VHE γ‐Ray Observation of the Crab Nebula and its Pulsar with the MAGIC Telescope

Albert, J.; Aliu, E.; Anderhub, H.; Antoranz, P.; Armada, A.; Baixeras, C.; Barrio, J. A.; Bartko, H.; Bastieri, D.; Becker, J.; Bednarek, W.; Berger, K.; Bigongiari, C.; Biland, A.; Böck, R.; Bordas, P.; Bosch‐Ramon, V.; Bretz, T.; Britvitch, I.; Cámara, Miguel; Carmona, E.; Chilingarian, A.; Coarasa, J. A.; Commichau, S.; Contreras, J. L.; Cortina, J.; Costado, M. T.; Curtef, V.; Danielyan, V.; Dazzi, F.; Angelis, A. De; Mendez, C. Delgado; Reyes, R. de los; Lotto, B. De; Domingo-Santamaría, E.; Dorner, D.; Doro, M.; Errando, M.; Fagiolini, M.; Ferenc, D.; Fernández, E.; Firpo, R.; Flix, J.; Fonseca, M. V.; Font, L.; Fuchs, M.; Galante, N.; García-López, R. J.; Garczarczyk, M.; Gaug, M.; Giller, M.; Göebel, F.; Hakobyan, D.; Hayashida, M.; Hengstebeck, T.; Herrero, A.; Höhne, D.; Hose, J.; Hsu, C. C.; Jacoń, P.; Jogler, T.; Kosyra, R.; Kranich, D.; Kritzer, R.; Laille, A.; Lindfors, E.; Lombardi, S.; Longo, F.; López, J.; López, M.; Lorenz, E.; Majumdar, P.; Maneva, G.; Mannheim, K.; Mansutti, O.; Mariotti, M.; Martı́nez, M.; Mazin, D.; Merck, C.; Meucci, M.; Meyer, M.; Miranda, J. M.; Mirzoyan, R.; Mizobuchi, S.; Moralejo, A.; Nieto, D.; Nilsson, K.; Ninković, J.; Oña-Wilhelmi, E.; Otte, A. N.; Oya, I.; Paneque, D.; Panniello, M.; Paoletti, R.; Paredes, J. M.; Pasanen, M.; Pascoli, D.; Pauß, F.; Pegna, R.; Peršić, M.; Peruzzo, L.; Piccioli, A.; Pöller, M.; Prandini, E.; Puchades, N.; Raymers, A.; Rhode, W.; Ribó, M.; Rico, J.; Rissi, M.; Robert, A.; Rügamer, S.; Saggion, A.; Sánchez, A.; Sartori, P.; Scalzotto, V.; Scapin, V.; Schmitt, R.; Schweizer, T.; Shayduk, M.; Shinozaki, K.; Shore, Steven N.; Sidro, N.; Sillanpää, A.; Sobczyńska, D.; Stamerra, A.; Stark, L. S.; Takalo, L. O.; Temnikov, P.; Tescaro, D.; Teshima, M.; Tonello, N.; Torres, D. F.; Turini, N.; Vankov, H.; Vitale, V.; Wagner, R. M.; Wibig, T.; Wittek, W.; Zandanel, F.; Zanin, R.; Zapatero, J.

doi:10.1086/525270

Cited by 276 publications

(259 citation statements)

References 63 publications

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“…The curvature seems to be smaller than reported in Albert et al (2008b), however the effective spectral slope is still within the systematic and statistical error. Note moreover, that the fitting range is slightly different than in Albert et al (2008b).…”

Section: Spectrum Of the Crab Nebulacontrasting

confidence: 56%

“…The second MAGIC telescope is a close copy of MAGIC I (Albert et al, 2008b) with a few important differences. Both telescopes have a 17 m diameter mirror dish and f /D close to 1, but contrary to MAGIC I, the outer mirrors of MAGIC II are made of glass rather than aluminium (Doro et al, 2008).…”

Section: The Magic Telescopesmentioning

confidence: 99%

“…In the first steps of the analysis (calibration, image cleaning, and parametrization of images, see Albert et al (2008b); Aliu et al (2009)) of the MAGIC stereo data each telescope is treated separately. The procedure is similar for both telescopes with some small differences.…”

Section: Image Processingmentioning

confidence: 99%

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Performance of the MAGIC stereo system obtained with Crab Nebula data

Aleksić

Álvarez

Antonelli

et al. 2012

Astroparticle Physics

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MAGIC is a system of two Imaging Atmospheric Cherenkov Telescopes located in the Canary island of La Palma. Since autumn 2009 both telescopes have been working together in stereoscopic mode, providing a significant improvement with respect to the previous single-telescope observations. We use observations of the Crab Nebula taken at low zenith angles to assess the performance of the MAGIC stereo system. The trigger threshold of the MAGIC telescopes is 50 − 60 GeV. Advanced stereo analysis techniques allow MAGIC to achieve a sensitivity as good as (0.76 ± 0.03) % of the Crab Nebula flux in 50 h of observations above 290 GeV. The angular resolution at those energies is better than ∼ 0.07 • . We also perform a detailed study of possible systematic effects which may influence the analysis of the data taken with the MAGIC telescopes.

