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1. Virial clouds to explain rotational asymmetry in galactic halos

Author: Qadir, Asghar, Tahir, Noraiz, De Paolis, Francesco, and Nucita, Achille A.
Subjects: Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysics::Galaxy Astrophysics
Abstract: The rotation of the galactic objects has been seen by asymmetric Doppler shift in the CMB data. Molecular hydrogen clouds at virial temperature may contribute to the galactic halo dark matter and they might be the reason for the observed rotational asymmetry in the galactic halos. We present a method to constrain the parameters of these virial clouds given that they are composed of a single fluid. The method is such that it should be possible to extend it to more than one fluid., 15th Marcel Grossmann Meeting Rome
Published: 2022
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2. The upgrade of the Pierre Auger Observatory with the Scintillator Surface Detector

Author: Pierre Auger Collaboration, Cataldi, G., Abreu, Pedro, Aglietta, Marco, Albury, Justin M., Allekotte, Ingomar, Almela, Alejandro, Alvarez-Muniz, Jaime, Alves Batista, Rafael, Anastasi, Gioacchino Alex, Anchordoqui, Luis A., Andrada, Belén, Andringa, Sofia, Aramo, Carla, Araújo Ferreira, Paulo Ricardo, Arteaga Velazquez, Juan Carlos, Asorey, Hernán Gonzalo, Assis, Pedro, Avila, Gualberto, Badescu, Alina Mihaela, Bakalova, Alena, Balaceanu, Alexandru, Barbato, Felicia, Barreira Luz, Ricardo Jorge, Becker, Karl-Heinz, Bellido, Jose A., Berat, Corinne, Bertaina, Mario Edoardo, Bertou, Xavier, Biermann, Peter L., Binet, Virginia, Bismark, Kathrin, Bister, Teresa, Biteau, Jonathan, Blazek, Jiri, Bleve, Carla, Bohacova, Martina, boncioli, denise, Bonifazi, Carla, Bonneau Arbeletche, Luan, Borodai, Nataliia, Botti, Ana Martina, Brack, Jeffrey, Bretz, Thomas, Brichetto Orchera, P. Gabriel, Briechle, Florian Lukas, Buchholz, Peter, Bueno, Antonio, Buitink, Stijn, Buscemi, Mario, Büsken, Max, Caballero-Mora, Karen S., Caccianiga, Lorenzo, Canfora, Fabrizia, Caracas, Ioana, Carceller, Juan Miguel, Caruso, Rossella, Castellina, Antonella, Catalani, Fernando, Cataldi, Gabriella, Cazon, Lorenzo, Cerda, Marcos, Chinellato, Jose Augusto, Chudoba, Jiri, Chytka, Ladislav, Clay, Roger W., Cobos Cerutti, Agustín, Colalillo, Roberta, Coleman, Alan, Coluccia, Maria Rita, Conceição, Rúben, Condorelli, Antonio, Consolati, Giovanni, Contreras, Fernando, Convenga, Fabio, Correia dos Santos, Diego, Covault, Corbin, Dasso, Sergio, Daumiller, Kai, Dawson, Bruce R., Day, Jarryd A., Almeida, Rogerio M. de, Jesús, Joaquín de, Jong, Sijbrand J. de, De Mauro, Giuseppe, Mello Neto, João de, De Mitri, Ivan, Oliveira, Jaime de, Oliveira Franco, Danelise de, Palma, Francesco de, Souza, Vitor de, De Vito, Emanuele, Río, Mariano del, Deligny, Olivier, Deval, Luca, Matteo, Armando di, Dobrigkeit, Carola, D'Olivo, Juan Carlos, Domingues Mendes, Luis Miguel, Anjos, Rita dos, Santos, Diego dos, Dova, Maria Teresa, Ebr, Jan, Engel, Ralph, Epicoco, Italo, Erdmann, Martin, Escobar, Carlos O., Etchegoyen, Alberto, Falcke, Heino, Farmer, John, Farrar, Glennys R., Fauth, Anderson, Fazzini, Norberto, Feldbusch, Fridtjof, Fenu, Francesco, Fick, Brian, Figueira, Juan Manuel, Filipcic, Andrej, Fitoussi, Thomas, Fodran, Tomáš, Freire, Martín Miguel, Fujii, Toshihiro, Fuster, Alan, Galea, Cristina, Galelli, Claudio, García, Beatriz, García Vegas, Adrianna Luz, Gemmeke, Hartmut, Gesualdi, Flavia, Gherghel-Lascu, Alexandru, Ghia, Piera Luisa, GIACCARI, Ugo, Giammarchi, Marco, Glombitza, Jonas, Gobbi, Fabian, Gollan, Fernando, Golup, Geraldina, Gómez Berisso, Mariano, Gómez Vitale, Primo F., Gongora, Juan Pablo, González, Juan Manuel, Gonzalez, Nicolas Martin, Goos, Isabel, Gora, Dariusz, Gorgi, Alessio, Gottowik, Marvin, Grubb, Trent D., Guarino, Fausto, Guedes, Germano, Guido, Eleonora, Hahn, Steffen, Hamal, Petr, Hampel, Matías Rolf, Hansen, Patricia María, Harari, Diego, Harvey, Violet M., Haungs, Andreas, Hebbeker, Thomas, Heck, Dieter, Hill, Gary C., Hojvat, Carlos, Hörandel, Jörg, Horvath, Pavel, Hrabovsky, Miroslav, Huege, Tim, Insolia, Antonio, Isar, Paula Gina, Janecek, Petr, Johnsen, Jeffrey A., Juryšek, Jakub, Kääpä, Alex, Kampert, Karl-Heinz, Karastathis, Nikolaos, Keilhauer, Bianca, Kemp, Julian, Khakurdikar, Abha, Kizakke Covilakam, Varada Varma, Klages, Hans, Kleifges, Matthias, Kleinfeller, Jonny, Köpke, Marcel, Kunka, Norbert, Lago, Bruno L., Lang, Rodrigo Guedes, Langner, Niklas, Leigui de Oliveira, Marcelo Augusto, Lenok, Vladimir, Letessier-Selvon, Antoine, Lhenry-Yvon, Isabelle, Lo Presti, Domenico, LOPES, Luis, López, Rebeca, Lu, Lu, Luce, Quentin, Lundquist, Jon Paul, Machado Payeras, Allan, Mancarella, Giovanni, Mandat, Dusan, Manning, Bradley C., Manshanden, Julien, Mantsch, Paul, Marafico, Sullivan, Mariazzi, Analisa, Maris, Ioana Codrina, Marsella, Giovanni, Martello, Daniele, Martinelli, Sara, Martínez Bravo, Oscar, Mastrodicasa, Massimo, Mathes, Hermann-Josef, Matthews, James, Matthiae, Giorgio, Mayotte, Eric, Mazur, Peter, Medina-Tanco, Gustavo, Melo, Diego, Menshikov, Alexander, Merenda, Kevin-Druis, Michal, Stanislav, Micheletti, Maria Isabel, Miramonti, Lino, Mollerach, Silvia, Montanet, François, Morello, Carlo, Mostafa, Miguel, Müller, Ana L., Muller, Marcio Aparecido, Mulrey, Katharine, Mussa, Roberto, Muzio, Marco Stein, Namasaka, Wilson M., Nasr-Esfahani, Alina, Nellen, Lukas, Niculescu-Oglinzanu, Mihai, Niechciol, Marcus, Nitz, Dave, Nosek, Dalibor, Novotný, Vladimír, Nozka, Libor, Nucita, Achille, Nunez, Luis A., Palatka, Miroslav, Pallotta, Juan, Papenbreer, Philipp, Parente, Gonzalo, Parra, Alejandra, Pawlowsky, Jannis, Pech, Miroslav, Pedreira, Francisco, Pękala, Jan, Pelayo, Rodrigo, Peña-Rodríguez, Jesús, Pereira Martins, Edyvania Emily, Perez Armand, Johnnier, Pérez Bertolli, Carmina, Perlin, Matías, Perrone, Lorenzo, Petrera, Sergio, Pierog, Tanguy, Pimenta, Mário, Pirronello, Valerio, Platino, Manuel, Pont, Bjarni, Pothast, Mart, Privitera, Paolo, Prouza, Michael, Puyleart, Andrew, Querchfeld, Sven, Rautenberg, Julian, Ravignani, Diego, Reininghaus, Maximilian, Ridky, Jan, Riehn, Felix, Risse, Markus, Rizi, Vincenzo, Rodrigues de Carvalho, Washington, Rodriguez Rojo, Jorge Rubén, Roncoroni, Matías J., Rossoni, Simone, Roth, Markus, Roulet, Esteban, Rovero, Adrian, Ruehl, Philip, Saftoiu, Alexandra, Salamida, Francesco, Salazar, Humberto Ibarguen, Salina, Gaetano, Sanabria Gomez, Jose, Sánchez, Federico Andrés, Santos, Edivaldo Moura, Santos, Eva, Sarazin, Fred, Sarmento, Raul, Sarmiento-Cano, Christian, Sato, Ricardo, Savina, Pierpaolo, Schäfer, Christoph M., Scherini, Viviana, Schieler, Harald, Schimassek, Martin, Schimp, Michael, Schlüter, Felix, Schmidt, David, Scholten, Olaf, Schovanek, Petr, Schröder, Frank G., Schröder, Sonja, Schulte, Josina, Sciutto, Sergio, Scornavacche, Marina, Segreto, Alberto, Sehgal, Srijan, Shellard, Ronald C., Sigl, Guenter, Silli, Gaia, Sima, Octavian, Smida, Radomir, Sommers, Paul, Soriano, Jorge F., Souchard, Julien, Squartini, Ruben, Stadelmaier, Maximilian, Stanca, Denis, Stanič, Samo, Stasielak, Jaroslaw, Stassi, Patrick, Streich, Alexander, Suárez-Durán, Mauricio, Sudholz, Tristan, Suomijarvi, Tiina, Supanitsky, A. Daniel, Szadkowski, Zbigniew, Tapia, Alex, Taricco, Carla, Timmermans, Charles, Tkachenko, Olena, Tobiska, Petr, Todero Peixoto, Carlos J., Tomé, Bernardo, Torrès, Zoé, Travaini, Andres, Travnicek, Petr, Trimarelli, Caterina, Tueros, Matias, Ulrich, Ralf, Unger, Michael, Vaclavek, Lukáš, Vacula, Martin, Valdés Galicia, Jose F., Valore, Laura, Varela, Enrique, Vásquez-Ramírez, Adriana, Veberic, Darko, Ventura, Cynthia, Vergara Quispe, Indira D., Verzi, Valerio, Vicha, Jakub, Vink, Jacco, Vorobiov, Serguei, Wahlberg, Hernan, Watanabe, Clara Keiko Oliveira, Watson, Alan, Weber, Marc, Weindl, Andreas, Wiencke, Lawrence, Wilczyński, Henryk, Wirtz, Marcus, Wittkowski, David, Wundheiler, Brian, Yushkov, Alexey, Zapparrata, Orazio, Zas, Enrique, Zavrtanik, Danilo, Zavrtanik, Marko, and Zehrer, Lukas
Subjects: Pierre Auger Observatory, Photomultiplier, business.industry, Physics, Astronomy, Detector, Electrical engineering, Scintillator, Data acquisition, Upgrade, Observatory, Experimental High Energy Physics, ddc:530, Electronics, High Energy Physics, business
Abstract: Since its full commissioning in 2008, the Pierre Auger Observatory has consistently demonstrated its scientific productivity. A major upgrade of the Surface Detector array (SD) improves the capabilities of measuring the different components of extensive air showers. One of the elements of the upgrade consists of new Scintillator Surface Detectors (SSD) placed on top of the Water-Cherenkov stations of the SD. At the Observatory, the integration of the SSD components and their deployment in the array is well advanced. In this paper, the main challenges and characteristics of the construction and installation will be reviewed. Started in 2016, an Engineering Array of twelve upgraded stations has been taking data in the field. In March 2019, a preproduction array of 77 SSDs started data acquisition with an adapted version of non-upgraded electronics. It is collecting events and proving the goodness of SSD design. Since December 2020, the upgraded electronics boards are being deployed in the field together with the photomultiplier tubes, increasing the number of SSD detectors, which are taking data continuosly with good stability. In this paper, the-long term performance of a subset of stations acquiring data for more than two years will be discussed. The data collected so far demonstrate the quality of the new detectors and the physics potential of the upgrade project
Published: 2022

3. Indication of a mass-dependent anisotropy above 10 18.7 eV in the hybrid data of the Pierre Auger Observatory

Author: Pierre Auger Collaboration, Mayotte, Eric, Abreu, Pedro, Aglietta, Marco, Albury, Justin M., Allekotte, Ingomar, Almela, Alejandro, Alvarez-Muniz, Jaime, Alves Batista, Rafael, Anastasi, Gioacchino Alex, Anchordoqui, Luis A., Andrada, Belén, Andringa, Sofia, Aramo, Carla, Araújo Ferreira, Paulo Ricardo, Arteaga Velazquez, Juan Carlos, Asorey, Hernán Gonzalo, Assis, Pedro, Avila, Gualberto, Badescu, Alina Mihaela, Bakalova, Alena, Balaceanu, Alexandru, Barbato, Felicia, Barreira Luz, Ricardo Jorge, Becker, Karl-Heinz, Bellido, Jose A., Berat, Corinne, Bertaina, Mario Edoardo, Bertou, Xavier, Biermann, Peter L., Binet, Virginia, Bismark, Kathrin, Bister, Teresa, Biteau, Jonathan, Blazek, Jiri, Bleve, Carla, Bohacova, Martina, boncioli, denise, Bonifazi, Carla, Bonneau Arbeletche, Luan, Borodai, Nataliia, Botti, Ana Martina, Brack, Jeffrey, Bretz, Thomas, Brichetto Orchera, P. Gabriel, Briechle, Florian Lukas, Buchholz, Peter, Bueno, Antonio, Buitink, Stijn, Buscemi, Mario, Büsken, Max, Caballero-Mora, Karen S., Caccianiga, Lorenzo, Canfora, Fabrizia, Caracas, Ioana, Carceller, Juan Miguel, Caruso, Rossella, Castellina, Antonella, Catalani, Fernando, Cataldi, Gabriella, Cazon, Lorenzo, Cerda, Marcos, Chinellato, Jose Augusto, Chudoba, Jiri, Chytka, Ladislav, Clay, Roger W., Cobos Cerutti, Agustín, Colalillo, Roberta, Coleman, Alan, Coluccia, Maria Rita, Conceição, Rúben, Condorelli, Antonio, Consolati, Giovanni, Contreras, Fernando, Convenga, Fabio, Correia dos Santos, Diego, Covault, Corbin, Dasso, Sergio, Daumiller, Kai, Dawson, Bruce R., Day, Jarryd A., Almeida, Rogerio M. de, Jesús, Joaquín de, Jong, Sijbrand J. de, De Mauro, Giuseppe, Mello Neto, João de, De Mitri, Ivan, Oliveira, Jaime de, Oliveira Franco, Danelise de, Palma, Francesco de, Souza, Vitor de, De Vito, Emanuele, Río, Mariano del, Deligny, Olivier, Deval, Luca, Matteo, Armando di, Dobrigkeit, Carola, D'Olivo, Juan Carlos, Domingues Mendes, Luis Miguel, Anjos, Rita dos, Santos, Diego dos, Dova, Maria Teresa, Ebr, Jan, Engel, Ralph, Epicoco, Italo, Erdmann, Martin, Escobar, Carlos O., Etchegoyen, Alberto, Falcke, Heino, Farmer, John, Farrar, Glennys R., Fauth, Anderson, Fazzini, Norberto, Feldbusch, Fridtjof, Fenu, Francesco, Fick, Brian, Figueira, Juan Manuel, Filipcic, Andrej, Fitoussi, Thomas, Fodran, Tomáš, Freire, Martín Miguel, Fujii, Toshihiro, Fuster, Alan, Galea, Cristina, Galelli, Claudio, García, Beatriz, García Vegas, Adrianna Luz, Gemmeke, Hartmut, Gesualdi, Flavia, Gherghel-Lascu, Alexandru, Ghia, Piera Luisa, GIACCARI, Ugo, Giammarchi, Marco, Glombitza, Jonas, Gobbi, Fabian, Gollan, Fernando, Golup, Geraldina, Gómez Berisso, Mariano, Gómez Vitale, Primo F., Gongora, Juan Pablo, González, Juan Manuel, Gonzalez, Nicolas Martin, Goos, Isabel, Gora, Dariusz, Gorgi, Alessio, Gottowik, Marvin, Grubb, Trent D., Guarino, Fausto, Guedes, Germano, Guido, Eleonora, Hahn, Steffen, Hamal, Petr, Hampel, Matías Rolf, Hansen, Patricia María, Harari, Diego, Harvey, Violet M., Haungs, Andreas, Hebbeker, Thomas, Heck, Dieter, Hill, Gary C., Hojvat, Carlos, Hörandel, Jörg, Horvath, Pavel, Hrabovsky, Miroslav, Huege, Tim, Insolia, Antonio, Isar, Paula Gina, Janecek, Petr, Johnsen, Jeffrey A., Juryšek, Jakub, Kääpä, Alex, Kampert, Karl-Heinz, Karastathis, Nikolaos, Keilhauer, Bianca, Kemp, Julian, Khakurdikar, Abha, Kizakke Covilakam, Varada Varma, Klages, Hans, Kleifges, Matthias, Kleinfeller, Jonny, Köpke, Marcel, Kunka, Norbert, Lago, Bruno L., Lang, Rodrigo Guedes, Langner, Niklas, Leigui de Oliveira, Marcelo Augusto, Lenok, Vladimir, Letessier-Selvon, Antoine, Lhenry-Yvon, Isabelle, Lo Presti, Domenico, LOPES, Luis, López, Rebeca, Lu, Lu, Luce, Quentin, Lundquist, Jon Paul, Machado Payeras, Allan, Mancarella, Giovanni, Mandat, Dusan, Manning, Bradley C., Manshanden, Julien, Mantsch, Paul, Marafico, Sullivan, Mariazzi, Analisa, Maris, Ioana Codrina, Marsella, Giovanni, Martello, Daniele, Martinelli, Sara, Martínez Bravo, Oscar, Mastrodicasa, Massimo, Mathes, Hermann-Josef, Matthews, James, Matthiae, Giorgio, Mazur, Peter, Medina-Tanco, Gustavo, Melo, Diego, Menshikov, Alexander, Merenda, Kevin-Druis, Michal, Stanislav, Micheletti, Maria Isabel, Miramonti, Lino, Mollerach, Silvia, Montanet, François, Morello, Carlo, Mostafa, Miguel, Müller, Ana L., Muller, Marcio Aparecido, Mulrey, Katharine, Mussa, Roberto, Muzio, Marco Stein, Namasaka, Wilson M., Nasr-Esfahani, Alina, Nellen, Lukas, Niculescu-Oglinzanu, Mihai, Niechciol, Marcus, Nitz, Dave, Nosek, Dalibor, Novotný, Vladimír, Nozka, Libor, Nucita, Achille, Nunez, Luis A., Palatka, Miroslav, Pallotta, Juan, Papenbreer, Philipp, Parente, Gonzalo, Parra, Alejandra, Pawlowsky, Jannis, Pech, Miroslav, Pedreira, Francisco, Pękala, Jan, Pelayo, Rodrigo, Peña-Rodríguez, Jesús, Pereira Martins, Edyvania Emily, Perez Armand, Johnnier, Pérez Bertolli, Carmina, Perlin, Matías, Perrone, Lorenzo, Petrera, Sergio, Pierog, Tanguy, Pimenta, Mário, Pirronello, Valerio, Platino, Manuel, Pont, Bjarni, Pothast, Mart, Privitera, Paolo, Prouza, Michael, Puyleart, Andrew, Querchfeld, Sven, Rautenberg, Julian, Ravignani, Diego, Reininghaus, Maximilian, Ridky, Jan, Riehn, Felix, Risse, Markus, Rizi, Vincenzo, Rodrigues de Carvalho, Washington, Rodriguez Rojo, Jorge Rubén, Roncoroni, Matías J., Rossoni, Simone, Roth, Markus, Roulet, Esteban, Rovero, Adrian, Ruehl, Philip, Saftoiu, Alexandra, Salamida, Francesco, Salazar, Humberto Ibarguen, Salina, Gaetano, Sanabria Gomez, Jose, Sánchez, Federico Andrés, Santos, Edivaldo Moura, Santos, Eva, Sarazin, Fred, Sarmento, Raul, Sarmiento-Cano, Christian, Sato, Ricardo, Savina, Pierpaolo, Schäfer, Christoph M., Scherini, Viviana, Schieler, Harald, Schimassek, Martin, Schimp, Michael, Schlüter, Felix, Schmidt, David, Scholten, Olaf, Schovanek, Petr, Schröder, Frank G., Schröder, Sonja, Schulte, Josina, Sciutto, Sergio, Scornavacche, Marina, Segreto, Alberto, Sehgal, Srijan, Shellard, Ronald C., Sigl, Guenter, Silli, Gaia, Sima, Octavian, Smida, Radomir, Sommers, Paul, Soriano, Jorge F., Souchard, Julien, Squartini, Ruben, Stadelmaier, Maximilian, Stanca, Denis, Stanič, Samo, Stasielak, Jaroslaw, Stassi, Patrick, Streich, Alexander, Suárez-Durán, Mauricio, Sudholz, Tristan, Suomijarvi, Tiina, Supanitsky, A. Daniel, Szadkowski, Zbigniew, Tapia, Alex, Taricco, Carla, Timmermans, Charles, Tkachenko, Olena, Tobiska, Petr, Todero Peixoto, Carlos J., Tomé, Bernardo, Torrès, Zoé, Travaini, Andres, Travnicek, Petr, Trimarelli, Caterina, Tueros, Matias, Ulrich, Ralf, Unger, Michael, Vaclavek, Lukáš, Vacula, Martin, Valdés Galicia, Jose F., Valore, Laura, Varela, Enrique, Vásquez-Ramírez, Adriana, Veberic, Darko, Ventura, Cynthia, Vergara Quispe, Indira D., Verzi, Valerio, Vicha, Jakub, Vink, Jacco, Vorobiov, Serguei, Wahlberg, Hernan, Watanabe, Clara Keiko Oliveira, Watson, Alan, Weber, Marc, Weindl, Andreas, Wiencke, Lawrence, Wilczyński, Henryk, Wirtz, Marcus, Wittkowski, David, Wundheiler, Brian, Yushkov, Alexey, Zapparrata, Orazio, Zas, Enrique, Zavrtanik, Danilo, Zavrtanik, Marko, and Zehrer, Lukas
Subjects: Physics, Pierre Auger Observatory, Astronomy, Astrophysics, Galactic plane, Mass composition, Threshold energy, Distribution (mathematics), Experimental High Energy Physics, Sensitivity (control systems), High Energy Physics, ddc:620, Anisotropy, Hybrid data, Engineering & allied operations
Abstract: We test the hypothesis of an anisotropy laying along the galactic plane which depends on the mass of primary cosmic-rays. The sensitivity to primary mass is provided by the depth of shower maximum, $X_\text{max}$, from hybrid events measured at the Pierre Auger Observatory. The 14 years of available data are split into on- and off-plane regions using the galactic latitude of each event to form two distributions in $X_\text{max}$, which are compared using the Anderson-Darling 2-samples test. A scan over a subset of the data is used to select an optimal threshold energy of $10^{18.7}$ eV and a galactic latitude splitting at $|b| = 30^\circ$, which are then set as a prescription for the remaining data. With these thresholds, the distribution of $X_\text{max}$ from the on-plane region is found to have a $9.1 \pm 1.6^{+2.1}_{-2.2}$ g/cm$^{2}$ shallower mean and a $5.9\pm2.1^{+3.5}_{-2.5}$ g/cm$^{2}$ narrower width than that of the off-plane region. These differences are as such to indicate that the mean mass of primary particles arriving from the on-plane region is greater than that of those coming from the off-plane region. Monte-Carlo studies yield a $4.4\,\sigma$ post-penalization statistical significance for the independent data. Including the scanned data results in a $4.9^{+1.4}_{-1.5}\,\sigma$ post-penalization statistical significance, where the uncertainties are of systematic origin. Accounting for systematic uncertainties leads to an indication for anisotropy in mass composition above $10^{18.7}$ eV at a confidence level of $3.3\,\sigma$. The anisotropy is observed independently at each of the four fluorescence telescope sites. Interpretations of possible causes of the observed effect are discussed.
Published: 2022
Full Text: View/download PDF

