Observation of Very High Energy Gamma‐Ray Emission from the Active Galactic Nucleus 1ES 1959+650 Using the MAGIC Telescope

Albert, J.; Aliu, E.; Anderhub, H.; Antoranz, P.; Armada, A.; Asensio, M.; Baixeras, C.; Barrio, J. A.; Bartko, H.; Bastieri, D.; Bednarek, W.; Berger, K.; Bigongiari, C.; Biland, A.; Bisesi, Erica; Böck, R.; Bretz, T.; Britvitch, I.; Cámara, Miguel; Chilingarian, A.; Ciprini, S.; Coarasa, J. A.; Commichau, S.; Contreras, J. L.; Cortina, J.; Danielyan, V.; Dazzi, F.; Angelis, A. De; Reyes, R. de los; Lotto, B. De; Domingo-Santamaría, E.; Dorner, D.; Doro, M.; Errando, M.; Ferenc, D.; Fernández, E.; Firpo, R.; Flix, J.; Fonseca, M. V.; Font, L.; Galante, N.; Garczarczyk, M.; Gaug, M.; Gebauer, J.; Giannitrapani, R.; Giller, M.; Göebel, F.; Hakobyan, D.; Hayashida, M.; Hengstebeck, T.; Höhne, D.; Hose, J.; Jacoń, P.; Kalekin, O.; Kranich, D.; Laille, A.; Lenisa, T.; Liebing, P.; Lindfors, E.; Longo, F.; López, J.; López, M.; Lorenz, E.; Lucarelli, F.; Majumdar, P.; Maneva, G.; Mannheim, K.; Mariotti, M.; Martı́nez, M.; Mase, K.; Mazin, D.; Merck, C.; Merck, M.; Meucci, M.; Meyer, M.; Miranda, J. M.; Mirzoyan, R.; Mizobuchi, S.; Moralejo, A.; Nilsson, K.; Oña-Wilhelmi, E.; Orduña, R.; Otte, A. N.; Oya, I.; Paneque, D.; Paoletti, R.; Pasanen, M.; Pascoli, D.; Pauß, F.; Pavel, N.; Pegna, R.; Peruzzo, L.; Piccioli, A.; Pin, Massimo Del; Prandini, E.; Rico, J.; Rhode, W.; Riegel, B.; Rissi, M.; Robert, A.; Rossato, G.; Rügamer, S.; Saggion, A.; Sánchez, A.; Sartori, P.; Scalzotto, V.; Schmitt, R.; Schweizer, T.; Shayduk, M.; Shinozaki, K.; Sidro, N.; Sillanpää, A.; Sobczyńska, D.; Stamerra, A.; Stark, L. S.; Takalo, L. O.; Temnikov, P.; Tescaro, D.; Teshima, M.; Tonello, N.; Torres, A. de; Torres, D. F.; Turini, N.; Vankov, H.; Vitale, V.; Wagner, R. M.; Wibig, T.; Wittek, W.; Zapatero, J.

doi:10.1086/499421

Cited by 62 publications

(16 citation statements)

References 26 publications

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“…It is also possible that optical emission may come from ''old'' components that do not shine in X-rays anymore, but could in fact be closer to the central engine. The examination of a possible correlation between the TeV -ray flux and X-ray flux will benefit greatly from more-sensitive Cerenkov telescopes such as VERITAS or MAGIC (MAGIC detected 1ES 1959+650 in 2004 September and October in a state of low activity, with a significance of 8.2 after $6.0 hr of observations; Albert et al 2006). …”

Section: Sed and Ssc Modelingmentioning

confidence: 99%

Multiwavelength Observations of 1ES 1959+650, 1 Year after the Strong Outburst of 2002

Gutierrez¹,

Badran²,

Bradbury³

et al. 2006

ApJ

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In 2003 April-May, the blazar 1ES 1959+650 showed an increased level of X-ray activity. This prompted a multiwavelength observation campaign with the Whipple 10 m -ray telescope, the Rossi X-Ray Timing Explorer, the Bordeaux Optical Observatory, and the University of Michigan Radio Astronomy Observatory. We present the multiwavelength data taken from 2003 May 2 to June 7 and compare the source characteristics with those measured during observations taken during the years 2000 and 2002. The X-ray observations gave a data set with high signal-tonoise ratio light curves and energy spectra; however, the -ray observations did not reveal a major TeV -ray flare. Furthermore, we find that the radio and optical fluxes do not show statistically significant deviations from those measured during the 2002 flaring periods. While the X-ray flux and X-ray photon index appear correlated during subsequent observations, the apparent correlation evolved significantly among the years 2000, 2002, and 2003. We discuss the implications of this finding for the mechanism that causes the flaring activity.

