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282 results on '"Strafella, F"'

256. THE M31 PIXEL LENSING PLAN CAMPAIGN: MACHO LENSING AND SELF-LENSING SIGNALS.

Author

Novati, S. Calchi, Bozza, V., Bruni, I., Dall'Ora, M., Paolis, F. De, Dominik, M., Gualandi, R., Ingrosso, G., Jetzer, Ph., Mancini, L., Nucita, A., Safonova, M., Scarpetta, G., Sereno, M., Strafella, F., Subramaniam, A., Gould, A., and Collaboration, PLAN

Subjects
DARK matter, HALOS (Meteorology), GRAVITATIONAL lenses, MICROLENSING (Astrophysics), INTERSTELLAR medium
Abstract

We present the final analysis of the observational campaign carried out by the PLAN (Pixel Lensing Andromeda) collaboration to detect a dark matter signal in form of MACHOs through the microlensing effect. The campaign consists of about 1 month/year observations carried out over 4 years (2007-2010) at the 1.5 m Cassini telescope in Loiano (Astronomical Observatory of BOLOGNA, OAB) plus 10 days of data taken in 2010 at the 2 m Himalayan Chandra Telescope monitoring the central part of M31 (two fields of about 13′ × 12.′6). We establish a fully automated pipeline for the search and the characterization of microlensing flux variations. As a result, we detect three microlensing candidates. We evaluate the expected signal through a full Monte Carlo simulation of the experiment completed by an analysis of the detection efficiency of our pipeline. We consider both “self lensing” and “MACHO lensing” lens populations, given by M31 stars and dark matter halo MACHOs, in M31 and the Milky Way, respectively. The total number of events is consistent with the expected self-lensing rate. Specifically, we evaluate an expected signal of about two self-lensing events. As for MACHO lensing, for full 0.5(10–2) M☼ MACHO halos, our prediction is for about four (seven) events. The comparatively small number of expected MACHO versus self-lensing events, together with the small number statistics at our disposal, do not enable us to put strong constraints on that population. Rather, the hypothesis, suggested by a previous analysis, on the MACHO nature of OAB-07-N2, one of the microlensing candidates, translates into a sizeable lower limit for the halo mass fraction in form of the would-be MACHO population, f, of about 15% for 0.5 M☼ MACHOs. [ABSTRACT FROM AUTHOR]

Published
2014
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257. A Herschelstudy of YSO evolutionary stages and formation timelines in two fields of the Hi-GAL survey*

Author

Elia, D., Schisano, E., Molinari, S., Robitaille, T., Anglés-Alcázar, D., Bally, J., Battersby, C., Benedettini, M., Billot, N., Calzoletti, L., Di Giorgio, A. M., Faustini, F., Li, J. Z., Martin, P., Morgan, L., Motte, F., Mottram, J. C., Natoli, P., Olmi, L., Paladini, R., Piacentini, F., Pestalozzi, M., Pezzuto, S., Polychroni, D., Smith, M. D., Strafella, F., Stringfellow, G. S., Testi, L., Thompson, M. A., Traficante, A., and Veneziani, M.

Abstract

We present a first study of the star-forming compact dust condensations revealed by Herschelin the two 2° × 2° Galactic Plane fields centered at [$\ell$, b] = [30°, 0°] and [$\ell$, b] =[59°, 0°] , respectively, and observed during the science demonstration phase for the HerschelInfrared GALactic plane survey (Hi-GAL) key-project. Compact source catalogs extracted for the two fields in the five Hi-GAL bands (70, 160, 250, 350 and 500 μm) were merged based on simple criteria of positional association and spectral energy distribution (SED) consistency into a final catalog which contains only coherent SEDs with counterparts in at least three adjacent Herschelbands. These final source lists contain 528 entries for the $\ell$= 30° field, and 444 entries for the $\ell$= 59° field. The SED coverage has been augmented with ancillary data at 24 μm and 1.1 mm. SED modeling for the subset of 318 and 101 sources (in the two fields, respectively) for which the distance is known was carried out using both a structured star/disk/envelope radiative transfer model and a simple isothermal grey-body. Global parameters like mass, luminosity, temperature and dust properties have been estimated. The Lbol/Menvratio spans four orders of magnitudes from values compatible with the pre-protostellar phase to embedded massive zero-age main sequence stars. Sources in the $\ell$= 59° field have on average lower L/M, possibly outlining an overall earlier evolutionary stage with respect to the sources in the $\ell$= 30° field. Many of these cores are actively forming high-mass stars, although the estimated core surface densities appear to be an order of magnitude below the 1 g cm-2critical threshold for high-mass star formation.

Published
2010

258. Direct estimate of cirrus noise in HerschelHi-GAL images*

Author

Martin, P. G., Miville-Deschênes, M.-A., Roy, A., Bernard, J.-P., Molinari, S., Billot, N., Brunt, C., Calzoletti, L., DiGiorgio, A. M., Elia, D., Faustini, F., Joncas, G., Mottram, J. C., Natoli, P., Noriega-Crespo, A., Paladini, R., Robitaille, J. F., Strafella, F., Traficante, A., and Veneziani, M.

Abstract

In Herschelimages of the Galactic plane and many star forming regions, a major factor limiting our ability to extract faint compact sources is cirrus confusion noise, operationally defined as the “statistical error to be expected in photometric measurements due to confusion in a background of fluctuating surface brightness”. The histogram of the flux densities of extracted sources shows a distinctive faint-end cutoff below which the catalog suffers from incompleteness and the flux densities become unreliable. This empirical cutoff should be closely related to the estimated cirrus noise and we show that this is the case. We compute the cirrus noise directly, both on Herschelimages from which the bright sources have been removed and on simulated images of cirrus with statistically similar fluctuations. We connect these direct estimates with those from power spectrum analysis, which has been used extensively to predict the cirrus noise and provides insight into how it depends on various statistical properties and photometric operational parameters. We report multi-wavelength power spectra of diffuse Galactic dust emission from Hi-GAL observations at 70 to 500 μm within Galactic plane fields at l= 30 °and l= 59 °. We find that the exponent of the power spectrum is about –3. At 250 μm, the amplitude of the power spectrum increases roughly as the square of the median brightness of the map and so the expected cirrus noise scales linearly with the median brightness. For a given region, the wavelength dependence of the amplitude can be described by the square of the spectral energy distribution (SED) of the dust emission. Generally, the confusion noise will be a worse problem at longer wavelengths, because of the combination of lower angular resolution and the rising power spectrum of cirrus toward lower spatial frequencies, but the photometric signal to noise will also depend on the relative SED of the source compared to the cirrus.

Published
2010

259. Timing analysis of a sample of five cataclysmic variable candidates observed by the XMM–Newton satellite.

Author

Nucita, A A, Lezzi, S M, De Paolis, F, Strafella, F, Licchelli, D, Franco, A, and Maiorano, M

Subjects
*CATACLYSMIC variable stars, *X-ray binaries, *PHOTOMETRY
Abstract

Intermediate polars are a class of cataclysmic variables in which a white dwarf accretes material from a companion star. The intermediate polar nature confirmation usually derives from the detection of two periods in both X -ray and optical photometry. In this respect, the high-energy signal is often characterized by modulations on the white dwarf spin and the orbital period. However, noting that the periodograms may be characterized by strong features also at the synodic period and/or other sidebands, the timing analysis of the X -ray signal may offer the unique possibility to firmly discover an intermediate polar candidate. Here, we concentrate on a sample of five cataclysmic variable binary candidates: i.e. SAXJ1748.2-2808, 1RXS J211336.1 + 542226, CXOGC J174622.7-285218, CXOGC J174517.4-290650, and V381 Vel, listed in the IPHome catalogue. Our main aim is to confirm if they belong to the intermediate polar class or not. The results of our analysis show that we can safely assess the intermediate polar nature of all the considered sources, apart for the case of V381 Vel which instead behaves like a cataclysmic variable of the polar subclass. Moreover, the source SAXJ1748.2-2808, previously classified as an HMXB, appears to be, most likely, an intermediate polar variable. [ABSTRACT FROM AUTHOR]

Published
2022
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260. Cavezzo, the first Italian meteorite recovered by the PRISMA fireball network. Orbit, trajectory, and strewn-field

Author

C. A. Volpicelli, Enrico Cascone, M. Belluso, Stefano Basso, Riccardo Smareglia, Cyril Blanpain, A. Andreis, G. Monti, M. E. Bertaina, S. Masiero, Tonino Pisanu, G. Interrante, F. Lippolis, G. Tigani Sava, G. Valente, D. Barghini, Sonia Zorba, Alberto Buzzoni, V. Gagliarducci, M. Soldi, Fabio Manca, Cristina Knapic, Cristian Carli, M. Montesarchio, Giovanni Pratesi, S. Rubinetti, D. Licchelli, T. Avoscan, A. Misiano, D. Cricchio, F. Federici, P. Colombetti, M. Romeo, G. Ascione, Daniele Gardiol, Alberto Cellino, A. Gerardi, François Colas, M. Suvieri, F. Strafella, R. Di Luca, F. Bernardi, A. Nastasi, J. L. Rault, S. Jeanne, C. Simoncelli, R. Stanga, Monica Lazzarin, C. Romeni, C. Cattaneo, S. Rasetti, Albino Carbognani, A. Malgoyre, Jader Monari, P. Demaria, Carla Taricco, M. Tombelli, Gabriele Giuli, Giuseppe Leto, A. Di Dato, N. Rizzi, M. Di Carlo, R. Serra, A. Pegoraro, Sylvain Bouley, S. Pietronave, Matteo Albani, R. Baldini, D. Guidetti, F. Salvati, M. Montemaggi, G. D’Agostino, Elisa Londero, A. Zollo, Chiara Marmo, F. Mannucci, W. Riva, J. Vaubaillon, Brigitte Zanda, Mirel Birlan, M. Rigoni, P. Morini, Jérôme Gattacceca, U. Repetti, M. Pavone, R. Zagarella, G. Cremonese, S. Meucci, S. Lera, R. Bellitto, M. D’Elia, A. Balestrero, F. Affaticati, M. De Maio, T. Carriero, R. Masi, S. Mancuso, Giovanni B. Valsecchi, Emilio Molinari, N. Pugno, R. Salerno, R. Bonino, R. Pardini, Pierre Vernazza, P. Russo, A. Bussi, V. Moggi Cecchi, C. Benna, G. M. Stirpe, K. Boros, J. Lecubin, P. Bacci, Gabriele Umbriaco, M. Costa, D. Selvestrel, E. Pace, M. Di Martino, R. Vairetti, E. Colombi, L. Betti, P. Trivero, P. Volpini, Institut de Mécanique Céleste et de Calcul des Ephémérides (IMCCE), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Lille-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Centre européen de recherche et d'enseignement des géosciences de l'environnement (CEREGE), Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Collège de France (CdF (institution))-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Collège de France (CdF (institution))-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Institut National de la Recherche Agronomique (INRA), Gardiol, D., Barghini, D., Buzzoni, A., Carbognani, A., Di Carlo, M., Di Martino, M., Knapic, C., Londero, E., Pratesi, G., Rasetti, S., Riva, W., Salerno, R., Stirpe, G. M., Valsecchi, G. B., Volpicelli, C. A., Zorba, S., Colas, F., Zanda, B., Bouley, S., Jeanne, S., Malgoyre, A., Birlan, M., Blanpain, C., Gattacceca, J., Lecubin, J., Marmo, C., Rault, J. L., Vaubaillon, J., Vernazza, P., Affaticati, F., Albani, M., Andreis, A., Ascione, G., Avoscan, T., Bacci, P., Baldini, R., Balestrero, A., Basso, S., Bellitto, R., Belluso, M., Benna, C., Bernardi, F., Bertaina, M. E., Betti, L., Bonino, R., Boros, K., Bussi, A., Carli, C., Carriero, T., Cascone, E., Cattaneo, C., Cellino, A., Colombetti, P., Colombi, E., Costa, M., Cremonese, G., Cricchio, D., D'Agostino, G., D'Elia, M., De Maio, M., Demaria, P., Di Dato, A., Di Luca, R., Federici, F., Gagliarducci, V., Gerardi, A., Giuli, G., Guidetti, D., Interrante, G., Lazzarin, M., Lera, S., Leto, G., Licchelli, D., Lippolis, F., Manca, F., Mancuso, S., Mannucci, F., Masi, R., Masiero, S., Meucci, S., Misiano, A., Moggi Cecchi, V., Molinari, E., Monari, J., Montemaggi, M., Montesarchio, M., Monti, G., Morini, P., Nastasi, A., Pace, E., Pardini, R., Pavone, M., Pegoraro, A., Pietronave, S., Pisanu, T., Pugno, N., Repetti, U., Rigoni, M., Rizzi, N., Romeni, C., Romeo, M., Rubinetti, S., Russo, P., Salvati, F., Selvestrel, D., Serra, R., Simoncelli, C., Smareglia, R., Soldi, M., Stanga, R., Strafella, F., Suvieri, M., Taricco, C., Tigani Sava, G., Tombelli, M., Trivero, P., Umbriaco, G., Vairetti, R., Valente, G., Volpini, P., Zagarella, R., Zollo, A., Gardiol D., Barghini D., Buzzoni A., Carbognani A., Di Carlo M., Di Martino M., Knapic C., Londero E., Pratesi G., Rasetti S., Riva W., Salerno R., Stirpe G.M., Valsecchi G.B., Volpicelli C.A., Zorba S., Colas F., Zanda B., Bouley S., Jeanne S., Malgoyre A., Birlan M., Blanpain C., Gattacceca J., Lecubin J., Marmo C., Rault J.L., Vaubaillon J., Vernazza P., Affaticati F., Albani M., Andreis A., Ascione G., Avoscan T., Bacci P., Baldini R., Balestrero A., Basso S., Bellitto R., Belluso M., Benna C., Bernardi F., Bertaina M.E., Betti L., Bonino R., Boros K., Bussi A., Carli C., Carriero T., Cascone E., Cattaneo C., Cellino A., Colombetti P., Colombi E., Costa M., Cremonese G., Cricchio D., D'Agostino G., D'Elia M., De Maio M., Demaria P., Di Dato A., Di Luca R., Federici F., Gagliarducci V., Gerardi A., Giuli G., Guidetti D., Interrante G., Lazzarin M., Lera S., Leto G., Licchelli D., Lippolis F., Manca F., Mancuso S., Mannucci F., Masi R., Masiero S., Meucci S., Misiano A., Moggi Cecchi V., Molinari E., Monari J., Montemaggi M., Montesarchio M., Monti G., Morini P., Nastasi A., Pace E., Pardini R., Pavone M., Pegoraro A., Pietronave S., Pisanu T., Pugno N., Repetti U., Rigoni M., Rizzi N., Romeni C., Romeo M., Rubinetti S., Russo P., Salvati F., Selvestrel D., Serra R., Simoncelli C., Smareglia R., Soldi M., Stanga R., Strafella F., Suvieri M., Taricco C., Tigani Sava G., Tombelli M., Trivero P., Umbriaco G., Vairetti R., Valente G., Volpini P., Zagarella R., Zollo A., and ITA

Subjects
meteoroids -methods: data analysis -techniques: image processing, 010502 geochemistry & geophysics, 01 natural sciences, Strewn field, meteorites, 0103 physical sciences, meteors, meteoroids, 010303 astronomy & astrophysics, meteoroid, 0105 earth and related environmental sciences, Physics, Meteoroid, image processing, methods: data analysis, techniques, meteor, Astronomy, Astronomy and Astrophysics, meteorite, Meteorite, Space and Planetary Science, [SDU]Sciences of the Universe [physics], data analysi [methods], Trajectory, Orbit (control theory)
Abstract

Two meteorite pieces have been recovered in Italy, near the town of Cavezzo (Modena), on 2020 January 4th. The associated fireball was observed on the evening of New Year’s Day 2020 by eight all-sky cameras of the PRISMA fireball network, a partner of FRIPON. The computed trajectory had an inclination angle of approximately 68° and a velocity at infinity of 12.8 km s−1. Together with the relatively low terminal height, estimated as 21.5 km, those values were indicating the significant possibility of a meteorite dropping event, as additionally confirmed by the non-zero residual total mass. The strewn-field was computed taking into account the presence of two bright light flashes, revealing that the meteoroid had been very likely subject to fragmentation. Three days after the event, two samples, weighing 3.1 and 52.2 g, were collected as a result of a dedicated field search and thanks to the involvement of the local people. The two pieces were immediately recognized as freshly fallen fragments of meteorite. The computed orbital elements, compared with the ones of known Near-Earth Asteroids from the NEODyS database, are compatible with one asteroid only; 2013 VC10. The estimated original mass of the meteoroid, 3.5 kg, and size, approximately 13 cm, is so far the smallest among the current 35 cases in which meteorites were recovered from precise strewn-field computation thanks to observational data. This result demonstrates the effectiveness of accurate processing of fireball network data even on challenging events generated by small size meteoroids.

