VHE γ-ray observation of the Crab Nebula and its pulsar with the MAGIC telescope

J. Albert; E. Aliu; H. Anderhub; P. Antoranz; A. Armada; C. Baixeras; J. A. Barrio; H. Bartko; D. Bastiere; J. K. Becker; W. Bednarek; K. Berger; C. Bigongiari; A. Biland; R. K. Bock; P. Bordas; V. Bosch-Ramon; T. Bretz; I. Britvitch; M. Camara; E. Carmona; A. Chilingarian; J. A. Coarasa; S. Commichau; J. L. Contreras; J. Cortina; M. T. Costado; V. Curtef; V. Danielyan; F. Dazzi; A. De Angelis; C. Delgado; R. De Los Reyes; B. De Lotto; E. Domingo-Santamaría; D. Dorner; M. Doro; M. Errando; M. Fagiolini; D. Ferenc; E. Fernández; R. Firpo; J. Flix; M. V. Fonseca; L. Font; M. Fuchs; N. Galante; R. García-López; M. Garczarczyk; M. Gaug; M. Giller; F. Goebel; D. Hakobyan; M. Hayashida; T. Hengstebeck; A. Herrero; D. Höhne; J. Hose; C. C. Hsu; P. Jacon; T. Jogler; R. Kosyra; D. Kranich; R. Kritzer; A. Laille; E. Lindfors; S. Lombardi; F. Longo; J. López; M. López; E. Lorenz; P. Majumdar; G. Maneva; K. Mannheim; O. Mansutti; M. Mariotti; M. Martínez; D. Mazin; C. Merck; M. Meucci; M. Meyer; J. M. Miranda; R. Mirzoyan; S. Mizobuchi; A. Moralejo; D. Nieto; K. Nilsson; J. Ninkovic; E. Oña-Wilhelmi; N. Otte; I. Oya; D. Paneque; M. Panniello; R. Paoletti; J. M. Paredes; M. Pasanen; D. Pascoli; F. Pauss; R. Pegna; M. Persic

doi:10.1086/525270

VHE γ-ray observation of the Crab Nebula and its pulsar with the MAGIC telescope

J. Albert, E. Aliu, H. Anderhub, P. Antoranz, A. Armada, C. Baixeras, J. A. Barrio, H. Bartko, D. Bastiere, J. K. Becker, W. Bednarek, K. Berger, C. Bigongiari, A. Biland, R. K. Bock, P. Bordas, V. Bosch-Ramon, T. Bretz, I. Britvitch, M. CamaraE. Carmona, A. Chilingarian, J. A. Coarasa, S. Commichau, J. L. Contreras, J. Cortina, M. T. Costado, V. Curtef, V. Danielyan, F. Dazzi, A. De Angelis, C. Delgado, R. De Los Reyes, B. De Lotto, E. Domingo-Santamaría, D. Dorner, M. Doro, M. Errando, M. Fagiolini, D. Ferenc, E. Fernández, R. Firpo, J. Flix, M. V. Fonseca, L. Font, M. Fuchs, N. Galante, R. García-López, M. Garczarczyk, M. Gaug, M. Giller, F. Goebel, D. Hakobyan, M. Hayashida, T. Hengstebeck, A. Herrero, D. Höhne, J. Hose, C. C. Hsu, P. Jacon, T. Jogler, R. Kosyra, D. Kranich, R. Kritzer, A. Laille, E. Lindfors, S. Lombardi, F. Longo, J. López, M. López, E. Lorenz, P. Majumdar, G. Maneva, K. Mannheim, O. Mansutti, M. Mariotti, M. Martínez, D. Mazin, C. Merck, M. Meucci, M. Meyer, J. M. Miranda, R. Mirzoyan, S. Mizobuchi, A. Moralejo, D. Nieto, K. Nilsson, J. Ninkovic, E. Oña-Wilhelmi, N. Otte, I. Oya, D. Paneque, M. Panniello, R. Paoletti, J. M. Paredes, M. Pasanen, D. Pascoli, F. Pauss, R. Pegna, M. Persic

