VAMOS: A pathfinder for the HAWC gamma-ray observatory

Abeysekara, Anushka Udara; Alfaro, R.; Álvarez, C.; Álvarez, José David Ruiz; Ángeles, Fernando; Arceo, R.; Arteaga‐Velázquez, J. C.; Ávila-Aroche, A.; Solares, H. A. Ayala; Badillo, C.; Barber, Ahron S.; Baughman, B. M.; Bautista-Elivar, N.; González, J. Becerra; Belmont, E.; Benítez, E.; BenZvi, S.; Berley, D.; Bernal, A.; Rosales, M. Bonilla; Braun, J.; Caballero─López, R. A.; Caballero-Mora, K. S.; Cabrera, I.; Carramiñana, A.; Castañeda‐Martinez, Laura; Castillo, M.; Cotti, U.; Cotzomi, J.; Fuente, Eduardo de la; León, C. De; DeYoung, T.; Díaz-Azuara, A.; Díaz‐Cruz, L.; Hernández, R. Díaz; Díaz-Vélez, J. C.; Dingus, B. L.; Dultzin, D.; DuVernois, Michael; Ellsworth, R. W.; Fernández, A. Álvarez; Fiorino, D. W.; Fraija, N.; Galindo, A.; García–Torales, Guillermo; Garfias, F.; González, Antonio J.; González, L. X.; González, M. M.; Goodman, J. A.; Grabski, V.; Gussert, M.; Guzmán-Cerón, C.; Hampel-Arias, Z.; Harding, J. Patrick; Hernández–Cervantes, L.; Hui, C. M.; Hüntemeyer, P.; Imran, Asif; Iriarte, A.; Karn, P.; Kieda, D.; Kunde, G. J.; Langarica, R.; Lara, A.; Lara, Gerardo; Lauer, R.; Lee, W.H.; Lennarz, D.; Vargas, H. León; Linares, Edgar Casimiro; Linnemann, J.; Longo, M.; Luna-García, R.; Marinelli, A.; Martínez, L. A.; Martínez, H.; Martı́nez, O.; Martínez-Castro, J.; Martos, M.; Matthews, John; McEnery, J. E.; Torres, E. Mendoza; Miranda-Romagnoli, P.; Moreno, E.; Mostafá, M.; Nava, J.; Nellen, L.; Newbold, M.; Noriega-Papaqui, R.; Oceguera-Becerra, T.; Page, Dany; Patricelli, B.; Pelayo, R.; Pérez-Pérez, E. G.; Pretz, J.; Ramírez, Iván; Rentería, A.; Rivière, C.; Rosa-González, D.; Ruiz-Sala, F.; Ruiz-Velasco, E.; Ryan, J. M.; Sacahui, J. R.; Salazar, H.; Salesa, F.; Sandoval, A.; Santos, E.; Schneider, M.; Silich, Sergiy; Sinnis, G.; Smith, A. J.; Woodle, K. Sparks; Springer, R. W.; Suárez, F.; Taboada, I.; Tepe, A.; Toale, P. A.; Tollefson, K.; Torres, I.; Tinoco, S.; Ukwatta, T. N.; Galicia, J. F. Valdés; Vanegas, Pablo; Vázquez, A.; Villaseñor, L.; Wall, W. F.; Weisgarber, T.; Westerhoff, S.; Wisher, I. G.; Wood, J.; Yodh, G.; Younk, P.; Zaborov, D.; Zepeda, A.; Zhou, H.

doi:10.1016/j.astropartphys.2014.08.004

Cited by 20 publications

(19 citation statements)

References 22 publications

(19 reference statements)

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“…Infrastructure The installation of one former HEGRA telescope mount at the HAWC site [17] and thus the easy availability of equipment and support from the HAWC observatory, allows to test equipment and procedures at this site. The HAWC site itself is also suitable for the operation of the telescope, but located at 4,100 m, it provides less stable weather conditions than Observatorio Astronomico Nacional (OAN) at San Pedro Mártir.…”