4. A tau scenario application to a search for upward-going showers with the Fluorescence Detector of the Pierre Auger Observatory

Author: Pierre Auger Collaboration, Caracas, Ioana Alexandra, Abreu, Pedro, Aglietta, Marco, Albury, Justin M., Allekotte, Ingomar, Almela, Alejandro, Alvarez-Muniz, Jaime, Alves Batista, Rafael, Anastasi, Gioacchino Alex, Anchordoqui, Luis A., Andrada, Belén, Andringa, Sofia, Aramo, Carla, Araújo Ferreira, Paulo Ricardo, Arteaga Velazquez, Juan Carlos, Asorey, Hernán Gonzalo, Assis, Pedro, Avila, Gualberto, Badescu, Alina Mihaela, Bakalova, Alena, Balaceanu, Alexandru, Barbato, Felicia, Barreira Luz, Ricardo Jorge, Becker, Karl-Heinz, Bellido, Jose A., Berat, Corinne, Bertaina, Mario Edoardo, Bertou, Xavier, Biermann, Peter L., Binet, Virginia, Bismark, Kathrin, Bister, Teresa, Biteau, Jonathan, Blazek, Jiri, Bleve, Carla, Bohacova, Martina, boncioli, denise, Bonifazi, Carla, Bonneau Arbeletche, Luan, Borodai, Nataliia, Botti, Ana Martina, Brack, Jeffrey, Bretz, Thomas, Brichetto Orchera, P. Gabriel, Briechle, Florian Lukas, Buchholz, Peter, Bueno, Antonio, Buitink, Stijn, Buscemi, Mario, Büsken, Max, Caballero-Mora, Karen S., Caccianiga, Lorenzo, Canfora, Fabrizia, Caracas, Ioana, Carceller, Juan Miguel, Caruso, Rossella, Castellina, Antonella, Catalani, Fernando, Cataldi, Gabriella, Cazon, Lorenzo, Cerda, Marcos, Chinellato, Jose Augusto, Chudoba, Jiri, Chytka, Ladislav, Clay, Roger W., Cobos Cerutti, Agustín, Colalillo, Roberta, Coleman, Alan, Coluccia, Maria Rita, Conceição, Rúben, Condorelli, Antonio, Consolati, Giovanni, Contreras, Fernando, Convenga, Fabio, Correia dos Santos, Diego, Covault, Corbin, Dasso, Sergio, Daumiller, Kai, Dawson, Bruce R., Day, Jarryd A., Almeida, Rogerio M. de, Jesús, Joaquín de, Jong, Sijbrand J. de, De Mauro, Giuseppe, Mello Neto, João de, De Mitri, Ivan, Oliveira, Jaime de, Oliveira Franco, Danelise de, Palma, Francesco de, Souza, Vitor de, De Vito, Emanuele, Río, Mariano del, Deligny, Olivier, Deval, Luca, Matteo, Armando di, Dobrigkeit, Carola, D'Olivo, Juan Carlos, Domingues Mendes, Luis Miguel, Anjos, Rita dos, Santos, Diego dos, Dova, Maria Teresa, Ebr, Jan, Engel, Ralph, Epicoco, Italo, Erdmann, Martin, Escobar, Carlos O., Etchegoyen, Alberto, Falcke, Heino, Farmer, John, Farrar, Glennys R., Fauth, Anderson, Fazzini, Norberto, Feldbusch, Fridtjof, Fenu, Francesco, Fick, Brian, Figueira, Juan Manuel, Filipcic, Andrej, Fitoussi, Thomas, Fodran, Tomáš, Freire, Martín Miguel, Fujii, Toshihiro, Fuster, Alan, Galea, Cristina, Galelli, Claudio, García, Beatriz, García Vegas, Adrianna Luz, Gemmeke, Hartmut, Gesualdi, Flavia, Gherghel-Lascu, Alexandru, Ghia, Piera Luisa, GIACCARI, Ugo, Giammarchi, Marco, Glombitza, Jonas, Gobbi, Fabian, Gollan, Fernando, Golup, Geraldina, Gómez Berisso, Mariano, Gómez Vitale, Primo F., Gongora, Juan Pablo, González, Juan Manuel, Gonzalez, Nicolas Martin, Goos, Isabel, Gora, Dariusz, Gorgi, Alessio, Gottowik, Marvin, Grubb, Trent D., Guarino, Fausto, Guedes, Germano, Guido, Eleonora, Hahn, Steffen, Hamal, Petr, Hampel, Matías Rolf, Hansen, Patricia María, Harari, Diego, Harvey, Violet M., Haungs, Andreas, Hebbeker, Thomas, Heck, Dieter, Hill, Gary C., Hojvat, Carlos, Hörandel, Jörg, Horvath, Pavel, Hrabovsky, Miroslav, Huege, Tim, Insolia, Antonio, Isar, Paula Gina, Janecek, Petr, Johnsen, Jeffrey A., Juryšek, Jakub, Kääpä, Alex, Kampert, Karl-Heinz, Karastathis, Nikolaos, Keilhauer, Bianca, Kemp, Julian, Khakurdikar, Abha, Kizakke Covilakam, Varada Varma, Klages, Hans, Kleifges, Matthias, Kleinfeller, Jonny, Köpke, Marcel, Kunka, Norbert, Lago, Bruno L., Lang, Rodrigo Guedes, Langner, Niklas, Leigui de Oliveira, Marcelo Augusto, Lenok, Vladimir, Letessier-Selvon, Antoine, Lhenry-Yvon, Isabelle, Lo Presti, Domenico, LOPES, Luis, López, Rebeca, Lu, Lu, Luce, Quentin, Lundquist, Jon Paul, Machado Payeras, Allan, Mancarella, Giovanni, Mandat, Dusan, Manning, Bradley C., Manshanden, Julien, Mantsch, Paul, Marafico, Sullivan, Mariazzi, Analisa, Maris, Ioana Codrina, Marsella, Giovanni, Martello, Daniele, Martinelli, Sara, Martínez Bravo, Oscar, Mastrodicasa, Massimo, Mathes, Hermann-Josef, Matthews, James, Matthiae, Giorgio, Mayotte, Eric, Mazur, Peter, Medina-Tanco, Gustavo, Melo, Diego, Menshikov, Alexander, Merenda, Kevin-Druis, Michal, Stanislav, Micheletti, Maria Isabel, Miramonti, Lino, Mollerach, Silvia, Montanet, François, Morello, Carlo, Mostafa, Miguel, Müller, Ana L., Muller, Marcio Aparecido, Mulrey, Katharine, Mussa, Roberto, Muzio, Marco Stein, Namasaka, Wilson M., Nasr-Esfahani, Alina, Nellen, Lukas, Niculescu-Oglinzanu, Mihai, Niechciol, Marcus, Nitz, Dave, Nosek, Dalibor, Novotný, Vladimír, Nozka, Libor, Nucita, Achille, Nunez, Luis A., Palatka, Miroslav, Pallotta, Juan, Papenbreer, Philipp, Parente, Gonzalo, Parra, Alejandra, Pawlowsky, Jannis, Pech, Miroslav, Pedreira, Francisco, Pękala, Jan, Pelayo, Rodrigo, Peña-Rodríguez, Jesús, Pereira Martins, Edyvania Emily, Perez Armand, Johnnier, Pérez Bertolli, Carmina, Perlin, Matías, Perrone, Lorenzo, Petrera, Sergio, Pierog, Tanguy, Pimenta, Mário, Pirronello, Valerio, Platino, Manuel, Pont, Bjarni, Pothast, Mart, Privitera, Paolo, Prouza, Michael, Puyleart, Andrew, Querchfeld, Sven, Rautenberg, Julian, Ravignani, Diego, Reininghaus, Maximilian, Ridky, Jan, Riehn, Felix, Risse, Markus, Rizi, Vincenzo, Rodrigues de Carvalho, Washington, Rodriguez Rojo, Jorge Rubén, Roncoroni, Matías J., Rossoni, Simone, Roth, Markus, Roulet, Esteban, Rovero, Adrian, Ruehl, Philip, Saftoiu, Alexandra, Salamida, Francesco, Salazar, Humberto Ibarguen, Salina, Gaetano, Sanabria Gomez, Jose, Sánchez, Federico Andrés, Santos, Edivaldo Moura, Santos, Eva, Sarazin, Fred, Sarmento, Raul, Sarmiento-Cano, Christian, Sato, Ricardo, Savina, Pierpaolo, Schäfer, Christoph M., Scherini, Viviana, Schieler, Harald, Schimassek, Martin, Schimp, Michael, Schlüter, Felix, Schmidt, David, Scholten, Olaf, Schovanek, Petr, Schröder, Frank G., Schröder, Sonja, Schulte, Josina, Sciutto, Sergio, Scornavacche, Marina, Segreto, Alberto, Sehgal, Srijan, Shellard, Ronald C., Sigl, Guenter, Silli, Gaia, Sima, Octavian, Smida, Radomir, Sommers, Paul, Soriano, Jorge F., Souchard, Julien, Squartini, Ruben, Stadelmaier, Maximilian, Stanca, Denis, Stanič, Samo, Stasielak, Jaroslaw, Stassi, Patrick, Streich, Alexander, Suárez-Durán, Mauricio, Sudholz, Tristan, Suomijarvi, Tiina, Supanitsky, A. Daniel, Szadkowski, Zbigniew, Tapia, Alex, Taricco, Carla, Timmermans, Charles, Tkachenko, Olena, Tobiska, Petr, Todero Peixoto, Carlos J., Tomé, Bernardo, Torrès, Zoé, Travaini, Andres, Travnicek, Petr, Trimarelli, Caterina, Tueros, Matias, Ulrich, Ralf, Unger, Michael, Vaclavek, Lukáš, Vacula, Martin, Valdés Galicia, Jose F., Valore, Laura, Varela, Enrique, Vásquez-Ramírez, Adriana, Veberic, Darko, Ventura, Cynthia, Vergara Quispe, Indira D., Verzi, Valerio, Vicha, Jakub, Vink, Jacco, Vorobiov, Serguei, Wahlberg, Hernan, Watanabe, Clara Keiko Oliveira, Watson, Alan, Weber, Marc, Weindl, Andreas, Wiencke, Lawrence, Wilczyński, Henryk, Wirtz, Marcus, Wittkowski, David, Wundheiler, Brian, Yushkov, Alexey, Zapparrata, Orazio, Zas, Enrique, Zavrtanik, Danilo, Zavrtanik, Marko, and Zehrer, Lukas
Subjects: Pierre Auger Observatory, Physics, Astronomy, Astrophysics::High Energy Astrophysical Phenomena, Detector, Astrophysics::Instrumentation and Methods for Astrophysics, Flux, Astrophysics, Spectral line, Path length, Experimental High Energy Physics, High Energy Physics::Experiment, High Energy Physics, ddc:620, Engineering & allied operations, Energy (signal processing), Intensity (heat transfer), Zenith
Abstract: Recent observations of two coherent radio pulses with the ANITA detector can be interpreted as steeply upward-going cosmic-ray showers with energies of a few tenths of an EeV and remain unexplained. The Pierre Auger Observatory has a large exposure to such upward propagating shower-like events, and has used 14 years of its Fluorescence Detector (FD) data to perform a generic search for such events with elevation angles greater than 20$^\circ$ from the horizon. Here this search is recast to constrain models generating high energy $\tau$-leptons. For maximal flexibility, only the propagation, decay, and interactions of $\tau$-leptons are treated in this analysis, meaning that the results are independent of the $\tau$-production scenario. This treatment allows for the application of these results to the wide range of models producing $\tau$-leptons that have been proposed to describe the "anomalous" ANITA events. The goal of this study is accomplished by generating $\tau$-leptons within the Earth and its atmosphere with an intensity dependent on the media density. The zenith angle, location and calorimetric energy of any resulting $\tau$-induced air showers are then used to calculate the exposure of the FD of the Pierre Auger Observatory to $\tau$ primaries. Differential limits as low as $10^{-9}$GeV s$^{-1}$cm$^{-2}$sr$^{-1}$ to the flux of $\tau$-leptons produced with less than a 50 km path length below the Earth's surface are reported for several zenith angle ranges and primary energy spectra. Full exposure and sensitivity information is provided, facilitating the application of these results to different $\tau$-lepton production models.
Published: 2022
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5. Searches for Ultra-High-Energy Photons at the Pierre Auger Observatory

