Journal
ASTRONOMY & ASTROPHYSICS
Volume 569, Issue -, Pages -Publisher
EDP SCIENCES S A
DOI: 10.1051/0004-6361/201423484
Keywords
galaxies: active; galaxies: jets; gamma rays: galaxies; quasars: individual: PKS 1510-089
Categories
Funding
- German BMBF
- MPG
- Italian INFN
- Swiss National Fund SNF
- Spanish MICINN
- Spanish Consolider-Ingenio programme [CPAN CSD2007-00042, MultiDark CSD2009-00064]
- Bulgarian NSF [DO02-353]
- Academy of Finland [127740, 212656, 210338, 121148]
- DFG Cluster of Excellence Origin and Structure of the Universe
- DFG Collaborative Research Centres [SFB823/C4, SFB876/C3]
- Polish MNiSzW grant [745/N-HESS-MAGIC/2010/0]
- University of Rijeka Project [13.12.1.3.02]
- Croatian Science Foundation [09/176]
- JSPS KAKENHI [25800105, 24000004]
- ERDF
- Spanish MINECO [FPA2012-39502, JCI-2011-10019]
- National Aeronautics and Space Administration
- Department of Energy in the United States
- Commissariat a l'Energie Atomique
- Centre National de la Recherche Scientifique/Institut National de Physique Nucleaire et de Physique des Particules in France
- Agenzia Spaziale Italiana
- Istituto Nazionale di Fisica Nucleare in Italy
- Ministry of Education, Culture, Sports, Science and Technology (MEXT)
- High Energy Accelerator Research Organization (KEK)
- Japan Aerospace Exploration Agency (JAXA) in Japan
- K. A. Wallenberg Foundation
- Swedish Research Council
- Swedish National Space Board in Sweden
- ASI [I/089/06/2, I/042/10/0, I/028/12/0]
- Shota Rustaveli National Science Foundation [FR/638/6-320/12, 31/77]
- NASA [NNX08AW31G, NNX11A043G]
- NSF [AST-0808050, AST-1109911]
- NASA Fermi Guest Investigator grants [NNX11AQ03G, NNX11AO37G, NNX12AO90G]
- BU
- Lowell Observatory
- Smithsonian Institution
- Academia Sinica
- INSU/CNRS (France)
- MPG (Germany)
- IGN (Spain)
- International Max Planck Research School (IMPRS) for Astronomy and Astrophysics at the University of Bonn
- International Max Planck Research School (IMPRS) for Astronomy and Astrophysics at the University of Cologne
- [NNX08AW56G]
- [NNX09AU10G]
- [NNX12AO93G]
- STFC [ST/M003035/1, ST/J001465/1, ST/M000095/1] Funding Source: UKRI
- Grants-in-Aid for Scientific Research [12J09375, 25800105] Funding Source: KAKEN
- NASA [NNX12AO90G, 140747, NNX11AO37G, 139010, NNX11AQ03G, 13245] Funding Source: Federal RePORTER
- Science and Technology Facilities Council [ST/M000095/1, ST/M003035/1, ST/J001465/1] Funding Source: researchfish
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Aims. Amongst more than fifty blazars detected in very high energy (VHE, E > 100 GeV) gamma rays, only three belong to the subclass of flat spectrum radio quasars (FSRQs). The detection of FSRQs in the VHE range is challenging, mainly because of their soft spectra in the GeV-TeV regime. MAGIC observed PKS 1510-089 (z = 0.36) starting 2012 February 3 until April 3 during a high activity state in the high energy (HE, E > 100 MeV) gamma-ray band observed by AGILE and Fermi. MAGIC observations result in the detection of a source with significance of 6.0 standard deviations (sigma). We study the multi-frequency behaviour of the source at the epoch of MAGIC observation, collecting quasi-simultaneous data at radio and optical (GASP-WEBT and F-Gamma collaborations, REM, Steward, Perkins, Liverpool, OVRO, and VLBA telescopes), X-ray (Swift satellite), and HE gamma-ray frequencies. Methods. We study the VHE gamma-ray emission, together with the multi-frequency light curves, 43 GHz radio maps, and spectral energy distribution (SED) of the source. The quasi-simultaneous multi-frequency SED from the millimetre radio band to VHE gamma rays is modelled with a one-zone inverse Compton model. We study two different origins of the seed photons for the inverse Compton scattering, namely the infrared torus and a slow sheath surrounding the jet around the Very Long Baseline Array (VLBA) core. Results. We find that the VHE gamma-ray emission detected from PKS 1510-089 in 2012 February-April agrees with the previous VHE observations of the source from 2009 March-April. We find no statistically significant variability during the MAGIC observations on daily, weekly, or monthly time scales, while the other two known VHE FSRQs (3C 279 and PKS 1222+216) have shown daily scale to sub-hour variability. The gamma-ray SED combining AGILE, Fermi and MAGIC data joins smoothly and shows no hint of a break. The multi-frequency light curves suggest a common origin for the millimetre radio and HE gamma-ray emission, and the HE gamma-ray flaring starts when the new component is ejected from the 43GHz VLBA core and the studied SED models fit the data well. However, the fast HE gamma-ray variability requires that within the modelled large emitting region, more compact regions must exist. We suggest that these observed signatures would be most naturally explained by a turbulent plasma flowing at a relativistic speed down the jet and crossing a standing conical shock.
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