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tokens: 2000 ). The long-term X-ray pulse profile and pulsed fraction evolution, such as that presented in Section 4.1 , could be evidence for the slow, plastic deformation of the crust needed to produce slower regions of superfluid (Woods et al. 2004 ; Thompson et al. 2002 ). Alternatively, regions of the outer core could be involved as a result of the strong magnetic fields. Magnetar strength fields provide a strong pinning of vortices to flux tubes in the outer core, which leads to a rotation lag between the normal and superfluid components, which, when relaxed, would lead to a spin-down event (Kantor Gusakov 2014 ). In typical rotation-powered pulsars, the expected internal nature of these spin-up glitches is argued to be indicated by the lack of observed radiative changes. This “radiatively quiet” condition does not hold for many glitches in magnetars. Many magnetar glitches are accompanied by drastic changes in their X-ray flux and pulse profiles (e.g., Kaspi et al. 2003 ; Dib et al. 2009 ). This could indicate that external forces are at play in radiatively loud glitches, and these external forces may lead to the net spin-down events reported in several magnetars, including the new event reported here. We have compiled a list of all published confirmed and candidate net spin-down glitches in Table 3 . In this list, we present the magnitude of the change in spin frequency, . For net spin-down glitches that are due to overrecovering spin-up glitches, the of the glitch is presented. For events where there is no sign of a recovery, we show an upper limit for the time during which the spin-down had to occur. We also note that 6 of the 7 reported net spin-down glitches are accompanied by radiative changes. 8 8 This increases to 6 of 6 if we ignore the disputed event; see Table 3 . This is a much higher fraction of radiative activity than seen in spin-up events, where only 5 of 22 timing anomalies were accompanied by radiative changes (Dib Kaspi 2014 ). Table 3 Reported Net Spin-down Glitches Notes. a Accompanied by decaying spin-up glitch with Δ ν = 10.8(4) × 10 −5 Hz. b Possibly accompanied by second glitch event. c Accompanied by decaying spin-up glitch with Δ ν = 2.0(4) × 10 −7 Hz. d Accompanied by decaying spin-up glitch with Δ ν = 5.1(5) × 10 −8 Hz. e Disputed events, see the notes below. f Not seen in analysis of same data by Dib Kaspi ( 2014 ). For the net spin-down glitches in which the net spin down is measured to be due to an overrecovery, we also report the recovery fraction, Q . Recovering glitches are often classified by their recovery fraction, defined as . In younger pulsars, when recoveries are observed, Q tends to be larger than in older pulsars (Wang et al. 2000 ). For the new glitch we report here, we measure . Glitches with have only been seen twice before: once following the magnetar-like outburst of the pulsar PSR J1846−0258 that is powered by a high magnetic field rotation, which had (Livingstone et al. 2010 ), and once during