LONG-TERM MONITORING OF THE TeV EMISSION FROM Mrk 421 WITH THE ARGO-YBJ EXPERIMENT

Bartoli, B.; Bernardini, P.; Bi, X. J.; Bleve, C.; Bolognino, I.; Branchini, P.; Budano, A.; Melcarne, A. K. Calabrese; Camarri, P.; Cao, Z.; Cappa, A.; Cardarelli, R.; Catalanotti, S.; Cattaneo, Claudio; Celio, Paola; Chen, S. Z.; Chen, T. L.; Chen, Y.; Creti, P.; Cui, S. W.; Dai, B. Z.; Staiti, G. DʼAlí; Danzengluobu,; Dattoli, M.; Mitri, I. De; Piazzoli, B. D’Ettorre; Girolamo, T. Di; Ding, X. H.; Sciascio, G. Di; Feng, C.; Feng, Z.; Feng, Z. Y.; Galeazzi, F.; Galeotti, P.; Giroletti, E.; Gou, Q. B.; Guo, Y. Q.; He, H. H.; Hu, Haibing; Hu, Hongbo; Huang, Q.; Iacovacci, M.; Iuppa, R.; James, I.; Jia, H. Y.; Labaciren,; Li, H. J.; Li, J. Y.; Li, X. X.; Liguori, G.; Liu, C.; Liu, C. Q.; Liu, J.; Liu, M. Y.; Lü, H.; H., X.; Mancarella, G.; Mari, Stefano Maria; Marsella, G.; Martello, D.; Mastroianni, S.; Montini, P.; Ning, C. C.; Pagliaro, A.; Panareo, M.; Panico, B.; Perrone, L.; Pistilli, P.; Qu, X. B.; Rossi, E.; Ruggieri, F.; Salvini, P.; Santonico, R.; Shen, P. R.; Sheng, X. D.; Shi, Feng; Stănescu, C.; Surdo, A.; Tan, Y. H.; Vallania, P.; Vernetto, S.; Vigorito, C.; Wang, Bo; Wang, H.; Wu, C. Y.; Wu, H. R.; Xu, Benda; Xue, L.; Yan, Y. X.; Yang, Q. Y.; Yang, X. C.; Yao, Z. G.; Yuan, A. F.; Zha, M.; Zhang, H. M.; Zhang, Jilong; Zhang, Jianli; Zhang, L.; Zhang, P.; Zhang, X. Y.; Zhang, Y.; Zhaxiciren,; Zhaxisangzhu,; Zhou, X. X.; Zhu, F. R.; Zhu, Q. Q.; Zizzi, G.

doi:10.1088/0004-637x/734/2/110

Cited by 78 publications

(83 citation statements)

References 43 publications

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“…The existence of a correlation between the X-ray and VHE fluxes is well established on certain timescales and in certain activity states of Mrk 421: claims of correlated variability stem from long-term monitoring of fluxes in these bands that include high-activity states (Bartoli et al 2011;Acciari et al 2014), as well as observations of particular flaring events that probe correlated variability on timescales as short as 1 hr (Giebels et al 2007;Fossati et al 2008;Acciari et al 2009). The detection of such a correlation in a low state was reported for the first time in Aleksić et al (2015b), using the X-ray (Swift-XRT, RXTE-PCA) and VHE (MAGIC, VERITAS) data obtained during the 4.5-month multiwavelength campaign in 2009, when Mrk 421 did not show any flaring activity and varied around its typical Swift-XRT 0.3-10keV count rates of ∼25s −1 and VHE flux of 0.5Crab.…”

