Description of atmospheric conditions at the Pierre Auger Observatory using the Global Data Assimilation System (GDAS)

Abreu, P.; Aglietta, M.; Ahlers, M.; Ahn, E. J.; Albuquerque, I. F. M.; Allard, Denis; Allekotte, I.; Allen, Jeff; Allison, P.; Almela, A.; Castillo, J.; Álvarez-Muñiz, J.; Ambrosio, M.; Aminaei, A.; Anchordoqui, Luis A.; Andringa, S.; Antičić, T.; Aramo, C.; Arganda, E.; Arqueros, F.; Asorey, H.; Assis, P.; Aublin, J.; Ave, M.; Avenier, M.; Ávila, G.; Bäcker, T.; Badescu, A. M.; Balzer, M.; Barber, K. B.; Barbosa, A. F.; Bardenet, Rémi; Barroso, S. L. C.; Baughman, B. M.; Bäuml, J.; Beatty, J. J.; Becker, B. R.; Becker, Karl‐Heinz; Belĺetoile, A.; Bellido, J. A.; BenZvi, S.; Bérat, C.; Bertou, X.; Biermann, P. L.; Billoir, P.; Blanco, F.; Blanco, Miguel Rodríguez; Bleve, C.; Blümer, H.; Bohã̌cov́a, M.; Boncioli, D.; Bonifazi, C.; Bonino, R.; Borodai, N.; Brack, J.; Brancus, I. M.; Brogueira, P.; Brown, W. C.; Bruijn, R.; Buchholz, P.; Bueno, A.; Burton, R. E.; Caballero-Mora, K. S.; Caccianiga, B.; Caramete, L.; Caruso, R.; Castellina, A.; Catalano, O.; Cataldi, G.; Cazón, L.; Cester, R.; Chauvin, J.; Cheng, S. H.; Чиавасса, А.; Chinellato, J. A.; Diaz, J. C.; Chudoba, J.; Clay, R. W.; Coluccia, M. R.; Conceião, R.; Contreras, F.; Cook, H.; Cooper, M. J.; Coppens, J.; Cordier, A.; Coutu, S.; Covault, C. E.; Creusot, A.; Criss, A.; Cronin, J.; Curutiu, A.; Dagoret, S.; Dallier, R.; Daniel, B.; Dasso, S.; Daumiller, K.; Dawson, B. R.; Almeida, R. M. de; Domenico, Manlio De; Donato, C. De; Jong, S. J. De; Vega, G. De La; Mello, W. J. M. de; Neto, J. R. T. de Mello; Mitri, I. De; Souza, V. de; Vries, Krijn de; Peral, L. del; Río, Mariano del; Deligny, O.; Dembinski, H.-P.; Dhital, N.; Giulio, C. Di; Castro, M. L. Díaz; Diep, P. N.; Diogo, F.; Dobrigkeit, C.; Docters, W.; D’Olivo, J. C.; Dong, P. N.; Dorofeev, A.; Anjos, J. C. dos; Dova, M. T.; D’Urso, D.; Duţan, I.; Ebr, Jan; Engel, R.; Erdmann, M.; Escobar, C. O.; Espadanal, J.; Etchegoyen, A.; Luis, P. Facal San; Tapia, I. Fajardo; Falcke, H.; Farrar, Glennys R.; Fauth, A. C.; Fazzini, N.; Ferguson, A. P.; Fick, B.; Filevich, A.; Filipčić, A.; Fliescher, S.; Fracchiolla, C. E.; Fraenkel, E. D.; Fratu, Octavian; Fröhlich, U.; Fuchs, B.; Gaïor, R.; Gamarra, R. F.; Gambetta, S.; García, Beatriz; Roca, S. T. Garcia; García-Gámez, D.; Garcia-Pinto, D.; Gascón, A.; Gemmeke, H.; Ghia, P. L.; Giaccari, U.; Giller, M.; Glass, H.; Gold, M.; Golup, G.; Albarracin, F. Gómez; Berisso, M. Gómez; Vitale, Primo F. Gómez; Gonalves, P.; Gonzalez, D.; González, J. G.; Gookin, B.; Gorgi, A.; Gouffon, P.; Grashorn, E.; Grebe, S.; Griffith, N.; Grigat, M.; Grillo, A. F.; Guardincerri, Y.; Guarino, F.; Guedes, G. P.; Guzmán, A.; Hansen, P.; Harari, D.; Harrison, T. A.; Harton, J. L.; Haungs, A.; Hebbeker, T.; Heck, D.; Hervé, A. E.; Hojvat, C.; Hollon, N.; Holmes, V. C.; Homola, P.; Hörandel, J. R.; Horneffer, A.; Horváth, P.; Hrabovský, M.; Huber, Daniel; Huege, T.; Insolia, A.; Ionita, F.; Italiano, A.; Jarne, C.; Jiraskova, S.; Josebachuili, M.; Kadija, K.; Kampert, K.‐H.; Karhan, P.; Kasper, P. A.; Kégl, Balázs; Keilhauer, B.; Keivani, A.; Kelley, J. L.; Kemp, E.; Kieckhafer, R. M.; Klages, H. O.; Kleifges, M.; Kleinfeller, J.; Knapp, J.; Koang, D. H.; Kotera, Kumiko; Krohm, N.; Krömer, O.; Kruppke-Hansen, D.; Kuehn, F.; Kuempel, D.; Kulbartz, J. K.; Kunka, N.; Rosa, G. La; Lachaud, C.; LaHurd, D.; Latronico, L.; Lauer, R.; Lautridou, P.; Coz, S. Le; Leão, M. S. A. B.; Lebrun, D.; Lebrun, P.; Oliveira, M. A. Leigui