Volume 544, August 2012
|Number of page(s)||9|
|Section||Stellar structure and evolution|
|Published online||07 August 2012|
The near-infrared detection of PSR B0540–69 and its nebula⋆
1 Mullard Space Science Laboratory, University College London, Holmbury St. Mary, Dorking, Surrey, RH5 6NT, UK
2 Kepler Institute of Astronomy, University of Zielona Góra, Lubuska 2, 65-265, Zielona Góra, Poland
3 INAF – Istituto di Astrofisica Spaziale e Fisica Cosmica Milano, via E. Bassini 15, 20133 Milano, Italy
4 IUSS – Istituto Universitario di Studi Superiori, viale Lungo Ticino Sforza, 56, 27100 Pavia, Italy
5 INFN – Istituto Nazionale di Fisica Nucleare, sezione di Pavia, via A. Bassi 6, 27100 Pavia, Italy
6 European Southern Observatory, Karl Schwarzschild-Str. 2, 85748 Garching, Germany
7 Nicolaus Copernicus Astronomical Center, ul. Rabiańska 8, 87100 Toruń, Poland
8 LUPM, Université Montpellier 2, CNRS/IN2P3, place E. Bataillon, 34095 Montpellier, France
9 KAA UMK, Gagarina 11, 87-100 Toruń, Poland
10 Max-Planck Institut für Extraterrestrische Physik, Giessenbachstrasse 1, 85741 Garching bei München, Germany
Received: 6 March 2012
Accepted: 28 April 2012
Context. The ~1700 year old PSR B0540−69 in the Large Magellanic Clouds (LMC) is considered the twin of the Crab pulsar because of its similar spin parameters, magnetic field, and energetics. PSR B0540−69 (V ~ 22.5) is also one of the very few pulsars for which both optical pulsations and polarised emission have been measured. Its optical spectrum is fit by a power-law, ascribed to synchrotron radiation, like for the young Crab and Vela pulsars. At variance with them, however, a double break is required to join the X-ray and optical power-law spectra, with the first one possibly occurring in the near ultraviolet (nUV).
Aims. Near-infrared (nIR) observations, never performed for PSR B0540−69, are crucial to determine whether the optical power-law spectrum extends to longer wavelengths or a new break occurs, like it happens for both the Crab and Vela pulsars in the mid-infrared (mIR), hinting at an even more complex particle energy and density distribution in the pulsar magnetosphere.
Methods. We observed PSR B0540−69 in the J, H, and KS bands with the Very Large Telescope (VLT) to detect it, for the first time, in the nIR and characterise its optical-to-nIR spectrum. To disentangle the pulsar emission from that of its pulsar wind nebula (PWN), we obtained high-spatial resolution adaptive optics images with the NAOS-CONICA instrument (NACO).
Results. We could clearly identify PSR B0540−69 in our J, H, and KS-band images and measure its flux (J = 20.14, H = 19.33, KS = 18.55, with an overall error of ± 0.1 mag in each band). The joint fit to the available optical and nIR photometry with a power-law spectrum Fν ∝ ν−α gives a spectral index α = 0.70 ± 0.04, slightly more precise than measured in the optical only. This clearly implies that there is no spectral break between the optical and the nIR. We also detected, for the first time, the PSR B0540−69 PWN in the nIR. The comparison between our NACO images and Hubble Space Telescope (HST) optical ones does not reveal any apparent difference in the PWN morphology as a function of wavelength. The PWN optical-to-nIR spectrum is also fit by a single power-law, with spectral index α = 0.56 ± 0.03, slightly flatter than the pulsar’s.
Conclusions. Using NACO at the VLT, we obtained the first detection of PSR B0540−69 and its PWN in the nIR. Due to the small angular scale of the PWN (~4″) only the spatial resolution of the James Webb Space Telescope (JWST) will make it possible to extend the study of the pulsar and PWN spectrum towards the mid-IR.
Key words: pulsars: individual: PSR B0540-69 / ISM: supernova remnants
© ESO, 2012
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