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. Author manuscript; available in PMC: 2020 Nov 3.
Published in final edited form as: Mon Not R Astron Soc. 2020 Sep 1;498(4):4605–4614. doi: 10.1093/mnras/staa2640

Figure 1.

Figure 1.

Difference between the measured candidate spin frequency of PSR J0537–6910 and linear model for frequency evolution, v4 + v̇4(t − t4), where v4 and v̇4 are values from segment 4 at t4 = MJD 58493 (see Table 1). Segments are labeled by numbers and separated by the occurrence of a glitch, each of which is denoted by a vertical dashed line.