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1. 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

2. 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

3. 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

4. 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

5. Search for n-n ¯ oscillation in Super-Kamiokande SEARCH FOR n-n ¯ OSCILLATION IN SUPER-⋯ K. ABE et al.

Author

Abe, K, Hayato, Y, Iida, T, Ishihara, K, Kameda, J, Koshio, Y, Minamino, A, Mitsuda, C, Miura, M, Moriyama, S, Nakahata, M, Obayashi, Y, Ogawa, H, Sekiya, H, Shiozawa, M, Suzuki, Y, Takeda, A, Takeuchi, Y, Ueshima, K, Watanabe, H, Higuchi, I, Ishihara, C, Ishitsuka, M, Kajita, T, Kaneyuki, K, Mitsuka, G, Nakayama, S, Nishino, H, Okumura, K, Saji, C, Takenaga, Y, Clark, S, Desai, S, Dufour, F, Herfurth, A, Kearns, E, Likhoded, S, Litos, M, Raaf, JL, Stone, JL, Sulak, LR, Wang, W, Goldhaber, M, Casper, D, Cravens, JP, Dunmore, J, Griskevich, J, Kropp, WR, Liu, DW, Mine, S, Regis, C, Smy, MB, Sobel, HW, Vagins, MR, Ganezer, KS, Hartfiel, B, Hill, J, Keig, WE, Jang, JS, Jeoung, IS, Kim, JY, Lim, IT, Scholberg, K, Tanimoto, N, Walter, CW, Wendell, R, Ellsworth, RW, Tasaka, S, Guillian, G, Learned, JG, Matsuno, S, Messier, MD, Ichikawa, AK, Ishida, T, Ishii, T, Iwashita, T, Kobayashi, T, Nakadaira, T, Nakamura, K, Nishikawa, K, Nitta, K, Oyama, Y, Suzuki, AT, Hasegawa, M, Maesaka, H, Nakaya, T, Sasaki, T, Sato, H, Tanaka, H, Yamamoto, S, Yokoyama, M, Haines, TJ, Dazeley, S, Hatakeyama, S, Svoboda, R, Sullivan, GW, Gran, R, Habig, A, Fukuda, Y, and Itow, Y

Subjects
hep-ex, Nuclear & Particles Physics, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Quantum Physics, Atomic, Molecular, Nuclear, Particle and Plasma Physics
Abstract

A search for neutron-antineutron (n-n¯) oscillation was undertaken in Super-Kamiokande using the 1489 live-day or 2.45×1034 neutron-year exposure data. This process violates both baryon and baryon minus lepton numbers by an absolute value of two units and is predicted by a large class of hypothetical models where the seesaw mechanism is incorporated to explain the observed tiny neutrino masses and the matter-antimatter asymmetry in the Universe. No evidence for n-n¯ oscillation was found; the lower limit of the lifetime for neutrons bound in O16, in an analysis that included all of the significant sources of experimental uncertainties, was determined to be 1.9×1032years at the 90% confidence level. The corresponding lower limit for the oscillation time of free neutrons was calculated to be 2.7×108s using a theoretical value of the nuclear suppression factor of 0.517×1023s-1 and its uncertainty.

Published
2015

6. Search for n−n¯ oscillation in Super-Kamiokande

Author

Abe, K, Hayato, Y, Iida, T, Ishihara, K, Kameda, J, Koshio, Y, Minamino, A, Mitsuda, C, Miura, M, Moriyama, S, Nakahata, M, Obayashi, Y, Ogawa, H, Sekiya, H, Shiozawa, M, Suzuki, Y, Takeda, A, Takeuchi, Y, Ueshima, K, Watanabe, H, Higuchi, I, Ishihara, C, Ishitsuka, M, Kajita, T, Kaneyuki, K, Mitsuka, G, Nakayama, S, Nishino, H, Okumura, K, Saji, C, Takenaga, Y, Clark, S, Desai, S, Dufour, F, Herfurth, A, Kearns, E, Likhoded, S, Litos, M, Raaf, JL, Stone, JL, Sulak, LR, Wang, W, Goldhaber, M, Casper, D, Cravens, JP, Dunmore, J, Griskevich, J, Kropp, WR, Liu, DW, Mine, S, Regis, C, Smy, MB, Sobel, HW, Vagins, MR, Ganezer, KS, Hartfiel, B, Hill, J, Keig, WE, Jang, JS, Jeoung, IS, Kim, JY, Lim, IT, Scholberg, K, Tanimoto, N, Walter, CW, Wendell, R, Ellsworth, RW, Tasaka, S, Guillian, G, Learned, JG, Matsuno, S, Messier, MD, Ichikawa, AK, Ishida, T, Ishii, T, Iwashita, T, Kobayashi, T, Nakadaira, T, Nakamura, K, Nishikawa, K, Nitta, K, Oyama, Y, Suzuki, AT, Hasegawa, M, Maesaka, H, Nakaya, T, Sasaki, T, Sato, H, Tanaka, H, Yamamoto, S, Yokoyama, M, Haines, TJ, Dazeley, S, Hatakeyama, S, Svoboda, R, Sullivan, GW, Gran, R, Habig, A, Fukuda, Y, and Itow, Y

Subjects
Nuclear and Plasma Physics, Particle and High Energy Physics, Physical Sciences, hep-ex, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Quantum Physics, Nuclear & Particles Physics, Mathematical physics, Astronomical sciences, Particle and high energy physics
Abstract

A search for neutron-antineutron (n-n¯) oscillation was undertaken in Super-Kamiokande using the 1489 live-day or 2.45×1034 neutron-year exposure data. This process violates both baryon and baryon minus lepton numbers by an absolute value of two units and is predicted by a large class of hypothetical models where the seesaw mechanism is incorporated to explain the observed tiny neutrino masses and the matter-antimatter asymmetry in the Universe. No evidence for n-n¯ oscillation was found; the lower limit of the lifetime for neutrons bound in O16, in an analysis that included all of the significant sources of experimental uncertainties, was determined to be 1.9×1032years at the 90% confidence level. The corresponding lower limit for the oscillation time of free neutrons was calculated to be 2.7×108s using a theoretical value of the nuclear suppression factor of 0.517×1023s-1 and its uncertainty.

Published
2015

7. 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

8. 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

9. 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

10. 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

11. 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

12. Observation of the cosmic-ray shadow of the Moon with IceCube

Author

Aartsen, MG, Abbasi, R, Abdou, Y, Ackermann, M, Adams, J, Aguilar, JA, Ahlers, M, Altmann, D, Auffenberg, J, Bai, X, Baker, M, Barwick, SW, Baum, V, Bay, R, Beatty, JJ, Bechet, S, Tjus, J Becker, Becker, K-H, Bell, M, Benabderrahmane, ML, BenZvi, S, Berdermann, J, Berghaus, P, Berley, D, Bernardini, E, Bernhard, A, Bertrand, D, Besson, DZ, Binder, G, Bindig, D, Bissok, M, Blaufuss, E, Blumenthal, J, Boersma, DJ, Bohaichuk, S, Bohm, C, Bose, D, Böser, S, Botner, O, Brayeur, L, Bretz, H-P, Brown, AM, Bruijn, R, Brunner, J, Carson, M, Casey, J, Casier, M, Chirkin, D, Christov, A, Christy, B, Clark, K, Clevermann, F, Coenders, S, Cohen, S, Cowen, DF, Silva, AH Cruz, Danninger, M, Daughhetee, J, Davis, JC, De Clercq, C, De Ridder, S, Desiati, P, de With, M, DeYoung, T, Díaz-Vélez, JC, Dunkman, M, Eagan, R, Eberhardt, B, Eisch, J, Ellsworth, RW, Euler, S, Evenson, PA, Fadiran, O, Fazely, AR, Fedynitch, A, Feintzeig, J, Feusels, T, Filimonov, K, Finley, C, Fischer-Wasels, T, Flis, S, Franckowiak, A, Franke, R, Frantzen, K, Fuchs, T, Gaisser, TK, Gallagher, J, Gerhardt, L, Gladstone, L, Glüsenkamp, T, Goldschmidt, A, Golup, G, Gonzalez, JG, Goodman, JA, Góra, D, Grandmont, DT, Grant, D, Groß, A, Ha, C, and Ismail, A Haj

Subjects
Particle and High Energy Physics, Physical Sciences, astro-ph.HE
Abstract

We report on the observation of a significant deficit of cosmic rays from the direction of the Moon with the IceCube detector. The study of this "Moon shadow" is used to characterize the angular resolution and absolute pointing capabilities of the detector. The detection is based on data taken in two periods before the completion of the detector: between April 2008 and May 2009, when IceCube operated in a partial configuration with 40 detector strings deployed in the South Pole ice, and between May 2009 and May 2010 when the detector operated with 59 strings. Using two independent analysis methods, the Moon shadow has been observed to high significance (>6σ) in both detector configurations. The observed location of the shadow center is within 0.2° of its expected position when geomagnetic deflection effects are taken into account. This measurement validates the directional reconstruction capabilities of IceCube. © 2014 American Physical Society.

