The High-Altitude Water Cherenkov (HAWC) observatory in México: The primary detector

Abeysekara, Anushka Udara; Albert, A.; Alfaro, R.; Álvarez, C.; Álvarez, José David Ruiz; Araya, Miguel; Arteaga‐Velázquez, J. C.; Arunbabu, K. P.; Rojas, D. Avila; Solares, H. A. Ayala; Babu, Rishi; Barber, Ahron S.; Becerril, A.; Belmont‐Moreno, E.; BenZvi, S.; Blanco, O.; Braun, J.; Brisbois, C.; Caballero-Mora, K. S.; Martínez, J.I. Cabrera; Capistrán, T.; Carramiñana, A.; Casanova, S.; Castillo, M.; Chaparro-Amaro, Oscar; Cotti, U.; Cotzomi, J.; León, S. Coutińo de; Fuente, Eduardo de la; León, C. De; Young, T.; Hernández, R. Díaz; Dingus, B. L.; DuVernois, Michael; Durocher, Mora; Díaz–Vélez, Juan Carlos; Ellsworth, R. W.; Engel, Kristi; Espinoza, C.; Fan, Kwok Lung; Fang, Ke; Fick, B.; Fleischhack, Henrike; Flores, Jorge L.; Fraija, N.; García-González, J. A.; García–Torales, Guillermo; Garfias, F.; Giacinti, Gwenael; Goksu, Hazal; González, M. M.; González-Muñoz, A.; Goodman, J. A.; Harding, J. Patrick; Hernández, Emma González; Hernández, S.; Hinton, J. A.; Hona, B.; Huang, Dezhi; Hueyotl-Zahuantitla, Filiberto; Hui, C. M.; Humensky, T. B.; Hüntemeyer, P.; Iriarte, A.; Imran, Asif; Jardin-Blicq, A.; Joshi, Vikas; Kaufmann, S.; Kieda, D. B.; Kunde, G. J.; Lara, A.; Lauer, R.; Lee, W.H.; Lennarz, D.; Vargas, H. León; Linnemann, J. T.; Longinotti, A. L.; Luis-Raya, G.; Lundeen, J.; Malone, K.; Marandon, V.; Marinelli, A.; Martı́nez, O.; Martínez-Castellanos, I.; Martínez-Castro, J.; Martínez-Huerta, H.; Matthews, John; Miranda-Romagnoli, P.; Montaruli, T.; Morales-Soto, J. A.; Moreno, E.; Mostafá, M.; Nayerhoda, A.; Nellen, Lukas; Newbold, M.; Nisa, Mehr; Noriega‐Papaqui, R.; Oceguera-Becerra, T.; Olivera-Nieto, Laura; Omodei, N.; Peisker, A.; Araujo, Yunior Pérez; Pérez-Pérez, E. G.; Ponce, E.; Pretz, J.; Rho, Chang Dong; Rosa-González, D.; Ruiz-Velasco, E.; Salazar, H.; Salazar-Gallegos, Daniel; Greus, F. Salesa; Sandoval, A.; Schneider, M.; Schoorlemmer, H.; Serna-Franco, José; Sinnis, G.; Smith, A. J.; Son, Y.; Woodle, K. Sparks; Springer, R. W.; Taboada, I.; Tepe, A.; Tibolla, O.; Tollefson, K.; Torres, I.; Torres-Escobedo, R.; Turner, Rhiannon; Ureña-Mena, Fernando; Ukwatta, T. N.; Varela, E.; Vargas-Magaña, Mariana; Villaseñor, L.; Wang, X.; Watson, I. J.; Werner, F.; Westerhoff, S.; Willox, Elijah; Wisher, I. G.; Wood, J.; Yodh, G.; Zaborov, D.; Zepeda, A.; Zhou, Huan

doi:10.1016/j.nima.2023.168253

Cited by 19 publications

(9 citation statements)

References 49 publications

(54 reference statements)

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“…The main array of HAWC consists of 300 water Cherenkov detectors of 7.3 m diameter and 4.5 m height filled with highly purified water and instrumented with four photomultipliers (PMTs). The main array covers an area of about 22,000 m 2 (for a detailed description of the HAWC array see Abeysekara et al 2023).…”

Section: Hawc Array and Datamentioning

confidence: 99%

Exploring the Coronal Magnetic Field with Galactic Cosmic Rays: The Sun Shadow Observed by HAWC

Alfaro,

Alvarez,

Arteaga-Velázquez

et al. 2024

ApJ

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Galactic cosmic rays (GCRs) are charged particles that reach the heliosphere almost isotropically in a wide energy range. In the inner heliosphere, the GCR flux is modulated by solar activity so that only energetic GCRs reach the lower layers of the solar atmosphere. In this work, we propose that high-energy GCRs can be used to explore the solar magnetic fields at low coronal altitudes. We used GCR data collected by the High-Altitude Water Cherenkov observatory to construct maps of GCR flux coming from the Sun’s sky direction and studied the observed GCR deficit, known as Sun shadow (SS), over a 6 yr period (2016–2021) with a time cadence of 27.3 days. We confirm that the SS is correlated with sunspot number, but we focus on the relationship between the photospheric solar magnetic field measured at different heliolatitudes and the relative GCR deficit at different energies. We found a linear relationship between the relative deficit of GCRs represented by the depth of the SS and the solar magnetic field. This relationship is evident in the observed energy range of 2.5–226 TeV, but is strongest in the range of 12.4 33.4 TeV, which implies that this is the best energy range to study the evolution of magnetic fields in the low solar atmosphere.

