An optical counterpart to the anomalous X-ray pulsar 4U0142+61

F. Hulleman, M. H. van Kerkwijk () and S. R. Kulkarni
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F. Hulleman: Astronomical Institute, Utrecht University
M. H. van Kerkwijk: Astronomical Institute, Utrecht University
S. R. Kulkarni: Palomar Observatory 105-24, California Institute of Technology

Nature, 2000, vol. 408, issue 6813, 689-692

Abstract: Abstract The energy source of the anomalous X-ray pulsars1 (AXPs) is not understood, hence their designation as anomalous. Unlike binary X-ray pulsars, no companions are seen, so the energy cannot be supplied by accretion of matter from a companion star. The loss of rotational energy, which powers radio pulsars, is insufficient to power AXPs. Two models are generally considered: accretion from a large disk left over from the birth process2,3, or decay of a very strong magnetic field (1015 G) associated with a ‘magnetar’4. The lack of counterparts at other wavelengths has hampered progress in our understanding of these objects. Here we report deep optical observations of the field around 4U0142+61, which is the brightest AXP in X-rays. The source has no associated supernova remnant, which, together with its spin-down timescale of ∼105 yr (ref. 5), suggests that it may be relatively old. We find an object with peculiar optical colours at the position of the X-ray source, and argue that it is the optical counterpart. The optical emission is too faint to admit the presence of a large accretion disk, but may be consistent with magnetospheric emission from a magnetar.

Date: 2000
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DOI: 10.1038/35047024

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