Published
2014

13. Milagro observations of potential TeV emitters

Author

Abdo, AA, Abeysekara, AU, Allen, BT, Aune, T, Barber, AS, Berley, D, Braun, J, Chen, C, Christopher, GE, DeYoung, T, Dingus, BL, Ellsworth, RW, Gonzalez, MM, Goodman, JA, Hays, E, Hoffman, CM, Hüntemeyer, PH, Imran, A, Kolterman, BE, Linnemann, JT, McEnery, JE, Morgan, T, Mincer, AI, Nemethy, P, Pretz, J, Ryan, JM, Parkinson, PM Saz, Schneider, M, Shoup, A, Sinnis, G, Smith, AJ, Vasileiou, V, Walker, GP, Williams, DA, and Yodh, GB

Subjects
Astroparticle physics, Pulsars, Galaxies, Active galactic nuclei, Gamma-rays, astro-ph.HE, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Nuclear & Particles Physics
Abstract

This paper reports the results from three targeted searches of Milagro TeV sky maps: two extragalactic point source lists and one pulsar source list. The first extragalactic candidate list consists of 709 candidates selected from the Fermi-LAT 2FGL catalog. The second extragalactic candidate list contains 31 candidates selected from the TeVCat source catalog that have been detected by imaging atmospheric Cherenkov telescopes (IACTs). In both extragalactic candidate lists Mkn 421 was the only source detected by Milagro. This paper presents the Milagro TeV flux for Mkn 421 and flux limits for the brighter Fermi-LAT extragalactic sources and for all TeVCat candidates. The pulsar list extends a previously published Milagro targeted search for Galactic sources. With the 32 new gamma-ray pulsars identified in 2FGL, the number of pulsars that are studied by both Fermi-LAT and Milagro is increased to 52. In this sample, we find that the probability of Milagro detecting a TeV emission coincident with a pulsar increases with the GeV flux observed by the Fermi-LAT in the energy range from 0.1 GeV to 100 GeV. © 2014 Elsevier B.V. All rights reserved.

Published
2014

14. THE STUDY OF TeV VARIABILITY AND THE DUTY CYCLE OF Mrk 421 FROM 3 Yr OF OBSERVATIONS WITH THE MILAGRO OBSERVATORY

Author

Abdo, AA, Abeysekara, AU, Allen, BT, Aune, T, Barber, AS, Berley, D, Braun, J, Chen, C, Christopher, GE, Delay, RS, DeYoung, T, Dingus, BL, Ellsworth, RW, Fraija, N, González, MM, Goodman, JA, Hays, E, Hoffman, CM, Hüntemeyer, PH, Imran, A, Kolterman, BE, Linnemann, JT, Marinelli, A, McEnery, JE, Morgan, T, Mincer, AI, Nemethy, P, Patricelli, B, Pretz, J, Ryan, JM, Parkinson, PM Saz, Schneider, M, Shoup, A, Sinnis, G, Smith, AJ, Vasileiou, V, Walker, GP, Williams, DA, and Yodh, GB

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

TeV-flaring activity with timescales as short as tens of minutes and an orphan TeV flare have been observed from the blazar Markarian 421 (Mrk 421). The TeV emission from Mrk 421 is believed to be produced by leptonic synchrotron self-Compton (SSC) emission. In this scenario, correlations between the X-ray and the TeV fluxes are expected, TeV orphan flares are hardly explained, and the activity (measured as duty cycle) of the source at TeV energies is expected to be equal to or less than that observed in X-rays if only SSC is considered. To estimate the TeV duty cycle of Mrk 421 and to establish limits on its variability at different timescales, we continuously observed Mrk 421 with the Milagro observatory. Mrk 421 was detected by Milagro with a statistical significance of 7.1 standard deviations between 2005 September 21 and 2008 March 15. The observed spectrum is consistent with previous observations by VERITAS. We estimate the duty cycle of Mrk 421 for energies above 1 TeV for different hypotheses of the baseline flux and for different flare selections and we compared our results with the X-ray duty cycle estimated by Resconi et al. The robustness of the results is discussed. © 2014. The American Astronomical Society. All rights reserved..

Published
2014

15. 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

16. Evidence for High-Energy Extraterrestrial Neutrinos at the IceCube Detector

Author

Aartsen, MG, Abbasi, R, Abdou, Y, Ackermann, M, Adams, J, Aguilar, JA, Ahlers, M, Altmann, D, Auffenberg, J, Bai, X, Baker, M, Barwick, SW, Baum, V, Bay, R, Beatty, JJ, Bechet, S, Becker Tjus, J, Becker, K-H, Benabderrahmane, ML, BenZvi, S, Berghaus, P, Berley, D, Bernardini, E, Bernhard, A, Bertrand, D, Besson, DZ, Binder, G, Bindig, D, Bissok, M, Blaufuss, E, Blumenthal, J, Boersma, DJ, Bohaichuk, S, Bohm, C, Bose, D, Böser, S, Botner, O, Brayeur, L, Bretz, H-P, Brown, AM, Bruijn, R, Brunner, J, Carson, M, Casey, J, Casier, M, Chirkin, D, Christov, A, Christy, B, Clark, K, Clevermann, F, Coenders, S, Cohen, S, Cowen, DF, Cruz Silva, AH, Danninger, M, Daughhetee, J, Davis, JC, Day, M, De Clercq, C, De Ridder, S, Desiati, P, de Vries, KD, de With, M, DeYoung, T, Díaz-Vélez, JC, Dunkman, M, Eagan, R, Eberhardt, B, Eichmann, B, Eisch, J, Ellsworth, RW, Euler, S, Evenson, PA, Fadiran, O, Fazely, AR, Fedynitch, A, Feintzeig, J, Feusels, T, Filimonov, K, Finley, C, Fischer-Wasels, T, Flis, S, Franckowiak, A, Frantzen, K, Fuchs, T, Gaisser, TK, Gallagher, J, Gerhardt, L, Gladstone, L, Glüsenkamp, T, Goldschmidt, A, Golup, G, Gonzalez, JG, Goodman, JA, Góra, D, Grandmont, DT, Grant, D, Groß, A, Ha, C, and Haj Ismail, A

Subjects
Nuclear and Plasma Physics, Particle and High Energy Physics, Physical Sciences, IceCube Collaboration, astro-ph.HE, astro-ph.CO, hep-ex, General Science & Technology
Abstract

We report on results of an all-sky search for high-energy neutrino events interacting within the IceCube neutrino detector conducted between May 2010 and May 2012. The search follows up on the previous detection of two PeV neutrino events, with improved sensitivity and extended energy coverage down to about 30 TeV. Twenty-six additional events were observed, substantially more than expected from atmospheric backgrounds. Combined, both searches reject a purely atmospheric origin for the 28 events at the 4σ level. These 28 events, which include the highest energy neutrinos ever observed, have flavors, directions, and energies inconsistent with those expected from the atmospheric muon and neutrino backgrounds. These properties are, however, consistent with generic predictions for an additional component of extraterrestrial origin.

Published
2013

17. Evidence for high-energy extraterrestrial neutrinos at the IceCube detector.

Author

IceCube Collaboration, Aartsen, MG, Abbasi, R, Abdou, Y, Ackermann, M, Adams, J, Aguilar, JA, Ahlers, M, Altmann, D, Auffenberg, J, Bai, X, Baker, M, Barwick, SW, Baum, V, Bay, R, Beatty, JJ, Bechet, S, Becker Tjus, J, Becker, K-H, Benabderrahmane, ML, BenZvi, S, Berghaus, P, Berley, D, Bernardini, E, Bernhard, A, Bertrand, D, Besson, DZ, Binder, G, Bindig, D, Bissok, M, Blaufuss, E, Blumenthal, J, Boersma, DJ, Bohaichuk, S, Bohm, C, Bose, D, Böser, S, Botner, O, Brayeur, L, Bretz, H-P, Brown, AM, Bruijn, R, Brunner, J, Carson, M, Casey, J, Casier, M, Chirkin, D, Christov, A, Christy, B, Clark, K, Clevermann, F, Coenders, S, Cohen, S, Cowen, DF, Cruz Silva, AH, Danninger, M, Daughhetee, J, Davis, JC, Day, M, De Clercq, C, De Ridder, S, Desiati, P, de Vries, KD, de With, M, DeYoung, T, Díaz-Vélez, JC, Dunkman, M, Eagan, R, Eberhardt, B, Eichmann, B, Eisch, J, Ellsworth, RW, Euler, S, Evenson, PA, Fadiran, O, Fazely, AR, Fedynitch, A, Feintzeig, J, Feusels, T, Filimonov, K, Finley, C, Fischer-Wasels, T, Flis, S, Franckowiak, A, Frantzen, K, Fuchs, T, Gaisser, TK, Gallagher, J, Gerhardt, L, Gladstone, L, Glüsenkamp, T, Goldschmidt, A, Golup, G, Gonzalez, JG, Goodman, JA, Góra, D, Grandmont, DT, Grant, D, Groß, A, and Ha, C

Subjects
IceCube Collaboration, astro-ph.HE, astro-ph.CO, hep-ex, General Science & Technology
Abstract

We report on results of an all-sky search for high-energy neutrino events interacting within the IceCube neutrino detector conducted between May 2010 and May 2012. The search follows up on the previous detection of two PeV neutrino events, with improved sensitivity and extended energy coverage down to about 30 TeV. Twenty-six additional events were observed, substantially more than expected from atmospheric backgrounds. Combined, both searches reject a purely atmospheric origin for the 28 events at the 4σ level. These 28 events, which include the highest energy neutrinos ever observed, have flavors, directions, and energies inconsistent with those expected from the atmospheric muon and neutrino backgrounds. These properties are, however, consistent with generic predictions for an additional component of extraterrestrial origin.