Section: Project Plan and Statusmentioning

confidence: 99%

Monitoring at TeV Energies with M@TE

Alfaro¹,

Bernal²,

Bretz³

et al. 2017

Proceedings of 35th International Cosmic Ray Conference — PoS(ICRC2017)

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Blazars are extremely variable objects emitting radiation across the electromagnetic spectrum and showing variability on time scales from minutes to years. Simultaneous multi-wavelength observations are crucial for understanding the emission mechanisms. In particular the study of their TeV emission is relevant to test the dominant radiative process at such energies (e.g. leptonic models predict a correlation between X-ray and TeV emission). As well, the correlation with the bump at low energy or the possible common detection with a neutrino signal can be relevant to constrain the physical model. From radio via optical and from X-ray to gamma rays, a variety of instruments, as OVRO and Fermi, are already monitoring blazars. At TeV energies, long-term monitoring is currently carried out by HAWC and FACT. Towards 24/7 continuous observations, the goal is to have similar monitoring telescopes at locations around the globe in order to close temporal gaps and compile light curves with homogeneous sensitivity. With the M@TE (Monitoring at TeV energies) project, we are planning to install an Imaging Air Cherenkov Telescope equipped with an improved version of the FACT camera and the mechanical structure of one of the mounts of the HEGRA experiment at the site of San Pedro Mártir in Mexico. Featuring excellent observation conditions, this location provides a variety of instruments from radio to optical wavelength allowing for coordinated multi-wavelength blazar studies. In this work, we will present the status of the project.

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Section: Project Plan and Statusmentioning

confidence: 99%

Monitoring at TeV Energies with M@TE

Alfaro¹,

Bernal²,

Bretz³

et al. 2017

Proceedings of 35th International Cosmic Ray Conference — PoS(ICRC2017)

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“…After the operation of the engineering prototype "The Verification And Measuring of the Observatory System (VAMOS)" [12] built in 2011, 4 stages were considered during the modular construction of HAWC. In September 2012, the first 30 WCD were completed and operated as an engineering prototype.…”

Section: The Main Detectormentioning

confidence: 99%

Cosmic Ray Astrophysics using The High Altitude Water Cherenkov (HAWC) Observatory in México

et al. 2017

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Abstract. The High-Altitude Water Cherenkov (HAWC) TeV gamma-ray Observatory in México is ready to search and study gamma-ray emission regions, extremely high-energy cosmic-ray sources, and to identify transient phenomena. With a better Gamma/Hadron rejection method than other similar experiments, it will play a key role in triggering multi-wavelength and multi-messenger studies of active galaxies (AGN), gammaray bursts (GRB), supernova remnants (SNR), pulsar wind nebulae (PWN), Galactic Plane Sources, and Cosmic Ray Anisotropies. It has an instantaneous field-of-view of ∼2 str, equivalent to 15% of the whole sky and continuous operation (24 hours per day). The results obtained by HAWC-111 (111 detectors in operation) were presented on the proceedings of the International Cosmic Ray Conference 2015 and in [1]. The results obtained by HAWC-300 (full operation) are now under analysis and will be published in forthcoming papers starting in 2017 (see preliminary results on http://www.hawc-observatory.org/news/). Here we present the HAWC contributions on cosmic ray astrophysics via anisotropies studies, summarizing the HAWC detector and its upgrading by the installation of "outriggers".

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“…It took 15 years to extend the measurements to higher energies. This year two collaborations, Tibet and HAWC, presented the highest-energy Crab Nebula spectra [1], [2]; both spectra continue beyond 100 TeV. Besides improving the knowledge about the source, this detection allows us to better constrain some scenarios of new physics such as hypothetical violation of Lorentz Invariance (LI).…”

mentioning

confidence: 99%

“…LV in the electron sector is not considered here since those constraints are more stronger than in the photon sector [17], see also discussion in [16]. 2 The mass scale M LV corresponds to the parameter c…”

mentioning

confidence: 99%