Fig. 7.
Long-term spin down of CXOU J225355.1+624336 from ROSAT, Swift, Chandra, and XMM–Newton measurements (updated from Esposito et al. 2013). We attributed an error of 0.02 s to each point, reflecting the uncertainty due to the orbital motion (see Esposito et al. 2013 for details). The grey line indicates the best-fitting period derivative, Ṗ ≈ 5.3 × 10−10 s s−1.
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