Energy dependent $\gamma$-ray morphology in the pulsar wind nebula HESS J1825-137

31 Dipartimento di Fisica, Universit`a di Udine and Istituto Nazionale di Fisica Nucleare, Sezione di Trieste, Gruppo Collegato di Udine, I-33100 Udine, Italy.. 32 Los Alamos

We have tested gtbary and gtpphase with giant radio pulses from the Crab pulsar B0531+21 and from the millisecond pulsar B1937+21, recorded at the Nançay radio telescope, X-ray

We announce the discovery of 1–100 GeV gamma-ray emission from the archetypal TeV pulsar wind nebula (PWN) HESS J1825−137 using 20 months of survey data from the Fermi-Large

Name Time span Observing Galactic Period Ecliptic DM Log Observations sites coo. The table reports the source name, the covered time span, the number of observing sites that have

To derive the X-ray properties of the pulsar, and in particular the column density along the line of sight to discuss its dis- tance, we extracted a spectrum in a 15 ′′ radius

As part of this survey, we carried out a blind search for pulsed emission from a point source in the third Fermi-LAT source catalog (3FGL, Acero et al. 2012), is highly signif-

Previous studies have concluded that, while the subpulses appear to move through the pulse window approximately linearly at low frequencies (<500 MHz), a discrete step of ∼180 ◦

Best-fit parameters for the radiative model of the X-ray and gamma-ray spectrum of the Vela X cocoon for the case of turbulent magnetic field in the three regions shown in Fig..