The major upgrade of the MAGIC telescopes, Part I: The hardware improvements and the commissioning of the system

Aleksić, J.; Ansoldi, S.; Antonelli, L. A.; Antoranz, P.; Babić, Ana; Bangale, P.; Barceló, M.; Barrio, J. A.; González, J. Becerra; Bednarek, W.; Bernardini, E.; Biasuzzi, B.; Biland, A.; Bitossi, M.; Blanch, O.; Bonnefoy, S.; Bonnoli, G.; Borracci, F.; Bretz, T.; Carmona, E.; Carosi, A.; Cecchi, Roberto; Colin, P.; Colombo, E.; Contreras, J. L.; Corti, Daniele; Cortina, J.; Covino, S.; Vela, P. Da; Dazzi, F.; Deangelis, A.; Caneva, G. De; Lotto, B. De; Wilhelmi, E. de Oña; Mendez, C. Delgado; Dettlaff, A.; Prester, D. Dominis; Dorner, D.; Doro, M.; Einecke, S.; Eisenacher, D.; Elsäesser, D.; Fidalgo, D.; Fink, David J.; Fonseca, M. V.; Font, L.; Frantzen, K.; Fruck, C.; Galindo, D.; López, R. J. García; Garczarczyk, M.; Terrats, D. Garrido; Gaug, M.; Giavitto, G.; Godinović, N.; Muñoz, A. González; Gozzini, S. R.; Haberer, W.; Hadasch, D.; Hanabata, Y.; Hayashida, M.; Herrera, Javier; Hildebrand, D.; Hose, J.; Hrupec, Dario; Idec, W.; Illa, J. M.; Kadenius, V.; Kellermann, H.; Knoetig, M. L.; Kodani, K.; Konno, Y.; Krause, J.; Kubo, H.; Kushida, J.; Barbera, A. La; Lelas, D.; Lemus, Jesús; Lewandowska, N.; Lindfors, E.; Lombardi, S.; Longo, F.; López, M.; López-Coto, R.; López-Oramas, A.; Lorca, 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.; Negrello, M.; Neustroev, V.; Niedźwiecki, A.; 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; Rügamer, S.; Saito, T.; Saito, Koji; Satalecka, K.; Scalzotto, V.; Scapin, V.; Schultz, C.; Schlammer, J.; Schmidl, S.; Schweizer, T.; Sillanpää, A.; Sitarek, J.; Šnidarić, Iva; Sobczyńska, D.; Spanier, F.; Stamerra, A.; Steinbring, T.; Storz, J.; Strzys, M.; Takalo, L. O.; Takami, H.; Tavecchio, F.; Tejedor, Luis; Temnikov, P.; Terzić, T.; Tescaro, D.; Teshima, M.; Thaele, J.; Tibolla, O.; Torres, D. F.; Toyama, Takeshi; Treves, A.; Vogler, P.; Wetteskind, H.; Will, Martin; Zanin, R.

doi:10.1016/j.astropartphys.2015.04.004

Cited by 217 publications

(128 citation statements)

References 20 publications

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“…MAGIC (Major Atmospheric Gamma Imaging Cherenkov) is a system of two Imaging Atmospheric Cherenkov Telescopes (IACTs) designed to observe VHE gamma rays from 50 GeV up to tens of TeV (Aleksić et al, 2016a). It is located in the Canary island of La Palma, at ∼2,200 m above the sea level.…”

Section: The Magic Telescopesmentioning

confidence: 99%

Probing the Diffuse Optical-IR Background with TeV Blazars Detected with the MAGIC Telescopes

Prandini

Domínguez

Ramazani

et al. 2017

Front. Astron. Space Sci.