Author: Abreu, Pedro, Aglietta, Marco, Allekotte, Ingomar, Almeida Cheminant, Kevin, Almela, Alejandro, Alvarez-Muñiz, Jaime, Ammerman Yebra, Juan, Anastasi, Gioacchino Alex, Anchordoqui, Luis, Andrada, Belén, Andringa, Sofia, Aramo, Carla, Araújo Ferreira, Paulo Ricardo, Arnone, Enrico, Arteaga Velázquez, Juan Carlos, Asorey, Hernán Gonzalo, Assis, Pedro, Avila, Gualberto, Avocone, Emanuele, Badescu, Alina Mihaela, Bakalova, Alena, Balaceanu, Alexandru, Barbato, Felicia, Bellido, Jose A., Berat, Corinne, Bertaina, Mario Edoardo, Bhatta, Gopal, Biermann, Peter, Binet, Virginia, Bismark, Kathrin, Bister, Teresa Karolin, Biteau, Jonathan, Blazek, Jiri, Bleve, Carla, Blümer, Johannes, Boháčová, Martina, Boncioli, Denise, Bonifazi, Carla, Bonneau Arbeletche, Luan, Borodai, Nataliia, Brack, Jeffrey, Bretz, Thomas, Brichetto Orchera, P. Gabriel, Briechle, Florian Lukas, Buchholz, Peter, Bueno, Antonio, Buitink, Stijn, Buscemi, Mario, Büsken, Max, Bwembya, Anthony, Caballero-Mora, Karen S., Caccianiga, Lorenzo, Caracas, Ioana, Caruso, Rossella, Castellina, Antonella, Catalani, Fernando, Cataldi, Gabriella, Cazon, Lorenzo, Cerda, Marcos, Chinellato, Jose Augusto, Chudoba, Jiri, Chytka, Ladislav, Clay, Roger W., Cobos Cerutti, Agustín, Colalillo, Roberta, Coleman, Alan, Coluccia, Maria Rita, Conceição, Ruben, Condorelli, Antonio, Consolati, Giovanni, Contreras, Fernando, Convenga, Fabio, Correia dos Santos, Diego, Covault, Corbin, Cristinziani, Markus, Dasso, Sergio, Daumiller, Kai, Dawson, Bruce R., de Almeida, Rogerio M., de Jesús, Joaquín, de Jong, Sijbrand J., de Mello Neto, Joao, De Mitri, Ivan, de Oliveira, Jaime, de Oliveira Franco, Danelise, de Palma, Francesco, de Souza, Vitor, De Vito, Emanuele, Del Popolo, Antonino, Deligny, Olivier, Deval, Luca, di Matteo, Armando, Dobre, Madalina, Dobrigkeit, Carola, D'Olivo, Juan Carlos, Domingues Mendes, Luis Miguel, dos Anjos, Rita, Ebr, Jan, Eman, Mohamed, Engel, Ralph, Epicoco, Italo, Erdmann, Martin, Etchegoyen, Alberto, Falcke, Heino, Farmer, John, Farrar, Glennys, Fauth, Anderson, Fazzini, Norberto, Feldbusch, Fridtjof, Fenu, Francesco, Fick, Brian, Figueira, Juan Manuel, Filipčič, Andrej, Fitoussi, Thomas, Fodran, Tomas, Fujii, Toshihiro, Fuster, Alan, Galea, Cristina, Galelli, Claudio, García, Beatriz, Gemmeke, Hartmut, Gesualdi, Flavia, Gherghel-Lascu, Alexandru, Ghia, Piera Luisa, Giaccari, Ugo, Giammarchi, Marco, Glombitza, Jonas, Gobbi, Fabian, Gollan, Fernando, Golup, Geraldina, Gómez Berisso, Mariano, Gómez Vitale, Primo F., Gongora, Juan Pablo, González, Juan Manuel, González, Nicolás, Goos, Isabel, Góra, Dariusz, Gorgi, Alessio, Gottowik, Marvin, Grubb, Trent D., Guarino, Fausto, Guedes, Germano, Guido, Eleonora, Hahn, Steffen, Hamal, Petr, Hampel, Matías Rolf, Hansen, Patricia, Harari, Diego, Harvey, Violet M., Haungs, Andreas, Hebbeker, Thomas, Heck, Dieter, Hojvat, Carlos, Hörandel, Jörg, Horvath, Pavel, Hrabovský, Miroslav, Huege, Tim, Insolia, Antonio, Isar, Paula Gina, Janecek, Petr, Johnsen, Jeffrey A., Jurysek, Jakub, Kääpä, Alex, Kampert, Karl-Heinz, Keilhauer, Bianca, Khakurdikar, Abha, Kizakke Covilakam, Varada Varma, Klages, Hans, Kleifges, Matthias, Kleinfeller, Jonny, Knapp, Felix, Kunka, Norbert, Lago, Bruno L., Langner, Niklas Uwe, Leigui de Oliveira, Marcelo Augusto, Lenok, Vladimir, Letessier-Selvon, Antoine, Lhenry-Yvon, Isabelle, Lo Presti, Domenico, Lopes, Luis, López, Rebeca, Lu, Lu, Luce, Quentin, Lundquist, Jon Paul, Machado Payeras, Allan, Mancarella, Giovanni, Mandat, Dusan, Manning, Bradley C., Manshanden, Julien, Mantsch, Paul, Marafico, Sullivan, Mariani, Federico Maria, Mariazzi, Analisa, Mariş, Ioana, Marsella, Giovanni, Martello, Daniele, Martinelli, Sara, Martínez Bravo, Oscar, Martins, Miguel A., Mastrodicasa, Massimo, Mathes, Hermann-Josef, Matthews, James, Matthiae, Giorgio, Mayotte, Eric, Mayotte, Sonja, Mazur, Peter, Medina-Tanco, Gustavo, Melo, Diego, Menshikov, Alexander, Michal, Stanislav, Micheletti, Maria Isabel, Miramonti, Lino, Mollerach, Silvia, Montanet, François, Morejon, Leonel, Morello, Carlo, Müller, Ana L., Mulrey, Katharine, Mussa, Roberto, Muzio, Marco, Namasaka, Wilson M., Nasr-Esfahani, Alina, Nellen, Lukas, Nicora, Gabriela, Niculescu-Oglinzanu, Mihai, Niechciol, Marcus, Nitz, Dave, Norwood, Ian, Nosek, Dalibor, Novotny, Vladimir, Nožka, Libor, Nucita, Achille, Núñez, Luis, Oliveira, Cainã, Palatka, Miroslav, Pallotta, Juan, Parente, Gonzalo, Parra, Alejandra, Pawlowsky, Jannis, Pech, Miroslav, Pękala, Jan, Pelayo, Rodrigo, Pereira Martins, Edyvania Emily, Perez Armand, Johnnier, Pérez Bertolli, Carmina, Perrone, Lorenzo, Petrera, Sergio, Petrucci, Camilla, Pierog, Tanguy, Pimenta, Mário, Platino, Manuel, Pont, Bjarni, Pothast, Mart, Pourmohammad Shavar, Mohsen, Privitera, Paolo, Prouza, Michael, Puyleart, Andrew, Querchfeld, Sven, Rautenberg, Julian, Ravignani, Diego, Reininghaus, Maximilian, Ridky, Jan, Riehn, Felix, Risse, Markus, Rizi, Vincenzo, Rodrigues de Carvalho, Washington, Rodriguez Rojo, Jorge Rubén, Roncoroni, Matías J., Rossoni, Simone, Roth, Markus, Roulet, Esteban, Rovero, Adrian, Ruehl, Philip, Saftoiu, Alexandra, Saharan, Mohit, Salamida, Francesco, Salazar, Humberto, Salina, Gaetano, Sanabria Gomez, Jose, Sánchez, Federico, Moura Santos, Edivaldo, Santos, Eva, Sarazin, Fred, Sarmento, Raul, Sato, Ricardo, Savina, Pierpaolo, Schäfer, Christoph M., Scherini, Viviana, Schieler, Harald, Schimassek, Martin, Schimp, Michael, Schlüter, Felix, Schmidt, David, Scholten, Olaf, Schoorlemmer, Harm, Schovánek, Petr, Schröder, Frank G., Schulte, Josina, Schulz, Tobias, Sciutto, Sergio, Scornavacche, Marina, Segreto, Alberto, Sehgal, Srijan, Shivashankara, Shima Ujjani, Sigl, Guenter, Silli, Gaia, Sima, Octavian, Smau, Raluca, Šmída, Radomir, Sommers, Paul, Soriano, Jorge F., Squartini, Ruben, Stadelmaier, Maximilian, Stanca, Denis, Stanič, Samo, Stasielak, Jaroslaw, Stassi, Patrick, Straub, Maximilian Philipp, Streich, Alexander, Suárez-Durán, Mauricio, Sudholz, Tristan, Suomijärvi, Tiina, Supanitsky, A. Daniel, Szadkowski, Zbigniew, Tapia, Alex, Taricco, Carla, Timmermans, Charles, Tkachenko, Olena, Tobiska, Petr, Todero Peixoto, Carlos J., Tomé, Bernardo, Torrès, Zoé, Travaini, Andres, Travnicek, Petr, Trimarelli, Caterina, Tueros, Matias, Ulrich, Ralf, Unger, Michael, Vaclavek, Lukáš, Vacula, Martin, Valdés Galicia, Jose F., Valore, Laura, Varela, Enrique, Vásquez-Ramírez, Adriana, Veberič, Darko, Ventura, Cynthia, Vergara Quispe, Indira D., Verzi, Valerio, Vicha, Jakub, Vink, Jacco, Vorobiov, Serguei, Watanabe, Clara, Watson, Alan, Weindl, Andreas, Wiencke, Lawrence, Wilczyński, Henryk, Wittkowski, David, Wundheiler, Brian, Yushkov, Alexey, Zapparrata, Orazio, Zas, Enrique, Zavrtanik, Danilo, Zavrtanik, Marko, Zehrer, Lukas, The Pierre Auger Collaboration, Abreu, P, Aglietta, M, Allekotte, I, Cheminant, Ka, Almela, A, Alvarez-Muniz, J, Yebra, Ja, Anastasi, Ga, Anchordoqui, L, Andrada, B, Andringa, S, Aramo, C, Ferreira, Pra, Arnone, E, Velazquez, Jca, Asorey, H, Assis, P, Avila, G, Avocone, E, Badescu, Am, Bakalova, A, Balaceanu, A, Barbato, F, Bellido, Ja, Berat, C, Bertaina, Me, Bhatta, G, Biermann, Pl, Binet, V, Bismark, K, Bister, T, Biteau, J, Blazek, J, Bleve, C, Blumer, J, Bohacova, M, Boncioli, D, Bonifazi, C, Arbeletche, Lb, Borodai, N, Brack, J, Bretz, T, Orchera, Pgb, Briechle, Fl, Buchholz, P, Bueno, A, Buitink, S, Buscemi, M, Busken, M, Bwembya, A, Caballero-Mora, K, Caccianiga, L, Caracas, I, Caruso, R, Castellina, A, Catalani, F, Cataldi, G, Cazon, L, Cerda, M, Chinellato, Ja, Chudoba, J, Chytka, L, Clay, Rw, Cerutti, Acc, Colalillo, R, Coleman, A, Coluccia, Mr, Conceicao, R, Condorelli, A, Consolati, G, Contreras, F, Convenga, F, dos Santos, Dc, Covault, Ce, Cristinziani, M, Dasso, S, Daumiller, K, Dawson, Br, de Almeida, Rm, de Jesus, J, de Jong, Sj, Neto, Jrtd, De Mitri, I, de Oliveira, J, Franco, Dd, de Palma, F, de Souza, V, De Vito, E, Del Popolo, A, Deligny, O, Deval, L, di Matteo, A, Dobre, M, Dobrigkeit, C, D'Olivo, Jc, Mendes, Lmd, dos Anjos, Rc, Ebr, J, Eman, M, Engel, R, Epicoco, I, Erdmann, M, Etchegoyen, A, Falcke, H, Farmer, J, Farrar, G, Fauth, Ac, Fazzini, N, Feldbusch, F, Fenu, F, Fick, B, Figueira, Jm, Filipcic, A, Fitoussi, T, Fodran, T, Fujii, T, Fuster, A, Galea, C, Galelli, C, Garcia, B, Gemmeke, H, Gesualdi, F, Gherghel-Lascu, A, Ghia, Pl, Giaccari, U, Giammarchi, M, Glombitza, J, Gobbi, F, Gollan, F, Golup, G, Berisso, Mg, Vitale, Pfg, Gongora, Jp, Gonzalez, Jm, Gonzalez, N, Goos, I, Gora, D, Gorgi, A, Gottowik, M, Grubb, Td, Guarino, F, Guedes, Gp, Guido, E, Hahn, S, Hamal, P, Hampel, Mr, Hansen, P, Harari, D, Harvey, Vm, Haungs, A, Hebbeker, T, Heck, D, Hojvatd, C, Horandel, Jr, Horvath, P, Hrabovsky, M, Huege, T, Insolia, A, Isar, Pg, Janecek, P, Johnsen, Ja, Jurysek, J, Kaapa, A, Kampert, Kh, Keilhauer, B, Khakurdikar, A, Covilakam, Vvk, Klages, Ho, Kleifges, M, Kleinfeller, J, Knapp, F, Kunka, N, Lago, Bl, Langner, N, de Oliveira, Mal, Lenok, V, Letessier-Selvon, A, Lhenry-Yvon, I, Lo Presti, D, Lopes, L, Lopez, R, Lu, L, Luce, Q, Lundquist, Jp, Payeras, Am, Mancarella, G, Mandat, D, Manning, Bc, Manshan-den, J, Mantschd, P, Marafico, S, Mariani, Fm, Mariazzi, Ag, Maris, Ic, Marsella, G, Martello, D, Martinelli, S, Bravo, Om, Martins, Ma, Mastrodicasa, M, Mathes, Hj, Matthews, J, Matthiae, G, May-otte, E, Mayotte, S, Mazurd, Po, Medina-Tanco, G, Melo, D, Menshikov, A, Michal, S, Micheletti, Mi, Miramonti, L, Mollerach, S, Montanet, F, Morejon, L, Morello, C, Muller, Al, Mulrey, K, Mussa, R, Muzio, M, Namasaka, Wm, Nasr-Esfahani, A, Nellen, L, Nicora, G, Niculescu-Oglinzanu, M, Niechciol, M, Nitz, D, Norwood, I, Nosek, D, Novotny, V, Nozka, L, Nucita, A, Nunez, La, Oliveira, C, Palatka, M, Pallotta, J, Parente, G, Parra, A, Pawlowsky, J, Pech, M, Pelayo, R, Martins, Eep, Armand, Jp, Bertolli, Cp, Perrone, L, Petrera, S, Petrucci, C, Pierog, T, Pimenta, M, Platino, M, Pont, B, Pothast, M, Shavar, Mp, Privitera, P, Prouza, M, Puyleart, A, Querchfeld, S, Rautenberg, J, Ravignani, D, Reininghaus, M, Ridky, J, Riehn, F, Risse, M, Rizi, V, de Carvalho, Wr, Rojo, Jr, Roncoroni, Mj, Rossoni, S, Roth, M, Roulet, E, Rovero, Ac, Ruehl, P, Saftoiu, A, Saharan, M, Salamida, F, Salazar, H, Salina, G, Gomez, Jd, Sanchez, F, Santos, Em, Santos, E, Sarazin, F, Sarmento, R, Sato, R, Sav-ina, P, Schafer, Cm, Scherini, V, Schieler, H, Schimassek, M, Schimp, M, Schluter, F, Schmidt, D, Scholten, O, Schoorlemmer, H, Schovanek, P, Schroder, Fg, Schulte, J, Schulz, T, Sciutto, Sj, Scornavacche, M, Segreto, A, Sehgal, S, Shivashankara, Su, Sigl, G, Silli, G, Sima, O, Smau, R, Smida, R, Sommersh, P, Soriano, Jf, Squartini, R, Stadelmaier, M, Stanca, D, Stanic, S, Stasielak, J, Stassi, P, Straub, M, Streich, A, Suarez-Duran, M, Sudholz, T, Suomijarvi, T, Supanitsky, Ad, Szadkowski, Z, Tapia, A, Taricco, C, Timmermans, C, Tkachenko, O, Tobiska, P, Peixoto, Cjt, Tome, B, Torres, Z, Travaini, A, Travnicek, P, Trimarelli, C, Tueros, M, Ulrich, R, Unger, M, Vaclavek, L, Vacula, M, Galicia, Jfv, Valore, L, Varela, E, Vasquez-Ramirez, A, Veberic, D, Ventura, C, Quispe, Idv, Verzi, V, Vicha, J, Vink, J, Vorobiov, S, Watanabe, C, Watson, Aa, Weindl, A, Wiencke, L, Wilczynski, H, Wittkowski, D, Wundheiler, B, Yushkov, A, Zapparrata, O, Zas, E, Zavrtanik, D, Zavrtanik, M, and Zehrer, L
Subjects: transients, Astronomy, FOS: Physical sciences, General Physics and Astronomy, Photons, ultra-high energies, air showers, Pierre Auger Observatory, upper limits, transients, photons, ultra-high energies, air showers, Pierre Auger Observatory, upper limits, Transients, Air showers, ddc:530, High Energy Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Photons, showers: atmosphere, Ultra-high energies, photon, gravitational radiation, ASTROFÍSICA, UHE [gamma ray], Upper limits, Auger, flux, observatory, neutral particle, gamma ray: UHE, Experimental High Energy Physics, Astrophysics - High Energy Astrophysical Phenomena, atmosphere [showers]
Abstract: The Pierre Auger Observatory, which is the largest air-shower experiment in the world, offers unprecedented exposure to neutral particles at the highest energies. Since the start of data collection more than 18 years ago, various searches for ultra-high-energy (UHE, E & 1017 eV) photons have been performed, either for a diffuse flux of UHE photons, for point sources of UHE photons or for UHE photons associated with transient events such as gravitational wave events. In the present paper, we summarize these searches and review the current results obtained using the wealth of data collected by the Pierre Auger Observatory., Argentina-Comision Nacional de Energia Atomica, ANPCyT, Consejo Nacional de Investigaciones Cientificas y Tecnicas (CONICET), Gobierno de la Provincia de Mendoza, Municipalidad de Malargue, NDM Holdings, Valle Las Lenas, Australian Research Council, Belgium-Fonds de la Recherche Scientifique (FNRS), FWO, Conselho Nacional de Desenvolvimento Cientifico e Tecnologico (CNPQ) Fundacao de Apoio a Pesquisa do Distrito Federal (FAPDF) Financiadora de Inovacao e Pesquisa (Finep) Fundacao Carlos Chagas Filho de Amparo a Pesquisa do Estado do Rio De Janeiro (FAPERJ) Fundacao de Amparo a Pesquisa do Estado de Sao Paulo (FAPESP) 2019/10151-2 2010/07359-6 1999/05404-3, Ministerio da Ciencia, Tecnologia, Inovacoes e Comunicacoes (MCTIC), France-Centre de Calcul IN2P3/CNRS Centre National de la Recherche Scientifique (CNRS) Region Ile-de-France Centre National de la Recherche Scientifique (CNRS) Departement Sciences de l'Univers (SDU-INSU/CNRS) French National Research Agency (ANR) LABEX ANR-10-LABX-63 ANR-11-IDEX-0004-02, Federal Ministry of Education & Research (BMBF) German Research Foundation (DFG) Finanzministerium Baden-Wurttemberg Helmholtz Alliance for Astroparticle Physics (HAP) Helmholtz Association Ministerium fur Kultur und Wissenschaft des Landes Nordrhein-Westfalen Ministerium fur Wissenschaft, Forschung und Kunst des Landes Baden-Wurttemberg, Italy-Istituto Nazionale di Fisica Nucleare (INFN) Istituto Nazionale Astrofisica (INAF), Ministry of Education, Universities and Research (MIUR), CETEMPS Center of Excellence, Ministry of Foreign Affairs and International Cooperation (Italy), Consejo Nacional de Ciencia y Tecnologia (CONACyT) 167733 Universidad Nacional Autonoma de Mexico Programa de Apoyo a Proyectos de Investigacion e Innovacion Tecnologica (PAPIIT) Universidad Nacional Autonoma de Mexico, Netherlands-Ministry of Education, Culture and Science Netherlands Organization for Scientific Research (NWO), SURF Cooperative, Poland-Ministry of Education and Science DIR/WK/2018/11 National Science Centre, Poland 2016/22/M/ST9/00198 2016/23/B/ST9/01635 2020/39/B/ST9/01398, Portuguese Foundation for Science and Technology FEDER funds within Programa Operacional Factores de Competitividade through FundacAo para a Ciencia e a Tecnologia (COMPETE), Romania-Ministry of Research, Innovation and Digitization, CNCS/CCCDI UEFISCDI within the National Nucleus Program PN19150201/16N/2019 PN1906010 PNCDI III TE128 PN-III-P1-1.1-TE-2021-0924/TE57/2022 PED289, Slovenian Research Agency - Slovenia P1-0031 P1-0385 I0-0033 N1-0111, Spanish Government FPA2017-85114-P PID2019-104676GB-C32, Xunta de Galicia, European Commission ED431C 2017/07, Junta de Andalucia SOMM17/6104/UGR P18-FR-4314, European Commission, RENATA Red Nacional Tematica de Astroparticulas FPA2015-68783-REDT, Maria de Maeztu Unit of Excellence MDM-2016-0692, United States Department of Energy (DOE) DE-AC02-07CH11359 DE-FR02-04ER41300 DE-FG02-99ER41107 DE-SC0011689, National Science Foundation (NSF) 0450696, Grainger Foundation, Marie Curie-IRSES/EPLANET, European Particle Physics Latin American Network, UNESCO, MSMT CR LTT18004 LM2015038 LM2018102 CZ.02.1.01/0.0/0.0/16_013/0001402 CZ.02.1.01/0.0/0.0/18_046/0016010 CZ.02.1.01/0.0/0.0/17_049/0008422
Published: 2022
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6. Study on multi-ELVES in the Pierre Auger Observatory

Author: Collaboration, Pierre Auger, V��squez Ram��rez, Adriana, Abreu, Pedro, Aglietta, Marco, Albury, Justin M., Allekotte, Ingomar, Almela, Alejandro, Alvarez-Muniz, Jaime, Alves Batista, Rafael, Anastasi, Gioacchino Alex, Anchordoqui, Luis A., Andrada, Bel��n, Andringa, Sofia, Aramo, Carla, Ara��jo Ferreira, Paulo Ricardo, Arteaga Velazquez, Juan Carlos, Asorey, Hern��n Gonzalo, Assis, Pedro, Avila, Gualberto, Badescu, Alina Mihaela, Bakalova, Alena, Balaceanu, Alexandru, Barbato, Felicia, Barreira Luz, Ricardo Jorge, Becker, Karl-Heinz, Bellido, Jose A., Berat, Corinne, Bertaina, Mario Edoardo, Bertou, Xavier, Biermann, Peter L., Binet, Virginia, Bismark, Kathrin, Bister, Teresa, Biteau, Jonathan, Blazek, Jiri, Bleve, Carla, Bohacova, Martina, Boncioli, Denise, Bonifazi, Carla, Bonneau Arbeletche, Luan, Borodai, Nataliia, Botti, Ana Martina, Brack, Jeffrey, Bretz, Thomas, Brichetto Orchera, P. Gabriel, Briechle, Florian Lukas, Buchholz, Peter, Bueno, Antonio, Buitink, Stijn, Buscemi, Mario, B��sken, Max, Caballero-Mora, Karen S., Caccianiga, Lorenzo, Canfora, Fabrizia, Caracas, Ioana, Carceller, Juan Miguel, Caruso, Rossella, Castellina, Antonella, Catalani, Fernando, Cataldi, Gabriella, Cazon, Lorenzo, Cerda, Marcos, Chinellato, Jose Augusto, Chudoba, Jiri, Chytka, Ladislav, Clay, Roger W., Cobos Cerutti, Agust��n, Colalillo, Roberta, Coleman, Alan, Coluccia, Maria Rita, Concei��o, R��ben, Condorelli, Antonio, Consolati, Giovanni, Contreras, Fernando, Convenga, Fabio, Correia Dos Santos, Diego, Covault, Corbin, Dasso, Sergio, Daumiller, Kai, Dawson, Bruce R., Day, Jarryd A., Almeida, Rogerio M. De, Jes��s, Joaqu��n De, Jong, Sijbrand J. De, De Mauro, Giuseppe, Mello Neto, Jo��o De, De Mitri, Ivan, Oliveira, Jaime De, Oliveira Franco, Danelise De, Palma, Francesco De, Souza, Vitor De, De Vito, Emanuele, R��o, Mariano Del, Deligny, Olivier, Deval, Luca, Matteo, Armando Di, Dobrigkeit, Carola, D'Olivo, Juan Carlos, Domingues Mendes, Luis Miguel, Anjos, Rita Dos, Santos, Diego Dos, Dova, Maria Teresa, Ebr, Jan, Engel, Ralph, Epicoco, Italo, Erdmann, Martin, Escobar, Carlos O., Etchegoyen, Alberto, Falcke, Heino, Farmer, John, Farrar, Glennys R., Fauth, Anderson, Fazzini, Norberto, Feldbusch, Fridtjof, Fenu, Francesco, Fick, Brian, Figueira, Juan Manuel, Filipcic, Andrej, Fitoussi, Thomas, Fodran, Tom��, Freire, Mart��n Miguel, Fujii, Toshihiro, Fuster, Alan, Galea, Cristina, Galelli, Claudio, Garc��a, Beatriz, Garc��a Vegas, Adrianna Luz, Gemmeke, Hartmut, Gesualdi, Flavia, Gherghel-Lascu, Alexandru, Ghia, Piera Luisa, GIACCARI, Ugo, Giammarchi, Marco, Glombitza, Jonas, Gobbi, Fabian, Gollan, Fernando, Golup, Geraldina, G��mez Berisso, Mariano, G��mez Vitale, Primo F., Gongora, Juan Pablo, Gonz��lez, Juan Manuel, Gonzalez, Nicolas Martin, Goos, Isabel, Gora, Dariusz, Gorgi, Alessio, Gottowik, Marvin, Grubb, Trent D., Guarino, Fausto, Guedes, Germano, Guido, Eleonora, Hahn, Steffen, Hamal, Petr, Hampel, Mat��as Rolf, Hansen, Patricia Mar��a, Harari, Diego, Harvey, Violet M., Haungs, Andreas, Hebbeker, Thomas, Heck, Dieter, Hill, Gary C., Hojvat, Carlos, H��randel, J��rg, Horvath, Pavel, Hrabovsky, Miroslav, Huege, Tim, Insolia, Antonio, Isar, Paula Gina, Janecek, Petr, Johnsen, Jeffrey A., Jury��ek, Jakub, K��p��, Alex, Kampert, Karl-Heinz, Karastathis, Nikolaos, Keilhauer, Bianca, Kemp, Julian, Khakurdikar, Abha, Kizakke Covilakam, Varada Varma, Klages, Hans, Kleifges, Matthias, Kleinfeller, Jonny, K��pke, Marcel, Kunka, Norbert, Lago, Bruno L., Lang, Rodrigo Guedes, Langner, Niklas, Leigui De Oliveira, Marcelo Augusto, Lenok, Vladimir, Letessier-Selvon, Antoine, Lhenry-Yvon, Isabelle, Lo Presti, Domenico, LOPES, Luis, L��pez, Rebeca, Lu, Lu, Luce, Quentin, Lundquist, Jon Paul, Machado Payeras, Allan, Mancarella, Giovanni, Mandat, Dusan, Manning, Bradley C., Manshanden, Julien, Mantsch, Paul, Marafico, Sullivan, Mariazzi, Analisa, Maris, Ioana Codrina, Marsella, Giovanni, Martello, Daniele, Martinelli, Sara, Mart��nez Bravo, Oscar, Mastrodicasa, Massimo, Mathes, Hermann-Josef, Matthews, James, Matthiae, Giorgio, Mayotte, Eric, Mazur, Peter, Medina-Tanco, Gustavo, Melo, Diego, Menshikov, Alexander, Merenda, Kevin-Druis, Michal, Stanislav, Micheletti, Maria Isabel, Miramonti, Lino, Mollerach, Silvia, Montanet, Fran��ois, Morello, Carlo, Mostafa, Miguel, M��ller, Ana L., Muller, Marcio Aparecido, Mulrey, Katharine, Mussa, Roberto, Muzio, Marco Stein, Namasaka, Wilson M., Nasr-Esfahani, Alina, Nellen, Lukas, Niculescu-Oglinzanu, Mihai, Niechciol, Marcus, Nitz, Dave, Nosek, Dalibor, Novotn��, Vladim��r, Nozka, Libor, Nucita, Achille, Nunez, Luis A., Palatka, Miroslav, Pallotta, Juan, Papenbreer, Philipp, Parente, Gonzalo, Parra, Alejandra, Pawlowsky, Jannis, Pech, Miroslav, Pedreira, Francisco, P��kala, Jan, Pelayo, Rodrigo, Pe��a-Rodr��guez, Jes��s, Pereira Martins, Edyvania Emily, Perez Armand, Johnnier, P��rez Bertolli, Carmina, Perlin, Mat��as, Perrone, Lorenzo, Petrera, Sergio, Pierog, Tanguy, Pimenta, M��rio, Pirronello, Valerio, Platino, Manuel, Pont, Bjarni, Pothast, Mart, Privitera, Paolo, Prouza, Michael, Puyleart, Andrew, Querchfeld, Sven, Rautenberg, Julian, Ravignani, Diego, Reininghaus, Maximilian, Ridky, Jan, Riehn, Felix, Risse, Markus, Rizi, Vincenzo, Rodrigues De Carvalho, Washington, Rodriguez Rojo, Jorge Rub��n, Roncoroni, Mat��as J., Rossoni, Simone, Roth, Markus, Roulet, Esteban, Rovero, Adrian, Ruehl, Philip, Saftoiu, Alexandra, Salamida, Francesco, Salazar, Humberto Ibarguen, Salina, Gaetano, Sanabria Gomez, Jose, S��nchez, Federico Andr��s, Santos, Edivaldo Moura, Santos, Eva, Sarazin, Fred, Sarmento, Raul, Sarmiento-Cano, Christian, Sato, Ricardo, Savina, Pierpaolo, Sch��fer, Christoph M., Scherini, Viviana, Schieler, Harald, Schimassek, Martin, Schimp, Michael, Schl��ter, Felix, Schmidt, David, Scholten, Olaf, Schovanek, Petr, Schr��der, Frank G., Schr��der, Sonja, Schulte, Josina, Sciutto, Sergio, Scornavacche, Marina, Segreto, Alberto, Sehgal, Srijan, Shellard, Ronald C., Sigl, Guenter, Silli, Gaia, Sima, Octavian, Smida, Radomir, Sommers, Paul, Soriano, Jorge F., Souchard, Julien, Squartini, Ruben, Stadelmaier, Maximilian, Stanca, Denis, Stani��, Samo, Stasielak, Jaroslaw, Stassi, Patrick, Streich, Alexander, Su��rez-Dur��n, Mauricio, Sudholz, Tristan, Suomijarvi, Tiina, Supanitsky, A. Daniel, Szadkowski, Zbigniew, Tapia, Alex, Taricco, Carla, Timmermans, Charles, Tkachenko, Olena, Tobiska, Petr, Todero Peixoto, Carlos J., Tom��, Bernardo, Torr��s, Zo��, Travaini, Andres, Travnicek, Petr, Trimarelli, Caterina, Tueros, Matias, Ulrich, Ralf, Unger, Michael, Vaclavek, Luk��, Vacula, Martin, Vald��s Galicia, Jose F., Valore, Laura, Varela, Enrique, V��squez-Ram��rez, Adriana, Veberic, Darko, Ventura, Cynthia, Vergara Quispe, Indira D., Verzi, Valerio, Vicha, Jakub, Vink, Jacco, Vorobiov, Serguei, Wahlberg, Hernan, Watanabe, Clara Keiko Oliveira, Watson, Alan, Weber, Marc, Weindl, Andreas, Wiencke, Lawrence, Wilczy��ski, Henryk, Wirtz, Marcus, Wittkowski, David, Wundheiler, Brian, Yushkov, Alexey, Zapparrata, Orazio, Zas, Enrique, Zavrtanik, Danilo, Zavrtanik, Marko, and Zehrer, Lukas
Subjects: Physics, Pierre Auger Observatory, Polarity (physics), Astronomy, Astrophysics, Lightning, Lightning strike, Altitude, Experimental High Energy Physics, Light emission, Satellite, High Energy Physics, ddc:620, Ionosphere, Engineering & allied operations
Abstract: Since 2013, the four sites of the Fluorescence Detector (FD) of the Pierre Auger Observatory record ELVES with a dedicated trigger. These UV light emissions are correlated to distant lightning strikes. The length of recorded traces has been increased from 100 $\mu$s (2013), to 300 $\mu$s (2014-16), to 900 $\mu$s (2017-present), to progressively extend the observation of the light emission towards the vertical of the causative lightning and beyond. A large fraction of the observed events shows double ELVES within the time window, and, in some cases, even more complex structures are observed. The nature of the multi-ELVES is not completely understood but may be related to the different types of lightning in which they are originated. For example, it is known that Narrow Bipolar Events can produce double ELVES, and Energetic In-cloud Pulses, occurring between the main negative and upper positive charge layer of clouds, can induce double and even quadruple ELVES in the ionosphere. This report shows the seasonal and daily dependence of the time gap, amplitude ratio, and correlation between the pulse widths of the peaks in a sample of 1000+ multi-ELVES events recorded during the period 2014-20. The events have been compared with data from other satellite and ground-based sensing devices to study the correlation of their properties with lightning observables such as altitude and polarity.
Published: 2022
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7. Including Millisecond Pulsars inside the Core of Globular Clusters in Pulsar Timing Arrays

