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32 results on '"Arteaga-Velázquez JC"'

1. Multimessenger Gamma-Ray and Neutrino Coincidence Alerts Using HAWC and IceCube Subthreshold Data

Author

Solares, HA Ayala, Coutu, S, DeLaunay, JJ, Fox, DB, Grégoire, T, Keivani, A, Krauß, F, Mostafá, M, Murase, K, Turley, CF, Albert, A, Alfaro, R, Alvarez, C, Camacho, JR Angeles, Arteaga-Velázquez, JC, Arunbabu, KP, Rojas, D Avila, Belmont-Moreno, E, Brisbois, C, Caballero-Mora, KS, Carramiñana, A, Casanova, S, Cotti, U, De la Fuente, E, Hernandez, R Diaz, Dingus, BL, DuVernois, MA, Durocher, M, Díaz-Vélez, JC, Espinoza, C, Fan, KL, Fleischhack, H, Fraija, N, Galván-Gámez, A, Garcia, D, García-González, JA, Garfias, F, González, MM, Goodman, JA, Harding, JP, Hona, B, Huang, D, Hueyotl-Zahuantitla, F, Hüntemeyer, P, Iriarte, A, Jardin-Blicq, A, Joshi, V, Vargas, H León, Linnemann, JT, Longinotti, AL, Luis-Raya, G, Lundeen, J, Malone, K, Martinez, O, Martinez-Castellanos, I, Martínez-Castro, J, Matthews, JA, Miranda-Romagnoli, P, Moreno, E, Nellen, L, Newbold, M, Nisa, MU, Noriega-Papaqui, R, Peisker, A, Pérez-Pérez, EG, Rho, CD, Rosa-González, D, Salazar, H, Greus, F Salesa, Sandoval, A, Smith, AJ, Springer, RW, Tollefson, K, Torres, I, Torres-Escobedo, R, Ureña-Mena, F, Villaseñor, L, Weisgarber, T, Willox, E, Zepeda, A, Zhou, H, de León, C, Aartsen, MG, Abbasi, R, Ackermann, M, Adams, J, Aguilar, JA, Ahlers, M, Ahrens, M, Alispach, C, Amin, NM, Andeen, K, Anderson, T, Ansseau, I, Anton, G, Argüelles, C, Auffenberg, J, Axani, S, Bagherpour, H, and Bai, X

Subjects
Nuclear and Plasma Physics, Particle and High Energy Physics, Physical Sciences, astro-ph.HE, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry (incl. Structural), Astronomy & Astrophysics, Astronomical sciences, Particle and high energy physics, Space sciences
Abstract

The High Altitude Water Cerenkov (HAWC) and IceCube observatories, through the Astrophysical Multimessenger Observatory Network (AMON) framework, have developed a multimessenger joint search for extragalactic astrophysical sources. This analysis looks for sources that emit both cosmic neutrinos and gamma rays that are produced in photohadronic or hadronic interactions. The AMON system is running continuously, receiving subthreshold data (i.e., data that are not suited on their own to do astrophysical searches) from HAWC and IceCube, and combining them in real time. Here we present the analysis algorithm, as well as results from archival data collected between 2015 June and 2018 August, with a total live time of 3.0 yr. During this period we found two coincident events that have a false-alarm rate (FAR) of

Published
2021

2. All-sky Measurement of the Anisotropy of Cosmic Rays at 10 TeV and Mapping of the Local Interstellar Magnetic Field

Author

Abeysekara, AU, Alfaro, R, Alvarez, C, Arceo, R, Arteaga-Velázquez, JC, Rojas, D Avila, Belmont-Moreno, E, BenZvi, SY, Brisbois, C, Capistrán, T, Carramiana, A, Casanova, S, Cotti, U, Cotzomi, J, Díaz-Vélez, JC, De León, C, De la Fuente, E, Dichiara, S, DuVernois, MA, Espinoza, C, Fiorino, DW, Fleischhack, H, Fraija, N, Galván-Gámez, A, García-González, JA, González, MM, Goodman, JA, Hampel-Arias, Z, Harding, JP, Hernandez, S, Hona, B, Hueyotl-Zahuantitla, F, Iriarte, A, Jardin-Blicq, A, Joshi, V, Lara, A, Vargas, H León, Luis-Raya, G, Malone, K, Marinelli, SS, Martínez-Castro, J, Martinez, O, Matthews, JA, Miranda-Romagnoli, P, Moreno, E, Mostafá, M, Nellen, L, Newbold, M, Nisa, MU, Noriega-Papaqui, R, Pérez-Pérez, EG, Pretz, J, Ren, Z, Rho, CD, Rivière, C, Rosa-González, D, Rosenberg, M, Salazar, H, Greus, F Salesa, Sandoval, A, Schneider, M, Schoorlemmer, H, Sinnis, G, Smith, AJ, Surajbali, P, Taboada, I, Tollefson, K, Torres, I, Villaseor, L, Weisgarber, T, Wood, J, Zepeda, A, Zhou, H, Álvarez, JD, Aartsen, MG, Ackermann, M, Adams, J, Aguilar, JA, Ahlers, M, Ahrens, M, Altmann, D, Andeen, K, Anderson, T, Ansseau, I, Anton, G, Argüelles, C, Auffenberg, J, Axani, S, Backes, P, Bagherpour, H, Bai, X, Barbano, A, Barron, JP, Barwick, SW, Baum, V, Bay, R, Beatty, JJ, Tjus, J Becker, Becker, K-H, and BenZvi, S

Subjects
Particle and High Energy Physics, Astronomical Sciences, Physical Sciences, astroparticle physics, cosmic rays, ISM: magnetic fields, astro-ph.HE, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry (incl. Structural), Astronomy & Astrophysics, Astronomical sciences, Particle and high energy physics, Space sciences
Abstract

We present the first full-sky analysis of the cosmic ray arrival direction distribution with data collected by the High-Altitude Water Cherenkov and IceCube observatories in the northern and southern hemispheres at the same median primary particle energy of 10 TeV. The combined sky map and angular power spectrum largely eliminate biases that result from partial sky coverage and present a key to probe into the propagation properties of TeV cosmic rays through our local interstellar medium and the interaction between the interstellar and heliospheric magnetic fields. From the map, we determine the horizontal dipole components of the anisotropy δ 0h = 9.16 ×10-4 and δ 6h = 7.25 ×10-4 (±0.04 × 10-4). In addition, we infer the direction (229.°2 ± 3.°5 R.A., 11.°4 ± 3.°0 decl.) of the interstellar magnetic field from the boundary between large-scale excess and deficit regions from which we estimate the missing corresponding vertical dipole component of the large-scale anisotropy to be δN ∼ -3.97+1.0-2.0 × 10-4.

Published
2019

3. All-sky Measurement of the Anisotropy of Cosmic Rays at 10 TeV and Mapping of the Local Interstellar Magnetic Field

Author

Collaboration, H, Collaboration, I, Abeysekara, AU, Alfaro, R, Alvarez, C, Arceo, R, Arteaga-Velázquez, JC, Rojas, DA, Belmont-Moreno, E, Benzvi, SY, Brisbois, C, Capistrán, T, Carramiana, A, Casanova, S, Cotti, U, Cotzomi, J, Diaz-Vélez, JC, De León, C, Fuente, EDL, Dichiara, S, Duvernois, MA, Espinoza, C, Fiorino, DW, Fleischhack, H, Fraija, N, Galván-Gámez, A, Garcia-González, JA, González, MM, Goodman, JA, Hampel-Arias, Z, Harding, JP, Hernandez, S, Hona, B, Hueyotl-Zahuantitla, F, Iriarte, A, Jardin-Blicq, A, Joshi, V, Lara, A, Vargas, HL, Luis-Raya, G, Malone, K, Marinelli, SS, Martinez-Castro, J, Martinez, O, Matthews, JA, Miranda-Romagnoli, P, Moreno, E, Mostafá, M, Nellen, L, Newbold, M, Nisa, MU, Noriega-Papaqui, R, Pérez-Pérez, EG, Pretz, J, Ren, Z, Rho, CD, Riviere, C, Rosa-González, D, Rosenberg, M, Salazar, H, Greus, FS, Sandoval, A, Schneider, M, Schoorlemmer, H, Sinnis, G, Smith, AJ, Surajbali, P, Taboada, I, Tollefson, K, Torres, I, Villaseor, L, Weisgarber, T, Wood, J, Zepeda, A, Zhou, H, Alvarez, JD, Aartsen, MG, Ackermann, M, Adams, J, Aguilar, JA, Ahlers, M, Ahrens, M, Altmann, D, Andeen, K, Anderson, T, Ansseau, I, Anton, G, Argüelles, C, Auffenberg, J, Axani, S, Backes, P, Bagherpour, H, Bai, X, Barbano, A, Barron, JP, Barwick, SW, Baum, V, Bay, R, Beatty, JJ, and Tjus, JB

Subjects
astroparticle physics, cosmic rays, ISM: magnetic fields, astro-ph.HE, Astronomy & Astrophysics, Astronomical and Space Sciences, Organic Chemistry, Physical Chemistry, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry (incl. Structural)
Abstract

We present the first full-sky analysis of the cosmic ray arrival direction distribution with data collected by the High-Altitude Water Cherenkov and IceCube observatories in the northern and southern hemispheres at the same median primary particle energy of 10 TeV. The combined sky map and angular power spectrum largely eliminate biases that result from partial sky coverage and present a key to probe into the propagation properties of TeV cosmic rays through our local interstellar medium and the interaction between the interstellar and heliospheric magnetic fields. From the map, we determine the horizontal dipole components of the anisotropy δ 0h = 9.16 ×10 -4 and δ 6h = 7.25 ×10 -4 (±0.04 × 10 -4 ). In addition, we infer the direction (229.°2 ± 3.°5 R.A., 11.°4 ± 3.°0 decl.) of the interstellar magnetic field from the boundary between large-scale excess and deficit regions from which we estimate the missing corresponding vertical dipole component of the large-scale anisotropy to be δN ∼ -3.97 +1.0-2.0 × 10 -4 .

Published
2019

4. Observation of the Crab Nebula with the HAWC Gamma-Ray Observatory

Author

Abeysekara, AU, Albert, A, Alfaro, R, Alvarez, C, Álvarez, JD, Arceo, R, Arteaga-Velázquez, JC, Solares, HA Ayala, Barber, AS, Bautista-Elivar, N, Becerril, A, Belmont-Moreno, E, BenZvi, SY, Berley, D, Braun, J, Brisbois, C, Caballero-Mora, KS, Capistrán, T, Carramiñana, A, Casanova, S, Castillo, M, Cotti, U, Cotzomi, J, de León, S Coutiño, de la Fuente, E, De León, C, DeYoung, T, Dingus, BL, DuVernois, MA, Díaz-Vélez, JC, Ellsworth, RW, Fiorino, DW, Fraija, N, García-González, JA, Gerhardt, M, Munöz, A González, González, MM, Goodman, JA, Hampel-Arias, Z, Harding, JP, Hernandez, S, Hernandez-Almada, A, Hinton, J, Hui, CM, Hüntemeyer, P, Iriarte, A, Jardin-Blicq, A, Joshi, V, Kaufmann, S, Kieda, D, Lara, A, Lauer, RJ, Lee, WH, Lennarz, D, Vargas, H León, Linnemann, JT, Longinotti, AL, Raya, G Luis, Luna-García, R, López-Coto, R, Malone, K, Marinelli, SS, Martinez, O, Martinez-Castellanos, I, Martínez-Castro, J, Martínez-Huerta, H, Matthews, JA, Miranda-Romagnoli, P, Moreno, E, Mostafá, M, Nellen, L, Newbold, M, Nisa, MU, Noriega-Papaqui, R, Pelayo, R, Pretz, J, Pérez-Pérez, EG, Ren, Z, Rho, CD, Rivière, C, Rosa-González, D, Rosenberg, M, Ruiz-Velasco, E, Salazar, H, Greus, F Salesa, Sandoval, A, Schneider, M, Schoorlemmer, H, Sinnis, G, Smith, AJ, Springer, RW, Surajbali, P, Taboada, I, Tibolla, O, Tollefson, K, Torres, I, Ukwatta, TN, Villaseñor, L, Weisgarber, T, and Westerhoff, S

Subjects
acceleration of particles, gamma rays: general, ISM: individual objects, astro-ph.HE, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry (incl. Structural), Astronomy & Astrophysics
Abstract

The Crab Nebula is the brightest TeV gamma-ray source in the sky and has been used for the past 25 years as a reference source in TeV astronomy, for calibration and verification of new TeV instruments. The High Altitude Water Cherenkov Observatory (HAWC), completed in early 2015, has been used to observe the Crab Nebula at high significance across nearly the full spectrum of energies to which HAWC is sensitive. HAWC is unique for its wide field of view, nearly 2 sr at any instant, and its high-energy reach, up to 100 TeV. HAWC's sensitivity improves with the gamma-ray energy. Above ∼1 TeV the sensitivity is driven by the best background rejection and angular resolution ever achieved for a wide-field ground array. We present a time-integrated analysis of the Crab using 507 live days of HAWC data from 2014 November to 2016 June. The spectrum of the Crab is fit to a function of the form φ(E)= φ0(E/E0)-α-β In(E/E0). The data is well fitted with values of α = 2.63 ±0.03, β = 0.15 ±0.03, and log10(φ0cm2s TeV)=-12.60±0.02 when E 0 is fixed at 7 TeV and the fit applies between 1 and 37 TeV. Study of the systematic errors in this HAWC measurement is discussed and estimated to be ±50% in the photon flux between 1 and 37 TeV. Confirmation of the Crab flux serves to establish the HAWC instrument's sensitivity for surveys of the sky. The HAWC all-sky survey will be the deepest survey of the northern sky ever conducted in the multi-TeV band.

