B3 Non-refereed article in a conference publication
MAGIC Upper Limits on the VHE emission from Flat Spectrum Radio Quasars
Authors: Mondal, Habib Ahammad; Gliwny, Pawel; Principe, Giacomo; Longo, Francesco; Żywucka-Hejzner, Natalia; Lindfors, Elina; Majumdar, Pratik; Sitarek, Julian; the MAGIC collaboration and the Fermi-LAT collaboration
Editors: Saito, Takayuki; Okumura, Kimihiro
Conference name: International Cosmic Ray Conference
Publisher: Sissa Medialab Srl
Publication year: 2024
Journal: POS Proceedings of Science
Book title : 38th International Cosmic Ray Conference
Journal name in source: Proceedings of Science
Article number: 777
Volume: 444
eISSN: 1824-8039
DOI: https://doi.org/10.22323/1.444.0777
Web address : https://doi.org/10.22323/1.444.0777
Self-archived copy’s web address: https://research.utu.fi/converis/portal/detail/Publication/478135410
Blazars are a class of active galactic nuclei (AGN) where the relativistic jet is pointed towards the observer. They are powerful sources of non-thermal radiation from radio to very high energy (VHE, E>100 GeV) gamma-rays. Flat Spectrum Radio Quasars (FSRQs) are a subclass of blazars where there are absorption or emission lines present in the optical spectra. The observed properties of FSRQs are strongly affected by the magnetic field in the accretion disk which changes the UV emission of Broad Line Region (BLR) and infra-red emission from the Dusty Torus. While many (774 as reported in 4FGL-DR2 catalogue [1]) FSRQs have been detected at high energies (HE; E>100 MeV), only a few (9 as of now) could be detected at VHE. In this contribution, we present observations of nine FSRQs performed by Major Atmospheric Gamma-ray Imaging Cherenkov (MAGIC)telescopes between 2008 and 2020 with a total observation time of 174 hours. We also include a few observations from the Fermi-LAT, Swift-UVOT, Swift-XRT and optical observations from Kungliga Vetenskapsakademien (KVA) for two sources CTA 102 and B2 2234+28. We also modelled the broad band emission of the sources to look for signatures of absorption in the BLR region and hence to put constraints on the location of the emission region.
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Funding information in the publication:
GP acknowledges support by ICSC – Centro Nazionale di Ricerca in High Performance Computing, Big Data and Quantum Computing, funded by European Union – NextGenerationEU. HAM greatly acknowledges the Department of Atomic Energy, Government of India for the necessary funding; the Homi Bhaba National Institute and the Saha Institute of Nuclear Physics for the excellent computing cluster facility at the institute. On behalf of the MAGIC Collaboration, we would like to thank the Instituto de Astrofísica de Canarias for the excellent working conditions at the Observatorio del Roque de los Muchachos in La Palma. The financial support of the German BMBF, MPG and HGF; the Italian INFN and INAF; the Swiss National Fund SNF; the ERDF under the Spanish Ministerio de Ciencia e Innovación (MICINN) (PID2019-104114RB-C31, PID2019-104114RB-C32, PID2019-104114RBC33, PID2019-05510GB C31,PID2019-107847RB-C41, PID2019-107847RB-C42, PID2019-107847RBC44, PID2019-107988GB-C22); the Indian Department of Atomic Energy; the Japanese ICRR, the University of Tokyo, JSPS, and MEXT; the Bulgarian Ministry of Education and Science, National RI Roadmap Project DO1-400/18.12.2020 and the Academy of Finland grant nr. 320045 is gratefully acknowledged.
The Fermi LAT Collaboration acknowledges generous ongoing support from a number of agencies and institutes that have supported both the development and the operation of the LAT as well as scientific data analysis. These include the National Aeronautics and Space Administration and the Department of Energy in the United States, the Commissariat à l’Energie Atomique and the Centre National de la Recherche Scientifique / Institut National de Physique Nucléaire et de Physique des Particules in France, the Agenzia Spaziale Italiana and the Istituto Nazionale di Fisica Nucleare in Italy, the Ministry of Education, Culture, Sports, Science and Technology (MEXT), High Energy Accelerator Research Organization (KEK) and Japan Aerospace Exploration Agency (JAXA) in Japan, and the K. A. Wallenberg Foundation, the Swedish Research Council and the Swedish National Space Board in Sweden. Additional support for science analysis during the operations phase is gratefully acknowledged from the Istituto Nazionale di Astrofisica in Italy and the Centre National d’Etudes Spatiales in France. This work is performed in part under DOE Contract DE-AC02-76SF00515.