Published
2013

18. 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

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, 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

20. 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

21. 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

22. The IceCube Neutrino Observatory Part I: Point Source Searches

Author

Collaboration, IceCube, Aartsen, MG, Abbasi, R, Abdou, Y, Ackermann, M, Adams, J, Aguilar, JA, Ahlers, M, Altmann, D, Auffenberg, J, Bai, X, Baker, M, Barwick, SW, Baum, V, Bay, R, Beatty, JJ, Bechet, S, Tjus, J Becker, Becker, K-H, Bell, M, Benabderrahmane, ML, BenZvi, S, Berghaus, P, Berley, D, Bernardini, E, Bernhard, A, Bertrand, D, Besson, DZ, Binder, G, Bindig, D, Bissok, M, Blaufuss, E, Blumenthal, J, Boersma, DJ, Bohaichuk, S, Bohm, C, Bose, D, Böser, S, Botner, O, Brayeur, L, Bretz, H-P, Brown, AM, Bruijn, R, Brunner, J, Carson, M, Casey, J, Casier, M, Chirkin, D, Christov, A, Christy, B, Clark, K, Clevermann, F, Coenders, S, Cohen, S, Cowen, DF, Silva, AH Cruz, Danninger, M, Daughhetee, J, Davis, JC, Clercq, C De, Ridder, S De, Desiati, P, Vries, KD de, With, M de, DeYoung, T, Díaz-Vélez, JC, Dunkman, M, Eagan, R, Eberhardt, B, Eisch, J, Ellsworth, RW, Euler, S, Evenson, PA, Fadiran, O, Fazely, AR, Fedynitch, A, Feintzeig, J, Feusels, T, Filimonov, K, Finley, C, Fischer-Wasels, T, Flis, S, Franckowiak, A, Frantzen, K, Fuchs, T, Gaisser, TK, Gallagher, J, Gerhardt, L, Gladstone, L, Glüsenkamp, T, Goldschmidt, A, Golup, G, Gonzalez, JG, Goodman, JA, Góra, D, Grandmont, DT, Grant, D, Groß, A, Ha, C, and Ismail, A Haj

Subjects
astro-ph.HE
Abstract

Papers on point source searches submitted to the 33nd International CosmicRay Conference (Rio de Janeiro 2013) by the IceCube Collaboration.

Published
2013

23. The IceCube Neutrino Observatory Part III: Cosmic Rays

Author

Collaboration, IceCube, Aartsen, MG, Abbasi, R, Abdou, Y, Ackermann, M, Adams, J, Aguilar, JA, Ahlers, M, Altmann, D, Auffenberg, J, Bai, X, Baker, M, Barwick, SW, Baum, V, Bay, R, Beatty, JJ, Bechet, S, Tjus, J Becker, Becker, K-H, Bell, M, Benabderrahmane, ML, BenZvi, S, Berghaus, P, Berley, D, Bernardini, E, Bernhard, A, Bertrand, D, Besson, DZ, Binder, G, Bindig, D, Bissok, M, Blaufuss, E, Blumenthal, J, Boersma, DJ, Bohaichuk, S, Bohm, C, Bose, D, Böser, S, Botner, O, Brayeur, L, Bretz, H-P, Brown, AM, Bruijn, R, Brunner, J, Carson, M, Casey, J, Casier, M, Chirkin, D, Christov, A, Christy, B, Clark, K, Clevermann, F, Coenders, S, Cohen, S, Cowen, DF, Silva, AH Cruz, Danninger, M, Daughhetee, J, Davis, JC, Clercq, C De, Ridder, S De, Desiati, P, Vries, KD de, With, M de, DeYoung, T, Díaz-Vélez, JC, Dunkman, M, Eagan, R, Eberhardt, B, Eisch, J, Ellsworth, RW, Euler, S, Evenson, PA, Fadiran, O, Fazely, AR, Fedynitch, A, Feintzeig, J, Feusels, T, Filimonov, K, Finley, C, Fischer-Wasels, T, Flis, S, Franckowiak, A, Frantzen, K, Fuchs, T, Gaisser, TK, Gallagher, J, Gerhardt, L, Gladstone, L, Glüsenkamp, T, Goldschmidt, A, Golup, G, Gonzalez, JG, Goodman, JA, Góra, D, Grandmont, DT, Grant, D, Groß, A, Ha, C, and Ismail, A Haj

Subjects
astro-ph.HE
Abstract

Papers on cosmic rays submitted to the 33nd International Cosmic RayConference (Rio de Janeiro 2013) by the IceCube Collaboration.

Published
2013

24. The IceCube Neutrino Observatory Part IV: Searches for Dark Matter and Exotic Particles

Author

Collaboration, IceCube, Aartsen, MG, Abbasi, R, Abdou, Y, Ackermann, M, Adams, J, Aguilar, JA, Ahlers, M, Altmann, D, Auffenberg, J, Bai, X, Baker, M, Barwick, SW, Baum, V, Bay, R, Beatty, JJ, Bechet, S, Tjus, J Becker, Becker, K-H, Bell, M, Benabderrahmane, ML, BenZvi, S, Berghaus, P, Berley, D, Bernardini, E, Bernhard, A, Bertrand, D, Besson, DZ, Binder, G, Bindig, D, Bissok, M, Blaufuss, E, Blumenthal, J, Boersma, DJ, Bohaichuk, S, Bohm, C, Bose, D, Böser, S, Botner, O, Brayeur, L, Bretz, H-P, Brown, AM, Bruijn, R, Brunner, J, Carson, M, Casey, J, Casier, M, Chirkin, D, Christov, A, Christy, B, Clark, K, Clevermann, F, Coenders, S, Cohen, S, Cowen, DF, Silva, AH Cruz, Danninger, M, Daughhetee, J, Davis, JC, Clercq, C De, Ridder, S De, Desiati, P, Vries, KD de, With, M de, DeYoung, T, Díaz-Vélez, JC, Dunkman, M, Eagan, R, Eberhardt, B, Eisch, J, Ellsworth, RW, Euler, S, Evenson, PA, Fadiran, O, Fazely, AR, Fedynitch, A, Feintzeig, J, Feusels, T, Filimonov, K, Finley, C, Fischer-Wasels, T, Flis, S, Franckowiak, A, Frantzen, K, Fuchs, T, Gaisser, TK, Gallagher, J, Gerhardt, L, Gladstone, L, Glüsenkamp, T, Goldschmidt, A, Golup, G, Gonzalez, JG, Goodman, JA, Góra, D, Grandmont, DT, Grant, D, Groß, A, Ha, C, and Ismail, A Haj

Subjects
astro-ph.HE
Abstract

Papers on searches for Dark Matter and exotic particles submitted to the 33ndInternational Cosmic Ray Conference (Rio de Janeiro 2013) by the IceCubeCollaboration.

