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

J. Aleksić; S. Ansoldi; L. A. Antonelli; P. Antoranz; A. Babic; P. Bangale; U. Barres De Almeida; J. A. Barrio; J. Becerra González; W. Bednarek; E. Bernardini; B. Biasuzzi; A. Biland; O. Blanch; S. Bonnefoy; G. Bonnoli; F. Borracci; T. Bretz; E. Carmona; A. Carosi; P. Colin; E. Colombo; J. L. Contreras; J. Cortina; S. Covino; P. Da Vela; F. Dazzi; A. De Angelis; G. De Caneva; B. De Lotto; C. Delgado Mendez; M. Doert; D. Dominis Prester; D. Dorner; M. Doro; S. Einecke; D. Eisenacher; D. Elsaesser; E. Farina; D. Ferenc; D. Fidalgo; M. V. Fonseca; L. Font; K. Frantzen; C. Fruck; R. J.García López; M. Garczarczyk; D. Garrido Terrats; M. Gaug; N. Godinović; A. González Muñoz; S. R. Gozzini; D. Hadasch; M. Hayashida; J. Herrera; A. Herrero; D. Hildebrand; K. Hirotani; J. Hose; D. Hrupec; W. Idec; V. Kadenius; H. Kellermann; K. Kodani; Y. Konno; J. Krause; H. Kubo; J. Kushida; A. La Barbera; D. Lelas; N. Lewandowska; E. Lindfors; S. Lombardi; M. López; R. López-Coto; A. López-Oramas; E. Lorenz; I. Lozano; M. Makariev; K. Mallot; G. Maneva; N. Mankuzhiyil; K. Mannheim; L. Maraschi; B. Marcote; M. Mariotti; M. Martínez; D. Mazin; U. Menzel; J. M. Miranda; R. Mirzoyan; A. Moralejo; P. Munar-Adrover; D. Nakajima; A. Niedzwiecki; K. Nilsson; K. Nishijima; K. Noda; N. Nowak; R. Orito

doi:10.1051/0004-6361/201423664

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

J. Aleksić, S. Ansoldi, L. A. Antonelli, P. Antoranz, A. Babic, P. Bangale, U. Barres De Almeida, J. A. Barrio, J. Becerra González, W. Bednarek, E. Bernardini, B. Biasuzzi, A. Biland, O. Blanch, S. Bonnefoy, G. Bonnoli, F. Borracci, T. Bretz, E. Carmona, A. CarosiP. Colin, E. Colombo, J. L. Contreras, J. Cortina, S. Covino, P. Da Vela, F. Dazzi, A. De Angelis, G. De Caneva, B. De Lotto, C. Delgado Mendez, M. Doert, D. Dominis Prester, D. Dorner, M. Doro, S. Einecke, D. Eisenacher, D. Elsaesser, E. Farina, D. Ferenc, D. Fidalgo, M. V. Fonseca, L. Font, K. Frantzen, C. Fruck, R. J.García López, M. Garczarczyk, D. Garrido Terrats, M. Gaug, N. Godinović, A. González Muñoz, S. R. Gozzini, D. Hadasch, M. Hayashida, J. Herrera, A. Herrero, D. Hildebrand, K. Hirotani, J. Hose, D. Hrupec, W. Idec, V. Kadenius, H. Kellermann, K. Kodani, Y. Konno, J. Krause, H. Kubo, J. Kushida, A. La Barbera, D. Lelas, N. Lewandowska, E. Lindfors, S. Lombardi, M. López, R. López-Coto, A. López-Oramas, E. Lorenz, I. Lozano, M. Makariev, K. Mallot, G. Maneva, N. Mankuzhiyil, K. Mannheim, L. Maraschi, B. Marcote, M. Mariotti, M. Martínez, D. Mazin, U. Menzel, J. M. Miranda, R. Mirzoyan, A. Moralejo, P. Munar-Adrover, D. Nakajima, A. Niedzwiecki, K. Nilsson, K. Nishijima, K. Noda, N. Nowak, R. Orito

Institut de Física d'Altes Energies (IFAE)