Published
2017

5. Search for Very High-energy Gamma Rays from the Northern Fermi Bubble Region with HAWC

Author

Abeysekara, AU, Albert, A, Alfaro, R, Alvarez, C, Álvarez, JD, Arceo, R, Arteaga-Velázquez, JC, Solares, HA Ayala, Barber, AS, Bautista-Elivar, N, Becerril, A, Belmont-Moreno, E, BenZvi, SY, Berley, D, Braun, J, Brisbois, C, Caballero-Mora, KS, Capistrán, T, Carramiñana, A, Casanova, S, Castillo, M, Cotti, U, Cotzomi, J, de León, S Coutiño, De León, C, De la Fuente, E, Hernandez, R Diaz, Dingus, BL, DuVernois, MA, Díaz-Vélez, JC, Ellsworth, RW, Engel, K, Fick, B, Fiorino, DW, Fleischhack, H, Fraija, N, García-González, JA, Garfias, F, Gerhardt, M, Muñoz, A González, González, MM, Goodman, JA, Hampel-Arias, Z, Harding, JP, Hernandez, S, Hernandez-Almada, A, Hinton, J, Hona, B, Hui, CM, Hüntemeyer, P, Iriarte, A, Jardin-Blicq, A, Joshi, V, Kaufmann, S, Kieda, D, Lara, A, Lauer, RJ, Lee, WH, Lennarz, D, Vargas, H León, Linnemann, JT, Longinotti, AL, Raya, G Luis, Luna-García, R, López-Coto, R, Malone, K, Marinelli, SS, Martinez, O, Martinez-Castellanos, I, Martínez-Castro, J, Martínez-Huerta, H, Matthews, JA, Miranda-Romagnoli, P, Moreno, E, Mostafá, M, Nellen, L, Newbold, M, Nisa, MU, Noriega-Papaqui, R, Pelayo, R, Pretz, J, Pérez-Pérez, EG, Ren, Z, Rho, CD, Rivière, C, Rosa-González, D, Rosenberg, M, Ruiz-Velasco, E, Salazar, H, Greus, F Salesa, Sandoval, A, Schneider, M, Schoorlemmer, H, Sinnis, G, Smith, AJ, Springer, RW, Surajbali, P, Taboada, I, Tibolla, O, and Tollefson, K

Subjects
astroparticle physics, Galaxy: general, Galaxy: structure, gamma rays: diffuse background, astro-ph.HE, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry (incl. Structural), Astronomy & Astrophysics
Abstract

We present a search for very high-energy gamma-ray emission from the Northern Fermi Bubble region using data collected with the High Altitude Water Cherenkov gamma-ray observatory. The size of the data set is 290 days. No significant excess is observed in the Northern Fermi Bubble region, so upper limits above 1 TeV are calculated. The upper limits are between and . The upper limits disfavor a proton injection spectrum that extends beyond 100 TeV without being suppressed. They also disfavor a hadronic injection spectrum derived from neutrino measurements.

Published
2017

6. SEARCH FOR TeV GAMMA-RAY EMISSION FROM POINT-LIKE SOURCES IN THE INNER GALACTIC PLANE WITH A PARTIAL CONFIGURATION OF THE HAWC OBSERVATORY

Author

Abeysekara, AU, Alfaro, R, Alvarez, C, Álvarez, JD, Arceo, R, Arteaga-Velázquez, JC, Solares, HA Ayala, Barber, AS, Baughman, BM, Bautista-Elivar, N, Reyes, AD Becerril, Belmont, E, BenZvi, SY, Bernal, A, Braun, J, Caballero-Mora, KS, Capistrán, T, Carramiñana, A, Casanova, S, Castillo, M, Cotti, U, Cotzomi, J, de León, S Coutińo, de la Fuente, E, De León, C, DeYoung, T, Hernandez, R Diaz, Dingus, BL, DuVernois, MA, Ellsworth, RW, Enriquez-Rivera, O, Fiorino, DW, Fraija, N, Garfias, F, González, MM, Goodman, JA, Gussert, M, Hampel-Arias, Z, Harding, JP, Hernandez, S, Hüntemeyer, P, Hui, CM, Imran, A, Iriarte, A, Karn, P, Kieda, D, Lara, A, Lauer, RJ, Lee, WH, Lennarz, D, Vargas, H León, Linnemann, JT, Longo, M, Raya, G Luis, Malone, K, Marinelli, A, Marinelli, SS, Martinez, H, Martinez, O, Martínez-Castro, J, Matthews, JA, Miranda-Romagnoli, P, Moreno, E, Mostafá, M, Nellen, L, Newbold, M, Noriega-Papaqui, R, Patricelli, B, Pelayo, R, Pérez-Pérez, EG, Pretz, J, Ren, Z, Rivière, C, Rosa-González, D, Salazar, H, Greus, F Salesa, Sandoval, A, Schneider, M, Sinnis, G, Smith, AJ, Woodle, K Sparks, Springer, RW, Taboada, I, Tibolla, O, Tollefson, K, Torres, I, Ukwatta, TN, Villaseñor, L, Vrabel, K, Weisgarber, T, Westerhoff, S, Wisher, IG, Wood, J, Yapici, T, Yodh, GB, Younk, PW, Zaborov, D, Zepeda, A, and Zhou, H

Subjects
astroparticle physics, gamma rays: diffuse background, gamma rays: general, astro-ph.HE, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry (incl. Structural), Astronomy & Astrophysics
Abstract

A survey of the inner Galaxy region of Galactic longitude l ∈[+15,+50] and latitude b ∈ [-4, +4] is performed using one-third of the High Altitude Water Cherenkov Observatory, operated during ts construction phase. To address the ambiguities arising from unresolved sources in the data, we use a maximum likelihood technique to identify point source candidates. Ten sources and candidate sources are identified in this analysis. Eight of these are associated with known TeV sources but not all have ifferential fluxes that are compatible with previous measurements. Three sources are detected with significances >5 sigma; after accounting for statistical trials, and are associated with known TeV sources.

Published
2016

7. HAWC Contributions to the 34th International Cosmic Ray Conference (ICRC2015)

Author

Collaboration, HAWC, Abeysekara, AU, Alfaro, R, Alvarez, C, Álvarez, JD, Arceo, R, Arteaga-Velázquez, JC, Solares, HA Ayala, Barber, AS, Baughman, BM, Bautista-Elivar, N, Gonzalez, J Becerra, Becerril, A, Belmont, E, BenZvi, SY, Berley, D, Bernal, A, Braun, J, Caballero-Mora, KS, Capistrán, T, Carramiñana, A, Castillo, M, Cotti, U, Cotzomi, J, León, S Coutiño de, Fuente, E de la, León, C De, DeYoung, T, Hernandez, R Diaz, Diaz-Cruz, L, Díaz-Vélez, JC, Dingus, BL, DuVernois, MA, Ellsworth, RW, Engel, K, Enriquez-Rivera, O, Fick, B, Fiorino, DW, Flores, JL, Fraija, N, Garcia-Torales, G, Garfias, F, González, MM, Goodman, JA, Gussert, M, Hampel-Arias, Z, Hansen, P, Harding, J Patrick, Hernandez, S, Hui, CM, Hüntemeyer, P, Imran, A, Iriarte, A, Karn, P, Kieda, D, Kunde, GJ, Lara, A, Lauer, RJ, Lee, WH, Lennarz, D, Vargas, H León, Linnemann, JT, Proper, M Longo, Raya, G Luis, Luna-García, R, Malone, K, Marinelli, A, Marinelli, SS, Martinez, H, Martinez, O, Martínez-Castro, J, Matthews, JAJ, McEnery, J, Miranda-Romagnoli, P, Moreno, E, Mostafá, M, Nellen, L, Newbold, M, Nisa, M Un, Noriega-Papaqui, R, Oceguera-Becerra, T, Patricelli, B, Pelayo, R, Pérez-Pérez, EG, Pretz, J, Ren, Z, Rho, CD, Rivière, C, Rosa-González, D, Ryan, J, Salazar, H, Greus, F Salesa, Sandoval, A, Schneider, M, Sinnis, G, Smith, AJ, Smith, AW, Woodle, K Sparks, Springer, RW, and Taboada, I

Subjects
astro-ph.HE, hep-ex
Abstract

List of proceedings from the HAWC Collaboration presented at the 34thInternational Cosmic Ray Conference, 30 July - 6 August 2015, The Hague, TheNetherlands.

Published
2015

8. Milagro limits and HAWC sensitivity for the rate-density of evaporating Primordial Black Holes

Author

Abdo, AA, Abeysekara, AU, Alfaro, R, Allen, BT, Alvarez, C, Álvarez, JD, Arceo, R, Arteaga-Velázquez, JC, Aune, T, Solares, HA Ayala, Barber, AS, Baughman, BM, Bautista-Elivar, N, Gonzalez, J Becerra, Belmont, E, BenZvi, SY, Berley, D, Rosales, M Bonilla, Braun, J, Caballero-Lopez, RA, Caballero-Mora, KS, Carramiñana, A, Castillo, M, Christopher, GE, Cotti, U, Cotzomi, J, de la Fuente, E, De León, C, DeYoung, T, Hernandez, R Diaz, Diaz-Cruz, L, Díaz-Vélez, JC, Dingus, BL, DuVernois, MA, Ellsworth, RW, Fiorino, DW, Fraija, N, Galindo, A, Garfias, F, González, MM, Goodman, JA, Grabski, V, Gussert, M, Hampel-Arias, Z, Harding, JP, Hays, E, Hoffman, CM, Hui, CM, Hüntemeyer, P, Imran, A, Iriarte, A, Karn, P, Kieda, D, Kolterman, BE, Kunde, GJ, Lara, A, Lauer, RJ, Lee, WH, Lennarz, D, Vargas, H León, Linares, EC, Linnemann, JT, Longo, M, Luna-GarcIa, R, MacGibbon, JH, Marinelli, A, Marinelli, SS, Martinez, H, Martinez, O, Martínez-Castro, J, Matthews, JAJ, McEnery, J, Torres, E Mendoza, Mincer, AI, Miranda-Romagnoli, P, Moreno, E, Morgan, T, Mostafá, M, Nellen, L, Nemethy, P, Newbold, M, Noriega-Papaqui, R, Oceguera-Becerra, T, Patricelli, B, Pelayo, R, Pérez-Pérez, EG, Pretz, J, Rivière, C, Rosa-González, D, Ruiz-Velasco, E, Ryan, J, Salazar, H, Salesa, F, Sandoval, A, Parkinson, PM Saz, Schneider, M, Silich, S, Sinnis, G, Smith, AJ, and Stump, D

Subjects
Primordial Black Holes, HAWC, Milagro, Very High Energy Bursts, astro-ph.HE, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Nuclear & Particles Physics
Abstract

Primordial Black Holes (PBHs) are gravitationally collapsed objects that may have been created by density fluctuations in the early universe and could have arbitrarily small masses down to the Planck scale. Hawking showed that due to quantum effects, a black hole has a temperature inversely proportional to its mass and will emit all species of fundamental particles thermally. PBHs with initial masses of ∼5.0 × 1014 g should be expiring in the present epoch with bursts of high-energy particles, including gamma radiation in the GeV-TeV energy range. The Milagro high energy observatory, which operated from 2000 to 2008, is sensitive to the high end of the PBH evaporation gamma-ray spectrum. Due to its large field-of-view, more than 90% duty cycle and sensitivity up to 100 TeV gamma rays, the Milagro observatory is well suited to perform a search for PBH bursts. Based on a search on the Milagro data, we report new PBH burst rate density upper limits over a range of PBH observation times. In addition, we report the sensitivity of the Milagro successor, the High Altitude Water Cherenkov (HAWC) observatory, to PBH evaporation events.