Published
2013

25. The IceCube Neutrino Observatory Part VI: Ice Properties, Reconstruction and Future Developments

Author

Collaboration, IceCube, Aartsen, MG, Abbasi, R, Abdou, Y, Ackermann, M, Adams, J, Aguilar, JA, Ahlers, M, Altmann, D, Auffenberg, J, Bai, X, Baker, M, Barwick, SW, Baum, V, Bay, R, Beatty, JJ, Bechet, S, Tjus, J Becker, Becker, K-H, Bell, M, Benabderrahmane, ML, BenZvi, S, Berghaus, P, Berley, D, Bernardini, E, Bernhard, A, Bertrand, D, Besson, DZ, Binder, G, Bindig, D, Bissok, M, Blaufuss, E, Blumenthal, J, Boersma, DJ, Bohaichuk, S, Bohm, C, Bose, D, Böser, S, Botner, O, Brayeur, L, Bretz, H-P, Brown, AM, Bruijn, R, Brunner, J, Carson, M, Casey, J, Casier, M, Chirkin, D, Christov, A, Christy, B, Clark, K, Clevermann, F, Coenders, S, Cohen, S, Cowen, DF, Silva, AH Cruz, Danninger, M, Daughhetee, J, Davis, JC, Clercq, C De, Ridder, S De, Desiati, P, Vries, KD de, With, M de, DeYoung, T, Díaz-Vélez, JC, Dunkman, M, Eagan, R, Eberhardt, B, Eisch, J, Ellsworth, RW, Euler, S, Evenson, PA, Fadiran, O, Fazely, AR, Fedynitch, A, Feintzeig, J, Feusels, T, Filimonov, K, Finley, C, Fischer-Wasels, T, Flis, S, Franckowiak, A, Frantzen, K, Fuchs, T, Gaisser, TK, Gallagher, J, Gerhardt, L, Gladstone, L, Glüsenkamp, T, Goldschmidt, A, Golup, G, Gonzalez, JG, Goodman, JA, Góra, D, Grandmont, DT, Grant, D, Groß, A, Ha, C, and Ismail, A Haj

Subjects
astro-ph.HE
Abstract

Papers on ice properties, reconstruction and future developments submitted tothe 33nd International Cosmic Ray Conference (Rio de Janeiro 2013) by theIceCube Collaboration.

Published
2013

26. The IceCube Neutrino Observatory Part II: Atmospheric and Diffuse UHE Neutrino Searches of All Flavors

Author

Collaboration, IceCube, Aartsen, MG, Abbasi, R, Abdou, Y, Ackermann, M, Adams, J, Aguilar, JA, Ahlers, M, Altmann, D, Auffenberg, J, Bai, X, Baker, M, Barwick, SW, Baum, V, Bay, R, Beatty, JJ, Bechet, S, Tjus, J Becker, Becker, K-H, Bell, M, Benabderrahmane, ML, BenZvi, S, Berghaus, P, Berley, D, Bernardini, E, Bernhard, A, Bertrand, D, Besson, DZ, Binder, G, Bindig, D, Bissok, M, Blaufuss, E, Blumenthal, J, Boersma, DJ, Bohaichuk, S, Bohm, C, Bose, D, Böser, S, Botner, O, Brayeur, L, Bretz, H-P, Brown, AM, Bruijn, R, Brunner, J, Carson, M, Casey, J, Casier, M, Chirkin, D, Christov, A, Christy, B, Clark, K, Clevermann, F, Coenders, S, Cohen, S, Cowen, DF, Silva, AH Cruz, Danninger, M, Daughhetee, J, Davis, JC, Clercq, C De, Ridder, S De, Desiati, P, Vries, KD de, With, M de, DeYoung, T, Díaz-Vélez, JC, Dunkman, M, Eagan, R, Eberhardt, B, Eisch, J, Ellsworth, RW, Euler, S, Evenson, PA, Fadiran, O, Fazely, AR, Fedynitch, A, Feintzeig, J, Feusels, T, Filimonov, K, Finley, C, Fischer-Wasels, T, Flis, S, Franckowiak, A, Frantzen, K, Fuchs, T, Gaisser, TK, Gallagher, J, Gerhardt, L, Gladstone, L, Glüsenkamp, T, Goldschmidt, A, Golup, G, Gonzalez, JG, Goodman, JA, Góra, D, Grandmont, DT, Grant, D, Groß, A, Ha, C, and Ismail, A Haj

Subjects
astro-ph.HE
Abstract

Papers on atmospheric and diffuse UHE neutrino searches of all flavorssubmitted to the 33nd International Cosmic Ray Conference (Rio de Janeiro 2013)by the IceCube Collaboration.

Published
2013

27. The IceCube Neutrino Observatory Part V: Neutrino Oscillations and Supernova Searches

Author

Collaboration, IceCube, Aartsen, MG, Abbasi, R, Abdou, Y, Ackermann, M, Adams, J, Aguilar, JA, Ahlers, M, Altmann, D, Auffenberg, J, Bai, X, Baker, M, Barwick, SW, Baum, V, Bay, R, Beatty, JJ, Bechet, S, Tjus, J Becker, Becker, K-H, Bell, M, Benabderrahmane, ML, BenZvi, S, Berghaus, P, Berley, D, Bernardini, E, Bernhard, A, Bertrand, D, Besson, DZ, Binder, G, Bindig, D, Bissok, M, Blaufuss, E, Blumenthal, J, Boersma, DJ, Bohaichuk, S, Bohm, C, Bose, D, Böser, S, Botner, O, Brayeur, L, Bretz, H-P, Brown, AM, Bruijn, R, Brunner, J, Carson, M, Casey, J, Casier, M, Chirkin, D, Christov, A, Christy, B, Clark, K, Clevermann, F, Coenders, S, Cohen, S, Cowen, DF, Silva, AH Cruz, Danninger, M, Daughhetee, J, Davis, JC, Clercq, C De, Ridder, S De, Desiati, P, Vries, KD de, With, M de, DeYoung, T, Díaz-Vélez, JC, Dunkman, M, Eagan, R, Eberhardt, B, Eisch, J, Ellsworth, RW, Euler, S, Evenson, PA, Fadiran, O, Fazely, AR, Fedynitch, A, Feintzeig, J, Feusels, T, Filimonov, K, Finley, C, Fischer-Wasels, T, Flis, S, Franckowiak, A, Frantzen, K, Fuchs, T, Gaisser, TK, Gallagher, J, Gerhardt, L, Gladstone, L, Glüsenkamp, T, Goldschmidt, A, Golup, G, Gonzalez, JG, Goodman, JA, Góra, D, Grandmont, DT, Grant, D, Groß, A, Ha, C, and Ismail, A Haj

Subjects
astro-ph.HE
Abstract

Papers on neutrino oscillation and supernova searches submitted to the 33ndInternational Cosmic Ray Conference (Rio de Janeiro 2013) by the IceCubeCollaboration.

Published
2013

28. Search for relativistic magnetic monopoles with the AMANDA-II neutrino telescope

Author

The IceCube Collaboration, Abbasi, R, Abdou, Y, Abu-Zayyad, T, Adams, J, Aguilar, JA, Ahlers, M, Andeen, K, Auffenberg, J, Bai, X, Baker, M, Barwick, SW, Bay, R, Bazo Alba, JL, Beattie, K, Beatty, JJ, Bechet, S, Becker, JK, Becker, K-H, Benabderrahmane, ML, BenZvi, S, Berdermann, J, Berghaus, P, Berley, D, Bernardini, E, Bertrand, D, Besson, DZ, Bissok, M, Blaufuss, E, Boersma, DJ, Bohm, C, Böser, S, Botner, O, Bradley, L, Braun, J, Buitink, S, Carson, M, Chirkin, D, Christy, B, Clem, J, Clevermann, F, Cohen, S, Colnard, C, Cowen, DF, D’Agostino, MV, Danninger, M, Davis, JC, De Clercq, C, Demirörs, L, Depaepe, O, Descamps, F, Desiati, P, de Vries-Uiterweerd, G, DeYoung, T, Díaz-Vélez, JC, Dierckxsens, M, Dreyer, J, Dumm, JP, Duvoort, MR, Ehrlich, R, Eisch, J, Ellsworth, RW, Engdegård, O, Euler, S, Evenson, PA, Fadiran, O, Fazely, AR, Feusels, T, Filimonov, K, Finley, C, Foerster, MM, Fox, BD, Franckowiak, A, Franke, R, Gaisser, TK, Gallagher, J, Geisler, M, Gerhardt, L, Gladstone, L, Glüsenkamp, T, Goldschmidt, A, Goodman, JA, Grant, D, Griesel, T, Groß, A, Grullon, S, Gurtner, M, Ha, C, Hallgren, A, Halzen, F, Han, K, Hanson, K, Helbing, K, Herquet, P, Hickford, S, Hill, GC, Hoffman, KD, Homeier, A, Hoshina, K, and Hubert, D

Subjects
Nuclear and Plasma Physics, Particle and High Energy Physics, Astronomical Sciences, Physical Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Quantum Physics, Nuclear & Particles Physics, Astronomical sciences, Atomic, molecular and optical physics, Particle and high energy physics
Abstract

We present the search for Cherenkov signatures from relativistic magnetic monopoles in data taken with the AMANDA-II detector, a neutrino telescope deployed in the Antarctic ice cap at the Geographic South Pole. The non-observation of a monopole signal in data collected during the year 2000 improves present experimental limits on the flux of relativistic magnetic monopoles: Our flux limit varies between 3.8 × 10-17 cm-2 s-1 sr-1 (for monopoles moving at the vacuum speed of light) and 8.8 × 10-16 cm-2 s-1 sr-1 (for monopoles moving at a speed β=v/c=0.76, just above the Cherenkov threshold in ice). These limits apply to monopoles that are energetic enough to penetrate the Earth and enter the detector from below the horizon. The limit obtained for monopoles reaching the detector from above the horizon is less stringent by roughly an order of magnitude, due to the much larger background from down-going atmospheric muons. This looser limit is however valid for a larger class of magnetic monopoles, since the monopoles are not required to pass through the Earth. © 2010 The Author(s).