Published
2021
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261. Search for ultrarelativistic magnetic monopoles with the Pierre Auger Observatory

Author

Johannes Schulz, M. Pimenta, A. Aab, J. Biteau, E.M. Holt, A. Saleh, L. Caramete, Maria-Teresa Dova, M. R. Hampel, H. Gemmeke, Florian Lukas Briechle, M. I. Micheletti, Sarka Wykes, D. Torres Machado, Octavian Fratu, Paula Gina Isar, F. Salesa Greus, R.C. dos Anjos, Julian Rautenberg, J. Espadanal, M. Palatka, G. Cataldi, A. C. Fauth, Luis A. Nunez, Carla Bonifazi, Jose A. Bellido, Jaime Alvarez-Muñiz, G. Kukec Mezek, John N. Matthews, R. M. Kieckhafer, E. Varela, J.D. Sanabria Gomez, D. Yelos, M. E. Bertaina, I. Naranjo, A. Menshikov, R. Sarmento, S. Sonntag, Marcus Niechciol, Jesús Peña-Rodríguez, O. Wainberg, Alexandru Gherghel-Lascu, T. Suomijärvi, A. van Vliet, Andreas Haungs, B. García, Tobias Winchen, Antonio Bueno, M. Josebachuili, L. Lopes, Alberto Daniel Supanitsky, G. De Mauro, C. A. Sarmiento, I.D. Vergara Quispe, A. Dorofeev, Gualberto Avila, R. López, Ingomar Allekotte, Jörg R. Hörandel, Karen S. Caballero-Mora, F. Canfora, Z. Zong, Diego Harari, B. Gookin, S. Querchfeld, M. Zavrtanik, Paul Sommers, A. Blanco, L. Ochilo, Angela V. Olinto, C. Di Giulio, Markus Roth, J. F. Valdés Galicia, Miroslav Hrabovský, I. De Mitri, Dieter Heck, P. Gouffon, Igor Katkov, P. H. Nguyen, E. M. Santos, L. Niemietz, R.J. Barreira Luz, G. P. Guedes, Toshihiro Fujii, G. A. Anastasi, P. Abreu, Martin Urban, A. Kuotb Awad, J. L. Harton, S. G. Blaess, B. Vargas Cárdenas, Fausto Guarino, J. Pallotta, E. J. Quel, M. J. Cooper, F. Sánchez, Q. Luce, Carlos Medina, Martin Erdmann, D. Ravignani, I. A. Minaya, B. Keilhauer, André Schulz, L. Villaseñor, Luis A. Anchordoqui, J. Debatin, Peter Hansen, Tim Niggemann, Peter Buchholz, D. Nosek, Bruce R. Dawson, A. Fuster, Tim Huege, H. Glass, I. Valiño, S. J. Sciutto, Katrin Link, Valerio Pirronello, M. A. Leigui de Oliveira, I.M. Brancus, M. Platino, Danielle LaHurd, Olivier Deligny, J. Neuser, Johannes Schumacher, C. Aramo, Juan Carlos D'Olivo, Roger W Clay, B. Revenu, J. R. Vázquez, G. S. Varner, Marco Aglietta, V. Scherini, Esteban Roulet, M. Suarez Durán, Andreas Weindl, B. Mitrica, Heino Falcke, Francesco Strafella, I. C. Mariş, Hernan Wahlberg, C. J. Todero Peixoto, Stefano D'Amico, P. Sanchez-Lucas, P. Kasper, M. Gómez Berisso, M. Ambrosio, R. C. Shellard, F. Salamida, J. Stasielak, S. Coutu, J. Vicha, Norberto Fazzini, D. Garcia-Pinto, Miroslav Pech, R. R. Prado, Petr Schovanek, Antonio Insolia, Maria Rita Coluccia, Bruno Daniel, A. Parra, Foteini Oikonomou, J. J. Masías Meza, Jeffrey A. Johnsen, S. Quinn, Günter Sigl, D. Nitz, Andrej Dundovic, Lorenzo Caccianiga, V. M. Theodoro, Dusan Mandat, P. Ristori, M. Trini, Alexandra Saftoiu, Alina Mihaela Badescu, I. Lhenry-Yvon, A. Cancio, Pavel Horvath, N. Krohm, G. Rodriguez Fernandez, G. Torralba Elipe, R. Krause, P. Stassi, C. Porowski, M. Prouza, V. Verzi, Mariangela Settimo, J. Rodriguez Rojo, Nicolás González, Radomir Smida, S. Müller, Jan Pękala, A. E. Herve, L. R. Wiencke, B. Sarkar, H. Nožka, Jose Chinellato, Christian Glaser, A. Yushkov, B. Andrada, Marco Torri, J. D. Swain, David Schmidt, M. L. Díaz Castro, G. Farrar, Carola Dobrigkeit, M. Plum, A. G. Chavez, A. Gorgi, Denis Stanca, Sofia Andringa, R. Cester, Nicusor Arsene, A. Tapia, Florian Gaté, M. Kleifges, D. Zavrtanik, B. Tome, Peter Mazur, G. Müller, V. de Souza, Max Malacari, Lili Yang, Enrique Zas, Alan Watson, A. Di Matteo, Francesca Zuccarello, A. Letessier-Selvon, Denise Boncioli, B. Wundheiler, H. Wilczyński, P. Billoir, Dariusz Glas, Fernando Contreras, O. Kambeitz, Corinne Berat, E. Mayotte, K. H. Becker, M. Unger, Gregory R Snow, A. Segreto, Philipp Papenbreer, Lorenzo Cazon, Q. Hasankiadeh, Mihai Niculescu-Oglinzanu, J. Alvarez Castillo, L. Molina-Bueno, D. Melo, I. Al Samarai, Piotr Homola, David Walz, Ana Martina Botti, I. Jandt, F. Diogo, R. M. de Almeida, G. Marsella, Marco Giammarchi, R. Squartini, T. Paul, L. A. S. Pereira, Maria Giller, A. Taboada, D. Pakk Selmi-Dei, R. Sato, L. Nellen, Ralf Ulrich, C. Morello, P.F. Gómez Vitale, G. C. Hill, R. A. Vázquez, Gaia Silli, Ralph Engel, A. Filipčič, Paul M. Mantsch, F. Sarazin, A. Bridgeman, G. Medina-Tanco, J. Ridky, G. van Aar, D. Reinert, Marc Weber, M. Mallamaci, Tanguy Pierog, S. J. Saffi, F. G. Schröder, Benedikt Zimmermann, Rúben Conceição, Zbigniew Szadkowski, Peter L. Biermann, Rodrigo Pelayo, Stijn Buitink, E. Santos, R. Piegaia, Markus Lauscher, F. Pedreira, A. Śmiałkowski, J. Phuntsok, M. M. Freire, R. Ramos-Pollan, Paolo Privitera, J. Hulsman, W. Rodrigues de Carvalho, J. W. Cronin, P. van Bodegom, P. Lebrun, Nataliia Borodai, Lukas Middendorf, Christine Peters, Hernán Asorey, Martina Bohacova, J. Sorokin, S. J. De Jong, V. Novotny, L. Valore, Rossella Caruso, A. Lucero, S. Mathys, M. Erfani, Octavian Sima, Ugo Giaccari, F. Montanet, Petr Travnicek, M. Schauer, Alan Coleman, Trent D. Grubb, Juan Manuel Figueira, Roberta Colalillo, A. G. Mariazzi, J. R. T. de Mello Neto, Peter Gorham, P. L. Ghia, Charles Timmermans, L. Collica, Marcio Aparecido Muller, L. Perrone, Jiri Chudoba, Thomas Harrison, P. Pieroni, F. Arqueros, N. Kunka, R. Gaior, F. Suarez, Thomas Hebbeker, Sergio Dasso, Tristan Sudholz, Hermann-Josef Mathes, Kai Daumiller, J. A.J. Matthews, Xavier Bertou, Jeffrey Brack, Olaf Scholten, A. Zepeda, Humberto Ibarguen Salazar, Pedro Assis, Harald Schieler, A. Etchegoyen, P. Heimann, E. Kemp, Serguei Vorobiov, D. Mockler, O. A. Taborda, H. Martinez, Miguel Mostafa, L. Tomankova, A. López Casado, Brian Fick, Samo Stanič, J. J. Beatty, Silvia Mollerach, G. Matthiae, Julien Aublin, A. Shadkam, D. Martello, S. Jansen, David Wittkowski, A. C. Rovero, C. Bleve, Alexandru Balaceanu, Vincenzo Rizi, M. Ziolkowski, O. Martínez Bravo, Thomas Bretz, Corbin Covault, Geraldina Golup, Alexander Grillo, Lino Miramonti, M. Risse, Jonathan Blazek, G. Parente, Carlos Hojvat, R. Legumina, M. Buscemi, Jan Ebr, Sergio Petrera, D. Rogozin, J. de Oliveira, H.O. Klages, Alejandro Almela, S. Messina, Julian Kemp, Gaetano Salina, Michael Schimp, A.M. van den Berg, Darko Veberič, Alex Kääpä, Colin Baus, J. Kleinfeller, Daniel Kuempel, Carlos Escobar, Ivone F. M. Albuquerque, Ke Fang, Karl-Heinz Kampert, Antonella Castellina, Research unit Astroparticle Physics, Research unit Nuclear & Hadron Physics, Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE), Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Pierre et Marie Curie - Paris 6 (UPMC), Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Institut de Physique Nucléaire d'Orsay (IPNO), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), Laboratoire SUBATECH Nantes (SUBATECH), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Nantes (UN)-Mines Nantes (Mines Nantes), Pierre Auger, Aab A., Abreu P., Aglietta M., Al Samarai I., Albuquerque I.F.M., Allekotte I., Almela A., Alvarez Castillo J., Alvarez-Muñiz J., Ambrosio M., Anastasi G.A., Anchordoqui L., Andrada B., Andringa S., Aramo C., Arqueros F., Arsene N., Asorey H., Assis P., Aublin J., Avila G., Badescu A.M., Balaceanu A., Barreira Luz R.J., Baus C., Beatty J.J., Becker K.H., Bellido J.A., Berat C., Bertaina M.E., Bertou X., Biermann P.L., Billoir P., Biteau J., Blaess S.G., Blanco A., Blazek J., Bleve C., Boháčová M., Boncioli D., Bonifazi C., Borodai N., Botti A.M., Brack J., Brancus I., Bretz T., Bridgeman A., Briechle F.L., Buchholz P., Bueno A., Buitink S., Buscemi M., Caballero-Mora K.S., Caccianiga L., Cancio A., Canfora F., Caramete L., Caruso R., Castellina A., Cataldi G., Cazon L., Cester R., Chavez A.G., Chinellato J.A., Chudoba J., Clay R.W., Colalillo R., Coleman A., Collica L., Coluccia M.R., Conceição R., Contreras F., Cooper M.J., Coutu S., Covault C.E., Cronin J., D'Amico S., Daniel B., Dasso S., Daumiller K., Dawson B.R., de Almeida R.M., de Jong S.J., De Mauro G., de Mello Neto J.R.T., De Mitri I., de Oliveira J., de Souza V., Debatin J., Deligny O., Di Giulio C., Di Matteo A., Díaz Castro M.L., Diogo F., Dobrigkeit C., D'Olivo J.C., Dorofeev A., dos Anjos R.C., Dova M.T., Dundovic A., Ebr J., Engel R., Erdmann M., Erfani M., Escobar C.O., Espadanal J., Etchegoyen A., Falcke H., Fang K., Farrar G., Fauth A.C., Fazzini N., Fick B., Figueira J.M., Filipčič A., Fratu O., Freire M.M., Fujii T., Fuster A., Gaior R., García B., Garcia-Pinto D., Gaté F., Gemmeke H., Gherghel-Lascu A., Ghia P.L., Giaccari U., Giammarchi M., Giller M., Głas D., Glaser C., Glass H., Golup G., Gómez Berisso M., Gómez Vitale P.F., González N., Gookin B., Gorgi A., Gorham P., Gouffon P., Grillo A.F., Grubb T.D., Guarino F., Guedes G.P., Hampel M.R., Hansen P., Harari D., Harrison T.A., Harton J.L., Hasankiadeh Q., Haungs A., Hebbeker T., Heck D., Heimann P., Herve A.E., Hill G.C., Hojvat C., Holt E., Homola P., Hörandel J.R., Horvath P., Hrabovský M., Huege T., Hulsman J., Insolia A., Isar P.G., Jandt I., Jansen S., Johnsen J.A., Josebachuili M., Kääpä A., Kambeitz O., Kampert K.H., Kasper P., Katkov I., Keilhauer B., Kemp E., Kemp J., Kieckhafer R.M., Klages H.O., Kleifges M., Kleinfeller J., Krause R., Krohm N., Kuempel D., Kukec Mezek G., Kunka N., Kuotb Awad A., Lahurd D., Lauscher M., Lebrun P., Legumina R., Leigui de Oliveira M.A., Letessier-Selvon A., Lhenry-Yvon I., Link K., Lopes L., López R., López Casado A., Luce Q., Lucero A., Malacari M., Mallamaci M., Mandat D., Mantsch P., Mariazzi A.G., Mariş I.C., Marsella G., Martello D., Martinez H., Martínez Bravo O., Masías Meza J.J., Mathes H.J., Mathys S., Matthews J., Matthews J.A.J., Matthiae G., Mayotte E., Mazur P.O., Medina C., Medina-Tanco G., Melo D., Menshikov A., Messina S., Micheletti M.I., Middendorf L., Minaya I.A., Miramonti L., Mitrica B., Mockler D., Molina-Bueno L., Mollerach S., Montanet F., Morello C., Mostafá M., Müller G., Muller M.A., Müller S., Naranjo I., Nellen L., Neuser J., Nguyen P.H., Niculescu-Oglinzanu M., Niechciol M., Niemietz L., Niggemann T., Nitz D., Nosek D., Novotny V., Nožka H., Núñez L.A., Ochilo L., Oikonomou F., Olinto A., Pakk Selmi-Dei D., Palatka M., Pallotta J., Papenbreer P., Parente G., Parra A., Paul T., Pech M., Pedreira F., Pękala J., Pelayo R., Peña-Rodriguez J., Pereira L. A. S., Perrone L., Peters C., Petrera S., Phuntsok J., Piegaia R., Pierog T., Pieroni P., Pimenta M., Pirronello V., Platino M., Plum M., Porowski C., Prado R.R., Privitera P., Prouza M., Quel E.J., Querchfeld S., Quinn S., Ramos-Pollan R., Rautenberg J., Ravignani D., Reinert D., Revenu B., Ridky J., Risse M., Ristori P., Rizi V., Rodrigues de Carvalho W., Rodriguez Fernandez G., Rodriguez Rojo J., Rogozin D., Roth M., Roulet E., Rovero A.C., Saffi S.J., Saftoiu A., Salamida F., Salazar H., Saleh A., Salesa Greus F., Salina G., Sanabria Gomez J.D., Sánchez F., Sanchez-Lucas P., Santos E.M., Santos E., Sarazin F., Sarkar B., Sarmento R., Sarmiento C.A., Sato R., Schauer M., Scherini V., Schieler H., Schimp M., Schmidt D., Scholten O., Schovánek P., Schröder F.G., Schulz A., Schulz J., Schumacher J., Sciutto S.J., Segreto A., Settimo M., Shadkam A., Shellard R.C., Sigl G., Silli G., Sima O., Śmiałkowski A., Šmída R., Snow G.R., Sommers P., Sonntag S., Sorokin J., Squartini R., Stanca D., Stanič S., Stasielak J., Stassi P., Strafella F., Suarez F., Suarez Durán M., Sudholz T., Suomijärvi T., Supanitsky A.D., Swain J., Szadkowski Z., Taboada A., Taborda O.A., Tapia A., Theodoro V.M., Timmermans C., Todero Peixoto C.J., Tomankova L., Tomé B., Torralba Elipe G., Torres Machado D., Torri M., Travnicek P., Trini M., Ulrich R., Unger M., Urban M., Valdés Galicia J.F., Valiño I., Valore L., van Aar G., van Bodegom P., van den Berg A.M., van Vliet A., Varela E., Vargas Cárdenas B., Varner G., Vázquez J.R., Vázquez R.A., Veberič D., Vergara Quispe I.D., Verzi V., Vicha J., Villaseñor L., Vorobiov S., Wahlberg H., Wainberg O., Walz D., Watson A.A., Weber M., Weindl A., Wiencke L., Wilczyński H., Winchen T., Wittkowski D., Wundheiler B., Wykes S., Yang L., Yelos D., Yushkov A., Zas E., Zavrtanik D., Zavrtanik M., Zepeda A., Zimmermann B., Ziolkowski M., Zong Z., Zuccarello F., Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Mines Nantes (Mines Nantes)-Université de Nantes (UN)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Aab, A., Abreu, P., Aglietta, M., Al Samarai, I., Albuquerque, I. F. M., Allekotte, I., Almela, A., Alvarez Castillo, J., Alvarez Muñiz, J., Ambrosio, M., Anastasi, G. A., Anchordoqui, L., Andrada, B., Andringa, S., Aramo, C., Arqueros, F., Arsene, N., Asorey, H., Assis, P., Aublin, J., Avila, G., Badescu, A. M., Balaceanu, A., Barreira Luz, R. J., Baus, C., Beatty, J. J., Becker, K. H., Bellido, J. A., Berat, C., Bertaina, M. E., Bertou, X., Biermann, P. L., Billoir, P., Biteau, J., Blaess, S. G., Blanco, A., Blazek, J., Bleve, Carla, Boháčová, M., Boncioli, D., Bonifazi, C., Borodai, N., Botti, A. M., Brack, J., Brancus, I., Bretz, T., Bridgeman, A., Briechle, F. L., Buchholz, P., Bueno, A., Buitink, S., Buscemi, M., Caballero Mora, K. S., Caccianiga, L., Cancio, A., Canfora, F., Caramete, L., Caruso, R., Castellina, A., Cataldi, G., Cazon, L., Cester, R., Chavez, A. G., Chinellato, J. A., Chudoba, J., Clay, R. W., Colalillo, R., Coleman, A., Collica, L., Coluccia, MARIA RITA, Conceição, R., Contreras, F., Cooper, M. J., Coutu, S., Covault, C. E., Cronin, J., D'Amico, Stefano, Daniel, B., Dasso, S., Daumiller, K., Dawson, B. R., de Almeida, R. M., de Jong, S. J., De Mauro, G., de Mello Neto, J. R. T., DE MITRI, Ivan, de Oliveira, J., de Souza, V., Debatin, J., Deligny, O., Di Giulio, C., Di Matteo, A., Díaz Castro, M. L., Diogo, F., Dobrigkeit, C., D'Olivo, J. C., Dorofeev, A., dos Anjos, R. C., Dova, M. T., Dundovic, A., Ebr, J., Engel, R., Erdmann, M., Erfani, M., Escobar, C. O., Espadanal, J., Etchegoyen, A., Falcke, H., Fang, K., Farrar, G., Fauth, A. C., Fazzini, N., Fick, B., Figueira, J. M., Filipčič, A., Fratu, O., Freire, M. M., Fujii, T., Fuster, A., Gaior, R., García, B., Garcia Pinto, D., Gaté, F., Gemmeke, H., Gherghel Lascu, A., Ghia, P. L., Giaccari, U., Giammarchi, M., Giller, M., Głas, D., Glaser, C., Glass, H., Golup, G., Gómez Berisso, M., Gómez Vitale, P. F., González, N., Gookin, B., Gorgi, A., Gorham, P., Gouffon, P., Grillo, A. F., Grubb, T. D., Guarino, F., Guedes, G. P., Hampel, M. R., Hansen, P., Harari, D., Harrison, T. A., Harton, J. L., Hasankiadeh, Q., Haungs, A., Hebbeker, T., Heck, D., Heimann, P., Herve, A. E., Hill, G. C., Hojvat, C., Holt, E., Homola, P., Hörandel, J. R., Horvath, P., Hrabovský, M., Huege, T., Hulsman, J., Insolia, A., Isar, P. G., Jandt, I., Jansen, S., Johnsen, J. A., Josebachuili, M., Kääpä, A., Kambeitz, O., Kampert, K. H., Kasper, P., Katkov, I., Keilhauer, B., Kemp, E., Kemp, J., Kieckhafer, R. M., Klages, H. O., Kleifges, M., Kleinfeller, J., Krause, R., Krohm, N., Kuempel, D., Kukec Mezek, G., Kunka, N., Kuotb Awad, A., Lahurd, D., Lauscher, M., Lebrun, P., Legumina, R., Leigui de Oliveira, M. A., Letessier Selvon, A., Lhenry Yvon, I., Link, K., Lopes, L., López, R., López Casado, A., Luce, Q., Lucero, A., Malacari, M., Mallamaci, M., Mandat, D., Mantsch, P., Mariazzi, A. G., Mariş, I. C., Marsella, Giovanni, Martello, Daniele, Martinez, H., Martínez Bravo, O., Masías Meza, J. J., Mathes, H. J., Mathys, S., Matthews, J., Matthews, J. A. J., Matthiae, G., Mayotte, E., Mazur, P. O., Medina, C., Medina Tanco, G., Melo, D., Menshikov, A., Messina, S., Micheletti, M. I., Middendorf, L., Minaya, I. A., Miramonti, L., Mitrica, B., Mockler, D., Molina Bueno, L., Mollerach, S., Montanet, F., Morello, C., Mostafá, M., Müller, G., Muller, M. A., Müller, S., Naranjo, I., Nellen, L., Neuser, J., Nguyen, P. H., Niculescu Oglinzanu, M., Niechciol, M., Niemietz, L., Niggemann, T., Nitz, D., Nosek, D., Novotny, V., Nožka, H., Núñez, L. A., Ochilo, L., Oikonomou, F., Olinto, A., Pakk Selmi Dei, D., Palatka, M., Pallotta, J., Papenbreer, P., Parente, G., Parra, A., Paul, T., Pech, M., Pedreira, F., Pękala, J., Pelayo, R., Peña Rodriguez, J., Pereira, L. A. S., Perrone, Lorenzo, Peters, C., Petrera, S., Phuntsok, J., Piegaia, R., Pierog, T., Pieroni, P., Pimenta, M., Pirronello, V., Platino, M., Plum, M., Porowski, C., Prado, R. R., Privitera, P., Prouza, M., Quel, E. J., Querchfeld, S., Quinn, S., Ramos Pollan, R., Rautenberg, J., Ravignani, D., Reinert, D., Revenu, B., Ridky, J., Risse, M., Ristori, P., Rizi, V., Rodrigues de Carvalho, W., Rodriguez Fernandez, G., Rodriguez Rojo, J., Rogozin, D., Roth, M., Roulet, E., Rovero, A. C., Saffi, S. J., Saftoiu, A., Salamida, F., Salazar, H., Saleh, A., Salesa Greus, F., Salina, G., Sanabria Gomez, J. D., Sánchez, F., Sanchez Lucas, P., Santos, E. M., Santos, E., Sarazin, F., Sarkar, B., Sarmento, R., Sarmiento, C. A., Sato, R., Schauer, M., Scherini, V., Schieler, H., Schimp, M., Schmidt, D., Scholten, O., Schovánek, P., Schröder, F. G., Schulz, A., Schulz, J., Schumacher, J., Sciutto, S. J., Segreto, A., Settimo, M., Shadkam, A., Shellard, R. C., Sigl, G., Silli, G., Sima, O., Śmiałkowski, A., Šmída, R., Snow, G. R., Sommers, P., Sonntag, S., Sorokin, J., Squartini, R., Stanca, D., Stanič, S., Stasielak, J., Stassi, P., Strafella, Francesco, Suarez, F., Suarez Durán, M., Sudholz, T., Suomijärvi, T., Supanitsky, A. D., Swain, J., Szadkowski, Z., Taboada, A., Taborda, O. A., Tapia, A., Theodoro, V. M., Timmermans, C., Todero Peixoto, C. J., Tomankova, L., Tomé, B., Torralba Elipe, G., Torres Machado, D., Torri, M., Travnicek, P., Trini, M., Ulrich, R., Unger, M., Urban, M., Valdés Galicia, J. F., Valiño, I., Valore, L., van Aar, G., van Bodegom, P., van den Berg, A. M., van Vliet, A., Varela, E., Vargas Cárdenas, B., Varner, G., Vázquez, J. R., Vázquez, R. A., Veberič, D., Vergara Quispe, I. D., Verzi, V., Vicha, J., Villaseñor, L., Vorobiov, S., Wahlberg, H., Wainberg, O., Walz, D., Watson, A. A., Weber, M., Weindl, A., Wiencke, L., Wilczyński, H., Winchen, T., Wittkowski, D., Wundheiler, B., Wykes, S., Yang, L., Yelos, D., Yushkov, A., Zas, E., Zavrtanik, D., Zavrtanik, M., Zepeda, A., Zimmermann, B., Ziolkowski, M., Zong, Z., Zuccarello, F., Bleve, C., Colalillo, Roberta, Coluccia, M. R., D'Amico, S., De Almeida, R. M., De Jong, S. J., De Mello Neto, J. R. T., De Mitri, I., De Oliveira, J., De Souza, V., Dos Anjos, R. C., Guarino, Fausto, Leigui De Oliveira, M. A., Marsella, G., Martello, D., Pkala, J., Perrone, L., Rodrigues De Carvalho, W., Strafella, F., Valore, Laura, Van Aar, G., Van Bodegom, P., Van Den Berg, A. M., and Van Vliet, A.

