English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Plus monthly

Global: Zendy Tools annual

Global: Zendy Tools monthly

Global: Zendy Free Plan

We analyzed a deep {\it XMM-Newton} observation of the radio-quiet$\gamma$-ray PSR J2055+2539. The spectrum of the X-ray counterpart isnon-thermal, with a photon index of $\Gamma$=2.36$\pm$0.14 (1$\sigma$confidence). We detected X-ray pulsations with a pulsed fraction of(25$\pm$3)\% and a sinusoidal shape. Taking into account considerations on the$\gamma$-ray efficiency of the pulsar and on its X-ray spectrum, we can infer apulsar distance ranging from 450 pc to 750 pc. We found two different nebularfeatures associated to PSR J2055+2539 and protruding from it. The angle betweenthe two nebular main axes is $\sim$ (162.8$\pm$0.7)$^{\circ}$. The main,brighter feature is 12' long and $<$20" thick, characterized by an asymmetrywith respect to the main axis that evolves with the distance from the pulsar,possibly forming a helical pattern. The secondary feature is 250" $\times$ 30".Both nebulae present an almost flat brightness profile with a sudden decreaseat the end. The nebulae can be fitted either by a power-law model or a thermalbremsstrahlung model. A plausible interpretation of the brighter nebula is interms of a collimated ballistic jet. The secondary nebula is most likely aclassical synchrotron-emitting tail.

The tale of the two tails of the oldish PSR J2055+2539