Published
2010

29. Search for relativistic magnetic monopoles with the AMANDA-II neutrino telescope: The IceCube Collaboration

Author

Abbasi, R, Abdou, Y, Abu-Zayyad, T, Adams, J, Aguilar, JA, Ahlers, M, Andeen, K, Auffenberg, J, Bai, X, Baker, M, Barwick, SW, Bay, R, Bazo Alba, JL, Beattie, K, Beatty, JJ, Bechet, S, Becker, JK, Becker, KH, Benabderrahmane, ML, BenZvi, S, Berdermann, J, Berghaus, P, Berley, D, Bernardini, E, Bertrand, D, Besson, DZ, Bissok, M, Blaufuss, E, Boersma, DJ, Bohm, C, Böser, S, Botner, O, Bradley, L, Braun, J, Buitink, S, Carson, M, Chirkin, D, Christy, B, Clem, J, Clevermann, F, Cohen, S, Colnard, C, Cowen, DF, D'Agostino, MV, Danninger, M, Davis, JC, de Clercq, C, Demirörs, L, Depaepe, O, Descamps, F, Desiati, P, de Vries-Uiterweerd, G, DeYoung, T, Díaz-Vélez, JC, Dierckxsens, M, Dreyer, J, Dumm, JP, Duvoort, MR, Ehrlich, R, Eisch, J, Ellsworth, RW, Engdegård, O, Euler, S, Evenson, PA, Fadiran, O, Fazely, AR, Feusels, T, Filimonov, K, Finley, C, Foerster, MM, Fox, BD, Franckowiak, A, Franke, R, Gaisser, TK, Gallagher, J, Geisler, M, Gerhardt, L, Gladstone, L, Glüsenkamp, T, Goldschmidt, A, Goodman, JA, Grant, D, Griesel, T, Groß, A, Grullon, S, Gurtner, M, Ha, C, Hallgren, A, Halzen, F, Han, K, Hanson, K, Helbing, K, Herquet, P, Hickford, S, Hill, GC, Hoffman, KD, Homeier, A, Hoshina, K, Hubert, D, and Huelsnitz, W

Subjects
Nuclear & Particles Physics, Quantum Physics, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Atomic, Molecular, Nuclear, Particle and Plasma Physics
Abstract

We present the search for Cherenkov signatures from relativistic magnetic monopoles in data taken with the AMANDA-II detector, a neutrino telescope deployed in the Antarctic ice cap at the Geographic South Pole. The non-observation of a monopole signal in data collected during the year 2000 improves present experimental limits on the flux of relativistic magnetic monopoles: Our flux limit varies between 3.8 × 10-17 cm-2 s-1 sr-1 (for monopoles moving at the vacuum speed of light) and 8.8 × 10-16 cm-2 s-1 sr-1 (for monopoles moving at a speed β=v/c=0.76, just above the Cherenkov threshold in ice). These limits apply to monopoles that are energetic enough to penetrate the Earth and enter the detector from below the horizon. The limit obtained for monopoles reaching the detector from above the horizon is less stringent by roughly an order of magnitude, due to the much larger background from down-going atmospheric muons. This looser limit is however valid for a larger class of magnetic monopoles, since the monopoles are not required to pass through the Earth. © 2010 The Author(s).

Published
2010

30. First results of a study of TeV emission from GRBs in Milagrito

Author

McEnery, JE, Atkins, R, Benbow, W, Berley, D, Chen, ML, Coyne, DG, Dingus, BL, Dorfan, DE, Ellsworth, RW, Evans, D, Falcone, A, Fleysher, L, Fleysher, R, Gisler, G, Goodman, JA, Haines, TJ, Hoffman, CM, Hugenberger, S, Kelley, LA, Leonor, I, McConnell, M, McCullough, JF, Miller, RS, Mincer, AI, Morales, MF, Nemethy, P, Ryan, JM, Shen, B, Shoup, A, Sinnis, C, Smith, AJ, Sullivan, GW, Tumer, T, Wang, K, Wascko, MO, Westerhoff, S, Williams, DA, Yang, T, and Yodh, GB

Subjects
astro-ph
Abstract

Milagrito, a detector sensitive to gamma-rays at TeV energies, monitored thenorthern sky during the period February 1997 through May 1998. With a largefield of view and high duty cycle, this instrument was used to perform a searchfor TeV counterparts to gamma-ray bursts. Within the Milagrito field of view 54gamma-ray bursts at keV energies were observed by the Burst And TransientSatellite Experiment (BATSE) aboard the Compton Gamma-Ray Observatory. Thispaper describes the results of a preliminary analysis to search for TeVemission correlated with BATSE detected bursts. Milagrito detected an excess ofevents coincident both spatially and temporally with GRB 970417a, with chanceprobability $2.8 \times 10^{-5}$ within the BATSE error radius. No othersignificant correlations were detected. Since 54 bursts were examined thechance probability of observing an excess with this significance in any ofthese bursts is $1.5 \times 10^{-3}$. The statistical aspects and physicalimplications of this result are discussed.

Published
2000

31. First results of a study of TeV emission from GRBs in Milagrito

Author

Miller, RS, Atkins, R, Benbow, W, Berley, D, Chen, ML, Coyne, DG, Dingus, BL, Dorfan, DE, Ellsworth, RW, Evans, D, Falcone, A, Fleysher, L, Fleysher, R, Gisler, G, Goodman, JA, Haines, TJ, Hoffman, CM, Hugenberger, S, Kelley, LA, Leonor, I, McConnell, M, McCullough, JF, McEnery, JE, Mincer, AI, Morales, MF, Nemethy, P, Ryan, JM, Shen, B, Shoup, A, Sinnis, C, Smith, AJ, Sullivan, GW, Tumer, T, Wang, K, Wascko, MO, Westerhoff, S, Williams, DA, Yang, T, and Yodh, GB

Subjects
astro-ph
Abstract

Milagrito, a detector sensitive to gamma-rays at TeV energies, monitored thenorthern sky during the period February 1997 through May 1998. With a largefield of view and high duty cycle, this instrument was used to perform a searchfor TeV counterparts to gamma-ray bursts. Within the Milagrito field of view 54gamma-ray bursts at keV energies were observed by the Burst And TransientSatellite Experiment (BATSE) aboard the Compton Gamma-Ray Observatory. Thispaper describes the results of a preliminary analysis to search for TeVemission correlated with BATSE detected bursts. Milagrito detected an excess ofevents coincident both spatially and temporally with GRB 970417a, with chanceprobability $2.8 \times 10^{-5}$ within the BATSE error radius. No othersignificant correlations were detected. Since 54 bursts were examined thechance probability of observing an excess with this significance in any ofthese bursts is $1.5 \times 10^{-3}$. The statistical aspects and physicalimplications of this result are discussed.

Published
2000

32. Instrumented Water Tanks can Improve Air Shower Detector Sensitivity

Author

Atkins, R, Benbow, W, Berley, D, Chen, M-L, Coyne, DG, Delay, RS, Dingus, BL, Dorfan, DE, Ellsworth, RW, Evans, D, Falcone, A, Fleysher, L, Fleysher, R, Gisler, G, Goodman, JA, Haines, TJ, Hoffman, CM, Hugenberger, S, Kelley, LA, Leonor, I, Macri, J, McConnell, M, McCullough, JF, McEnery, JE, Miller, RS, Mincer, AI, Morales, MF, Nemethy, P, Ryan, JM, Schneider, M, Shen, B, Shoup, A, Sinnis, G, Smith, AJ, Sullivan, GW, Thompson, TN, Tumer, OT, Wang, K, Wascko, MO, Westerhoff, S, Williams, DA, Yang, T, and Yodh, GB

Subjects
astro-ph
Abstract

Previous works have shown that water Cherenkov detectors have superiorsensitivity to those of scintillation counters as applied to detectingextensive air showers (EAS). This is in large part due to their much highersensitivity to EAS photons which are more than five times more numerous thanEAS electrons. Large area water Cherenkov detectors can be constructedrelatively cheaply and operated reliably. A sparse detector array has beendesigned which uses these types of detectors to substantially increase the areaover which the Milagro Gamma Ray Observatory collects EAS information.Improvements to the Milagro detector's performance characteristics andsensitivity derived from this array and preliminary results from a prototypearray currently installed near the Milagro detector will be presented.

