Temporal and spectral gamma-ray properties of Mkn 421  above 250 GeV from CAT observations between 1996 and 2000

Piron, F.; Djannati‐Ataï, A.; Punch, M.; Tavernet, J.‐P.; Barrau, A.; Bazer‐Bachi, R.; Chounet, L.‐M.; Debiais, G.; Degrange, B.; Dezalay, J. P.; Espigat, P.; Fabre, B.; Fleury, P.; Fontaine, G.; Goret, P.; Gouiffès, C.; Khélifi, B.; Malet, Isabelle; Masterson, C.; Mohanty, G.; Nuss, E.; Renault, C.; Rivoal, M.; Rob, L.; Vorobiov, S.

doi:10.1051/0004-6361:20010798

Cited by 140 publications

(123 citation statements)

References 26 publications

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“…Publicly available lightcurve data from 1992 until today were collected from the Whipple (Kerrick et al 1995;Schubnell et al 1996;Buckley et al 1996;Maraschi et al 1999a), HEGRA (Aharonian et al 1999b,a;Krawczynski et al 2001b;Aharonian et al 2001Aharonian et al , 2002Aharonian et al , 2003Aharonian et al , 2004Kestel 2002), CAT (Piron 2000;Piron et al 2001), HESS (Aharonian et al 2005(Aharonian et al , 2006, MAGIC (Albert et al 2008a;Donnarumma et al 2009), and VERITAS (Rebillot et al 2006;Donnarumma et al 2009) experiments. We are also working on collecting more data from these and other experiments such as the Crimean GT-48 Cherenkov telescope (e.g.…”

Section: Lightcurve Datamentioning

confidence: 99%

Long-term lightcurves from combined unified very high energyγ-ray data

Tluczykont

Bernardini²,

Satalecka³

et al. 2010

A&A

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Context. Very high-energy (VHE, E > 100 GeV) γ-ray data are a valuable input for multi-wavelength and multi-messenger (e.g. combination with neutrino data) studies. Aims. We aim at the conservation and homogenization of historical, current, and future VHE γ-ray-data on active galactic nuclei (AGN). Methods. We have collected lightcurve data taken by major VHE experiments since 1991 and combined them into long-term lightcurves for several AGN, and now provide our collected datasets for further use. Due to the lack of common data formats in VHE γ-ray astronomy, we have defined relevant datafields to be stored in standard data formats. The time variability of the combined VHE lightcurve data was investigated, and correlation with archival X-ray data collected by RXTE/ASM tested.Results. The combination of data on the prominent blazar Mrk 421 from different experiments yields a lightcurve spanning more than a decade. From this combined dataset we derive an integral baseline flux from Mrk 421 that must be lower than 33% of the Crab Nebula flux above 1 TeV. The analysis of the time variability yields log-normal flux variations in the VHE-data on Mrk 421. Conclusions. Existing VHE data contain valuable information concerning the variability of AGN and can be an important ingredient for multi-wavelength or multi-messenger studies. In the future, upcoming and planned experiments will provide more data from many transient objects, and the interaction of VHE astronomy with classical astronomy will intensify. In this context a unified and exchangeable data format will become increasingly important.

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Section: Lightcurve Datamentioning

confidence: 99%

Long-term lightcurves from combined unified very high energyγ-ray data

Tluczykont

Bernardini²,

Satalecka³

et al. 2010

A&A

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“…The time-averaged differential VHE γ-ray spectrum of the source, derived using the forward-folding technique described in Piron et al (2001), is presented in Fig. 4.…”

Section: Hess Observations and Resultsmentioning

confidence: 99%

Discovery of VHEγ-ray emission and multi-wavelength observations of the BL Lacertae object 1RXS J101015.9 − 311909

Abramowski¹,

Acero²,

Aharonian³

et al. 2012

A&A

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ABSTRACT1RXS J101015.9−311909 is a galaxy located at a redshift of z = 0.14 hosting an active nucleus (called AGN) belonging to the class of bright BL Lac objects. Observations at high (HE, E > 100 MeV) and very high (VHE, E > 100 GeV) energies provide insights into the origin of very energetic particles present in such sources and the radiation processes at work. We report on results from VHE observations performed between 2006 and 2010 with the H.E.S.S. instrument, an array of four imaging atmospheric Cherenkov telescopes. H.E.S.S. data have been analysed with enhanced analysis methods, making the detection of faint sources more significant. VHE emission at a position coincident with 1RXS J101015.9−311909 is detected with H.E.S.S. for the first time. In a total good-quality livetime of about 49 h, we measure 263 excess counts, corresponding to a significance of 7.1 standard deviations. The photon spectrum above 0.2 TeV can be described by a power-law with a photon index of Γ = 3.08 ± 0.42 stat ± 0.20 sys . The integral flux above 0.2 TeV is about 0.8% of the flux of the Crab nebula and shows no significant variability over the time reported. In addition, public Fermi/LAT data are analysed to search for high energy emission from the source. The Fermi/LAT HE emission in the 100 MeV to 200 GeV energy range is significant at 8.3 standard deviations in the chosen 25-month dataset. UV and X-ray contemporaneous observations with the Swift satellite in May 2007 are also reported, together with optical observations performed with the atom telescope located at the H.E.S.S. site. Swift observations reveal an absorbed X-ray flux of F (0.3−7) keV = 1.04 +0.04 −0.05 × 10 −11 erg cm −2 s −1 in the 0.3−7 keV range. Finally, all the available data are used to study the multi-wavelength properties of the source. The spectral energy distribution (SED) can be reproduced using a simple one-zone Synchrotron Self Compton (SSC) model with emission from a region with a Doppler factor of 30 and a magnetic field between 0.025 and 0.16 G. These parameters are similar to those obtained for other sources of this type.

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“…1, green circle) was used as an integration region for extracting the differential VHE γ-ray spectrum of the source. The spectrum was derived using the forward folding technique [9], and is well described by a power-law with an exponential cut-off function dN/dE = Φ 0 (E/1 TeV) −Γ exp(−E/E c ) with Φ 0 = (8.62 ± 0.73 stat ± 1.72 sys ) × 10 13 cm −2 s −1 TeV −1 , Γ = 1.61 ± 0.11 stat ± 0.20 sys and a cut-off energy of E c = 12.5 +4.0 −2. 4 TeV.…”

Section: Spectral Analysismentioning

confidence: 99%

HESS J1826−130: A very hard γ-ray spectrum source in the galactic plane

Angüner¹,

Aharonian

Bordas³

et al. 2017

AIP Conference Proceedings

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Abstract. HESS J1826−130 is an unidentified hard spectrum source discovered by H.E.S.S. along the Galactic plane, the spectral index being Γ = 1.6 with an exponential cut-off at about 12 TeV. While the source does not have a clear counterpart at longer wavelengths, the very hard spectrum emission at TeV energies implies that electrons or protons accelerated up to several hundreds of TeV are responsible for the emission. In the hadronic case, the VHE emission can be produced by runaway cosmic-rays colliding with the dense molecular clouds spatially coincident with the H.E.S.S. source.

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Temporal and spectral gamma-ray properties of Mkn 421 above 250 GeV from CAT observations between 1996 and 2000

Cited by 140 publications

References 26 publications

Long-term lightcurves from combined unified very high energyγ-ray data

Long-term lightcurves from combined unified very high energyγ-ray data

Discovery of VHEγ-ray emission and multi-wavelength observations of the BL Lacertae object 1RXS J101015.9 − 311909

HESS J1826−130: A very hard γ-ray spectrum source in the galactic plane

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