Research output: Contribution to journal › Article › Research › peer-review

304 Citations (Scopus)

Abstract

We report about very high energy (VHE) γ-ray observations of the Crab Nebula with the MAGIC telescope. The γ-ray flux from the nebula was measured between 60 GeV and 9 TeV The energy spectrum can be described by a curved power law dF/dE = f0(E/300 GeV) [a-b log10(E300 GeV)] with a flux normalization f0 of (6.0 ± 0.2stat) × 10-10 cm-2s -1 TeV-1, a = -2.31 ± 0.06stat, and b = -0.26 ± 0.07stat. The peak in the spectral energy distribution is estimated at 77 ± 35 GeV Within the observation time and the experimental resolution of the telescope, the γ-ray emission is steady and pointlike. The emission's center of gravity coincides with the position of the pulsar. Pulsed γ-ray emission from the pulsar could not be detected. We constrain the cutoff energy of the pulsed spectrum to be less than 27 GeV, assuming that the differential energy spectrum has an exponential cutoff. For a superexponential shape, the cutoff energy can be as high as 60 GeV. © 2008. The American Astronomical Society. All rights reserved.

Original language	English
Pages (from-to)	1037-1055
Journal	Astrophysical Journal
Volume	674
Issue number	2
DOIs	https://doi.org/10.1086/525270
Publication status	Published - 20 Feb 2008

Keywords

Acceleration of particles
Gamma rays: observations
Radiation mechanisms: nonthermal

Access to Document

10.1086/525270

Cite this

Albert, J., Aliu, E., Anderhub, H., Antoranz, P., Armada, A., Baixeras, C., Barrio, J. A., Bartko, H., Bastiere, D., Becker, J. K., Bednarek, W., Berger, K., Bigongiari, C., Biland, A., Bock, R. K., Bordas, P., Bosch-Ramon, V., Bretz, T., Britvitch, I., ... Persic, M. (2008). VHE γ-ray observation of the Crab Nebula and its pulsar with the MAGIC telescope. Astrophysical Journal, 674(2), 1037-1055. https://doi.org/10.1086/525270

@article{33fa88d5d530471f851364d7edfc23a5,

title = "VHE γ-ray observation of the Crab Nebula and its pulsar with the MAGIC telescope",

abstract = "We report about very high energy (VHE) γ-ray observations of the Crab Nebula with the MAGIC telescope. The γ-ray flux from the nebula was measured between 60 GeV and 9 TeV The energy spectrum can be described by a curved power law dF/dE = f0(E/300 GeV) [a-b log10(E300 GeV)] with a flux normalization f0 of (6.0 ± 0.2stat) × 10-10 cm-2s -1 TeV-1, a = -2.31 ± 0.06stat, and b = -0.26 ± 0.07stat. The peak in the spectral energy distribution is estimated at 77 ± 35 GeV Within the observation time and the experimental resolution of the telescope, the γ-ray emission is steady and pointlike. The emission's center of gravity coincides with the position of the pulsar. Pulsed γ-ray emission from the pulsar could not be detected. We constrain the cutoff energy of the pulsed spectrum to be less than 27 GeV, assuming that the differential energy spectrum has an exponential cutoff. For a superexponential shape, the cutoff energy can be as high as 60 GeV. {\textcopyright} 2008. The American Astronomical Society. All rights reserved.",

keywords = "Acceleration of particles, Gamma rays: observations, Radiation mechanisms: nonthermal",

author = "J. Albert and E. Aliu and H. Anderhub and P. Antoranz and A. Armada and C. Baixeras and Barrio, {J. A.} and H. Bartko and D. Bastiere and Becker, {J. K.} and W. Bednarek and K. Berger and C. Bigongiari and A. Biland and Bock, {R. K.} and P. Bordas and V. Bosch-Ramon and T. Bretz and I. Britvitch and M. Camara and E. Carmona and A. Chilingarian and Coarasa, {J. A.} and S. Commichau and Contreras, {J. L.} and J. Cortina and Costado, {M. T.} and V. Curtef and V. Danielyan and F. Dazzi and {De Angelis}, A. and C. Delgado and {De Los Reyes}, R. and {De Lotto}, B. and E. Domingo-Santamar{\'i}a and D. Dorner and M. Doro and M. Errando and M. Fagiolini and D. Ferenc and E. Fern{\'a}ndez and R. Firpo and J. Flix and Fonseca, {M. V.} and L. Font and M. Fuchs and N. Galante and R. Garc{\'i}a-L{\'o}pez and M. Garczarczyk and M. Gaug and M. Giller and F. Goebel and D. Hakobyan and M. Hayashida and T. Hengstebeck and A. Herrero and D. H{\"o}hne and J. Hose and Hsu, {C. C.} and P. Jacon and T. Jogler and R. Kosyra and D. Kranich and R. Kritzer and A. Laille and E. Lindfors and S. Lombardi and F. Longo and J. L{\'o}pez and M. L{\'o}pez and E. Lorenz and P. Majumdar and G. Maneva and K. Mannheim and O. Mansutti and M. Mariotti and M. Mart{\'i}nez and D. Mazin and C. Merck and M. Meucci and M. Meyer and Miranda, {J. M.} and R. Mirzoyan and S. Mizobuchi and A. Moralejo and D. Nieto and K. Nilsson and J. Ninkovic and E. O{\~n}a-Wilhelmi and N. Otte and I. Oya and D. Paneque and M. Panniello and R. Paoletti and Paredes, {J. M.} and M. Pasanen and D. Pascoli and F. Pauss and R. Pegna and M. Persic",

