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تسجيل مستخدم جديدHighlights of the VERITAS Blazar Program
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Wystan Benbow
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The VERITAS array of 12-m atmospheric-Cherenkov telescopes in southern Arizona began full-scale operations in 2007, and is one of the worlds most-sensitive detectors of astrophysical VHE (E>100 GeV) gamma rays. Approximately 50 blazars are known to emit VHE photons, and observations of blazars are a major focus of the VERITAS Collaboration. Nearly 2000 hours have been devoted to this program and ~130 blazars have already been observed with the array, in most cases with the deepest-ever VHE exposure. These observations have resulted in 21 detections, including 10 VHE discoveries. Recent highlights of the VERITAS blazar observation program, and the collaborations long-term blazar observation strategy, are presented.
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The VERITAS array of 12-m atmospheric-Cherenkov telescopes in southern Arizona began full-scale operations in 2007, and it is one of the worlds most sensitive detectors of astrophysical VHE (E > 100 GeV) gamma rays. Forty-one blazars are known to emi
t VHE photons, and observations of blazars are one of the VERITAS Collaborations Key Science Projects (KSPs). More than 400 hours per year are devoted to this program, and ~100 blazars have already been observed with the array, in most cases with the deepest-ever VHE exposure. These observations have resulted in 20 detections, including 10 new VHE blazars. Highlights of the VERITAS blazar observation program, and the collaborations long-term blazar observation strategy, are presented.
VERITAS is one of the worlds most sensitive detectors of astrophysical VHE (E $>$ 100 GeV) gamma rays. This array of four 12-m imaging atmospheric-Cherenkov telescopes has operated for 12 years, and $>$6,000 hours of observations have been targeted o
n active galactic nuclei (AGN). Approximately 300 AGN have been observed with VERITAS, and 39 are detected. Most of these detections are accompanied by contemporaneous, broadband observations, which enable detailed studies of the underlying jet-powered processes. Recent highlights from the VERITAS AGN observation program and scientific results are presented.
The VERITAS array of four 12-m imaging atmospheric-Cherenkov telescopes began full-scale operations in 2007, and is one of the worlds most sensitive detectors of astrophysical VHE (E>100 GeV) $gamma$-rays. Observations of active galactic nuclei (AGN)
are a major focus of the VERITAS Collaboration, and more than 60 AGN, primarily blazars, are known to emit VHE photons. Approximately 3400 hours have been devoted to the VERITAS AGN observation program and roughly 160 AGN are already observed with the array, in most cases with the deepest VHE exposure to date. These observations have resulted in 34 detections, most of which are accompanied by contemporaneous, multi-wavelength observations, enabling a more detailed study of the underlying jet-powered processes. Recent highlights of the VERITAS AGN observation program, and the collaborations long-term AGN observation strategy, are presented.
The VERITAS array of four 12-m imaging atmospheric-Cherenkov telescopes began full-scale operations in 2007, and is one of the worlds most sensitive detectors of astrophysical very high energy (VHE; E>100 GeV) gamma rays. Observations of active galac
tic nuclei (AGN) are a major focus of the VERITAS Collaboration, and more than 60 AGN, primarily blazars, are known to emit VHE photons. Approximately 4000 hours have been devoted to the VERITAS AGN observation program, resulting in 34 detections. Most of these detections are accompanied by contemporaneous, broadband observations, enabling a more detailed study of the underlying jet-powered processes. Recent highlights of the VERITAS AGN observation program are presented.
The VERITAS telescope array has been operating smoothly since 2007, and has detected gamma-ray emission above 100 GeV from 40 astrophysical sources. These include blazars, pulsar wind nebulae, supernova remnants, gamma-ray binary systems, a starburst
galaxy, a radio galaxy, the Crab pulsar, and gamma-ray sources whose origin remains unidentified. In 2009, the array was reconfigured, greatly improving the sensitivity. We summarize the current status of the observatory, describe some of the scientific highlights since 2009, and outline plans for the future.
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