Published
1999

33. Calibration of the Milagro Cosmic Ray Telescope

Author

Atkins, R, Benbow, W, Berley, D, Chen, M-L, Coyne, DG, Delay, RS, Dingus, BL, Dorfan, DE, Ellsworth, RW, Evans, D, Falcone, A, Fleysher, L, Fleysher, R, Gisler, G, Goodman, JA, Haines, TJ, Hoffman, CM, Hugenberger, S, Kelley, LA, Leonor, I, Macri, J, McConnell, M, McCullough, JF, McEnery, JE, Miller, RS, Mincer, AI, Morales, MF, Nemethy, P, Ryan, JM, Schneider, M, Shen, B, Shoup, A, Sinnis, G, Smith, AJ, Sullivan, GW, Thompson, TN, Tumer, OT, Wang, K, Wascko, MO, Westerhoff, S, Williams, DA, Yang, T, and Yodh, GB

Subjects
astro-ph
Abstract

The Milagro detector is an air shower array which uses the water Cherenkovtechnique and is capable of continuously monitoring the sky at energies near 1TeV. The detector consists of 20000 metric tons of pure water instrumented with723 photo-multiplier tubes (PMTs). The PMTs are arranged in a two-layerstructure on a lattice of 3 m spacing covering 5000 $m^2$ area. The directionof the shower is determined from the relative timing of the PMT signals,necessitating a common time reference and amplitude slewing corrections toimprove the time resolution. The calibration system to provide these consistsof a pulsed laser driving 30 diffusing light sources deployed in the pond toallow cross-calibration of the PMTs. The system is capable of calibrating timesand the pulse-heights from the PMTs using the time-over-threshold technique.The absolute energy scale is provided using single muons passing through thedetector. The description of the calibration system of the Milagro detector andits prototype Milagrito will be presented.

Published
1999

34. Status of the Milagro Gamma Ray Observatory

Author

Atkins, R, Benbow, W, Berley, D, Chen, M-L, Coyne, DG, Delay, RS, Dingus, BL, Dorfan, DE, Ellsworth, RW, Evans, D, Falcone, A, Fleysher, L, Fleysher, R, Gisler, G, Goodman, JA, Haines, TJ, Hoffman, CM, Hugenberger, S, Kelley, LA, Leonor, I, Macri, J, McConnell, M, McCullough, JF, McEnery, JE, Miller, RS, Mincer, AI, Morales, MF, Nemethy, P, Ryan, JM, Schneider, M, Shen, B, Shoup, A, Sinnis, G, Smith, AJ, Sullivan, GW, Thompson, TN, Tumer, OT, Wang, K, Wascko, MO, Westerhoff, S, Williams, DA, Yang, T, and Yodh, GB

Subjects
astro-ph
Abstract

The Milagro Gamma Ray Observatory is the world's first large-area waterCherenkov detector capable of continuously monitoring the sky at TeV energies.Located in northern New Mexico, Milagro will perform an all sky survey of theNorthern Hemisphere at energies between ~250 GeV and 50 TeV. With a high dutycycle, large detector area (~5000 square meters), and a wide field-of-view (~1sr), Milagro is uniquely capable of searching for transient and DC sources ofhigh-energy gamma-ray emission. Milagro has been operating since February,1999. The current status of the Milagro Observatory and initial results will bediscussed.

Published
1999

35. Study of the Shadows of the Moon and the Sun with VHE Cosmic Rays

Author

Atkins, R, Benbow, W, Berley, D, Chen, M-L, Coyne, DG, Delay, RS, Dingus, BL, Dorfan, DE, Ellsworth, RW, Evans, D, Falcone, A, Fleysher, L, Fleysher, R, Gisler, G, Goodman, JA, Haines, TJ, Hoffman, CM, Hugenberger, S, Kelley, LA, Leonor, I, Macri, J, McConnell, M, McCullough, JF, McEnery, JE, Miller, RS, Mincer, AI, Morales, MF, Nemethy, P, Ryan, JM, Schneider, M, Shen, B, Shoup, A, Sinnis, G, Smith, AJ, Sullivan, GW, Thompson, TN, Tumer, OT, Wang, K, Wascko, MO, Westerhoff, S, Williams, DA, Yang, T, and Yodh, GB

Subjects
astro-ph
Abstract

Milagrito, a prototype for the Milagro detector, operated for 15 months in1997-8 and collected 8.9 billion events. It was the first extensive air shower(EAS) array sensitive to showers intiated by primaries with energy below 1 TeV.The shadows of the sun and moon observed with cosmic rays can be used to studysystematic pointing shifts and measure the angular resolution of EAS arrays.Below a few TeV, the paths of cosmic rays coming toward the earth are bent bythe helio- and geo-magnetic fields. This is expected to distort and displacethe shadows of the sun and the moon. The moon shadow, offset from the nominal(undeflected) position, has been observed with high statistical significance inMilagrito. This can be used to establish energy calibrations, as well as tosearch for the anti-matter content of the VHE cosmic ray flux. The shadow ofthe sun has also been observed with high significance.

Published
1999

36. Search for Short Duration Bursts of TeV Gamma Rays with the Milagrito Telescope

Author

Atkins, R, Benbow, W, Berley, D, Chen, M-L, Coyne, DG, Delay, RS, Dingus, BL, Dorfan, DE, Ellsworth, RW, Evans, D, Falcone, A, Fleysher, L, Fleysher, R, Gisler, G, Goodman, JA, Haines, TJ, Hoffman, CM, Hugenberger, S, Kelley, LA, Leonor, I, Macri, J, McConnell, M, McCullough, JF, McEnery, JE, Miller, RS, Mincer, AI, Morales, MF, Nemethy, P, Ryan, JM, Schneider, M, Shen, B, Shoup, A, Sinnis, G, Smith, AJ, Sullivan, GW, Thompson, TN, Tumer, OT, Wang, K, Wascko, MO, Westerhoff, S, Williams, DA, Yang, T, and Yodh, GB

Subjects
astro-ph
Abstract

The Milagrito water Cherenkov telescope operated for over a year. The mostprobable gamma-ray energy was ~1 TeV and the trigger rate was as high as 400Hz. We have developed an efficient technique for searching the entire sky forshort duration bursts of TeV photons. Such bursts may result from "traditional"gamma-ray bursts that were not in the field-of-view of any other instruments,the evaporation of primordial black holes, or some as yet undiscoveredphenomenon. We have begun to search the Milagrito data set for bursts ofduration 10 seconds. Here we will present the technique and the expectedresults. Final results will be presented at the conference.

Published
1999

37. Detection of 6 November 1997 Ground Level Event by Milagrito

Author

Atkins, R, Benbow, W, Berley, D, Chen, M-L, Coyne, DG, Delay, RS, Dingus, BL, Dorfan, DE, Ellsworth, RW, Evans, D, Falcone, A, Fleysher, L, Fleysher, R, Gisler, G, Goodman, JA, Haines, TJ, Hoffman, CM, Hugenberger, S, Kelley, LA, Leonor, I, Macri, J, McConnell, M, McCullough, JF, McEnery, JE, Miller, RS, Mincer, AI, Morales, MF, Nemethy, P, Ryan, JM, Schneider, M, Shen, B, Shoup, A, Sinnis, G, Smith, AJ, Sullivan, GW, Thompson, TN, Tumer, OT, Wang, K, Wascko, MO, Westerhoff, S, Williams, DA, Yang, T, and Yodh, GB

Subjects
astro-ph
Abstract

Solar Energetic Particles from the 6 November 1997 solar flare/CME(coronalmass ejection) with energies exceeding 10 GeV have been detected by Milagrito,a prototype of the Milagro Gamma Ray Observatory. While particle accelerationbeyond 1 GeV at the Sun is well established, few data exist for protons or ionsbeyond 10 GeV. The Milagro observatory, a ground based water Cherenkov detectordesigned for observing very high energy gamma ray sources, can also be used tostudy the Sun. Milagrito, which operated for approximately one year in 1997/98,was sensitive to solar proton and neutron fluxes above ~5- 10 GeV. Milagritooperated in a scaler mode, which was primarily sensitive to muons, low energyphotons, and electrons, and the detector operated in a mode sensitive toshowers and high zenith angle muons. In its scaler mode, Milagrito registered arate increase coincident with the 6 November 1997 ground level event observedby Climax and other neutron monitors. A preliminary analysis suggests thepresence of >10 GeV particles.

