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Detection of persistent VHE gamma-ray emission from PKS 1510–089 by the MAGIC telescopes during low states between 2012 and 2017

Acciari, V. A. and Kiehlmann, S. (2018) Detection of persistent VHE gamma-ray emission from PKS 1510–089 by the MAGIC telescopes during low states between 2012 and 2017. Astronomy and Astrophysics, 619 . Art. No. A159. ISSN 0004-6361. http://resolver.caltech.edu/CaltechAUTHORS:20181210-112439274

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Abstract

Context. PKS 1510–089 is a flat spectrum radio quasar strongly variable in the optical and GeV range. To date, very high-energy (VHE, > 100 GeV) emission has been observed from this source either during long high states of optical and GeV activity or during short flares. Aims. We search for low-state VHE gamma-ray emission from PKS 1510–089. We characterize and model the source in a broadband context, which would provide a baseline over which high states and flares could be better understood. Methods. PKS 1510–089 has been monitored by the MAGIC telescopes since 2012. We use daily binned Fermi-LAT flux measurements of PKS 1510–089 to characterize the GeV emission and select the observation periods of MAGIC during low state of activity. For the selected times we compute the average radio, IR, optical, UV, X-ray, and gamma-ray emission to construct a low-state spectral energy distribution of the source. The broadband emission is modeled within an external Compton scenario with a stationary emission region through which plasma and magnetic fields are flowing. We also perform the emission-model-independent calculations of the maximum absorption in the broad line region (BLR) using two different models. Results. The MAGIC telescopes collected 75 hr of data during times when the Fermi-LAT flux measured above 1 GeV was below 3  ×  10^(−8) cm^(−2) s^(−1), which is the threshold adopted for the definition of a low gamma-ray activity state. The data show a strongly significant (9.5σ) VHE gamma-ray emission at the level of (4.27 ± 0.61_(stat))  ×  10^(−12) cm^(−2) s^(−1) above 150 GeV, a factor of 80 lower than the highest flare observed so far from this object. Despite the lower flux, the spectral shape is consistent with earlier detections in the VHE band. The broadband emission is compatible with the external Compton scenario assuming a large emission region located beyond the BLR. For the first time the gamma-ray data allow us to place a limit on the location of the emission region during a low gamma-ray state of a FSRQ. For the used model of the BLR, the 95% confidence level on the location of the emission region allows us to place it at a distance > 74% of the outer radius of the BLR.