Author: Maiorano, Michele, de Paolis, Francesco, and Nucita, Achille
Subjects: Astrophysics::High Energy Astrophysical Phenomena, Astrophysics of Galaxies (astro-ph.GA), Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astrophysics - Astrophysics of Galaxies
Abstract: We suggest the possibility of including millisecond pulsars inside the core of globular clusters in pulsar timing array experiments. Since they are very close to each other, their gravitational wave induced timing residuals are expected to be almost the same, because both the Earth and the pulsar terms are correlated. We simulate the expected timing residuals, due to the gravitational wave signal emitted by a uniform supermassive black-hole binary population, on the millisecond pulsars inside a globular cluster core. In this respect, Terzan 5 has been adopted as a globular cluster prototype and, in our simulations, we adopted similar distance, core radius, and number of millisecond pulsars contained in it. Our results show that the presence of a strong correlation between the timing residuals of the globular cluster core millisecond pulsars can provide a remarkable gravitational wave signature. This result can be therefore exploited for the detection of gravitational waves through pulsar timing, especially in conjunction with the standard cross-correlation search carried out by the pulsar timing array collaborations., Comment: 12 pages, 6 figures, in press on EPJ Plus (EPJP-D-21-03367R1)
Published: 2021
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8. Large-scale and multipolar anisotropies of cosmic rays detected at the Pierre Auger Observatory with energies above 4 EeV

Author: Pierre Auger Collaboration, Almeida, Rogerio de, Abreu, Pedro, Aglietta, Marco, Albury, Justin M., Allekotte, Ingomar, Almela, Alejandro, Alvarez-Muniz, Jaime, Alves Batista, Rafael, Anastasi, Gioacchino Alex, Anchordoqui, Luis A., Andrada, Belén, Andringa, Sofia, Aramo, Carla, Araújo Ferreira, Paulo Ricardo, Arteaga Velazquez, Juan Carlos, Asorey, Hernán Gonzalo, Assis, Pedro, Avila, Gualberto, Badescu, Alina Mihaela, Bakalova, Alena, Balaceanu, Alexandru, Barbato, Felicia, Barreira Luz, Ricardo Jorge, Becker, Karl-Heinz, Bellido, Jose A., Berat, Corinne, Bertaina, Mario Edoardo, Bertou, Xavier, Biermann, Peter L., Binet, Virginia, Bismark, Kathrin, Bister, Teresa, Biteau, Jonathan, Blazek, Jiri, Bleve, Carla, Bohacova, Martina, boncioli, denise, Bonifazi, Carla, Bonneau Arbeletche, Luan, Borodai, Nataliia, Botti, Ana Martina, Brack, Jeffrey, Bretz, Thomas, Brichetto Orchera, P. Gabriel, Briechle, Florian Lukas, Buchholz, Peter, Bueno, Antonio, Buitink, Stijn, Buscemi, Mario, Büsken, Max, Caballero-Mora, Karen S., Caccianiga, Lorenzo, Canfora, Fabrizia, Caracas, Ioana, Carceller, Juan Miguel, Caruso, Rossella, Castellina, Antonella, Catalani, Fernando, Cataldi, Gabriella, Cazon, Lorenzo, Cerda, Marcos, Chinellato, Jose Augusto, Chudoba, Jiri, Chytka, Ladislav, Clay, Roger W., Cobos Cerutti, Agustín, Colalillo, Roberta, Coleman, Alan, Coluccia, Maria Rita, Conceição, Rúben, Condorelli, Antonio, Consolati, Giovanni, Contreras, Fernando, Convenga, Fabio, Correia dos Santos, Diego, Covault, Corbin, Dasso, Sergio, Daumiller, Kai, Dawson, Bruce R., Day, Jarryd A., Almeida, Rogerio M. de, Jesús, Joaquín de, Jong, Sijbrand J. de, De Mauro, Giuseppe, Mello Neto, João de, De Mitri, Ivan, Oliveira, Jaime de, Oliveira Franco, Danelise de, Palma, Francesco de, Souza, Vitor de, De Vito, Emanuele, Río, Mariano del, Deligny, Olivier, Deval, Luca, Matteo, Armando di, Dobrigkeit, Carola, D'Olivo, Juan Carlos, Domingues Mendes, Luis Miguel, Anjos, Rita dos, Santos, Diego dos, Dova, Maria Teresa, Ebr, Jan, Engel, Ralph, Epicoco, Italo, Erdmann, Martin, Escobar, Carlos O., Etchegoyen, Alberto, Falcke, Heino, Farmer, John, Farrar, Glennys R., Fauth, Anderson, Fazzini, Norberto, Feldbusch, Fridtjof, Fenu, Francesco, Fick, Brian, Figueira, Juan Manuel, Filipcic, Andrej, Fitoussi, Thomas, Fodran, Tomáš, Freire, Martín Miguel, Fujii, Toshihiro, Fuster, Alan, Galea, Cristina, Galelli, Claudio, García, Beatriz, García Vegas, Adrianna Luz, Gemmeke, Hartmut, Gesualdi, Flavia, Gherghel-Lascu, Alexandru, Ghia, Piera Luisa, GIACCARI, Ugo, Giammarchi, Marco, Glombitza, Jonas, Gobbi, Fabian, Gollan, Fernando, Golup, Geraldina, Gómez Berisso, Mariano, Gómez Vitale, Primo F., Gongora, Juan Pablo, González, Juan Manuel, Gonzalez, Nicolas Martin, Goos, Isabel, Gora, Dariusz, Gorgi, Alessio, Gottowik, Marvin, Grubb, Trent D., Guarino, Fausto, Guedes, Germano, Guido, Eleonora, Hahn, Steffen, Hamal, Petr, Hampel, Matías Rolf, Hansen, Patricia María, Harari, Diego, Harvey, Violet M., Haungs, Andreas, Hebbeker, Thomas, Heck, Dieter, Hill, Gary C., Hojvat, Carlos, Hörandel, Jörg, Horvath, Pavel, Hrabovsky, Miroslav, Huege, Tim, Insolia, Antonio, Isar, Paula Gina, Janecek, Petr, Johnsen, Jeffrey A., Juryšek, Jakub, Kääpä, Alex, Kampert, Karl-Heinz, Karastathis, Nikolaos, Keilhauer, Bianca, Kemp, Julian, Khakurdikar, Abha, Kizakke Covilakam, Varada Varma, Klages, Hans, Kleifges, Matthias, Kleinfeller, Jonny, Köpke, Marcel, Kunka, Norbert, Lago, Bruno L., Lang, Rodrigo Guedes, Langner, Niklas, Leigui de Oliveira, Marcelo Augusto, Lenok, Vladimir, Letessier-Selvon, Antoine, Lhenry-Yvon, Isabelle, Lo Presti, Domenico, LOPES, Luis, López, Rebeca, Lu, Lu, Luce, Quentin, Lundquist, Jon Paul, Machado Payeras, Allan, Mancarella, Giovanni, Mandat, Dusan, Manning, Bradley C., Manshanden, Julien, Mantsch, Paul, Marafico, Sullivan, Mariazzi, Analisa, Maris, Ioana Codrina, Marsella, Giovanni, Martello, Daniele, Martinelli, Sara, Martínez Bravo, Oscar, Mastrodicasa, Massimo, Mathes, Hermann-Josef, Matthews, James, Matthiae, Giorgio, Mayotte, Eric, Mazur, Peter, Medina-Tanco, Gustavo, Melo, Diego, Menshikov, Alexander, Merenda, Kevin-Druis, Michal, Stanislav, Micheletti, Maria Isabel, Miramonti, Lino, Mollerach, Silvia, Montanet, François, Morello, Carlo, Mostafa, Miguel, Müller, Ana L., Muller, Marcio Aparecido, Mulrey, Katharine, Mussa, Roberto, Muzio, Marco Stein, Namasaka, Wilson M., Nasr-Esfahani, Alina, Nellen, Lukas, Niculescu-Oglinzanu, Mihai, Niechciol, Marcus, Nitz, Dave, Nosek, Dalibor, Novotný, Vladimír, Nozka, Libor, Nucita, Achille, Nunez, Luis A., Palatka, Miroslav, Pallotta, Juan, Papenbreer, Philipp, Parente, Gonzalo, Parra, Alejandra, Pawlowsky, Jannis, Pech, Miroslav, Pedreira, Francisco, Pękala, Jan, Pelayo, Rodrigo, Peña-Rodríguez, Jesús, Pereira Martins, Edyvania Emily, Perez Armand, Johnnier, Pérez Bertolli, Carmina, Perlin, Matías, Perrone, Lorenzo, Petrera, Sergio, Pierog, Tanguy, Pimenta, Mário, Pirronello, Valerio, Platino, Manuel, Pont, Bjarni, Pothast, Mart, Privitera, Paolo, Prouza, Michael, Puyleart, Andrew, Querchfeld, Sven, Rautenberg, Julian, Ravignani, Diego, Reininghaus, Maximilian, Ridky, Jan, Riehn, Felix, Risse, Markus, Rizi, Vincenzo, Rodrigues de Carvalho, Washington, Rodriguez Rojo, Jorge Rubén, Roncoroni, Matías J., Rossoni, Simone, Roth, Markus, Roulet, Esteban, Rovero, Adrian, Ruehl, Philip, Saftoiu, Alexandra, Salamida, Francesco, Salazar, Humberto Ibarguen, Salina, Gaetano, Sanabria Gomez, Jose, Sánchez, Federico Andrés, Santos, Edivaldo Moura, Santos, Eva, Sarazin, Fred, Sarmento, Raul, Sarmiento-Cano, Christian, Sato, Ricardo, Savina, Pierpaolo, Schäfer, Christoph M., Scherini, Viviana, Schieler, Harald, Schimassek, Martin, Schimp, Michael, Schlüter, Felix, Schmidt, David, Scholten, Olaf, Schovanek, Petr, Schröder, Frank G., Schröder, Sonja, Schulte, Josina, Sciutto, Sergio, Scornavacche, Marina, Segreto, Alberto, Sehgal, Srijan, Shellard, Ronald C., Sigl, Guenter, Silli, Gaia, Sima, Octavian, Smida, Radomir, Sommers, Paul, Soriano, Jorge F., Souchard, Julien, Squartini, Ruben, Stadelmaier, Maximilian, Stanca, Denis, Stanič, Samo, Stasielak, Jaroslaw, Stassi, Patrick, Streich, Alexander, Suárez-Durán, Mauricio, Sudholz, Tristan, Suomijarvi, Tiina, Supanitsky, A. Daniel, Szadkowski, Zbigniew, Tapia, Alex, Taricco, Carla, Timmermans, Charles, Tkachenko, Olena, Tobiska, Petr, Todero Peixoto, Carlos J., Tomé, Bernardo, Torrès, Zoé, Travaini, Andres, Travnicek, Petr, Trimarelli, Caterina, Tueros, Matias, Ulrich, Ralf, Unger, Michael, Vaclavek, Lukáš, Vacula, Martin, Valdés Galicia, Jose F., Valore, Laura, Varela, Enrique, Vásquez-Ramírez, Adriana, Veberic, Darko, Ventura, Cynthia, Vergara Quispe, Indira D., Verzi, Valerio, Vicha, Jakub, Vink, Jacco, Vorobiov, Serguei, Wahlberg, Hernan, Watanabe, Clara Keiko Oliveira, Watson, Alan, Weber, Marc, Weindl, Andreas, Wiencke, Lawrence, Wilczyński, Henryk, Wirtz, Marcus, Wittkowski, David, Wundheiler, Brian, Yushkov, Alexey, Zapparrata, Orazio, Zas, Enrique, Zavrtanik, Danilo, Zavrtanik, Marko, and Zehrer, Lukas
Subjects: Physics, Pierre Auger Observatory, Astrophysics::High Energy Astrophysical Phenomena, media_common.quotation_subject, Astronomy, Astrophysics::Instrumentation and Methods for Astrophysics, Spectral density, Cosmic ray, Astrophysics, Azimuth, Sky, Observatory, Experimental High Energy Physics, ddc:530, High Energy Physics, Right ascension, Zenith, media_common
Abstract: More than half a century after the discovery of ultra-high energy cosmic rays (UHECRs), their origin is still an open question. The study of anisotropies in the arrival directions of such particles is an essential ingredient to solve this puzzle. We update our previous analysis of large-scale anisotropies observed by the Pierre Auger Observatory using the latest data collected before the AugerPrime upgrade. We select events with zenith angles up to 80 degrees, implying a sky coverage of 85$\%$, and energies above 4 EeV, for which the surface detector of the Observatory is fully efficient. Dipolar and quadrupolar amplitudes are evaluated through a combined Fourier analysis of the event count rate in right ascension and azimuth. The analysis is performed in three energy bins with boundaries at 4, 8, 16 and 32 EeV and two additional cumulative bins with energies above 8 and 32 EeV. The most significant signal is a dipolar modulation in right ascension for energies above 8 EeV, as previously reported, with statistical significance of $6.6\sigma$. Additionally, we report the measurements of the angular power spectrum for the same energy bins with the same dataset.

