Performance of the MAGIC stereo system obtained with Crab Nebula data

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); 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); B. Marcote (15); 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); D.; Nieto (2); K. Nilsson (10,29); R. Orito (13); I. Oya (2); 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) ((1); IFAE; Edifici Cn.; Campus UAB; E-08193 Bellaterra; Spain; (2) Universidad; Complutense; E-28040 Madrid; Spain; (3) INAF National Institute for; Astrophysics; I-00136 Rome; Italy; (4) Universit\`a di Siena; and INFN Pisa,; I-53100 Siena; Italy; (5) Technische Universit\"at Dortmund; D-44221; Dortmund; Germany; (6) Universit\`a di Padova; INFN; I-35131 Padova,; Italy; (7) Inst. de Astrof\'isica de Canarias; E-38200 La Laguna; Tenerife,; Spain; (8) Depto. de Astrof\'isica; Universidad de La Laguna; E-38206 La; Laguna; Spain; (9) University of \L\'od\'z; PL-90236 Lodz; Poland; (10); Tuorla Observatory; University of Turku; FI-21500 Piikki\"o; Finland; (11); Deutsches Elektronen-Synchrotron (DESY); D-15738 Zeuthen; Germany; (12) ETH; Zurich; CH-8093 Zurich; Switzerland; (13) Max-Planck-Institut f\"ur Physik,; D-80805 M\"unchen; Germany; (14) Universit\"at W\"urzburg; D-97074; W\"urzburg; Germany; (15) Universitat de Barcelona (ICC/IEEC); E-08028; Barcelona; Spain; (16) Universit\`a di Udine; and INFN Trieste; I-33100; Udine; Italy; (17) Institut de Ci\`encies de l'Espai (IEEC-CSIC); E-08193; Bellaterra; Spain; (18) Inst. de Astrof\'isica de Andaluc\'ia (CSIC); E-18080; Granada; Spain; (19) Croatian MAGIC Consortium; Rudjer Boskovic Institute,; University of Rijeka; University of Split; HR-10000 Zagreb; Croatia; (20); Universitat Aut\`onoma de Barcelona; E-08193 Bellaterra; Spain; (21) Inst.; for Nucl. Research; Nucl. Energy; BG-1784 Sofia; Bulgaria; (22); INAF/Osservatorio Astronomico; INFN; I-34143 Trieste; Italy; (23); Universit\`a dell'Insubria; Como; I-22100 Como; Italy; (24) Universit\`a di; Pisa; and INFN Pisa; I-56126 Pisa; Italy; (25) ICREA; E-08010 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)

arXiv:1108.1477·astro-ph.IM·August 31, 2012

Performance of the MAGIC stereo system obtained with Crab Nebula data

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)

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TL;DR

This paper evaluates the performance of the MAGIC stereo system using Crab Nebula data, demonstrating improved sensitivity, angular resolution, and systematic analysis for gamma-ray observations above 290 GeV.

Contribution

It provides the first detailed assessment of MAGIC stereo system performance with Crab Nebula data, highlighting sensitivity and resolution improvements.

Findings

01

Sensitivity as good as 0.76% of Crab flux in 50 hours above 290 GeV

02

Angular resolution better than 0.07 degrees at high energies

03

Trigger threshold of 50-60 GeV for the MAGIC telescopes

Abstract

MAGIC is a system of two Imaging Atmospheric Cherenkov Telescopes located in the Canary island of La Palma. Since autumn 2009 both telescopes have been working together in stereoscopic mode, providing a significant improvement with respect to the previous single-telescope observations. We use observations of the Crab Nebula taken at low zenith angles to assess the performance of the MAGIC stereo system. The trigger threshold of the MAGIC telescopes is 50-60 GeV. Advanced stereo analysis techniques allow MAGIC to achieve a sensitivity as good as (0.76 +/- 0.03)% of the Crab Nebula flux in 50 h of observations above 290 GeV. The angular resolution at those energies is better than ~0.07 degree. We also perform a detailed study of possible systematic effects which may influence the analysis of the data taken with the MAGIC telescopes.

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