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Section: Spectrum Of the Crab Nebulacontrasting

confidence: 56%

Section: The Magic Telescopesmentioning

confidence: 99%

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Performance of the MAGIC stereo system obtained with Crab Nebula data

Aleksić

Álvarez

Antonelli

et al. 2012

Astroparticle Physics

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206

117

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“…Upper limits (ULs) on the flux were computed following the Rolke et al (2005) method for 95% confidence level (CL), assuming a Gaussian background and a systematic uncertainty of 30% on the effective area of the instrument (Albert et al 2008). The spectrum that we assumed was a power-law function, dF/dE ∝ E −Γ , with a spectral index of 2.6.…”

Section: Observations and Resultsmentioning

confidence: 99%

Very-high-energy gamma-ray observations of the Type Ia supernova SN 2014J with the MAGIC telescopes

Fernández-Barral¹,

Fruck²,

Blanch³

et al. 2017

AIP Conference Proceedings

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Context. In this work we present data from observations with the MAGIC telescopes of SN 2014J detected in January 21 2014, the closest Type Ia supernova since Imaging Air Cherenkov Telescopes started to operate. Aims. We probe the possibility of very-high-energy (VHE; E ≥ 100 GeV) gamma rays produced in the early stages of Type Ia supernova explosions. Methods. We performed follow-up observations after this supernova explosion for 5 days, between January 27 and February 2 in 2014. We search for gamma-ray signal in the energy range between 100 GeV and several TeV from the location of SN 2014J using data from a total of ∼ 5.5 hours of observations. Prospects for observing gamma-rays of hadronic origin from SN 2014J in the near future are also being addressed. Results. No significant excess was detected from the direction of SN 2014J. Upper limits at 95% confidence level on the integral flux, assuming a power-law spectrum, dF/dE ∝ E −Γ , with a spectral index of Γ = 2.6, for energies higher than 300 GeV and 700 GeV, are established at 1.3 × 10 −12 and 4.1 × 10 −13 photons cm −2 s −1 , respectively. Conclusions. For the first time, upper limits on the VHE emission of a Type Ia supernova are established. The energy fraction isotropically emitted into TeV gamma rays during the first ∼ 10 days after the supernova explosion for energies greater than 300 GeV is limited to 10 −6 of the total available energy budget (∼ 10 51 erg). Within the assumed theoretical scenario, the MAGIC upper limits on the VHE emission suggest that SN 2014J will not be detectable in the future by any current or planned generation of Imaging Atmospheric Cherenkov Telescopes.

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“…before the second MAGIC telescope was operational (mono data), and in 2010 when both telescopes were already taking stereoscopic data. Details about the performance of MAGIC in mono and stereo mode can be found in Albert et al (2008) and Aleksić et al (2012). All data presented in this work were taken in the so-called wobble mode and were analyzed using the MARS analysis framework (Moralejo et al 2009;Aleksić et al 2012).…”

Section: The Magic Telescopes Analysis and Datamentioning

confidence: 99%

Observations of the magnetars 4U 0142+61 and 1E 2259+586 with the MAGIC telescopes

Aleksić

Antonelli

Antoranz

et al. 2012

A&A

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Context. Magnetars are an extreme, highly magnetized class of isolated neutron stars whose large X-ray luminosity is believed to be driven by their high magnetic field. Aims. We study for the first time the possible very high energy γ-ray emission above 100 GeV from magnetars, observing the sources 4U 0142+61 and 1E 2259+586. Methods. We observed the two sources with atmospheric Cherenkov telescopes in the very high energy range (E > 100 GeV). 4U 0142+61 was observed with the MAGIC I telescope in 2008 for about 25 h and 1E 2259+586 was observed with the MAGIC stereoscopic system in 2010 for about 14 h. The data were analyzed with the standard MAGIC analysis software. Results. Neither magnetar was detected. Upper limits to the differential and integral flux above 200 GeV were computed using the Rolke algorithm. We obtain integral upper limits to the flux of 1.52 × 10 −12 cm −2 s −1 and 2.7 × 10 −12 cm −2 s −1 with a confidence level of 95% for 4U 0142+61 and 1E 2259+586, respectively. The resulting differential upper limits are presented together with X-ray data and upper limits in the GeV energy range.

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VHE γ‐Ray Observation of the Crab Nebula and its Pulsar with the MAGIC Telescope

Cited by 276 publications

References 63 publications

Performance of the MAGIC stereo system obtained with Crab Nebula data

Performance of the MAGIC stereo system obtained with Crab Nebula data

Very-high-energy gamma-ray observations of the Type Ia supernova SN 2014J with the MAGIC telescopes

Observations of the magnetars 4U 0142+61 and 1E 2259+586 with the MAGIC telescopes

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