9. Monte Carlo simulations for the Pierre Auger Observatory using the VO auger grid resources

Author: Pierre Auger Collaboration, Santos, Eva, Abreu, Pedro, Aglietta, Marco, Albury, Justin M., Allekotte, Ingomar, Almela, Alejandro, Alvarez-Muniz, Jaime, Alves Batista, Rafael, Anastasi, Gioacchino Alex, Anchordoqui, Luis A., Andrada, Belén, Andringa, Sofia, Aramo, Carla, Araújo Ferreira, Paulo Ricardo, Arteaga Velazquez, Juan Carlos, Asorey, Hernán Gonzalo, Assis, Pedro, Avila, Gualberto, Badescu, Alina Mihaela, Bakalova, Alena, Balaceanu, Alexandru, Barbato, Felicia, Barreira Luz, Ricardo Jorge, Becker, Karl-Heinz, Bellido, Jose A., Berat, Corinne, Bertaina, Mario Edoardo, Bertou, Xavier, Biermann, Peter L., Binet, Virginia, Bismark, Kathrin, Bister, Teresa, Biteau, Jonathan, Blazek, Jiri, Bleve, Carla, Bohacova, Martina, boncioli, denise, Bonifazi, Carla, Bonneau Arbeletche, Luan, Borodai, Nataliia, Botti, Ana Martina, Brack, Jeffrey, Bretz, Thomas, Brichetto Orchera, P. Gabriel, Briechle, Florian Lukas, Buchholz, Peter, Bueno, Antonio, Buitink, Stijn, Buscemi, Mario, Büsken, Max, Caballero-Mora, Karen S., Caccianiga, Lorenzo, Canfora, Fabrizia, Caracas, Ioana, Carceller, Juan Miguel, Caruso, Rossella, Castellina, Antonella, Catalani, Fernando, Cataldi, Gabriella, Cazon, Lorenzo, Cerda, Marcos, Chinellato, Jose Augusto, Chudoba, Jiri, Chytka, Ladislav, Clay, Roger W., Cobos Cerutti, Agustín, Colalillo, Roberta, Coleman, Alan, Coluccia, Maria Rita, Conceição, Rúben, Condorelli, Antonio, Consolati, Giovanni, Contreras, Fernando, Convenga, Fabio, Correia dos Santos, Diego, Covault, Corbin, Dasso, Sergio, Daumiller, Kai, Dawson, Bruce R., Day, Jarryd A., Almeida, Rogerio M. de, Jesús, Joaquín de, Jong, Sijbrand J. de, De Mauro, Giuseppe, Mello Neto, João de, De Mitri, Ivan, Oliveira, Jaime de, Oliveira Franco, Danelise de, Palma, Francesco de, Souza, Vitor de, De Vito, Emanuele, Río, Mariano del, Deligny, Olivier, Deval, Luca, Matteo, Armando di, Dobrigkeit, Carola, D'Olivo, Juan Carlos, Domingues Mendes, Luis Miguel, Anjos, Rita dos, Santos, Diego dos, Dova, Maria Teresa, Ebr, Jan, Engel, Ralph, Epicoco, Italo, Erdmann, Martin, Escobar, Carlos O., Etchegoyen, Alberto, Falcke, Heino, Farmer, John, Farrar, Glennys R., Fauth, Anderson, Fazzini, Norberto, Feldbusch, Fridtjof, Fenu, Francesco, Fick, Brian, Figueira, Juan Manuel, Filipcic, Andrej, Fitoussi, Thomas, Fodran, Tomáš, Freire, Martín Miguel, Fujii, Toshihiro, Fuster, Alan, Galea, Cristina, Galelli, Claudio, García, Beatriz, García Vegas, Adrianna Luz, Gemmeke, Hartmut, Gesualdi, Flavia, Gherghel-Lascu, Alexandru, Ghia, Piera Luisa, GIACCARI, Ugo, Giammarchi, Marco, Glombitza, Jonas, Gobbi, Fabian, Gollan, Fernando, Golup, Geraldina, Gómez Berisso, Mariano, Gómez Vitale, Primo F., Gongora, Juan Pablo, González, Juan Manuel, Gonzalez, Nicolas Martin, Goos, Isabel, Gora, Dariusz, Gorgi, Alessio, Gottowik, Marvin, Grubb, Trent D., Guarino, Fausto, Guedes, Germano, Guido, Eleonora, Hahn, Steffen, Hamal, Petr, Hampel, Matías Rolf, Hansen, Patricia María, Harari, Diego, Harvey, Violet M., Haungs, Andreas, Hebbeker, Thomas, Heck, Dieter, Hill, Gary C., Hojvat, Carlos, Hörandel, Jörg, Horvath, Pavel, Hrabovsky, Miroslav, Huege, Tim, Insolia, Antonio, Isar, Paula Gina, Janecek, Petr, Johnsen, Jeffrey A., Juryšek, Jakub, Kääpä, Alex, Kampert, Karl-Heinz, Karastathis, Nikolaos, Keilhauer, Bianca, Kemp, Julian, Khakurdikar, Abha, Kizakke Covilakam, Varada Varma, Klages, Hans, Kleifges, Matthias, Kleinfeller, Jonny, Köpke, Marcel, Kunka, Norbert, Lago, Bruno L., Lang, Rodrigo Guedes, Langner, Niklas, Leigui de Oliveira, Marcelo Augusto, Lenok, Vladimir, Letessier-Selvon, Antoine, Lhenry-Yvon, Isabelle, Lo Presti, Domenico, LOPES, Luis, López, Rebeca, Lu, Lu, Luce, Quentin, Lundquist, Jon Paul, Machado Payeras, Allan, Mancarella, Giovanni, Mandat, Dusan, Manning, Bradley C., Manshanden, Julien, Mantsch, Paul, Marafico, Sullivan, Mariazzi, Analisa, Maris, Ioana Codrina, Marsella, Giovanni, Martello, Daniele, Martinelli, Sara, Martínez Bravo, Oscar, Mastrodicasa, Massimo, Mathes, Hermann-Josef, Matthews, James, Matthiae, Giorgio, Mayotte, Eric, Mazur, Peter, Medina-Tanco, Gustavo, Melo, Diego, Menshikov, Alexander, Merenda, Kevin-Druis, Michal, Stanislav, Micheletti, Maria Isabel, Miramonti, Lino, Mollerach, Silvia, Montanet, François, Morello, Carlo, Mostafa, Miguel, Müller, Ana L., Muller, Marcio Aparecido, Mulrey, Katharine, Mussa, Roberto, Muzio, Marco Stein, Namasaka, Wilson M., Nasr-Esfahani, Alina, Nellen, Lukas, Niculescu-Oglinzanu, Mihai, Niechciol, Marcus, Nitz, Dave, Nosek, Dalibor, Novotný, Vladimír, Nozka, Libor, Nucita, Achille, Nunez, Luis A., Palatka, Miroslav, Pallotta, Juan, Papenbreer, Philipp, Parente, Gonzalo, Parra, Alejandra, Pawlowsky, Jannis, Pech, Miroslav, Pedreira, Francisco, Pękala, Jan, Pelayo, Rodrigo, Peña-Rodríguez, Jesús, Pereira Martins, Edyvania Emily, Perez Armand, Johnnier, Pérez Bertolli, Carmina, Perlin, Matías, Perrone, Lorenzo, Petrera, Sergio, Pierog, Tanguy, Pimenta, Mário, Pirronello, Valerio, Platino, Manuel, Pont, Bjarni, Pothast, Mart, Privitera, Paolo, Prouza, Michael, Puyleart, Andrew, Querchfeld, Sven, Rautenberg, Julian, Ravignani, Diego, Reininghaus, Maximilian, Ridky, Jan, Riehn, Felix, Risse, Markus, Rizi, Vincenzo, Rodrigues de Carvalho, Washington, Rodriguez Rojo, Jorge Rubén, Roncoroni, Matías J., Rossoni, Simone, Roth, Markus, Roulet, Esteban, Rovero, Adrian, Ruehl, Philip, Saftoiu, Alexandra, Salamida, Francesco, Salazar, Humberto Ibarguen, Salina, Gaetano, Sanabria Gomez, Jose, Sánchez, Federico Andrés, Santos, Edivaldo Moura, Sarazin, Fred, Sarmento, Raul, Sarmiento-Cano, Christian, Sato, Ricardo, Savina, Pierpaolo, Schäfer, Christoph M., Scherini, Viviana, Schieler, Harald, Schimassek, Martin, Schimp, Michael, Schlüter, Felix, Schmidt, David, Scholten, Olaf, Schovanek, Petr, Schröder, Frank G., Schröder, Sonja, Schulte, Josina, Sciutto, Sergio, Scornavacche, Marina, Segreto, Alberto, Sehgal, Srijan, Shellard, Ronald C., Sigl, Guenter, Silli, Gaia, Sima, Octavian, Smida, Radomir, Sommers, Paul, Soriano, Jorge F., Souchard, Julien, Squartini, Ruben, Stadelmaier, Maximilian, Stanca, Denis, Stanič, Samo, Stasielak, Jaroslaw, Stassi, Patrick, Streich, Alexander, Suárez-Durán, Mauricio, Sudholz, Tristan, Suomijarvi, Tiina, Supanitsky, A. Daniel, Szadkowski, Zbigniew, Tapia, Alex, Taricco, Carla, Timmermans, Charles, Tkachenko, Olena, Tobiska, Petr, Todero Peixoto, Carlos J., Tomé, Bernardo, Torrès, Zoé, Travaini, Andres, Travnicek, Petr, Trimarelli, Caterina, Tueros, Matias, Ulrich, Ralf, Unger, Michael, Vaclavek, Lukáš, Vacula, Martin, Valdés Galicia, Jose F., Valore, Laura, Varela, Enrique, Vásquez-Ramírez, Adriana, Veberic, Darko, Ventura, Cynthia, Vergara Quispe, Indira D., Verzi, Valerio, Vicha, Jakub, Vink, Jacco, Vorobiov, Serguei, Wahlberg, Hernan, Watanabe, Clara Keiko Oliveira, Watson, Alan, Weber, Marc, Weindl, Andreas, Wiencke, Lawrence, Wilczyński, Henryk, Wirtz, Marcus, Wittkowski, David, Wundheiler, Brian, Yushkov, Alexey, Zapparrata, Orazio, Zas, Enrique, Zavrtanik, Danilo, Zavrtanik, Marko, and Zehrer, Lukas
Subjects: Pierre Auger Observatory, Physics, Large Hadron Collider, Physics::Instrumentation and Detectors, Astronomy, Astrophysics::High Energy Astrophysical Phenomena, Detector, Monte Carlo method, Astrophysics::Instrumentation and Methods for Astrophysics, Cosmic ray, Grid, Computational physics, Auger, Upgrade, Experimental High Energy Physics, ddc:530, High Energy Physics
Abstract: The Pierre Auger Observatory, located near Malargue, Argentina, is the world's largest cosmic-ray detector. It comprises a $3000\,\mathrm{km}^{2}$ surface detector and 27 fluorescence telescopes, which measure the lateral and longitudinal distributions of the many millions of air-shower particles produced in the interactions initiated by a cosmic ray in the Earth's atmosphere. The determination of the nature of cosmic rays and studies of the detector performances rely on extensive Monte Carlo simulations describing the physics processes occurring in extensive air showers and the detector responses. The aim of the Monte Carlo simulations task is to produce and provide the Auger Collaboration with reference libraries used in a wide variety of analyses. All multipurpose detector simulations are currently produced in local clusters using Slurm and HTCondor. The bulk of the shower simulations are produced on the grid, via the Virtual Organization auger, using the DIRAC middleware. The job submission is made via python scripts using the DIRAC-API. The Auger site is undergoing a major upgrade, which includes the installation of new types of detectors, demanding increased simulation resources. The novel detection of the radio component of extensive air showers is the most challenging endeavor, requiring dedicated shower simulations with very long computation times, not optimized for the grid production. For data redundancy, the simulations are stored on the Lyon server and the grid Disk Pool Manager and are accessible to the Auger members via iRODS and DIRAC, respectively. The CERN VM-File System is used for software distribution where, soon, the Auger Offline software will also be made available.

10. Outreach activities at the Pierre Auger Observatory

Author: Collaboration, Pierre Auger, Caballero Mora, Karen Salom��, Abreu, Pedro, Aglietta, Marco, Albury, Justin M., Allekotte, Ingomar, Almela, Alejandro, Alvarez-Muniz, Jaime, Alves Batista, Rafael, Anastasi, Gioacchino Alex, Anchordoqui, Luis A., Andrada, Bel��n, Andringa, Sofia, Aramo, Carla, Ara��jo Ferreira, Paulo Ricardo, Arteaga Velazquez, Juan Carlos, Asorey, Hern��n Gonzalo, Assis, Pedro, Avila, Gualberto, Badescu, Alina Mihaela, Bakalova, Alena, Balaceanu, Alexandru, Barbato, Felicia, Barreira Luz, Ricardo Jorge, Becker, Karl-Heinz, Bellido, Jose A., Berat, Corinne, Bertaina, Mario Edoardo, Bertou, Xavier, Biermann, Peter L., Binet, Virginia, Bismark, Kathrin, Bister, Teresa, Biteau, Jonathan, Blazek, Jiri, Bleve, Carla, Bohacova, Martina, Boncioli, Denise, Bonifazi, Carla, Bonneau Arbeletche, Luan, Borodai, Nataliia, Botti, Ana Martina, Brack, Jeffrey, Bretz, Thomas, Brichetto Orchera, P. Gabriel, Briechle, Florian Lukas, Buchholz, Peter, Bueno, Antonio, Buitink, Stijn, Buscemi, Mario, B��sken, Max, Caballero-Mora, Karen S., Caccianiga, Lorenzo, Canfora, Fabrizia, Caracas, Ioana, Carceller, Juan Miguel, Caruso, Rossella, Castellina, Antonella, Catalani, Fernando, Cataldi, Gabriella, Cazon, Lorenzo, Cerda, Marcos, Chinellato, Jose Augusto, Chudoba, Jiri, Chytka, Ladislav, Clay, Roger W., Cobos Cerutti, Agust��n, Colalillo, Roberta, Coleman, Alan, Coluccia, Maria Rita, Concei��o, R��ben, Condorelli, Antonio, Consolati, Giovanni, Contreras, Fernando, Convenga, Fabio, Correia Dos Santos, Diego, Covault, Corbin, Dasso, Sergio, Daumiller, Kai, Dawson, Bruce R., Day, Jarryd A., Almeida, Rogerio M. De, Jes��s, Joaqu��n De, Jong, Sijbrand J. De, De Mauro, Giuseppe, Mello Neto, Jo��o De, De Mitri, Ivan, Oliveira, Jaime De, Oliveira Franco, Danelise De, Palma, Francesco De, Souza, Vitor De, De Vito, Emanuele, R��o, Mariano Del, Deligny, Olivier, Deval, Luca, Matteo, Armando Di, Dobrigkeit, Carola, D'Olivo, Juan Carlos, Domingues Mendes, Luis Miguel, Anjos, Rita Dos, Santos, Diego Dos, Dova, Maria Teresa, Ebr, Jan, Engel, Ralph, Epicoco, Italo, Erdmann, Martin, Escobar, Carlos O., Etchegoyen, Alberto, Falcke, Heino, Farmer, John, Farrar, Glennys R., Fauth, Anderson, Fazzini, Norberto, Feldbusch, Fridtjof, Fenu, Francesco, Fick, Brian, Figueira, Juan Manuel, Filipcic, Andrej, Fitoussi, Thomas, Fodran, Tom��, Freire, Mart��n Miguel, Fujii, Toshihiro, Fuster, Alan, Galea, Cristina, Galelli, Claudio, Garc��a, Beatriz, Garc��a Vegas, Adrianna Luz, Gemmeke, Hartmut, Gesualdi, Flavia, Gherghel-Lascu, Alexandru, Ghia, Piera Luisa, GIACCARI, Ugo, Giammarchi, Marco, Glombitza, Jonas, Gobbi, Fabian, Gollan, Fernando, Golup, Geraldina, G��mez Berisso, Mariano, G��mez Vitale, Primo F., Gongora, Juan Pablo, Gonz��lez, Juan Manuel, Gonzalez, Nicolas Martin, Goos, Isabel, Gora, Dariusz, Gorgi, Alessio, Gottowik, Marvin, Grubb, Trent D., Guarino, Fausto, Guedes, Germano, Guido, Eleonora, Hahn, Steffen, Hamal, Petr, Hampel, Mat��as Rolf, Hansen, Patricia Mar��a, Harari, Diego, Harvey, Violet M., Haungs, Andreas, Hebbeker, Thomas, Heck, Dieter, Hill, Gary C., Hojvat, Carlos, H��randel, J��rg, Horvath, Pavel, Hrabovsky, Miroslav, Huege, Tim, Insolia, Antonio, Isar, Paula Gina, Janecek, Petr, Johnsen, Jeffrey A., Jury��ek, Jakub, K��p��, Alex, Kampert, Karl-Heinz, Karastathis, Nikolaos, Keilhauer, Bianca, Kemp, Julian, Khakurdikar, Abha, Kizakke Covilakam, Varada Varma, Klages, Hans, Kleifges, Matthias, Kleinfeller, Jonny, K��pke, Marcel, Kunka, Norbert, Lago, Bruno L., Lang, Rodrigo Guedes, Langner, Niklas, Leigui De Oliveira, Marcelo Augusto, Lenok, Vladimir, Letessier-Selvon, Antoine, Lhenry-Yvon, Isabelle, Lo Presti, Domenico, LOPES, Luis, L��pez, Rebeca, Lu, Lu, Luce, Quentin, Lundquist, Jon Paul, Machado Payeras, Allan, Mancarella, Giovanni, Mandat, Dusan, Manning, Bradley C., Manshanden, Julien, Mantsch, Paul, Marafico, Sullivan, Mariazzi, Analisa, Maris, Ioana Codrina, Marsella, Giovanni, Martello, Daniele, Martinelli, Sara, Mart��nez Bravo, Oscar, Mastrodicasa, Massimo, Mathes, Hermann-Josef, Matthews, James, Matthiae, Giorgio, Mayotte, Eric, Mazur, Peter, Medina-Tanco, Gustavo, Melo, Diego, Menshikov, Alexander, Merenda, Kevin-Druis, Michal, Stanislav, Micheletti, Maria Isabel, Miramonti, Lino, Mollerach, Silvia, Montanet, Fran��ois, Morello, Carlo, Mostafa, Miguel, M��ller, Ana L., Muller, Marcio Aparecido, Mulrey, Katharine, Mussa, Roberto, Muzio, Marco Stein, Namasaka, Wilson M., Nasr-Esfahani, Alina, Nellen, Lukas, Niculescu-Oglinzanu, Mihai, Niechciol, Marcus, Nitz, Dave, Nosek, Dalibor, Novotn��, Vladim��r, Nozka, Libor, Nucita, Achille, Nunez, Luis A., Palatka, Miroslav, Pallotta, Juan, Papenbreer, Philipp, Parente, Gonzalo, Parra, Alejandra, Pawlowsky, Jannis, Pech, Miroslav, Pedreira, Francisco, P��kala, Jan, Pelayo, Rodrigo, Pe��a-Rodr��guez, Jes��s, Pereira Martins, Edyvania Emily, Perez Armand, Johnnier, P��rez Bertolli, Carmina, Perlin, Mat��as, Perrone, Lorenzo, Petrera, Sergio, Pierog, Tanguy, Pimenta, M��rio, Pirronello, Valerio, Platino, Manuel, Pont, Bjarni, Pothast, Mart, Privitera, Paolo, Prouza, Michael, Puyleart, Andrew, Querchfeld, Sven, Rautenberg, Julian, Ravignani, Diego, Reininghaus, Maximilian, Ridky, Jan, Riehn, Felix, Risse, Markus, Rizi, Vincenzo, Rodrigues De Carvalho, Washington, Rodriguez Rojo, Jorge Rub��n, Roncoroni, Mat��as J., Rossoni, Simone, Roth, Markus, Roulet, Esteban, Rovero, Adrian, Ruehl, Philip, Saftoiu, Alexandra, Salamida, Francesco, Salazar, Humberto Ibarguen, Salina, Gaetano, Sanabria Gomez, Jose, S��nchez, Federico Andr��s, Santos, Edivaldo Moura, Santos, Eva, Sarazin, Fred, Sarmento, Raul, Sarmiento-Cano, Christian, Sato, Ricardo, Savina, Pierpaolo, Sch��fer, Christoph M., Scherini, Viviana, Schieler, Harald, Schimassek, Martin, Schimp, Michael, Schl��ter, Felix, Schmidt, David, Scholten, Olaf, Schovanek, Petr, Schr��der, Frank G., Schr��der, Sonja, Schulte, Josina, Sciutto, Sergio, Scornavacche, Marina, Segreto, Alberto, Sehgal, Srijan, Shellard, Ronald C., Sigl, Guenter, Silli, Gaia, Sima, Octavian, Smida, Radomir, Sommers, Paul, Soriano, Jorge F., Souchard, Julien, Squartini, Ruben, Stadelmaier, Maximilian, Stanca, Denis, Stani��, Samo, Stasielak, Jaroslaw, Stassi, Patrick, Streich, Alexander, Su��rez-Dur��n, Mauricio, Sudholz, Tristan, Suomijarvi, Tiina, Supanitsky, A. Daniel, Szadkowski, Zbigniew, Tapia, Alex, Taricco, Carla, Timmermans, Charles, Tkachenko, Olena, Tobiska, Petr, Todero Peixoto, Carlos J., Tom��, Bernardo, Torr��s, Zo��, Travaini, Andres, Travnicek, Petr, Trimarelli, Caterina, Tueros, Matias, Ulrich, Ralf, Unger, Michael, Vaclavek, Luk��, Vacula, Martin, Vald��s Galicia, Jose F., Valore, Laura, Varela, Enrique, V��squez-Ram��rez, Adriana, Veberic, Darko, Ventura, Cynthia, Vergara Quispe, Indira D., Verzi, Valerio, Vicha, Jakub, Vink, Jacco, Vorobiov, Serguei, Wahlberg, Hernan, Watanabe, Clara Keiko Oliveira, Watson, Alan, Weber, Marc, Weindl, Andreas, Wiencke, Lawrence, Wilczy��ski, Henryk, Wirtz, Marcus, Wittkowski, David, Wundheiler, Brian, Yushkov, Alexey, Zapparrata, Orazio, Zas, Enrique, Zavrtanik, Danilo, Zavrtanik, Marko, and Zehrer, Lukas
Subjects: Outreach, Pierre Auger Observatory, Engineering, business.industry, Astronomy, Experimental High Energy Physics, Library science, High Energy Physics, ddc:620, business, Engineering & allied operations
Abstract: Contains fulltext : 249220.pdf (Publisher’s version ) (Open Access)

11. Editorial for the Special Issue 'Relativistic Astrophysics'

Author: Achille Nucita, Alexander Zakharov, Francesco De Paolis, DE PAOLIS, Francesco, Nucita, Achille A., and Zakharov, Alexander F.
Subjects: n/a, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Instrumentation and Methods for Astrophysics, Elementary particle physics, General Physics and Astronomy, QC793-793.5, Physics::History of Physics
Abstract: Relativistic Astrophysics is the branch of astrophysics that studies astronomical phenomena and celestial bodies, for which classical mechanics and Newton’s law of gravitation are inapplicable to creation of suitable models and we have to generalize these approaches following general relativistic prescriptions [...]
Published: 2022
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12. Predictions on the detection of the free-floating planet population with K2 and spitzer microlensing campaigns

Author: Mimoza Hafizi, Lindita Hamolli, A. A. Nucita, F. De Paolis, Hamolli, L., DE PAOLIS, Francesco, Hafizi, M., and Nucita, Achille
Subjects: Einstein ring, Microlensing, Population, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Gravitational microlensing, 01 natural sciences, law.invention, Telescope, symbols.namesake, Bulge, Planet, law, 0103 physical sciences, education, 010303 astronomy & astrophysics, Instrumentation, Astrophysics::Galaxy Astrophysics, Physics, education.field_of_study, 010308 nuclear & particles physics, Astronomy, Astronomy and Astrophysics, Galaxy, Orbit, symbols, Astrophysics::Earth and Planetary Astrophysics
Abstract: The K2’s Campaign 9 (K2C9) by the Kepler satellite for microlensing observations towards the Galactic bulge started on April 7, 2016, and is going to last for about three months. It offers the first chance to measure the masses of members of the large population of the isolated dark low-mass objects further away in our Galaxy, free-floating planets (FFPs). Intentionally, this observational period of K2 will overlap with that of the 2016 Spitzer follow-up microlensing project expected to start in June, 2016. Therefore, for the first time it is going to be possible to observe simultaneously the same microlensing events from a ground-based telescope and two satellites. This will help in removing the two-fold degeneracy of the impact parameter and in estimating the FFP mass, provided that the angular Einstein ring radius ΘE is measured. In this paper we calculate the probability that a microlensing event is detectable by two or more telescopes and study how it depends on the mass function index of FFPs and the position of the observers on the orbit.
Published: 2017
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13. Estimating Finite Source Effects in Microlensing Events due to Free-Floating Planets with the Euclid Survey

