期刊
ASTRONOMY & ASTROPHYSICS
卷 488, 期 3, 页码 1027-1030出版社
EDP SCIENCES S A
DOI: 10.1051/0004-6361:200810212
关键词
astrometry; stars : pulsars : individual : PSR J0108-1431
资金
- Rolling Grant
- ESO/Chile Science Visitor Programme
- STFC [PP/E001173/1] Funding Source: UKRI
- Science and Technology Facilities Council [PP/E001173/1] Funding Source: researchfish
Context. The multi-wavelength study of old (> 100 Myr) radio pulsars holds the key to understanding the long-term evolution of neutron stars, including the advanced stages of neutron star cooling and the evolution of the magnetosphere. Optical/UV observations are particularly useful for such studies because they allow one to explore both thermal and non-thermal emission processes. In particular, studying the optical/UV emission constrains the temperature of the bulk of the neutron star surface, too cold to be measured in X-ray observations. Aims. Aim of this work is to identify the optical counterpart of the very old (166 Myr) radio pulsar J0108-1431. Methods. We have re-analyzed our original Very Large Telescope (VLT) observations, where a very faint object was tentatively detected close to the radio position, near the edge of a field galaxy. Results. We found that the backward extrapolation of the PSR J0108-1431 proper motion recently measured by Chandra fits the position of this object. Based on that, we propose it as a viable candidate for the optical counterpart to PSR J0108-1431. The object fluxes (U = 26.4 +/- 0.3; B approximate to 27.9; V >= 27.8) are consistent with a thermal spectrum with a brightness temperature of similar to 9 x 10(4) K (for R = 13 km at a distance of 130 pc), emitted from the bulk of the neutron star surface. Conclusions. New optical observations are required to confirm the optical identification of PSR J0108-1431 and measure its spectrum.
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