Exploring <i>γ</i>-Ray Flares from High-Redshift Blazar B3 1343+451 at GeV Energies

Exploring <i>γ</i>-Ray Flares from High-Redshift Blazar B3 1343+451 at GeV Energies

We study the temporal and spectral variability properties of the high-redshift blazar B3 1343+451 utilizing Fermi-LAT data from 2008 to 2022 in the energy range of 0.1–300 GeV. We identify six major flares with many substructures and analyze their temporal and spectral properties in detail. The fast...

Full description

Saved in:
Bibliographic Details
Main Authors: Xiongfei Geng, Yang Liu, Gang Cao, Jing Fan, Xiongbang Yang, Nan Ding, Minghu Gao, Yehui Yang, Zhijie Zhang
Format: Article
Language:English
Published: MDPI AG 2024-11-01
Series:Universe
Subjects:
blazars
γ-ray
active galactic nuclei
B3 1343+451
Online Access:https://www.mdpi.com/2218-1997/10/11/423
Tags: Add Tag
No Tags, Be the first to tag this record!
Description
Summary:We study the temporal and spectral variability properties of the high-redshift blazar B3 1343+451 utilizing Fermi-LAT data from 2008 to 2022 in the energy range of 0.1–300 GeV. We identify six major flares with many substructures and analyze their temporal and spectral properties in detail. The fastest rise and decay timescales are found to be 4.8 ± 0.48 h and 5.28 ± 0.72 h, respectively. The size of the emission region is constrained to be <i>R</i> ∼ 5.18 × <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><msup><mn>10</mn><mn>15</mn></msup></semantics></math></inline-formula>–1.56 × <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><msup><mn>10</mn><mn>16</mn></msup></semantics></math></inline-formula> cm with the typical Doppler factors of <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><mi>δ</mi></semantics></math></inline-formula> ∼ 10–30. Most of the peaks from the flares exhibit a symmetric temporal profile within the error bars, implying that the rise and decay timescales are dominated by the disturbances caused by dense plasma blobs passing through the standing shock front in the jet region. We also find that four flares are better fitted with a log-parabolic distribution, while two flares are better fitted with a power-law distribution. Our results indicate that the emission regions vary from one flare to another, which is consistent with earlier results.
ISSN:2218-1997

Similar Items