Published
2015

9. VAMOS: A pathfinder for the HAWC gamma-ray observatory

Author

Abeysekara, AU, Alfaro, R, Alvarez, C, Álvarez, JD, Ángeles, F, Arceo, R, Arteaga-Velázquez, JC, Avila-Aroche, A, Solares, HA Ayala, Badillo, C, Barber, AS, Baughman, BM, Bautista-Elivar, N, Gonzalez, J Becerra, Belmont, E, Benítez, E, BenZvi, SY, Berley, D, Bernal, A, Rosales, M Bonilla, Braun, J, Caballero-Lopez, RA, Caballero-Mora, KS, Cabrera, I, Carramiñana, A, Castañeda-Martínez, L, Castillo, M, Cotti, U, Cotzomi, J, de la Fuente, E, De León, C, DeYoung, T, Diaz-Azuara, A, Diaz-Cruz, L, Hernandez, R Diaz, Díaz-Vélez, JC, Dingus, BL, Dultzin, D, DuVernois, MA, Ellsworth, RW, Fernandez, A, Fiorino, DW, Fraija, N, Galindo, A, García-Torales, G, Garfias, F, González, A, González, LX, González, MM, Goodman, JA, Grabski, V, Gussert, M, Guzmán-Cerón, C, Hampel-Arias, Z, Harding, JP, Hernández-Cervantes, L, Hui, CM, Hüntemeyer, P, Imran, A, Iriarte, A, Karn, P, Kieda, D, Kunde, GJ, Langarica, R, Lara, A, Lara, G, Lauer, RJ, Lee, WH, Lennarz, D, Vargas, H León, Linares, EC, Linnemann, JT, Longo, M, Luna-Garcia, R, Marinelli, A, Martínez, LA, Martínez, H, Martínez, O, Martínez-Castro, J, Martos, M, Matthews, JAJ, McEnery, J, Torres, E Mendoza, Miranda-Romagnoli, P, Moreno, E, Mostafá, M, Nava, J, Nellen, L, Newbold, M, Noriega-Papaqui, R, Oceguera-Becerra, T, Page, DP, Patricelli, B, Pelayo, R, Pérez-Pérez, EG, Pretz, J, Ramírez, I, Rentería, A, Rivière, C, and Rosa-González, D

Subjects
Detector prototype, Scientific verification, TeV cosmic rays, astro-ph.IM, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Nuclear & Particles Physics
Abstract

VAMOS1 was a prototype detector built in 2011 at an altitude of 4100 m a.s.l. in the state of Puebla, Mexico. The aim of VAMOS was to finalize the design, construction techniques and data acquisition system of the HAWC observatory. HAWC is an air-shower array currently under construction at the same site of VAMOS with the purpose to study the TeV sky. The VAMOS setup included six water Cherenkov detectors and two different data acquisition systems. It was in operation between October 2011 and May 2012 with an average live time of 30%. Besides the scientific verification purposes, the eight months of data were used to obtain the results presented in this paper: the detector response to the Forbush decrease of March 2012, and the analysis of possible emission, at energies above 30 GeV, for long gamma-ray bursts GRB111016B and GRB120328B.

Published
2015

10. SEARCH FOR GAMMA-RAYS FROM THE UNUSUALLY BRIGHT GRB 130427A WITH THE HAWC GAMMA-RAY OBSERVATORY

Author

Abeysekara, AU, Alfaro, R, Alvarez, C, Álvarez, JD, Arceo, R, Arteaga-Velázquez, JC, Solares, HA Ayala, Barber, AS, Baughman, BM, Bautista-Elivar, N, BenZvi, SY, Rosales, M Bonilla, Braun, J, Caballero-Mora, KS, Carramiñana, A, Castillo, M, Cotti, U, Cotzomi, J, de la Fuente, E, De León, C, DeYoung, T, Hernandez, R Diaz, Dingus, BL, DuVernois, MA, Ellsworth, RW, Fiorino, DW, Fraija, N, Galindo, A, Garfias, F, González, MM, Goodman, JA, Gussert, M, Hampel-Arias, Z, Harding, JP, Hüntemeyer, P, Hui, CM, Imran, A, Iriarte, A, Karn, P, Kieda, D, Kunde, GJ, Lara, A, Lauer, RJ, Lee, WH, Lennarz, D, Vargas, H León, Linnemann, JT, Longo, M, Luna-García, R, Malone, K, Marinelli, A, Marinelli, SS, Martinez, H, Martinez, O, Martínez-Castro, J, Matthews, JAJ, Torres, E Mendoza, Miranda-Romagnoli, P, Moreno, E, Mostafá, M, Nellen, L, Newbold, M, Noriega-Papaqui, R, Oceguera-Becerra, TO, Patricelli, B, Pelayo, R, Pérez-Pérez, EG, Pretz, J, Rivière, C, Rosa-González, D, Salazar, H, Greus, F Salesa, Sandoval, A, Schneider, M, Sinnis, G, Smith, AJ, Woodle, K Sparks, Springer, RW, Taboada, I, Tollefson, K, Torres, I, Ukwatta, TN, Villaseñor, L, Weisgarber, T, Westerhoff, S, Wisher, IG, Wood, J, Yodh, GB, Younk, PW, Zaborov, D, Zepeda, A, and Zhou, and H

Subjects
gamma-ray burst: individual, gamma rays: general, astro-ph.HE, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry (incl. Structural), Astronomy & Astrophysics
Abstract

The first limits on the prompt emission from the long gamma-ray burst (GRB) 130427A in the >100 GeV energy band are reported. GRB 130427A was the most powerful burst ever detected with a redshift z ≲ 0.5 and featured the longest lasting emission above 100 MeV. The energy spectrum extends at least up to 95 GeV, clearly in the range observable by the High Altitude Water Cherenkov (HAWC) Gamma-Ray Observatory, a new extensive air shower detector currently under construction in central Mexico. The burst occurred under unfavorable observation conditions, low in the sky and when HAWC was running 10% of the final detector. Based on the observed light curve at MeV-GeV energies, eight different time periods have been searched for prompt and delayed emission from this GRB. In all cases, no statistically significant excess of counts has been found and upper limits have been placed. It is shown that a similar GRB close to zenith would be easily detected by the full HAWC detector, which will be completed soon. The detection rate of the full HAWC detector may be as high as one to two GRBs per year. A detection could provide important information regarding the high energy processes at work and the observation of a possible cut-off beyond the Fermi Large Area Telescope energy range could be the signature of gamma-ray absorption, either in the GRB or along the line of sight due to the extragalactic background light.

Published
2015

11. Sensitivity of HAWC to high-mass dark matter annihilations

Author

Abeysekara, AU, Alfaro, R, Alvarez, C, Álvarez, JD, Arceo, R, Arteaga-Velázquez, JC, Solares, HA Ayala, Barber, AS, Baughman, BM, Bautista-Elivar, N, Gonzalez, J Becerra, Belmont, E, BenZvi, SY, Berley, D, Rosales, M Bonilla, Braun, J, Caballero-Lopez, RA, Caballero-Mora, KS, Carramiñana, A, Castillo, M, Cotti, U, Cotzomi, J, de la Fuente, E, De León, C, DeYoung, T, Hernandez, R Diaz, Diaz-Cruz, L, Díaz-Vélez, JC, Dingus, BL, DuVernois, MA, Ellsworth, RW, Fiorino, DW, Fraija, N, Galindo, A, Garfias, F, González, MM, Goodman, JA, Grabski, V, Gussert, M, Hampel-Arias, Z, Harding, JP, Hui, CM, Hüntemeyer, P, Imran, A, Iriarte, A, Karn, P, Kieda, D, Kunde, GJ, Lara, A, Lauer, RJ, Lee, WH, Lennarz, D, Vargas, H León, Linares, EC, Linnemann, JT, Longo, M, Luna-Garcia, R, Marinelli, A, Martinez, H, Martinez, O, Martínez-Castro, J, Matthews, JAJ, McEnery, J, Torres, E Mendoza, Miranda-Romagnoli, P, Moreno, E, Mostafá, M, Nellen, L, Newbold, M, Noriega-Papaqui, R, Oceguera-Becerra, T, Patricelli, B, Pelayo, R, Pérez-Pérez, EG, Pretz, J, Rivière, C, Rosa-González, D, Ryan, J, Salazar, H, Salesa, F, Sanchez, FE, Sandoval, A, Schneider, M, Silich, S, Sinnis, G, Smith, AJ, Woodle, K Sparks, Springer, RW, Taboada, I, Toale, PA, Tollefson, K, Torres, I, Ukwatta, TN, Villaseñor, L, Weisgarber, T, Westerhoff, S, Wisher, IG, Wood, J, Yodh, GB, and Younk, PW

Subjects
astro-ph.HE, astro-ph.CO, hep-ph, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Quantum Physics, Nuclear & Particles Physics
Abstract

The High Altitude Water Cherenkov (HAWC) observatory is a wide field-of-view detector sensitive to gamma rays of 100 GeV to a few hundred TeV. Located in central Mexico at 19° North latitude and 4100 m above sea level, HAWC will observe gamma rays and cosmic rays with an array of water Cherenkov detectors. The full HAWC array is scheduled to be operational in Spring 2015. In this paper, we study the HAWC sensitivity to the gamma-ray signatures of high-mass (multi-TeV) dark matter annihilation. The HAWC observatory will be sensitive to diverse searches for dark matter annihilation, including annihilation from extended dark matter sources, the diffuse gamma-ray emission from dark matter annihilation, and gamma-ray emission from nonluminous dark matter subhalos. Here we consider the HAWC sensitivity to a subset of these sources, including dwarf galaxies, the M31 galaxy, the Virgo cluster, and the Galactic center. We simulate the HAWC response to gamma rays from these sources in several well-motivated dark matter annihilation channels. If no gamma-ray excess is observed, we show the limits HAWC can place on the dark matter cross section from these sources. In particular, in the case of dark matter annihilation into gauge bosons, HAWC will be able to detect a narrow range of dark matter masses to cross sections below thermal. HAWC should also be sensitive to nonthermal cross sections for masses up to nearly 1000 TeV. The constraints placed by HAWC on the dark matter cross section from known sources should be competitive with current limits in the mass range where HAWC has similar sensitivity. HAWC can additionally explore higher dark matter masses than are currently constrained.

Published
2014

12. OBSERVATION OF SMALL-SCALE ANISOTROPY IN THE ARRIVAL DIRECTION DISTRIBUTION OF TeV COSMIC RAYS WITH HAWC

Author

Abeysekara, AU, Alfaro, R, Alvarez, C, Álvarez, JD, Arceo, R, Arteaga-Velázquez, JC, Solares, HA Ayala, Barber, AS, Baughman, BM, Bautista-Elivar, N, Belmont, E, BenZvi, SY, Berley, D, Rosales, M Bonilla, Braun, J, Caballero-Mora, KS, Carramiñana, A, Castillo, M, Cotti, U, Cotzomi, J, de la Fuente, E, De León, C, DeYoung, T, Hernandez, R Diaz, Díaz-Vélez, JC, Dingus, BL, DuVernois, MA, Ellsworth, RW, Fiorino, DW, Fraija, N, Galindo, A, Garfias, F, González, MM, Goodman, JA, Gussert, M, Hampel-Arias, Z, Harding, JP, Hüntemeyer, P, Hui, CM, Imran, A, Iriarte, A, Karn, P, Kieda, D, Kunde, GJ, Lara, A, Lauer, RJ, Lee, WH, Lennarz, D, Vargas, H León, Linnemann, JT, Longo, M, Luna-García, R, Malone, K, Marinelli, A, Marinelli, SS, Martinez, H, Martinez, O, Martínez-Castro, J, Matthews, JAJ, McEnery, J, Torres, E Mendoza, Miranda-Romagnoli, P, Moreno, E, Mostafá, M, Nellen, L, Newbold, M, Noriega-Papaqui, R, Oceguera-Becerra, T, Patricelli, B, Pelayo, R, Pérez-Pérez, EG, Pretz, J, Rivière, C, Rosa-González, D, Ruiz-Velasco, E, Ryan, J, Salazar, H, Greus, F Salesa, Sandoval, A, Schneider, M, Sinnis, G, Smith, AJ, Woodle, K Sparks, Springer, RW, Taboada, I, Toale, PA, Tollefson, K, Torres, I, Ukwatta, TN, Villaseñor, L, Weisgarber, T, Westerhoff, S, Wisher, IG, Wood, J, Yodh, GB, Younk, PW, Zaborov, D, Zepeda, A, and Zhou, and H

Subjects
Astroparticle physics, Cosmic rays, astroparticle physics, cosmic rays, astro-ph.HE, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry (incl. Structural), Astronomy & Astrophysics
Abstract

The High-Altitude Water Cherenkov (HAWC) Observatory is sensitive to gamma rays and charged cosmic rays at TeV energies. The detector is still under construction, but data acquisition with the partially deployed detector started in 2013. An analysis of the cosmic-ray arrival direction distribution based on 4.9 × 1010 events recorded between 2013 June and 2014 February shows anisotropy at the 10-4 level on angular scales of about 10°. The HAWC cosmic-ray sky map exhibits three regions of significantly enhanced cosmic-ray flux; two of these regions were first reported by the Milagro experiment. A third region coincides with an excess recently reported by the ARGO-YBJ experiment. An angular power spectrum analysis of the sky shows that all terms up to l = 15 contribute significantly to the excesses.

