Optical Observations of PSR J0205+6449 - the next optical pulsar?

TL;DR

This study reports the detection of a candidate optical counterpart to the young pulsar PSR J0205+6449, revealing non-thermal optical emission and suggesting a spectral break between optical and X-ray energies, which is unusual among similar pulsars.

Contribution

First optical detection of PSR J0205+6449's candidate counterpart, providing insights into its non-thermal emission and spectral properties, and highlighting differences from other well-studied pulsars.

Findings

Detected optical counterpart at i ≈ 25.5 magnitude

Optical spectrum fits a power law with photon index 1.9±0.5

Indicates a double spectral break between X-ray and optical energies

Abstract

PSR J0205+6449 is a young ({\approx} 5400 years), Crab-like pulsar detected in radio and at X and {\gamma}-ray energies and has the third largest spin-down flux among known rotation powered pulsars. It also powers a bright synchrotron nebula detected in the optical and X-rays. At a distance of {\approx} 3.2 kpc and with an extinction comparable to the Crab, PSR J0205+6449 is an obvious target for optical observations. We observed PSR J0205+6449 with several optical facilities, including 8m class ground-based telescopes, such as the Gemini and the Gran Telescopio Canarias. We detected a point source, at a significance of 5.5{\sigma}, of magnitude i {\approx} 25.5, at the centre of the optical synchrotron nebula, coincident with the very accurate Chandra and radio positions of the pulsar. Thus, we discovered a candidate optical counterpart to PSR J0205+6449. The pulsar candidate counterpart is also detected in the g ({\approx}27.4) band and weakly in the r ({\approx}26.2) band. Its optical spectrum is fit by a power law with photon index {\Gamma}0 = 1.9{\pm}0.5, proving that the optical emission if of non-thermal origin, is as expected for a young pulsar. The optical photon index is similar to the X-ray one ({\Gamma}X = 1.77{\pm}0.03), although the optical fluxes are below the extrapolation of the X-ray power spectrum. This would indicate the presence of a double spectral break between the X-ray and optical energy range, at variance with what is observed for the Crab and Vela pulsars, but similar to the Large Magellanic Cloud pulsar PSR B0540-69.