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On the spin-down rate of Swift J1822.3-1606

ATel #3944; G. L. Israel (INAF-OAR), P. Esposito (INAF-OAC), N. Rea (CSIC-IEEC), R. Turolla (U. Padua), S. Zane (MSSL/UCL), S. Mereghetti (INAF-IASF Mi), A. Tiengo (INAF-IASF Mi) on behalf of a larger collaboration
on 29 Feb 2012; 15:14 UT
Credential Certification: GianLuca Israel (gianluca@mporzio.astro.it)

Subjects: X-ray, Neutron Star, Soft Gamma-ray Repeater, Transient, Variables, Pulsar

After more than 7.5 months since the burst detection from Swift J1822.3-1606 (occurred on 2011 July the 14th; Cummings et al. ATel. \#3488) more than 60 pointings have been collected. We used all public data available to date (RXTE, Swift, Suzaku) plus two proprietary XMM-Newton pointings in order to infer a refined phase-coherent timing solution.

We obtained the following best-fit coherent solution: P=8.43772012(3) s and dP/dt = 9.2(6) x 10^-14 s/s (MJD 55757.0 was used as reference epoch; 1sigma c.l. is assumed for the uncertainties; validity time range MJD 55757.0-55985.2). This implies a surface dipolar magnetic field strength of B ~ 2.8 x 10^13 G (assuming a neutron star radius of 10km and a mass of 1.4 solar masses).

The above solution is not consistent, within 3sigma, with those already reported in literature and based on reduced datasets (Kuiper et al. 2011; Livingstone et al. 2011; valid up to 70 and 90 days from the BAT trigger, respectively).