Author: Lindita Hamolli, Achille A. Nucita, Mimoza Hafizi, Francesco De Paolis, Hamolli, Lindita, Hafizi, Mimoza, DE PAOLIS, Francesco, and Nucita, Achille
Subjects: Earth and Planetary Astrophysics (astro-ph.EP), Physics, Photosphere, Article Subject, lcsh:Astronomy, Microlensing, FOS: Physical sciences, Astronomy, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Gravitational microlensing, Einstein radius, lcsh:QB1-991, Stars, Space and Planetary Science, Observatory, Planet, Bulge, Range (statistics), Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Galaxy Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract: In recent years free-loating planets (FFPs) have drawn a great interest among astrophysicists. Gravitational microlensing is a unique and exclusive method for their investigation which may allow obtaining precious information about their mass and spatial distribution. The planned Euclid space-based observatory will be able to detect a substantial number of microlensing events caused by FFPs towards the Galactic bulge. Making use of a synthetic population algorithm, we investigate the possibility of detecting finite source effects in simulated microlensing events due to FFPs. We find a significant efficiency for finite source effect detection that turns out to be between 20% and 40% for a FFP power law mass function index in the range [0.9, 1.6]. For many of such events it will also be possible to measure the angular Einstein radius and therefore constrain the lens physical parameters. These kinds of observations will also offer a unique possibility to investigate the photosphere and atmosphere of Galactic bulge stars., Comment: 8 pages, 5 figures, published in Advances in Astronomy, Volume 2015, Article ID 402303
Published: 2015
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14. XMM-Newton observation of MV Lyr and the sandwiched model confirmation

Author: Shin Mineshige, A. Dobrotka, A. A. Nucita, Jan-Uwe Ness, Dobrotka, A., Ness, J. U., Mineshige, S., and Nucita, Achille
Subjects: astro-ph.HE, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), astro-ph.SR, 010308 nuclear & particles physics, Astrophysics::High Energy Astrophysical Phenomena, White dwarf, FOS: Physical sciences, Astronomy and Astrophysics, Plasma, Astrophysics, Cooling flow, Light curve, 01 natural sciences, Spectral line, Wavelength, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, 0103 physical sciences, Emission spectrum, Astrophysics - High Energy Astrophysical Phenomena, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Power density
Abstract: We present spectral and timing analyses of simultaneous X-ray and UV observations of the VY Scl system MV Lyr taken by XMM-Newton, containing the longest continuous X-ray+UV light curve and highest signal-to-noise X-ray (EPIC) spectrum to date. The RGS spectrum displays emission lines plus continuum, confirming model approaches to be based on thermal plasma models. We test the sandwiched model based on fast variability that predicts a geometrically thick corona that surrounds an inner geometrically thin disc. The EPIC spectra are consistent with either a cooling flow model or a 2-T collisional plasma plus Fe emission lines in which the hotter component may be partially absorbed which would then originate in a central corona or a partially obscured boundary layer, respectively. The cooling flow model yields a lower mass accretion rate than expected during the bright state, suggesting an evaporated plasma with a low density, thus consistent with a corona. Timing analysis confirms the presence of a dominant break frequency around log(f/Hz) = -3 in the X-ray Power Density Spectrum (PDS) as in the optical PDS. The complex soft/hard X-ray light curve behaviour is consistent with a region close to the white dwarf where the hot component is generated. The soft component can be connected to an extended region. We find another break frequency around log(f/Hz) = -3.4 that is also detected by Kepler. We compared flares at different wavelengths and found that the peaks are simultaneous but the rise to maximum is delayed in X-rays with respect to UV., Comment: 17 pages, 21 figures, 4 tables, Accepted for publication in MNRAS
Published: 2017
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15. The puzzling source IGR J17361–4441 in NGC 6388: a possible planetary tidal disruption event

Author: F. De Paolis, A. Segreto, Giuseppe Lodato, Jay Farihi, L. Manni, A. A. Nucita, M. Del Santo, G. De Cesare, M., Del Santo, Nucita, Achille, G., Lodato, Manni, Luigi, DE PAOLIS, Francesco, J., Farihi, G., De Cesare, and A., Segreto
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), Physics, general [White dwarfs], Astrophysics::High Energy Astrophysical Phenomena, Milky Way, FOS: Physical sciences, White dwarf, Astronomy, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Type (model theory), Light curve, Luminosity, Tidal disruption event, Space and Planetary Science, Intermediate-mass black hole, Globular cluster, NGC 6388 [Globular Clusters], Astrophysics::Earth and Planetary Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics::Galaxy Astrophysics
Abstract: On 2011 August 11, INTEGRAL discovered the hard X-ray source IGR J17361-4441 near the centre of the globular cluster NGC 6388. Follow up observations with Chandra showed the position of the transient was inconsistent with the cluster dynamical centre, and thus not related to its possible intermediate mass black hole. The source showed a peculiar hard spectrum (Gamma \approx 0.8) and no evidence of QPOs, pulsations, type-I bursts, or radio emission. Based on its peak luminosity, IGR J17361-4441 was classified as a very faint X-ray transient, and most likely a low-mass X-ray binary. We re-analysed 200 days of Swift/XRT observations, covering the whole outburst of IGR J17361-4441 and find a t^{-5/3} trend evident in the light curve, and a thermal emission component that does not evolve significantly with time. We investigate whether this source could be a tidal disruption event, and for certain assumptions find an accretion efficiency epsilon \approx 3.5E-04 (M_{Ch}/M) consistent with a massive white dwarf, and a disrupted minor body mass M_{mb}=1.9E+27(M/M_{Ch}) g in the terrestrial-icy planet regime. These numbers yield an inner disc temperature of the order kT_{in} \approx 0.04 keV, consistent with the blackbody temperature of kT_{in} \approx 0.08 keV estimated by spectral fitting. Although the density of white dwarfs and the number of free-floating planets are uncertain, we estimate the rate of planetary tidal disruptions in NGC 6388 to be in the range 3E-06 to 3E-04 yr^{-1}. Averaged over the Milky Way globular clusters, the upper limit value corresponds to 0.05 yr^{-1}, consistent with the observation of a single event by INTEGRAL and Swift., Comment: Accepted for publication in Monthly Notices of the Royal Astronomical Society Main Journal on 2014 July 16; 9 pages, 5 figures. Added references; corrected typos
Published: 2014
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16. Signatures of rotating binaries in microlensing experiments

Author: G. Ingrosso, M. Giordano, A. A. Nucita, F. De Paolis, Nucita, Achille, Giordano, Mose', DE PAOLIS, Francesco, and Ingrosso, Gabriele
Subjects: Physics, Orbital elements, Oscillation, Exoplanets, FOS: Physical sciences, Binary number, Astronomy and Astrophysics, Astrophysics, Gravitational microlensing, Orbital period, Light curve, Astrophysics - Astrophysics of Galaxies, law.invention, Lens (optics), Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, law, Astrophysics of Galaxies (astro-ph.GA), Orbital motion, Solar and Stellar Astrophysics (astro-ph.SR)
Abstract: Gravitational microlensing offers a powerful method with which to probe a variety of binary-lens systems, as the binarity of the lens introduces deviations from the typical (single-lens) Paczy\'nski behaviour in the event light curves. Generally, a static binary lens is considered to fit the observed light curve and, when the orbital motion is taken into account, an oversimplified model is usually employed. In this paper, we treat the binary-lens motion in a realistic way and focus on simulated events that are fitted well by a Paczy\'nski curve. We show that an accurate timing analysis of the residuals (calculated with respect to the best-fitting Paczy\'nski model) is usually sufficient to infer the orbital period of the binary lens. It goes without saying that the independently estimated period may be used to further constrain the orbital parameters obtained by the best-fitting procedure, which often gives degenerate solutions. We also present a preliminary analysis of the event OGLE-2011-BLG-1127 / MOA-2011-BLG-322, which has been recognized to be the result of a binary lens. The period analysis results in a periodicity of \simeq 12 days, which confirms the oscillation of the observed data around the best-fitting model. The estimated periodicity is probably associated with an intrinsic variability of the source star, and therefore there is an opportunity to use this technique to investigate either the intrinsic variability of the source or the effects induced by the binary-lens orbital motion., Comment: In press on MNRAS, 2014. 8 pages, 4 figures. On-line material available on the Journal web-page
Published: 2014
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17. Planck confirmation of the disk and halo rotation of M 31

Author: Daniele Vetrugno, Vahe Gurzadyan, Asghar Qadir, H. G. Khachatryan, S. Mirzoyan, A. A. Nucita, F. De Paolis, A. L. Kashin, Ph. Jetzer, G. Ingrosso, E. Poghosian, DE PAOLIS, Francesco, V. G., Gurzadyan, Nucita, Achille, Ingrosso, Gabriele, A. L., Kashin, H. G., Khachatryan, S., Mirzoyan, E., Poghosian, Jetzer, P. h., A., Qadir, and Vetrugno, Daniele
Subjects: Physics, 010308 nuclear & particles physics, media_common.quotation_subject, Cosmic microwave background, Local Group, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Rotation, 01 natural sciences, Asymmetry, CMB cold spot, Galaxy, symbols.namesake, Space and Planetary Science, 0103 physical sciences, symbols, Galactic halos, Halo, Planck, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, media_common
Abstract: Planck data acquired during the first 15.4 months of observations toward both the disk and halo of the M 31 galaxy were analyzed. We confirm the temperature asymmetry that was previously detected by using the seven-year WMAP data in the direction of the rotation of M 31, which indicates that this is a Doppler-induced effect. The asymmetry extends to about 10° (≃130 kpc) from the center of M 31. We also investigated the recent problem raised in Rubin and Loeb (2014, JCAP, 01, 051) about the kinetic Sunyaev-Zel’dovich effect from the diffuse hot gas in the Local Group, which is predicted to generate a hot spot of a few degrees in size in the cosmic microwave background maps in the direction of M 31, where the free electron optical depth is highest. We also considered whether the same effect in the opposite direction with respect to the M 31 galaxy induces a minimum in temperature in the Planck maps of the sky. We find that the Planck data at 100 GHz show an even stronger effect than that expected.
Published: 2014
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18. The Scales of Gravitational Lensing

Author: M. Giordano, G. Ingrosso, Francesco Strafella, Francesco De Paolis, L. Manni, A. A. Nucita, DE PAOLIS, Francesco, Giordano, Mose', Ingrosso, Gabriele, Manni, Luigi, Nucita, Achille, and Strafella, Francesco
Subjects: lcsh:QC793-793.5, Angular momentum, Cosmology and Nongalactic Astrophysics (astro-ph.CO), General relativity, Milky Way, gravitational lensing, General Physics and Astronomy, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Cosmology, 0103 physical sciences, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Physics, Supermassive black hole, 010308 nuclear & particles physics, lcsh:Elementary particle physics, Physics::History of Physics, Galaxy, Gravitational lens, Astrophysics - Solar and Stellar Astrophysics, Dark energy, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: After exactly a century since the formulation of the general theory of relativity, the phenomenon of gravitational lensing is still an extremely powerful method for investigating in astrophysics and cosmology. Indeed, it is adopted to study the distribution of the stellar component in the Milky Way, to study dark matter and dark energy on very large scales and even to discover exoplanets. Moreover, thanks to technological developments, it will allow the measure of the physical parameters (mass, angular momentum and electric charge) of supermassive black holes in the center of ours and nearby galaxies., Comment: 22 pages, 10 figures. Invited review for Universe
Published: 2016
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19. Parallax and orbital effects in astrometric microlensing with binary sources

Author: G. Ingrosso, F. De Paolis, L. Manni, M. Giordano, A. A. Nucita, Nucita, Achille, DE PAOLIS, Francesco, Ingrosso, Gabriele, Giordano, Mose', and Manni, Luigi
Subjects: Physics, 010308 nuclear & particles physics, Astrophysics::Instrumentation and Methods for Astrophysics, Binary number, FOS: Physical sciences, Astronomy and Astrophysics, Astrometry, Astrophysics, Gravitational microlensing, Light curve, 01 natural sciences, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Position (vector), microlensing, astrometry, 0103 physical sciences, Orbital motion, Caustic (optics), Astrophysics::Earth and Planetary Astrophysics, Parallax, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Solar and Stellar Astrophysics (astro-ph.SR)
Abstract: In gravitational microlensing, binary systems may act as lenses or sources. Identifying lens binarity is generally easy especially in events characterized by caustic crossing since the resulting light curve exhibits strong deviations from smooth single-lensing light curve. On the contrary, light curves with minor deviations from a Paczy\'nski behaviour do not allow one to identify the source binarity. A consequence of the gravitational microlensing is the shift of the position of the multiple image centroid with respect to the source star location - the so called astrometric microlensing signal. When the astrometric signal is considered, the presence of a binary source manifests with a path that largely differs from that expected for single-source events. Here, we investigate the astrometric signatures of binary sources taking into account their orbital motion and the parallax effect due to the Earth motion, which turn out not to be negligible in most cases. We also show that considering the above-mentioned effects is important in the analysis of astrometric data in order to correctly estimate the lens-event parameters., Comment: Published on ApJ, 2016, 823, 120
Published: 2016
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20. Constraints on parameters of dark matter and black hole in the Galactic Center

Author: G. Ingrosso, F. De Paolis, A. A. Nucita, Alexander F. Zakharov, A. F., Zakharov, DE PAOLIS, Francesco, Ingrosso, Gabriele, and Nucita, Achille
Subjects: Physics, Nuclear and High Energy Physics, General relativity, Milky Way, Galactic Center, Dark matter, Astronomy, Astrophysics, Cosmological constant, Atomic and Molecular Physics, and Optics, Galaxy, Gravitation, Black hole, Galactic center (Sgr A*), Astrophysics::Galaxy Astrophysics
Abstract: A concept of dark matter (DM) is introduced. As for other anomalies, we describe two ways to solve DM problem, namely a conservative way when we have to ﬁnd substances with DM properties or we have to change a fundamental gravity law. We discuss constraints on DM concentration near the Galactic Center from apocenter shift data.
Published: 2010
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21. M31 PIXEL LENSING EVENT OAB-N2: A STUDY OF THE LENS PROPER MOTION

Author: I. Bruni, G. Ingrosso, Massimo Dall'Ora, Ph. Jetzer, Andrew Gould, F. De Paolis, R. Gualandi, Mauro Sereno, Gaetano Scarpetta, V. Bozza, A. A. Nucita, S. Calchi Novati, Luigi Mancini, Francesco Strafella, Martin Dominik, University of Zurich, Calchi Novati, S, Calchi Novati, S., Dall'Ora, M., Gould, A., Bozza, V., Bruni, I., DE PAOLIS, Francesco, Dominik, M., Gualandi, R., Ingrosso, Gabriele, Jetzer, P. h., Mancini, L., Nucita, Achille, Scarpetta, G., Sereno, M., and Strafella, Francesco
Subjects: Proper motion, 530 Physics, materia oscura, NGC 224) – Galaxy: halo – gravitational lensing: micro, FOS: Physical sciences, individuali: M31 NGC 224 [galassie], Astrophysics, Parameter space, halo [Galassia], Lower limit, dark matter – galaxies: halos – galaxies: individual (M31, Photometry (optics), 1912 Space and Planetary Science, Settore FIS/05 - Astronomia e Astrofisica, aloni [galassie], micro [lensing gravitazionale], Physics, Pixel, Astronomy and Astrophysics, Astrometry, Light curve, Astrophysics - Astrophysics of Galaxies, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), 10231 Institute for Computational Science, 3103 Astronomy and Astrophysics
Abstract: We present an updated analysis of the M31 pixel lensing candidate event OAB-N2 previously reported in Calchi Novati et al. (2009). Here we take advantage of new data both astrometric and photometric. Astrometry: using archival 4m-KPNO and HST/WFPC2 data we perform a detailed analysis on the event source whose result, although not fully conclusive on the source magnitude determination, is confirmed by the following light curve photometry analysis. Photometry: first, unpublished WeCAPP data allows us to confirm OAB-N2, previously reported only as a viable candidate, as a well constrained pixel lensing event. Second, this photometry enables a detailed analysis in the event parameter space including the effects due to finite source size. The combined results of these analyses allow us to put a strong lower limit on the lens proper motion. This outcome favors the MACHO lensing hypothesis over self lensing for this individual event and points the way toward distinguishing between the MACHO and self-lensing hypotheses from larger data sets., Accepted for publication in ApJ - minor changes to match the accepted version - Figure 1 updated
Published: 2010
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22. Pixel lensing as a way to detect extrasolar planets in M31

Author: Alexander F. Zakharov, Ph. Jetzer, S. Calchi Novati, Achille A. Nucita, G. Ingrosso, F. De Paolis, University of Zurich, Ingrosso, G, Ingrosso, Gabriele, Calchi Novati, S., DE PAOLIS, Francesco, Jetzer, P. h., Nucita, Achille, and Zakharov, A. F.
Subjects: 530 Physics, gravitational lensing, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Gravitational microlensing, Jupiter, 1912 Space and Planetary Science, Planet, halo [Galaxy], Astrophysics::Galaxy Astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Earth and Planetary Astrophysics (astro-ph.EP), Physics, Order (ring theory), Astronomy and Astrophysics, Giant star, Light curve, Exoplanet, Galaxy: halo, M31 [galaxies], Astrophysics - Solar and Stellar Astrophysics, galaxies: individual: M31, Space and Planetary Science, 10231 Institute for Computational Science, 3103 Astronomy and Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Planetary mass, Astrophysics - Earth and Planetary Astrophysics
Abstract: We study the possibility to detect extrasolar planets in M31 through pixel-lensing observations. Using a Monte Carlo approach, we select the physical parameters of the binary lens system, a star hosting a planet, and we calculate the pixel-lensing light curve taking into account the finite source effects. Indeed, their inclusion is crucial since the sources in M31 microlensing events are mainly giant stars. Light curves with detectable planetary features are selected by looking for significant deviations from the corresponding Paczy\'{n}ski shapes. We find that the time scale of planetary deviations in light curves increase (up to 3-4 days) as the source size increases. This means that only few exposures per day, depending also on the required accuracy, may be sufficient to reveal in the light curve a planetary companion. Although the mean planet mass for the selected events is about $2 M_{\rm {Jupiter}}$, even small mass planets ($M_{\rm P} < 20 M_{\oplus}$) can cause significant deviations, at least in the observations with large telescopes. However, even in the former case, the probability to find detectable planetary features in pixel-lensing light curves is at most a few percent of the detectable events, and therefore many events have to be collected in order to detect an extrasolar planet in M31. Our analysis also supports the claim that the anomaly found in the candidate event PA-99-N2 towards M31 can be explained by a companion object orbiting the lens star., Comment: Accepted for publication on Monthly Notices of the Royal Astronomical Society (MNRAS), 2009
Published: 2009
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23. A serendipitous XMM-Newton observation of MACHO 104.20906.960: A dwarf nova candidate with a 2 h period

Author: F. De Paolis, S. Carpano, B. M. T. Maiolo, A. A. Nucita, Matteo Guainazzi, G. Ingrosso, Nucita, Achille, Carpano, S, DE PAOLIS, Francesco, Ingrosso, Gabriele, Maiolo, BERLINDA MARIA TERESA, and Guainazzi, M.
Subjects: Physics, general [White dwarfs], general [Binaries], Astronomy, Flux, White dwarf, Binary number, Astronomy and Astrophysics, Astrophysics, Orbital period, Luminosity, Space and Planetary Science, Bulge, Primary (astronomy), Instrumentation, Dwarf nova
Abstract: The binaries known as cataclysmic variables are particular binary systems in which the primary star (a white dwarf) accretes material from a secondary via Roche-lobe mechanism. Usually, these objects have orbital period of a few hours so that a detailed temporal analysis can be performed. Here, we present Chandra and XMM-Newton observations of a dwarf nova candidate identified in the past by optical observations towards the galactic Bulge and labeled as MACHO 104.20906.960. After a spectral analysis, we used the Lomb-Scargle technique for the period search and evaluated the confidence level using Monte-Carlo simulations. In this case, we found that the X-ray source shows a period of 2.03 - 0.07 + 0.09 h ( 3 σ error) so that it is most likely a system of interacting objects. The modulation of the signal was found with a confidence level of > 99 % . The spectrum can be described by a two thermal plasma components with X-ray flux in the 0.3–10 keV energy band of 1.77 - 0.19 + 0.16 × 10 - 13 erg s - 1 cm - 2 . We find that the distance of the source is approximately 1 kpc thus corresponding to a luminosity L X ≃ 2 × 10 31 erg s - 1 .
Published: 2009
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24. XMM-Newton and Chandra observations of the globular cluster NGC 6388

Author: G. Ingrosso, S. Carpano, Achille A. Nucita, Matteo Guainazzi, F. De Paolis, Nucita, Achille, DE PAOLIS, Francesco, Ingrosso, Gabriele, S., Carpano, and M., Guainazzi
Subjects: Physics, Astrophysics::High Energy Astrophysical Phenomena, Astronomy, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Compact star, Luminosity, Black hole, symbols.namesake, Star cluster, Space and Planetary Science, Globular cluster, Eddington luminosity, symbols, Astrophysics::Solar and Stellar Astrophysics, globular clusters [Galaxy], Surface brightness, Low Mass, Astrophysics::Galaxy Astrophysics
Abstract: Context. By studying the optical brightness surface density of the globular cluster NGC 6388, it has been recently proposed that it harbors a central intermediate-mass black hole with mass ≃5.7 x 10 3 M ⊙ . Aims. We expect that the compact object in the center of NGC 6388 emits radiation in the X-ray band as a consequence of the accretion from the surrounding matter. We searched for XMM-Newton and Chandra observations towards NGC 6388 to test this hypothesis. Methods. We determine both the hardness ratios and luminosity with a minimum set of assumptions for each of the identified field sources. Results. The Chandra satellite disentangles several point-like X-ray sources, probably low mass X-ray binaries, well within the core radius of the globular cluster. However, three of them, coinciding with the cluster center of gravity, remain unresolved. Their total luminosity is L Obs X ≃ 2.7 x 10 33 erg s -1 . If one of these sources is the X-ray counterpart of the intermediate-mass black hole in NGC 6388, the corresponding upper limit on the accretion efficiency, with respect to the Eddington luminosity, is 3 x 10 -9 . This measurement could be tightened if moderately deep radio observations of the field were performed.
Published: 2007
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25. XMM observation of 1RXS J180431.1-273932: a new M-type X-ray binary with a 494 s-pulse period neutron star?