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

25 Citations (Scopus)

Abstract

Context. The Crab pulsar is the only astronomical pulsed source detected at very high energy (VHE, E > 100 GeV) gamma rays. The emission mechanism of VHE pulsation is not yet fully understood, although several theoretical models have been proposed. Aims. In order to test new models, we measured the light curve and the spectra of the Crab pulsar with high precision by means of deep observations. Methods. We analyzed 135 h of selected MAGIC data taken between 2009 and 2013 in stereoscopic mode. In order to discuss the spectral shape in connection with lower energies, 5.5 years of Fermi-LAT data were also analyzed. Results. The known two pulses per period were detected with a significance of 8.0σ and 12.6σ. In addition, significant emission was found between the two pulses with 6.2σ. Conclusions. We discovered the bridge emission above 50 GeV between the two main pulses. This emission can not be explained with the existing theories. These data can be used for testing new theoretical models. © ESO, 2014.

Original language	English
Article number	L12
Journal	Astronomy and Astrophysics
Volume	565
DOIs	https://doi.org/10.1051/0004-6361/201423664
Publication status	Published - 1 Jan 2014

Keywords

Gamma rays: stars
Pulsars: individual: Crab pulsar
Stars: neutron

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10.1051/0004-6361/201423664

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Aleksić, J., Ansoldi, S., Antonelli, L. A., Antoranz, P., Babic, A., Bangale, P., De Almeida, U. B., Barrio, J. A., González, J. B., Bednarek, W., Bernardini, E., Biasuzzi, B., Biland, A., Blanch, O., Bonnefoy, S., Bonnoli, G., Borracci, F., Bretz, T., Carmona, E., ... Orito, R. (2014). Detection of bridge emission above 50 GeV from the Crab pulsar with the MAGIC telescopes. Astronomy and Astrophysics, 565, [L12]. https://doi.org/10.1051/0004-6361/201423664

@article{f76554debe5f48c4a802a189a3721963,

title = "Detection of bridge emission above 50 GeV from the Crab pulsar with the MAGIC telescopes",

abstract = "Context. The Crab pulsar is the only astronomical pulsed source detected at very high energy (VHE, E > 100 GeV) gamma rays. The emission mechanism of VHE pulsation is not yet fully understood, although several theoretical models have been proposed. Aims. In order to test new models, we measured the light curve and the spectra of the Crab pulsar with high precision by means of deep observations. Methods. We analyzed 135 h of selected MAGIC data taken between 2009 and 2013 in stereoscopic mode. In order to discuss the spectral shape in connection with lower energies, 5.5 years of Fermi-LAT data were also analyzed. Results. The known two pulses per period were detected with a significance of 8.0σ and 12.6σ. In addition, significant emission was found between the two pulses with 6.2σ. Conclusions. We discovered the bridge emission above 50 GeV between the two main pulses. This emission can not be explained with the existing theories. These data can be used for testing new theoretical models. {\textcopyright} ESO, 2014.",

keywords = "Gamma rays: stars, Pulsars: individual: Crab pulsar, Stars: neutron",

author = "J. Aleksi{\'c} and S. Ansoldi and Antonelli, {L. A.} and P. Antoranz and A. Babic and P. Bangale and {De Almeida}, {U. Barres} and Barrio, {J. A.} and Gonz{\'a}lez, {J. Becerra} and W. Bednarek and E. Bernardini and B. Biasuzzi and A. Biland and O. Blanch and S. Bonnefoy and G. Bonnoli and F. Borracci and T. Bretz and E. Carmona and A. Carosi and P. Colin and E. Colombo and Contreras, {J. L.} and J. Cortina and S. Covino and {Da Vela}, P. and F. Dazzi and {De Angelis}, A. and {De Caneva}, G. and {De Lotto}, B. and Mendez, {C. Delgado} and M. Doert and Prester, {D. Dominis} and D. Dorner and M. Doro and S. Einecke and D. Eisenacher and D. Elsaesser and E. Farina and D. Ferenc and D. Fidalgo and Fonseca, {M. V.} and L. Font and K. Frantzen and C. Fruck and L{\'o}pez, {R. J.Garc{\'i}a} and M. Garczarczyk and Terrats, {D. Garrido} and M. Gaug and N. Godinovi{\'c} and Mu{\~n}oz, {A. Gonz{\'a}lez} and Gozzini, {S. R.} and D. Hadasch and M. Hayashida and J. Herrera and A. Herrero and D. Hildebrand and K. Hirotani and J. Hose and D. Hrupec and W. Idec and V. Kadenius and H. Kellermann and K. Kodani and Y. Konno and J. Krause and H. Kubo and J. Kushida and {La Barbera}, A. and D. Lelas and N. Lewandowska and E. Lindfors and S. Lombardi and M. L{\'o}pez and R. L{\'o}pez-Coto and A. L{\'o}pez-Oramas and E. Lorenz and I. Lozano and M. Makariev and K. Mallot and G. Maneva and N. Mankuzhiyil and K. Mannheim and L. Maraschi and B. Marcote and M. Mariotti and M. Mart{\'i}nez and D. Mazin and U. Menzel and Miranda, {J. M.} and R. Mirzoyan and A. Moralejo and P. Munar-Adrover and D. Nakajima and A. Niedzwiecki and K. Nilsson and K. Nishijima and K. Noda and N. Nowak and R. Orito",

