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تسجيل مستخدم جديدMultiwavelength observations of the blazar BL Lacertae: a new fast TeV gamma-ray flare
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Combined with very-long-baseline interferometry measurements, the observations of fast TeV gamma-ray flares probe the structure and emission mechanism of blazar jets. However, only a handful of such flares have been detected to date, and only within the last few years have these flares been observed from lower-frequency-peaked BL~Lac objects and flat-spectrum radio quasars. We report on a fast TeV gamma-ray flare from the blazar BL~Lacertae observed by VERITAS, with a rise time of $sim$2.3~hr and a decay time of $sim$36~min. The peak flux above 200 GeV is $(4.2 pm 0.6) times 10^{-6} ;text{photon} ;text{m}^{-2}; text{s}^{-1}$ measured with a 4-minute-binned light curve, corresponding to $sim$180% of the flux which is observed from the Crab Nebula above the same energy threshold. Variability contemporaneous with the TeV gamma-ray flare was observed in GeV gamma-ray, X-ray, and optical flux, as well as in optical and radio polarization. Additionally, a possible moving emission feature with superluminal apparent velocity was identified in VLBA observations at 43 GHz, potentially passing the radio core of the jet around the time of the gamma-ray flare. We discuss the constraints on the size, Lorentz factor, and location of the emitting region of the flare, and the interpretations with several theoretical models which invoke relativistic plasma passing stationary shocks.
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Observations of fast TeV $gamma$-ray flares from blazars reveal the extreme compactness of emitting regions in blazar jets. Combined with very-long-baseline radio interferometry measurements, they probe the structure and emission mechanism of the jet
. We report on a fast TeV $gamma$-ray flare from BL Lacertae observed by VERITAS, with a rise time of about 2.3 hours and a decay time of about 36 minutes. The peak flux at $>$200 GeV measured with the 4-minute binned light curve is $(4.2 pm 0.6) times 10^{-6} ;text{photons} ;text{m}^{-2}, text{s}^{-1}$, or $sim$180% the Crab Nebula flux. Variability in GeV $gamma$-ray, X-ray, and optical flux, as well as in optical and radio polarization was observed around the time of the TeV $gamma$-ray flare. A possible superluminal knot was identified in the VLBA observations at 43 GHz. The flare constrains the size of the emitting region, and is consistent with several theoretical models with stationary shocks.
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gral flux above 200 GeV reached $(3.4pm0.6) times 10^{-6} ;text{photons};text{m}^{-2}text{s}^{-1}$, roughly 125% of the Crab Nebula flux measured by VERITAS. The light curve indicates that the observations missed the rising phase of the flare but covered a significant portion of the decaying phase. The exponential decay time was determined to be $13pm4$ minutes, making it one of the most rapid gamma-ray flares seen from a TeV blazar. The gamma-ray spectrum of BL Lacertae during the flare was soft, with a photon index of $3.6pm 0.4$, which is in agreement with the measurement made previously by MAGIC in a lower flaring state. Contemporaneous radio observations of the source with the Very Long Baseline Array (VLBA) revealed the emergence of a new, superluminal component from the core around the time of the TeV gamma-ray flare, accompanied by changes in the optical polarization angle. Changes in flux also appear to have occurred at optical, UV, and GeV gamma-ray wavelengths at the time of the flare, although they are difficult to quantify precisely due to sparse coverage. A strong flare was seen at radio wavelengths roughly four months later, which might be related to the gamma-ray flaring activities. We discuss the implications of these multiwavelength results.
The mechanisms producing fast variability of the $gamma$-ray emission in active galactic nuclei are under debate. The MAGIC telescopes detected a fast very high energy (VHE, E$>100$ GeV) $gamma$-ray flare from BL Lacertae on 2015 June 15. The flare h
ad a maximum flux of $(1.5pm 0.3)times 10^{-10}$ photons cm$^{-2}$ s$^{-1}$ and halving time of $26pm8$ minutes. The MAGIC observations were triggered by a high state in the optical and high energy (HE, E$>100$ MeV) $gamma$-ray bands. In this paper we present the MAGIC VHE $gamma$-ray data together with multiwavelength data from radio, optical, X-rays, and HE $gamma$ rays from 2015 May 1 to July 31. Well-sampled multiwavelength data allow us to study the variability in detail and compare it to the other epochs when fast VHE $gamma$-ray flares have been detected from this source. Interestingly, we find that the behaviour in radio, optical, X-rays and HE $gamma$-rays is very similar to two other observed VHE $gamma$-ray flares. In particular, also during this flare there was an indication of rotation of the optical polarization angle and of activity at the 43,GHz core. These repeating patterns indicate a connection between the three events. We also test modelling of the spectral energy distribution, based on constraints from the light curves and VLBA observations, with two different geometrical setups of two-zone inverse Compton models. In addition we model the $gamma$-ray data with the star-jet interaction model. We find that all of the tested emission models are compatible with the fast VHE $gamma$-ray flare, but all have some tension with the multiwavelength observations.
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