Constraints on the Very High Energy Emission from BL Lacertae Objects

Horan, D.; Badran, H. M.; Bond, I. H.; Boyle, P. J.; Bradbury, S. M.; Buckley, J. H.; Carter‐Lewis, D. A.; Catanese, M.; Çelik, Ö.; Cui, Wei; Daniel, M. K.; D'Vali, M.; Pérez, I. de la Calle; Duke, C.; Falcone, A.; Fegan, D. J.; Fegan, S. J.; Finley, J. P.; Fortson, L.; Gaidos, J. A.; Gammell, S.; Gibbs, K.; Gillanders, G. H.; Grube, J.; Hall, J.; Hall, T. A.; Hanna, D.; Hillas, A. M.; Holder, J.; Jarvis, A.; Jordan, M.; Kenny, G. E.; Kertzman, M.; Kieda, D.; Kildea, J.; Knapp, J.; Kosack, K.; Krawczynski, H.; Krennrich, F.; Lang, M. J.; Bohec, S. Le; Linton, E.; Lloyd‐Evans, J.; Milovanovic, A.; Moriarty, P.; Müller, D.; Nagai, T.; Nolan, S. J.; Ong, R. A.; Pallassini, R.; Petry, D.; Power-Mooney, B.; Quinn, J.; Quinn, M.; Ragan, K.; Rebillot, P.; Reynolds, P. T.; Rose, H. J.; Schroedter, M.; Sembroski, G. H.; Swordy, S. P.; Syson, A.; Vassiliev, V. V.; Wakely, S. P.; Walker, G.; Weekes, T. C.; Zweerink, J.

doi:10.1086/381430

Cited by 54 publications

(23 citation statements)

References 56 publications

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“…1999), the source became even more interesting for VHE observations. However, W Com was not detected by the Whipple IACT above in 1993/1994(Kerrick et al 1995) 300 GeV and 1995/1996/1998(Horan et al 2004, nor by the solar heliostat Cerenkov telescope STACEE (Scalzo et al 2004 this Letter we report the discovery of VHE g-ray emission from W Com with VERITAS.…”

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confidence: 66%

VERITAS Discovery of >200 GeV Gamma-Ray Emission from the Intermediate-Frequency-Peaked BL Lacertae Object W Comae

Acciari

Aliu

Beilicke

et al. 2008

ApJ

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We report the detection of very high energy g-ray emission from the intermediate-frequency-peaked BL Lacertae object W Comae ( ) by VERITAS. The source was observed between 2008 January and April. A strong z p 0.102 outburst of g-ray emission was measured in the middle of March, lasting for only 4 days. The energy spectrum measured during the two highest flare nights is fit by a power law and is found to be very steep, with a differential photon spectral index of . The integral photon flux above during those G p 3.81 ‫ע‬ 0.35 ‫ע‬ 0.34 200 GeV stat syst two nights corresponds to roughly of the flux from the Crab Nebula. Quasi-simultaneous Swift observations 9% at X-ray energies were triggered by the VERITAS observations. The spectral energy distribution of the flare data can be described by synchrotron self-Compton (SSC) or external Compton (EC) leptonic jet models.

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confidence: 66%

VERITAS Discovery of >200 GeV Gamma-Ray Emission from the Intermediate-Frequency-Peaked BL Lacertae Object W Comae

Acciari

Aliu

Beilicke

et al. 2008

ApJ

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“…The Crimean Astrophysical Observatory claimed detections of 3C 66A above 900 GeV with an integral flux of (3 ± 1) × 10 −11 cm −2 s −1 (Stepanyan et al 2002). Later observations by HEGRA and Whipple reported upper limits of F (> 630 GeV) < 1.42 × 10 −11 cm −2 s −1 (Aharonian et al 2000) and F (> 350 GeV) < 0.59 × 10 −11 cm −2 s −1 (Horan et al 2004), respectively. Additionally, the STACEE observation found a hint of a signal at a 2.2 significance level and derived upper limits of <1.0×10 −11 cm −2 s −1 and <1.8×10 −11 cm −2 s −1 for thresholds of 147 GeV and 200 GeV, respectively (Bramel et al 2005 (Acciari et al 2009).…”

