Teraelectronvolt pulsed emission from the Crab Pulsar detected by MAGIC

Ansoldi, S.; Antonelli, L. A.; Antoranz, P.; Babić, Ana; Bangale, P.; Almeida, U. Barres de; Barrio, J. A.; González, J. Becerra; Bednarek, W.; Bernardini, E.; Biasuzzi, B.; Biland, A.; Blanch, O.; Bonnefoy, S.; Bonnoli, G.; Borracci, F.; Bretz, T.; Carmona, E.; Carosi, A.; Colin, P.; Colombo, E.; Contreras, J. L.; Cortina, J.; Covino, S.; Vela, P. Da; Dazzi, F.; Angelis, A. De; Caneva, G. De; Lotto, B. De; Wilhelmi, E. de Oña; Mendez, C. Delgado; Pierro, F. Di; Prester, D. Dominis; Dorner, D.; Doro, M.; Einecke, S.; Glawion, D.; Elsäesser, D.; Fernández-Barral, A.; Fidalgo, D.; Fonseca, M. V.; Font, L.; Frantzen, K.; Fruck, C.; Galindo, D.; López, R. J. García; Garczarczyk, M.; Terrats, D. Garrido; Gaug, M.; Godinović, N.; Muñoz, A. González; Gozzini, S. R.; Hanabata, Y.; Hayashida, M.; Herrera, Javier; Hirotani, Kouichi; Hose, J.; Hrupec, Dario; Hughes, G.; Idec, W.; Kellermann, H.; Knoetig, M. L.; Kodani, K.; Konno, Y.; Krause, J.; Kubo, H.; Kushida, J.; Barbera, A. La; Lelas, D.; Lewandowska, N.; Lindfors, E.; Lombardi, S.; Longo, Elson; López, M.; López-Coto, R.; López-Oramas, A.; Lorenz, E.; Makariev, M.; Mallot, K.; Maneva, G.; Mannheim, K.; Maraschi, L.; Marcote, B.; Mariotti, M.; Martı́nez, M.; Mazin, D.; Menzel, U.; Miranda, J. M.; Mirzoyan, R.; Moralejo, A.; Munar-Adrover, P.; Nakajima, D.; Neustroev, V.; Niedźwiecki, A.; Rosillo, M. Nevas; Nilsson, K.; Nishijima, K.; Noda, K.; Orito, R.; Overkemping, A.; Paiano, S.; Palatiello, M.; Paneque, D.; Paoletti, R.; Paredes, J. M.; Paredes-Fortuny, X.; Peršić, M.; Poutanen, Juri; Moroni, P. G. Prada; Prandini, E.; Puljak, I.; Reinthal, R.; Rhode, W.; Ribó, M.; Rico, J.; Garcia, J. Rodriguez; Saito, T.; Saito, Koji; Satalecka, K.; Scalzotto, V.; Scapin, V.; Schultz, C.; Schweizer, T.; Shore, S. N.; Sillanpää, A.; Sitarek, J.; Šnidarić, Iva; Sobczyńska, D.; Stamerra, A.; Steinbring, T.; Strzys, M.; Takalo, L. O.; Takami, H.; Tavecchio, F.; Temnikov, P.; Terzić, T.; Tescaro, D.; Teshima, M.; Thaele, J.; Torres, D. F.; Toyama, Takeshi; Treves, A.; Ward, J. E.; Will, Martin; Zanin, R.

doi:10.1051/0004-6361/201526853

Cited by 127 publications

(125 citation statements)

References 42 publications

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“…Neutron stars are well known to emit a broadband electromagnetic spectrum from the radio wavelength (Manchester et al 2005) through optical/UV up to high and very highenergy, in GeV/subTeV (Abdo et al 2013), and even TeV for the Crab pulsar (Ansoldi et al 2016). However, it is still unclear where precisely in the magnetosphere or the wind these photons are coming from and how they are produced.…”

Section: Introductionmentioning

confidence: 99%

Radiative pulsar magnetospheres: aligned rotator

Pétri

2019

Monthly Notices of the Royal Astronomical Society: Letters

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Force-free neutron star magnetospheres are nowadays well known and found through numerical simulations. Even extension to general relativity has recently been achieved. However, those solutions are by definition dissipationless, meaning that the star is unable to accelerate particles and let them radiate any photon. Interestingly, the forcefree model has no free parameter however it must be superseded by a dissipative mechanism within the plasma. In this paper, we investigate the magnetosphere electrodynamics for particles moving in the radiation reaction regime, using the limit where acceleration is fully balanced by radiation, also called Aristotelian dynamics. An Ohm's law is derived, from which the dissipation rate is controlled by a one parameter family of solutions depending on the pair multiplicity κ. The spatial extension of the dissipation zone is found self-consistently from the simulations. We show that the radiative magnetosphere of an aligned rotator tends to the force-free regime whenever the pair multiplicity becomes moderately large, κ 1. However, for low multiplicity, a substantial fraction of the spindown energy goes into particle acceleration and radiation in addition to the Poynting flux, the latter remaining only dominant for large multiplicities. We show that the work done on the plasma occurs predominantly in the equatorial current sheet right outside the light-cylinder.

