Volume 473, Number 3, October III 2007
|Page(s)||883 - 889|
|Section||Stellar structure and evolution|
|Published online||13 August 2007|
VLT observations of the central compact object in the Vela Jr. supernova remnant *
Mullard Space Science Laboratory, University College London, Holmbury St. Mary, Dorking, Surrey, RH5 6NT, UK e-mail: firstname.lastname@example.org
2 INAF, Istituto di Astrofisica Spaziale, via Bassini 15, Milan 20133, Italy e-mail: [deluca;sester;alberto;sandro;pat]@iasf-milano.inaf.it
3 INAF, Osservatorio Astronomico di Padova, Vicolo dell'Osservatorio 5, Padua 35122, Italy e-mail: email@example.com
Accepted: 3 July 2007
Context.X-ray observations have unveiled the existence of enigmatic point-like sources at the center of young (a few kyrs) supernova remnants. These sources, known as central compact objects (CCOs), are thought to be neutron stars produced by the supernova explosion, although their X-ray phenomenology makes them markedly different from all other young neutron stars discovered to date.
Aims.The aim of this work is to search for the optical/IR counterpart of the Vela Junior CCO and to understand the nature of the associated Hα nebula discovered by Pellizzoni et al. (2002).
Methods.We used deep optical (R-band) and IR (-bands) observations recently performed by our group with the ESO VLT to obtain the first deep, high resolution images of the field to resolve the nebula structure and pinpoint a point-like source possibly associated with the neutron star.
Results.Our R-band image shows that the nebula's flux and structure are very similar to those of, the Hα one, suggesting that the nebula spectrum is dominated by pure Hα line emission. However, the nebula is not detected in our IR observations, which makes it impossible to to constrain its spectrum. A faint point-like object (, , ) compatible with the neutron star's Chandra X-ray position is detected in our IR images (H and Ks) but not in the optical image (), where it is buried by the nebula background.
Conclusions.The nebula is most likely a bow-shock produced by the neutron star motion through the ISM or, alternatively, a photo-ionization nebula powered by UV radiation from a hot neutron star. A synchrotron nebula, powered by the relativistic particle wind from the neutron star, is the less likely interpretation because of its non-detection in the X-rays and the apparent lack of continuum emission. The candidate CCO counterpart could be the neutron star itself, a fallback disk left over from the supernova explosion, or a mid M-type star, or later, at a distance of 2 kpc.
Key words: stars: neutron / X-rays: individuals: CXO J085201.4-461753 / ISM: supernova remnants
© ESO, 2007
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