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- gamma rays: galaxies (16)
- gamma rays: general (15)
- BL Lacertae objects: general (9)
- galaxies: active (9)
- radiation mechanisms: non-thermal (7)
- acceleration of particles (6)
- astroparticle physics (6)
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- BL Lacertae objects: individual: Mrk 421 (2)
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- ISM: supernova remnants (2)
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- gamma-rays: general (2)
- magnetic fields (2)
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- AGN (1)
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- BL Lacertae objects: individual (1ES 0229+200, VER J0232+202) (1)
- BL Lacertae objects: individual (1ES 1959+650) (1)
- BL Lacertae objects: individual (1ES1218+30.4) (1)
- BL Lacertae objects: individual (BL Lacertae = VER J2202+422) (1)
- BL Lacertae objects: individual (Mrk 501) (1)
- BL Lacertae objects: individual (RBS 0413-VER J0319+187) (1)
- BL Lacertae objects: individual (RX J0648.7+1516, 1FGL J0648.8+1516, VER J0648+152) (1)
- BL Lacertae objects: individual (TXS 0506+056, VER J0509+057) (1)
- BL Lacertae objects: individual (VER J0521+211) (1)
- BL Lacertae objects: individual: 1ES 2344+514=VERJ2347+517 (1)
- BL Lacertae objects: individual: Markarian 501 (1)
- BL Lacertae objects: individual: Mrk 501 (1)
- BL Lacertae objects: individual: Mrk501 (1)
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- ISM: individual objects (Crab Nebula) (1)
- ISM: individual objects (G120.1+01.4, Tycho=VER J0025+641) (1)
- Markarian 421 (1)
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- TeV gamma-ray astronomy (1)
- X-rays: individual (Cygnus X-3) (1)
- X-rays: individual (RX J0007.0+7303) (1)
- accretion, accretion disks (1)
- astrobiology (1)
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- black hole physics (1)
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- galaxies: clusters: general (1)
- galaxies: clusters: individual (Coma (ACO 1656)) (1)
- galaxies: individual (BL Lacertae, VER J2202+422) (1)
- galaxies: individual (M 87) (1)
- galaxies: individual (M 87, VER J1230+123) (1)
- galaxies: individual (RGB J2243+203) (1)
- galaxies: individual: 1ES 1741+196=VER J1744+195 (1)
- gamma rays : stars (1)
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- gamma rays: general(HESS J0632+057, VER J0633+057) (1)
- gamma-ray burst: general (1)
- gamma-ray burst: individual (GRB 130427A) (1)
- gamma-ray burst: individual (MGRO J1908+06, VER J1907+062) (1)
- gamma-rays: galaxies (1)
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- line: identification (1)
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- novae, cataclysmic variables (1)
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- planetary nebulae: individual: PN G029.0+00.4 (1)
- pulsars : individual (PSR J2021+3651) (1)
- pulsars: individual (PSR J0007+7303) (1)
- pulsars: individual (PSR J0633+1746, Geminga) (1)
- pulsars: individual (PSR J1023+0038) (1)
- pulsars: individual (PSR J1907+0602) (1)
- pulsars: individual (PSR J2032+4127) (1)
- pulsars: individual (PSR J2032+4127, VER J2032+414, MAGIC J2032+4127) (1)
- pulsars: individual: B0531+21 (1)
- quasars: general (1)
- rays: stars (1)
- relativistic processes (1)
- stars: AGB and post-AGB (1)
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- stars: abundances (1)
- stars: emission-line, Be (1)
- stars: evolution (1)
- stars: individual ( KIC 8462852) (1)
- stars: individual (1A 0535+262) (1)
- stars: individual (LS I+61 degrees 303, VER J0240+612) (1)
- stars: individual (MT91 213) (1)
- stars: individual: Hen 3-1383 (1)
- stars: mass-loss (1)
- stars: massive (1)
- stars: neutron (1)
- supernovae : individual (CTB 87) (1)
- supernovae: individual (G0.9+0.1) (1)
- supernovae: individual (G119.5+10.2) (1)
- techniques: photometric (1)
- white dwarfs (1)
Institute
Cosmic-ray electrons and positrons (CREs) at GeV-TeV energies are a unique probe of our local Galactic neighborhood. CREs lose energy rapidly via synchrotron radiation and inverse-Compton scattering processes while propagating within the Galaxy, and these losses limit their propagation distance. For electrons with TeV energies, the limit is on the order of a kiloparsec. Within that distance, there are only a few known astrophysical objects capable of accelerating electrons to such high energies. It is also possible that the CREs are the products of the annihilation or decay of heavy dark matter (DM) particles. VERITAS, an array of imaging air Cherenkov telescopes in southern Arizona, is primarily utilized for gamma-ray astronomy but also simultaneously collects CREs during all observations. We describe our methods of identifying CREs in VERITAS data and present an energy spectrum, extending from 300 GeV to 5 TeV, obtained from approximately 300 hours of observations. A single power-law fit is ruled out in VERITAS data. We find that the spectrum of CREs is consistent with a broken power law, with a break energy at 710 +/- 40(stat) +/- 140(syst) GeV.
A Search for Pulsed Very High-energy Gamma-Rays from 13 Young Pulsars in Archival VERITAS Data
(2019)
We conduct a search for periodic emission in the very high-energy (VHE) gamma-ray band (E > 100 GeV) from a total of 13 pulsars in an archival VERITAS data set with a total exposure of over 450 hr. The set of pulsars includes many of the brightest young gamma-ray pulsars visible in the Northern Hemisphere. The data analysis resulted in nondetections of pulsed VHE gamma-rays from each pulsar. Upper limits on a potential VHE gamma-ray flux are derived at the 95% confidence level above three energy thresholds using two methods. These are the first such searches for pulsed VHE emission from each of the pulsars, and the obtained limits constrain a possible flux component manifesting at VHEs as is seen for the Crab pulsar.