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



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Antoranz Canales, Pedro y Barrio Uña, Juan Abel y Contreras González, José Luis y Fonseca González, Mª Victoria y López Moya, Marcos y Miranda Pantoja, José Miguel y Satalecka, Konstanzja y Scapin, Valeria (2014) Discovery of very high energy gamma-ray emission from the blazar 1ES 1727+502 with the MAGIC Telescopes. Astronomy & Astrophysics, 563 . ISSN 0004-6361

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URL Oficial: http://dx.doi.org/10.1051/0004-6361/201321360

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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) gamma 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, 0.1GeV-100 GeV) gamma-ray data from the Fermi-LAT instrument. We detected, for the first time, VHE gamma-ray emission from 1ES 1727+502 at a statistical significance of 5.5 sigma. 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.

Tipo de documento:Artículo
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© ESO, 2014.

Palabras clave:Large-Area Telescope, BL-Lacertae Objects, Lac Objects, Source Catalog, Crab-Nebula, Calibration, Radiation, Constraints, Connection, Photometry.
Materias:Ciencias > Física > Electricidad
Ciencias > Física > Electrónica
Ciencias > Física > Física nuclear
Código ID:26618
Depositado:08 Sep 2014 09:02
Última Modificación:25 Feb 2015 09:13

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