PSR J0357+3205: the tail of the turtle
Martino Marelli, Andrea De Luca, David Salvetti, Nicola Sartore,, Angelica Sartori, Patrizia Caraveo, Fabio Pizzolato, Pablo M. Saz Parkinson, and Andrea Belfiore

TL;DR
This study characterizes the X-ray properties of pulsar J0357+3205 and its tail, proposing thermal bremsstrahlung from shocked interstellar medium as the emission mechanism, and introduces a new class of nebulae called 'turtle's tail'.
Contribution
It presents the first detailed analysis of Morla's tail as a thermally-emitting nebula, proposing a novel emission mechanism and class of pulsar wind nebulae.
Findings
Pulsar's X-ray emission includes non-thermal and hot spot thermal components.
The tail's emission is best explained by thermal bremsstrahlung from shocked ISM.
Estimated pulsar distance is 300-900 pc with a velocity around 1900 km/s.
Abstract
Using a new XMM-Newton observation, we have characterized the X-ray properties of the middle-aged radio-quiet gamma-ray pulsar J0357+3205 (named Morla) and its tail. The X-ray emission from the pulsar is consistent with a magnetospheric non-thermal origin plus a thermal emission from a hot spot (or hot spots). The lack of a thermal component from the whole surface makes Morla the coldest neutron star in its age range. We found marginal evidence for a double-peaked modulation of the X-ray emission. The study of the 9'-long tail confirmed the lack of extended emission near the pulsar itself. The tail shows a very asymmetric brightness profile and its spectrum lacks any spatial variation. We found the nebular emission to be inconsistent with a classical bow-shock, ram-pressure dominated pulsar wind nebula. We propose thermal bremsstrahlung as an alternative mechanism for Morla's tail…
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