English   español  
Please use this identifier to cite or link to this item: http://hdl.handle.net/10261/45417
logo share SHARE logo core CORE   Add this article to your Mendeley library MendeleyBASE

Visualizar otros formatos: MARC | Dublin Core | RDF | ORE | MODS | METS | DIDL
Exportar a otros formatos:

MAGIC TeV Gamma-Ray Observations of Markarian 421 during Multiwavelength Campaigns in 2006

AuthorsAleksic, J.; Cea del Pozo, Elsa de ; Domínguez, A. ; Hadasch, Daniela ; Moles, Mariano ; Pérez-Torres, Miguel A. ; Prada, Francisco ; Sánchez-Conde, Miguel A. ; Torres, Diego F. ; Zandanel, Fabio
KeywordsRadiation mechanisms: non-thermal
BL Lacertae objects: individual: Mkn 421
Gamma rays: galaxies
Issue DateSep-2010
CitationAstronomy and Astrophysics 519: A32 (2010)
Abstract[Context]: Wide-range spectral coverage of blazar-type active galactic nuclei is of paramount importance for understanding the particle acceleration mechanisms assumed to take place in their jets. The Major Atmospheric Gamma Imaging Cerenkov (MAGIC) telescope participated in three multiwavelength (MWL) campaigns, observing the blazar Markarian (Mkn) 421 during the nights of April 28 and 29, 2006, and June 14, 2006. [Aims]: We analyzed the corresponding MAGIC very-high energy observations during 9 nights from April 22 to 30, 2006 and on June 14, 2006. We inferred light curves with sub-day resolution and night-by-night energy spectra. [Methods]: MAGIC detects γ-rays by observing extended air showers in the atmosphere. The obtained air-shower images were analyzed using the standard MAGIC analysis chain. [Results]: A strong γ-ray signal was detected from Mkn 421 on all observation nights. The flux (E > 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 April 2006. There is a clear indication for intra-night variability with a doubling time of 36± min on the night of April 29, 2006, establishing once more rapid flux variability for this object. For all individual nights γ-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.
Description10 páginas, 7 figuras, 6 tablas.-- El Pdf del artículo es la versión pre-print: arXiv:1001.1291.-- MAGIC Collaboration: et al.
Publisher version (URL)http://dx.doi.org/10.1051/0004-6361/200913945
Appears in Collections:(IAA) Artículos
(ICE) Artículos
Files in This Item:
File Description SizeFormat 
1001.1291.pdf331,33 kBAdobe PDFThumbnail
Show full item record
Review this work

Related articles:

WARNING: Items in Digital.CSIC are protected by copyright, with all rights reserved, unless otherwise indicated.