Published
2014

13. Sensitivity of the high altitude water Cherenkov detector to sources of multi-TeV gamma rays

Author

Abeysekara, AU, Alfaro, R, Alvarez, C, Álvarez, JD, Arceo, R, Arteaga-Velázquez, JC, Solares, HA Ayala, Barber, AS, Baughman, BM, Bautista-Elivar, N, Belmont, E, BenZvi, SY, Berley, D, Rosales, M Bonilla, Braun, J, Caballero-Lopez, RA, Carramiñana, A, Castillo, M, Cotti, U, Cotzomi, J, de la Fuente, E, De León, C, DeYoung, T, Hernandez, R Diaz, Diaz-Velez, JC, Dingus, BL, DuVernois, MA, Ellsworth, RW, Fernandez, A, Fiorino, DW, Fraija, N, Galindo, A, Garcia-Luna, JL, Garcia-Torales, G, Garfias, F, González, LX, González, MM, Goodman, JA, Grabski, V, Gussert, M, Hampel-Arias, Z, Hui, CM, Hüntemeyer, P, Imran, A, Iriarte, A, Karn, P, Kieda, D, Kunde, GJ, Lara, A, Lauer, RJ, Lee, WH, Lennarz, D, Vargas, H León, Linares, EC, Linnemann, JT, Longo, M, Luna-García, R, Marinelli, A, Martinez, O, Martínez-Castro, J, Matthews, JAJ, Miranda-Romagnoli, P, Moreno, E, Mostafá, M, Nava, J, Nellen, L, Newbold, M, Noriega-Papaqui, R, Oceguera-Becerra, T, Patricelli, B, Pelayo, R, Pérez-Pérez, EG, Pretz, J, Rivière, C, Ryan, J, Rosa-González, D, Salazar, H, Salesa, F, Sandoval, A, Santos, E, Schneider, M, Silich, S, Sinnis, G, Smith, AJ, Sparks, K, Springer, RW, Taboada, I, Toale, PA, Tollefson, K, Torres, I, Ukwatta, TN, Villaseñor, L, Weisgarber, T, Westerhoff, S, Wisher, IG, Wood, J, Yodh, GB, Younk, PW, Zaborov, D, and Zepeda, A

Subjects
TeV gamma-ray astronomy, Water cherenkov, Cosmic ray, astro-ph.HE, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Nuclear & Particles Physics
Abstract

The High Altitude Water Cherenkov (HAWC) observatory is an array of large water Cherenkov detectors sensitive to gamma rays and hadronic cosmic rays in the energy band between 100 GeV and 100 TeV. The observatory will be used to measure high-energy protons and cosmic rays via detection of the energetic secondary particles reaching the ground when one of these particles interacts in the atmosphere above the detector. HAWC is under construction at a site 4100 meters above sea level on the northern slope of the volcano Sierra Negra, which is located in central Mexico at 19 N latitude. It is scheduled for completion in 2014. In this paper we estimate the sensitivity of the HAWC instrument to point-like and extended sources of gamma rays. The source fluxes are modeled using both unbroken power laws and power laws with exponential cutoffs. HAWC, in one year, is sensitive to point sources with integral power-law spectra as low as 5×10-13 cm-2sec-1 above 2 TeV (approximately 50 mCrab) over 5 sr of the sky. This is a conservative estimate based on simple event parameters and is expected to improve as the data analysis techniques are refined. We discuss known TeV sources and the scientific contributions that HAWC can make to our understanding of particle acceleration in these sources. © 2013 Elsevier B.V. All rights reserved.

Published
2013

14. The HAWC Gamma-Ray Observatory: Sensitivity to Steady and Transient Sources of Gamma Rays

Author

Collaboration, HAWC, Abeysekara, AU, Alfaro, R, Alvarez, C, Álvarez, JD, Arceo, R, Arteaga-Velázquez, JC, Solares, HA Ayala, Barber, AS, Baughman, BM, Bautista-Elivar, N, Belmont, E, BenZvi, SY, Berley, D, Rosales, M Bonilla, Braun, J, Caballero-Lopez, RA, Caballero-Mora, KS, Carramiñana, A, Castillo, M, Cotti, U, Cotzomi, J, Fuente, E de la, León, C De, DeYoung, T, Hernandez, R Diaz, Díaz-Vélez, JC, Dingus, BL, DuVernois, MA, Ellsworth, RW, Fernandez, A, Fiorino, DW, Fraija, N, Galindo, A, Garfias, F, González, LX, González, MM, Goodman, JA, Grabski, V, Gussert, M, Hampel-Arias, Z, Hui, CM, Hüntemeyer, P, Imran, A, Iriarte, A, Karn, P, Kieda, D, Kunde, GJ, Lara, A, Lauer, RJ, Lee, WH, Lennarz, D, Vargas, H León, Linares, EC, Linnemann, JT, Longo, M, Luna-GarcIa, R, Marinelli, A, Martinez, H, Martinez, O, Martínez-Castro, J, Matthews, JAJ, Miranda-Romagnoli, P, Moreno, E, Mostafá, M, Nava, J, Nellen, L, Newbold, M, Noriega-Papaqui, R, Oceguera-Becerra, T, Patricelli, B, Pelayo, R, Pérez-Pérez, EG, Pretz, J, Rivière, C, Rosa-González, D, Salazar, H, Salesa, F, Sanchez, FE, Sandoval, A, Santos, E, Schneider, M, Silich, S, Sinnis, G, Smith, AJ, Sparks, K, Springer, RW, Taboada, I, Toale, PA, Tollefson, K, Torres, I, Ukwatta, TN, Villaseñor, L, Weisgarber, T, Westerhoff, S, Wisher, IG, Wood, J, Yodh, GB, Younk, PW, and Zaborov, D

Subjects
astro-ph.HE
Abstract

The High-Altitude Water Cherenkov (HAWC) Gamma-Ray Observatory is designed torecord air showers produced by cosmic rays and gamma rays between 100 GeV and100 TeV. Because of its large field of view and high livetime, HAWC iswell-suited to measure gamma rays from extended sources, diffuse emission, andtransient sources. We describe the sensitivity of HAWC to emission from theextended Cygnus region as well as other types of galactic diffuse emission;searches for flares from gamma-ray bursts and active galactic nuclei; and thefirst measurement of the Crab Nebula with HAWC-30.

Published
2013

15. The HAWC Gamma-Ray Observatory: Observations of Cosmic Rays

Author

Collaboration, HAWC, Abeysekara, AU, Alfaro, R, Alvarez, C, Álvarez, JD, Arceo, R, Arteaga-Velázquez, JC, Solares, HA Ayala, Barber, AS, Baughman, BM, Bautista-Elivar, N, Belmont, E, BenZvi, SY, Berley, D, Rosales, M Bonilla, Braun, J, Caballero-Lopez, RA, Caballero-Mora, KS, Carramiñana, A, Castillo, M, Cotti, U, Cotzomi, J, Fuente, E de la, León, C De, DeYoung, T, Hernandez, R Diaz, Díaz-Vélez, JC, Dingus, BL, DuVernois, MA, Ellsworth, RW, Fernandez, A, Fiorino, DW, Fraija, N, Galindo, A, Garfias, F, González, LX, González, MM, Goodman, JA, Grabski, V, Gussert, M, Hampel-Arias, Z, Hui, CM, Hüntemeyer, P, Imran, A, Iriarte, A, Karn, P, Kieda, D, Kunde, GJ, Lara, A, Lauer, RJ, Lee, WH, Lennarz, D, Vargas, H León, Linares, EC, Linnemann, JT, Longo, M, Luna-GarcIa, R, Marinelli, A, Martinez, H, Martinez, O, Martínez-Castro, J, Matthews, JAJ, Miranda-Romagnoli, P, Moreno, E, Mostafá, M, Nava, J, Nellen, L, Newbold, M, Noriega-Papaqui, R, Oceguera-Becerra, T, Patricelli, B, Pelayo, R, Pérez-Pérez, EG, Pretz, J, Rivière, C, Rosa-González, D, Salazar, H, Salesa, F, Sanchez, FE, Sandoval, A, Santos, E, Schneider, M, Silich, S, Sinnis, G, Smith, AJ, Sparks, K, Springer, RW, Taboada, I, Toale, PA, Tollefson, K, Torres, I, Ukwatta, TN, Villaseñor, L, Weisgarber, T, Westerhoff, S, Wisher, IG, Wood, J, Yodh, GB, Younk, PW, and Zaborov, D

Subjects
astro-ph.HE
Abstract

We describe measurements of GeV and TeV cosmic rays with the High-AltitudeWater Cherenkov Gamma-Ray Observatory, or HAWC. The measurements include theobservation of the shadow of the moon; the observation of small-scale andlarge-scale angular clustering of the TeV cosmic rays; the prospects formeasurement of transient solar events with HAWC; and the observation of Forbushdecreases with the HAWC engineering array and HAWC-30.

Published
2013

16. The HAWC Gamma-Ray Observatory: Design, Calibration, and Operation

Author

Collaboration, HAWC, Abeysekara, AU, Alfaro, R, Alvarez, C, Álvarez, JD, Arceo, R, Arteaga-Velázquez, JC, Solares, HA Ayala, Barber, AS, Baughman, BM, Bautista-Elivar, N, Belmont, E, BenZvi, SY, Berley, D, Rosales, M Bonilla, Braun, J, Caballero-Lopez, RA, Caballero-Mora, KS, Carramiñana, A, Castillo, M, Cotti, U, Cotzomi, J, Fuente, E de la, León, C De, DeYoung, T, Hernandez, R Diaz, Díaz-Vélez, JC, Dingus, BL, DuVernois, MA, Ellsworth, RW, Fernandez, A, Fiorino, DW, Fraija, N, Galindo, A, Garfias, F, González, LX, González, MM, Goodman, JA, Grabski, V, Gussert, M, Hampel-Arias, Z, Hui, CM, Hüntemeyer, P, Imran, A, Iriarte, A, Karn, P, Kieda, D, Kunde, GJ, Lara, A, Lauer, RJ, Lee, WH, Lennarz, D, Vargas, H León, Linares, EC, Linnemann, JT, Longo, M, Luna-GarcIa, R, Marinelli, A, Martinez, H, Martinez, O, Martínez-Castro, J, Matthews, JAJ, Miranda-Romagnoli, P, Moreno, E, Mostafá, M, Nava, J, Nellen, L, Newbold, M, Noriega-Papaqui, R, Oceguera-Becerra, T, Patricelli, B, Pelayo, R, Pérez-Pérez, EG, Pretz, J, Rivière, C, Rosa-González, D, Salazar, H, Salesa, F, Sanchez, FE, Sandoval, A, Santos, E, Schneider, M, Silich, S, Sinnis, G, Smith, AJ, Sparks, K, Springer, RW, Taboada, I, Toale, PA, Tollefson, K, Torres, I, Ukwatta, TN, Villaseñor, L, Weisgarber, T, Westerhoff, S, Wisher, IG, Wood, J, Yodh, GB, Younk, PW, and Zaborov, D

Subjects
astro-ph.IM, astro-ph.HE
Abstract

The High-Altitude Water Cherenkov Gamma Ray Observatory (HAWC) is underconstruction 4100 meters above sea level at Sierra Negra, Mexico. We describethe design and cabling of the detector, the characterization of thephotomultipliers, and the timing calibration system. We also outline anext-generation detector based on the water Cherenkov technique.

Published
2013

17. The HAWC Gamma-Ray Observatory: Dark Matter, Cosmology, and Fundamental Physics

Author

Collaboration, HAWC, Abeysekara, AU, Alfaro, R, Alvarez, C, Álvarez, JD, Arceo, R, Arteaga-Velázquez, JC, Solares, HA Ayala, Barber, AS, Baughman, BM, Bautista-Elivar, N, Belmont, E, BenZvi, SY, Berley, D, Rosales, M Bonilla, Braun, J, Caballero-Lopez, RA, Caballero-Mora, KS, Carramiñana, A, Castillo, M, Cotti, U, Cotzomi, J, Fuente, E de la, León, C De, DeYoung, T, Hernandez, R Diaz, Díaz-Vélez, JC, Dingus, BL, DuVernois, MA, Ellsworth, RW, Fernandez, A, Fiorino, DW, Fraija, N, Galindo, A, Garfias, F, González, LX, González, MM, Goodman, JA, Grabski, V, Gussert, M, Hampel-Arias, Z, Hui, CM, Hüntemeyer, P, Imran, A, Iriarte, A, Karn, P, Kieda, D, Kunde, GJ, Lara, A, Lauer, RJ, Lee, WH, Lennarz, D, Vargas, H León, Linares, EC, Linnemann, JT, Longo, M, Luna-GarcIa, R, Marinelli, A, Martinez, H, Martinez, O, Martínez-Castro, J, Matthews, JAJ, Miranda-Romagnoli, P, Moreno, E, Mostafá, M, Nava, J, Nellen, L, Newbold, M, Noriega-Papaqui, R, Oceguera-Becerra, T, Patricelli, B, Pelayo, R, Pérez-Pérez, EG, Pretz, J, Rivière, C, Rosa-González, D, Salazar, H, Salesa, F, Sanchez, FE, Sandoval, A, Santos, E, Schneider, M, Silich, S, Sinnis, G, Smith, AJ, Sparks, K, Springer, RW, Taboada, I, Toale, PA, Tollefson, K, Torres, I, Ukwatta, TN, Villaseñor, L, Weisgarber, T, Westerhoff, S, Wisher, IG, Wood, J, Yodh, GB, Younk, PW, and Zaborov, D

Subjects
astro-ph.HE
Abstract

The High-Altitude Water Cherenkov Gamma Ray Observatory (HAWC) is designed toperform a synoptic survey of the TeV sky. The high energy coverage of theexperiment will enable studies of fundamental physics beyond the StandardModel, and the large field of view of the detector will enable detailed studiesof cosmologically significant backgrounds and magnetic fields. We describe thesensitivity of the full HAWC array to these phenomena in five contributionsshown at the 33rd International Cosmic Ray Conference in Rio de Janeiro, Brazil(July 2013).

