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29 March 2024 |
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Study of the variable broadband emission of Markarian 501 during the most extreme Swift X-ray activity | MAGIC Collaboration
; V. A. Acciari
; S. Ansoldi
; L. A. Antonelli
; A. Babić
; B. Banerjee
; U. Barres de Almeida
; J. A. Barrio
; J. Becerra González
; W. Bednarek
; E. Bernardini
; A. Berti
; J. Besenrieder
; W. Bhattacharyya
; C. Bigongiari
; O. Blanch
; G. Bonnoli
; G. Busetto
; R. Carosi
; G. Ceribella
; S. Cikota
; S. M. Colak
; P. Colin
; E. Colombo
; J. L. Contreras
; J. Cortina
; S. Covino
; V. D'Elia
; P. Da Vela
; F. Dazzi
; A. De Angelis
; B. De Lotto
; M. Delfino
; J. Delgado
; F. Di Pierro
; E. Do Souto Espi nera
; A. Domínguez
; D. Dominis Prester
; M. Doro
; V. Fallah Ramazani
; A. Fattorini
; A. Fernández-Barral
; G. Ferrara
; D. Fidalgo
; L. Foffano
; M. V. Fonseca
; L. Font
; C. Fruck
; D. Galindo
; S. Gallozzi
; R. J. García López
; M. Garczarczyk
; S. Gasparyan
; M. Gaug
; P. Giammaria
; N. Godinović
; D. Guberman
; D. Hadasch
; A. Hahn
; T. Hassan
; J. Herrera
; J. Hoang
; D. Hrupec
; S. Inoue
; K. Ishio
; Y. Iwamura
; H. Kubo
; J. Kushida
; D. Kuveždić
; A. Lamastra
; D. Lelas
; F. Leone
; E. Lindfors
; S. Lombardi
; F. Longo
; M. López
; A. López-Oramas
; B. Machado de Oliveira Fraga
; C. Maggio
; P. Majumdar
; M. Makariev
; M. Mallamaci
; G. Maneva
; M. Manganaro
; L. Maraschi
; M. Mariotti
; M. Martínez
; S. Masuda
; D. Mazin
; M. Minev
; J. M. Miranda
; R. Mirzoyan
; E. Molina
; A. Moralejo
; V. Moreno
; E. Moretti
; P. Munar-Adrove r
; V. Neustroev
; A. Niedzwiecki
; M. Nievas Rosillo
; C. Nigro
; K. Nilsson
; D. Ninci
; K. Nishijima
; K. Noda
; L. Nogués
; S. Paiano
; J. Palacio
; D. Paneque
; R. Paoletti
; J. M. Paredes
; G. Pedaletti
; P. Peñil
; M. Peresano
; M. Persic
; P. G. Prada Moroni
; E. Prandini
; I. Puljak
; J. R. Garcia
; M. Ribó
; J. Rico
; C. Righi
; A. Rugliancich
; L. Saha
; N. Sahakyan
; T. Saito
; K. Satalecka
; T. Schweizer
; J. Sitarek
; I. Šnidarić
; D. Sobczynska
; A. Somero
; A. Stamerra
; M. Strzys
; T. Surić
; F. Tavecchio
; P. Temnikov
; T. Terzić
; M. Teshima
; N. Torres-Albá
; S. Tsujimoto
; J. van Scherpenberg
; G. Vanzo
; M. Vazquez Acosta
; I. Vovk
; M. Will
; D. Zarić
; FACT Collaboration
; A. Arbet-Engels
; D. Baack
; M. Balbo
; A. Biland
; M. Blank
; T. Bretz
; K. Bruegge
; M. Bulinski
; J. Buss
; M. Doerr
; D. Dorner
; S. Einecke
; D. Elsaesser
; D. Hildebrand
; L. Linhoff
; K. Mannheim
; S. Mueller
; D. Neise
; A. Neronov
; M. Noethe
; A. Paravac
; W. Rhode
; B. Schleicher
; F. Schulz
; K. Sedlaczek
; A. Shukla
; V. Sliusar
; E. von Willert
; R. Walter
; C. Wendel
; A. Tramacere
; A. Lien
; M. Perri
; F. Verrecchia
; M. Armas Padilla
; C. Leto
; A. Lähteenmäki
; M. Tornikoski
; J. Tammi
; | Date: |
21 Jan 2020 | Abstract: | Mrk501 is a very high-energy (VHE) gamma-ray blazar located at z=0.034.
During a period of two weeks in July 2014, the highest X-ray activity of Mrk501
was observed in ~14 years of operation of the Neil Gehrels Swift Gamma-ray
Burst Observatory. We characterize the broadband variability of Mrk501 from
radio to VHE gamma rays, and evaluate whether it can be interpreted within
theoretical scenarios widely used to explain the broadband emission from
blazars. The temporal evolution of the most prominent and variable segments of
the SED is described with a one-zone synchrotron self-Compton model with
variations in the break energy of the electron energy distribution (EED), and
with some adjustments in the magnetic field strength and spectral shape of the
EED. A narrow feature at ~3 TeV was observed in the VHE spectrum measured on
2014 July 19 (MJD 56857.98), which is the day with the highest X-ray flux
($>0.3$ keV) measured during the entire Swift mission. This feature is
inconsistent with the classical analytic functions to describe the measured VHE
spectra (power law, log-parabola, and log-parabola with exponential cutoff) at
more than 3$sigma$. A fit with a log-parabola plus a narrow component is
preferred over the fit with a single log-parabola at more than 4$sigma$, and a
dedicated Monte Carlo simulation estimated the significance of this extra
component to be larger than 3$sigma$. Under the assumption that this VHE
spectral feature is real, we show that it can be reproduced with three distinct
theoretical scenarios: a) a pileup in the EED due to stochastic acceleration;
b) a structured jet with two-SSC emitting regions, with one region dominated by
an extremely narrow EED; and c) an emission from an IC pair cascade. | Source: | arXiv, 2001.7729 | Services: | Forum | Review | PDF | Favorites |
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