Detection of Gamma Rays of up to 50 T[CLC]e[/CLC]V from the Crab Nebula

Tanimori, T.; Sakurazawa, K.; Dazeley, S.; Edwards, Philip; Hara, T.; Hayami, Y.; Kamei, S.; Kifune, T.; Konishi, T.; Matsubara, Y.; Matsuoka, Taro; Mizumoto, Y.; Masaike, A.; Mori, M.; Muraishi, H.; Muraki, Y.; Naito, T.; Oda, S.; Ogio, S.; Osaki, T.; Patterson, J. R.; Roberts, M.; Rowell, G.; Suzuki, A.; Suzuki, Ryo; Sako, T. K.; Tamura, T.; Thornton, G.; Susukita, R.; Yanagita, S.; Yoshida, Tsuyoshi; Yoshikoshi, T.

doi:10.1086/311077

Cited by 113 publications

(82 citation statements)

References 16 publications

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“…It was the first high-confidence TeV detection in 1989 using the Whipple telescope (Weekes et al 1989) and is the brightest steady source in the Northern sky above 1 TeV. It has been observed with imaging atmospheric Cherenkov telescopes (IACTs) since (Tanimori et al 1998;Aharonian et al 2004Aharonian et al , 2006Celik 2008;Aleksić et al 2015). The first observation using a ground array was the 2003 Milagro detection (Atkins et al 2003), and the signal was subsequently seen in other ground arrays (Amenomori et al 2009;Bartoli et al 2015).…”

Section: Introductionmentioning

confidence: 99%

Observation of the Crab Nebula with the HAWC Gamma-Ray Observatory

Abeysekara

Albert

Alfaro

et al. 2017

ApJ

291

387

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The Crab Nebula is the brightest TeV gamma-ray source in the sky and has been used for the past 25 years as a reference source in TeV astronomy, for calibration and verification of new TeV instruments. The High Altitude Water Cherenkov Observatory (HAWC), completed in early 2015, has been used to observe the Crab Nebula at high significance across nearly the full spectrum of energies to which HAWC is sensitive. HAWC is unique for its wide field-of-view, nearly 2 sr at any instant, and its high-energy reach, up to 100 TeV. HAWC's sensitivity improves with the gamma-ray energy. Above ∼1 TeV the sensitivity is driven by the best background rejection and angular resolution ever achieved for a wide-field ground array.We present a time-integrated analysis of the Crab using 507 live days of HAWC data from 2014 November to 2016 June. The spectrum of the Crab is fit to a function of the form φ(E) = φ 0 (E/E 0 ) −α−β·ln(E/E0) . The data is well-fit with values of α = 2.63 ± 0.03, β = 0.15 ± 0.03, and log 10 (φ 0 cm 2 s TeV) = −12.60 ± 0.02 when E 0 is fixed at 7 TeV and the fit applies between 1 and 37 TeV. Study of the systematic errors in this HAWC measurement is discussed and estimated to be ±50% in the photon flux between 1 and 37 TeV.Confirmation of the Crab flux serves to establish the HAWC instrument's sensitivity for surveys of the sky. The HAWC survey will exceed sensitivity of current-generation observatories and open a new view of 2/3 of the sky above 10 TeV.

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Section: Introductionmentioning

confidence: 99%

Observation of the Crab Nebula with the HAWC Gamma-Ray Observatory

Abeysekara

Albert

Alfaro

et al. 2017

ApJ

291

387

View full text Add to dashboard Cite

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“…Since photons have been observed with energies E γ ≥ 50 TeV from the Crab nebula [15], we deduce for this case that E max ≥ 50 TeV, or that |δ| < 2 × 10 −16 [3]. Stronger bounds on δ can be set through observations of very high energy (TeV) photons.…”

Section: High Energy Consequences Of Breaking Of Lorentz Invariancementioning

confidence: 84%

Constraints on Lorentz invariance violating quantum gravity and large extra dimensions models using high energy γ-ray observations

Stecker

2003

Astroparticle Physics

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Observations of the multi-TeV spectra of the nearby BL objects Mkn 421 and Mkn 501 exhibit the high energy cutoffs predicted to be the result of intergalactic annihilation interactions, primarily with infrared photons having a flux level as determined by various astronomical observations. After correction for this absorption effect, the derived intrinsic spectra of these multi-TeV sources can be explained within the framework of simple synchrotron self-Compton emission models. Stecker and Glashow have shown that the existence of such annihilations via electron-positron pair production interactions up to an energy of 20 TeV puts strong constraints on Lorentz invariance violation. Such constraints have important implications for Lorentz invariance violating (LIV) quantum gravity models as well as LIV models involving large extra dimensions. We also discuss the implications of observations of high energy γ-rays from the Crab Nebula on constraining quantum gravity models.

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“…(18), we can for simplicity assume that the electron has the same energy and mass as that of the muon neutrino in the OPERA experiment. The observations of UHECR refer to the existence of electrons with energies E e ≃ 1×10 12 eV [48] and γ-rays with energies E γ ≥ 50×10 12 eV [49] are observed. These observation would set upper limits to D e ≃ 1.3 × 10 −13 and D γ 2 × 10 −16 , respectively.…”

Section: Ultra High Energy Cosmic Raysmentioning

confidence: 99%

Lorentz invariance violation and generalized uncertainty principle

Tawfik

Magdy

Ali

2016

Phys. Part. Nuclei Lett.

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There are several theoretical indications that the quantum gravity approaches may have predictions for a minimal measurable length, and a maximal observable momentum and throughout a generalization for Heisenberg uncertainty principle. The generalized uncertainty principle (GUP) is based on a momentum-dependent modification in the standard dispersion relation which is conjectured to violate the principle of Lorentz invariance. From the resulting Hamiltonian, the velocity and time of flight of relativistic distant particles at Planck energy can be derived. A first comparison is made with recent observations for Hubble parameter in redshift-dependence in early-type galaxies. We find that LIV has two types of contributions to the time of flight delay ∆t comparable with that observations. Although the wrong OPERA measurement on faster-than-light muon neutrino anomaly, ∆t, and the relative change in the speed of muon neutrino ∆v in dependence on redshift z turn to be wrong, we utilize its main features to estimate ∆v. Accordingly, the results could not be interpreted as LIV. A third comparison is made with the ultra high-energy cosmic rays (UHECR). It is found that an essential ingredient of the approach combining string theory, loop quantum gravity, black hole physics and doubly spacial relativity and the one assuming a perturbative departure from exact Lorentz invariance. Fixing the sensitivity factor and its energy dependence are essential inputs for a reliable confronting of our calculations to UHECR. The sensitivity factor is related to the special time of flight delay and the time structure of the signal. Furthermore, the upper and lower bounds to the parameter, α that characterizes the generalized uncertainly principle, have to be fixed in related physical systems such as the gamma rays bursts.

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Detection of Gamma Rays of up to 50 T[CLC]e[/CLC]V from the Crab Nebula

Cited by 113 publications

References 16 publications

Observation of the Crab Nebula with the HAWC Gamma-Ray Observatory

Observation of the Crab Nebula with the HAWC Gamma-Ray Observatory

Constraints on Lorentz invariance violating quantum gravity and large extra dimensions models using high energy γ-ray observations

Lorentz invariance violation and generalized uncertainty principle

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