We report X-ray timing and spectral properties of the pulsar PSR J0205+6449 measured using NuSTAR and Chandra observatories. We measure the pulsar's rotation frequency v = 15:20102357(9) s-1 and its derivative v = -4.5(1) X 10-11 s-2 during the observation period, and model the 2~30 keV on-pulse spectrum of the pulsar with a power law having a photon index Γpsr = 1.07 ± 0.16 and a 2~30 keV flux F2-30 keV = 7.3±0.6 X 10-13 erg cm-2 s-1. The Chandra 0.5-10 keV data are analyzed for an investigation of the pulsar's thermal emission properties. We use thermal and non-thermal emission models to t the Chandra spectra and infer the surface temperature T1 and luminosity Lth of the neutron star to be T∞ = 0.5 - 0.8 MK and Lth = 1 - 5 X 1032 erg s-1. This agrees with previous results which indicated that PSR J0205+6449 has a low surface temperature and luminosity for its age of 800{5600 yrs.

We present IR ux density measurements, models of the broadband SED, and results of SED modeling for the Pulsar Wind Nebula (PWN) 3C 58. We nd that the Herschel ux density seems to be slightly lower than suggested by interpolation of previous measurements in nearby wavebands, implying that there may be multiple electron populations in 3C 58. We model the SED using a simple stationary one-zone and a more realistic time-evolving multi-zone scenario. The latter includes variations of ow properties in the PWN (injected energy, magnetic eld, and bulk speed), radiative energy losses, adiabatic expansion, and diusion, similar to previous PWN models. From the modeling, we nd that a PWN age of 2900{5400 yrs is preferred and that there may be excess emission at  1011 Hz. The latter may imply multiple populations of electrons in the PWN.

To celebrate the tenth anniversary since the launch of Fermi Gamma-ray Space Telescope, we take a retrospect to a series of breakthroughs Fermi has contributed to pulsar astronomy in the last decade. Apart from significantly enlarging the population of ɤ−ray pulsars, observations with the Large Area Telescope onboard Fermi also show the population is not homogeneous. Instead, many classes and sub-classes have been revealed. In this paper, we will review the properties of different types of ɤ−ray pulsars, including radio-quiet ɤ−ray pulsars, millisecond pulsars, ɤ−ray binaries. Also, we will discuss the prospects of pulsar astronomy in the high energy regime.

The main goals of the Parkes Pulsar Timing Array (PPTA) project are to 1) detect ultra-low-frequency gravitational waves, 2) improve the solar system planetary ephemeris and 3) provide a long-term, stable time standard. In this paper, we highlight the main results from the project so far and discuss our expectations for the future.

The results of the Crab pulsar observations with the photometrical MANIA (Multichannel Analysis of Nanosecond Intensity Alterations) complex at the 6-m telescope are presented. More than 12 millions photons in UBVR-bands simultaneously with time resolution of 10-7s were detected. Using the original software for search for optical pulsar period, we obtained the light curves of the object with time resolution of about 3.3 μs. Their detailed analysis gives the spectral change during pulse and subpulse, the shape of the pulse peaks, which are plateaus (with the duration of about 50 μs for the main pulse), limits for an amplitude of fine temporal (stochastic and regular) structure of pulse and sub pulse and the interpulse space intensity. The results of CCD-spectroscopy of the Crab pulsar show that its summarized spectrum is flat. There are no lines, neither emission nor absorbtion ones. Upper limit for line intensity or depth is 3.5% with the confidence probability of 95%.