Subjects
FLUORESCENCE YIELD, Astronomy, magnetic monopole, magnetic field, Astrophysics, 7. Clean energy, 01 natural sciences, Observatory, UHE Cosmic Rays, air-shower, Monte Carlo, 010303 astronomy & astrophysics, Magnetic Monopoles, media_common, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Settore FIS/01 - Fisica Sperimentale, Astrophysics::Instrumentation and Methods for Astrophysics, critical phenomena, ENERGY LOSS, DETECTOR, Auger, Magnetic field, observatory, Lorentz factor, ComputingMethodologies_DOCUMENTANDTEXTPROCESSING, symbols, Física nuclear, fluorescence, Astrophysics - High Energy Astrophysical Phenomena, spatial distribution [showers], Lorentz, atmosphere [showers], energy, FLUX, Nuclear and High Energy Physics, [PHYS.ASTR.HE]Physics [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], air, media_common.quotation_subject, Astrophysics::High Energy Astrophysical Phenomena, UHE [cosmic radiation], Magnetic monopole, FOS: Physical sciences, Cosmic ray, Nuclear physics, symbols.namesake, cosmic rays, 0103 physical sciences, ddc:530, High Energy Physics, Ciencias Exactas, fluorescence [detector], Pierre Auger Observatory, background, 010308 nuclear & particles physics, Física, ASTROFÍSICA, Universe, flux, ultrarelativistic magnetic monopoles, Air shower, 13. Climate action, Experimental High Energy Physics, relativistic, galaxy, ENERGY-LOSS
Abstract

We present a search for ultra-relativistic magnetic monopoles with the Pierre Auger Observatory. Such particles, possibly a relic of phase transitions in the early universe, would deposit a large amount of energy along their path through the atmosphere, comparable to that of ultrahigh-energy cosmic rays (UHECRs). The air shower profile of a magnetic monopole can be effectively distinguished by the fluorescence detector from that of standard UHECRs. No candidate was found in the data collected between 2004 and 2012, with an expected background of less than 0.1 event from UHECRs. The corresponding 90% confidence level (C.L.) upper limits on the flux of ultra-relativistic magnetic monopoles range from 10⁻¹⁹ (cm² sr s)⁻¹ for a Lorentz factor γ = 10⁹ to 2.5 × 10⁻²¹ (cm² sr s)⁻¹ for γ = 10¹². These results -the first obtained with a UHECR detector- improve previously published limits by up to an order of magnitude., La lista completa de autores que integran el documento puede consultarse en el archivo., Facultad de Ciencias Exactas, Instituto de Física La Plata

Published
2016
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262. New variable sources revealed by DECam toward the LMC: The first 15 deg2.

Author

Franco, A., Nucita, A.A., De Paolis, F., Strafella, F., and Sacquegna, S.

Subjects
*SIGNAL-to-noise ratio, *LIGHT curves, *DARK energy
Abstract

The Dark Energy Camera (DECam) is a sensitive, wide field instrument mounted at the prime focus of the 4 mV. Blanco Telescope in Chile. Beside its main objectives, i.e. understanding the growth and evolution of structures in the Universe, the camera offers the opportunity to observe a ∼ 3 deg 2 field of view in one single pointing and, with an adequate cadence, to identify the variable sources contained. In this paper, we present the result of a DECam observational campaign toward the LMC and give a catalogue of the observed variable sources. We considered all the available DECam observations of the LMC, acquired during 32 nights over a period of two years (from February 2018 to January 2020), and set up a specific pipeline for detecting and characterizing variable sources in the observed fields. Here, we report on the first 15 deg 2 in and around the LMC as observed by DECam, testing the capabilities of our pipeline. Since many of the observed fields cover a rather crowded region of the sky, we adopted the ISIS subtraction package which, even in these conditions, can detect variables at a very low signal to noise ratio. All the potentially identified variable sources were then analysed and each light curve tested for periodicity by using the Lomb–Scargle and Schwarzenberg-Czerny algorithms. Furthermore, we classified the identified sources by using the UPSILoN neural network. This analysis allowed us to find 70 981 variable stars, 1266 of which were previously unknown. We estimated the period of the variables and compared it with the available values in the catalogues. Moreover, for the 1266 newly detected objects, an attempted classification based on light curve analysis is presented. • The Dark Energy Camera (DECam) is an instrument mounted at the Blanco Telescope. • We analysed seven DECam fields toward the LMC, covering 15 2 degrees. • We identified 70 981 variables stars, 1266 of which previously unknown. • We estimated the period and compared it with the available values in the catalogues. • For the 1266 newly detected objects, an attempted classification is presented. [ABSTRACT FROM AUTHOR]

Published
2023
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263. New variable sources revealed by DECam toward the LMC: the first 15 deg2

Author

A. Franco, A.A. Nucita, F. De Paolis, F. Strafella, S. Sacquegna, Franco, A., Nucita, A. A., De Paolis, F., Strafella, F., and Sacquegna, S.

Subjects
Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, Magellanic clouds, Methods: data analysis, Stars: variables: general, Techniques: image processing [(Galaxies)], Astronomy and Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation, Astrophysics - Astrophysics of Galaxies, Instrumentation and Methods for Astrophysics (astro-ph.IM), Solar and Stellar Astrophysics (astro-ph.SR)
Abstract

The Dark Energy Camera (DECam) is a sensitive, wide field instrument mounted at the prime focus of the 4 m V. Blanco Telescope in Chile. Beside its main objectives, i.e. understanding the growth and evolution of structures in the Universe, the camera offers the opportunity to observe a 3 deg2 field of view in one single pointing and, with an adequate cadence, to identify the variable sources contained. In this paper, we present the result of a DECam observational campaign toward the LMC and give a catalogue of the observed variable sources. We considered all the available DECam observations of the LMC, acquired during 32 nights over a period of two years (from February 2018 to January 2020), and set up a specific pipeline for detecting and characterizing variable sources in the observed fields. Here, we report on the first 15 deg2 in and around the LMC as observed by DECam, testing the capabilities of our pipeline. Since many of the observed fields cover a rather crowded region of the sky, we adopted the ISIS subtraction package which, even in these conditions, can detect variables at a very low signal to noise ratio. All the potentially identified variable sources were then analyzed and each light curve tested for periodicity by using the Lomb-Scargle and Schwarzenberg-Czerny algorithms. Furthermore, we classified the identified sources by using the UPSILoN neural network. This analysis allowed us to find 70 981 variable stars, 1266 of which were previously unknown. We estimated the period of the variables and compared it with the available values in the catalogues. Moreover, for the 1266 newly detected objects, an attempted classification based on light curve analysis is presented., Comment: 11 pages, 7 figures

Published
2023
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264. Timing analysis of a sample of five cataclysmic variable candidates observed by the XMM–Newton satellite

Author

A A Nucita, S M Lezzi, F De Paolis, F Strafella, D Licchelli, A Franco, M Maiorano, Nucita, A A, Lezzi, S M, De Paolis, F, Strafella, F, Licchelli, D, Franco, A, and Maiorano, M

Subjects
binaries [novae, cataclysmic variables, white dwarfs, X-rays], Space and Planetary Science, Astronomy and Astrophysics
Abstract

Intermediate polars are a class of cataclysmic variables in which a white dwarf accretes material from a companion star. The intermediate polar nature confirmation usually derives from the detection of two periods in both X-ray and optical photometry. In this respect, the high-energy signal is often characterized by modulations on the white dwarf spin and the orbital period. However, noting that the periodograms may be characterized by strong features also at the synodic period and/or other sidebands, the timing analysis of the X-ray signal may offer the unique possibility to firmly discover an intermediate polar candidate. Here, we concentrate on a sample of five cataclysmic variable binary candidates: i.e. SAXJ1748.2-2808, 1RXS J211336.1 + 542226, CXOGC J174622.7-285218, CXOGC J174517.4-290650, and V381 Vel, listed in the IPHome catalogue. Our main aim is to confirm if they belong to the intermediate polar class or not. The results of our analysis show that we can safely assess the intermediate polar nature of all the considered sources, apart for the case of V381 Vel which instead behaves like a cataclysmic variable of the polar subclass. Moreover, the source SAXJ1748.2-2808, previously classified as an HMXB, appears to be, most likely, an intermediate polar variable.

Published
2022

265. Automatic Detection of Accretion Bursts in Young Stellar Objects: a New Algorithm for Long--Term Sky Surveys

Author

F. Strafella, G. Altavilla, T. Giannini, A. Giunta, D. Lorenzetti, A. Nucita, A. Franco, Strafella, F., Altavilla, G., Giannini, T., Giunta, A., Lorenzetti, D., Nucita, A., and Franco, A.

Subjects
Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation, Instrumentation and Methods for Astrophysics (astro-ph.IM), Solar and Stellar Astrophysics (astro-ph.SR)
Abstract

Young stellar objects in their pre-main sequence phase are characterized by irregular changes in brightness, generally attributed to an increase of the mass accretion rate due to various kind of instabilities occurring in the circumstellar disk. In the era of large surveys aimed to monitor the sky, we present a pipeline to detect irregular bursts, in particular EXors-like ( EX Lupi type eruptive variables), in the light curves. The procedure follows a heuristic approach and is tested against the light curves already collected for a few objects presently recognized as bona fide or candidate EXors., Comment: 19 pages, 5 figures. In press in New Astronomy

Published
2022
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266. VZ Sex: X-Ray Confirmation of Its Intermediate Polar Nature

Author

F. De Paolis, Francesco Strafella, G. Ingrosso, M. Maiorano, A. A. Nucita, D. Licchelli, Nucita, A. A., De Paolis, F., Licchelli, D., Strafella, F., Ingrosso, G., and Maiorano, M.

Subjects
010504 meteorology & atmospheric sciences, Astrophysics::High Energy Astrophysical Phenomena, Population, X-ray binary, Cataclysmic variable star, FOS: Physical sciences, X-rays. White dwarfs. cataclysmic variables- Period analysis, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Luminosity, Intermediate polar, 0103 physical sciences, Binary star, Astrophysics::Solar and Stellar Astrophysics, education, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), education.field_of_study, Order (ring theory), White dwarf, Astronomy and Astrophysics, Space and Planetary Science, Astrophysics - High Energy Astrophysical Phenomena
Abstract

Intermediate polars are members of the cataclysmic variable binary stars. They are characterized by a moderately magnetized white dwarf accreting matter from a cool main-sequence companion star. In many cases, this accretion gives rise to a detectable $X$-ray emission. VZ Sex is an interesting $X$-ray source whose nature needs a robust confirmation. Here, we used archive $XMM$-Newton observation to assign the source to the intermediate polar class. We applied the Lomb-Scargle periodogram method to detect any relevant periodic feature in the $0.1$--$10$ keV light curve and performed a spectral fitting of the $X$-ray spectrum in order to get information on the on-going accretion mechanism. By inspecting the periodogram, we detected a clear periodic feature at $\simeq 20.3$ minutes that we interpret as the spin period of the white dwarf. We additionally found the typical side bands expected as the consequence of the beat between the spin and the orbital period of $\simeq 3.581$ hours. The source is characterized by a unabsorbed flux of $\simeq 2.98\times 10^{-12}$ erg cm$^{-2}$ s$^{-1}$ corresponding to an intrinsic luminosity {of $\simeq 7 \times 10^{31}$ erg s$^{-1}$ } {for a distance of $\simeq 433$ pc}. The existence of such features allow us to classify VZ Sex as a clear member of the intermediate polar class. Furthermore, with the estimated WD spin, the ratio $P_{spin}/P_{orb}$ is $\simeq 0.09$, i.e. consistent with that expected for a typical IP system above the period gap. In addition, the estimated intrinsic luminosity opens the possibility that a bridge linking the normally bright IPs to the faint population of sources does exist., Comment: Accepted for publication on The Astrophysical Journal. 10 pages, 5 figures

Published
2021

267. HP Cet and Swift J0820.6–2805: two candidate intermediate polars observed by XMM–Newton

Author

D. Licchelli, Francesco Strafella, A. A. Nucita, F. De Paolis, Nucita, A A, De paolis, F, Strafella, F, and Licchelli, D

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Photon, 010308 nuclear & particles physics, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, White dwarf, Astronomy and Astrophysics, Astrophysics, Orbital period, Light curve, 01 natural sciences, Luminosity, CV, White dwarfs, Magnetic Field driven accretion, intermediate polars, High Energy emission, Intermediate polar, Space and Planetary Science, 0103 physical sciences, ROSAT, Astrophysics::Solar and Stellar Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, 010303 astronomy & astrophysics, Spin-½
Abstract

We report on the XMM-Newton observation of HP Cet and Swift J0820.6-2805, two X-ray photon sources that are candidates to be members of the intermediate polar class of cataclysmic variables. If the historical optical light curve of HP Cet shows a periodic feature at $\simeq 96$ minutes, a clear identification of such a signature in the high energy band (apart for a variability on a time scale of $\simeq 8$ minutes as detected by the ROSAT satellite) is lacking. By using XMM-Newton archive data, we clearly identify a feature (at $\simeq 88$ minutes) which is marginally consistent with one of the binary system orbital periods reported in the literature. We also found a signature of a periodic features on the time scale of $\simeq 5.6$ minutes. In the case of Swift J0820.6-2805, the intermediate polar nature was previously unclear and the orbital and the white dwarf spin periods were unknown. Here, the 0.3-10 keV data undoubtedly reveal an orbital period and a white dwarf spin of $\simeq 87.5$ minutes and $\simeq 27.9$ minutes, respectively. The spectral analysis showed that both HP Cet and Swift J0820.6-280 are members of the under-luminous IP subclass since their luminosity in the $0.3-10$ keV band is estimated to be $\simeq 5\times 10^{30}$ erg s$^{-1}$ and $\simeq 3.8\times 10^{29}$ erg s$^{-1}$, respectively., Accepted for publication on MNRAS, main journal, 2020. 9 Pages. 9 Figures

Published
2020

268. A quasar microlensing event towards J1249+3449?

Author

F. De Paolis, G. Ingrosso, Francesco Strafella, A. A. Nucita, D. Licchelli, De Paolis, F., Nucita, A. A., Strafella, F., Licchelli, D., and Ingrosso, G.

