Detection of bridge emission above 50 GeV from the Crab pulsar with the MAGIC telescopes

Aleksić, J.; 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; Mendez, C. Delgado; Doert, M.; Prester, D. Dominis; Dorner, D.; Doro, M.; Einecke, S.; Eisenacher, D.; Elsäesser, D.; Farina, Emanuele Paolo; Ferenc, D.; Fidalgo, D.; Fonseca, M. V.; Font, L.; Frantzen, K.; Fruck, C.; López, R. J. García; Garczarczyk, M.; Terrats, D. Garrido; Gaug, M.; Godinović, N.; Muñoz, A. González; Gozzini, S. R.; Hadasch, D.; Hayashida, M.; Herrera, Javier; Herrero, A.; Hildebrand, D.; Hirotani, Kouichi; Hose, J.; Hrupec, Dario; Idec, W.; Kadenius, V.; Kellermann, H.; Kodani, K.; Konno, Y.; Krause, J.; Kubo, H.; Kushida, J.; Barbera, A. La; Lelas, D.; Lewandowska, N.; Lindfors, E.; Lombardi, S.; López, M.; López-Coto, R.; López-Oramas, A.; Lorenz, E.; Lozano, Irene Albarrán; Makariev, M.; Mallot, K.; Maneva, G.; Mankuzhiyil, N.; 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.; Niedźwiecki, A.; Nilsson, K.; Nishijima, K.; Noda, K.; Nowak, N.; Orito, R.; Overkemping, A.; Paiano, S.; Palatiello, M.; Paneque, D.; Paoletti, R.; Paredes, J. M.; Paredes-Fortuny, X.; Partini, S.; Peršić, M.; Moroni, P. G. Prada; Prandini, E.; Preziuso, S.; Puljak, I.; Reinthal, R.; Rhode, W.; Ribó, M.; Rico, J.; Garcia, J. Rodriguez; Rügamer, S.; Saggion, A.; 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.; Spanier, F.; Stamatescu, V.; Stamerra, A.; Steinbring, T.; Storz, J.; Strzys, M.; Sun, S.; Surić, T.; Takalo, L. O.; Takami, H.; Tavecchio, F.; Temnikov, P.; Terzić, T.; Tescaro, D.; Teshima, M.; Thaele, J.; Tibolla, O.; Torres, D. F.; Toyama, Takeshi; Treves, A.; Uellenbeck, M.; Vogler, P.; Wagner, R. M.; Zanin, R.

doi:10.1051/0004-6361/201423664

Cited by 36 publications

(29 citation statements)

References 29 publications

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“…This choice decreases the background contamination from the off-peak phase intervals and increases the signal-to-noise ratio, leading to higher detection significances as compared to the phase-averaged ones. Different gamma-ray observations (Abdo et al 2010b;Aliu et al 2011;Aleksić et al 2012b;Ackermann et al 2013;Aleksić et al 2014;Ansoldi et al 2016) showed that there is a trend of narrowing of the pulsars peaks with energy. Therefore, in this respect our results can be considered as rather conservative.…”

Section: Discussionmentioning

confidence: 99%

“…The Crab nebula was detected already with Whipple (Weekes et al 1989) and HEGRA (Aharonian et al 2004) and then it was investigated with all three currently operating Cherenkov telescopes (MAGIC, Aleksić et al 2012aAleksić et al , 2015VERITAS, Aliu et al 2014a; H.E.S.S., Aharonian et al 2006b). The discovery of new unexpected VHE gamma-ray emission (up to TeV energies) from the Crab pulsar (Aliu et al 2011;Aleksić et al 2012bAleksić et al , 2014Ansoldi et al 2016) put rather strong constrains on emission models. The existence of VHE photons requires an emission region located in the outer parts of the pulsars magnetosphere or even outside it.…”

Section: Iacts Investigations Of He Fermi Pulsarsmentioning

confidence: 99%

“…PSR J0835−4510 inFig. 4eis shown with its PWN.Crab pulsar (MAGIC,Aleksić et al 2012bAleksić et al , 2014Ansoldi et al 2016; VERITAS, Aliu et al 2011) and the Vela pulsar (H.E.S.S. 20 ).…”

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confidence: 94%

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Prospects for the detection of high-energy (E > 25 GeV) Fermi pulsars with the Cherenkov Telescope Array

Burtovoi

Saito

Zampieri

et al. 2017

Monthly Notices of the Royal Astronomical Society

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Around 160 gamma-ray pulsars were discovered by the Fermi Large Area Telescope (LAT) since 2008. The most energetic of them, 12 objects with emission above 25 GeV, are suitable candidates for the detection with the current and future Imaging Atmospheric Cherenkov Telescopes above few tens of GeV. We perform an analysis of the Fermi-LAT data of these high-energy pulsars in order to determine if such objects can be detected with the Cherenkov Telescope Array (CTA). Our goal is to forecast the significance of their point source detection with CTA. We analyze 5 years of the Fermi-LAT data fitting the spectra of each pulsar at energies E >10 GeV with a power-law function. Assuming no spectral cut-off, we extrapolate the resulting spectra to the very high energy range (VHE, E >0.1 TeV) and simulate CTA observations of all 12 pulsars with the ctools software package. Using different analysis tools, individual CTA sensitivity curves are independently calculated for each pulsar and cross-checked with the ctools results. Our simulations result in significant CTA detections of up to 8 pulsars in 50 h. Observations of the most energetic Fermi pulsars with CTA will shed light on the nature of the high-energy emission of pulsars, clarifying whether the VHE emission detected in the Crab pulsar spectrum is present also in other gamma-ray pulsars.