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Section: Sed and Ssc Modelingmentioning

confidence: 99%

Multiwavelength Observations of 1ES 1959+650, 1 Year after the Strong Outburst of 2002

Gutierrez¹,

Badran²,

Bradbury³

et al. 2006

ApJ

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“…Since then it has shown several flaring episodes at VHE ( > 100 GeV) γ-ray energies, with the most noticeable one being in 2002 when it showed enhanced TeV emission without any contemporaneous X-ray flare (Aharonian et al 2003;Krawczynski et al 2004;Daniel et al 2005;Reimer et al 2005). In 2004, the source was observed in low state by MAGIC collaboration with a flux of about 20% of the Crab and at ∼ 8σ significance level above ∼ 180 GeV (Albert et al 2006). Broadband variability of the source was studied in 2012 using strictly simultaneous observations from VERITAS and Swift and reflected emission scenario was used to explain the variability (Aliu et al 2014).…”

Section: Introductionmentioning

confidence: 99%

Broadband study of blazar 1ES 1959+650 during flaring state in 2016

Patel

Shukla

Chitnis

et al. 2018

A&A

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Aims. The nearby TeV blazar 1ES 1959+650 (z=0.047) was reported to be in flaring state during June -July 2016 by Fermi-LAT, FACT, MAGIC and VERITAS collaborations. We studied the spectral energy distributions (SEDs) in different states of the flare during MJD 57530 -57589 using simultaneous multiwaveband data to understand the possible broadband emission scenario during the flare. Methods. The UV/optical and X-ray data from UVOT and XRT respectively on board Swift and high energy γ-ray data from Fermi-LAT are used to generate multiwaveband lightcurves as well as to obtain high flux states and quiescent state SEDs. The correlation and lag between different energy bands is quantified using discrete correlation function. The synchrotron self Compton (SSC) model was used to reproduce the observed SEDs during flaring and quiescent states of the source. Results. A decent correlation is seen between X-ray and high energy γ-ray fluxes. The spectral hardening with increase in the flux is seen in X-ray band. The powerlaw index vs flux plot in γ-ray band indicates the different emission regions for 0.1 -3 GeV and 3-300 GeV energy photons. Two zone SSC model satisfactorily fits the observed broadband SEDs. The inner zone is mainly responsible for producing synchrotron peak and high energy γ-ray part of the SED in all states. The second zone is mainly required to produce less variable optical/UV and low energy γ-ray emission. Conclusions. Conventional single zone SSC model does not satisfactorily explain broadband emission during observation period considered. There is an indication of two emission zones in the jet which are responsible for producing broadband emission from optical to high energy γ-rays.

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“…It was shown only recently that quiescent states can be detected now in short (∼hours) observations (Aharonian et al 2005a). Little is known about average activity cycles and flare time scales, except for a few sources: Mkn 421 (e.g., Aharonian et al 2002b;Błażejowski et al 2005), Mkn 501 (e.g., Aharonian et al 1999;Krawczynski et al 2002), and 1ES 1959+650 (e.g., Krawczynski et al 2004;Albert et al 2006). (2) Source photons above ∼100 GeV are attenuated by the EBL through γ-γ-interactions.…”

Section: Introductionmentioning

confidence: 99%

Detection of VHE gamma-ray emission from the distant blazar 1ES 1101-232 with HESS and broadband characterisation

Aharonian

Akhperjanian

Bazer‐Bachi

et al. 2007

A&A

119

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Context. The blazar 1ES 1101-232 was observed with the High Energy Stereoscopic System (HESS) of Atmospheric Cherenkov Telescopes (ACT) in 2004 and 2005, for a live time of 43 h. VHE (E > 10 11 eV) γ-rays were detected for the first time from this object. Aims. VHE observations of blazars are used to investigate the inner parts of the blazar jets, and also to study the extragalactic background light (EBL) in the near-infrared band. Methods. Observations in 2005 were conducted in a multiwavelength campaign, together with the RXTE satellite and optical observations. In 2004, simultaneous observations with XMM-Newton were obtained. Results. 1ES 1101-232 was detected with HESS with an excess of 649 photons, at a significance of 10σ. The measured VHE γ-ray flux amounts to dN/dE = (5.63 ± 0.89) × 10 −13 (E/TeV) −(2.94±0.20) cm −2 s −1 TeV −1 , above a spectral energy threshold of 225 GeV. No significant variation of the VHE γ-ray flux on any time scale was found. 1ES 1101-232 exhibits a very hard spectrum, and at a redshift of z = 0.186, is the blazar with the highest confirmed redshift detected in VHE γ-rays so far. Conclusions. The data allow the construction of truly simultaneous spectral energy distributions of the source, from the optical to the VHE band. Using an EBL model with νF ν = 14 nWm −2 sr −1 at 1.5 µm as presented in Aharonian et al. (2006a) suggests an intrinsic VHE power output peak of the source at above 3 TeV.

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Observation of Very High Energy Gamma‐Ray Emission from the Active Galactic Nucleus 1ES 1959+650 Using the MAGIC Telescope

Cited by 62 publications

References 26 publications

Multiwavelength Observations of 1ES 1959+650, 1 Year after the Strong Outburst of 2002

Multiwavelength Observations of 1ES 1959+650, 1 Year after the Strong Outburst of 2002

Broadband study of blazar 1ES 1959+650 during flaring state in 2016

Detection of VHE gamma-ray emission from the distant blazar 1ES 1101-232 with HESS and broadband characterisation

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