Subjects
Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Active galactic nucleus, Event (relativity), Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astronomy and Astrophysics, Quasar, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Star (graph theory), Gravitational microlensing, Astrophysics - Astrophysics of Galaxies, law.invention, Binary black hole, Space and Planetary Science, law, Astrophysics of Galaxies (astro-ph.GA), Astrophysics - High Energy Astrophysical Phenomena, Microlensing. Dark Matter. Planetary events. Quasars, Astrophysics::Galaxy Astrophysics, Flare
Abstract

We show that the optical flare event discovered by Graham et al. (2020) towards the active galactic nucleus J1249+3449 is fully consistent with being a quasar microlensing event due to a $\simeq 0.1 M_{\odot}$ star, although other explanations, such as that, mainly supported by Graham et al. (2020), of being the electromagnetic counterpart associated to a binary black hole merger, cannot be completely excluded at present., Accepted for publication on the Monthly Notices of the Royal Astronomical Society Letters - (MNRAS Letter) -, 2020, 5 pages, 2 figures

Published
2020

269. Discovery of a bright microlensing event with planetary features towards the Taurus region: a super-Earth planet

Author

F. De Paolis, G. Ingrosso, Francesco Strafella, S.Y. Shugarov, D. Licchelli, Natalia Katysheva, A. A. Nucita, Nucita, A A, Licchelli, D, De Paolis, F, Ingrosso, G, Strafella, F, Katysheva, N, and Shugarov, S

Subjects
Earth and Planetary Astrophysics (astro-ph.EP), Physics, Super-Earth, 010308 nuclear & particles physics, Monte Carlo method, FOS: Physical sciences, Binary number, Astronomy and Astrophysics, Astrophysics, Planetary system, Gravitational microlensing, 01 natural sciences, Microlensing, Exo Planets, Space and Planetary Science, Planet, 0103 physical sciences, Astrophysics::Earth and Planetary Astrophysics, Low Mass, 010303 astronomy & astrophysics, Event (particle physics), Astrophysics - Earth and Planetary Astrophysics
Abstract

The transient event labeled as TCP J05074264+2447555 recently discovered towards the Taurus region was quickly recognized to be an ongoing microlensing event on a source located at distance of only $700-800$ pc from Earth. Here, we show that observations with high sampling rate close to the time of maximum magnification revealed features that imply the presence of a binary lens system with very low mass ratio components. We present a complete description of the binary lens system which hosts an Earth-like planet with most likely mass of $9.2\pm 6.6$ M$_{\oplus}$. Furthermore, the source estimated location and detailed Monte Carlo simulations allowed us to classify the event as due to the closest lens system, being at a distance of $\simeq 380$ pc and mass $\simeq 0.25$ M$_{\odot}$., Accepted for publication on MNRAS, 2018. 6 Pages, 5 Figures. References updated

Published
2018
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270. Dense cores and star formation in the giant molecular cloud Vela C

Author

Frederic Schuller, Fabrizio Massi, Davide Elia, T. Hill, Frédérique Motte, Achim Weiss, Timea Csengeri, E. Schisano, Friedrich Wyrowski, M. De Luca, Luca Olmi, Francesco Strafella, Dario Lorenzetti, Teresa Giannini, Karl M. Menten, Università degli Studi di Roma 'La Sapienza' = Sapienza University [Rome], Max Planck Institute for Radio Astronomy, Istituto di Astrofisica e Planetologia Spaziali - INAF (IAPS), Istituto Nazionale di Astrofisica (INAF), Institute of Hydrology, INAF - Osservatorio Astronomico di Roma (OAR), Antarctic Research a European Network for Astrophysics (ARENA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), Sciences pour l'environnement (SPE), Centre National de la Recherche Scientifique (CNRS)-Université Pascal Paoli (UPP), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Max-Planck-Institut für Radioastronomie (MPIFR), ITA, FRA, DEU, FORMATION STELLAIRE 2020, Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Massi, F., Weiss, A., Elia, D., Csengeri, T., Schisano, E., Giannini, T., Hill, T., Lorenzetti, D., Menten, K., Olmi, L., Schuller, F., Strafella, F., De Luca, M., Motte, F., Wyrowski, F., Università degli Studi di Roma 'La Sapienza' [Rome], Osservatorio di Astrofisica di Roma (OAR), École normale supérieure - Paris (ENS Paris)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université de Cergy Pontoise (UCP), Université Pascal Paoli (UPP)-Centre National de la Recherche Scientifique (CNRS), Centre National d'Études Spatiales [Toulouse] (CNES)-Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), Università degli Studi di Roma 'La Sapienza' = Sapienza University [Rome] (UNIROMA), and École normale supérieure - Paris (ENS-PSL)

Subjects
Initial mass function, FOS: Physical sciences, Context (language use), Astrophysics, Vela, 01 natural sciences, 0103 physical sciences, protostar [Stars], individual objects: Vela Molecular Ridge [ISM], 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), formation [Stars], ComputingMilieux_MISCELLANEOUS, O-type star, Physics, [PHYS]Physics [physics], [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Star formation, Molecular cloud, ISM [Submillimeter], Astronomy and Astrophysics, Galactic plane, Astrophysics - Astrophysics of Galaxies, Galaxy, Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), structure [ISM], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

Context The Vela Molecular Ridge is one of the nearest (700 pc) giant molecular cloud (GMC) complexes hosting intermediate-mass (up to early B, late O stars) star formation, and is located in the outer Galaxy, inside the Galactic plane. Vela C is one of the GMCs making up the Vela Molecular Ridge, and exhibits both sub-regions of robust and sub-regions of more quiescent star formation activity, with both low- and intermediate(high)-mass star formation in progress. Aims We aim to study the individual and global properties of dense dust cores in Vela C, and aim to search for spatial variations in these properties which could be related to different environmental properties and/or evolutionary stages in the various sub-regions of Vela C. Methods We mapped the submillimetre (345 GHz) emission from vela C with LABOCA (beam size 19.2", spatial resolution ~0.07 pc at 700 pc) at the APEX telescope. We used the clump-finding algorithm CuTEx to identify the compact submillimetre sources. We also used SIMBA (250 GHz) observations, and Herschel and WISE ancillary data. The association with WISE red sources allowed the protostellar and starless cores to be separated, whereas the Herschel dataset allowed the dust temperature to be derived for a fraction of cores. The protostellar and starless core mass functions (CMFs) were constructed following two different approaches, achieving a mass completeness limit of 3.7 Msun. Results We retrieved 549 submillimetre cores, 316 of which are starless and mostly gravitationally bound (therefore prestellar in nature). Both the protostellar and the starless CMFs are consistent with the shape of a Salpeter initial mass function in the high-mass part of the distribution. Clustering of cores at scales of 1--6 pc is also found, hinting at fractionation of magnetised, turbulent gas., Comment: 21 pages, 19 figures, to be published in Astronomy & Astrophysics

Published
2019
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271. Subsequent outbursts of the same EXor source possibly present similar features

Author

A. Giunta, S. Antoniucci, Vincenzo Testa, G. Altavilla, Teresa Giannini, Dario Lorenzetti, Francesco Strafella, ITA, Giannini, T., Giunta, A., Lorenzetti, D., Altavilla, G., Antoniucci, S., Strafella, F., and Testa, V.

Subjects
Physics, 010308 nuclear & particles physics, Space and Planetary Science, pre-main sequence [Stars], individual: V1118 Ori [Stars], 0103 physical sciences, Astronomy and Astrophysics, Astrophysics, 010303 astronomy & astrophysics, 01 natural sciences, ExOR, variables: T Tauri, Herbig Ae/Be [Stars]
Abstract

Context. V1118 Ori is a classical EXor source whose light curve has been monitored, although not continuously, over the past 30 years. This source underwent a powerful outburst in 2005, followed by 10 years of quiescence and a less intense outburst in 2015. In 2019, a new intense brightness increase was observed (Δg ∼ 3 mag). Aims. This new accretion episode offers the opportunity to compare the photometric and spectroscopic properties of multiple outbursts of the same source. This allows us to highlight the differences and similarities among various events by removing any possible bias related to the intrinsic properties of the star-disk system. Methods. We discovered the 2019 V1118 Ori outburst by examining the g-band light curve acquired by the Zwicky Transient Facility and followed the declining phase with the Rapid Eye Mount telescope in the griz bands. Two near-infrared spectra were also acquired at different brightness stages with the Large Binocular Telescope. Results. The last event shows the following characteristics: (1) an amplitude similar to that of 2015 and lower than that of 2005; (2) a duration of less than one year as in previous events; (3) a increasing (decreasing) speed of 0.018 (0.031) mag day−1, which is different from previous cases; (4) a gradually blueing of the [g − r] color is observed over time, while the [r − i] color remains roughly unchanged; (5) with few exceptions, the near-infrared lines (mainly H I recombination) are the same as those observed in 2015; and (6) the mass accretion rate peaks at Ṁacc ∼ 10−7 M⊙ yr−1 and decreases in about a month down to a few 10−8 M⊙ yr−1. Conclusions. Our analysis shows that the comparison of data from different outbursts of the same source is a nontrivial exercise, which allows us to obtain important clues that are useful to drive theoretical efforts toward a better understanding of the EXor phenomenon.

Published
2020
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272. Optical, near-IR and $X$-ray observations of SN 2015J and its host galaxy

Author

F. De Paolis, G. Ingrosso, Francesco Strafella, Konstantina Boutsia, A. A. Nucita, Vincenzo Testa, A. M. Read, R. Saxton, D. Licchelli, Fabio Convenga, ITA, USA, GBR, GRC, Nucita, A. A., Paolis, F. De, Saxton, R., Testa, V., Strafella, F., Read, A., Licchelli, D., Ingrosso, G., Convenga, F., and Boutsia, K.

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Physics, 010504 meteorology & atmospheric sciences, Astrophysics::High Energy Astrophysical Phenomena, X-ray, individual (SN 2015J) [supernovae], FOS: Physical sciences, Flux, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astronomy and Astrophysic, 01 natural sciences, Galaxy, Luminosity, law.invention, Telescope, Supernova, Space and Planetary Science, law, 0103 physical sciences, Astrophysics - High Energy Astrophysical Phenomena, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences
Abstract

SN 2015J was discovered on April 27th 2015 and is classified as a type IIn supernova. At first, it appeared to be an orphan SN candidate, i.e. without any clear identification of its host galaxy. Here, we present the analysis of the observations carried out {by the VLT 8-m class telescope with the FORS2 camera in the R band and the Magellan telescope (6.5 m) equipped with the IMACS Short-Camera (V and I filters) and the FourStar camera (Ks filter)}. We show that SN 2015J resides in what appears to be a very compact galaxy establishing a relation between the SN event and its natural host. We also present and discuss archival and new $X$-ray data centred on SN 2015J. At the time of the supernova explosion, Swift/XRT observations were made and a weak X-ray source was detected at the location of SN 2015J. Almost one year later, the same source was unambiguously identified during serendipitous observations by Swift/XRT and $XMM$-Newton, clearly showing an enhancement of the 0.3-10 keV band flux by a factor $\simeq 30$ with respect to the initial state. Swift/XRT observations show that the source is still active in the $X$-rays at a level of $\simeq 0.05$ counts s$^{-1}$. The unabsorbed X-ray luminosity derived from the {\it XMM}-Newton slew and SWIFT observations, $L_{x}\simeq 5\times10^{41}$ erg s$^{-1}$, places SN 2015J among the brightest young supernovae in X-rays., The Astrophysical Journal, Volume 850, Number 2

Published
2017

273. The Hi-GAL compact source catalogue – I. The physical properties of the clumps in the inner Galaxy (−71$_.^circ$0 < ℓ < 67$_.^circ$0)

Author

Takahiro Hayakawa, David Eden, Melvin Hoare, Francesco Strafella, F. Piacentini, Kenneth A. Marsh, Sergio Molinari, S. E. Jaffa, Pedro García-Lario, Alessio Traficante, Peter Schilke, Kengo Tachihara, G. Joncas, J.-P. Bernard, M. R. Pestalozzi, S. Martinavarro-Armengol, Amata Mercurio, Alessandro Costa, Friedrich Wyrowski, Eva Sciacca, Robert Butora, B. Maiolo, Joseph C. Mottram, Mark Thompson, D. Polychroni, H. Yamamoto, G. Li Causi, P. Palmeirim, M. Benedettini, D. Russeil, Hidetoshi Sano, Kazi L.J. Rygl, Eugenio Schisano, Stefano Cavuoti, Annie Zavagno, Sarah Ragan, John Bally, M. Veneziani, Carla Buemi, A. P. Whitworth, K. Torii, Massimo Brescia, Péter Kacsuk, Davide Elia, Marco Molinaro, Nicola Schneider, Ugo Becciani, Rene Plume, Göran Pilbratt, A. M. di Giorgio, F. Faustini, P. Mège, Luca Calzoletti, Grazia Umana, Stefano Pezzuto, H. Arab, E. Fiorellino, Derek Ward-Thompson, S. J. Liu, Marilena Bandieramonte, M. T. Beltrán, Paolo Leto, Y. Maruccia, Roberta Paladini, Toby J. T. Moore, Giuseppe Riccio, Fabio Vitello, Luca Olmi, N. Marchili, Frédérique Motte, Corrado Trigilio, Ákos Hajnal, Yasuo Fukui, Nicolas Peretto, Alberto Noriega-Crespo, A. Baldeschi, Riccardo Cesaroni, Leonardo Testi, Lorenzo Piazzo, Manuel Merello, L. Cambrésy, Filomena Bufano, Peter G. Martin, Nicolas Billot, Meng-Lin Huang, Paolo Natoli, Elia, D., Molinari, S., Schisano, E., Pestalozzi, M., Pezzuto, Marilena, Merello, M., Noriega-Crespo, A., Moore, T. J. T., Russeil, D., Mottram, J. C., Paladini, R., Strafella, F., Benedettini, M., Bernard, J. P., Di Giorgio, A., Eden, D. J., Fukui, Y., Plume, R., Bally, J., Martin, P. G., Ragan, S. E., Jaffa, S. E., Motte, F., Olmi, L., Schneider, N., Testi, L., Wyrowski, F., Zavagno, A., Calzoletti, L., Faustini, F., Natoli, P., Palmeirim, P., Piacentini, F., Piazzo, L., Pilbratt, G. L., Polychroni, D., Baldeschi, A., Beltrán, M. T., Billot, N., Cambrésy, L., Cesaroni, R., García-Lario, P., Hoare, M. G., Huang, M., Joncas, G., Liu, S. J., Maiolo, B. M. T., Marsh, K. A., Maruccia, Y., Mège, P., Peretto, N., Rygl, K. L. J., Schilke, P., Thompson, M. A., Traficante, A., Umana, G., Veneziani, M., Ward-Thompson, D., Whitworth, A. P., Arab, H., Bandieramonte, M., Becciani, U., Brescia, M., Buemi, C., Bufano, F., Butora, R., Cavuoti, S., Costa, A., Fiorellino, E., Hajnal, A., Hayakawa, T., Kacsuk, P., Leto, P., Li Causi, G., Marchili, N., Martinavarro-Armengol, S., Mercurio, A., Molinaro, M., Riccio, G., Sano, H., Sciacca, E., Tachihara, K., Torii, K., Trigilio, C., Vitello, F., Yamamoto, H., Elia, Davide, Pezzuto, S., Noriega Crespo, A., Strafella, Francesco, García Lario, P., Maiolo, BERLINDA MARIA TERESA, Maruccia, Ylenia, Ward Thompson, D., and Martinavarro Armengol, S.

Subjects
Astrophysics and Astronomy, Infrared, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, cataloghi astronomici, mezzo interstellare, osservazioni infrarosse, osservazioni submillimetriche, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, QC, QB, Physics, Spiral galaxy, 010308 nuclear & particles physics, Star formation, Spectral density, Astronomy, Astronomy and Astrophysics, Galactic plane, Galaxy, Stars, Space and Planetary Science, Astrophysics::Earth and Planetary Astrophysics, catalogues, ISM clouds, dust, extinction, local interstellar matter, infrared ISM, submillimetre ISM, Longitude
Abstract

Hi-GAL (Herschel InfraRed Galactic Plane Survey) is a large-scale survey of the Galactic plane, performed with Herschel in five infrared continuum bands between 70 and 500 μm. We present a band-merged catalogue of spatially matched sources and their properties derived from fits to the spectral energy distributions (SEDs) and heliocentric distances, based on the photometric catalogues presented in Molinari et al., covering the portion of Galactic plane −71 ∘. 0 < ℓ < 67 ∘. 0. The band-merged catalogue contains 100 922 sources with a regular SED, 24 584 of which show a 70-μm counterpart and are thus considered protostellar, while the remainder are considered starless. Thanks to this huge number of sources, we are able to carry out a preliminary analysis of early stages of star formation, identifying the conditions that characterize different evolutionary phases on a statistically significant basis. We calculate surface densities to investigate the gravitational stability of clumps and their potential to form massive stars. We also explore evolutionary status metrics such as the dust temperature, luminosity and bolometric temperature, finding that these are higher in protostellar sources compared to pre-stellar ones. The surface density of sources follows an increasing trend as they evolve from pre-stellar to protostellar, but then it is found to decrease again in the majority of the most evolved clumps. Finally, we study the physical parameters of sources with respect to Galactic longitude and the association with spiral arms, finding only minor or no differences between the average evolutionary status of sources in the fourth and first Galactic quadrants, or between ‘on-arm’ and ‘interarm’ positions. Hi-GAL is a large-scale survey of the Galactic plane, performed with Herschel in five infrared continuum bands between 70 and 500 $\mu$m. We present a band-merged catalogue of spatially matched sources and their properties derived from fits to the spectral energy distributions (SEDs) and heliocentric distances, based on the photometric catalogs presented in Molinari et al. (2016a), covering the portion of Galactic plane $-71.0^{\circ}< \ell < 67.0^{\circ}$. The band-merged catalogue contains 100922 sources with a regular SED, 24584 of which show a 70 $\mu$m counterpart and are thus considered proto-stellar, while the remainder are considered starless. Thanks to this huge number of sources, we are able to carry out a preliminary analysis of early stages of star formation, identifying the conditions that characterise different evolutionary phases on a statistically significant basis. We calculate surface densities to investigate the gravitational stability of clumps and their potential to form massive stars. We also explore evolutionary status metrics such as the dust temperature, luminosity and bolometric temperature, finding that these are higher in proto-stellar sources compared to pre-stellar ones. The surface density of sources follows an increasing trend as they evolve from pre-stellar to proto-stellar, but then it is found to decrease again in the majority of the most evolved clumps. Finally, we study the physical parameters of sources with respect to Galactic longitude and the association with spiral arms, finding only minor or no differences between the average evolutionary status of sources in the fourth and first Galactic quadrants, or between "on-arm" and "inter-arm" positions.