de; Letessier‐Selvon, A.; Lhenry-Yvon, I.; Link, K.; López, R.; Agúera, A. López; Louedec, K.; Bahilo, J. J. Lozano; Lu, Lu; Lucero, A.; Ludwig, M.; Lyberis, H.; Maccarone, M. C.; Macolino, C.; Maldera, S.; Mandat, D.; Mantsch, P.; Mariazzi, A. G.; Marín, J.; Marin, V.; Maris, Ioana Codrina; Falcon, H. R. Marquez; Marsella, G.; Martello, D.; Martin, L.; Martinez, O.; Bravo, O. Martínez; Mathes, H.J.; Matthews, John; Matthiae, G.; Maurel, D.; Maurizio, D.; Mazur, Péter; Medina‐Tanco, G.; Melissas, M.; Melo, D.; Menichetti, E.; Menshikov, A.; Mertsch, Philipp; Meurer, C.; Mićanović, Saša; Micheletti, M. I.; Minaya, I. A.; Miramonti, L.; Molina-Bueno, L.; Mollerach, Silvia; Monasor, M.; Ragaigne, D. Monnier; Montanet, F.; Morales, B.; Morello, C.; Moreno, E.; Moreno, J. C.; Mostafá, M.; Moura, C. A.; Müller, M. A.; Müller, G.; Münchmeyer, Moritz; Mussa, R.; Navarra, G.; Navarro, J. L. La Rosa; Navas, S.; Nečesal, P.; Nellen, L.; Nelles, A.; Neuser, J.; Nhung, P. T.; Niechciol, Marcus; Niemietz, L.; Nierstenhoefer, N.; Nitz, D.; Nosek, D.; Nožka, L.; Oehlschläger, J.; Olinto, Angela V.; Ortiz, María J.; Pacheco, N.; Selmi-Dei, D. Pakk; Palatka, M.; Pallotta, J.; Palmieri, N.; Parente, G.; Parizot, E.; Parra, A.; Pastor, S.; Paul, T.; Pech, M.; Pękala, Jan; Pelayo, R.; Pepe, I. M.; Perrone, L.; Pesce, R.; Petermann, E.; Petrera, S.; Petrinca, P.; Petrolini, A.; Petrov, Y.; Pfendner, C.; Piegaia, R.; Pierog, T.; Pieroni, P.; Pimenta, M.; Pirronello, V.; Platino, M.; Ponce, V. H.; Pontz, M.; Porcelli, A.; Privitera, P.; Prouza, M.; Quel, E. J.; Querchfeld, S.; Rautenberg, J.; Ravel, O.; Ravignani, D.; Revenu, B.; Řídký, J.; Riggi, S.; Risse, M.; Ristori, P.; Rivera, H.; Rizi, Vincenzo; Roberts, J.; Carvalho, W. Rodrigues de; Rodríguez, G.; Martino, J. Rodrı́guez; Rojo, Juan; Rodríguez-Cabo, I.; Rodríguez-Friás, M. D.; Ros, G.; Rosado, J.; Rössler, T.; Roth, M.; Rouillé-d’Orfeuil, B.; Roulet, Esteban; Rovero, A. C.; Rühle, C.; Sǎftoiu, A.; Salamida, F.; Salazar, H.; Greus, F. Salesa; Salina, G.; Sánchez, F.; Santo, C. E.; Santos, Edivaldo Moura; Santos, Eva; Sarazin, F.; Sarkar, Biswajit; Sarkar, Subir; Sato, R.; Scharf, N.; Scherini, V.; Schieler, H.; Schiffer, P.; Schmidt, A.; Scholten, Olaf; Schoorlemmer, H.; Schovancová, J.; Schovánek, Petr; Schröder, Frank G.; Schulte, S.; Schuster, David M.; Sciutto, S. J.; Scuderi, M.; Segreto, A.; Settimo, M.; Shadkam, A.; Shellard, R. C.; Sidelnik, I.; Sigl, G.; López, H. H. Silva; Sima, O.; Śmiałkowski, A.; Šmída, R.; Snow, G. R.; Sommers, P.; Sorokin, J.; Spinka, H.; Squartini, R.; Srivastava, Y. N.; Stanič, S.; Stapleton, J.; Stasielak, J.; Stéphan, M.; Stutz, A.; Suárez, F.; Suomijärvi, T.; Supanitsky, A. D.; Šuša, T.; Sutherland, M.; Swain, J.; Szadkowski, Z.; Szuba, M.; Tapia, A.; Tartare, M.; Tacu, O.; Ruiz, C. G. Tavera; Tcaciuc, R.; Thảo, Nguyễn Thị Phương; Thomas, D.; Tiffenberg, J.; Timmermans, C.; Tkaczyk, W.; Peixoto, C. J. Todero; Toma, G.; Tomankova, L.; Tomé, B.; Tonachini, A.; Trávničék, P.; Tridapalli, D. B.; Tristram, G.; Trovato, E.; Tueros, M.; Ulrich, R.; Unger, Michael; Urban, M.; Galicia, J. F. Valdés; Valiño, I.; Valore, L.; Berg, A. M. van den; Varela, E.; Vargascárdenas, B.; Vázquez, J. R.; Vázquez, R. A.; Veberič, D.; Verzi, V.; Vícha, J.; Videla, M.; Villaseñor, L.; Wahlberg, H.; Wahrlich, P.; Wainberg, O.; Walz, D.; Watson, A. A.; Weber, M.; Weidenhaupt, K.; Weindl, A.; Werner, F.; Westerhoff, S.; Whelan, B. J.; Widom, A.; Wieczorek, G.; Wiencke, L.; Wilczyñska, B.; Wilczyński, H.; Will, Martin; Williams, Christopher B.; Winchen, T.; Wommer, M.; Wundheiler, B.; Yamamoto, Tokonatsu; Yapici, T.; Younk, P.; Yuan, G.; Yushkov, A.; Zamorano, B.; Zas, E.; Zavrtanik, D.; Zavrtanik, M.; Zaw, I.; Zepeda, A.; Zhu, Yan; Silva, M. Zimbres; Ziolkowski, M.

