, 0.19 30 16.6 8.1 3.5 −1.3 ∼88 D, G?
20/02-07:40 ∼15 0.86, 0.10 80 47.2 7.1 2.7 −0.9 ∼68 D?
20/02-13:00 ∼10 0.68, 0.12 100 59.7 6.8 2.2 −1.4 ∼76 D?

Notes. The third column indicates the central phases, Φ1 and Φ2, when the light curve is folded with the primary and secondary period from Bouma et al. (2024). The variability timescale, τvar, is evaluated as the time it takes for the flux to rise to the peak value, from half of it. This provides the approximate constraints on the maximum size of the emitting region as Rmax = var, the minimum associated brightness temperature (Tbmin, see e.g. Smith et al. 2003). The last column indicates the tentative labeling of burst type proposed by Bloot et al. (2024), relying on the case-by-case evaluation of duration, drift rate, and polarization fraction listed in the purely phenomenological classification of Bloot et al. (2024). The luminosity is defined as L = Fνfbd2Δν (see text for more details).

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