Item Type:Article
Related URLs:
URLURL TypeDescription
https://doi.org/10.1051/0004-6361/201833618DOIArticle
https://arxiv.org/abs/1806.05367arXivDiscussion Paper
ORCID:
AuthorORCID
Kiehlmann, S.0000-0001-6314-9177
Additional Information:© 2018 ESO. Article published by EDP Sciences. Received 12 June 2018; Accepted 31 August 2018; Published online 20 November 2018. 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 and MPG, the Italian INFN and INAF, the Swiss National Fund SNF, the ERDF under the Spanish MINECO (FPA2015-69818-P, FPA2012-36668, FPA2015-68378-P, FPA2015-69210-C6-2-R, FPA2015-69210-C6-4-R, FPA2015-69210-C6-6-R, AYA2015-71042-P, AYA2016-76012-C3-1-P, ESP2015-71662-C2-2-P, CSD2009-00064), and the Japanese JSPS and MEXT is gratefully acknowledged. This work was also supported by the Spanish Centro de Excelencia “Severo Ochoa” SEV-2012-0234 and SEV-2015-0548, and Unidad de Excelencia “María de Maeztu” MDM-2014-0369, by the Croatian Science Foundation (HrZZ) Project IP-2016-06-9782 and the University of Rijeka Project 13.12.1.3.02, by the DFG Collaborative Research Centers SFB823/C4 and SFB876/C3, the Polish National Research Centre grant UMO-2016/22/M/ST9/00382, and by the Brazilian MCTIC, CNPq and FAPERJ. 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’Études Spatiales in France. This work was performed in part under DOE Contract DE-AC02-76SF00515. This paper has made use of up-to-date SMARTS optical/near-infrared light curves that are available at www.astro.yale.edu/smarts/glast/home.php. IA acknowledges support from a Ramón y Cajal grant of the Ministerio de Economía, Industria, y Competitividad (MINECO) of Spain. Acquisition and reduction of the POLAMI and MAPCAT data was supported in part by MINECO through grants AYA2010-14844, AYA2013-40825-P, and AYA2016-80889-P, and by the Regional Government of Andalucía through grant P09-FQM-4784. The POLAMI observations were carried out at the IRAM 30m Telescope. IRAM is supported by INSU/CNRS (France), MPG (Germany), and IGN (Spain). The MAPCAT observations were carried out at the German-Spanish Calar Alto Observatory, which is jointly operated by the Max-Plank-Institut für Astronomie and the Instituto de Astrofísica de Andalucía-CSIC. This research has made use of data from the OVRO 40m monitoring program (Richards et al. 2011), which is supported in part by NASA grants NNX08AW31G, NNX11A043G, and NNX14AQ89G and NSF grants AST-0808050 and AST-1109911. This publication makes use of data obtained at the Metsähovi Radio Observatory, operated by Aalto University, Finland. The authors would like to thank a number of people who provided comments to the manuscript: R. Angioni, N. MacDonald, M. Giroletti, R. Caputo, D. Thompson, and the anonymous reviewer. We would also like to thank M. Böttcher for providing us with the numerical values of the optical depths calculated in Böttcher & Els (2016).
Funders:
Funding AgencyGrant Number
Bundesministerium für Bildung und Forschung (BMBF)UNSPECIFIED
Max-Planck-GesellschaftUNSPECIFIED
Istituto Nazionale di Fisica Nucleare (INFN)UNSPECIFIED
Istituto Nazionale di Astrofisica (INAF)UNSPECIFIED
Swiss National Fund (SNF)UNSPECIFIED
Ministerio de Economía, Industria y Competitividad (MINECO)FPA2015-69818-P
Ministerio de Economía, Industria y Competitividad (MINECO)FPA2012-36668
Ministerio de Economía, Industria y Competitividad (MINECO)FPA2015-68378-P
Ministerio de Economía, Industria y Competitividad (MINECO)FPA2015-69210-C6-2-R
Ministerio de Economía, Industria y Competitividad (MINECO)FPA2015-69210-C6-4-R
Ministerio de Economía, Industria y Competitividad (MINECO)FPA2015-69210-C6-6-R
Ministerio de Economía, Industria y Competitividad (MINECO)AYA2015-71042-P
Ministerio de Economía, Industria y Competitividad (MINECO)AYA2016-76012-C3-1-P
Ministerio de Economía, Industria y Competitividad (MINECO)ESP2015-71662-C2-2-P
MultiDarkCSD2009-00064
Japan Society for the Promotion of Science (JSPS)UNSPECIFIED
Ministry of Education, Culture, Sports, Science and Technology (MEXT)UNSPECIFIED