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Blazars are radio loud quasars whose jet points toward the observer. The observed emission is mostly non-thermal, dominated by the jet emission, and in some cases extends up to the very high energy gamma rays (VHE; E > 100 GeV). To date, more than 60 blazars have been detected at VHE mainly with ground-based imaging atmospheric Cherenkov telescopes (IACTs) such as MAGIC, H.E.S.S., and VERITAS. Energetic photons from a blazar may interact with the diffuse optical and IR background (the extragalactic background light, EBL) leaving an imprint on the blazar energy spectrum. This effect can be used to constrain the EBL, with basic assumptions on the intrinsic energy spectrum. Current generation of IACTs is providing valuable measurements of the EBL density and energy spectrum from optical to infrared frequencies. In this contribution, we present the latest results obtained with the data taken with the MAGIC telescopes: using 32 spectra from 12 blazars, the scale factor of the optical density predicted by the EBL model from Domínguez et al. (2011) is constrained to be 0.95 (+0.11, −0.12) stat (+0.16, −0.07) sys , where a value of 1 means the perfect match with the model.

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Section: The Magic Telescopesmentioning

confidence: 99%

Probing the Diffuse Optical-IR Background with TeV Blazars Detected with the MAGIC Telescopes

Prandini

Domínguez

Ramazani

et al. 2017

Front. Astron. Space Sci.

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“…[17]. The large mirror dish of the MAGIC telescopes allows us to observe gamma rays with energies as low as ∼50 GeV [18].…”

Section: Observations and Data Analysismentioning

confidence: 99%

Broad Band Observations of Gravitationally Lensed Blazar during a Gamma-Ray Outburst

et al. 2016

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QSO B0218+357 is a gravitationally lensed blazar located at a cosmological redshift of 0.944. In July 2014 a GeV flare was observed by Fermi-LAT, triggering follow-up observations with the MAGIC telescopes at energies above 100 GeV. The MAGIC observations at the expected time of arrival of the trailing component resulted in the first detection of QSO B0218+357 in Very-High-Energy (VHE, >100 GeV) gamma rays. We report here the observed multiwavelength emission during the 2014 flare.

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“…Observations of the Geminga pulsar and nebula were performed between December 2012 and March 2013, with the upgraded MAGIC telescopes (Aleksić et al 2016a). During this period, a total of ∼ 75 hours were taken at zenith angles below 35…”

Section: Magic Observations and Data Analysismentioning

confidence: 99%

Search for VHE gamma-ray emission from the Geminga pulsar and nebula with the MAGIC telescopes

Bonnefoy¹,

Moya²,

López-Coto³

et al. 2016

Proceedings of the 34th International Cosmic Ray Conference — PoS(ICRC2015)

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The Geminga pulsar, one of the brighest gamma-ray sources, is a promising candidate for emission of very-high-energy (VHE > 100 GeV) pulsed gamma rays. Also, detection of a large nebula have been claimed by water Cherenkov instruments. We performed deep observations of Geminga with the MAGIC telescopes, yielding 63 hours of good-quality data, and searched for emission from the pulsar and pulsar wind nebula. We did not find any significant detection, and derived 95% confidence level upper limits. The resulting upper limits of 5.3 × 10 −13 TeV cm −2 s −1 for the Geminga pulsar and 3.5 × 10 −12 TeV cm −2 s −1 for the surrounding nebula at 50 GeV are the most constraining ones obtained so far at VHE. To complement the VHE observations, we also analyzed 5 years of Fermi-LAT data from Geminga, finding that the sub-exponential cut-off is preferred over the exponential cut-off that has been typically used in the literature. We also find that, above 10 GeV, the gamma-ray spectra from Geminga can be described with a power law with index softer than 5. The extrapolation of the power-law Fermi-LAT pulsed spectra to VHE goes well below the MAGIC upper limits, indicating that the detection of pulsed emission from Geminga with the current generation of Cherenkov telescopes is very difficult.

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The major upgrade of the MAGIC telescopes, Part I: The hardware improvements and the commissioning of the system

Cited by 217 publications

References 20 publications

Probing the Diffuse Optical-IR Background with TeV Blazars Detected with the MAGIC Telescopes

Probing the Diffuse Optical-IR Background with TeV Blazars Detected with the MAGIC Telescopes

Broad Band Observations of Gravitationally Lensed Blazar during a Gamma-Ray Outburst

Search for VHE gamma-ray emission from the Geminga pulsar and nebula with the MAGIC telescopes

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