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Section: Hawc Array and Datamentioning

confidence: 99%

Exploring the Coronal Magnetic Field with Galactic Cosmic Rays: The Sun Shadow Observed by HAWC

Alfaro,

Alvarez,

Arteaga-Velázquez

et al. 2024

ApJ

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“…A WCD has a height of 5.4 m and a diameter of 7.3 m. Four photomultiplier tubes (PMTs) are located at the bottom of each WCD to collect the Cherenkov light emitted by air shower particles. For more detailed information on the design and operation of HAWC, refer to Abeysekara et al (2017aAbeysekara et al ( , 2023.…”

Section: Hawcmentioning

confidence: 99%

“…The HAWC observatory is a ground-based particle sampling array located on Sierra Negra, Mexico, at an altitude of 4100 m. It is designed to observe very-high-energy (VHE) γ-ray photons by detecting Cherenkov radiation produced from electromagnetic air showers as they propagate through the water Cherenkov detectors (WCDs). The main array of HAWC, composed of 300 WCDs, covers a geometrical area of 22,000 m 2 (Abeysekara et al 2023). Each WCD consists of a bladder containing 180,000 L of purified water that is protected by a metal casing with a roof on top.…”

Section: Hawcmentioning

confidence: 99%

HAWC Study of the Very-high-energy γ-Ray Spectrum of HAWC J1844−034

Albert,

Alvarez,

Avila Rojas

et al. 2023

ApJ

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Recently, the region surrounding eHWC J1842−035 has been studied extensively by γ-ray observatories due to its extended emission reaching up to a few hundred TeV and potential as a hadronic accelerator. In this work, we use 1910 days of cumulative data from the High Altitude Water Cherenkov (HAWC) observatory to carry out a dedicated systematic source search of the eHWC J1842−035 region. During the search, we found three sources in the region, namely, HAWC J1844−034, HAWC J1843−032, and HAWC J1846−025. We have identified HAWC J1844−034 as the extended source that emits photons with energies up to 175 TeV. We compute the spectrum for HAWC J1844−034, and by comparing with the observational results from other experiments, we have identified HESS J1843−033, LHAASO J1843−0338, and TASG J1844−038 as very-high-energy γ-ray sources with a matching origin. Also, we present and use the multiwavelength data to fit the hadronic and leptonic particle spectra. We have identified four pulsar candidates in the nearby region in which PSR J1844−0346 is found to be the most likely candidate due to its proximity to HAWC J1844−034 and the computed energy budget. We have also found SNR G28.6−0.1 as a potential counterpart source of HAWC J1844−034 for which both leptonic and hadronic scenarios are feasible.

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“…The detector observes the Cherenkov lights in the water produced by the charged secondary particles. Thanks to its large field of view, it monitors two-thirds of the sky daily with a >95% duty cycle (Abeysekara et al 2017b(Abeysekara et al , 2023.…”

Section: Introductionmentioning

confidence: 99%

Galactic Gamma-Ray Diffuse Emission at TeV Energies with HAWC Data

Alfaro,

Alvarez,

Arteaga-Velázquez

et al. 2024

ApJ

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Galactic gamma-ray diffuse emission (GDE) is emitted by cosmic rays (CRs), ultra-relativistic protons, and electrons, interacting with gas and electromagnetic radiation fields in the interstellar medium. Here we present the analysis of teraelectronvolt diffuse emission from a region of the Galactic plane over the range in longitude of l ∈ [43°, 73°], using data collected with the High Altitude Water Cherenkov (HAWC) detector. Spectral, longitudinal, and latitudinal distributions of the teraelectronvolt diffuse emission are shown. The radiation spectrum is compatible with the spectrum of the emission arising from a CR population with an index similar to that of the observed CRs. When comparing with the DRAGON base model, the HAWC GDE flux is higher by about a factor of 2. Unresolved sources such as pulsar wind nebulae and teraelectronvolt halos could explain the excess emission. Finally, deviations of the Galactic CR flux from the locally measured CR flux may additionally explain the difference between the predicted and measured diffuse fluxes.

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The High-Altitude Water Cherenkov (HAWC) observatory in México: The primary detector

Cited by 19 publications

References 49 publications

Exploring the Coronal Magnetic Field with Galactic Cosmic Rays: The Sun Shadow Observed by HAWC

Exploring the Coronal Magnetic Field with Galactic Cosmic Rays: The Sun Shadow Observed by HAWC

HAWC Study of the Very-high-energy γ-Ray Spectrum of HAWC J1844−034

Galactic Gamma-Ray Diffuse Emission at TeV Energies with HAWC Data

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