Centro de Excelencia Severo OchoaSEV-2012-0234
Centro de Excelencia Severo OchoaSEV-2015-0548
Ministerio de Economía, Industria y Competitividad (MINECO)MDM-2014-0369
Croatian Science FoundationIP-2016-06-9782
University of Rijeka13.12.1.3.02
Deutsche Forschungsgemeinschaft (DFG)SFB823/C4
Deutsche Forschungsgemeinschaft (DFG)SFB876/C3
National Science Centre (Poland)UMO-2016/22/M/ST9/00382
Ministério da Ciência, Tecnologia, Inovações e Comunicações (MCTIC)UNSPECIFIED
Conselho Nacional de Desenvolvimento Científico e Tecnológico (CNPq)UNSPECIFIED
Fundação de Amparo à Pesquisa do Estado do Rio de Janeiro (FAPERJ)UNSPECIFIED
Department of Energy (DOE)DE-AC02-76SF00515
Ramón y Cajal ProgrammeUNSPECIFIED
Ministerio de Economía, Industria y Competitividad (MINECO)AYA2010-14844
Ministerio de Economía, Industria y Competitividad (MINECO)AYA2013-40825-P
Ministerio de Economía, Industria y Competitividad (MINECO)AYA2016-80889-P
Regional Government of AndalucíaP09-FQM-4784
NASANNX08AW31G
NASANNX11A043G
NASANNX14AQ89G
NSFAST-0808050
NSFAST-1109911
Subject Keywords:galaxies: active – galaxies: jets – gamma rays: galaxies – quasars: individual: PKS 1510–089
Record Number:CaltechAUTHORS:20181210-112439274
Persistent URL:http://resolver.caltech.edu/CaltechAUTHORS:20181210-112439274
Official Citation:Detection of persistent VHE gamma-ray emission from PKS 1510–089 by the MAGIC telescopes during low states between 2012 and 2017. MAGIC Collaboration:, V. A. Acciari, S. Ansoldi, L. A. Antonelli, A. Arbet Engels, C. Arcaro, D. Baack, A. Babić, B. Banerjee, P. Bangale, U. Barres de Almeida, J. A. Barrio, W. Bednarek, E. Bernardini, A. Berti, J. Besenrieder, W. Bhattacharyya, C. Bigongiari, A. Biland, O. Blanch, G. Bonnoli, R. Carosi, G. Ceribella, S. Cikota, S. M. Colak, P. Colin, E. Colombo, J. L. Contreras, J. Cortina, S. Covino, V. D’Elia, P. Da Vela, F. Dazzi, A. De Angelis, B. De Lotto, M. Delfino, J. Delgado, F. Di Pierro, E. Do Souto Espiñera, A. Domínguez, D. Dominis Prester, D. Dorner, M. Doro, S. Einecke, D. Elsaesser, V. Fallah Ramazani, A. Fattorini, A. Fernández-Barral, G. Ferrara, D. Fidalgo, L. Foffano, M. V. Fonseca, L. Font, C. Fruck, D. Galindo, S. Gallozzi, R. J. García López, M. Garczarczyk, M. Gaug, P. Giammaria, N. Godinović, D. Guberman, D. Hadasch, A. Hahn, T. Hassan, J. Herrera, J. Hoang, D. Hrupec, S. Inoue, K. Ishio, Y. Iwamura, H. Kubo, J. Kushida, D. Kuveždić, A. Lamastra, D. Lelas, F. Leone, E. Lindfors, S. Lombardi, F. Longo, M. López, A. López-Oramas, C. Maggio, P. Majumdar, M. Makariev, G. Maneva, M. Manganaro, K. Mannheim, L. Maraschi, M. Mariotti, M. Martínez, S. Masuda, D. Mazin, M. Minev, J. M. Miranda, R. Mirzoyan, E. Molina, A. Moralejo, V. Moreno, E. Moretti, P. Munar-Adrover, V. Neustroev, A. Niedzwiecki, M. Nievas Rosillo, C. Nigro, K. Nilsson, D. Ninci, K. Nishijima, K. Noda, L. Nogués, S. Paiano, J. Palacio, D. Paneque, R. Paoletti, J. M. Paredes, G. Pedaletti, P. Peñil, M. Peresano, M. Persic, P. G. Prada Moroni, E. Prandini, I. Puljak, J. R. Garcia, W. Rhode, M. Ribó, J. Rico, C. Righi, A. Rugliancich, L. Saha, T. Saito, K. Satalecka, T. Schweizer, J. Sitarek, I. Šnidarić, D. Sobczynska, A. Somero, A. Stamerra, M. Strzys, T. Surić, F. Tavecchio, P. Temnikov, T. Terzić, M. Teshima, N. Torres-Albà, S. Tsujimoto, J. van Scherpenberg, G. Vanzo, M. Vazquez Acosta, I. Vovk, J. E. Ward, M. Will, D. Zarić, Fermi-LAT Collaboration:, J. Becerra González, C. M. Raiteri, A. Sandrinelli, T. Hovatta, S. Kiehlmann, W. Max-Moerbeck, M. Tornikoski, A. Lähteenmäki, J. Tammi, V. Ramakrishnan, C. Thum, I. Agudo, S. N. Molina, J. L. Gómez, A. Fuentes, C. Casadio, E. Traianou, I. Myserlis and J.-Y. Kim A&A, 619 (2018) A159 DOI: https://doi.org/10.1051/0004-6361/201833618
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ID Code:91640
Collection:CaltechAUTHORS
Deposited By: Tony Diaz
Deposited On:10 Dec 2018 19:40
Last Modified:10 Dec 2018 19:40

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