Author: S. Carpano, Matteo Guainazzi, Achille A. Nucita, Nucita, Achille, Carpano, S., and Guainazzi, M.
Subjects: Physics, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), X-ray binary, FOS: Physical sciences, Astronomy and Astrophysics, Context (language use), Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Compact star, Giant star, Luminosity, Neutron star, Apparent magnitude, Pulsar, Space and Planetary Science, Astrophysics::Solar and Stellar Astrophysics
Abstract: Low-mass X-ray binaries are binary systems composed of a compact object and a low-mass star. Recently, a new class of these systems, known as symbiotic $X$-ray binaries (with a neutron star with a M-type giant companion), has been discovered. Here, we present long-duration ${\it XMM}$ observations of the source 1RXS J180431.1-273932. Temporal and spectral analysis of the source was performed along with a search for an optical counterpart. We used a Lomb-Scargle periodogram analysis for the period search and evaluated the confidence level using Monte-Carlo simulations. The source is characterized by regular pulses so that it is most likely a neutron star. A modulation of $494.1\pm0.2$ s (3$\sigma$ error) was found with a confidence level of $>$99%. Evidence of variability is also present, since the data show a rate of change in the signal of $\sim -7.7\times 10^{-4}$ counts s$^{-1}$ hr$^{-1}$. A longer observation will be necessary in order to determine if the source shows any periodic behavior. The spectrum can be described by a power law with photon index $\Gamma\sim 1$ and a Gaussian line at 6.6 keV. The X-ray flux in the 0.2--10 keV energy band is $5.4\times 10^{-12}$ erg s$^{-1}$ cm$^{-2}$. The identification of an optical counterpart (possibly an M6III red-giant star with an apparent visual magnitude of $\simeq 17.6$) allows a conservative distance of $\sim 10$ kpc to be estimated. Other possibilities are also discussed. Once the distance was estimated, we got an $X$-ray luminosity of $L_X\ut, Comment: in press on A&A
Published: 2007
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26. Starspot induced effects in microlensing events with rotating source star

Author: A. A. Nucita, G. Ingrosso, M. Giordano, F. De Paolis, Giordano, Mose', Nucita, Achille, DE PAOLIS, Francesco, and Ingrosso, Gabriele
Subjects: Physics, Gravitational Lensing, Starspot, Astronomy, Binary number, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Star (graph theory), Light curve, Rotation, Gravitational microlensing, law.invention, Lens (optics), Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, law, Orbital motion, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Galaxy Astrophysics, Solar and Stellar Astrophysics (astro-ph.SR)
Abstract: We consider the effects induced by the presence of hot and cold spots on the source star in the light curves of simulated microlensing events due to either single or binary lenses taking into account the rotation of the source star and the orbital motion of the lens system. Our goal is to study the anomalies induced by these effects on simulated microlensing light curves., Comment: 5 pages, 2 figures, accepted for publication in MNRAS
Published: 2015
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27. AnXMM‐NewtonSearch for X‐Ray Emission from the Microlensing Event MACHO‐96‐BLG‐5

Author: Davide Elia, J. de Plaa, A. A. Nucita, Jelle Kaastra, G. Ingrosso, F. De Paolis, Nucita, Achille, DE PAOLIS, Francesco, Ingrosso, Gabriele, Elia, Davide Quintino, DE PLAA, J, and Kaastra, J. S.
Subjects: Physics, Absolute magnitude, Astrophysics::High Energy Astrophysical Phenomena, Astronomy, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Black hole physics, Gravitational microlensing, Galaxy, Accretion (astrophysics), Interstellar medium, Black hole, Stars, Space and Planetary Science, Bulge, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: MACHO-96-BLG-5 was a microlensing event observed toward the bulge of the Galaxy with an exceptionally long duration of ~970 days. The microlensing parallax fit parameters were used to estimate a lens mass M = 6 M☉, corresponding to a distance d in the range 0.5-2 kpc. The upper limit on the absolute brightness for main-sequence stars of the same mass is less than 1 L☉, so the lens is a good black hole candidate. Such a black hole would accrete from the interstellar medium, thereby emitting in the X-ray band. Here we report the analysis of a deep XMM-Newton observation toward the MACHO-96-BLG-5 lens position. Only an upper limit (99.8% confidence level) to the X-ray flux from the lens position, 9.10 × 10-15 to 1.45 × 10-14 ergs cm-2 s-1 in the 0.2-10 keV energy band, is obtained, allowing us to constrain the putative black hole's accretion parameters.
Published: 2006
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28. Measuring the black hole parameters in the galactic center with RADIOASTRON

Author: F. DePaolis, Alexander F. Zakharov, A. A. Nucita, G. Ingrosso, ZAKHAROV A., F, Nucita, Achille, DE PAOLIS, Francesco, and Ingrosso, Gabriele
Subjects: Physics, Gravitational lense, Astrophysics::High Energy Astrophysical Phenomena, Microlensing, Astronomy and Astrophysics, Astrophysics, Black hole, Black hole physic, General Relativity and Quantum Cosmology, Rotating black hole, Binary black hole, Space and Planetary Science, Extremal black hole, Stellar black hole, Spin-flip, Instrumentation, Schwarzschild radius, Ring singularity
Abstract: Recently Holz & Wheeler (2002) considered a very attracting possibility to detect retro-MACHOs, i.e. retro-images of the Sun by a Schwarzschild black hole. In this paper we discuss glories (mirages) formed near rapidly rotating Kerr black hole horizons and propose a procedure to measure masses and rotation parameters analyzing these forms of mirages. In some sense that is a manifestation of gravitational lens effect in the strong gravitational field near black hole horizon and a generalization of the retro-gravitational lens phenomenon. We analyze the case of a Kerr black hole rotating at arbitrary speed for some selected positions of a distant observer with respect to the equatorial plane of a Kerr black hole. We discuss glories (mirages) formed near rapidly rotating Kerr black hole horizons and propose a procedure to measure masses and rotation parameters analyzing these forms of mirages. Some time ago Falcke et al. (2000) suggested to search shadows at the Galactic Center. In this paper we present the boundaries for shadows calculated numerically. We also propose to use future radio interferometer RADIOASTRON facilities to measure shapes of mirages (glories) and to evaluate the black hole spin as a function of the position angle of a distant observer.
Published: 2005
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29. Influence of magnification threshold on pixel lensing optical depth, event rate and time scale distributions towards M 31

Author: Alexander F. Zakharov, F. De Paolis, G. Ingrosso, A. A. Nucita, DE PAOLIS, Francesco, Ingrosso, Gabriele, Nucita, Achille, and Zakharov, A. F.
Subjects: Physics, Newtonian telescope, Astrophysics (astro-ph), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Gravitational microlensing, Luminosity, law.invention, Stars, Space and Planetary Science, law, Optical depth (astrophysics), Halo, Impact parameter, Event (particle physics), Astrophysics::Galaxy Astrophysics
Abstract: Pixel lensing is the gravitational microlensing of light from unresolved stars contributing to the luminosity flux collected by a single pixel. A star must be sufficiently magnified, that is, the lens impact parameter must be less than a threshold value $u_T$ if the excess photon flux in a pixel is to be detected over the background. Assuming the parameters of the Isaac Newton Telescope and typical observing conditions, we present maps in the sky plane towards M31 of threshold impact parameter, optical depth, event number and event time scale, analyzing in particular how these quantities depend on $u_T$ in pixel lensing searches. We use an analytical approach consisting of averaging on $u_T$ and the star column density the optical depth, microlensing rate and event duration time scale. An overall decrease in the expected optical depth and event number with respect to the classical microlensing results is found, particularly towards the high luminosity M31 inner regions. As expected, pixel lensing events towards the inner region of M31 are mostly due to self-lensing, while in the outer region dark events dominate even for a 20% MACHO halo fraction. We also find a far-disk/near-disk asymmetry in the expected event number, smaller than that found by \cite{Kerins04}. Both for self and dark lensing events, the pixel lensing time scale we obtain is $\simeq 1 - 7$ days, dark events lasting roughly twice as long as self-lensing events. The shortest events are found to occur towards the M31 South Semisphere. We also note that the pixel lensing results depend on $$ and $$ values and ultimately on the observing conditions and telescope capabilities., Comment: Appeared on A&A 432, 501, 2005. Low resolution black and white figures
Published: 2005
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30. A super massive black hole binary in 3C 66B: Future observational perspectives

Author: F. De Paolis, G. Ingrosso, A. A. Nucita, DE PAOLIS, Francesco, Ingrosso, Gabriele, and Nucita, Achille
Subjects: Physics, Supermassive black hole, Active galactic nucleus, Radio galaxy, Gravitational wave, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), FOS: Physical sciences, Binary number, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Black hole physics, Light curve, Galaxy, binary black hole, Space and Planetary Science, Very-long-baseline interferometry, Astrophysics::Galaxy Astrophysics
Abstract: Supermassive black hole binaries (SMBHBs) may exist in the centers of galaxies and active galactic nuclei (AGN) and are expected to be fairly common in the Universe as a consequence of merging processes between galaxies. The existence of SMBHBs can be probed by looking for double nuclei in galaxy centers or, more easily, detecting periodic behavior in the observed radio light curves. In a recent paper, Sudou et al. \cite{sudou2003} announced the first direct observation of an SMBHB. Using VLBI observations they found that the unresolved radio core of the radio galaxy 3C66B shows a well defined elliptical motion with a period of $1.05\pm 0.03$ yrs, implying the presence of a couple of massive black holes in the center of the galaxy. In the present paper we study the astrophysical implications of the existence of such an SMBHB in 3C66B. In particular we focus on the information that can be obtained from detecting a signal periodicity either in the $X$-ray and/or $\gamma$-ray light curves as a consequence of the motion of the black holes. These observations could be used to extract further information on the physical parameters of the SMBHB and partially solve the system parameter degeneracy. The detection of the gravitational wave spectrum emitted by such system may be used to completely determine the physical parameters of the binary system., Comment: 8 pages, 8 figures, in Press on Astronomy & Astrophysics
Published: 2004
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31. M31 Pixel Lensing PLAN Campaign: MACHO Lensing and Self Lensing Signals

Author: Massimo Dall'Ora, Ph. Jetzer, Annapurni Subramaniam, S. Calchi Novati, Francesco Strafella, Martin Dominik, Mauro Sereno, G. Ingrosso, Valerio Bozza, A. A. Nucita, Luigi Mancini, Margarita Safonova, Andrew Gould, F. De Paolis, Gaetano Scarpetta, R. Gualandi, Ivan Bruni, University of Zurich, The Royal Society, University of St Andrews. School of Physics and Astronomy, S., Calchi Novati, V., Bozza, I., Bruni, M., Dall'Ora, DE PAOLIS, Francesco, M., Dominik, R., Gualandi, Ingrosso, Gabriele, Jetzer, P. h., L., Mancini, Nucita, Achille, M., Safonova, G., Scarpetta, M., Sereno, Strafella, Francesco, A., Subramaniam, A., Gould, S. Calchi Novati, V. Bozza, I. Bruni, M. Dall'Ora, F. De Paoli, M. Dominik, R. Gualandi, G. Ingrosso, Ph. Jetzer, L. Mancini, A. Nucita, M. Safonova, G. Scarpetta, M. Sereno, F. Strafella, A. Subramaniam, and A. Gould
Subjects: 530 Physics, Milky Way, astro-ph.GA, Dark matter, FOS: Physical sciences, NGC 224), Galaxy: halo, gravitational lensing: micro, 10192 Physics Institute, Gravitational microlensing, 01 natural sciences, law.invention, micro [Gravitational lensing], Telescope, Galactic halo, Settore FIS/05 - Astronomia e Astrofisica, 1912 Space and Planetary Science, law, Observatory, individual (M31, NGC 224) [Galaxies], 0103 physical sciences, dark matter, galaxies: halos, galaxies: individual ( M31, halo [Galaxy], QB Astronomy, 010303 astronomy & astrophysics, QC, QB, Physics, 010308 nuclear & particles physics, Astronomy, Astronomy and Astrophysics, halos galaxies: indiv [Galaxies], Astrophysics - Astrophysics of Galaxies, Dark matter halo, Stars, QC Physics, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), 3103 Astronomy and Astrophysics
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 during 4 years (2007-2010) at the 1.5m Cassini telescope in Loiano ("Astronomical Observatory of BOLOGNA", OAB) plus 10 days of data taken in 2010 at the 2m Himalayan Chandra Telescope (HCT) monitoring the central part of M31 (two fields of about 13'x12.6'). We establish a fully automated pipeline for the search and the characterization of microlensing flux variations: as a result we detect 3 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 the M31 and the Milky Way (MW), respectively. The total number of events is compatible with the expected self-lensing rate. Specifically, we evaluate an expected signal of about 2 self-lensing events. As for MACHO lensing, for full 0.5 (0.01) solar mass MACHO halos, our prediction is for about 4 (7) events. The comparatively small number of expected MACHO versus self lensing events, together with the small number statistics at 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 solar mass MACHOs., Comment: ApJ accepted, 13 pages, 5 figures, 2 tables
Published: 2014
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32. Exoplanetary searches with gravitational microlensing: polarization issues

Author: Francesco De Paolis, Francesco Strafella, Alexander F. Zakharov, Philippe Jetzer, A. A. Nucita, G. Ingrosso, Sebastiano Calchi Novati, A. F., Zakharov, Ingrosso, Gabriele, DE PAOLIS, Francesco, Nucita, Achille, Strafella, Francesco, S., Calchi Novati, Jetzer, P. h., University of Zurich, and Zakharov, Alexander F
Subjects: Atmospheric Science, 530 Physics, Astronomical unit, Polarimetry, Aerospace Engineering, FOS: Physical sciences, 10192 Physics Institute, Astrophysics, General Relativity and Quantum Cosmology (gr-qc), Gravitational microlensing, General Relativity and Quantum Cosmology, symbols.namesake, 1912 Space and Planetary Science, 2202 Aerospace Engineering, Planet, Polarization, 1902 Atmospheric Science, 1908 Geophysics, Solar and Stellar Astrophysics (astro-ph.SR), Physics, Earth and Planetary Astrophysics (astro-ph.EP), Brewster's angle, 1900 General Earth and Planetary Sciences, Stellar atmosphere, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, Astronomy and Astrophysics, Polarization (waves), Astrophysics - Astrophysics of Galaxies, Exoplanet, Extrasolar planets, Geophysics, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), symbols, 3103 Astronomy and Astrophysics, General Earth and Planetary Sciences, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract: There are different methods for finding exoplanets such as radial spectral shifts, astrometrical measurements, transits, timing etc. Gravitational microlensing (including pixel-lensing) is among the most promising techniques with the potentiality of detecting Earth-like planets at distances about a few astronomical units from their host star or near the so-called snow line with a temperature in the range $0-100^0$ C on a solid surface of an exoplanet. We emphasize the importance of polarization measurements which can help to resolve degeneracies in theoretical models. In particular, the polarization angle could give additional information about the relative position of the lens with respect to the source., Comment: 17 pages, 3 figures, presented at the IX Serbian Conference on Spectral Lines in Astrophysics and the COST Action MP1104 "Polarization as a tool to study the Solar System and beyond", accepted for publication in Advances in Space Research
Published: 2013
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33. Polarization in binary microlensing events

Author: Ph. Jetzer, G. Ingrosso, S. Calchi Novati, Francesco Strafella, A. A. Nucita, Giuliano Liuzzi, F. De Paolis, Alexander F. Zakharov, Ingrosso, Gabriele, DE PAOLIS, Francesco, Nucita, Achille, Strafella, Francesco, S., Calchi Novati, Ph, Jetzer, Liuzzi, Giuliano, and A., Zakharov
Subjects: Physics, Internal cavity, Stellar atmosphere, Binary number, FOS: Physical sciences, Observable, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Gravitational microlensing, Condensed Matter Physics, Polarization (waves), Giant star, Astrophysics - Astrophysics of Galaxies, Atomic and Molecular Physics, and Optics, Stars, Astrophysics - Solar and Stellar Astrophysics, Polarization, Astrophysics of Galaxies (astro-ph.GA), Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Mathematical Physics, Astrophysics::Galaxy Astrophysics, Solar and Stellar Astrophysics (astro-ph.SR)
Abstract: The light received by source stars in microlensing events may be significantly polarized if both an efficient photon scattering mechanism is active in the source stellar atmosphere and a differential magnification is therein induced by the lensing system. The best candidate events for observing polarization are highly magnified events with source stars belonging to the class of cool, giant stars {in which the stellar light is polarized by photon scattering on dust grains contained in their envelopes. The presence in the stellar atmosphere of an internal cavity devoid of dust produces polarization profiles with a two peaks structure. Hence, the time interval between them gives an important observable quantity directly related to the size of the internal cavity and to the model parameters of the lens system.} We show that {during a microlensing event} the expected polarization variability can solve an ambiguity, that arises in some cases, related to the binary or planetary lensing interpretation of the perturbations observed near the maximum of the event light-curve. We consider a specific event case for which the parameter values corresponding to the two solutions are given. Then, assuming a polarization model for the source star, we compute the two expected polarization profiles. The position of the two peaks appearing in the polarization curves and the characteristic time interval between them allow us to distinguish between the binary and planetary lens solutions., Comment: In press on Physica Scripta (IOPscience), 2013
Published: 2013
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34. Optical identification of X-ray source 1RXS J180431.1-273932 as a magnetic cataclysmic variable

Author: N. Masetti, Pietro Parisi, A. A. Nucita, Masetti, N., Nucita, Achille, and Parisi, P.
Subjects: Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Red giant, Astrophysics::High Energy Astrophysical Phenomena, Bremsstrahlung, Balmer series, Cataclysmic variable star, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Compact star, Luminosity, symbols.namesake, Neutron star, Intermediate polar, Space and Planetary Science, symbols, Astrophysics - High Energy Astrophysical Phenomena
Abstract: The X-ray source 1RXS J180431.1-273932 has been proposed as a new member of the symbiotic X-ray binary (SyXB) class of systems, which are composed of a late-type giant that loses matter to an extremely compact object, most likely a neutron star. In this paper, we present an optical campaign of imaging plus spectroscopy on selected candidate counterparts of this object. We also reanalyzed the available archival X-ray data collected with XMM-Newton. We find that the brightest optical source inside the 90% X-ray positional error circle is spectroscopically identified as a magnetic cataclysmic variable (CV), most likely of intermediate polar type, through the detection of prominent Balmer, He I, He II, and Bowen blend emissions. On either spectroscopic or statistical grounds, we discard as counterparts of the X-ray source the other optical objects in the XMM-Newton error circle. A red giant star of spectral type M5 III is found lying just outside the X-ray position: we consider this latter object as a fore-/background one and likewise rule it out as a counterpart of 1RXS J180431.1-273932. The description of the X-ray spectrum of the source using a bremsstrahlung plus black-body model gives temperatures of around 40 keV and around 0.1 keV for these two components, respectively. We estimate a distance of about 450 pc and a 0.2-10 keV X-ray luminosity of about 1.7e32 erg/s for this system and, using the information obtained from the X-ray spectral analysis, a mass of about 0.8 solar masses for the accreting white dwarf (WD). We also confirm an X-ray periodicity of 494 s for this source, which we interpret as the spin period of the WD. In summary, 1RXS J180431.1-273932 is identified as a magnetic CV and its SyXB nature is excluded., Comment: 9 pages, 7 figures, 3 tables, accepted for publication on Astronomy & Astrophysics, main journal. Version 2 includes the A&A Language Editor's corrections
Published: 2012
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35. High resolution spectroscopy as a tool to study line emitting material in AGNs

Author: A. A. Nucita, M. Guainazzi, A. L. Longinotti, G. Risaliti, M. Santos-Lleo, S. Bianchi, A. Comastri, L. Angelini, M. Cappi, Nucita, Achille, Guainazzi, M., Longinotti, A. L., Santos Lleo, M., Maruccia, Ylenia, and Bianchi, S.
Subjects: Physics, X-ray spectroscopy, X-ray, Astronomy, High resolution, Astrophysics, Galactic nuclei, Spectroscopy, Galaxy, Line (formation)
Abstract: High resolution spectroscopy is acquiring increasing importance in the study of AGNs. We discuss the results on three Seyfert galaxies (Mrk 335, NGC 4051, and NGC 1365).
Published: 2010
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36. The nuclear environment of Radio Galaxies: what’s new

Author: E. Torresi, P. Grandi, A. L. Longinotti, M. Guainazzi, F. Tombesi, A. Nucita, A. Comastri, L. Angelini, M. Cappi, A. Comastri, INAF-OABO L. Angelini, GSFC/NASA M. Cappi, INAF-IASF, Torresi, E., Grandi, P., Longinotti, A. L., Guainazzi, M., Tombesi, F., and Nucita, Achille
Subjects: Physics, Settore FIS/05 - Astronomia e Astrofisica, Radio galaxy, Astrophysics::High Energy Astrophysical Phenomena, Astronomy, Astrophysics::Cosmology and Extragalactic Astrophysics, Plasma, Astrophysics, Galactic nuclei, Nuclear environment, Astrophysics::Galaxy Astrophysics, Galaxy, Accretion (astrophysics)
Abstract: While in Radio–Quiet (RQ) AGN warm gas photoionised by the nuclear engine has been well revealed and studied in X‐rays, it is still unclear whether a similar gaseous environment can survive in Radio–Loud (RL) objects. The exploration of the environment surrounding the nuclei of RL sources is an important point to be addressed. It can help to understand the physical link among accretion flows, winds and jet, and the influence that each component can have on the host galaxy. We report on the recent discovery of warm gas in RL AGN, indicating that relativistic collimated plasma (jet) and slower outflows of photoionised gas can coexist in the same source. The physical properties of this gas seem to be very similar to RQ ones, suggesting that RL and RQ AGN environment becomes indistinguishable at large distances from the central engine (e.g. the Narrow Line Region).
Published: 2010
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37. AGN/starburst connection in action: the half million second RGS spectrum of NGC1365