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confidence: 98%

Observations of the Blazar 3c 66a With the Magic Telescopes in Stereoscopic Mode

Aleksić¹,

Antonelli²,

Antoranz³

et al. 2010

ApJ

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We report new observations of the intermediate-frequency peaked BL Lacertae object 3C 66A with the MAGIC telescopes. The data sample we use were taken in 2009 December and 2010 January, and comprises 2.3 hr of good quality data in stereoscopic mode. In this period, we find a significant signal from the direction of the blazar 3C 66A. The new MAGIC stereoscopic system is shown to play an essential role for the separation between 3C 66A and the nearby radio galaxy 3C 66B, which is at a distance of only 6 . The derived integral flux above 100 GeV is 8.3% of the Crab Nebula flux and the energy spectrum is reproduced by a power law of photon index 3.64 ± 0.39 stat ± 0.25 sys . Within errors, this is compatible with the one derived by VERITAS in 2009. From the spectra corrected for absorption by the extragalactic background light, we only find small differences between the four models that we applied, and constrain the redshift of the blazar to z < 0.68.

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“…055, de Vaucouleurs et al 1991) was observed with the Whipple 10 m γ-ray telescope, in March-April 1995 and April-May 1996 for a total of 4.6 h but no signal from this source was detected. Upper limits above 300 GeV were reported for both data sets at the levels of 1.08 × 10 −11 erg cm −2 s −1 (8.6% Crab), and 1.58 × 10 −11 erg cm −2 s −1 (15% Crab), respectively (Horan et al 2004). It was also a target of the single telescope MAGIC-I (Albert et al 2008a), before starting stereoscopic observations with two MAGIC telescopes (Aleksić et al 2012c).…”

Section: Introductionmentioning

confidence: 99%

Discovery of very high energy gamma-ray emission from the blazar 1ES 1727+502 with the MAGIC Telescopes

Aleksić¹,

Antonelli²,

Antoranz³

et al. 2014

A&A

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Motivated by the prediction of a high TeV luminosity we investigated whether the blazar 1ES 1727+502 (z = 0.055) is emitting very high energy (VHE, E > 100 GeV) γ rays. We observed the BL Lac object 1ES 1727+502 in stereoscopic mode with the two MAGIC telescopes for 14 nights between May 6th and June 10th 2011, for a total effective observing time of 12.6 h. To study the multiwavelength spectral energy distribution (SED), we used simultaneous optical R-band data from the KVA telescope, archival UV/optical and X-ray observations from instruments UVOT and XRT on board of the Swift satellite, and high energy (HE, 0.1 GeV-100 GeV) γ-ray data from the Fermi-LAT instrument. We detected, for the first time, VHE γ-ray emission from 1ES 1727+502 at a statistical significance of 5.5σ. The integral flux above 150 GeV is estimated to be (2.1 ± 0.4)% of the Crab nebula flux and the de-absorbed VHE spectrum has a photon index of (2.7 ± 0.5). No significant short-term variability was found in any of the wavebands presented here. We model the SED using a one-zone synchrotron self-Compton model obtaining parameters typical for this class of sources.

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Constraints on the Very High Energy Emission from BL Lacertae Objects

Cited by 54 publications

References 56 publications

VERITAS Discovery of >200 GeV Gamma-Ray Emission from the Intermediate-Frequency-Peaked BL Lacertae Object W Comae

VERITAS Discovery of >200 GeV Gamma-Ray Emission from the Intermediate-Frequency-Peaked BL Lacertae Object W Comae

Observations of the Blazar 3c 66a With the Magic Telescopes in Stereoscopic Mode

Discovery of very high energy gamma-ray emission from the blazar 1ES 1727+502 with the MAGIC Telescopes

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