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Parsec-Scale Structure And Kinematics Of Faint Tev Hbls, B. Glenn Piner, Philip G. Edwards
Parsec-Scale Structure And Kinematics Of Faint Tev Hbls, B. Glenn Piner, Philip G. Edwards
Physics
We present new multi-epoch Very Long Baseline Array (VLBA) observations of a set of TeV blazars drawn from our VLBA program to monitor all TeV-detected high-frequency peaked BL Lac objects (HBLs) at parsec scales. Most of these sources are faint in the radio, so they have not been well observed with VLBI by other surveys. Our previous measurements of apparent jet speeds in TeV HBLs showed apparent jet speeds that were subluminal or barely superluminal, suggesting jets with velocity structures at the parsec-scale. Here we present apparent jet speed measurements for eight new TeV HBLs, which for the first time …
The Giant Radio Array For Neutrino Detection, Jordan C. Hanson, Olivier Martineau-Huynh, Kumiko Kotera, Mauricio Bustamente, Didier Charrier, Sijbrand De Jong, Krijn D. De Vries, Ke Fang, Zhaoyang Feng, Chad Finley, Quanbu Gou, Junhua Gu, Hongbo Hu, Kohta Murase, Valentin Niess, Foteini Oikonomou, Nicolas Renault-Tinacci, Julia Schmid, Charles Timmermans, Zhen Wang, Xiangping Wu, Jianli Zhang, Yi Zhang
The Giant Radio Array For Neutrino Detection, Jordan C. Hanson, Olivier Martineau-Huynh, Kumiko Kotera, Mauricio Bustamente, Didier Charrier, Sijbrand De Jong, Krijn D. De Vries, Ke Fang, Zhaoyang Feng, Chad Finley, Quanbu Gou, Junhua Gu, Hongbo Hu, Kohta Murase, Valentin Niess, Foteini Oikonomou, Nicolas Renault-Tinacci, Julia Schmid, Charles Timmermans, Zhen Wang, Xiangping Wu, Jianli Zhang, Yi Zhang
Physics
High-energy neutrino astronomy will probe the working of the most violent phenomena in the Universe. The Giant Radio Array for Neutrino Detection (GRAND) project consists of an array of ∼ 105 radio antennas deployed over ∼ 200 000 km2 in a mountainous site. It aims at detecting high-energy neutrinos via the measurement of air showers induced by the decay in the atmosphere of τ leptons produced by the interaction of cosmic neutrinos under the Earth surface. Our objective with GRAND is to reach a neutrino sensitivity of 5 × 10−11E−2 GeV−1 cm−2 s …