doi:10.1016/j.astropartphys.2011.12.002

Cited by 75 publications

(57 citation statements)

References 13 publications

Supporting

Mentioning

Contrasting

Unclassified

Order By: Relevance

“…We follow the approach that is used by the Pierre Auger Collaboration as described by Abreu et al [43] This work also contains comparisons of atmospheric depth profiles predicted by GDAS and in situ measurements with weather balloons. The differences are typically smaller than 1 g=cm 2 , except for altitudes very close to the ground.…”

Section: Uncertainty On X Maxmentioning

confidence: 99%

Method for high precision reconstruction of air showerXmaxusing two-dimensional radio intensity profiles

et al. 2014

Self Cite

View full text Add to dashboard Cite

The mass composition of cosmic rays contains important clues about their origin. Accurate measurements are needed to resolve longstanding issues such as the transition from Galactic to extraGalactic origin and the nature of the cutoff observed at the highest energies. Composition can be studied by measuring the atmospheric depth of the shower maximum X max of air showers generated by high-energy cosmic rays hitting the Earth's atmosphere. We present a new method to reconstruct X max based on radio measurements. The radio emission mechanism of air showers is a complex process that creates an asymmetric intensity pattern on the ground. The shape of this pattern strongly depends on the longitudinal development of the shower. We reconstruct X max by fitting two-dimensional intensity profiles, simulated with CoREAS, to data from the Low Frequency Array (LOFAR) radio telescope. In the dense LOFAR core, air showers are detected by hundreds of antennas simultaneously. The simulations fit the data very well, indicating that the radiation mechanism is now well understood. The typical uncertainty on the reconstruction of X max for LOFAR showers is 17 g=cm 2 .

