Gamma-ray observations of low-luminosity active galactic nuclei

Autor(es)

de Menezes, Raniere ^{[1, 2]} ; Nemmen, Rodrigo ^[1] ; Finke, Justin D. ^[3] ; Almeida, Ivan ^[1] ; Rani, Bindu ^{[4, 5, 6, 7]}

Afiliação do(s) autor(es)

^[1] Univ Sao Paulo, Geofis & Ciencias Atmosfer, Inst Astron, Dept Astron, BR-05508090 Sao Paulo, SP - Brazil

^[2] Univ Torino, Dipartimento Fis, Via Pietro Giuria 1, I-10125 Troino - Italy

^[3] US Naval Res Lab, Code 7653, 4555 Overlook Ave SW, Washington, DC 20375 - USA

^[4] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 - USA

^[5] Korea Astron & Space Sci Inst, Daejeon 34055 - South Korea

^[6] Southeastent Univ Res Assoc, Washington, DC 20005 - USA

^[7] NASA, GSFC, Ctr Res & Explorat Space Sci & Technol, Greenbelt, MD 20771 - USA

• Tipo de documento: Artigo Científico
• Fonte: Monthly Notices of the Royal Astronomical Society; v. 492, n. 3, p. 4120-4130, MAR 2020.
• Citações Web of Science: 0

Resumo

The majority of the activity around nearby (z approximate to 0) supermassive black holes is found in low-luminosity active galactic nuclei (LLAGN), the most of them being classified as low ionization nuclear emission regions. Although these sources are well studied from radio up to X-rays, they are poorly understood in gamma-rays. In this work, we take advantage of the all sky-surveying capabilities of the Large Area Telescope on board Fermi Gamma-ray Space Telescope to study the whole Palomar sample of LLAGN in gamma-rays. Precisely, the four radio brightest LLAGN in the sample are identified as significant gamma-ray emitters, all of which are recognized as powerful Fanaroff-Riley 1 galaxies. These results suggest that the presence of powerful radio jets is of substantial importance for observing a significant gamma-ray counterpart even if these jets are misaligned with respect to the line of sight. We also find that most of the X-ray-brightest LLAGN do not have a significant gamma-ray and strong radio emission, suggesting that the X-rays come mainly from the accretion flow in these cases. A detailed analysis of the spectral energy distributions (SEDs) of NGC 315 and NGC 4261, both detected in gamma-rays, is provided where we make a detailed comparison between the predicted hadronic gamma-ray emission from a radiatively inefficient accretion flow (RIAF) and the gamma-ray emission from a leptonic jet-dominated synchrotron self-Compton (SSC) model. Both SEDs are better described by the SSC model, while the RIAF fails to explain the gamma-ray observations. (AU)

• Processo FAPESP: 18/24801-6 - Espectroscopia de fendas múltiplas de fontes de raios gama não-identificadas
• Beneficiário: Raniere Maciel de Menezes
• Linha de fomento: Bolsas no Exterior - Estágio de Pesquisa - Doutorado
• Processo FAPESP: 19/10054-7 - Ventos e feedback de buracos negros
• Beneficiário: Ivan Carlos de Almeida
• Linha de fomento: Bolsas no Brasil - Doutorado
• Processo FAPESP: 17/01461-2 - O universo extremo: buracos negros e o telescópio Fermi
• Beneficiário: Rodrigo Nemmen da Silva
• Linha de fomento: Auxílio à Pesquisa - Apoio a Jovens Pesquisadores
• Processo FAPESP: 16/24857-6 - Ventos e feedback de buracos negros supermassivos
• Beneficiário: Ivan Carlos de Almeida
• Linha de fomento: Bolsas no Brasil - Mestrado