Published
2017

274. Impact of atmospheric effects on the energy reconstruction of air showers observed by the surface detectors of the Pierre Auger Observatory

Author

Marco Torri, Denis Stanca, P. Abreu, D. Ravignani, M. Platino, M. Urban, A. C. Rovero, Alexandru Balaceanu, Vincenzo Rizi, D. Martello, M. Ziolkowski, Silvia Mollerach, O. Martínez Bravo, I. Jandt, Ralf Ulrich, R. Piegaia, G. Cataldi, V. Scherini, C. J. Todero Peixoto, N. Krohm, Alexandra Saftoiu, B. Sarkar, Christian Glaser, J. Espadanal, H. Wilczyński, B. García, Tobias Winchen, P. Lebrun, R. López, Karen S. Caballero-Mora, Alberto Daniel Supanitsky, Jose Chinellato, J. Kleinfeller, J. D. Swain, Martin Erdmann, E. Santos, Daniel Kuempel, Carlos Escobar, G. Torralba Elipe, Markus Roth, A. Letessier-Selvon, Gioacchino Alex Anastasi, Jesús Peña-Rodríguez, R. Krause, A. Śmiałkowski, Roger W Clay, D. Melo, P. Ruehl, A. Insolia, M. Kleifges, D. Zavrtanik, Stefano D'Amico, Lorenzo Cazon, A. Fuster, A. C. Fauth, Carla Bonifazi, Jose A. Bellido, S. Sonntag, J. J. Beatty, J. Pȩkala, L. Valore, I.D. Vergara Quispe, Mariangela Settimo, L. Nellen, N. Fazzini, Jeffrey A. Johnsen, B. Vargas Cárdenas, T. Suomijärvi, J. Pallotta, E. J. Quel, A. van Vliet, Max Malacari, Lili Yang, Thomas Bretz, I. Valiño, C. Morello, J. Neuser, Corbin Covault, M. Zavrtanik, Piotr Homola, Julien Aublin, M. Josebachuili, David Walz, Ivone F. M. Albuquerque, M. Suarez Durán, Matías Rolf Hampel, Gaia Silli, A. Filipčič, R. M. Kieckhafer, David Wittkowski, Hernan Wahlberg, G. Salina, Igor Katkov, Eric Mayotte, M. Gómez Berisso, M. I. Micheletti, R. R. Prado, J. Rautenberg, Danielle LaHurd, Olivier Deligny, A. Parra, O. Wainberg, P. Ristori, Peter L. Biermann, M. Trini, S. Quinn, G. Kukec Mezek, Lino Miramonti, F. Sarazin, R. C. Shellard, A. Cancio, E. Varela, I. Allekotte, Dusan Mandat, Johannes Schulz, K.-H. Becker, M. Pimenta, J.D. Sanabria Gomez, Paolo Privitera, L. Villaseñor, S. Petrera, J. F. Valdés Galicia, Brian Fick, Marc Weber, Michael Unger, Francesco Strafella, I. De Mitri, Mario Buscemi, A. Segreto, Günter Sigl, Benedikt Zimmermann, Rúben Conceição, P. Heimann, Florian Lukas Briechle, J. Hulsman, A. Menshikov, Z. Zong, Petr Schovanek, A. Aab, Julian Kemp, G. Matthiae, M. A. Leigui de Oliveira, Roberto Mussa, D. Pakk Selmi-Dei, E. Kemp, R. Sato, Marco Giammarchi, L. Caramete, Serguei Vorobiov, J. R. Vázquez, D. Torres Machado, Alex Kääpä, Antonio Bueno, P. Sanchez-Lucas, D. Harari, D. Garcia-Pinto, Colin Baus, O. A. Taborda, Lourenco Lopes, Paul Sommers, A. Blanco, François Montanet, R. Squartini, G. S. Varner, T. Paul, Alfred Müller, L. Ochilo, P. Gouffon, H. Schieler, M. J. Cooper, H. Martinez, Carla Bleve, Karl-Heinz Kampert, F. Sánchez, Belén Andrada, Carlos Medina, Federico Suarez, Ricardo Vázquez, Ivo Nicolas Naranjo, Antonella Castellina, Paula Gina Isar, F. Salesa Greus, Gualberto Avila, M. Risse, Jonathan Blazek, G. C. Hill, Alina Mihaela Badescu, Radomir Smida, G. Medina-Tanco, G. van Aar, A. Di Matteo, Maria Rita Coluccia, Bruno Daniel, I. C. Mariç, Ralph Engel, M. Mallamaci, B. Wundheiler, Foteini Oikonomou, J. J. Masías Meza, G. De Mauro, C. Aramo, Gregory R Snow, P. H. Kasper, Jonathan Biteau, M. Prouza, Nicolás González, A.M. van den Berg, Darko Veberič, J. Ridky, Angela V. Olinto, Jörg R. Hörandel, B. Mitrica, S. Müller, Heino Falcke, E.M. Holt, Nicusor Arsene, A. Tapia, G. Parente, Fabrizia Canfora, R. Legumina, Esteban Roulet, H. Gemmeke, J. Vicha, I. Lhenry-Yvon, Corinne Berat, M. Giller, G. Marsella, A. Saleh, Maria-Teresa Dova, Q. Hasankiadeh, M. Perlin, D. Rogozin, J. de Oliveira, P. H. Nguyen, D. Nosek, C. Hojvat, Jan Ebr, R.J. Barreira Luz, E. M. Santos, Alejandro Almela, H.O. Klages, Bruce R. Dawson, P.O. Mazur, S. Messina, Johannes Schumacher, Andrej Dundovic, Lorenzo Caccianiga, V. M. Theodoro, Octavian Fratu, Valerio Verzi, B. Tome, G. Müller, Dariusz Glas, R.C. dos Anjos, V. de Souza, M. Palatka, A. Bridgeman, Luis A. Nunez, J. Stasielak, S. Coutu, S. J. Saffi, C. Porowski, Denise Boncioli, Marcus Niechciol, S. Querchfeld, M. J. Roncoroni, L. Niemietz, M. L. Díaz Castro, G. Farrar, Francesca Zuccarello, Tim Niggemann, I. Al Samarai, A. Criss, L. A. S. Pereira, Q. Luce, A. Taboada, G. P. Guedes, P.F. Gómez Vitale, Toshihiro Fujii, J. Debatin, A. Shadkam, Markus Lauscher, A. F. Grillo, Juan Carlos D'Olivo, T. Pierog, F. Pedreira, J. Phuntsok, Piera Luisa Ghia, Raul Sarmento, H. J. Mathes, A. Weindl, P. Stassi, David Schmidt, J. Rodriguez Rojo, A. G. Chavez, F.G. Schröder, Enrique Zas, Octavian Sima, C. Di Giulio, Fernando Contreras, M. Schauer, B. Revenu, D. Heck, Peter Gorham, Charles Timmermans, L. Collica, T. Huege, Jeffrey Brack, Olaf Scholten, Humberto Ibarguen Salazar, C. A. Sarmiento, F. Gate, Peter Hansen, Miguel Mostafa, L. Perrone, Jiri Chudoba, L. Tomankova, Alessio Gorgi, F. Guarino, John Matthews, A. López Casado, Samo Stanič, Peter Buchholz, R. Gaior, I.M. Brancus, Thomas Hebbeker, Sergio Dasso, Tristan Sudholz, Thomas Harrison, H. Glass, Martín Miguel Freire, Carola Dobrigkeit, M. Plum, V. Pirronello, Marco Aglietta, P. Pieroni, M. E. Bertaina, F. Arqueros, Alan Watson, Kai Daumiller, Martina Bohacova, Mihai Niculescu-Oglinzanu, J. Alvarez Castillo, K. Link, J. Sorokin, A. Lucero, Miroslav Hrabovský, O. Kambeitz, M. Schimp, A. Haungs, A. Kuotb Awad, J. L. Harton, S. G. Blaess, P. Mantsch, Z. Szadkowski, Ana Martina Botti, F. Diogo, V. Novotny, Rossella Caruso, S. Mathys, M. Erfani, R. M. de Almeida, Lukas Middendorf, Christine Peters, Miroslav Pech, A. Yushkov, Rodrigo Pelayo, Stijn Buitink, Pavel Horvath, D. Yelos, G. Rodriguez Fernandez, Hernán Asorey, R. Ramos-Pollan, Sofia Andringa, Marcio Aparecido Muller, H. Nožka, Daniela Mockler, W. Rodrigues de Carvalho, J. W. Cronin, P. van Bodegom, G. Golup, Nataliia Borodai, N. Kunka, S. J. De Jong, Pierre Billoir, Ugo Giaccari, J. R. T. de Mello Neto, J. A.J. Matthews, Xavier Bertou, A. Zepeda, Pedro Assis, A. Etchegoyen, Luis A. Anchordoqui, Jaime Alvarez-Muñiz, Philipp Papenbreer, Alexandru Gherghel-Lascu, Petr Travnicek, Alan Coleman, Trent D. Grubb, Juan Manuel Figueira, Roberta Colalillo, A. G. Mariazzi, I. A. Minaya, B. Keilhauer, André Schulz, S. J. Sciutto, D. Nitz, A. E. Herve, L. R. Wiencke, S. Jansen, Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Laboratoire SUBATECH Nantes (SUBATECH), Mines Nantes (Mines Nantes)-Université de Nantes (UN)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Pierre AUGER, Aab, A., Abreu, P., Aglietta, M., Samarai, I. Al, Albuquerque, I. F. M., Allekotte, I., Almela, A., Castillo, J. Alvarez, Alvarez Muñiz, J., Anastasi, G. A., Anchordoqui, L., Andrada, B., Andringa, S., Aramo, C., Arqueros, F., Arsene, N., Asorey, H., Assis, P., Aublin, J., Avila, G., Badescu, A. M., Balaceanu, A., Luz, R. J. Barreira, Baus, C., Beatty, J. J., Becker, K. H., Bellido, J. A., Berat, C., Bertaina, M. E., Bertou, X., Biermann, P. L., Billoir, P., Biteau, J., Blaess, S. G., Blanco, A., Blazek, J., Bleve, C., Boháčová, M., Boncioli, D., Bonifazi, C., Borodai, N., Botti, A. M., Brack, J., Brancus, I., Bretz, T., Bridgeman, A., Briechle, F. L., Buchholz, P., Bueno, A., Buitink, S., Buscemi, M., Caballero Mora, K. S., Caccianiga, L., Cancio, A., Canfora, F., Caramete, L., Caruso, R., Castellina, A., Cataldi, G., Cazon, L., Chavez, A. G., Chinellato, J. A., Chudoba, J., Clay, R. W., Colalillo, Roberta, Coleman, A., Collica, L., Coluccia, M. R., Conceição, R., Contreras, F., Cooper, M. J., Coutu, S., Covault, C. E., Criss, A., Cronin, J., D'Amico, S., Daniel, B., Dasso, S., Daumiller, K., Dawson, B. R., de Almeida, R. M., de Jong, S. J., Mauro, G. De, Neto, J. R. T. de Mello, Mitri, I. De, de Oliveira, J., de Souza, V., Debatin, J., Deligny, O., Giulio, C. Di, Matteo, A. Di, Castro, M. L. Díaz, Diogo, F., Dobrigkeit, C., D'Olivo, J. C., Anjos, R. C. do, Dova, M. T., Dundovic, A., Ebr, J., Engel, R., Erdmann, M., Erfani, M., Escobar, C. O., Espadanal, J., Etchegoyen, A., Falcke, H., Farrar, G., Fauth, A. C., Fazzini, N., Fick, B., Figueira, J. M., Filipčič, A., Fratu, O., Freire, M. M., Fujii, T., Fuster, A., Gaior, R., García, B., Garcia Pinto, D., Gaté, F., Gemmeke, H., Gherghel Lascu, A., Ghia, P. L., Giaccari, U., Giammarchi, M., Giller, M., Głas, D., Glaser, C., Glass, H., Golup, G., Berisso, M. Gómez, Vitale, P. F. Gómez, González, N., Gorgi, A., Gorham, P., Gouffon, P., Grillo, A. F., Grubb, T. D., Guarino, Fausto, Guedes, G. P., Hampel, M. R., Hansen, P., Harari, D., Harrison, T. A., Harton, J. L., Hasankiadeh, Q., Haungs, A., Hebbeker, T., Heck, D., Heimann, P., Herve, A. E., Hill, G. C., Hojvat, C., Holt, E., Homola, P., Hörandel, J. R., Horvath, P., Hrabovský, M., Huege, T., Hulsman, J., Insolia, A., Isar, P. G., Jandt, I., Jansen, S., Johnsen, J. A., Josebachuili, M., Kääpä, A., Kambeitz, O., Kampert, K. H., Kasper, P., Katkov, I., Keilhauer, B., Kemp, E., Kemp, J., Kieckhafer, R. M., Klages, H. O., Kleifges, M., Kleinfeller, J., Krause, R., Krohm, N., Kuempel, D., Mezek, G. Kukec, Kunka, N., Awad, A. Kuotb, Lahurd, D., Lauscher, M., Lebrun, P., Legumina, R., de Oliveira, M. A. Leigui, Letessier Selvon, A., Lhenry Yvon, I., Link, K., Lopes, L., López, R., Casado, A. López, Luce, Q., Lucero, A., Malacari, M., Mallamaci, M., Mandat, D., Mantsch, P., Mariazzi, A. G., Mariç, I. C., Marsella, G., Martello, D., Martinez, H., Bravo, O. Martínez, Meza, J. J. Masía, Mathes, H. J., Mathys, S., Matthews, J., Matthews, J. A. J., Matthiae, G., Mayotte, E., Mazur, P. O., Medina, C., Medina Tanco, G., Melo, D., Menshikov, A., Messina, S., Micheletti, M. I., Middendorf, L., Minaya, I. A., Miramonti, L., Mitrica, B., Mockler, D., Mollerach, S., Montanet, F., Morello, C., Mostafá, M., Müller, A. L., Müller, G., Muller, M. A., Müller, S., Mussa, R., Naranjo, I., Nellen, L., Neuser, J., Nguyen, P. H., Niculescu Oglinzanu, M., Niechciol, M., Niemietz, L., Niggemann, T., Nitz, D., Nosek, D., Novotny, V., Nožka, H., Núñez, L. A., Ochilo, L., Oikonomou, F., Olinto, A., Selmi Dei, D. Pakk, Palatka, M., Pallotta, J., Papenbreer, P., Parente, G., Parra, A., Paul, T., Pech, M., Pedreira, F., Pȩkala, J., Pelayo, R., Peña Rodriguez, J., Pereira, L. A. S., Perlín, M., Perrone, L., Peters, C., Petrera, S., Phuntsok, J., Piegaia, R., Pierog, T., Pieroni, P., Pimenta, M., Pirronello, V., Platino, M., Plum, M., Porowski, C., Prado, R. R., Privitera, P., Prouza, M., Quel, E. J., Querchfeld, S., Quinn, S., Ramos Pollan, R., Rautenberg, J., Ravignani, D., Revenu, B., Ridky, J., Risse, M., Ristori, P., Rizi, V., de Carvalho, W. Rodrigue, Fernandez, G. Rodriguez, Rojo, J. Rodriguez, Rogozin, D., Roncoroni, M. J., Roth, M., Roulet, E., Rovero, A. C., Ruehl, P., Saffi, S. J., Saftoiu, A., Salazar, H., Saleh, A., Greus, F. Salesa, Salina, G., Gomez, J. D. Sanabria, Sánchez, F., Sanchez Lucas, P., Santos, E. M., Santos, E., Sarazin, F., Sarkar, B., Sarmento, R., Sarmiento, C. A., Sato, R., Schauer, M., Scherini, V., Schieler, H., Schimp, M., Schmidt, D., Scholten, O., Schovánek, P., Schröder, F. G., Schulz, A., Schulz, J., Schumacher, J., Sciutto, S. J., Segreto, A., Settimo, M., Shadkam, A., Shellard, R. C., Sigl, G., Silli, G., Sima, O., Śmiałkowski, A., Šmída, R., Snow, G. R., Sommers, P., Sonntag, S., Sorokin, J., Squartini, R., Stanca, D., Stanič, S., Stasielak, J., Stassi, P., Strafella, F., Suarez, F., Durán, M. Suarez, Sudholz, T., Suomijärvi, T., Supanitsky, A. D., Swain, J., Szadkowski, Z., Taboada, A., Taborda, O. A., Tapia, A., Theodoro, V. M., Timmermans, C., Peixoto, C. J. Todero, Tomankova, L., Tomé, B., Elipe, G. Torralba, Machado, D. Torre, Torri, M., Travnicek, P., Trini, M., Ulrich, R., Unger, M., Urban, M., Galicia, J. F. Valdé, Valiño, I., Valore, Laura, Aar, G. van, Bodegom, P. van, Berg, A. M. van den, Vliet, A. van, Varela, E., Cárdenas, B. Varga, Varner, G., Vázquez, J. R., Vázquez, R. A., Veberič, D., Quispe, I. D. Vergara, Verzi, V., Vicha, J., Villaseñor, L., Vorobiov, S., Wahlberg, H., Wainberg, O., Walz, D., Watson, A. A., Weber, M., Weindl, A., Wiencke, L., Wilczyński, H., Winchen, T., Wittkowski, D., Wundheiler, B., Yang, L., Yelos, D., Yushkov, A., Zas, E., Zavrtanik, D., Zavrtanik, M., Zepeda, A., Zimmermann, B., Ziolkowski, M., Zong, Z., Zuccarello, F., Bleve, Carla, Colalillo, R., Coluccia, MARIA RITA, D'Amico, Stefano, DE MITRI, Ivan, Guarino, F., Marsella, Giovanni, Martello, Daniele, Perrone, Lorenzo, Strafella, Francesco, Valore, L., Physics, Elementary Particle Physics, Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Pierre et Marie Curie - Paris 6 (UPMC), and Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Nantes (UN)-Mines Nantes (Mines Nantes)

Subjects
[PHYS.ASTR.HE]Physics [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], Astronomy, Astrophysics::High Energy Astrophysical Phenomena, Cherenkov detectors, Data analysis, Large detector systems for particle and astroparticle physics, Systematic effects, FOS: Physical sciences, Cosmic ray, Cherenkov detectors Data analysis, Instrumentation, Mathematical Physics, 01 natural sciences, Auger, Nuclear physics, Observatory, 0103 physical sciences, Density of air, High Energy Physics, 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Physics::Atmospheric and Oceanic Physics, Pierre Auger Observatory, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), 010308 nuclear & particles physics, Detector, Astrophysics::Instrumentation and Methods for Astrophysics, Física, 13. Climate action, Experimental High Energy Physics, RECONHECIMENTO DE PADRÕES, ComputingMethodologies_DOCUMENTANDTEXTPROCESSING, Física nuclear, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, Event (particle physics), ultra-high energy cosmic rays, extensive air showers, atmospheric effects, Energy (signal processing)
Abstract

Atmospheric conditions, such as the pressure (P), temperature (T) or air density ( / P=T), affect the development of extended air showers initiated by energetic cosmic rays. We study the impact of the atmospheric variations on the reconstruction of air showers with data from the arrays of surface detectors of the Pierre Auger Observatory, considering separately the one with detector spacings of 1500m and the one with 750m spacing. We observe modulations in the event rates that are due to the influence of the air density and pressure variations on the measured signals, from which the energy estimators are obtained. We show how the energy assignment can be corrected to account for such atmospheric effects., La lista completa de autores puede verse al final del archivo asociado a este registro., Instituto de Física La Plata

Published
2017
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275. Evidence for a mixed mass composition at the 'ankle' in the cosmic-ray spectrum

