MAGIC TeV Gamma-Ray Observations of Markarian 421 during Multiwavelength Campaigns in 2006
Creators: name: MAGIC Collaboration
name: Aleksić, J.
name: Antonelli, L. A.
name: Antoranz, P.
name: Backes, M.
name: Baixeras, C.
name: Balestra, S.
name: Barrio, J. A.
name: Bastieri, D.
name: González, J. Becerra
name: Bednarek, W.
name: Berdyugin, A.
name: Berger, K.
name: Bernardini, E.
name: Biland, A.
name: Bock, R. K.
name: Bonnoli, G.
name: Bordas, P.
name: Tridon, D. Borla
name: Bosch-Ramon, V.
name: Bose, D.
name: Braun, I.
name: Bretz, T.
name: Britzger, D.
name: Camara, M.
name: Carmona, E.
name: Carosi, A.
name: Colin, P.
name: Commichau, S.
name: Contreras, J. L.
name: Cortina, J.
name: Costado, M. T.
name: Covino, S.
name: Dazzi, F.
name: De Angelis, A.
name: del Pozo, E. De Cea
name: Mendez, C. Delgado
name: Reyes, R. De los
name: De Lotto, B.
name: De Maria, M.
name: De Sabata, F.
name: Doert, M.
name: Domínguez, A.
name: Prester, D. Dominis
name: Dorner, D.
name: Doro, M.
name: Elsaesser, D.
name: Errando, M.
name: Ferenc, D.
name: Fonseca, M. V.
name: Font, L.
name: López, R. J. García
name: Garczarczyk, M.
name: Gaug, M.
name: Godinovic, N.
name: Hadasch, D.
name: Herrero, A.
name: Hildebrand, D.
name: Höhne-Mönch, D.
name: Hose, J.
name: Hrupec, D.
name: Hsu, C. C.
name: Jogler, T.
name: Klepser, S.
name: Krähenbühl, T.
name: Kranich, D.
name: La Barbera, A.
name: Laille, A.
name: Leonardo, E.
name: Lindfors, E.
name: Lombardi, S.
name: Longo, F.
name: López, M.
name: Lorenz, E.
name: Majumdar, P.
name: Maneva, G.
name: Mankuzhiyil, N.
name: Mannheim, K.
name: Maraschi, L.
name: Mariotti, M.
name: Martínez, M.
name: Mazin, D.
name: Meucci, M.
name: Miranda, J. M.
name: Mirzoyan, R.
name: Miyamoto, H.
name: Moldón, J.
name: Moles, M.
name: Moralejo, A.
name: Nieto, D.
name: Nilsson, K.
name: Ninkovic, J.
name: Orito, R.
name: Oya, I.
name: Paiano, S.
name: Paoletti, R.
name: Paredes, J. M.
name: Partini, S.
name: Pasanen, M.
name: Pascoli, D.
name: Pauss, F.
name: Pegna, R. G.
name: Perez-Torres, M. A.
name: Persic, M.
name: Peruzzo, L.
name: Prada, F.
name: Prandini, E.
name: Puchades, N.
name: Puljak, I.
name: Reichardt, I.
name: Rhode, W.
name: Ribó, M.
name: Rico, J.
name: Rissi, M.
name: Rügamer, S.
name: Saggion, A.
name: Saito, T. Y.
name: Salvati, M.
name: Sánchez-Conde, M.
name: Satalecka, K.
name: Scalzotto, V.
name: Scapin, V.
name: Schultz, C.
name: Schweizer, T.
name: Shayduk, M.
name: Shore, S. N.
name: Sierpowska-Bartosik, A.
name: Sillanpää, A.
name: Sitarek, J.
name: Sobczynska, D.
name: Spanier, F.
name: Spiro, S.
name: Stamerra, A.
name: Steinke, B.
name: Struebig, J. C.
name: Suric, T.
name: Takalo, L.
name: Tavecchio, F.
name: Temnikov, P.
name: Terzic, T.
name: Tescaro, D.
name: Teshima, M.
name: Torres, D. F.
name: Vankov, H.
name: Wagner, R. M.
name: Zabalza, V.
name: Zandanel, F.
name: Zanin, R.
Publisher: name: arXiv
Year: 2010
Subjects: subject: Cosmology and Nongalactic Astrophysics (astro-ph.CO)
subject: FOS: Physical sciences
subject: FOS: Physical sciences

description: The Major Atmospheric Gamma Imaging Cerenkov (MAGIC) telescope participated in three multiwavelength (MWL) campaigns, observing the blazar Markarian (Mkn) 421 during the nights of 2006 April 28, 29, and 2006 June 14. We analyzed the corresponding MAGIC very-high energy observations during 9 nights from 2006 April 22 to 30 and on 2006 June 14. We inferred light curves with sub-day resolution and night-by-night energy spectra. A strong gamma-ray signal was detected from Mkn 421 on all observation nights. The flux (E &gt; 250 GeV) varied on night-by-night basis between (0.92+-0.11)10^-10 cm^-2 s^-1 (0.57 Crab units) and (3.21+-0.15)10^-10 cm^-2 s^-1 (2.0 Crab units) in 2006 April. There is a clear indication for intra-night variability with a doubling time of 36+-10(stat) minutes on the night of 2006 April 29, establishing once more rapid flux variability for this object. For all individual nights gamma-ray spectra could be inferred, with power-law indices ranging from 1.66 to 2.47. We did not find statistically significant correlations between the spectral index and the flux state for individual nights. During the June 2006 campaign, a flux substantially lower than the one measured by the Whipple 10-m telescope four days later was found. Using a log-parabolic power law fit we deduced for some data sets the location of the spectral peak in the very-high energy regime. Our results confirm the indications of rising peak energy with increasing flux, as expected in leptonic acceleration models.
description: 11 pages, 7 figures, accepted for publication by Astron. Astrophys