Published
2013

18. Multimessenger Gamma-Ray and Neutrino Coincidence Alerts Using HAWC and IceCube Subthreshold Data

Author

Solares, HAA, Coutu, S, DeLaunay, JJ, Fox, DB, Grégoire, T, Keivani, A, Krauß, F, Mostafá, M, Murase, K, Turley, CF, Albert, A, Alfaro, R, Alvarez, C, Angeles Camacho, JR, Arteaga-Velázquez, JC, Arunbabu, KP, Rojas, DA, Belmont-Moreno, E, Brisbois, C, Caballero-Mora, KS, Carramiñana, A, Casanova, S, Cotti, U, De la Fuente, E, Hernandez, RD, Dingus, BL, DuVernois, MA, Durocher, M, Díaz-Vélez, JC, Espinoza, C, Fan, KL, Fleischhack, H, Fraija, N, Galván-Gámez, A, Garcia, D, García-González, JA, Garfias, F, González, MM, Goodman, JA, Harding, JP, Hona, B, Huang, D, Hueyotl-Zahuantitla, F, Hüntemeyer, P, Iriarte, A, Jardin-Blicq, A, Joshi, V, Vargas, HL, Linnemann, JT, Longinotti, AL, Luis-Raya, G, Lundeen, J, Malone, K, Martinez, O, Martinez-Castellanos, I, Martínez-Castro, J, Matthews, JA, Miranda-Romagnoli, P, Moreno, E, Nellen, L, Newbold, M, Nisa, MU, Noriega-Papaqui, R, Peisker, A, Pérez-Pérez, EG, Rho, CD, Rosa-González, D, Salazar, H, Greus, FS, Sandoval, A, Smith, AJ, Springer, RW, Tollefson, K, Torres, I, Torres-Escobedo, R, Ureña-Mena, F, Villaseñor, L, Weisgarber, T, Willox, E, Zepeda, A, Zhou, H, de León, C, Aartsen, MG, Abbasi, R, Ackermann, M, Adams, J, Aguilar, JA, Ahlers, M, Ahrens, M, Alispach, C, Amin, NM, Andeen, K, Anderson, T, Ansseau, I, Anton, G, Argüelles, C, Auffenberg, J, Axani, S, Bagherpour, H, and Bai, X

Subjects
astro-ph.HE, Particle and Plasma Physics, Molecular, Nuclear, Astronomy & Astrophysics, Atomic, Astronomical and Space Sciences, Physical Chemistry (incl. Structural)
Abstract

The High Altitude Water Cerenkov (HAWC) and IceCube observatories, through the Astrophysical Multimessenger Observatory Network (AMON) framework, have developed a multimessenger joint search for extragalactic astrophysical sources. This analysis looks for sources that emit both cosmic neutrinos and gamma rays that are produced in photohadronic or hadronic interactions. The AMON system is running continuously, receiving subthreshold data (i.e., data that are not suited on their own to do astrophysical searches) from HAWC and IceCube, and combining them in real time. Here we present the analysis algorithm, as well as results from archival data collected between 2015 June and 2018 August, with a total live time of 3.0 yr. During this period we found two coincident events that have a false-alarm rate (FAR) of

Published
2021

19. The HAWC Gamma-Ray Observatory: Observations of Cosmic Rays

Author

Collaboration, HAWC, Abeysekara, AU, Alfaro, R, Alvarez, C, Álvarez, JD, Arceo, R, Arteaga-Velázquez, JC, Solares, HAA, Barber, AS, Baughman, BM, Bautista-Elivar, N, Belmont, E, BenZvi, SY, Berley, D, Rosales, MB, Braun, J, Caballero-Lopez, RA, Caballero-Mora, KS, Carramiñana, A, Castillo, M, Cotti, U, Cotzomi, J, Fuente, EDL, León, CD, DeYoung, T, Hernandez, RD, Díaz-Vélez, JC, Dingus, BL, DuVernois, MA, Ellsworth, RW, Fernandez, A, Fiorino, DW, Fraija, N, Galindo, A, Garfias, F, González, LX, González, MM, Goodman, JA, Grabski, V, Gussert, M, Hampel-Arias, Z, Hui, CM, Hüntemeyer, P, Imran, A, Iriarte, A, Karn, P, Kieda, D, Kunde, GJ, Lara, A, Lauer, RJ, Lee, WH, Lennarz, D, Vargas, HL, Linares, EC, Linnemann, JT, Longo, M, Luna-GarcIa, R, Marinelli, A, Martinez, H, Martinez, O, Martínez-Castro, J, Matthews, JAJ, Miranda-Romagnoli, P, Moreno, E, Mostafá, M, Nava, J, Nellen, L, Newbold, M, Noriega-Papaqui, R, Oceguera-Becerra, T, Patricelli, B, Pelayo, R, Pérez-Pérez, EG, Pretz, J, Rivière, C, Rosa-González, D, Salazar, H, Salesa, F, Sanchez, FE, Sandoval, A, Santos, E, Schneider, M, Silich, S, Sinnis, G, Smith, AJ, Sparks, K, Springer, RW, Taboada, I, Toale, PA, Tollefson, K, Torres, I, Ukwatta, TN, Villaseñor, L, Weisgarber, T, Westerhoff, S, Wisher, IG, Wood, J, Yodh, GB, Younk, PW, Zaborov, D, Zepeda, A, Zhou, H, Collaboration, HAWC, Abeysekara, AU, Alfaro, R, Alvarez, C, Álvarez, JD, Arceo, R, Arteaga-Velázquez, JC, Solares, HAA, Barber, AS, Baughman, BM, Bautista-Elivar, N, Belmont, E, BenZvi, SY, Berley, D, Rosales, MB, Braun, J, Caballero-Lopez, RA, Caballero-Mora, KS, Carramiñana, A, Castillo, M, Cotti, U, Cotzomi, J, Fuente, EDL, León, CD, DeYoung, T, Hernandez, RD, Díaz-Vélez, JC, Dingus, BL, DuVernois, MA, Ellsworth, RW, Fernandez, A, Fiorino, DW, Fraija, N, Galindo, A, Garfias, F, González, LX, González, MM, Goodman, JA, Grabski, V, Gussert, M, Hampel-Arias, Z, Hui, CM, Hüntemeyer, P, Imran, A, Iriarte, A, Karn, P, Kieda, D, Kunde, GJ, Lara, A, Lauer, RJ, Lee, WH, Lennarz, D, Vargas, HL, Linares, EC, Linnemann, JT, Longo, M, Luna-GarcIa, R, Marinelli, A, Martinez, H, Martinez, O, Martínez-Castro, J, Matthews, JAJ, Miranda-Romagnoli, P, Moreno, E, Mostafá, M, Nava, J, Nellen, L, Newbold, M, Noriega-Papaqui, R, Oceguera-Becerra, T, Patricelli, B, Pelayo, R, Pérez-Pérez, EG, Pretz, J, Rivière, C, Rosa-González, D, Salazar, H, Salesa, F, Sanchez, FE, Sandoval, A, Santos, E, Schneider, M, Silich, S, Sinnis, G, Smith, AJ, Sparks, K, Springer, RW, Taboada, I, Toale, PA, Tollefson, K, Torres, I, Ukwatta, TN, Villaseñor, L, Weisgarber, T, Westerhoff, S, Wisher, IG, Wood, J, Yodh, GB, Younk, PW, Zaborov, D, Zepeda, A, and Zhou, H

Abstract

We describe measurements of GeV and TeV cosmic rays with the High-Altitude Water Cherenkov Gamma-Ray Observatory, or HAWC. The measurements include the observation of the shadow of the moon; the observation of small-scale and large-scale angular clustering of the TeV cosmic rays; the prospects for measurement of transient solar events with HAWC; and the observation of Forbush decreases with the HAWC engineering array and HAWC-30.

Published
2017

20. The HAWC Gamma-Ray Observatory: Dark Matter, Cosmology, and Fundamental Physics

Author

Collaboration, HAWC, Abeysekara, AU, Alfaro, R, Alvarez, C, Álvarez, JD, Arceo, R, Arteaga-Velázquez, JC, Solares, HAA, Barber, AS, Baughman, BM, Bautista-Elivar, N, Belmont, E, BenZvi, SY, Berley, D, Rosales, MB, Braun, J, Caballero-Lopez, RA, Caballero-Mora, KS, Carramiñana, A, Castillo, M, Cotti, U, Cotzomi, J, Fuente, EDL, León, CD, DeYoung, T, Hernandez, RD, Díaz-Vélez, JC, Dingus, BL, DuVernois, MA, Ellsworth, RW, Fernandez, A, Fiorino, DW, Fraija, N, Galindo, A, Garfias, F, González, LX, González, MM, Goodman, JA, Grabski, V, Gussert, M, Hampel-Arias, Z, Hui, CM, Hüntemeyer, P, Imran, A, Iriarte, A, Karn, P, Kieda, D, Kunde, GJ, Lara, A, Lauer, RJ, Lee, WH, Lennarz, D, Vargas, HL, Linares, EC, Linnemann, JT, Longo, M, Luna-GarcIa, R, Marinelli, A, Martinez, H, Martinez, O, Martínez-Castro, J, Matthews, JAJ, Miranda-Romagnoli, P, Moreno, E, Mostafá, M, Nava, J, Nellen, L, Newbold, M, Noriega-Papaqui, R, Oceguera-Becerra, T, Patricelli, B, Pelayo, R, Pérez-Pérez, EG, Pretz, J, Rivière, C, Rosa-González, D, Salazar, H, Salesa, F, Sanchez, FE, Sandoval, A, Santos, E, Schneider, M, Silich, S, Sinnis, G, Smith, AJ, Sparks, K, Springer, RW, Taboada, I, Toale, PA, Tollefson, K, Torres, I, Ukwatta, TN, Villaseñor, L, Weisgarber, T, Westerhoff, S, Wisher, IG, Wood, J, Yodh, GB, Younk, PW, Zaborov, D, Zepeda, A, Zhou, H, Collaboration, HAWC, Abeysekara, AU, Alfaro, R, Alvarez, C, Álvarez, JD, Arceo, R, Arteaga-Velázquez, JC, Solares, HAA, Barber, AS, Baughman, BM, Bautista-Elivar, N, Belmont, E, BenZvi, SY, Berley, D, Rosales, MB, Braun, J, Caballero-Lopez, RA, Caballero-Mora, KS, Carramiñana, A, Castillo, M, Cotti, U, Cotzomi, J, Fuente, EDL, León, CD, DeYoung, T, Hernandez, RD, Díaz-Vélez, JC, Dingus, BL, DuVernois, MA, Ellsworth, RW, Fernandez, A, Fiorino, DW, Fraija, N, Galindo, A, Garfias, F, González, LX, González, MM, Goodman, JA, Grabski, V, Gussert, M, Hampel-Arias, Z, Hui, CM, Hüntemeyer, P, Imran, A, Iriarte, A, Karn, P, Kieda, D, Kunde, GJ, Lara, A, Lauer, RJ, Lee, WH, Lennarz, D, Vargas, HL, Linares, EC, Linnemann, JT, Longo, M, Luna-GarcIa, R, Marinelli, A, Martinez, H, Martinez, O, Martínez-Castro, J, Matthews, JAJ, Miranda-Romagnoli, P, Moreno, E, Mostafá, M, Nava, J, Nellen, L, Newbold, M, Noriega-Papaqui, R, Oceguera-Becerra, T, Patricelli, B, Pelayo, R, Pérez-Pérez, EG, Pretz, J, Rivière, C, Rosa-González, D, Salazar, H, Salesa, F, Sanchez, FE, Sandoval, A, Santos, E, Schneider, M, Silich, S, Sinnis, G, Smith, AJ, Sparks, K, Springer, RW, Taboada, I, Toale, PA, Tollefson, K, Torres, I, Ukwatta, TN, Villaseñor, L, Weisgarber, T, Westerhoff, S, Wisher, IG, Wood, J, Yodh, GB, Younk, PW, Zaborov, D, Zepeda, A, and Zhou, H

Abstract

The High-Altitude Water Cherenkov Gamma Ray Observatory (HAWC) is designed to perform a synoptic survey of the TeV sky. The high energy coverage of the experiment will enable studies of fundamental physics beyond the Standard Model, and the large field of view of the detector will enable detailed studies of cosmologically significant backgrounds and magnetic fields. We describe the sensitivity of the full HAWC array to these phenomena in five contributions shown at the 33rd International Cosmic Ray Conference in Rio de Janeiro, Brazil (July 2013).