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Section: Discussionmentioning

confidence: 99%

Section: Iacts Investigations Of He Fermi Pulsarsmentioning

confidence: 99%

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Prospects for the detection of high-energy (E > 25 GeV) Fermi pulsars with the Cherenkov Telescope Array

Burtovoi

Saito

Zampieri

et al. 2017

Monthly Notices of the Royal Astronomical Society

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“…We used φ ∈ [0.3558, 0.4495] to define the ON region (optimized through simulations), φ ∈ [0.52, 0.87] [30] for the OFF region, and E ∈ [0.4, 7] TeV. This choice for the ON region excludes contributions of P1 and practically all possible contributions from bridge emission [31]. unnecessarily complicating the PDF and adding systematic uncertainties to the results.…”

Section: Maximum Likelihood Methodsmentioning

confidence: 99%

Constraining Lorentz invariance violations using the Crab pulsar TeV emission

Gaug¹,

Garrido²

2017

Proceedings of 35th International Cosmic Ray Conference — PoS(ICRC2017)

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Fast variations of gamma-ray flux from Active Galactic Nuclei and Gamma-Ray Bursts can constrain Lorentz Invariance Violation (LIV) because of the delayed (or advanced) arrival of photons with higher energies: this approach has lead to the current world-best limits on the energy scale of Quantum Gravity. Here we report on constraints on LIV studying the gamma-ray emission up to TeV energies from the Galactic Crab pulsar, recently discovered by the MAGIC collaboration. A likelihood analysis of the pulsar events reconstructed for energies above 400 GeV finds no significant variation of energy-dependent arrival time, and 95% CL limits are then obtained on the effective LIV energy scale after taking into account systematic uncertainties. Only a factor of about two less constraining than the current world-best limit on a quadratic LIV scenario, pulsars are now well established as a third and independent class of astrophysical objects suitable to constrain the characteristic energy scale of LIV.

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“…Gamma-ray (>100 MeV) observations were performed by AGILE (Pellizzoni et al 2009) and Fermi -LAT (Abdo et al 2010). Finally, recent observations with ground based Cherenkov telescopes, such as MAGIC (Aleksić et al 2012b(Aleksić et al , 2014MAGIC Collaboration et al 2015) and VER-ITAS (Aliu et al 2011), have obtained pulse profiles of the Crab pulsar in VHE gamma rays.…”

Section: Introductionmentioning

confidence: 99%

Simulated gamma-ray pulse profile of the Crab pulsar with the Cherenkov Telescope Array

Burtovoi

Zampieri

2016

Mon. Not. R. Astron. Soc.

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We present simulations of the very high energy (VHE) gamma-ray light curve of the Crab pulsar as observed by the Cherenkov Telescope Array (CTA). The CTA pulse profile of the Crab pulsar is simulated with the specific goal of determining the accuracy of the position of the interpulse. We fit the pulse shape obtained by the MAGIC telescope with a three-Gaussian template and rescale it to account for the different CTA instrumental and observational configurations. Simulations are performed for different configurations of CTA and for the ASTRI mini-array. The northern CTA configuration will provide an improvement of a factor of ∼3 in accuracy with an observing time comparable to that of MAGIC (73 hours). Unless the VHE spectrum above 1 TeV behaves differently from what we presently know, unreasonably long observing times are required for a significant detection of the pulsations of the Crab pulsar with the high-energy-range sub-arrays. We also found that an independent VHE timing analysis is feasible with Large Size Telescopes (LSTs). CTA will provide a significant improvement in determining the VHE pulse shape parameters necessary to constrain theoretical models of the gamma-ray emission of the Crab pulsar. One of such parameters is the shift in phase between peaks in the pulse profile at VHE and in other energy bands that, if detected, may point to different locations of the emission regions.

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Detection of bridge emission above 50 GeV from the Crab pulsar with the MAGIC telescopes

Cited by 36 publications

References 29 publications

Prospects for the detection of high-energy (E > 25 GeV) Fermi pulsars with the Cherenkov Telescope Array

Prospects for the detection of high-energy (E > 25 GeV) Fermi pulsars with the Cherenkov Telescope Array

Constraining Lorentz invariance violations using the Crab pulsar TeV emission

Simulated gamma-ray pulse profile of the Crab pulsar with the Cherenkov Telescope Array

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