Author

S. Stanič, Denis Stanca, J. A.J. Matthews, Xavier Bertou, M. L. Díaz Castro, C. Porowski, Jakub Vicha, Francesca Zuccarello, Pedro Assis, R. Sato, Jose Chinellato, I. Jandt, Hermann-Josef Mathes, M. Ziolkowski, Denise Boncioli, Markus Risse, Muller, F. Canfora, J. Blazek, A. Tonachini, Antonio Bueno, M. Josebachuili, J.D. Sanabria Gomez, Eric Mayotte, A. C. Rovero, J. Biteau, P.F. Gómez Vitale, G. A. Anastasi, Kai Daumiller, Alberto Filevich, Peter Hansen, John Matthews, Christian Sarmiento-Cano, Gualberto Avila, W. Rodrigues de Carvalho, Marco Torri, Nicolás González, M. Gómez Berisso, R. C. Shellard, Leigui de Oliveira, Paul M. Mantsch, Diego Ravignani, J. R. Vázquez, P. Sanchez-Lucas, S. Vorobiov, Ingomar Allekotte, F. Sánchez, J. W. Cronin, Lorenzo Cazon, Peter Buchholz, R. Piegaia, I. Al Samarai, Ivo Nicolas Naranjo, Antonio Insolia, A. Aab, L. Caramete, Alina Mihaela Badescu, P. Heimann, Anderson Fauth, M. Zavrtanik, G. Marsella, R. Ramos-Pollant, Valerio Pirronello, G. Torralba Elipe, O. Ravel, P. van Bodegom, Angela V. Olinto, C. Di Giulio, S. Navas, I.M. Brancus, H. Glass, Marco Aglietta, Johannes Schumacher, Joshua A. Gordon, Bruno Daniel, Corinne Berat, R. Krause, Gaia Silli, A. Filipčič, Foteini Oikonomou, G. S. Varner, Alessio Gorgi, Fred Sarazin, H. Gemmeke, Lukas Nellen, M. I. Micheletti, L. A. S. Pereira, Maria Giller, J. J. Masías Meza, C. J. Todero Peixoto, A.E. Herve, Octavian Sima, Nataliia Borodai, D. Mockler, Manuel Platino, E.M. Holt, B. Wundheiler, A. Fuster, Q. Hasankiadeh, A. Saleh, Jeffrey Brack, J. F. Valdés Galicia, Olaf Scholten, Ioana Codrina Maris, I. De Mitri, Dieter Heck, Martin Urban, Hans Klages, H. Nožka, A. Chiavassa, Maria-Teresa Dova, M. R. Hampel, O. A. Taborda, Carlos Hojvat, Miroslav Palatka, A. Menshikov, Diego Harari, B. Gookin, S. Müller, Carola Dobrigkeit, M. Schauer, Humberto Ibarguen Salazar, Ricardo Vázquez, Antoine Letessier-Selvon, Ernesto Kemp, R. Legumina, P. H. Nguyen, Lawrence Wiencke, B. Sarkar, Sarka Wykes, C. Morello, E. M. Santos, G. Kukec Mezek, L. Molina-Bueno, M. Plum, Z. Zong, David Walz, Harald Schieler, O. Kambeitz, Jeffrey A. Johnsen, Sven Querchfeld, L. Perrone, Marco Giammarchi, Bruce R. Dawson, S. Quinn, Christian Glaser, J. Espadanal, Octavian Fratu, M. E. Bertaina, Alan Watson, Mihai Niculescu-Oglinzanu, Jonny Kleinfeller, Sergio Sciutto, L. Ochilo, M. Mallamaci, Alberto Segreto, Nicusor Arsene, D. Rogozin, J. de Oliveira, R.R. Prado, Alejandro Almela, P. Billoir, Tim Huege, Ana Martina Botti, Belén Andrada, J. Alvarez Castillo, G. C. Hill, R.C. dos Anjos, Lukas Middendorf, D. Pakk Selmi-Dei, F. Diogo, G. De Mauro, Henryk Wilczyński, Ralph Engel, J. J. Beatty, Norbert Kunka, D. Nitz, Günter Sigl, Silvia Mollerach, A. Śmiałkowski, Jörg R. Hörandel, Sutherland, Julian Rautenberg, Peter L. Biermann, F. Montanet, L. Niemietz, R. M. de Almeida, L. Tomankova, Christine Peters, Radomir Smida, Alberto Etchegoyen, John L. Harton, Peter Gorham, T. Paul, Paolo Privitera, Federico Suarez, A. Schulz, D. Reinert, A. López Casado, G. Matthiae, Andreas Weindl, D. Garcia-Pinto, Paul Sommers, Petr Schovanek, A. Di Matteo, Charles Timmermans, Luis A. Nunez, A. Blanco, P. Gouffon, N. Krohm, D. Torres Machado, L. Collica, P. Abreu, Brian Fick, Zbigniew Szadkowski, Alberto Daniel Supanitsky, D. Melo, Julien Aublin, A. Shadkam, M. J. Cooper, Miguel Mostafá, Mário Pimenta, Gregory R Snow, Pablo Ristori, Miroslav Pech, P. H. Kasper, Carlos Medina, M. Settimo, R. Ulrich, Rodrigo Pelayo, Stijn Buitink, E. Varela, D. Yelos, Andrej Dundovic, Marcus Niechciol, D. Martello, Luis A. Anchordoqui, Pavel Horvath, Danilo Zavrtanik, Lorenzo Caccianiga, V. M. Theodoro, Paula Gina Isar, F. Salesa Greus, G. Cataldi, Florian Gaté, Michael Unger, S. Jansen, Gero Müller, P. W. Younk, Sofia Andringa, Eun-Joo Ahn, P. Lautridou, C. Scarso, Elton J. G. Santos, Jiri Chudoba, Markus Roth, G. van Aar, Dusan Mandat, Q. Luce, V. de Souza, Alex Kääpä, Maria Rita Coluccia, A. van Vliet, Tanguy Pierog, R. Cester, Gustavo Medina-Tanco, Miroslav Hrabovský, L. del Peral, Jaroslaw Stasielak, Andreas Haungs, Matthias Kleifges, V. Verzi, Philipp Papenbreer, Colin Baus, Glennys R. Farrar, David Schmidt, J. Sorokin, K. H. Becker, H. Martinez, A. G. Mariazzi, A. Kuotb Awad, S. G. Blaess, C. Aramo, Sergio Dasso, Tristan Sudholz, Fausto Guarino, Juan Pallotta, R. López, B. Tome, C. Bleve, Alexandru Balaceanu, Petr Travnicek, Rodríguez-Frías, V. Scherini, Arnulfo Zepeda, Eduardo Quel, David Wittkowski, Laura Valore, Martín Miguel Freire, Thomas Harrison, Benoît Revenu, Germano Guedes, Danielle LaHurd, Olivier Deligny, P. Pieroni, Alan Coleman, T. Hebbeker, Vincenzo Rizi, Trent D. Grubb, G. Rodriguez Fernandez, Benedikt Zimmermann, Rúben Conceição, Toshihiro Fujii, M. Ambrosio, L. Lopes, J. Debatin, O. Martínez Bravo, Dariusz Glas, Juan Manuel Figueira, F. Arqueros, Alexandra Saftoiu, Tim Niggemann, Roberta Colalillo, J. Hulsman, B. Mitrica, Hernán Asorey, Francesco Strafella, Martina Bohacova, Patrick Allison, Heino Falcke, Jaime Alvarez-Muñiz, Alexandru Gherghel-Lascu, I. Lhenry-Yvon, A. Lucero, Juan Carlos D'Olivo, O. Wainberg, A. Valbuena-Delgado, Esteban Roulet, T. Suomijärvi, Karl-Heinz Kampert, Antonella Castellina, Piera Luisa Ghia, V. Novotny, Rossella Caruso, S. Mathys, M. Erfani, John Swain, Thomas Bretz, Ruben Squartini, I. A. Minaya, Corbin Covault, Peter Mazur, J. Pȩkala, Geraldina Golup, Alexander Grillo, S. J. De Jong, Katrin Link, Lino Miramonti, Ugo Giaccari, A. Tepe, J. R. T. de Mello Neto, M. Prouza, J. Rodriguez Rojo, Bianca Keilhauer, A. G. Chavez, F.G. Schröder, Enrique Zas, Fernando Contreras, Jesús Peña-Rodríguez, A. Dorofeev, L. Villaseñor, A. Bridgeman, S. J. Saffi, Markus Lauscher, F. Pedreira, J. Phuntsok, Raul Sarmento, M. Suarez Durán, H. Wahlberg, A. Parra, G. Parente, M. Trini, Johannes Schulz, Florian Lukas Briechle, A. Cancio, B. Caccianiga, Alexey Yushkov, Max Malacari, Lili Yang, Luca Latronico, Piotr Homola, Alex Tapia, Tobias Winchen, P. Lebrun, Karen S. Caballero-Mora, Martin Erdmann, Carla Bonifazi, Beatriz García, Roger W Clay, Stefano D'Amico, Jose A. Bellido, Daniel Kuempel, S. Sonntag, Carlos Escobar, Jaime Rosado, R.M. Kieckhafer, B. Vargas Cárdenas, I. Valiño, J. Neuser, Ivone F. M. Albuquerque, Ke Fang, I. Katkov, Richard Dallier, Gaetano Salina, A.M. van den Berg, Darko Veberič, Jan Ridky, Marc Weber, M. Buscemi, D. Nosek, Jan Ebr, Sergio Petrera, S. Messina, S. Coutu, Norberto Fazzini, Aab, A., Abreu, P., Aglietta, M., Ahn, E. J., Al Samarai, I., Albuquerque, I. F. M., Allekotte, I., Allison, P., Almela, A., Alvarez Castillo, J., Alvarez Muñiz, J., Ambrosio, M., Anastasi, G. A., Anchordoqui, L., Andrada, B., Andringa, S., Aramo, C., Arqueros, F., Arsene, N., Asorey, H., Assis, P., Aublin, J., Avila, G., Badescu, A. M., Balaceanu, A., Baus, C., Beatty, J. J., Becker, K. H., Bellido, J. A., Berat, C., Bertaina, M. E., Bertou, X., Biermann, P. L., Billoir, P., Biteau, J., Blaess, S. G., Blanco, A., Blazek, J., Bleve, Carla, Boháčová, M., Boncioli, D., Bonifazi, C., Borodai, N., Botti, A. M., Brack, J., Brancus, I., Bretz, T., Bridgeman, A., Briechle, F. L., Buchholz, P., Bueno, A., Buitink, S., Buscemi, M., Caballero Mora, K. S., Caccianiga, B., Caccianiga, L., Cancio, A., Canfora, F., Caramete, L., Caruso, R., Castellina, A., Cataldi, G., Cazon, L., Cester, R., Chavez, A. G., Chiavassa, A., Chinellato, J. A., Chudoba, J., Clay, R. W., Colalillo, R., Coleman, A., Collica, L., Coluccia, MARIA RITA, Conceição, R., Contreras, F., Cooper, M. J., Coutu, S., Covault, C. E., Cronin, J., Dallier, R., D'Amico, Stefano, Daniel, B., Dasso, S., Daumiller, K., Dawson, B. R., de Almeida, R. M., de Jong, S. J., De Mauro, G., de Mello Neto, J. R. T., DE MITRI, Ivan, de Oliveira, J., de Souza, V., Debatin, J., del Peral, L., Deligny, O., Di Giulio, C., Di Matteo, A., Díaz Castro, M. L., Diogo, F., Dobrigkeit, C., D'Olivo, J. C., Dorofeev, A., dos Anjos, R. C., Dova, M. T., Dundovic, A., Ebr, J., Engel, R., Erdmann, M., Erfani, M., Escobar, C. O., Espadanal, J., Etchegoyen, A., Falcke, H., Fang, K., Farrar, G., Fauth, A. C., Fazzini, N., Fick, B., Figueira, J. M., Filevich, A., Filipčič, A., Fratu, O., Freire, M. M., Fujii, T., Fuster, A., García, B., Garcia Pinto, D., Gaté, F., Gemmeke, H., Gherghel Lascu, A., Ghia, P. L., Giaccari, U., Giammarchi, M., Giller, M., Głas, D., Glaser, C., Glass, H., Golup, G., Gómez Berisso, M., Gómez Vitale, P. F., González, N., Gookin, B., Gordon, J., Gorgi, A., Gorham, P., Gouffon, P., Grillo, A. F., Grubb, T. D., Guarino, F., Guedes, G. P., Hampel, M. R., Hansen, P., Harari, D., Harrison, T. A., Harton, J. L., Hasankiadeh, Q., Haungs, A., Hebbeker, T., Heck, D., Heimann, P., Herve, A. E., Hill, G. C., Hojvat, C., Holt, E., Homola, P., Hörandel, J. R., Horvath, P., Hrabovský, M., Huege, T., Hulsman, J., Insolia, A., Isar, P. G., Jandt, I., Jansen, S., Johnsen, J. A., Josebachuili, M., Kääpä, A., Kambeitz, O., Kampert, K. H., Kasper, P., Katkov, I., Keilhauer, B., Kemp, E., Kieckhafer, R. M., Klages, H. O., Kleifges, M., Kleinfeller, J., Krause, R., Krohm, N., Kuempel, D., Kukec Mezek, G., Kunka, N., Kuotb Awad, A., Lahurd, D., Latronico, L., Lauscher, M., Lautridou, P., Lebrun, P., Legumina, R., Leigui de Oliveira, M. A., Letessier Selvon, A., Lhenry Yvon, I., Link, K., Lopes, L., López, R., López Casado, A., Luce, Q., Lucero, A., Malacari, M., Mallamaci, M., Mandat, D., Mantsch, P., Mariazzi, A. G., Mariş, I. C., Marsella, Giovanni, Martello, Daniele, Martinez, H., Martínez Bravo, O., Masías Meza, J. J., Mathes, H. J., Mathys, S., Matthews, J., Matthews, J. A. J., Matthiae, G., Mayotte, E., Mazur, P. O., Medina, C., Medina Tanco, G., Melo, D., Menshikov, A., Messina, S., Micheletti, M. I., Middendorf, L., Minaya, I. A., Miramonti, L., Mitrica, B., Mockler, D., Molina Bueno, L., Mollerach, S., Montanet, F., Morello, C., Mostafá, M., Müller, G., Muller, M. A., Müller, S., Naranjo, I., Navas, S., Nellen, L., Neuser, J., Nguyen, P. H., Niculescu Oglinzanu, M., Niechciol, M., Niemietz, L., Niggemann, T., Nitz, D., Nosek, D., Novotny, V., Nožka, H., Núñez, L. A., Ochilo, L., Oikonomou, F., Olinto, A., Pakk Selmi Dei, D., Palatka, M., Pallotta, J., Papenbreer, P., Parente, G., Parra, A., Paul, T., Pech, M., Pedreira, F., Pękala, J., Pelayo, R., Peña Rodriguez, J., Pereira, L. A. S., Perrone, Lorenzo, Peters, C., Petrera, S., Phuntsok, J., Piegaia, R., Pierog, T., Pieroni, P., Pimenta, M., Pirronello, V., Platino, M., Plum, M., Porowski, C., Prado, R. R., Privitera, P., Prouza, M., Quel, E. J., Querchfeld, S., Quinn, S., Ramos Pollant, R., Rautenberg, J., Ravel, O., Ravignani, D., Reinert, D., Revenu, B., Ridky, J., Risse, M., Ristori, P., Rizi, V., Rodrigues de Carvalho, W., Rodriguez Fernandez, G., Rodriguez Rojo, J., Rodríguez Frías, M. D., Rogozin, D., Rosado, J., Roth, M., Roulet, E., Rovero, A. C., Saffi, S. J., Saftoiu, A., Salazar, H., Saleh, A., Salesa Greus, F., Salina, G., Sanabria Gomez, J. D., Sánchez, F., Sanchez Lucas, P., Santos, E. M., Santos, E., Sarazin, F., Sarkar, B., Sarmento, R., Sarmiento Cano, C., Sato, R., Scarso, C., Schauer, M., Scherini, Viviana, Schieler, H., Schmidt, D., Scholten, O., Schovánek, P., Schröder, F. G., Schulz, A., Schulz, J., Schumacher, J., Sciutto, S. J., Segreto, A., Settimo, Mariangela, Shadkam, A., Shellard, R. C., Sigl, G., Silli, G., Sima, O., Śmiałkowski, A., Šmída, R., Snow, G. R., Sommers, P., Sonntag, S., Sorokin, J., Squartini, R., Stanca, D., Stanič, S., Stasielak, J., Strafella, Francesco, Suarez, F., Suarez Durán, M., Sudholz, T., Suomijärvi, T., Supanitsky, A. D., Sutherland, M. S., Swain, J., Szadkowski, Z., Taborda, O. A., Tapia, A., Tepe, A., Theodoro, V. M., Timmermans, C., Todero Peixoto, C. J., Tomankova, L., Tomé, B., Tonachini, A., Torralba Elipe, G., Torres Machado, D., Torri, M., Travnicek, P., Trini, M., Ulrich, R., Unger, M., Urban, M., Valbuena Delgado, A., Valdés Galicia, J. F., Valiño, I., Valore, L., van Aar, G., van Bodegom, P., van den Berg, A. M., van Vliet, A., Varela, E., Vargas Cárdenas, B., Varner, G., Vázquez, J. R., Vázquez, R. A., Veberič, D., Verzi, V., Vicha, J., Villaseñor, L., Vorobiov, S., Wahlberg, H., Wainberg, O., Walz, D., Watson, A. A., Weber, M., Weindl, A., Wiencke, L., Wilczyński, H., Winchen, T., Wittkowski, D., Wundheiler, B., Wykes, S., Yang, L., Yelos, D., Younk, P., Yushkov, A., Zas, E., Zavrtanik, D., Zavrtanik, M., Zepeda, A., Zimmermann, B., Ziolkowski, M., Zong, Z., Zuccarello, F., Bleve, C., Colalillo, Roberta, Coluccia, M. R., D'Amico, S., De Mitri, I., Guarino, Fausto, Marsella, G., Martello, D., Pȩkala, J., Perrone, L., Scherini, V., Settimo, M., Strafella, F., Valore, Laura, Physics, Astronomy and Astrophysics Research Group, Elementary Particle Physics, Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), and Pierre Auger Collaboration

Subjects
[PHYS.ASTR.HE]Physics [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], Nuclear and High Energy Physics, Proton, Pierre Auger Observatory, Cosmic Rays, Mass Composition, Astronomy, Astrophysics::High Energy Astrophysical Phenomena, Flux, FOS: Physical sciences, Cosmic ray, Ankle, Cosmic rays, Mass composition, Astrophysics, 01 natural sciences, Auger, Observatory, 0103 physical sciences, ddc:530, High Energy Physics, 010303 astronomy & astrophysics, GeneralLiterature_REFERENCE(e.g.,dictionaries,encyclopedias,glossaries), Cherenkov radiation, Ciencias Exactas, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Range (particle radiation), 010308 nuclear & particles physics, OBSERVATÓRIOS, Astrophysics::Instrumentation and Methods for Astrophysics, Física, lcsh:QC1-999, Physique atomique et nucléaire, Experimental High Energy Physics, Física nuclear, Astrophysics - High Energy Astrophysical Phenomena, lcsh:Physics
Abstract

We report a first measurement for ultrahigh energy cosmic rays of the correlation between the depth of shower maximum and the signal in the water Cherenkov stations of air-showers registered simultaneously by the fluorescence and the surface detectors of the Pierre Auger Observatory. Such a correlation measurement is a unique feature of a hybrid air-shower observatory with sensitivity to both the electromagnetic and muonic components. It allows an accurate determination of the spread of primary masses in the cosmic-ray flux. Up till now, constraints on the spread of primary masses have been dominated by systematic uncertainties. The present correlation measurement is not affected by systematics in the measurement of the depth of shower maximum or the signal in the water Cherenkov stations. The analysis relies on general characteristics of air showers and is thus robust also with respect to uncertainties in hadronic event generators. The observed correlation in the energy range around the ‘ankle’ at lg⁡(E/eV)=18.5–19.0 differs significantly from expectations for pure primary cosmic-ray compositions. A light composition made up of proton and helium only is equally inconsistent with observations. The data are explained well by a mixed composition including nuclei with mass A>4. Scenarios such as the proton dip model, with almost pure compositions, are thus disfavored as the sole explanation of the ultrahigh-energy cosmic-ray flux at Earth., 0, SCOPUS: ar.j, info:eu-repo/semantics/published

