Mancini Pires, A; Haberl, F; Zavlin, V; Motch, C; Zane, S; Hohle, M; (2014) The most magnificent of the seven? A candidate spin and spin down for RX J1605.3+3249. [Digital scholarly resource]. https://www.cosmos.esa.int/web/xmm-newton/2014-sym...

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Abstract

RX J1605.3+3249 is the third brightest source in the group of intriguing isolated neutron stars (INSs) known as the ``Magnificent Seven'' (M7). Crustal heating by means of magnetic field decay and an evolutionary link with magnetars may explain why these objects rotate slower and have higher thermal luminosities and magnetic field intensities than standard rotation-powered pulsars of similar age. A recent XMM-Newton observation of the source performed in AO11 finally revealed the neutron star spin period, P = 3.387864(16) s. Very interestingly, the amplitude of the modulation was found to be energy-dependent and is more significantly detected when the search is restricted to photons with E>0.5 keV. The coherent combination of the AO11 data with past observations of the source constrains the pulsar spin-down rate and dipolar magnetic field at the ˜3σ confidence level, at a value that is the highest amongst the M7, B_{dip}˜8.1×10^{14} G. Further observations are extremely important to determine a precise timing solution, as well as to perform phase-resolved spectroscopy. These will give invaluable constraints on the neutron star geometry and will allow one to confirm the high value of spin down, which would place the source closer to a magnetar than any other M7 INS

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