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  1. ; ; ; ; ; ; ; ; ; ( , npj Quantum Materials)
    Abstract TmVO 4 exhibits ferroquadrupolar order of the Tm 4f electronic orbitals at low temperatures, and is a model system for Ising nematicity. A magnetic field oriented along the c -axis constitutes a transverse effective field for the quadrupolar order parameter, continuously tuning the system to a quantum phase transition as the field is increased from zero. In contrast, in-plane magnetic fields couple to the order parameter only at second order, such that orienting along the primary axes of the quadrupole order results in an effective longitudinal field, whereas orienting at 45 degrees results in a second effective transverse field.more »Not only do in-plane fields engender a marked in-plane anisotropy of the critical magnetic and quadrupole fluctuations above the ferroquadrupolar ordering temperature, but in-plane transverse fields initially enhance the ferroquadrupolar order, before eventually suppressing it, an effect that we attribute to admixing of the higher crystalline electric field levels.« less
    Free, publicly-accessible full text available December 1, 2023
  2. ; ; ; ; ; ; ; ( , Physical Review B)
    Free, publicly-accessible full text available November 1, 2022
  3. ; ; ; ; ; ; ; ; ; ; et al ( , Nuclear Instruments and Methods in Physics Research Section A: Accelerators, Spectrometers, Detectors and Associated Equipment)
    Free, publicly-accessible full text available September 1, 2023
  4. ; ; ; ; ; ; ; ; ; ; et al ( , Astroparticle Physics)
    Free, publicly-accessible full text available April 1, 2023
  5. ; ; ; ; ; ; ; ; ; ; et al ( , The Astrophysical Journal)
    Abstract The High Altitude Water Cherenkov (HAWC) Gamma-Ray Observatory surveys the very high-energy sky in the 300 GeV to >100 TeV energy range. HAWC has detected two blazars above 11 σ , Markarian 421 (Mrk 421) and Markarian 501 (Mrk 501). The observations are comprised of data taken in the period between 2015 June and 2018 July, resulting in ∼1038 days of exposure. In this work, we report the time-averaged spectral analyses for both sources, above 0.5 TeV. Taking into account the flux attenuation due to the extragalactic background light, the intrinsic spectrum of Mrk 421 is described by amore »power law with an exponential energy cutoff with index α = 2.26 ± 0.12 stat − 0.2 + 0.17 sys and energy cutoff E c = 5.1 ± 1.6 stat − 2.5 + 1.4 sys TeV, while the intrinsic spectrum of Mrk 501 is better described by a simple power law with index α = 2.61 ± 0.11 stat − 0.07 + 0.01 sys . The maximum energies at which the Mrk 421 and Mrk 501 signals are detected are 9 and 12 TeV, respectively. This makes these some of the highest energy detections to date for spectra averaged over years-long timescales. Since the observation of gamma radiation from blazars provides information about the physical processes that take place in their relativistic jets, it is important to study the broadband spectral energy distributions (SEDs) of these objects. For this purpose, contemporaneous data in the gamma-ray band to the X-ray range, and literature data in the radio to UV range, were used to build time-averaged SEDs that were modeled within a synchrotron-self Compton leptonic scenario.« less
    Free, publicly-accessible full text available April 1, 2023
  6. ; ; ; ; ; ; ; ; ; ; et al ( , The Astrophysical Journal)
    Abstract We report TeV gamma-ray observations of the ultra-high-energy source MGRO J1908+06 using data from the High Altitude Water Cherenkov Observatory. This source is one of the highest-energy known gamma-ray sources, with emission extending past 200 TeV. Modeling suggests that the bulk of the TeV gamma-ray emission is leptonic in nature, driven by the energetic radio-faint pulsar PSR J1907+0602. Depending on what assumptions are included in the model, a hadronic component may also be allowed. Using the results of the modeling, we discuss implications for detection prospects by multi-messenger campaigns.
    Free, publicly-accessible full text available March 31, 2023
  7. ; ; ; ; ; ; ; ; ; ; et al ( , Solar Physics)
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  8. ; ; ; ; ; ; ; ; ; ; et al ( , The Astrophysical Journal)
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  9. ; ; ; ; ; ; ; ; ; ; et al ( , The Astrophysical Journal)
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  10. ; ; ; ; ; ; ; ; ; ; et al ( , The Astrophysical Journal)
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