A&A 479, 793-803 (2008)
Possible optical detection of a fast, nearby radio pulsar PSR B1133+16S. V. Zharikov1, Yu. A. Shibanov2, R. E. Mennickent3, and V. N. Komarova4, 5
1 Observatorio Astronómico Nacional SPM, Instituto de Astronomía, Universidad Nacional Autónomia de México, Ensenada, BC, México
2 Ioffe Physical Technical Institute, Politekhnicheskaya 26, St. Petersburg 194021, Russia
3 Departamento de Fisica, Universidad de Concepcion, Casilla 160-C, Concepcion, Chile
4 Special Astrophysical Observatory, Russian Academy of Science, Nizhnii Arkhyz, Russia, 369167
5 Isaac Newton Institute of Chile, SAO Branch, Russia
(Received 26 April 2007 / Accepted 1 November 2007)
Aims.We performed deep optical observations of the field of an old, fast-moving radio pulsar PSR B1133+16 in an attempt to detect its optical counterpart and a bow shock nebula.
Methods.The observations were carried out using the direct imaging mode of FORS1 at the ESO VLT/UT1 telescope in the B, R, and H bands. We also used archival images of the same field obtained with the VLT in the B band and with the Chandra/ACIS in X-rays.
Results. In the B band we detected a faint (B = 28 1 0 3) source that may be the optical counterpart of PSR B1133+16, as it is positionally consistent with the radio pulsar and with the X-ray counterpart candidate published earlier. Its upper limit in the R band implies a color index B-R 0 5, which is compatible with the index values for most pulsars identified in the optical range. The derived optical luminosity and its ratio to the X-ray luminosity of the candidate are consistent with expected values derived from a sample of pulsars detected in both spectral domains. No Balmer bow shock was detected, implying a low density of ambient matter around the pulsar. However, in the X-ray and H images we found the signature of a trail extending ~ behind the pulsar and coinciding with the direction of its proper motion. If confirmed by deeper studies, this is the first time such a trail has been seen in the optical and X-ray wavelengths.
Conclusions.Further observations at later epochs are necessary to confirm the identification of the pulsar by the candidate's proper motion measurements.
Key words: pulsars: general -- pulsars: individual: PSR B1133+16 -- stars: neutron
© ESO 2008