Volume 575, March 2015
|Number of page(s)||88|
|Section||Interstellar and circumstellar matter|
|Published online||10 February 2015|
Light-curve modelling constraints on the obliquities and aspect angles of the young Fermi pulsars⋆
1 Nicolaus Copernicus Astronomical Center, Rabiańska 8, 87-100 Toruń, Poland
2 INAF–Istituto di Astrofisica Spaziale e Fisica Cosmica, 20133 Milano, Italy
3 François Arago Centre, APC, Université Paris Diderot, CNRS/IN2P3, CEA/Irfu, Observatoire de Paris, Sorbonne Paris Cité, 10 rue A. Domon et L. Duquet, 75205 Paris Cedex 13, France
4 Astrophysics Science Division, NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA
5 Laboratoire AIM, Université Paris Diderot/CEA-IRFU/CNRS, Service d’Astrophysique, CEA Saclay, 91191 Gif sur Yvette, France
6 Institut Universitaire de France
7 National Research Council Research Associate, National Academy of Sciences, Washington, DC 20001, USA
8 Istituto Nazionale di Fisica Nucleare, Sezione di Pavia, via Bassi 6, 27100 Pavia, Italy
9 W. W. Hansen Experimental Physics Laboratory, Kavli Institute for Particle Astrophysics and Cosmology, Department of Physics and SLAC National Accelerator Laboratory, Stanford University, Stanford, CA 94305, USA
10 Hope College, Department of Physics, Holland MI, USA
Received: 15 March 2014
Accepted: 12 November 2014
In more than four years of observation the Large Area Telescope on board the Fermi satellite has identified pulsed γ-ray emission from more than 80 young or middle-aged pulsars, in most cases providing light curves with high statistics. Fitting the observed profiles with geometrical models can provide estimates of the magnetic obliquity α and of the line of sight angle ζ, yielding estimates of the radiation beaming factor and radiated luminosity. Using different γ-ray emission geometries (Polar Cap, Slot Gap, Outer Gap, One Pole Caustic) and core plus cone geometries for the radio emission, we fit γ-ray light curves for 76 young or middle-aged pulsars and we jointly fit their γ-ray plus radio light curves when possible. We find that a joint radio plus γ-ray fit strategy is important to obtain (α,ζ) estimates that can explain simultaneously detectable radio and γ-ray emission: when the radio emission is available, the inclusion of the radio light curve in the fit leads to important changes in the (α,ζ) solutions. The most pronounced changes are observed for Outer Gap and One Pole Caustic models for which the γ-ray only fit leads to underestimated α or ζ when the solution is found to the left or to the right of the main α-ζ plane diagonal respectively. The intermediate-to-high altitude magnetosphere models, Slot Gap, Outer Gap, and One pole Caustic, are favoured in explaining the observations. We find no apparent evolution of α on a time scale of 106 years. For all emission geometries our derived γ-ray beaming factors are generally less than one and do not significantly evolve with the spin-down power. A more pronounced beaming factor vs. spin-down power correlation is observed for Slot Gap model and radio-quiet pulsars and for the Outer Gap model and radio-loud pulsars. The beaming factor distributions exhibit a large dispersion that is less pronounced for the Slot Gap case and that decreases from radio-quiet to radio-loud solutions. For all models, the correlation between γ-ray luminosity and spin-down power is consistent with a square root dependence. The γ-ray luminosities obtained by using the beaming factors estimated in the framework of each model do not exceed the spin-down power. This suggests that assuming a beaming factor of one for all objects, as done in other studies, likely overestimates the real values. The data show a relation between the pulsar spectral characteristics and the width of the accelerator gap. The relation obtained in the case of the Slot Gap model is consistent with the theoretical prediction.
Key words: stars: neutron / pulsars: general / gamma rays: stars / radiation mechanisms: non-thermal / methods: statistical
Appendices are available in electronic form at http://www.aanda.org
© ESO, 2015
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