Phase-resolved energy spectra of the Crab Pulsar in the range of 50-400   GeV measured with the MAGIC Telescopes

MAGIC Collaboration: J. Aleksi\'c (1); E. A. Alvarez (2); L. A.; Antonelli (3); P. Antoranz (4); M. Asensio (2); M. Backes (5); J. A. Barrio; (2); D. Bastieri (6); J. Becerra Gonz\'alez (7,8); W. Bednarek (9); A.; Berdyugin (10); K. Berger (7,8); E. Bernardini (11); A. Biland (12); O.; Blanch (1); R. K. Bock (13); A. Boller (12); G. Bonnoli (3); D. Borla Tridon; (13); I. Braun (12); T. Bretz (14,26); A. Ca\~nellas (15); E. Carmona (13),; A. Carosi (3); P. Colin (13); E. Colombo (7); J. L. Contreras (2); J. Cortina; (1); L. Cossio (16); S. Covino (3); F. Dazzi (16,27); A. De Angelis (16); G.; De Caneva (11); E. De Cea del Pozo (17); B. De Lotto (16); C. Delgado Mendez; (7,28); A. Diago Ortega (7,8); M. Doert (5); A. Dom\'inguez (18); D. Dominis; Prester (19); D. Dorner (12); M. Doro (20); D. Eisenacher (14); D. Elsaesser; (14); D. Ferenc (19); M. V. Fonseca (2); L. Font (20); C. Fruck (13); R. J.; Garc\'ia L\'opez (7,8); M. Garczarczyk (7); D. Garrido (20); G. Giavitto (1),; N. Godinovi\'c (19); D. Hadasch (17); D. H\"afner (13); A. Herrero (7,8); D.; Hildebrand (12); D. H\"ohne-M\"onch (14); J. Hose (13); D. Hrupec (19); T.; Jogler (13); H. Kellermann (13); S. Klepser (1); T. Kr\"ahenb\"uhl (12); J.; Krause (13); J. Kushida (13); A. La Barbera (3); D. Lelas (19); E. Leonardo; (4); N. Lewandowska (14); E. Lindfors (10); S. Lombardi (6); M. L\'opez (2),; A. L\'opez-Oramas (1); E. Lorenz (12,13); M. Makariev (21); G. Maneva (21),; N. Mankuzhiyil (16); K. Mannheim (14); L. Maraschi (3); M. Mariotti (6); M.; Mart\'inez (1); D. Mazin (1,13); M. Meucci (4); J. M. Miranda (4); R.; Mirzoyan (13); J. Mold\'on (15); A. Moralejo (1); P. Munar-Adrover (15); A.; Niedzwiecki (9); D. Nieto (2); K. Nilsson (10,29); N. Nowak (13); R. Orito; (13); D. Paneque (13); R. Paoletti (4); S. Pardo (2); J. M. Paredes (15); S.; Partini (4); M. A. Perez-Torres (1); M. Persic (16,22); L. Peruzzo (6); M.; Pilia (23); J. Pochon (7); F. Prada (18); P. G. Prada Moroni (24); E.; Prandini (6); I. Puerto Gimenez (7); I. Puljak (19); I. Reichardt (1); R.; Reinthal (10); W. Rhode (5); M. Rib\'o (15); J. Rico (25,1); S. R\"ugamer; (14); A. Saggion (6); K. Saito (13); T. Y. Saito (13); M. Salvati (3); K.; Satalecka (2); V. Scalzotto (6); V. Scapin (2); C. Schultz (6); T. Schweizer; (13); M. Shayduk (13); S. N. Shore (24); A. Sillanp\"a\"a (10); J. Sitarek; (9); I. Snidaric (19); D. Sobczynska (9); F. Spanier (14); S. Spiro (3); V.; Stamatescu (1); A. Stamerra (4); B. Steinke (13); J. Storz (14); N. Strah; (5); T. Suri\'c (19); L. Takalo (10); H. Takami (13); F. Tavecchio (3); P.; Temnikov (21); T. Terzi\'c (19); D. Tescaro (24); M. Teshima (13); O. Tibolla; (14); D. F. Torres (25,17); A. Treves (23); M. Uellenbeck (5); H. Vankov; (21); P. Vogler (12); R. M. Wagner (13); Q. Weitzel (12); V. Zabalza (15); F.; Zandanel (18); R. Zanin (1); K. Hirotani (30) ((1) IFAE; Edifici Cn.; Campus; UAB; Bellaterra; Spain; (2) Universidad Complutense; Madrid; Spain; (3) INAF; National Institute for Astrophysics; Rome; Italy; (4) Universit\`a di Siena,; and INFN Pisa; Siena; Italy; (5) Technische Universit\"at Dortmund; Dortmund,; Germany; (6) Universit\`a di Padova; INFN; Padova; Italy; (7) Inst. de; Astrof\'isica de Canarias; La Laguna; Tenerife; Spain; (8) Depto. de; Astrof\'isica; Universidad de La Laguna; La Laguna; Spain; (9) University of; \L\'od\'z; Lodz; Poland; (10) Tuorla Observatory; University of Turku,; Piikki\"o; Finland; (11) Deutsches Elektronen-Synchrotron (DESY); Zeuthen,; Germany; (12) ETH Zurich; Zurich; Switzerland; (13) Max-Planck-Institut f\"ur; Physik; M\"unchen; Germany; (14) Universit\"at W\"urzburg; W\"urzburg,; Germany; (15) Universitat de Barcelona (ICC/IEEC); Barcelona; Spain; (16); Universit\`a di Udine; and INFN Trieste; Udine; Italy; (17) Institut de; Ci\`encies de l'Espai (IEEC-CSIC); Bellaterra; Spain; (18) Inst. de; Astrof\'isica de Andaluc\'ia (CSIC); Granada; Spain; (19) Croatian MAGIC; Consortium; Rudjer Boskovic Institute; University of Rijeka; University of; Split; Zagreb; Croatia; (20) Universitat Aut\`onoma de Barcelona; Bellaterra,; Spain; (21) Inst. for Nucl. Research; Nucl. Energy; Sofia; Bulgaria; (22); INAF/Osservatorio Astronomico; INFN; Trieste; Italy; (23) Universit\`a; dell'Insubria; Como; Como; Italy; (24) Universit\`a di Pisa; and INFN Pisa,; Pisa; Italy; (25) ICREA; Barcelona; Spain; (26) now at: Ecole polytechnique; f\'ed\'erale de Lausanne (EPFL); Lausanne; Switzerland; (27) supported by; INFN Padova; (28) now at: Centro de Investigaciones Energ\'eticas,; Medioambientales y Tecnol\'ogicas (CIEMAT); Madrid; Spain; (29) now at:; Finnish Centre for Astronomy with ESO (FINCA); University of Turku; Finland; (30) ASIAA/National Tsing Hua University-TIARA; Taipei; Taiwan)