Published
2017

21. The HAWC Gamma-Ray Observatory: Design, Calibration, and Operation

Author

Collaboration, HAWC, Abeysekara, AU, Alfaro, R, Alvarez, C, Álvarez, JD, Arceo, R, Arteaga-Velázquez, JC, Solares, HAA, Barber, AS, Baughman, BM, Bautista-Elivar, N, Belmont, E, BenZvi, SY, Berley, D, Rosales, MB, Braun, J, Caballero-Lopez, RA, Caballero-Mora, KS, Carramiñana, A, Castillo, M, Cotti, U, Cotzomi, J, Fuente, EDL, León, CD, DeYoung, T, Hernandez, RD, Díaz-Vélez, JC, Dingus, BL, DuVernois, MA, Ellsworth, RW, Fernandez, A, Fiorino, DW, Fraija, N, Galindo, A, Garfias, F, González, LX, González, MM, Goodman, JA, Grabski, V, Gussert, M, Hampel-Arias, Z, Hui, CM, Hüntemeyer, P, Imran, A, Iriarte, A, Karn, P, Kieda, D, Kunde, GJ, Lara, A, Lauer, RJ, Lee, WH, Lennarz, D, Vargas, HL, Linares, EC, Linnemann, JT, Longo, M, Luna-GarcIa, R, Marinelli, A, Martinez, H, Martinez, O, Martínez-Castro, J, Matthews, JAJ, Miranda-Romagnoli, P, Moreno, E, Mostafá, M, Nava, J, Nellen, L, Newbold, M, Noriega-Papaqui, R, Oceguera-Becerra, T, Patricelli, B, Pelayo, R, Pérez-Pérez, EG, Pretz, J, Rivière, C, Rosa-González, D, Salazar, H, Salesa, F, Sanchez, FE, Sandoval, A, Santos, E, Schneider, M, Silich, S, Sinnis, G, Smith, AJ, Sparks, K, Springer, RW, Taboada, I, Toale, PA, Tollefson, K, Torres, I, Ukwatta, TN, Villaseñor, L, Weisgarber, T, Westerhoff, S, Wisher, IG, Wood, J, Yodh, GB, Younk, PW, Zaborov, D, Zepeda, A, Zhou, H, Collaboration, HAWC, Abeysekara, AU, Alfaro, R, Alvarez, C, Álvarez, JD, Arceo, R, Arteaga-Velázquez, JC, Solares, HAA, Barber, AS, Baughman, BM, Bautista-Elivar, N, Belmont, E, BenZvi, SY, Berley, D, Rosales, MB, Braun, J, Caballero-Lopez, RA, Caballero-Mora, KS, Carramiñana, A, Castillo, M, Cotti, U, Cotzomi, J, Fuente, EDL, León, CD, DeYoung, T, Hernandez, RD, Díaz-Vélez, JC, Dingus, BL, DuVernois, MA, Ellsworth, RW, Fernandez, A, Fiorino, DW, Fraija, N, Galindo, A, Garfias, F, González, LX, González, MM, Goodman, JA, Grabski, V, Gussert, M, Hampel-Arias, Z, Hui, CM, Hüntemeyer, P, Imran, A, Iriarte, A, Karn, P, Kieda, D, Kunde, GJ, Lara, A, Lauer, RJ, Lee, WH, Lennarz, D, Vargas, HL, Linares, EC, Linnemann, JT, Longo, M, Luna-GarcIa, R, Marinelli, A, Martinez, H, Martinez, O, Martínez-Castro, J, Matthews, JAJ, Miranda-Romagnoli, P, Moreno, E, Mostafá, M, Nava, J, Nellen, L, Newbold, M, Noriega-Papaqui, R, Oceguera-Becerra, T, Patricelli, B, Pelayo, R, Pérez-Pérez, EG, Pretz, J, Rivière, C, Rosa-González, D, Salazar, H, Salesa, F, Sanchez, FE, Sandoval, A, Santos, E, Schneider, M, Silich, S, Sinnis, G, Smith, AJ, Sparks, K, Springer, RW, Taboada, I, Toale, PA, Tollefson, K, Torres, I, Ukwatta, TN, Villaseñor, L, Weisgarber, T, Westerhoff, S, Wisher, IG, Wood, J, Yodh, GB, Younk, PW, Zaborov, D, Zepeda, A, and Zhou, H

Abstract

The High-Altitude Water Cherenkov Gamma Ray Observatory (HAWC) is under construction 4100 meters above sea level at Sierra Negra, Mexico. We describe the design and cabling of the detector, the characterization of the photomultipliers, and the timing calibration system. We also outline a next-generation detector based on the water Cherenkov technique.

Published
2017

22. The HAWC Gamma-Ray Observatory: Sensitivity to Steady and Transient Sources of Gamma Rays

Author

Collaboration, HAWC, Abeysekara, AU, Alfaro, R, Alvarez, C, Álvarez, JD, Arceo, R, Arteaga-Velázquez, JC, Solares, HAA, Barber, AS, Baughman, BM, Bautista-Elivar, N, Belmont, E, BenZvi, SY, Berley, D, Rosales, MB, Braun, J, Caballero-Lopez, RA, Caballero-Mora, KS, Carramiñana, A, Castillo, M, Cotti, U, Cotzomi, J, Fuente, EDL, León, CD, DeYoung, T, Hernandez, RD, Díaz-Vélez, JC, Dingus, BL, DuVernois, MA, Ellsworth, RW, Fernandez, A, Fiorino, DW, Fraija, N, Galindo, A, Garfias, F, González, LX, González, MM, Goodman, JA, Grabski, V, Gussert, M, Hampel-Arias, Z, Hui, CM, Hüntemeyer, P, Imran, A, Iriarte, A, Karn, P, Kieda, D, Kunde, GJ, Lara, A, Lauer, RJ, Lee, WH, Lennarz, D, Vargas, HL, Linares, EC, Linnemann, JT, Longo, M, Luna-GarcIa, R, Marinelli, A, Martinez, H, Martinez, O, Martínez-Castro, J, Matthews, JAJ, Miranda-Romagnoli, P, Moreno, E, Mostafá, M, Nava, J, Nellen, L, Newbold, M, Noriega-Papaqui, R, Oceguera-Becerra, T, Patricelli, B, Pelayo, R, Pérez-Pérez, EG, Pretz, J, Rivière, C, Rosa-González, D, Salazar, H, Salesa, F, Sanchez, FE, Sandoval, A, Santos, E, Schneider, M, Silich, S, Sinnis, G, Smith, AJ, Sparks, K, Springer, RW, Taboada, I, Toale, PA, Tollefson, K, Torres, I, Ukwatta, TN, Villaseñor, L, Weisgarber, T, Westerhoff, S, Wisher, IG, Wood, J, Yodh, GB, Younk, PW, Zaborov, D, Zepeda, A, Zhou, H, Collaboration, HAWC, Abeysekara, AU, Alfaro, R, Alvarez, C, Álvarez, JD, Arceo, R, Arteaga-Velázquez, JC, Solares, HAA, Barber, AS, Baughman, BM, Bautista-Elivar, N, Belmont, E, BenZvi, SY, Berley, D, Rosales, MB, Braun, J, Caballero-Lopez, RA, Caballero-Mora, KS, Carramiñana, A, Castillo, M, Cotti, U, Cotzomi, J, Fuente, EDL, León, CD, DeYoung, T, Hernandez, RD, Díaz-Vélez, JC, Dingus, BL, DuVernois, MA, Ellsworth, RW, Fernandez, A, Fiorino, DW, Fraija, N, Galindo, A, Garfias, F, González, LX, González, MM, Goodman, JA, Grabski, V, Gussert, M, Hampel-Arias, Z, Hui, CM, Hüntemeyer, P, Imran, A, Iriarte, A, Karn, P, Kieda, D, Kunde, GJ, Lara, A, Lauer, RJ, Lee, WH, Lennarz, D, Vargas, HL, Linares, EC, Linnemann, JT, Longo, M, Luna-GarcIa, R, Marinelli, A, Martinez, H, Martinez, O, Martínez-Castro, J, Matthews, JAJ, Miranda-Romagnoli, P, Moreno, E, Mostafá, M, Nava, J, Nellen, L, Newbold, M, Noriega-Papaqui, R, Oceguera-Becerra, T, Patricelli, B, Pelayo, R, Pérez-Pérez, EG, Pretz, J, Rivière, C, Rosa-González, D, Salazar, H, Salesa, F, Sanchez, FE, Sandoval, A, Santos, E, Schneider, M, Silich, S, Sinnis, G, Smith, AJ, Sparks, K, Springer, RW, Taboada, I, Toale, PA, Tollefson, K, Torres, I, Ukwatta, TN, Villaseñor, L, Weisgarber, T, Westerhoff, S, Wisher, IG, Wood, J, Yodh, GB, Younk, PW, Zaborov, D, Zepeda, A, and Zhou, H

Abstract

The High-Altitude Water Cherenkov (HAWC) Gamma-Ray Observatory is designed to record air showers produced by cosmic rays and gamma rays between 100 GeV and 100 TeV. Because of its large field of view and high livetime, HAWC is well-suited to measure gamma rays from extended sources, diffuse emission, and transient sources. We describe the sensitivity of HAWC to emission from the extended Cygnus region as well as other types of galactic diffuse emission; searches for flares from gamma-ray bursts and active galactic nuclei; and the first measurement of the Crab Nebula with HAWC-30.

Published
2017

23. Ultra-high-energy gamma-ray bubble around microquasar V4641 Sgr.

Author

Alfaro R, Alvarez C, Arteaga-Velázquez JC, Avila Rojas D, Ayala Solares HA, Babu R, Belmont-Moreno E, Caballero-Mora KS, Capistrán T, Carramiñana A, Casanova S, Cotti U, Cotzomi J, Coutiño de León S, De la Fuente E, Depaoli D, Di Lalla N, Diaz Hernandez R, Dingus BL, DuVernois MA, Durocher M, Díaz-Vélez JC, Engel K, Espinoza C, Fan KL, Fang K, Fraija N, Fraija S, García-González JA, Garfias F, Gonzalez Muñoz A, González MM, Goodman JA, Groetsch S, Harding JP, Herzog I, Hinton J, Huang D, Hueyotl-Zahuantitla F, Hüntemeyer P, Iriarte A, Joshi V, Kaufmann S, Kieda D, de León C, Lee J, León Vargas H, Linnemann JT, Longinotti AL, Luis-Raya G, Malone K, Martinez O, Martínez-Castro J, Matthews JA, Miranda-Romagnoli P, Morales-Soto JA, Moreno E, Mostafá M, Nayerhoda A, Nellen L, Newbold M, Nisa MU, Noriega-Papaqui R, Olivera-Nieto L, Omodei N, Osorio M, Pérez Araujo Y, Pérez-Pérez EG, Rho CD, Rosa-González D, Ruiz-Velasco E, Salazar H, Salazar-Gallegos D, Sandoval A, Schneider M, Serna-Franco J, Smith AJ, Son Y, Springer RW, Tibolla O, Tollefson K, Torres I, Torres-Escobedo R, Turner R, Ureña-Mena F, Varela E, Villaseñor L, Wang X, Watson IJ, Willox E, Yun-Cárcamo S, and Zhou H

Abstract

Microquasars are laboratories for the study of jets of relativistic particles produced by accretion onto a spinning black hole. Microquasars are near enough to allow detailed imaging of spatial features across the multiwavelength spectrum. The recent extension measurement of the spatial morphology of a microquasar, SS 433, to TeV gamma rays 1 localizes the acceleration of electrons at shocks in the jet far from the black hole 2 . V4641 Sagittarii (V4641 Sgr) is a similar binary system with a black hole and B-type main-sequence companion star and has an orbit period of 2.8 days (refs.  3,4 ). It stands out for its super-Eddington accretion 5 and for its radio jet, which is one of the fastest superluminal jets in the Milky Way. Previous observations of V4641 Sgr did not report gamma-ray emission 6 . Here we report TeV gamma-ray emission from V4641 Sgr that reveals particle acceleration at similar distances from the black hole as SS 433. Furthermore, the gamma-ray spectrum of V4641 Sgr is among the hardest TeV spectra observed from any known gamma-ray source and is detected above 200 TeV. Gamma rays are produced by particles, either electrons or protons, of higher energies. Because energetic electrons lose energy more quickly the higher their energy, such a spectrum either very strongly constrains the electron-production mechanism or points to the acceleration of high-energy protons. This suggests that large-scale jets from microquasars could be more common than previously expected and that they could be a notable source of galactic cosmic rays 7-9 ., (© 2024. The Author(s), under exclusive licence to Springer Nature Limited.)

Published
2024
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24. Discovery of Gamma Rays from the Quiescent Sun with HAWC.