year = "2014",

month = jan,

day = "1",

doi = "10.1051/0004-6361/201423664",

language = "English",

volume = "565",

journal = "Astronomy and Astrophysics",

issn = "0004-6361",

}

Aleksić, J, Ansoldi, S, Antonelli, LA, Antoranz, P, Babic, A, Bangale, P, De Almeida, UB, Barrio, JA, González, JB, 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, JL, Cortina, J, Covino, S, Da Vela, P, Dazzi, F, De Angelis, A, De Caneva, G, De Lotto, B, Mendez, CD, Doert, M, Prester, DD, Dorner, D, Doro, M, Einecke, S, Eisenacher, D, Elsaesser, D, Farina, E, Ferenc, D, Fidalgo, D, Fonseca, MV, Font, L, Frantzen, K, Fruck, C, López, RJG, Garczarczyk, M, Terrats, DG, Gaug, M, Godinović, N, Muñoz, AG, Gozzini, SR, Hadasch, D, Hayashida, M, Herrera, J, Herrero, A, Hildebrand, D, Hirotani, K, Hose, J, Hrupec, D, Idec, W, Kadenius, V, Kellermann, H, Kodani, K, Konno, Y, Krause, J, Kubo, H, Kushida, J, La Barbera, A, Lelas, D, Lewandowska, N, Lindfors, E, Lombardi, S, López, M, López-Coto, R, López-Oramas, A, Lorenz, E, Lozano, I, Makariev, M, Mallot, K, Maneva, G, Mankuzhiyil, N, Mannheim, K, Maraschi, L, Marcote, B, Mariotti, M, Martínez, M, Mazin, D, Menzel, U, Miranda, JM, Mirzoyan, R, Moralejo, A, Munar-Adrover, P, Nakajima, D, Niedzwiecki, A, Nilsson, K, Nishijima, K, Noda, K, Nowak, N & Orito, R 2014, 'Detection of bridge emission above 50 GeV from the Crab pulsar with the MAGIC telescopes', Astronomy and Astrophysics, vol. 565, L12. https://doi.org/10.1051/0004-6361/201423664

TY - JOUR

T1 - Detection of bridge emission above 50 GeV from the Crab pulsar with the MAGIC telescopes

AU - Aleksić, J.

AU - Ansoldi, S.

AU - Antonelli, L. A.

AU - Antoranz, P.

AU - Babic, A.

AU - Bangale, P.

AU - De Almeida, U. Barres

AU - Barrio, J. A.

AU - González, J. Becerra

AU - Bednarek, W.

AU - Bernardini, E.

AU - Biasuzzi, B.

AU - Biland, A.

AU - Blanch, O.

AU - Bonnefoy, S.

AU - Bonnoli, G.

AU - Borracci, F.

AU - Bretz, T.

AU - Carmona, E.

AU - Carosi, A.

AU - Colin, P.

AU - Colombo, E.

AU - Contreras, J. L.

AU - Cortina, J.

AU - Covino, S.

AU - Da Vela, P.

AU - Dazzi, F.

AU - De Angelis, A.

AU - De Caneva, G.

AU - De Lotto, B.

AU - Mendez, C. Delgado

AU - Doert, M.

AU - Prester, D. Dominis

AU - Dorner, D.