Published
1999

38. Milagrito Detection of TeV Emission from Mrk 501

Author

Atkins, R, Benbow, W, Berley, D, Chen, M-L, Coyne, DG, Delay, RS, Dingus, BL, Dorfan, DE, Ellsworth, RW, Evans, D, Falcone, A, Fleysher, L, Fleysher, R, Gisler, G, Goodman, JA, Haines, TJ, Hoffman, CM, Hugenberger, S, Kelley, LA, Leonor, I, Macri, J, McConnell, M, McCullough, JF, McEnery, JE, Miller, RS, Mincer, AI, Morales, MF, Nemethy, P, Ryan, JM, Schneider, M, Shen, B, Shoup, A, Sinnis, G, Smith, AJ, Sullivan, GW, Thompson, TN, Tumer, OT, Wang, K, Wascko, MO, Westerhoff, S, Williams, DA, Yang, T, and Yodh, GB

Subjects
astro-ph
Abstract

The Milagro water Cherenkov detector near Los Alamos, New Mexico, has beenoperated as a sky monitor at energies of a few TeV between February 1997 andApril 1998. Serving as a test run for the full Milagro detector, Milagrito hastaken data during the strong and long-lasting 1997 flare of Mrk 501. We presentresults from the analysis of Mrk 501 and compare the excess and backgroundrates with expectations from the detector simulations.

Published
1999

39. Search for a TeV Component of GRBs using the Milagrito Detector

Author

Atkins, R, Benbow, W, Berley, D, Chen, M-L, Coyne, DG, Delay, RS, Dingus, BL, Dorfan, DE, Ellsworth, RW, Evans, D, Falcone, A, Fleysher, L, Fleysher, R, Gisler, G, Goodman, JA, Haines, TJ, Hoffman, CM, Hugenberger, S, Kelley, LA, Leonor, I, Macri, J, McConnell, M, McCullough, JF, McEnery, JE, Miller, RS, Mincer, AI, Morales, MF, Nemethy, P, Ryan, JM, Schneider, M, Shen, B, Shoup, A, Sinnis, G, Smith, AJ, Sullivan, GW, Thompson, TN, Tumer, OT, Wang, K, Wascko, MO, Westerhoff, S, Williams, DA, Yang, T, and Yodh, GB

Subjects
astro-ph
Abstract

Observing gamma ray bursts (GRBs) in the TeV energy range can be extremelyvaluable in providing insight to GRB radiation mechanisms and in constrainingsource distances. The Milagrito detector was an air shower array which used thewater Cherenkov technique to search for TeV sources. Data from this detectorwas analyzed to look for a TeV component of GRBs coincident with low energy-rays detected by the BATSE instrument on the Compton Gamma Ray Observatory. Asample of 54 BATSE GRBs which were in the field of view of the Milagritodetector during its lifetime (February 1997 to May 1998) was used.

Published
1999

40. An All-Sky Search for Steady VHE Gamma-Ray Sources

Author

Atkins, R, Benbow, W, Berley, D, Chen, M-L, Coyne, DG, Delay, RS, Dingus, BL, Dorfan, DE, Ellsworth, RW, Evans, D, Falcone, A, Fleysher, L, Fleysher, R, Gisler, G, Goodman, JA, Haines, TJ, Hoffman, CM, Hugenberger, S, Kelley, LA, Leonor, I, Macri, J, McConnell, M, McCullough, JF, McEnery, JE, Miller, RS, Mincer, AI, Morales, MF, Nemethy, P, Ryan, JM, Schneider, M, Shen, B, Shoup, A, Sinnis, G, Smith, AJ, Sullivan, GW, Thompson, TN, Tumer, OT, Wang, K, Wascko, MO, Westerhoff, S, Williams, DA, Yang, T, and Yodh, GB

Subjects
astro-ph
Abstract

The Milagrito water Cherenkov detector in the Jemez Mountains near LosAlamos, New Mexico took data from February 1997 to April 1998. Milagrito servedas a prototype for the larger Milagro detector, which has just begunoperations. Milagrito was the first large-aperture gamma-ray detector withsensitivity to gamma rays below 1 TeV. We report here on a search for steadyemission from point sources over most of the northern sky using data fromMilagrito.

Published
1999

41. 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

42. 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

43. An All-Sky Search for Steady VHE Gamma-Ray Sources

Author

Atkins, R, Benbow, W, Berley, D, Chen, M-L, Coyne, DG, Delay, RS, Dingus, BL, Dorfan, DE, Ellsworth, RW, Evans, D, Falcone, A, Fleysher, L, Fleysher, R, Gisler, G, Goodman, JA, Haines, TJ, Hoffman, CM, Hugenberger, S, Kelley, LA, Leonor, I, Macri, J, McConnell, M, McCullough, JF, McEnery, JE, Miller, RS, Mincer, AI, Morales, MF, Nemethy, P, Ryan, JM, Schneider, M, Shen, B, Shoup, A, Sinnis, G, Smith, AJ, Sullivan, GW, Thompson, TN, Tumer, OT, Wang, K, Wascko, MO, Westerhoff, S, Williams, DA, Yang, T, Yodh, GB, Atkins, R, Benbow, W, Berley, D, Chen, M-L, Coyne, DG, Delay, RS, Dingus, BL, Dorfan, DE, Ellsworth, RW, Evans, D, Falcone, A, Fleysher, L, Fleysher, R, Gisler, G, Goodman, JA, Haines, TJ, Hoffman, CM, Hugenberger, S, Kelley, LA, Leonor, I, Macri, J, McConnell, M, McCullough, JF, McEnery, JE, Miller, RS, Mincer, AI, Morales, MF, Nemethy, P, Ryan, JM, Schneider, M, Shen, B, Shoup, A, Sinnis, G, Smith, AJ, Sullivan, GW, Thompson, TN, Tumer, OT, Wang, K, Wascko, MO, Westerhoff, S, Williams, DA, Yang, T, and Yodh, GB

Abstract

The Milagrito water Cherenkov detector in the Jemez Mountains near Los Alamos, New Mexico took data from February 1997 to April 1998. Milagrito served as a prototype for the larger Milagro detector, which has just begun operations. Milagrito was the first large-aperture gamma-ray detector with sensitivity to gamma rays below 1 TeV. We report here on a search for steady emission from point sources over most of the northern sky using data from Milagrito.

Published
2017

44. 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

45. Study of the Shadows of the Moon and the Sun with VHE Cosmic Rays

Author

Atkins, R, Benbow, W, Berley, D, Chen, M-L, Coyne, DG, Delay, RS, Dingus, BL, Dorfan, DE, Ellsworth, RW, Evans, D, Falcone, A, Fleysher, L, Fleysher, R, Gisler, G, Goodman, JA, Haines, TJ, Hoffman, CM, Hugenberger, S, Kelley, LA, Leonor, I, Macri, J, McConnell, M, McCullough, JF, McEnery, JE, Miller, RS, Mincer, AI, Morales, MF, Nemethy, P, Ryan, JM, Schneider, M, Shen, B, Shoup, A, Sinnis, G, Smith, AJ, Sullivan, GW, Thompson, TN, Tumer, OT, Wang, K, Wascko, MO, Westerhoff, S, Williams, DA, Yang, T, Yodh, GB, Atkins, R, Benbow, W, Berley, D, Chen, M-L, Coyne, DG, Delay, RS, Dingus, BL, Dorfan, DE, Ellsworth, RW, Evans, D, Falcone, A, Fleysher, L, Fleysher, R, Gisler, G, Goodman, JA, Haines, TJ, Hoffman, CM, Hugenberger, S, Kelley, LA, Leonor, I, Macri, J, McConnell, M, McCullough, JF, McEnery, JE, Miller, RS, Mincer, AI, Morales, MF, Nemethy, P, Ryan, JM, Schneider, M, Shen, B, Shoup, A, Sinnis, G, Smith, AJ, Sullivan, GW, Thompson, TN, Tumer, OT, Wang, K, Wascko, MO, Westerhoff, S, Williams, DA, Yang, T, and Yodh, GB

Abstract

Milagrito, a prototype for the Milagro detector, operated for 15 months in 1997-8 and collected 8.9 billion events. It was the first extensive air shower (EAS) array sensitive to showers intiated by primaries with energy below 1 TeV. The shadows of the sun and moon observed with cosmic rays can be used to study systematic pointing shifts and measure the angular resolution of EAS arrays. Below a few TeV, the paths of cosmic rays coming toward the earth are bent by the helio- and geo-magnetic fields. This is expected to distort and displace the shadows of the sun and the moon. The moon shadow, offset from the nominal (undeflected) position, has been observed with high statistical significance in Milagrito. This can be used to establish energy calibrations, as well as to search for the anti-matter content of the VHE cosmic ray flux. The shadow of the sun has also been observed with high significance.