Author

Albert A, Alfaro R, Alvarez C, Arteaga-Velázquez JC, Avila Rojas D, Ayala Solares HA, Babu R, Belmont-Moreno E, Brisbois C, Caballero-Mora KS, Capistrán T, Carramiñana A, Casanova S, Chaparro-Amaro O, Cotti U, Cotzomi J, Coutiño de León S, De la Fuente E, Diaz Hernandez R, Dingus BL, DuVernois MA, Durocher M, Díaz-Vélez JC, Ellsworth RW, Engel K, Espinoza C, Fan KL, Fang K, Fernández Alonso M, Fleischhack H, Fraija N, García-González JA, Garfias F, González MM, Goodman JA, Harding JP, Hernandez S, Hinton J, Huang D, Hueyotl-Zahuantitla F, Hüntemeyer P, Iriarte A, Joshi V, Kaufmann S, Lee J, Linnemann JT, Longinotti AL, Luis-Raya G, Malone K, Martinez O, Martínez-Castro J, Matthews JA, Miranda-Romagnoli P, Morales-Soto JA, Moreno E, Mostafá M, Nayerhoda A, Nellen L, Nisa MU, Noriega-Papaqui R, Olivera-Nieto L, Omodei N, Pérez Araujo Y, Pérez-Pérez EG, Rho CD, Rosa-González D, Ruiz-Velasco E, Salazar H, Salazar-Gallegos D, Sandoval A, Schneider M, Serna-Franco J, Smith AJ, Son Y, Springer RW, Tibolla O, Tollefson K, Torres I, Torres-Escobedo R, Turner R, Ureña-Mena F, Varela E, Villaseñor L, Wang X, Watson IJ, Willox E, Yun-Cárcamo S, Zhou H, de León C, Beacom JF, Linden T, Ng KCY, Peter AHG, and Zhou B

Abstract

We report the first detection of a TeV γ-ray flux from the solar disk (6.3σ), based on 6.1 years of data from the High Altitude Water Cherenkov (HAWC) observatory. The 0.5-2.6 TeV spectrum is well fit by a power law, dN/dE=A(E/1  TeV)^{-γ}, with A=(1.6±0.3)×10^{-12}  TeV^{-1} cm^{-2} s^{-1} and γ=3.62±0.14. The flux shows a strong indication of anticorrelation with solar activity. These results extend the bright, hard GeV emission from the disk observed with Fermi-LAT, seemingly due to hadronic Galactic cosmic rays showering on nuclei in the solar atmosphere. However, current theoretical models are unable to explain the details of how solar magnetic fields shape these interactions. HAWC's TeV detection thus deepens the mysteries of the solar-disk emission.

Published
2023
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25. Limits to Gauge Coupling in the Dark Sector Set by the Nonobservation of Instanton-Induced Decay of Super-Heavy Dark Matter in the Pierre Auger Observatory Data.

Author

Abreu P, Aglietta M, Albury JM, Allekotte I, Almeida Cheminant K, Almela A, Aloisio R, Alvarez-Muñiz J, Alves Batista R, Ammerman Yebra J, Anastasi GA, Anchordoqui L, Andrada B, Andringa S, Aramo C, Araújo Ferreira PR, Arnone E, Arteaga Velázquez JC, Asorey H, Assis P, Avila G, Avocone E, Badescu AM, Bakalova A, Balaceanu A, Barbato F, Bellido JA, Berat C, Bertaina ME, Bhatta G, Biermann PL, Binet V, Bismark K, Bister T, Biteau J, Blazek J, Bleve C, Blümer J, Boháčová M, Boncioli D, Bonifazi C, Bonneau Arbeletche L, Borodai N, Botti AM, Brack J, Bretz T, Brichetto Orchera PG, Briechle FL, Buchholz P, Bueno A, Buitink S, Buscemi M, Büsken M, Caballero-Mora KS, Caccianiga L, Canfora F, Caracas I, Caruso R, Castellina A, Catalani F, Cataldi G, Cazon L, Cerda M, Chinellato JA, Chudoba J, Chytka L, Clay RW, Cobos Cerutti AC, Colalillo R, Coleman A, Coluccia MR, Conceição R, Condorelli A, Consolati G, Contreras F, Convenga F, Correia Dos Santos D, Covault CE, Dasso S, Daumiller K, Dawson BR, Day JA, de Almeida RM, de Jesús J, de Jong SJ, de Mello Neto JRT, De Mitri I, de Oliveira J, de Oliveira Franco D, de Palma F, de Souza V, De Vito E, Del Popolo A, Del Río M, Deligny O, Deval L, di Matteo A, Dobre M, Dobrigkeit C, D'Olivo JC, Domingues Mendes LM, Dos Anjos RC, Dova MT, Ebr J, Engel R, Epicoco I, Erdmann M, Escobar CO, Etchegoyen A, Falcke H, Farmer J, Farrar G, Fauth AC, Fazzini N, Feldbusch F, Fenu F, Fick B, Figueira JM, Filipčič A, Fitoussi T, Fodran T, Fujii T, Fuster A, Galea C, Galelli C, García B, Garcia Vegas AL, Gemmeke H, Gesualdi F, Gherghel-Lascu A, Ghia PL, Giaccari U, Giammarchi M, Glombitza J, Gobbi F, Gollan F, Golup G, Gómez Berisso M, Gómez Vitale PF, Gongora JP, González JM, González N, Goos I, Góra D, Gorgi A, Gottowik M, Grubb TD, Guarino F, Guedes GP, Guido E, Hahn S, Hamal P, Hampel MR, Hansen P, Harari D, Harvey VM, Haungs A, Hebbeker T, Heck D, Hill GC, Hojvat C, Hörandel JR, Horvath P, Hrabovský M, Huege T, Insolia A, Isar PG, Janecek P, Johnsen JA, Jurysek J, Kääpä A, Kampert KH, Keilhauer B, Khakurdikar A, Kizakke Covilakam VV, Klages HO, Kleifges M, Kleinfeller J, Knapp F, Kunka N, Lago BL, Langner N, Leigui de Oliveira MA, Lenok V, Letessier-Selvon A, Lhenry-Yvon I, Lo Presti D, Lopes L, López R, Lu L, Luce Q, Lundquist JP, Machado Payeras A, Mancarella G, Mandat D, Manning BC, Manshanden J, Mantsch P, Marafico S, Mariani FM, Mariazzi AG, Mariş IC, Marsella G, Martello D, Martinelli S, Martínez Bravo O, Mastrodicasa M, Mathes HJ, Matthews J, Matthiae G, Mayotte E, Mayotte S, Mazur PO, Medina-Tanco G, Melo D, Menshikov A, Michal S, Micheletti MI, Miramonti L, Mollerach S, Montanet F, Morejon L, Morello C, Mostafá M, Müller AL, Muller MA, Mulrey K, Mussa R, Muzio M, Namasaka WM, Nasr-Esfahani A, Nellen L, Nicora G, Niculescu-Oglinzanu M, Niechciol M, Nitz D, Norwood I, Nosek D, Novotny V, Nožka L, Nucita A, Núñez LA, Oliveira C, Palatka M, Pallotta J, Papenbreer P, Parente G, Parra A, Pawlowsky J, Pech M, Pękala J, Pelayo R, Peña-Rodriguez J, Pereira Martins EE, Perez Armand J, Pérez Bertolli C, Perrone L, Petrera S, Petrucci C, Pierog T, Pimenta M, Pirronello V, Platino M, Pont B, Pothast M, Privitera P, Prouza M, Puyleart A, Querchfeld S, Rautenberg J, Ravignani D, Reininghaus M, Ridky J, Riehn F, Risse M, Rizi V, Rodrigues de Carvalho W, Rodriguez Rojo J, Roncoroni MJ, Rossoni S, Roth M, Roulet E, Rovero AC, Ruehl P, Saftoiu A, Saharan M, Salamida F, Salazar H, Salina G, Sanabria Gomez JD, Sánchez F, Santos EM, Santos E, Sarazin F, Sarmento R, Sarmiento-Cano C, Sato R, Savina P, Schäfer CM, Scherini V, Schieler H, Schimassek M, Schimp M, Schlüter F, Schmidt D, Scholten O, Schoorlemmer H, Schovánek P, Schröder FG, Schulte J, Schulz T, Sciutto SJ, Scornavacche M, Segreto A, Sehgal S, Shellard RC, Sigl G, Silli G, Sima O, Smau R, Šmída R, Sommers P, Soriano JF, Squartini R, Stadelmaier M, Stanca D, Stanič S, Stasielak J, Stassi P, Streich A, Suárez-Durán M, Sudholz T, Suomijärvi T, Supanitsky AD, Szadkowski Z, Tapia A, Taricco C, Timmermans C, Tkachenko O, Tobiska P, Todero Peixoto CJ, Tomé B, Torrès Z, Travaini A, Travnicek P, Trimarelli C, Tueros M, Ulrich R, Unger M, Vaclavek L, Vacula M, Valdés Galicia JF, Valore L, Varela E, Vásquez-Ramírez A, Veberič D, Ventura C, Vergara Quispe ID, Verzi V, Vicha J, Vink J, Vorobiov S, Wahlberg H, Watanabe C, Watson AA, Weindl A, Wiencke L, Wilczyński H, Wittkowski D, Wundheiler B, Yushkov A, Zapparrata O, Zas E, Zavrtanik D, Zavrtanik M, and Zehrer L

Abstract

Instantons, which are nonperturbative solutions to Yang-Mills equations, provide a signal for the occurrence of quantum tunneling between distinct classes of vacua. They can give rise to decays of particles otherwise forbidden. Using data collected at the Pierre Auger Observatory, we search for signatures of such instanton-induced processes that would be suggestive of super-heavy particles decaying in the Galactic halo. These particles could have been produced during the post-inflationary epoch and match the relic abundance of dark matter inferred today. The nonobservation of the signatures searched for allows us to derive a bound on the reduced coupling constant of gauge interactions in the dark sector: α&#95;{X}≲0.09, for 10^{9}≲M&#95;{X}/GeV<10^{19}. Conversely, we obtain that, for instance, a reduced coupling constant α&#95;{X}=0.09 excludes masses M&#95;{X}≳3×10^{13}  GeV. In the context of dark matter production from gravitational interactions alone, we illustrate how these bounds are complementary to those obtained on the Hubble rate at the end of inflation from the nonobservation of tensor modes in the cosmological microwave background.

Published
2023
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26. Constraints on Lorentz Invariance Violation from HAWC Observations of Gamma Rays above 100 TeV.

Author

Albert A, Alfaro R, Alvarez C, Angeles Camacho JR, Arteaga-Velázquez JC, Arunbabu KP, Avila Rojas D, Ayala Solares HA, Baghmanyan V, Belmont-Moreno E, BenZvi SY, Brisbois C, Caballero-Mora KS, Capistrán T, Carramiñana A, Casanova S, Cotti U, Cotzomi J, Coutiño de León S, De la Fuente E, de León C, Dingus BL, DuVernois MA, Díaz-Vélez JC, Ellsworth RW, Engel K, Espinoza C, Fleischhack H, Fraija N, Galván-Gámez A, Garcia D, García-González JA, Garfias F, González MM, Goodman JA, Harding JP, Hernandez S, Hona B, Huang D, Hueyotl-Zahuantitla F, Hüntemeyer P, Iriarte A, Joshi V, Lara A, Lee WH, León Vargas H, Linnemann JT, Longinotti AL, Luis-Raya G, Lundeen J, López-Coto R, Malone K, Marinelli SS, Martinez-Castellanos I, Martínez-Castro J, Martínez-Huerta H, Matthews JA, Miranda-Romagnoli P, Morales-Soto JA, Moreno E, Nayerhoda A, Nellen L, Newbold M, Nisa MU, Noriega-Papaqui R, Omodei N, Peisker A, Pérez-Pérez EG, Rho CD, Rivière C, Rosa-González D, Rosenberg M, Ruiz-Velasco E, Salazar H, Salesa Greus F, Sandoval A, Schneider M, Schoorlemmer H, Sinnis G, Smith AJ, Springer RW, Surajbali P, Tabachnick E, Tanner M, Tibolla O, Tollefson K, Torres I, Torres-Escobedo R, Weisgarber T, Yodh G, Zepeda A, and Zhou H

Abstract

Because of the high energies and long distances to the sources, astrophysical observations provide a unique opportunity to test possible signatures of Lorentz invariance violation (LIV). Superluminal LIV enables the decay of photons at high energy. The high altitude water Cherenkov (HAWC) observatory is among the most sensitive gamma-ray instruments currently operating above 10 TeV. HAWC finds evidence of 100 TeV photon emission from at least four astrophysical sources. These observations exclude, for the strongest of the limits set, the LIV energy scale to 2.2×10^{31}  eV, over 1800 times the Planck energy and an improvement of 1 to 2 orders of magnitude over previous limits.

Published
2020
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27. Multiple Galactic Sources with Emission Above 56 TeV Detected by HAWC.

Author

Abeysekara AU, Albert A, Alfaro R, Angeles Camacho JR, Arteaga-Velázquez JC, Arunbabu KP, Avila Rojas D, Ayala Solares HA, Baghmanyan V, Belmont-Moreno E, BenZvi SY, Brisbois C, Caballero-Mora KS, Capistrán T, Carramiñana A, Casanova S, Cotti U, Cotzomi J, Coutiño de León S, De la Fuente E, de León C, Dichiara S, Dingus BL, DuVernois MA, Díaz-Vélez JC, Ellsworth RW, Engel K, Espinoza C, Fleischhack H, Fraija N, Galván-Gámez A, Garcia D, García-González JA, Garfias F, González MM, Goodman JA, Harding JP, Hernandez S, Hinton J, Hona B, Huang D, Hueyotl-Zahuantitla F, Hüntemeyer P, Iriarte A, Jardin-Blicq A, Joshi V, Kaufmann S, Kieda D, Lara A, Lee WH, León Vargas H, Linnemann JT, Longinotti AL, Luis-Raya G, Lundeen J, López-Coto R, Malone K, Marinelli SS, Martinez O, Martinez-Castellanos I, Martínez-Castro J, Martínez-Huerta H, Matthews JA, Miranda-Romagnoli P, Morales-Soto JA, Moreno E, Mostafá M, Nayerhoda A, Nellen L, Newbold M, Nisa MU, Noriega-Papaqui R, Peisker A, Pérez-Pérez EG, Pretz J, Ren Z, Rho CD, Rivière C, Rosa-González D, Rosenberg M, Ruiz-Velasco E, Salesa Greus F, Sandoval A, Schneider M, Schoorlemmer H, Sinnis G, Smith AJ, Springer RW, Surajbali P, Tabachnick E, Tanner M, Tibolla O, Tollefson K, Torres I, Torres-Escobedo R, Villaseñor L, Weisgarber T, Wood J, Yapici T, Zhang H, and Zhou H

Abstract

We present the first catalog of gamma-ray sources emitting above 56 and 100 TeV with data from the High Altitude Water Cherenkov Observatory, a wide field-of-view observatory capable of detecting gamma rays up to a few hundred TeV. Nine sources are observed above 56 TeV, all of which are likely galactic in origin. Three sources continue emitting past 100 TeV, making this the highest-energy gamma-ray source catalog to date. We report the integral flux of each of these objects. We also report spectra for three highest-energy sources and discuss the possibility that they are PeVatrons.

