A&A 492, 805-814 (2008)
DOI: 10.1051/0004-6361:200810429

A likely optical counterpart of the G292.0+1.8 pulsar wind nebula

S. V. Zharikov¹, Yu. A. Shibanov², D. A. Zyuzin^{2, 3}, R. E. Mennickent⁴, and V. N. Komarova<sup>5

1</sup>  Observatorio Astronómico Nacional SPM, Instituto de Astronomía, Universidad Nacional Autónomia de Mexico, Ensenada, BC, Mexico
    e-mail: zhar@astrosen.unam.mx
²  Ioffe Physical Technical Institute, Politekhnicheskaya 26, St. Petersburg 194021, Russia
    e-mail: shib@astro.ioffe.ru
³  Academical Physical Technical University, Khlopina 8, St. Petersburg 195220, Russia
⁴  Departamento de Fisica, Universidad de Concepcion, Casilla 160-C, Concepcion, Chile
    e-mail: rmennick@astro-udec.cl
⁵  Special Astrophysical Observatory Russian Academy of Science, Nizhnii Arkhyz, Russia
    e-mail: vkom@sao.ru

Received 19 June 2008 / Accepted 10 October 2008

Abstract
Context. G292.0+1.8 is a Cas A-like supernova remnant containing the young pulsar PSR J1124-5916, which powers a compact torus-like pulsar wind nebula with a jet visible in X-rays.
Aims. We have performed deep optical observations of the pulsar field to detect the optical counterpart of the pulsar and its nebula.
Methods. The observations were carried out using the direct imaging mode of FORS2 at the ESO VLT/UT1 telescope in the V, R, and I bands. We also analyzed archival images obtained with the Chandra/ACIS-I, ACIS-S, and HRC-S in X-rays.
Results. In all three optical bands we detect a faint elliptical nebulosity whose brightness peak and center position are consistent at a sub-arcsecond level with the X-ray position of the pulsar. The field is densely packed with background stars, but after subtraction of these stars the morphology of the object and the orientation of its major axis appear to be in good agreement with the brightest inner part of the pulsar nebula torus region seen almost edge on in X-rays. Within the nebulosity we do not resolve any point-like optical object that could be identified with the pulsar and estimate its contribution to the observed nebulosity flux as 20%. Extracting the X-ray spectrum from the physical region equivalent to the optical source position and extent and combining that with the measured optical fluxes, we compile a tentative multi-wavelength spectrum of the inner part of the nebula. Within uncertainties of the interstellar extinction towards G292.0+1.8 it is reminiscent of either the Crab or PSR B540-69 and J0205+6449 pulsar wind nebula spectra.
Conclusions. The position, morphology, and spectral properties of the detected nebulosity suggest that it is the likely optical counterpart of the pulsar plus its wind nebula system in G292.0+1.8. Higher spatial resolution optical observations and the extension of the broad-band spectrum of the proposed counterpart candidate towards the IR and UV are necessary to confirm its origin.

Key words: stars: pulsars: general -- stars: pulsars: individual: G292.0+1.8 -- stars: neutron

© ESO 2008

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