Published
2017

46. Search for Short Duration Bursts of TeV Gamma Rays with the Milagrito Telescope

Author

Atkins, R, Benbow, W, Berley, D, Chen, M-L, Coyne, DG, Delay, RS, Dingus, BL, Dorfan, DE, Ellsworth, RW, Evans, D, Falcone, A, Fleysher, L, Fleysher, R, Gisler, G, Goodman, JA, Haines, TJ, Hoffman, CM, Hugenberger, S, Kelley, LA, Leonor, I, Macri, J, McConnell, M, McCullough, JF, McEnery, JE, Miller, RS, Mincer, AI, Morales, MF, Nemethy, P, Ryan, JM, Schneider, M, Shen, B, Shoup, A, Sinnis, G, Smith, AJ, Sullivan, GW, Thompson, TN, Tumer, OT, Wang, K, Wascko, MO, Westerhoff, S, Williams, DA, Yang, T, Yodh, GB, Atkins, R, Benbow, W, Berley, D, Chen, M-L, Coyne, DG, Delay, RS, Dingus, BL, Dorfan, DE, Ellsworth, RW, Evans, D, Falcone, A, Fleysher, L, Fleysher, R, Gisler, G, Goodman, JA, Haines, TJ, Hoffman, CM, Hugenberger, S, Kelley, LA, Leonor, I, Macri, J, McConnell, M, McCullough, JF, McEnery, JE, Miller, RS, Mincer, AI, Morales, MF, Nemethy, P, Ryan, JM, Schneider, M, Shen, B, Shoup, A, Sinnis, G, Smith, AJ, Sullivan, GW, Thompson, TN, Tumer, OT, Wang, K, Wascko, MO, Westerhoff, S, Williams, DA, Yang, T, and Yodh, GB

Abstract

The Milagrito water Cherenkov telescope operated for over a year. The most probable gamma-ray energy was ~1 TeV and the trigger rate was as high as 400 Hz. We have developed an efficient technique for searching the entire sky for short duration bursts of TeV photons. Such bursts may result from "traditional" gamma-ray bursts that were not in the field-of-view of any other instruments, the evaporation of primordial black holes, or some as yet undiscovered phenomenon. We have begun to search the Milagrito data set for bursts of duration 10 seconds. Here we will present the technique and the expected results. Final results will be presented at the conference.

Published
2017

47. Instrumented Water Tanks can Improve Air Shower Detector Sensitivity

Author

Atkins, R, Benbow, W, Berley, D, Chen, M-L, Coyne, DG, Delay, RS, Dingus, BL, Dorfan, DE, Ellsworth, RW, Evans, D, Falcone, A, Fleysher, L, Fleysher, R, Gisler, G, Goodman, JA, Haines, TJ, Hoffman, CM, Hugenberger, S, Kelley, LA, Leonor, I, Macri, J, McConnell, M, McCullough, JF, McEnery, JE, Miller, RS, Mincer, AI, Morales, MF, Nemethy, P, Ryan, JM, Schneider, M, Shen, B, Shoup, A, Sinnis, G, Smith, AJ, Sullivan, GW, Thompson, TN, Tumer, OT, Wang, K, Wascko, MO, Westerhoff, S, Williams, DA, Yang, T, Yodh, GB, Atkins, R, Benbow, W, Berley, D, Chen, M-L, Coyne, DG, Delay, RS, Dingus, BL, Dorfan, DE, Ellsworth, RW, Evans, D, Falcone, A, Fleysher, L, Fleysher, R, Gisler, G, Goodman, JA, Haines, TJ, Hoffman, CM, Hugenberger, S, Kelley, LA, Leonor, I, Macri, J, McConnell, M, McCullough, JF, McEnery, JE, Miller, RS, Mincer, AI, Morales, MF, Nemethy, P, Ryan, JM, Schneider, M, Shen, B, Shoup, A, Sinnis, G, Smith, AJ, Sullivan, GW, Thompson, TN, Tumer, OT, Wang, K, Wascko, MO, Westerhoff, S, Williams, DA, Yang, T, and Yodh, GB

Abstract

Previous works have shown that water Cherenkov detectors have superior sensitivity to those of scintillation counters as applied to detecting extensive air showers (EAS). This is in large part due to their much higher sensitivity to EAS photons which are more than five times more numerous than EAS electrons. Large area water Cherenkov detectors can be constructed relatively cheaply and operated reliably. A sparse detector array has been designed which uses these types of detectors to substantially increase the area over which the Milagro Gamma Ray Observatory collects EAS information. Improvements to the Milagro detector's performance characteristics and sensitivity derived from this array and preliminary results from a prototype array currently installed near the Milagro detector will be presented.

Published
2017

48. Search for a TeV Component of GRBs using the Milagrito Detector

Author

Atkins, R, Benbow, W, Berley, D, Chen, M-L, Coyne, DG, Delay, RS, Dingus, BL, Dorfan, DE, Ellsworth, RW, Evans, D, Falcone, A, Fleysher, L, Fleysher, R, Gisler, G, Goodman, JA, Haines, TJ, Hoffman, CM, Hugenberger, S, Kelley, LA, Leonor, I, Macri, J, McConnell, M, McCullough, JF, McEnery, JE, Miller, RS, Mincer, AI, Morales, MF, Nemethy, P, Ryan, JM, Schneider, M, Shen, B, Shoup, A, Sinnis, G, Smith, AJ, Sullivan, GW, Thompson, TN, Tumer, OT, Wang, K, Wascko, MO, Westerhoff, S, Williams, DA, Yang, T, Yodh, GB, Atkins, R, Benbow, W, Berley, D, Chen, M-L, Coyne, DG, Delay, RS, Dingus, BL, Dorfan, DE, Ellsworth, RW, Evans, D, Falcone, A, Fleysher, L, Fleysher, R, Gisler, G, Goodman, JA, Haines, TJ, Hoffman, CM, Hugenberger, S, Kelley, LA, Leonor, I, Macri, J, McConnell, M, McCullough, JF, McEnery, JE, Miller, RS, Mincer, AI, Morales, MF, Nemethy, P, Ryan, JM, Schneider, M, Shen, B, Shoup, A, Sinnis, G, Smith, AJ, Sullivan, GW, Thompson, TN, Tumer, OT, Wang, K, Wascko, MO, Westerhoff, S, Williams, DA, Yang, T, and Yodh, GB

Abstract

Observing gamma ray bursts (GRBs) in the TeV energy range can be extremely valuable in providing insight to GRB radiation mechanisms and in constraining source distances. The Milagrito detector was an air shower array which used the water Cherenkov technique to search for TeV sources. Data from this detector was analyzed to look for a TeV component of GRBs coincident with low energy -rays detected by the BATSE instrument on the Compton Gamma Ray Observatory. A sample of 54 BATSE GRBs which were in the field of view of the Milagrito detector during its lifetime (February 1997 to May 1998) was used.

Published
2017

49. Milagrito Detection of TeV Emission from Mrk 501

Author

Atkins, R, Benbow, W, Berley, D, Chen, M-L, Coyne, DG, Delay, RS, Dingus, BL, Dorfan, DE, Ellsworth, RW, Evans, D, Falcone, A, Fleysher, L, Fleysher, R, Gisler, G, Goodman, JA, Haines, TJ, Hoffman, CM, Hugenberger, S, Kelley, LA, Leonor, I, Macri, J, McConnell, M, McCullough, JF, McEnery, JE, Miller, RS, Mincer, AI, Morales, MF, Nemethy, P, Ryan, JM, Schneider, M, Shen, B, Shoup, A, Sinnis, G, Smith, AJ, Sullivan, GW, Thompson, TN, Tumer, OT, Wang, K, Wascko, MO, Westerhoff, S, Williams, DA, Yang, T, Yodh, GB, Atkins, R, Benbow, W, Berley, D, Chen, M-L, Coyne, DG, Delay, RS, Dingus, BL, Dorfan, DE, Ellsworth, RW, Evans, D, Falcone, A, Fleysher, L, Fleysher, R, Gisler, G, Goodman, JA, Haines, TJ, Hoffman, CM, Hugenberger, S, Kelley, LA, Leonor, I, Macri, J, McConnell, M, McCullough, JF, McEnery, JE, Miller, RS, Mincer, AI, Morales, MF, Nemethy, P, Ryan, JM, Schneider, M, Shen, B, Shoup, A, Sinnis, G, Smith, AJ, Sullivan, GW, Thompson, TN, Tumer, OT, Wang, K, Wascko, MO, Westerhoff, S, Williams, DA, Yang, T, and Yodh, GB

Abstract

The Milagro water Cherenkov detector near Los Alamos, New Mexico, has been operated as a sky monitor at energies of a few TeV between February 1997 and April 1998. Serving as a test run for the full Milagro detector, Milagrito has taken data during the strong and long-lasting 1997 flare of Mrk 501. We present results from the analysis of Mrk 501 and compare the excess and background rates with expectations from the detector simulations.

Published
2017

50. 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

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