Published
2020
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28. Publisher Correction: Very-high-energy particle acceleration powered by the jets of the microquasar SS 433.

Author

Abeysekara AU, Albert A, Alfaro R, Alvarez C, Álvarez JD, Arceo R, Arteaga-Velázquez JC, Avila Rojas D, Ayala Solares HA, Belmont-Moreno E, BenZvi SY, Brisbois C, Caballero-Mora KS, Capistrán T, Carramiñana A, Casanova S, Castillo M, Cotti U, Cotzomi J, Coutiño de León S, De León C, De la Fuente E, Díaz-Vélez JC, Dichiara S, Dingus BL, DuVernois MA, Ellsworth RW, Engel K, Espinoza C, Fang K, Fleischhack H, Fraija N, Galván-Gámez A, García-González JA, Garfias F, González-Muñoz A, González MM, Goodman JA, Hampel-Arias Z, Harding JP, Hernandez S, Hinton J, Hona B, Hueyotl-Zahuantitla F, Hui CM, Hüntemeyer P, Iriarte A, Jardin-Blicq A, Joshi V, Kaufmann S, Kar P, Kunde GJ, Lauer RJ, Lee WH, León Vargas H, Li H, Linnemann JT, Longinotti AL, Luis-Raya G, López-Coto R, Malone K, Marinelli SS, Martinez O, Martinez-Castellanos I, Martínez-Castro J, Matthews JA, Miranda-Romagnoli P, Moreno E, Mostafá M, Nayerhoda A, Nellen L, Newbold M, Nisa MU, Noriega-Papaqui R, Pretz J, Pérez-Pérez EG, Ren Z, Rho CD, Rivière C, Rosa-González D, Rosenberg M, Ruiz-Velasco E, Salesa Greus F, Sandoval A, Schneider M, Schoorlemmer H, Seglar Arroyo M, Sinnis G, Smith AJ, Springer RW, Surajbali P, Taboada I, Tibolla O, Tollefson K, Torres I, Vianello G, Villaseñor L, Weisgarber T, Werner F, Westerhoff S, Wood J, Yapici T, Yodh G, Zepeda A, Zhang H, and Zhou H

Abstract

In this Letter, owing to a production error, the penultimate version of the PDF was published. The HTML version was always correct. The PDF has been corrected online.

Published
2018
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29. Very-high-energy particle acceleration powered by the jets of the microquasar SS 433.

Author

Abeysekara AU, Albert A, Alfaro R, Alvarez C, Álvarez JD, Arceo R, Arteaga-Velázquez JC, Avila Rojas D, Ayala Solares HA, Belmont-Moreno E, BenZvi SY, Brisbois C, Caballero-Mora KS, Capistrán T, Carramiñana A, Casanova S, Castillo M, Cotti U, Cotzomi J, Coutiño de León S, De León C, De la Fuente E, Díaz-Vélez JC, Dichiara S, Dingus BL, DuVernois MA, Ellsworth RW, Engel K, Espinoza C, Fang K, Fleischhack H, Fraija N, Galván-Gámez A, García-González JA, Garfias F, González-Muñoz A, González MM, Goodman JA, Hampel-Arias Z, Harding JP, Hernandez S, Hinton J, Hona B, Hueyotl-Zahuantitla F, Hui CM, Hüntemeyer P, Iriarte A, Jardin-Blicq A, Joshi V, Kaufmann S, Kar P, Kunde GJ, Lauer RJ, Lee WH, León Vargas H, Li H, Linnemann JT, Longinotti AL, Luis-Raya G, López-Coto R, Malone K, Marinelli SS, Martinez O, Martinez-Castellanos I, Martínez-Castro J, Matthews JA, Miranda-Romagnoli P, Moreno E, Mostafá M, Nayerhoda A, Nellen L, Newbold M, Nisa MU, Noriega-Papaqui R, Pretz J, Pérez-Pérez EG, Ren Z, Rho CD, Rivière C, Rosa-González D, Rosenberg M, Ruiz-Velasco E, Salesa Greus F, Sandoval A, Schneider M, Schoorlemmer H, Seglar Arroyo M, Sinnis G, Smith AJ, Springer RW, Surajbali P, Taboada I, Tibolla O, Tollefson K, Torres I, Vianello G, Villaseñor L, Weisgarber T, Werner F, Westerhoff S, Wood J, Yapici T, Yodh G, Zepeda A, Zhang H, and Zhou H

Abstract

SS 433 is a binary system containing a supergiant star that is overflowing its Roche lobe with matter accreting onto a compact object (either a black hole or neutron star) 1-3 . Two jets of ionized matter with a bulk velocity of approximately 0.26c (where c is the speed of light in vacuum) extend from the binary, perpendicular to the line of sight, and terminate inside W50, a supernova remnant that is being distorted by the jets 2,4-8 . SS 433 differs from other microquasars (small-scale versions of quasars that are present within our own Galaxy) in that the accretion is believed to be super-Eddington 9-11 , and the luminosity of the system is about 10 40 ergs per second 2,9,12,13 . The lobes of W50 in which the jets terminate, about 40 parsecs from the central source, are expected to accelerate charged particles, and indeed radio and X-ray emission consistent with electron synchrotron emission in a magnetic field have been observed 14-16 . At higher energies (greater than 100 gigaelectronvolts), the particle fluxes of γ-rays from X-ray hotspots around SS 433 have been reported as flux upper limits 6,17-20 . In this energy regime, it has been unclear whether the emission is dominated by electrons that are interacting with photons from the cosmic microwave background through inverse-Compton scattering or by protons that are interacting with the ambient gas. Here we report teraelectronvolt γ-ray observations of the SS 433/W50 system that spatially resolve the lobes. The teraelectronvolt emission is localized to structures in the lobes, far from the centre of the system where the jets are formed. We have measured photon energies of at least 25 teraelectronvolts, and these are certainly not Doppler-boosted, because of the viewing geometry. We conclude that the emission-from radio to teraelectronvolt energies-is consistent with a single population of electrons with energies extending to at least hundreds of teraelectronvolts in a magnetic field of about 16 microgauss.

Published
2018
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30. Extended gamma-ray sources around pulsars constrain the origin of the positron flux at Earth.

Author

Abeysekara AU, Albert A, Alfaro R, Alvarez C, Álvarez JD, Arceo R, Arteaga-Velázquez JC, Avila Rojas D, Ayala Solares HA, Barber AS, Bautista-Elivar N, Becerril A, Belmont-Moreno E, BenZvi SY, Berley D, Bernal A, Braun J, Brisbois C, Caballero-Mora KS, Capistrán T, Carramiñana A, Casanova S, Castillo M, Cotti U, Cotzomi J, Coutiño de León S, De León C, De la Fuente E, Dingus BL, DuVernois MA, Díaz-Vélez JC, Ellsworth RW, Engel K, Enríquez-Rivera O, Fiorino DW, Fraija N, García-González JA, Garfias F, Gerhardt M, González Muñoz A, González MM, Goodman JA, Hampel-Arias Z, Harding JP, Hernández S, Hernández-Almada A, Hinton J, Hona B, Hui CM, Hüntemeyer P, Iriarte A, Jardin-Blicq A, Joshi V, Kaufmann S, Kieda D, Lara A, Lauer RJ, Lee WH, Lennarz D, Vargas HL, Linnemann JT, Longinotti AL, Luis Raya G, Luna-García R, López-Coto R, Malone K, Marinelli SS, Martinez O, Martinez-Castellanos I, Martínez-Castro J, Martínez-Huerta H, Matthews JA, Miranda-Romagnoli P, Moreno E, Mostafá M, Nellen L, Newbold M, Nisa MU, Noriega-Papaqui R, Pelayo R, Pretz J, Pérez-Pérez EG, Ren Z, Rho CD, Rivière C, Rosa-González D, Rosenberg M, Ruiz-Velasco E, Salazar H, Salesa Greus F, Sandoval A, Schneider M, Schoorlemmer H, Sinnis G, Smith AJ, Springer RW, Surajbali P, Taboada I, Tibolla O, Tollefson K, Torres I, Ukwatta TN, Vianello G, Weisgarber T, Westerhoff S, Wisher IG, Wood J, Yapici T, Yodh G, Younk PW, Zepeda A, Zhou H, Guo F, Hahn J, Li H, and Zhang H

Abstract

The unexpectedly high flux of cosmic-ray positrons detected at Earth may originate from nearby astrophysical sources, dark matter, or unknown processes of cosmic-ray secondary production. We report the detection, using the High-Altitude Water Cherenkov Observatory (HAWC), of extended tera-electron volt gamma-ray emission coincident with the locations of two nearby middle-aged pulsars (Geminga and PSR B0656+14). The HAWC observations demonstrate that these pulsars are indeed local sources of accelerated leptons, but the measured tera-electron volt emission profile constrains the diffusion of particles away from these sources to be much slower than previously assumed. We demonstrate that the leptons emitted by these objects are therefore unlikely to be the origin of the excess positrons, which may have a more exotic origin., (Copyright © 2017, American Association for the Advancement of Science.)

Published
2017
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31. First Experimental Characterization of Microwave Emission from Cosmic Ray Air Showers.

Author

Smída R, Werner F, Engel R, Arteaga-Velázquez JC, Bekk K, Bertaina M, Blümer J, Bozdog H, Brancus IM, Chiavassa A, Cossavella F, Di Pierro F, Doll P, Fuchs B, Fuhrmann D, Grupen C, Haungs A, Heck D, Hörandel JR, Huber D, Huege T, Kampert KH, Kang D, Klages H, Kleifges M, Krömer O, Link K, Luczak P, Ludwig M, Mathes HJ, Mathys S, Mayer HJ, Melissas M, Morello C, Neunteufel P, Oehlschläger J, Palmieri N, Pekala J, Pierog T, Rautenberg J, Rebel H, Riegel M, Roth M, Salamida F, Schieler H, Schoo S, Schröder FG, Sima O, Stasielak J, Toma G, Trinchero GC, Unger M, Weber M, Weindl A, Wilczyński H, Will M, Wochele J, and Zabierowski J

Abstract

We report the first direct measurement of the overall characteristics of microwave radio emission from extensive air showers. Using a trigger provided by the KASCADE-Grande air shower array, the signals of the microwave antennas of the Cosmic-Ray Observation via Microwave Emission experiment have been read out and searched for signatures of radio emission by high-energy air showers in the GHz frequency range. Microwave signals have been detected for more than 30 showers with energies above 3×10^{16}  eV. The observations presented in this Letter are consistent with a mainly forward-directed and polarized emission process in the GHz frequency range. The measurements show that microwave radiation offers a new means of studying air showers at E≥10^{17}  eV.

Published
2014
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32. Kneelike structure in the spectrum of the heavy component of cosmic rays observed with KASCADE-Grande.

Author

Apel WD, Arteaga-Velázquez JC, Bekk K, Bertaina M, Blümer J, Bozdog H, Brancus IM, Buchholz P, Cantoni E, Chiavassa A, Cossavella F, Daumiller K, de Souza V, Di Pierro F, Doll P, Engel R, Engler J, Finger M, Fuhrmann D, Ghia PL, Gils HJ, Glasstetter R, Grupen C, Haungs A, Heck D, Hörandel JR, Huber D, Huege T, Isar PG, Kampert KH, Kang D, Klages HO, Link K, Łuczak P, Ludwig M, Mathes HJ, Mayer HJ, Melissas M, Milke J, Mitrica B, Morello C, Navarra G, Oehlschläger J, Ostapchenko S, Over S, Palmieri N, Petcu M, Pierog T, Rebel H, Roth M, Schieler H, Schröder FG, Sima O, Toma G, Trinchero GC, Ulrich H, Weindl A, Wochele J, Wommer M, and Zabierowski J

Abstract

We report the observation of a steepening in the cosmic ray energy spectrum of heavy primary particles at about 8×10(16) eV. This structure is also seen in the all-particle energy spectrum, but is less significant. Whereas the "knee" of the cosmic ray spectrum at 3-5×10(15) eV was assigned to light primary masses by the KASCADE experiment, the new structure found by the KASCADE-Grande experiment is caused by heavy primaries. The result is obtained by independent measurements of the charged particle and muon components of the secondary particles of extensive air showers in the primary energy range of 10(16) to 10(18) eV. The data are analyzed on a single-event basis taking into account also the correlation of the two observables., (© 2011 American Physical Society)

Published
2011
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