Published
2016
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276. Ultrahigh-energy neutrino follow-up of gravitational wave events GW150914 and GW151226 with the Pierre Auger Observatory

Author

F. Canfora, P. Heimann, Q. Luce, P. Abreu, R.J. Barreira Luz, G. A. Anastasi, E. Kemp, D. Ravignani, Serguei Vorobiov, D. Mockler, Luis A. Anchordoqui, C. Aramo, John N. Matthews, R. M. Kieckhafer, O. A. Taborda, Johannes Schumacher, G. Matthiae, M. Platino, Antonio Bueno, M. Josebachuili, O. Wainberg, K. H. Becker, Gualberto Avila, B. Mitrica, Heino Falcke, E.M. Holt, Ingomar Allekotte, G. De Mauro, A. Fuster, Maria-Teresa Dova, M. R. Hampel, S. Petrera, G. S. Varner, Sarka Wykes, Octavian Fratu, Angela V. Olinto, R.C. dos Anjos, Julian Rautenberg, M. Palatka, C. Di Giulio, G. C. Hill, M. Mallamaci, S. J. De Jong, Jörg R. Hörandel, J. Vicha, Petr Travnicek, Trent D. Grubb, R. Squartini, Jeffrey A. Johnsen, Juan Manuel Figueira, Roberta Colalillo, A. G. Mariazzi, Ralph Engel, T. Paul, J. Ridky, M. Suarez Durán, J. Stasielak, S. Coutu, Ugo Giaccari, F. Montanet, S. Quinn, Günter Sigl, M. Trini, David Wittkowski, M. Urban, Norberto Fazzini, J. F. Valdés Galicia, I. De Mitri, L. Molina-Bueno, D. Melo, David Walz, G. Medina-Tanco, D. Pakk Selmi-Dei, R. Sato, J. R. T. de Mello Neto, M. Hrabovský, G. van Aar, Radomir Smida, A. C. Rovero, C. Bleve, Alexandru Balaceanu, Hernan Wahlberg, Andreas Weindl, M. Zavrtanik, H. Nožka, R. Gaior, Dieter Heck, Lourenco Lopes, A. Gorgi, A. Saleh, Vincenzo Rizi, Octavian Sima, M. A. Leigui de Oliveira, G. Müller, N. Kunka, H. Glass, M. Ambrosio, V. Scherini, G. Torralba Elipe, R. R. Prado, G. Kukec Mezek, L. Nellen, Alexandra Saftoiu, M. Schauer, D. Yelos, C. Porowski, Florian Gaté, M. Erdmann, A. van Vliet, Andreas Haungs, A. Coleman, M. Ziolkowski, O. Martínez Bravo, C. J. Todero Peixoto, C. Morello, Dusan Mandat, A. Parra, I. Lhenry-Yvon, M. E. Bertaina, V. de Souza, L. Valore, O. Kambeitz, H. Martinez, I. Naranjo, A. Menshikov, F. Suarez, Thomas Hebbeker, M. A. Muller, J. J. Beatty, N. Krohm, Andrej Dundovic, P. Ristori, Danielle LaHurd, Olivier Deligny, E. Mayotte, E. Varela, J.D. Sanabria Gomez, Petr Schovanek, Sergio Dasso, Tristan Sudholz, W. Rodrigues de Carvalho, Paul Sommers, A. Blanco, B. Sarkar, Lorenzo Caccianiga, V. M. Theodoro, A. Kääpä, P. H. Nguyen, A. Segreto, Silvia Mollerach, D. Garcia-Pinto, Christian Glaser, P. Gouffon, J. W. Cronin, Philipp Papenbreer, J. Espadanal, Peter L. Biermann, P. Stassi, Denise Boncioli, J. Rodriguez Rojo, R. Krause, J. A.J. Matthews, Xavier Bertou, J. D. Swain, P. van Bodegom, A. Kuotb Awad, V. Pirronello, A. G. Chavez, Alberto Daniel Supanitsky, Francesco Strafella, J. L. Harton, P. Lebrun, Julien Aublin, D. Nosek, Paolo Privitera, M. J. Cooper, S. G. Blaess, Jaime Alvarez-Muñiz, F. Sánchez, Alexandru Gherghel-Lascu, A. Aab, J. Biteau, H. Wilczyński, P. Billoir, Tanguy Pierog, Pedro Assis, A. Insolia, B. Tome, Ana Martina Botti, M. Kleifges, D. Zavrtanik, A. Cancio, A. Etchegoyen, Peter Mazur, A. Shadkam, Carlos Medina, Nataliia Borodai, Hermann-Josef Mathes, Enrique Zas, A. Di Matteo, I. Al Samarai, G. Marsella, L. Caramete, Marco Giammarchi, Markus Roth, H. Gemmeke, Dariusz Glas, Denis Stanca, T. Suomijärvi, D. Martello, Jose Chinellato, C. Peters, Michael Unger, B. Wundheiler, L. A. S. Pereira, Maria Giller, M. I. Micheletti, Peter Gorham, Charles Timmermans, Lukas Middendorf, Fernando Contreras, Gregory R Snow, L. Collica, I. Jandt, A. Letessier-Selvon, J. Hulsman, I. A. Minaya, B. Keilhauer, G. P. Guedes, Toshihiro Fujii, S. Jansen, Kai Daumiller, S. Müller, Lorenzo Cazon, Ralf Ulrich, Paul M. Mantsch, B. Vargas Cárdenas, André Schulz, J. Debatin, M. Gómez Berisso, R. C. Shellard, L. Perrone, Jiri Chudoba, G. Rodriguez Fernandez, D. Torres Machado, V. Verzi, J. Pallotta, David Schmidt, M. L. Díaz Castro, G. Farrar, S. J. Sciutto, Katrin Link, Maria Rita Coluccia, Carola Dobrigkeit, Juan Carlos D'Olivo, M. Plum, Hernán Asorey, E. J. Quel, Bruno Daniel, Foteini Oikonomou, I. C. Mariş, Luis A. Nunez, R. Piegaia, Marcus Niechciol, Esteban Roulet, P. L. Ghia, Mario Buscemi, Francesca Zuccarello, Paula Gina Isar, J. J. Masías Meza, Jeffrey Brack, Olaf Scholten, Humberto Ibarguen Salazar, Thomas Harrison, Jesús Peña-Rodríguez, D. Nitz, A. Dorofeev, Alan Watson, Mihai Niculescu-Oglinzanu, F. Salesa Greus, G. Cataldi, Igor Katkov, J. Alvarez Castillo, P. Pieroni, Jan Pękala, Harald Schieler, F. Diogo, A. Taboada, A. E. Herve, A. Yushkov, Marco Torri, F. Arqueros, R. M. de Almeida, L. R. Wiencke, L. Villaseñor, Peter Hansen, Miguel Mostafa, Martina Bohacova, A. Śmiałkowski, D. Reinert, L. Tomankova, L. Ochilo, J. Sorokin, Z. Zong, Diego Harari, I. Valiño, P.F. Gómez Vitale, F. Guarino, Peter Buchholz, A. López Casado, Zbigniew Szadkowski, Brian Fick, Samo Stanič, Nicusor Arsene, A. Tapia, Rodrigo Pelayo, Stijn Buitink, E. Santos, I.M. Brancus, A. Bridgeman, B. Gookin, R. Ramos-Pollan, S. Messina, S. Querchfeld, S. J. Saffi, V. Novotny, Rossella Caruso, A. Lucero, S. Mathys, Marco Aglietta, J. Neuser, L. Niemietz, E. M. Santos, M. Erfani, R. A. Vázquez, Gaia Silli, F. Sarazin, Arnulfo Zepeda, Marc Weber, F. G. Schröder, B. Revenu, Markus Lauscher, Benedikt Zimmermann, Rúben Conceição, J. R. Vázquez, F. Pedreira, P. Sanchez-Lucas, P. Kasper, J. Phuntsok, Raul Sarmento, M. M. Freire, Bruce R. Dawson, Tim Huege, Alina Mihaela Badescu, M. Prouza, Tim Niggemann, Miroslav Pech, Nicolás González, A. C. Fauth, Corinne Berat, Q. Hasankiadeh, Pavel Horvath, Carla Bonifazi, A. Filipcic, Jose A. Bellido, S. Sonntag, B. Andrada, Sofia Andringa, R. Cester, C. A. Sarmiento, I.D. Vergara Quispe, M. Risse, Jonathan Blazek, G. Parente, Carlos Hojvat, R. Legumina, D. Rogozin, J. de Oliveira, Alejandro Almela, Julian Kemp, Michael Schimp, Colin Baus, Karl-Heinz Kampert, Antonella Castellina, Thomas Bretz, Corbin Covault, Geraldina Golup, Alexander Grillo, Lino Miramonti, B. García, Tobias Winchen, R. López, Karen S. Caballero-Mora, Roger W Clay, Stefano D'Amico, Johannes Schulz, M. Pimenta, Florian Lukas Briechle, Mariangela Settimo, Max Malacari, Lili Yang, Piotr Homola, J. Kleinfeller, Daniel Kuempel, Carlos Escobar, Ivone F. M. Albuquerque, Ke Fang, Jan Ebr, H.O. Klages, Gaetano Salina, A.M. van den Berg, Darko Veberič, Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Pierre Auger Collaboration, Research unit Astroparticle Physics, Aab, A., Abreu, P., Aglietta, M., Al Samarai, I., Albuquerque, I. . f. . m., Allekotte, I., Almela, A., Alvarez Castillo, J., Alvarez Muñiz, J., Ambrosio, M., Anastasi, G. . a., Anchordoqui, L., Andrada, B., Andringa, S., Aramo, C., Arqueros, F., Arsene, N., Asorey, H., Assis, P., Aublin, J., Avila, G., Badescu, A. . m., Balaceanu, A., Barreira Luz, R. . j., Baus, C., Beatty, J. . j., Becker, K. . h., Bellido, J. . a., Berat, C., Bertaina, M. . e., Bertou, X., Biermann, P. . l., Billoir, P., Biteau, J., Blaess, S. . g., Blanco, A., Blazek, J., Bleve, C., Boháčová, M., Boncioli, D., Bonifazi, C., Borodai, N., Botti, A. . m., Brack, J., Brancus, I., Bretz, T., Bridgeman, A., Briechle, F. . l., Buchholz, P., Bueno, A., Buitink, S., Buscemi, M., Caballero Mora, K. . s., Caccianiga, L., Cancio, A., Canfora, F., Caramete, L., Caruso, R., Castellina, A., Cataldi, G., Cazon, L., Cester, R., Chavez, A. . g., Chinellato, J. . a., Chudoba, J., Clay, R. . w., Colalillo, Roberta, Coleman, A., Collica, L., Coluccia, M. . r., Conceição, R., Contreras, F., Cooper, M. . j., Coutu, S., Covault, C. . e., Cronin, J., D’Amico, S., Daniel, B., Dasso, S., Daumiller, K., Dawson, B. . r., de Almeida, R. . m., de Jong, S. . j., De Mauro, G., de Mello Neto, J. . r. . t., De Mitri, I., de Oliveira, J., de Souza, V., Debatin, J., Deligny, O., Di Giulio, C., Di Matteo, A., Díaz Castro, M. . l., Diogo, F., Dobrigkeit, C., D’Olivo, J. . c., Dorofeev, A., dos Anjos, R. . c., Dova, M. . t., Dundovic, A., Ebr, J., Engel, R., Erdmann, M., Erfani, M., Escobar, C. . o., Espadanal, J., Etchegoyen, A., Falcke, H., Fang, K., Farrar, G., Fauth, A. . c., Fazzini, N., Fick, B., Figueira, J. . m., Filipčič, A., Fratu, O., Freire, M. . m., Fujii, T., Fuster, A., Gaior, R., García, B., Garcia Pinto, D., Gaté, F., Gemmeke, H., Gherghel Lascu, A., Ghia, P. . l., Giaccari, U., Giammarchi, M., Giller, M., Głas, D., Glaser, C., Glass, H., Golup, G., Gómez Berisso, M., Gómez Vitale, P. . f., González, N., Gookin, B., Gorgi, A., Gorham, P., Gouffon, P., Grillo, A. . f., Grubb, T. . d., Guarino, Fausto, Guedes, G. . p., Hampel, M. . r., Hansen, P., Harari, D., Harrison, T. . a., Harton, J. . l., Hasankiadeh, Q., Haungs, A., Hebbeker, T., Heck, D., Heimann, P., Herve, A. . e., Hill, G. . c., Hojvat, C., Holt, E., Homola, P., Hörandel, J. . r., Horvath, P., Hrabovský, M., Huege, T., Hulsman, J., Insolia, A., Isar, P. . g., Jandt, I., Jansen, S., Johnsen, J. . a., Josebachuili, M., Kääpä, A., Kambeitz, O., Kampert, K. . h., Kasper, P., Katkov, I., Keilhauer, B., Kemp, E., Kemp, J., Kieckhafer, R. . m., Klages, H. . o., Kleifges, M., Kleinfeller, J., Krause, R., Krohm, N., Kuempel, D., Kukec Mezek, G., Kunka, N., Kuotb Awad, A., Lahurd, D., Lauscher, M., Lebrun, P., Legumina, R., Leigui de Oliveira, M. . a., Letessier Selvon, A., Lhenry Yvon, I., Link, K., Lopes, L., López, R., López Casado, A., Luce, Q., Lucero, A., Malacari, M., Mallamaci, M., Mandat, D., Mantsch, P., Mariazzi, A. . g., Mariş, I. . c., Marsella, G., Martello, D., Martinez, H., Martínez Bravo, O., Masías Meza, J. . j., Mathes, H. . j., Mathys, S., Matthews, J., Matthews, J. . a. . j., Matthiae, G., Mayotte, E., Mazur, P. . o., Medina, C., Medina Tanco, G., Melo, D., Menshikov, A., Messina, S., Micheletti, M. . i., Middendorf, L., Minaya, I. . a., Miramonti, L., Mitrica, B., Mockler, D., Molina Bueno, L., Mollerach, S., Montanet, F., Morello, C., Mostafá, M., Müller, G., Muller, M. . a., Müller, S., Naranjo, I., Nellen, L., Neuser, J., Nguyen, P. . h., Niculescu Oglinzanu, M., Niechciol, M., Niemietz, L., Niggemann, T., Nitz, D., Nosek, D., Novotny, V., Nožka, H., Núñez, L. . a., Ochilo, L., Oikonomou, F., Olinto, A., Pakk Selmi Dei, D., Palatka, M., Pallotta, J., Papenbreer, P., Parente, G., Parra, A., Paul, T., Pech, M., Pedreira, F., Pękala, J., Pelayo, R., Peña Rodriguez, J., Pereira, L. . a. . s., Perrone, L., Peters, C., Petrera, S., Phuntsok, J., Piegaia, R., Pierog, T., Pieroni, P., Pimenta, M., Pirronello, V., Platino, M., Plum, M., Porowski, C., Prado, R. . r., Privitera, P., Prouza, M., Quel, E. . j., Querchfeld, S., Quinn, S., Ramos Pollan, R., Rautenberg, J., Ravignani, D., Reinert, D., Revenu, B., Ridky, J., Risse, M., Ristori, P., Rizi, V., Rodrigues de Carvalho, W., Rodriguez Fernandez, G., Rodriguez Rojo, J., Rogozin, D., Roth, M., Roulet, E., Rovero, A. . c., Saffi, S. . j., Saftoiu, A., Salazar, H., Saleh, A., Salesa Greus, F., Salina, G., Sanabria Gomez, J. . d., Sánchez, F., Sanchez Lucas, P., Santos, E. . m., Santos, E., Sarazin, F., Sarkar, B., Sarmento, R., Sarmiento, C. . a., Sato, R., Schauer, M., Scherini, V., Schieler, H., Schimp, M., Schmidt, D., Scholten, O., Schovánek, P., Schröder, F. . g., Schulz, A., Schulz, J., Schumacher, J., Sciutto, S. . j., Segreto, A., Settimo, M., Shadkam, A., Shellard, R. . c., Sigl, G., Silli, G., Sima, O., Śmiałkowski, A., Šmída, R., Snow, G. . r., Sommers, P., Sonntag, S., Sorokin, J., Squartini, R., Stanca, D., Stanič, S., Stasielak, J., Stassi, P., Strafella, F., Suarez, F., Suarez Durán, M., Sudholz, T., Suomijärvi, T., Supanitsky, A. . d., Swain, J., Szadkowski, Z., Taboada, A., Taborda, O. . a., Tapia, A., Theodoro, V. . m., Timmermans, C., Todero Peixoto, C. . j., Tomankova, L., Tomé, B., Torralba Elipe, G., Torres Machado, D., Torri, M., Travnicek, P., Trini, M., Ulrich, R., Unger, M., Urban, M., Valdés Galicia, J. . f., Valiño, I., Valore, Laura, van Aar, G., van Bodegom, P., van den Berg, A. . m., van Vliet, A., Varela, E., Vargas Cárdenas, B., Varner, G., Vázquez, J. . r., Vázquez, R. . a., Veberič, D., Vergara Quispe, I. . d., Verzi, V., Vicha, J., Villaseñor, L., Vorobiov, S., Wahlberg, H., Wainberg, O., Walz, D., Watson, A. . a., Weber, M., Weindl, A., Wiencke, L., Wilczyński, H., Winchen, T., Wittkowski, D., Wundheiler, B., Wykes, S., Yang, L., Yelos, D., Yushkov, A., Zas, E., Zavrtanik, D., Zavrtanik, M., Zepeda, A., Zimmermann, B., Ziolkowski, M., Zong, Z., Zuccarello, F., Bleve, Carla, Colalillo, R., Coluccia, MARIA RITA, D'Amico, Stefano, DE MITRI, Ivan, Guarino, F., Marsella, Giovanni, Martello, Daniele, Perrone, Lorenzo, Strafella, Francesco, Valore, L., Elementary Particle Physics, and Physics

Subjects
[PHYS.ASTR.HE]Physics [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], Astronomy, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, magnetic fields, 7. Clean energy, 01 natural sciences, Ultrahigh-energy neutrino, gravitational waves, ultra-high energy cosmic rays, Observatory, 0103 physical sciences, GW151226, binary systems, High Energy Physics, 010303 astronomy & astrophysics, GeneralLiterature_REFERENCE(e.g.,dictionaries,encyclopedias,glossaries), gravitational wave, Ciencias Exactas, Pierre Auger Observatory, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), GAMMA-RAY BURSTS, 010308 nuclear & particles physics, Gravitational wave, Física, neutrinos, ASTROFÍSICA, black holes, LIGO, Black hole, 13. Climate action, Experimental High Energy Physics, Física nuclear, High Energy Physics::Experiment, Neutrino, Gamma-ray burst, Astrophysics - High Energy Astrophysical Phenomena
Abstract