show abstract

Section: Uncertainty On X Maxmentioning

confidence: 99%

Method for high precision reconstruction of air showerXmaxusing two-dimensional radio intensity profiles

et al. 2014

Self Cite

View full text Add to dashboard Cite

show abstract

“…Measurements from a radiosonde campaign will provide the information to reduce the uncertainties in the models used to simulate the Cherenkov light at the CTA site. In addition, radiosondes can be used to validate global or mesoscale models, which have been used to characterize sites hosting experiments to detect high energy cosmic rays ( [6], [7]). …”

Section: Introductionmentioning

confidence: 99%

Density profile characterization and modeling at Paranal and Armazones 2k sites

2017

View full text Add to dashboard Cite

Abstract. The Cherenkov Telescope Array (CTA) in the southern hemisphere will be installed at Armazones 2k site in northern Chile. Scarce atmospheric observations are available in the region, particularly radiosonde data. This study analyzes radiosondes launched at Paranal observatory, located at about 21 km from the CTA site, from 24 October and 4 November 2011, to understand the behavior of density in the atmosphere near the CTA site. High-resolution numerical simulations with the Weather Research and Forecasting (WRF) model are validated with Paranal radiosondes to quantify its ability to represent the atmospheric conditions in the region. In addition, the seasonal and diurnal evolution of atmospheric density at the CTA site were studied during 2011 using the high-resolution weather forecasts from the WRF model.

show abstract

“…This is not possible with photometric observations of standard stars at robotic telescopes. As already shown by us in [1] and independently at the Pierre Auger facilities by [10], a properly adapted GDAS model already gives a very good description. This can be now further improved including the grid refinements down to 1 km resolution described by [15].…”

Section: Discussionmentioning

confidence: 68%

“…3). The AUGER facility in Argentina ( [10]) use a similar technique with better agreement, as this observing site is not as close to the sea. .…”

Section: Thermal Components Of the Atmospherementioning

confidence: 99%

The Innsbruck/ESO sky models and telluric correction tools

Kimeswenger

Kausch

Noll

et al. 2015

EPJ Web of Conferences

View full text Add to dashboard Cite

Abstract. Ground-based astronomical observations are influenced by scattering and absorption by molecules and aerosols in the Earth's atmosphere. They are additionally affected by background emission from scattered moonlight, zodiacal light, scattered starlight, the atmosphere, and the telescope. These influences vary with environmental parameters like temperature, humidity, and chemical composition. Nowadays, this is corrected during data processing, mainly using semi-empirical methods and calibration by known sources. Part of the Austrian ESO in-kind contribution was a new model of the sky background, which is more complete and comprehensive than previous models.While the ground based astronomical observatories just have to correct for the line-of-sight integral of these effects, thě Cerenkov telescopes use the atmosphere as the primary detector. The measured radiation originates at lower altitudes and does not pass through the entire atmosphere. Thus, a decent knowledge of the profile of the atmosphere at any time is required. The latter cannot be achieved by photometric measurements of stellar sources. We show here the capabilities of our sky background model and data reduction tools for ground-based optical/infrared telescopes. Furthermore, we discuss the feasibility of monitoring the atmosphere above any observing site, and thus, the possible application of the method forČerenkov telescopes.

show abstract

Description of atmospheric conditions at the Pierre Auger Observatory using the Global Data Assimilation System (GDAS)

Cited by 75 publications

References 13 publications

Method for high precision reconstruction of air showerXmaxusing two-dimensional radio intensity profiles

Method for high precision reconstruction of air showerXmaxusing two-dimensional radio intensity profiles

Density profile characterization and modeling at Paranal and Armazones 2k sites

The Innsbruck/ESO sky models and telluric correction tools

Contact Info

Product

Resources

About