Section: X-ray Versus Vhe γ-Ray Bandmentioning

confidence: 99%

MULTIWAVELENGTH STUDY OF QUIESCENT STATES OF Mrk 421 WITH UNPRECEDENTED HARD X-RAY COVERAGE PROVIDED BY NuSTAR IN 2013

Baloković¹,

Paneque²,

Madejski³

et al. 2016

ApJ

113

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We present coordinated multiwavelength observations of the bright, nearby BL Lacertae object Mrk 421 taken in 2013 January-March, involving GASP-WEBT, Swift, NuSTAR, Fermi-LAT, MAGIC, VERITAS, and other collaborations and instruments, providing data from radio to very high energy(VHE) γ-ray bands. NuSTAR yielded previously unattainable sensitivity in the 3-79keV range, revealing that the spectrum softens when the source is dimmer until the X-ray spectral shape saturates into a steep 3 G » power law, with no evidence for an exponential cutoff or additional hard components up to ∼80keV. For the first time, we observed both the synchrotron and the inverse-Compton peaks of the spectral energy distribution (SED) simultaneously shifted to frequencies below the typical quiescent state by an order of magnitude. The fractional variability as a function of photon energy shows a double-bump structure that relates to the two bumps of the broadband SED. In each bump, the variability increases with energy, which, in the framework of the synchrotron self-Compton model, implies that the electrons with higher energies are more variable. The measured multi band variability, the significant X-ray-to-VHE correlation down to some of the lowest fluxes ever observed in both bands, the lack of correlation between optical/UV and X-ray flux, the low degree of polarization and its significant (random) variations, the short estimated electron cooling time, and the significantly longer variability timescale observed in the NuSTAR light curves point toward in situ electron acceleration and suggest that there are multiple compact regions contributing to the broadband emission of Mrk 421 during low-activity states.

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Section: X-ray Versus Vhe γ-Ray Bandmentioning

confidence: 99%

MULTIWAVELENGTH STUDY OF QUIESCENT STATES OF Mrk 421 WITH UNPRECEDENTED HARD X-RAY COVERAGE PROVIDED BY NuSTAR IN 2013

Baloković¹,

Paneque²,

Madejski³

et al. 2016

ApJ

113

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“…ARGO-YBJ is currently the only experiment with duty-cycle sufficient (> 85%) to guarantee a continuous survey from ∼ 300 GeV to ∼ 20 TeV on a large field of view (∼ 2 sr in the local frame). More details can be found in [7].…”

Section: Physics Resultsmentioning

confidence: 99%

Results from the ARGO-YBJ experiment

Iuppa¹

2012

Proceedings of XI Workshop on Resistive Plate Chambers and Related Detectors — PoS(RPC2012)

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The ARGO-YBJ experiment consists of a 5000 m 2 single layer of Resistive Plate Chambers situated at Yangbajing, Tibet (P.R. of China), 4300 meters a.s.l. (atmospheric depth 600 g/cm 2 ). The percentage of active area all over the carpet is 92% and a partially instrumented guard ring (1700 m 2 ) around the central zone extends the instrumented area up to 11000 m 2 . The experiment is operated in scaler mode, shower mode and analog mode and is sensitive to cosmic rays in the 10 9 -10 15 eV energy range. From few hundreds GeV on, the arrival direction of cosmic rays is inferred by the study of the induced extensive air showers. A review of the most important results of the ARGO-YBJ experiment in gamma-ray astronomy and cosmic-ray physics will be given, focusing on the potential of RPCs in ground-based astroparticle physics.

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“…Details on the analysis procedure (e.g., reconstruction algorithms, data selection, background evaluation, systematic errors) are discussed in [5][6][7]. The performance of the detector (angular resolution, pointing accuracy, energy scale calibration) and the operation stability are continuously monitored by observing the Moon shadow, i.e., the deficit of CRs detected in its direction [6,8].…”

Section: The Argo-ybj Experimentsmentioning

confidence: 99%

The ARGO-YBJ legacy to next generation wide field-of-view experiments

Sciascio¹

2017

EPJ Web Conf.

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Abstract. The ARGO-YBJ experiment has been in stable data taking for more than 5 years at the YangBaJing Cosmic Ray Observatory (Tibet, P.R. China, 4300 m a.s.l., 606 g/cm 2 ). With a duty-cycle greater than 86% the detector collected about 5×10 11 events in a wide energy range, from few hundreds GeV up to about 10 PeV. High altitude location and detector features make ARGO-YBJ capable of investigating a wide range of important issues in Cosmic Ray and Astroparticle Physics by imaging the front of atmospheric showers with unprecedented resolution and detail. In this contribution some of the latest physics results obtained by ARGO-YBJ in gamma-ray astronomy and in cosmic ray physics are summarized. The prospects of TeV gamma-ray observations with new ground-based wide field-of-view detectors are presented.

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LONG-TERM MONITORING OF THE TeV EMISSION FROM Mrk 421 WITH THE ARGO-YBJ EXPERIMENT

Cited by 78 publications

References 43 publications

MULTIWAVELENGTH STUDY OF QUIESCENT STATES OF Mrk 421 WITH UNPRECEDENTED HARD X-RAY COVERAGE PROVIDED BY NuSTAR IN 2013

MULTIWAVELENGTH STUDY OF QUIESCENT STATES OF Mrk 421 WITH UNPRECEDENTED HARD X-RAY COVERAGE PROVIDED BY NuSTAR IN 2013

Results from the ARGO-YBJ experiment

The ARGO-YBJ legacy to next generation wide field-of-view experiments

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