AU - Doro, M.

AU - Einecke, S.

AU - Eisenacher, D.

AU - Elsaesser, D.

AU - Farina, E.

AU - Ferenc, D.

AU - Fidalgo, D.

AU - Fonseca, M. V.

AU - Font, L.

AU - Frantzen, K.

AU - Fruck, C.

AU - López, R. J.García

AU - Garczarczyk, M.

AU - Terrats, D. Garrido

AU - Gaug, M.

AU - Godinović, N.

AU - Muñoz, A. González

AU - Gozzini, S. R.

AU - Hadasch, D.

AU - Hayashida, M.

AU - Herrera, J.

AU - Herrero, A.

AU - Hildebrand, D.

AU - Hirotani, K.

AU - Hose, J.

AU - Hrupec, D.

AU - Idec, W.

AU - Kadenius, V.

AU - Kellermann, H.

AU - Kodani, K.

AU - Konno, Y.

AU - Krause, J.

AU - Kubo, H.

AU - Kushida, J.

AU - La Barbera, A.

AU - Lelas, D.

AU - Lewandowska, N.

AU - Lindfors, E.

AU - Lombardi, S.

AU - López, M.

AU - López-Coto, R.

AU - López-Oramas, A.

AU - Lorenz, E.

AU - Lozano, I.

AU - Makariev, M.

AU - Mallot, K.

AU - Maneva, G.

AU - Mankuzhiyil, N.

AU - Mannheim, K.

AU - Maraschi, L.

AU - Marcote, B.

AU - Mariotti, M.

AU - Martínez, M.

AU - Mazin, D.

AU - Menzel, U.

AU - Miranda, J. M.

AU - Mirzoyan, R.

AU - Moralejo, A.

AU - Munar-Adrover, P.

AU - Nakajima, D.

AU - Niedzwiecki, A.

AU - Nilsson, K.

AU - Nishijima, K.

AU - Noda, K.

AU - Nowak, N.

AU - Orito, R.

PY - 2014/1/1

Y1 - 2014/1/1

N2 - Context. The Crab pulsar is the only astronomical pulsed source detected at very high energy (VHE, E > 100 GeV) gamma rays. The emission mechanism of VHE pulsation is not yet fully understood, although several theoretical models have been proposed. Aims. In order to test new models, we measured the light curve and the spectra of the Crab pulsar with high precision by means of deep observations. Methods. We analyzed 135 h of selected MAGIC data taken between 2009 and 2013 in stereoscopic mode. In order to discuss the spectral shape in connection with lower energies, 5.5 years of Fermi-LAT data were also analyzed. Results. The known two pulses per period were detected with a significance of 8.0σ and 12.6σ. In addition, significant emission was found between the two pulses with 6.2σ. Conclusions. We discovered the bridge emission above 50 GeV between the two main pulses. This emission can not be explained with the existing theories. These data can be used for testing new theoretical models. © ESO, 2014.

AB - Context. The Crab pulsar is the only astronomical pulsed source detected at very high energy (VHE, E > 100 GeV) gamma rays. The emission mechanism of VHE pulsation is not yet fully understood, although several theoretical models have been proposed. Aims. In order to test new models, we measured the light curve and the spectra of the Crab pulsar with high precision by means of deep observations. Methods. We analyzed 135 h of selected MAGIC data taken between 2009 and 2013 in stereoscopic mode. In order to discuss the spectral shape in connection with lower energies, 5.5 years of Fermi-LAT data were also analyzed. Results. The known two pulses per period were detected with a significance of 8.0σ and 12.6σ. In addition, significant emission was found between the two pulses with 6.2σ. Conclusions. We discovered the bridge emission above 50 GeV between the two main pulses. This emission can not be explained with the existing theories. These data can be used for testing new theoretical models. © ESO, 2014.

KW - Gamma rays: stars

KW - Pulsars: individual: Crab pulsar

KW - Stars: neutron

U2 - 10.1051/0004-6361/201423664

DO - 10.1051/0004-6361/201423664

M3 - Article

SN - 0004-6361

VL - 565

JO - Astronomy and Astrophysics

JF - Astronomy and Astrophysics

M1 - L12

ER -

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

Abstract

Keywords

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