arXiv:1109.6124·astro-ph.HE·August 8, 2012

Phase-resolved energy spectra of the Crab Pulsar in the range of 50-400 GeV measured with the MAGIC Telescopes

MAGIC Collaboration: J. Aleksi\'c (1), E. A. Alvarez (2), L. A., Antonelli (3), P. Antoranz (4), M. Asensio (2), M. Backes (5), J. A. Barrio, (2), D. Bastieri (6), J. Becerra Gonz\'alez (7,8), W. Bednarek (9), A., Berdyugin (10), K. Berger (7,8), E. Bernardini (11)

PDF

TL;DR

This study presents detailed phase-resolved spectra of the Crab Pulsar's very high-energy gamma-ray emission between 50 and 400 GeV, confirming pulsed signals and extending spectral measurements to energies comparable with satellite observatories.

Contribution

It provides the widest spectra to date of the Crab Pulsar's VHE components, with high-resolution data confirming pulsed signals and supporting inverse Compton scattering as the emission mechanism.

Findings

01

Detection of significant pulsed signals in both main and interpulse phases.

02

Spectra extend up to 400 GeV, compatible with power-law models.

03

Spectral indices and flux ratios consistent with inverse Compton emission.

Abstract

We use 73 h of stereoscopic data taken with the MAGIC telescopes to investigate the very high-energy (VHE) gamma-ray emission of the Crab pulsar. Our data show a highly significant pulsed signal in the energy range from 50 to 400 GeV in both the main pulse (P1) and the interpulse (P2) phase regions. We provide the widest spectra to date of the VHE components of both peaks, and these spectra extend to the energy range of satellite-borne observatories. The good resolution and background rejection of the stereoscopic MAGIC system allows us to cross-check the correctness of each spectral point of the pulsar by comparison with the corresponding (strong and well-known) Crab nebula flux. The spectra of both P1 and P2 are compatible with power laws with photon indices of 4.0 \pm 0.8 (P1) and 3.42 \pm 0.26 (P2), respectively, and the ratio P1/P2 between the photon counts of the two pulses is…

Peer Reviews

No public reviews on file for this paper yet. If you reviewed it on a platform where reviews are public (OpenReview, ICLR, NeurIPS, ICML), you can paste yours below so the community can read it here.

Videos

No videos yet. Explain this paper in a talk, walkthrough, or lecture? Add one.