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Section: Introductionmentioning

confidence: 99%

Radiative pulsar magnetospheres: aligned rotator

Pétri

2019

Monthly Notices of the Royal Astronomical Society: Letters

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“…The lower energy limit is chosen to avoid complications in accounting for the Crab pulsar. Based on the spectra measured in Ansoldi et al (2016), the contribution of the pulsar above 50 GeV is 4% with respect to the nebula; thus the pulsar can be neglected for the purpose of this validation study. An accurate determination of the nebula spectrum at lower energies can be obtained by using an event selection based on the pulsar phase.…”

Section: Preparation Of Fermi-lat Datamentioning

confidence: 99%

Analysis of the H.E.S.S. public data release with ctools

Knödlseder

Tibaldo

Tiziani

et al. 2019

A&A

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The ctools open-source software package was developed for the scientific analysis of astronomical data from Imaging Air Cherenkov Telescopes (IACTs), such as H.E.S.S., VERITAS, MAGIC, and the future Cherenkov Telescope Array (CTA). To date, the software has been mainly tested using simulated CTA data; however, upon the public release of a small set of H.E.S.S. observations of the Crab nebula, MSH 15-52, RX J1713.7-3946, and PKS 2155-304 validation using real data is now possible. We analysed the data of the H.E.S.S. public data release using ctools version 1.6 and compared our results to those published by the H.E.S.S. Collaboration for the respective sources. We developed a parametric background model that satisfactorily describes the expected background rate as a function of reconstructed energy and direction for each observation. We used that model, and tested all analysis methods that are supported by ctools, including novel unbinned and joint or stacked binned analyses of the measured event energies and reconstructed directions, and classical On-Off analysis methods that are comparable to those used by the H.E.S.S. Collaboration. For all analysis methods, we found a good agreement between the ctools results and the H.E.S.S. Collaboration publications considering that they are not always directly comparable due to differences in the datatsets and event processing software. We also performed a joint analysis of H.E.S.S. and Fermi-LAT data of the Crab nebula, illustrating the multi-wavelength capacity of ctools. The joint Crab nebula spectrum is compatible with published literature values within the systematic uncertainties. We conclude that the ctools software is mature for the analysis of data from existing IACTs, as well as from the upcoming CTA.

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“…In its very center lies the Crab pulsar as an energetic engine. The Crab pulsar has a stable spin period of ∼ 33 ms with derivative of ∼ 4.2 × 10 −13 s/s, proximal distance of ∼ 2 kpc, and bright radiation over almost the full electromagnetic spectrum from radio (∼ 10 −5 eV) to high energy γ-rays (∼ 10 12 eV) [2,3]. These features make it one of the best studied celestial objects, and thus a common calibration source for astronomical missions [4].…”

Section: Introductionmentioning

confidence: 99%

Phase-resolved gamma-ray spectroscopy of the Crab pulsar observed by POLAR

Gauvin

et al. 2019

Journal of High Energy Astrophysics

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The POLAR detector is a space based Gamma-Ray Burst (GRB) polarimeter sensitive in the 15-500 keV energy range. Apart from its main scientific goal as a Gamma-Ray Burst polarimeter it is also able to detect photons from pulsars in orbit. By using the six-months in-orbit observation data, significant pulsation from the PSR B0531+21 (Crab pulsar) was obtained. In this work, we present the precise timing analysis of the Crab pulsar, together with a phase-resolved spectroscopic study using a joint-fitting method adapted for wide field of view instruments like POLAR. By using single power law fitting over the pulsed phase, we obtained spectral indices ranging from 1.718 to 2.315, and confirmed the spectral evolution in a reverse S shape which is homogenous with results from other missions over broadband. We will also show, based on the POLAR in-orbit performance and Geant4 Monte-Carlo simulation, the inferred capabilities of POLAR-2, the proposed follow-up mission of POLAR on board the China Space Station (CSS), for pulsars studies.

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Teraelectronvolt pulsed emission from the Crab Pulsar detected by MAGIC

Cited by 127 publications

References 42 publications

Radiative pulsar magnetospheres: aligned rotator

Radiative pulsar magnetospheres: aligned rotator

Analysis of the H.E.S.S. public data release with ctools

Phase-resolved gamma-ray spectroscopy of the Crab pulsar observed by POLAR

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