year = "2008",

month = feb,

day = "20",

doi = "10.1086/525270",

language = "English",

volume = "674",

pages = "1037--1055",

journal = "Astrophysical Journal",

issn = "0004-637X",

number = "2",

}

Albert, J, Aliu, E, Anderhub, H, Antoranz, P, Armada, A, Baixeras, C, Barrio, JA, Bartko, H, Bastiere, D, Becker, JK, Bednarek, W, Berger, K, Bigongiari, C, Biland, A, Bock, RK, Bordas, P, Bosch-Ramon, V, Bretz, T, Britvitch, I, Camara, M, Carmona, E, Chilingarian, A, Coarasa, JA, Commichau, S, Contreras, JL, Cortina, J, Costado, MT, Curtef, V, Danielyan, V, Dazzi, F, De Angelis, A, Delgado, C, De Los Reyes, R, De Lotto, B, Domingo-Santamaría, E, Dorner, D, Doro, M, Errando, M, Fagiolini, M, Ferenc, D, Fernández, E, Firpo, R, Flix, J, Fonseca, MV, Font, L, Fuchs, M, Galante, N, García-López, R, Garczarczyk, M, Gaug, M, Giller, M, Goebel, F, Hakobyan, D, Hayashida, M, Hengstebeck, T, Herrero, A, Höhne, D, Hose, J, Hsu, CC, Jacon, 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, Martínez, M, Mazin, D, Merck, C, Meucci, M, Meyer, M, Miranda, JM, Mirzoyan, R, Mizobuchi, S, Moralejo, A, Nieto, D, Nilsson, K, Ninkovic, J, Oña-Wilhelmi, E, Otte, N, Oya, I, Paneque, D, Panniello, M, Paoletti, R, Paredes, JM, Pasanen, M, Pascoli, D, Pauss, F, Pegna, R & Persic, M 2008, 'VHE γ-ray observation of the Crab Nebula and its pulsar with the MAGIC telescope', Astrophysical Journal, vol. 674, no. 2, pp. 1037-1055. https://doi.org/10.1086/525270

TY - JOUR

T1 - VHE γ-ray observation of the Crab Nebula and its pulsar with the MAGIC telescope

AU - Albert, J.

AU - Aliu, E.

AU - Anderhub, H.

AU - Antoranz, P.

AU - Armada, A.

AU - Baixeras, C.

AU - Barrio, J. A.

AU - Bartko, H.

AU - Bastiere, D.

AU - Becker, J. K.

AU - Bednarek, W.

AU - Berger, K.

AU - Bigongiari, C.

AU - Biland, A.

AU - Bock, R. K.

AU - Bordas, P.

AU - Bosch-Ramon, V.

AU - Bretz, T.

AU - Britvitch, I.

AU - Camara, M.

AU - Carmona, E.

AU - Chilingarian, A.

AU - Coarasa, J. A.

AU - Commichau, S.

AU - Contreras, J. L.

AU - Cortina, J.

AU - Costado, M. T.

AU - Curtef, V.

AU - Danielyan, V.

AU - Dazzi, F.

AU - De Angelis, A.

AU - Delgado, C.

AU - De Los Reyes, R.

AU - De Lotto, B.

AU - Domingo-Santamaría, E.

AU - Dorner, D.

AU - Doro, M.

AU - Errando, M.

AU - Fagiolini, M.

AU - Ferenc, D.

AU - Fernández, E.

AU - Firpo, R.