On September 14, 2015 the Advanced LIGO detectors observed their first gravitational wave (GW) transient GW150914. This was followed by a second GW event observed on December 26, 2015. Both events were inferred to have arisen from the merger of black holes in binary systems. Such a system may emit neutrinos if there are magnetic fields and disk debris remaining from the formation of the two black holes. With the surface detector array of the Pierre Auger Observatory we can search for neutrinos with energy Eν above 100 PeV from pointlike sources across the sky with equatorial declination from about -65° to +60°, and, in particular, from a fraction of the 90% confidence-level inferred positions in the sky of GW150914 and GW151226. A targeted search for highly inclined extensive air showers, produced either by interactions of downward-going neutrinos of all flavors in the atmosphere or by the decays of tau leptons originating from tau-neutrino interactions in the Earth's crust (Earth-skimming neutrinos), yielded no candidates in the Auger data collected within ±500 s around or 1 day after the coordinated universal time (UTC) of GW150914 and GW151226, as well as in the same search periods relative to the UTC time of the GW candidate event LVT151012. From the nonobservation we constrain the amount of energy radiated in ultrahigh-energy neutrinos from such remarkable events., La lista completa de autores que integran el documento puede consultarse en el archivo., Facultad de Ciencias Exactas, Instituto de Física La Plata

Published
2016
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277. Probing MACHOs by observation of M 31 pixel lensing with the 1.5 m Loiano telescope

Author

G. Ingrosso, Giovanni Covone, Gaetano Scarpetta, Ph. Jetzer, A. A. Nucita, Francesco Strafella, Martin Dominik, Andrew Gould, F. De Paolis, S. Calchi Novati, Y. Giraud-Héraud, Luigi Mancini, Calchi Novati, S., Covone, Giovanni, de Paolis, F., Dominik, M., Giraud Héraud, Y., Ingrosso, G., Jetzer, P., Mancini, L., Nucita, A., Scarpetta, G., Strafella, F., Gould, A., APC - Cosmologie, AstroParticule et Cosmologie (APC (UMR_7164)), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), CALCHI NOVATI, S, Covone, G, DE PAOLIS, Francesco, Dominik, M, GIRAUD HRAUD, Y, Ingrosso, Gabriele, Jetzer, Ph, Mancini, L, Nucita, Achille, Scarpetta, G, Strafella, Francesco, Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Physique Corpusculaire et Cosmologie - Collège de France (PCC), and Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Collège de France (CdF)-Centre National de la Recherche Scientifique (CNRS)

Subjects
[SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Gravitational lensing, FOS: Physical sciences, Astrophysics, Gravitational microlensing, 01 natural sciences, law.invention, Telescope, Galactic halo, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], astro-ph, law, 0103 physical sciences, 010303 astronomy & astrophysics, Galaxy: Halo, Physics, Pixel, 010308 nuclear & particles physics, Astrophysics (astro-ph), Astronomy and Astrophysics, Galaxy, Stars, Variable source, Gravitational lens, Space and Planetary Science, Galaxies: M31
Abstract

We analyse a series of pilot observations in order to study microlensing of (unresolved) stars in M31 with the 1.5m Loiano telescope, including observations on both identified variable source stars and reported microlensing events. We also look for previously unknown variability and discover a nova. We discuss an observing strategy for an extended campaign with the goal of determining whether MACHOs exist or whether all microlensing events are compatible with lens stars in M31., Accepted for publication as a research Note in Astronomy & Astrophysics

Published
2007
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279. Microlensing search towards M31

Author

G. Ingrosso, Ph. Jetzer, Andrew Gould, C. Rubano, F. De Paolis, A. A. Marino, A. Bouquet, R. de Ritis, Y. Le Du, Mauro Sereno, Giovanni Covone, Gerardo Iovane, V. F. Cardone, M. Roncadelli, S. Calchi Novati, V. Bozza, Gaetano Lambiase, Ester Piedipalumbo, P. Baillon, Salvatore Capozziello, Paolo Scudellaro, Michel Aurière, V. Re, Y. Giraud-Héraud, Gaetano Scarpetta, Luigi Mancini, Francesco Strafella, Jean Kaplan, M. Capaccioli, CALCHI NOVATI, S., Iovane, G., Marino, A. A., Auriere, M., Baillon, P., Bouquet, A., Bozza, V., Capaccioli, M., Capozziello, S., Cardone, V., Covone, G., DE PAOLIS, Francesco, DE RITIS, R., GIRAUD HERAUD, Y., Gould, A., Ingrosso, Gabriele, Jetzer, P. H., Kaplan, J., Lambiase, G., LE DOU, Y., Mancini, L., Piedipalumbo, E., Re, V., Roncadelli, M., Rubano, C., Scarpetta, G., Scudellaro, P., Sereno, M., Strafella, Francesco, Capaccioli, Massimo, Capozziello, Salvatore, DE PAOLIS, F., Ingrosso, G., LE DU, Y., Piedipalumbo, Ester, Rubano, Claudio, Scudellaro, Paolo, Strafella, F., Physique Corpusculaire et Cosmologie - Collège de France (PCC), and Collège de France (CdF (institution))-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Astrophysics and Astronomy, observational, methods : data analysis, cosmology : observations, dark matter, gravitational lensing, galaxies : M 31, Andromeda Galaxy, Astrophysics::High Energy Astrophysical Phenomena, Monte Carlo method, Dark matter, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Gravitational microlensing, 01 natural sciences, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Settore FIS/05 - Astronomia e Astrofisica, 0103 physical sciences, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Astrophysics (astro-ph), Astronomy and Astrophysics, Observable, Light curve, Space and Planetary Science, Data analysis, Halo
Abstract

We present the first results of the analysis of data collected during the 1998-99 observational campaign at the 1.3 meter McGraw-Hill Telescope, towards the Andromeda galaxy (M31), aimed to the detection of gravitational microlensing effects as a probe of the presence of dark matter in our and in M31 halo. The analysis is performed using the pixel lensing technique, which consists in the study of flux variations of unresolved sources and has been proposed and implemented by the AGAPE collaboration. We carry out a shape analysis by demanding that the detected flux variations be achromatic and compatible with a Paczynski light curve. We apply the Durbin-Watson hypothesis test to the residuals. Furthermore, we consider the background of variables sources. Finally five candidate microlensing events emerge from our selection. Comparing with the predictions of a Monte Carlo simulation, assuming a standard spherical model for the M31 and Galactic haloes, and typical values for the MACHO mass, we find that our events are only marginally consistent with the distribution of observable parameters predicted by the simulation., 13 pages, To appear in A&A

Published
2002
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280. The Hi-GAL compact source catalogue – II. The 360° catalogue of clump physical properties

Author

Stefano Pezzuto, Sarah Ragan, Kazi L.J. Rygl, Alberto Noriega-Crespo, Lorenzo Piazzo, Luca Olmi, David Eden, Alessio Traficante, Göran Pilbratt, Peter Schilke, Jonathan C. Tan, A. Baldeschi, Rene Plume, P. Palmeirim, Annie Zavagno, Roberta Paladini, M. Benedettini, John Bally, D. Russeil, E. Fiorellino, M. R. Pestalozzi, Peter G. Martin, Davide Elia, Sergio Molinari, D. Polychroni, Manuel Merello, S. J. Liu, A. M. di Giorgio, Toby J. T. Moore, P. Mège, Francesco Strafella, Eugenio Schisano, Elia, D., Merello, M., Molinari, S., Schisano, E., Zavagno, A., Russeil, D., Mege, P., Martin, P. G., Olmi, L., Pestalozzi, M., Plume, R., Ragan, S. E., Benedettini, M., Eden, D. J., Moore, T. J. T., Noriega-Crespo, A., Paladini, R., Palmeirim, P., Pezzuto, S., Pilbratt, G. L., Rygl, K. L. J., Schilke, P., Strafella, F., Tan, J. C., Traficante, A., Baldeschi, A., Bally, J., Giorgio, A. M. D., Fiorellino, E., Liu, S. J., Piazzo, L., Polychroni, D., Department of Physics and Astronomy [Calgary], University of Calgary, Istituto di Astrofisica e Planetologia Spaziali - INAF (IAPS), Istituto Nazionale di Astrofisica (INAF), Space Telescope Science Institute (STSci), Centre d'étude spatiale des rayonnements (CESR), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Universidade do Porto = University of Porto, INAF - Osservatorio Astronomico di Roma (OAR), Universität zu Köln = University of Cologne, European Southern Observatory (ESO), Università degli Studi di Roma Tor Vergata [Roma], Departamento de Astronomia (DAS), Laboratoire d'Astrophysique de Marseille (LAM), and Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Stars: formation, Extinction (astronomy), cloud [ISM], FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, ISM: clouds, 01 natural sciences, Luminosity, Photometry (optics), 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, ISM [submillimeter], 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, formation [Stars], infrared: ISM, Physics, Spiral galaxy, extinction, 010308 nuclear & particles physics, Star formation, local interstellar matter, ISM [infrared], Astronomy and Astrophysics, Galactic plane, Astrophysics - Astrophysics of Galaxies, Galaxy, [SDU]Sciences of the Universe [physics], Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), submillimeter: ISM, Spectral energy distribution, dust, dust, extinction
Abstract

We present the $360^\circ$ catalogue of physical properties of Hi-GAL compact sources, detected between 70 and 500 $\mu$m. This release not only completes the analogous catalogue previously produced by the Hi-GAL collaboration for $-71^\circ \lesssim \ell \lesssim 67^\circ$, but also meaningfully improves it thanks to a new set of heliocentric distances, 120808 in total. About a third of the 150223 entries are located in the newly added portion of the Galactic plane. A first classification based on detection at 70 $\mu$m as a signature of ongoing star-forming activity distinguishes between protostellar sources (23~per cent of the total) and starless sources, with the latter further classified as gravitationally bound (pre-stellar) or unbound. The integral of the spectral energy distribution, including ancillary photometry from $\lambda=21$ to 1100 $\mu$m, gives the source luminosity and other bolometric quantities, while a modified black body fitted to data for $\lambda \geq 160\, \mu$m yields mass and temperature. All tabulated clump properties are then derived using photometry and heliocentric distance, where possible. Statistics of these quantities are discussed with respect to both source Galactic location and evolutionary stage. No strong differences in the distributions of evolutionary indicators are found between the inner and outer Galaxy. However, masses and densities in the inner Galaxy are on average significantly larger, resulting in a higher number of clumps that are candidates to host massive star formation. Median behaviour of distance-independent parameters tracing source evolutionary status is examined as a function of the Galactocentric radius, showing no clear evidence of correlation with spiral arm positions., Comment: accepted by MNRAS, april 2021

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281. Testing Hadronic Interactions at Ultrahigh Energies with Air Showers Measured by the Pierre Auger Observatory.

Author

Aab A, Abreu P, Aglietta M, Ahn EJ, Al Samarai I, Albuquerque IF, Allekotte I, Allen JD, Allison P, Almela A, Alvarez Castillo J, Alvarez-Muñiz J, Ambrosio M, Anastasi GA, Anchordoqui L, Andrada B, Andringa S, Aramo C, Arqueros F, Arsene N, Asorey H, Assis P, Aublin J, Avila G, Badescu AM, Baus C, Beatty JJ, Becker KH, Bellido JA, Berat C, Bertaina ME, Bertou X, Biermann PL, Billoir P, Biteau J, Blaess SG, Blanco A, Blazek J, Bleve C, Blümer H, Boháčová M, Boncioli D, Bonifazi C, Borodai N, Botti AM, Brack J, Brancus I, Bretz T, Bridgeman A, Briechle FL, Buchholz P, Bueno A, Buitink S, Buscemi M, Caballero-Mora KS, Caccianiga B, Caccianiga L, Cancio A, Canfora F, Caramete L, Caruso R, Castellina A, Cataldi G, Cazon L, Cester R, Chavez AG, Chiavassa A, Chinellato JA, Chirinos Diaz JC, Chudoba J, Clay RW, Colalillo R, Coleman A, Collica L, Coluccia MR, Conceição R, Contreras F, Cooper MJ, Coutu S, Covault CE, Cronin J, Dallier R, D'Amico S, Daniel B, Dasso S, Daumiller K, Dawson BR, de Almeida RM, de Jong SJ, De Mauro G, de Mello Neto JR, De Mitri I, de Oliveira J, de Souza V, Debatin J, Del Peral L, Deligny O, Dhital N, Di Giulio C, Di Matteo A, Díaz Castro ML, Diogo F, Dobrigkeit C, D'Olivo JC, Dorofeev A, Dos Anjos RC, Dova MT, Dundovic A, Ebr J, Engel R, Erdmann M, Erfani M, Escobar CO, Espadanal J, Etchegoyen A, Falcke H, Fang K, Farrar GR, Fauth AC, Fazzini N, Ferguson AP, Fick B, Figueira JM, Filevich A, Filipčič A, Fratu O, Freire MM, Fujii T, Fuster A, Gallo F, García B, Garcia-Pinto D, Gate F, Gemmeke H, Gherghel-Lascu A, Ghia PL, Giaccari U, Giammarchi M, Giller M, Głas D, Glaser C, Glass H, Golup G, Gómez Berisso M, Gómez Vitale PF, González N, Gookin B, Gordon J, Gorgi A, Gorham P, Gouffon P, Griffith N, Grillo AF, Grubb TD, Guarino F, Guedes GP, Hampel MR, Hansen P, Harari D, Harrison TA, Harton JL, Hasankiadeh Q, Haungs A, Hebbeker T, Heck D, Heimann P, Herve AE, Hill GC, Hojvat C, Hollon N, Holt E, Homola P, Hörandel JR, Horvath P, Hrabovský M, Huege T, Hulsman J, Insolia A, Isar PG, Jandt I, Jansen S, Jarne C, Johnsen JA, Josebachuili M, Kääpä A, Kambeitz O, Kampert KH, Kasper P, Katkov I, Keilhauer B, Kemp E, Kieckhafer RM, Klages HO, Kleifges M, Kleinfeller J, Krause R, Krohm N, Kuempel D, Kukec Mezek G, Kunka N, Kuotb Awad A, LaHurd D, Latronico L, Lauscher M, Lautridou P, Lebrun P, Legumina R, Leigui de Oliveira MA, Letessier-Selvon A, Lhenry-Yvon I, Link K, Lopes L, López R, López Casado A, Lucero A, Malacari M, Mallamaci M, Mandat D, Mantsch P, Mariazzi AG, Marin V, Mariş IC, Marsella G, Martello D, Martinez H, Martínez Bravo O, Masías Meza JJ, Mathes HJ, Mathys S, Matthews J, Matthews JA, Matthiae G, Maurizio D, Mayotte E, Mazur PO, Medina C, Medina-Tanco G, Mello VB, Melo D, Menshikov A, Messina S, Micheletti MI, Middendorf L, Minaya IA, Miramonti L, Mitrica B, Molina-Bueno L, Mollerach S, Montanet F, Morello C, Mostafá M, Moura CA, Müller G, Muller MA, Müller S, Naranjo I, Navas S, Necesal P, Nellen L, Nelles A, Neuser J, Nguyen PH, Niculescu-Oglinzanu M, Niechciol M, Niemietz L, Niggemann T, Nitz D, Nosek D, Novotny V, Nožka H, Núñez LA, Ochilo L, Oikonomou F, Olinto A, Pakk Selmi-Dei D, Palatka M, Pallotta J, Papenbreer P, Parente G, Parra A, Paul T, Pech M, Pedreira F, Pękala J, Pelayo R, Peña-Rodriguez J, Pepe IM, Pereira LA, Perrone L, Petermann E, Peters C, Petrera S, Phuntsok J, Piegaia R, Pierog T, Pieroni P, Pimenta M, Pirronello V, Platino M, Plum M, Porowski C, Prado RR, Privitera P, Prouza M, Quel EJ, Querchfeld S, Quinn S, Rautenberg J, Ravel O, Ravignani D, Revenu B, Ridky J, Risse M, Ristori P, Rizi V, Rodrigues de Carvalho W, Rodriguez Rojo J, Rodríguez-Frías MD, Rogozin D, Rosado J, Roth M, Roulet E, Rovero AC, Saffi SJ, Saftoiu A, Salazar H, Saleh A, Salesa Greus F, Salina G, Sanabria Gomez JD, Sánchez F, Sanchez-Lucas P, Santos EM, Santos E, Sarazin F, Sarkar B, Sarmento R, Sarmiento-Cano C, Sato R, Scarso C, Schauer M, Scherini V, Schieler H, Schmidt D, Scholten O, Schoorlemmer H, Schovánek P, Schröder FG, Schulz A, Schulz J, Schumacher J, Sciutto SJ, Segreto A, Settimo M, Shadkam A, Shellard RC, Sigl G, Sima O, Śmiałkowski A, Šmída R, Snow GR, Sommers P, Sonntag S, Sorokin J, Squartini R, Stanca D, Stanič S, Stapleton J, Stasielak J, Strafella F, Stutz A, Suarez F, Suarez Durán M, Sudholz T, Suomijärvi T, Supanitsky AD, Sutherland MS, Swain J, Szadkowski Z, Taborda OA, Tapia A, Tepe A, Theodoro VM, Timmermans C, Todero Peixoto CJ, Tomankova L, Tomé B, Tonachini A, Torralba Elipe G, Torres Machado D, Travnicek P, Trini M, Ulrich R, Unger M, Urban M, Valbuena-Delgado A, Valdés Galicia JF, Valiño I, Valore L, van Aar G, van Bodegom P, van den Berg AM, van Vliet A, Varela E, Vargas Cárdenas B, Varner G, Vázquez JR, Vázquez RA, Veberič D, Verzi V, Vicha J, Videla M, Villaseñor L, Vorobiov S, Wahlberg H, Wainberg O, Walz D, Watson AA, Weber M, Weindl A, Wiencke L, Wilczyński H, Winchen T, Wittkowski D, Wundheiler B, Wykes S, Yang L, Yapici T, Yelos D, Zas E, Zavrtanik D, Zavrtanik M, Zepeda A, Zimmermann B, Ziolkowski M, Zong Z, and Zuccarello F

Abstract

Ultrahigh energy cosmic ray air showers probe particle physics at energies beyond the reach of accelerators. Here we introduce a new method to test hadronic interaction models without relying on the absolute energy calibration, and apply it to events with primary energy 6-16 EeV (E&#95;{CM}=110-170  TeV), whose longitudinal development and lateral distribution were simultaneously measured by the Pierre Auger Observatory. The average hadronic shower is 1.33±0.16 (1.61±0.21) times larger than predicted using the leading LHC-tuned models EPOS-LHC (QGSJetII-04), with a corresponding excess of muons.

Published
2016
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282. Simulation of emission spectra from nonuniform reactive laser-induced plasmas.

Author

Hermann J, Lorusso A, Perrone A, Strafella F, Dutouquet C, and Torralba B

Abstract

We demonstrate that chemical reactions leading to the formation of AlO radicals in plasmas produced by ablation of aluminum or Ti-sapphire with ultraviolet nanosecond laser pulses can be predicted by the model of local thermodynamic equilibrium. Therefore, emission spectra recorded with an echelle spectrometer and a gated detector were compared to the spectral radiance computed for uniform and nonuniform equilibrium plasmas. The calculations are based on analytical solutions of the radiation transfer equation. The simulations show that the plasmas produced in argon background gas are almost uniform, whereas temperature and density gradients are evidenced in air. Furthermore, chemical reactions exclusively occur in the cold plume periphery for ablation in air. The formation of AlO is negligible in argon as the plasma temperature is too large in the time interval of interest up to several microseconds. Finally, the validity of local thermodynamic equilibrium is shown to depend on time, space, and on the elemental composition. The presented conclusions are of interest for material analysis via laser-induced breakdown spectroscopy and for laser materials processing.

Published
2015
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