AU - Flix, J.

AU - Fonseca, M. V.

AU - Font, L.

AU - Fuchs, M.

AU - Galante, N.

AU - García-López, R.

AU - Garczarczyk, M.

AU - Gaug, M.

AU - Giller, M.

AU - Goebel, F.

AU - Hakobyan, D.

AU - Hayashida, M.

AU - Hengstebeck, T.

AU - Herrero, A.

AU - Höhne, D.

AU - Hose, J.

AU - Hsu, C. C.

AU - Jacon, P.

AU - Jogler, T.

AU - Kosyra, R.

AU - Kranich, D.

AU - Kritzer, R.

AU - Laille, A.

AU - Lindfors, E.

AU - Lombardi, S.

AU - Longo, F.

AU - López, J.

AU - López, M.

AU - Lorenz, E.

AU - Majumdar, P.

AU - Maneva, G.

AU - Mannheim, K.

AU - Mansutti, O.

AU - Mariotti, M.

AU - Martínez, M.

AU - Mazin, D.

AU - Merck, C.

AU - Meucci, M.

AU - Meyer, M.

AU - Miranda, J. M.

AU - Mirzoyan, R.

AU - Mizobuchi, S.

AU - Moralejo, A.

AU - Nieto, D.

AU - Nilsson, K.

AU - Ninkovic, J.

AU - Oña-Wilhelmi, E.

AU - Otte, N.

AU - Oya, I.

AU - Paneque, D.

AU - Panniello, M.

AU - Paoletti, R.

AU - Paredes, J. M.

AU - Pasanen, M.

AU - Pascoli, D.

AU - Pauss, F.

AU - Pegna, R.

AU - Persic, M.

PY - 2008/2/20

Y1 - 2008/2/20

N2 - We report about very high energy (VHE) γ-ray observations of the Crab Nebula with the MAGIC telescope. The γ-ray flux from the nebula was measured between 60 GeV and 9 TeV The energy spectrum can be described by a curved power law dF/dE = f0(E/300 GeV) [a-b log10(E300 GeV)] with a flux normalization f0 of (6.0 ± 0.2stat) × 10-10 cm-2s -1 TeV-1, a = -2.31 ± 0.06stat, and b = -0.26 ± 0.07stat. The peak in the spectral energy distribution is estimated at 77 ± 35 GeV Within the observation time and the experimental resolution of the telescope, the γ-ray emission is steady and pointlike. The emission's center of gravity coincides with the position of the pulsar. Pulsed γ-ray emission from the pulsar could not be detected. We constrain the cutoff energy of the pulsed spectrum to be less than 27 GeV, assuming that the differential energy spectrum has an exponential cutoff. For a superexponential shape, the cutoff energy can be as high as 60 GeV. © 2008. The American Astronomical Society. All rights reserved.

AB - We report about very high energy (VHE) γ-ray observations of the Crab Nebula with the MAGIC telescope. The γ-ray flux from the nebula was measured between 60 GeV and 9 TeV The energy spectrum can be described by a curved power law dF/dE = f0(E/300 GeV) [a-b log10(E300 GeV)] with a flux normalization f0 of (6.0 ± 0.2stat) × 10-10 cm-2s -1 TeV-1, a = -2.31 ± 0.06stat, and b = -0.26 ± 0.07stat. The peak in the spectral energy distribution is estimated at 77 ± 35 GeV Within the observation time and the experimental resolution of the telescope, the γ-ray emission is steady and pointlike. The emission's center of gravity coincides with the position of the pulsar. Pulsed γ-ray emission from the pulsar could not be detected. We constrain the cutoff energy of the pulsed spectrum to be less than 27 GeV, assuming that the differential energy spectrum has an exponential cutoff. For a superexponential shape, the cutoff energy can be as high as 60 GeV. © 2008. The American Astronomical Society. All rights reserved.

KW - Acceleration of particles

KW - Gamma rays: observations

KW - Radiation mechanisms: nonthermal

U2 - 10.1086/525270

DO - 10.1086/525270

M3 - Article

SN - 0004-637X

VL - 674

SP - 1037

EP - 1055

JO - Astrophysical Journal

JF - Astrophysical Journal

IS - 2

ER -

VHE γ-ray observation of the Crab Nebula and its pulsar with the MAGIC telescope

Abstract

Keywords

Access to Document

Fingerprint

Cite this