Author: Guido Risaliti, Roberto Soria, Junzhi Wang, Andreas Zezas, Matteo Guainazzi, Achille A. Nucita, Stefano Bianchi, M., Guainazzi, G., Risaliti, Nucita, Achille, J., Wang, S., Bianchi, R., Soria, A., Zezas, Guainazzi, M, Risaliti, G, Nucita, A, Wang, J, Bianchi, Stefano, Soria, R, and Zezas, A.
Subjects: galaxie [X-rays], Active galactic nucleus, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics::High Energy Astrophysical Phenomena, Doubly ionized oxygen, FOS: Physical sciences, Photoionization, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Seyfert [galaxies], Ionization, medicine, Astrophysics::Galaxy Astrophysics, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Star formation, starburst [galaxies], Astronomy and Astrophysics, Galaxy, Accretion (astrophysics), medicine.anatomical_structure, Space and Planetary Science, active [galaxies], NGC+1365<%2FASTROBJ>+[X-rays]%22">individuals: NGC 1365 [X-rays], Astrophysics - High Energy Astrophysical Phenomena, Nucleus, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present a deep (~5.8 days) 0.3-2 keV high-resolution spectrum of NGC1365, collected with the reflection grating spectrometer (RGS) on board XMM-Newton. The spectrum is dominated by strong recombination lines of He- and H-like transitions from carbon to silicon, as well as by L transitions from FeXVII. The continuum is strong, especially in the 10 to 20 Angstrom, range. Formal fits require two optically thin, collisionally ionised plasma components, with temperatures ~300 and ~640 eV. However, they leave the bulk of the forbidden components of the He-alpha OVII and NVI triplets unaccounted for. These features can be explained as being produced by photoionised gas. NGC1365 is therefore the first obscured AGN, whose high-resolution X-ray spectrum requires both collisional ionisation and photoionisation. The relative weakness of photoionisation does not stem from the intrinsic weakness of its AGN, whose X-ray luminosity is ~10^{42} erg/s. We suggest that it may instead come from the line-of-sight from the active nucleus to the NLR being blocked by optically thick matter in the broad line region, at the same time responsible for the large observed variation of the column density obscuring the X-ray active nucleus. Alternatively, NGC1365 could host a remarkably luminous nuclear starburst when compared to the AGN accretion power [abriged]., Comment: Accepted for publication in Astronomy & Astrophysics, 13 pages, 10 figures
Published: 2009
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38. GENERAL RELATIVITY (PLUS DARK MATTER AND DARK ENERGY) OR ALTERNATIVE THEORIES OF GRAVITY

Author: A. A. Nucita, G. Ingrosso, F. De Paolis, V. N. Pervushin, Alexander F. Zakharov, H. Volker Klapdor-Kleingrothaus, G. F. Lewis, A. F., Zakharov, V. N., Pervushin, Nucita, Achille, DE PAOLIS, Francesco, and Ingrosso, Gabriele
Subjects: Physics, General relativity, Hot dark matter, Dark matter, Scalar field dark matter, Lambda-CDM model, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Physics::History of Physics, General relativity and gravitation, Theoretical physics, Doubly special relativity, Dark energy, Dark fluid
Abstract: One could call 2006 as the year of cosmology since in the year two US scientists were awarded by the Nobel prize for their studies of Cosmic Microwave Back-ground (CMB) spectrum and anisotropy. Studies of CMB anisotropy done with the Soviet spacecraft Prognoz-9 by the Relikt-1 team are reminded. Problems of modern cosmology are outlined. We discuss conformal cosmology parameters from supernovae data in brief. Two approaches to solve the basic problems of cosmology, such as dark matter and dark energy, are discussed, the first (standard) possibility is to introduce new particles, fields etc, the second possibility is to try to change a gravity law to fit observational data. We discuss advantages and disadvantages of the second choice.
Published: 2008
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39. Dark matter and dark energy or alternative theories of gravity and cosmology

Author: Alexander F. Zakharov, Victor N. Pervushin, Francesco De Paolis, Gabriele Ingrosso, Achille A. Nucita, Carlo Luciano Bianco, She-Sheng Xue, ZAKHAROV A., F, PERVUSHIN V., N, DE PAOLIS, Francesco, Ingrosso, Gabriele, and Nucita, Achille
Subjects: Physics, Hot dark matter, Dark matter, Scalar field dark matter, Dark energy, Astronomy, Lambda-CDM model, Non-standard cosmology, Astrophysics::Cosmology and Extragalactic Astrophysics, Dark fluid, Physical cosmology
Abstract: One could call 2006 as the year of cosmology since in the year two US scientists were awarded by the Nobel prize for their studies of Cosmic Microwave Background (CMB) spectrum and anisotropy. Studies of CMB anisotropy done with the Soviet spacecraft Prognoz‐9 by the Relikt‐1 team are reminded. Problems of modern cosmology are outlined. We discuss conformal cosmology parameters from supernovae data in brief. Two approaches to solve the basic problems of cosmology, such as dark matter and dark energy, are discussed, the first (standard) possibility is to introduce new particles, fields etc, the second possibility is to try to change a gravity law to fit observational data. We discuss advantages and disadvantages of the second choice.
Published: 2008
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40. The Seyfert 1 Galaxy Mrk 335 at a very low flux state: mapping the soft X-ray photoionised gas

Author: Achille A. Nucita, M. Santos-Lleo, Anna Lia Longinotti, Matteo Guainazzi, Longinotti, A. L., Nucita, Achille, Santos Lleo, M., and Guainazzi, M.
Subjects: Physics, Soft x ray, Electron density, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), High resolution, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Plasma, Astrophysics::Cosmology and Extragalactic Astrophysics, Galaxy, Ion, Space and Planetary Science, Ionization, Target of opportunity, Astrophysics::Galaxy Astrophysics
Abstract: This paper reports on an XMM-Newton observation of the Seyfert 1 Galaxy Mrk 335 performed as a Target of Opportunity when the source was in an unusually low flux state. The low level of continuum emission unveiled an underlying line-rich soft X-ray spectrum, which can be studied with the Reflection Grating Spectrometer. The emission features have been analysed at high resolution with unprecedented detail for this source. Line ratios diagnostic from H-like and He-like ions indicates that the line emission arises in X-ray photoionised plasma. Extensive simulations have been performed with the CLOUDY photoionisation code. From the comparison of the expected and observed line intensities the physical properties of the line emitting material were derived. Because of the degeneracy in the ionisation parameter, a number of different solutions in terms of electron density and column density of the gas are consistent with the spectral diagnostics. This prevents us from determining uniquely the properties of the plasma; however, the location(s) of the X-ray photoionised gas can be constrained to be within 0.06 pc (outer boundary). This limit places the X-ray line emitting gas at the inner edge of the material where the broad optical lines are produced (Broad Line Region)., Comment: Accepted on A&A on 07/03/2008, final version after proofs, typos corrected, fig 4 replaced
Published: 2008
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41. Gravitational wave scintillation by a stellar cluster

Author: G. CONGEDO, F. DE PAOLIS, P. LONGO, A. A. NUCITA, D. VETRUGNO, ASGHAR QADIR, Congedo, G, DE PAOLIS, Francesco, Longo, P, Nucita, Achille, Vetrugno, D, and Qadir, A.
Subjects: Diffraction, Physics, Scintillation, Gravitational wave, Astrophysics (astro-ph), Physics::Optics, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Observer (physics), Intensity (physics), General Relativity and Quantum Cosmology, gravitational waves, Space and Planetary Science, Cluster (physics), Mathematical Physics, Fresnel diffraction
Abstract: The diffraction effects on gravitational waves propagating through a stellar cluster are analyzed in the relevant approximation of Fresnel diffraction limit. We find that a gravitational wave scintillation effect - similar to the radio source scintillation effect - comes out naturally, implying that the gravitational wave intensity changes in a characteristic way as the observer moves., Comment: 9 pages, in press in IJMP D
Published: 2006
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42. Solar system constraints on R$^n$ gravity

Author: Achille A. Nucita, G. Ingrosso, Alexander F. Zakharov, F. De Paolis, ZAKHAROV A., F, Nucita, Achille, DE PAOLIS, Francesco, and Ingrosso, Gabriele
Subjects: Physics, Nuclear and High Energy Physics, Gravity (chemistry), Astrophysics (astro-ph), FOS: Physical sciences, Newtonian limit, Astrophysics, Surface gravity, Gravitational microlensing, General relativity and gravitation, Newtonian dynamics, Gravitation, General Relativity and Quantum Cosmology, Classical mechanics, Gravitational field, Gravity well, Astrophysics::Earth and Planetary Astrophysics
Abstract: Recently, gravitational microlensing has been investigated in the framework of the weak field limit of fourth order gravity theory. However, solar system data (i.e. planetary periods and light bending) can be used to put strong constraints on the parameters of this class of gravity theories. We find that these parameters must be very close to those corresponding to the Newtonian limit of the theory., Comment: in press on Phys. Rev. D
Published: 2006
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43. XMM-NewtonandSwiftobservations of WZ Sagittae: spectral and timing analysis

Author: G. Ingrosso, F. De Paolis, Koji Mukai, A. A. Nucita, B. M. T. Maiolo, E. Kuulkers, Nucita, Achille, E., Kuulker, DE PAOLIS, Francesco, K., Mukai, Ingrosso, Gabriele, and Maiolo, BERLINDA MARIA TERESA
Subjects: Swift, Physics, Spectral shape analysis, binarie [X-rays], Astrophysics::High Energy Astrophysical Phenomena, White dwarf, Flux, white warfs [Stars], Astronomy and Astrophysics, Context (language use), Astrophysics, Light curve, Luminosity, Space and Planetary Science, Astrophysics::Solar and Stellar Astrophysics, Low Mass, computer, computer.programming_language
Abstract: Context. WZ Sagittae is the prototype object of a subclass of dwarf novae with rare and long (super)outbursts, in which a white dwarf primary accretes matter from a low mass companion. High-energy observations offer the possibility of a better understanding of the disk-accretion mechanism in WZ Sge-like binaries. Aims. We used archival XMM-Newton and Swift data to characterize the X-ray spectral and temporal properties of WZ Sge in quiescence. Methods. We performed a detailed timing analysis of the simultaneous X-ray and UV light curves obtained with the EPIC and OM instruments on board XMM-Newton in 2003. We employed several techniques in this study, including a correlation study between the two curves. We also performed an X-ray spectral analysis using the EPIC data and Swift/XRT data obtained in 2011. Results. We find that the X-ray intensity is clearly modulated at a period of � 28.96 s, confirming previously published preliminary results. We find that the X-ray spectral shape of WZ Sge remains practically unchanged between the XMM-Newton and Swift observations. However, after correcting for interstellar absorption, the intrinsic luminosity is estimated to be L Una = (2.65± 0.06) × 10 30 erg s −1 and L Una = (1.57 ± 0.03) × 10 30 erg s −1 in 2003 and 2011, respectively. During the Swift/XRT observation, the observed flux is a factor � 2 lower than that observed by XMM-Newton but is similar to the quiescent levels that are observed various times before the 2001 outburst.
Published: 2014
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44. The puzzling symbiotic X-ray system 4U1700+24

Author: A. A. Nucita, G. Ingrosso, S. Stefanelli, N. Masetti, L. Manni, M. Del Santo, F. De Paolis, Nucita, Achille, S., Stefanelli, DE PAOLIS, Francesco, N., Masetti, Ingrosso, Gabriele, M., Del Santo, and Manni, Luigi
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), Physics, general [White dwarfs], Red giant, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, symbiotic system, Light curve, Spectral line, Luminosity, Neutron star, Space and Planetary Science, Astrophysics::Solar and Stellar Astrophysics, Black-body radiation, Roche lobe, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics::Galaxy Astrophysics, Line (formation)
Abstract: Symbiotic X-ray binaries form a subclass of low-mass X-ray binary systems consisting of a neutron star accreting material from a red giant donor star via stellar wind or Roche lobe overflow. Only a few confirmed members are currently known; 4U 1700+24 is a good candidate as it is a relatively bright X-ray object, possibly associated with the late-type star V934 Her. We analysed the archive {\it XMM}-Newton and Swift/XRT observations of 4U 1700+24 in order to have a uniform high-energy ($0.3-10$ keV) view of the source. We confirmed the existence of a red-shifted O VIII Ly-$\alpha$ transition (already observed in the 2002 {\it XMM}-Newton data) in the high-resolution spectra collected via the RGS instruments. The red-shift of the line is found in all the analysed observations and, on average, it was estimated to be $\simeq 0.009$. We also observed a modulation of the centroid energy of the line on short time scales (a few days) and discuss the observations in the framework of different scenarios. If the modulation is due to the gravitational red-shift of the neutron star, it might arise from a sudden re-organization of the emitting $X$-ray matter on the scale of a few hundreds of km. Alternatively, we are witnessing a uni-polar jet of matter (with typical velocity of $1000-4000$ km s$^{-1}$) possibly emitted by the neutron star in an almost face-on system. The second possibility seems to be required by the apparent lack of any modulation in the observed $X$-ray light curve. We also note also that the low-resolution spectra (both {\it XMM}-Newton and Swift/XRT in the $0.3-10$ keV band) show the existence of a black body radiation emitted by a region (possibly associated with the neutron star polar cap) with typical size from a few tens to hundreds of meters. The size of this spot-like region reduces as the overall luminosity of 4U 1700+24 decreases., Comment: In press on A&A
Published: 2014
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45. GRAVITATIONAL WAVES AND EVOLUTION TIMESCALES OF RELATIVISTIC CLUSTERS

Author: G. Ingrosso, F. De Paolis, A. A. Nucita, V.G. Gurzadyan, R. Ruffini, Nucita, Achille, DE PAOLIS, Francesco, and Ingrosso, Gabriele
Subjects: Physics, Gravitational-wave observatory, Gravitational wave, Astronomy, relativistic clusters, Astrophysics, gravitational wave, Gravitational energy, Gravitational redshift
Published: 2000
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46. A THEORETICAL CALCULATION OF MICROLENSING SIGNATURES CAUSED BY FREE-FLOATING PLANETS TOWARDS THE GALACTIC BULGE

Author: Achille A. Nucita, Mimoza Hafizi, Lindita Hamolli, L., Hamolli, M., Hafizi, and Nucita, Achille
Subjects: Earth and Planetary Astrophysics (astro-ph.EP), Physics, Dark matter, Astrophysics::Instrumentation and Methods for Astrophysics, Brown dwarf, FOS: Physical sciences, Astronomy, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Gravitational microlensing, Galactic halo, Space and Planetary Science, Observatory, Bulge, Planet, Astrophysics::Earth and Planetary Astrophysics, Parallax, Astrophysics::Galaxy Astrophysics, Mathematical Physics, Astrophysics - Earth and Planetary Astrophysics
Abstract: Free-floating planets are recently drawing a special interest of the scientific community. Gravitational microlensing is up to now the exclusive method for the investigation of free-floating planets, including their spatial distribution function and mass function. In this work, we examine the possibility that the future Euclid space-based observatory may allow to discover a substantial number of microlensing events caused by free-floating planets. Based on latest results about the free-floating planet mass function in the mass range $[10^{-5}, 10^{-2}]M_{\odot}$, we calculate the optical depth towards the Galactic bulge as well as the expected microlensing rate and find that Euclid may be able to detect hundreds to thousands of these events per month. Making use of a synthetic population, we also investigate the possibility of detecting parallax effect in simulated microlensing events due to free-floating planets and find a significant efficiency for the parallax detection that turns out to be around 30%., Comment: Paper published in IJMPD 22, 1350072, 2013; 14 pages, 3 tables, 3 figures
Published: 2013
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47. TheXMM-Newtonview of the eclipse and dips of the dwarf nova Z Chamaleontis

Author: Daniele Vetrugno, G. Ingrosso, E. Kuulkers, B. M. T. Maiolo, F. De Paolis, A. A. Nucita, Nucita, Achille, E., Kuulker, Maiolo, BERLINDA MARIA TERESA, DE PAOLIS, Francesco, Ingrosso, Gabriele, and Vetrugno, Daniele
Subjects: cataclysmic variable, Physics, Astronomy, White dwarf, Cataclysmic variable star, Astronomy and Astrophysics, Astrophysics, Light curve, Luminosity, Space and Planetary Science, Bolometric correction, Roche lobe, novae [stars], Dwarf nova, Eclipse
Abstract: Context. A cataclysmic variable contains a white dwarf that accretes material from a secondary star via the Roche lobe mechanism. Systems with high line-of-sight inclination angles offer the possibility to pinpoint the location of the X-ray emitting region by characterizing the observed eclipse by the secondary star. Aims: We present an XMM-Newton observation of the dwarf nova Z Chamaleontis that we analyzed to determine the properties of the X-ray and optical light curves, as well as the high-energy spectrum. Methods: We performed a spectral analysis of the data taken by the EPIC camera, and a timing analysis of the observed X-ray and optical OM light curves. Results: We find that a multi-temperature plasma component absorbed by ionized material is required to describe the data. In particular, we estimate that the total absorbed flux in the 0.2-9.0 keV band is FAbs0.2-9.0 = (4.1±0.1) × 10-12 erg s-1 cm-2, which, when accounted for absorption and bolometric correction, corresponds to a bolometric luminosity of LBolX = (6.9±0.1) × 1030 erg s-1 at a distance of 97 pc. The mass accretion rate onto the white dwarf turns out to be about 1.1 × 10-11Msun yr-1. Our analysis of the optical and X-ray eclipse light curves and the mid-eclipse times of Z-Chamaleontis, in addition to the eclipse (during which the observed EPIC count rate is 0.033 ± 0.003 count s-1), implies that the X-ray light curve contains dips (at the orbital phases 0.30 ± 0.02 and 0.73 ± 0.02) that can be naturally explained as absorption effects by intervening stable gas clouds close to the accretor.
Published: 2011
Full Text: View/download PDF

48. SMBHBS as relics of galaxy encounters: The 3C66B example

Author: Paolis, F., Ingrosso, G., Achille Nucita, A. Wilson, DE PAOLIS, Francesco, Ingrosso, Gabriele, and Nucita, Achille
Subjects: 3C66B [Galaxies], Massive Black Hole
Abstract: Supermassive black hole binaries (SMBHBs) may exist in the centers of galaxies. These systems may be revealed by periodic behavior in the observed light curves. Sudou et al. (2003) announced the observation of an SMBHB in the radio galaxy 3C66B whose core shows a defined elliptical motion with a period of ~1 yr. Here, we focus on the information on the SMBHB parameters that can be obtained by X-ray, γ-ray and radio observations. In particular, future ALMA observations will help in further constraining the 3C66B SMBHB orbital parameters.

49. Downward Terrestrial Gamma-ray Flashes at the Pierre Auger Observatory?

Author: Colalillo, R., Abreu, P., Aglietta, M., Albury, J. M., Allekotte, I., Almela, A., Alvarez-Muñiz, J., Alves Batista, R., Anastasi, G. A., Anchordoqui, L., Andrada, B., Andringa, S., Aramo, C., Araújo Ferreira, P. R., Arteaga Velázquez, J. C., Asorey, H., Assis, P., Avila, G., Badescu, A. M., Bakalova, A., Balaceanu, A., Barbato, F., Barreira Luz, R. J., Becker, K. H., Bellido, J. A., Berat, C., Bertaina, M. E., Bertou, X., Biermann, P. L., Binet, V., Bismark, K., Bister, T., Biteau, J., Blazek, J., Bleve, C., Boháčová, M., Boncioli, D., Bonifazi, C., Bonneau Arbeletche, L., Borodai, N., Botti, A. M., Brack, J., Bretz, T., Brichetto Orchera, P. G., Briechle, F. L., Buchholz, P., Bueno, A., Buitink, S., Buscemi, M., Büsken, M., Caballero-Mora, K. S., Caccianiga, L., Canfora, F., Caracas, I., Carceller, J. M., Caruso, R., Castellina, A., Catalani, F., Cataldi, G., Cazon, L., Cerda, M., Chinellato, J. A., Chudoba, J., Chytka, L., Clay, R. W., Cobos Cerutti, A. C., Coleman, A., Coluccia, M. R., Ruben Conceição, Condorelli, A., Consolati, G., Contreras, F., Convenga, F., Correia Dos Santos, D., Covault, C. E., Dasso, S., Daumiller, K., Dawson, B. R., Day, J. A., Almeida, R. M., Jesús, J., Jong, S. J., Mauro, G., Mello Neto, J. R. T., Mitri, I., Oliveira, J., Oliveira Franco, D., Palma, F., Souza, V., Vito, E., Del Río, M., Deligny, O., Deval, L., Di Matteo, A., Dobrigkeit, C., D’olivo, J. C., Domingues Mendes, L. M., Dos Anjos, R. C., Dos Santos, D., Dova, M. T., Ebr, J., Engel, R., Epicoco, I., Erdmann, M., Escobar, C. O., Etchegoyen, A., Falcke, H., Farmer, J., Farrar, G., Fauth, A. C., Fazzini, N., Feldbusch, F., Fenu, F., Fick, B., Figueira, J. M., Filipčič, A., Fitoussi, T., Fodran, T., Freire, M. M., Fujii, T., Fuster, A., Galea, C., Galelli, C., García, B., Garcia Vegas, A. L., Gemmeke, H., Gesualdi, F., Gherghel-Lascu, A., Ghia, P. L., Giaccari, U., Giammarchi, M., Glombitza, J., Gobbi, F., Gollan, F., Golup, G., Gómez Berisso, M., Gómez Vitale, P. F., Gongora, J. P., González, J. M., González, N., Goos, I., Góra, D., Gorgi, A., Gottowik, M., Grubb, T. D., Guarino, F., Guedes, G. P., Guido, E., Hahn, S., Hamal, P., Hampel, M. R., Hansen, P., Harari, D., Harvey, V. M., Haungs, A., Hebbeker, T., Heck, D., Hill, G. C., Hojvat, C., Hörandel, J. R., Horvath, P., Hrabovský, M., Huege, T., Insolia, A., Isar, P. G., Janecek, P., Johnsen, J. A., Jurysek, J., Kääpä, A., Kampert, K. H., Karastathis, N., Keilhauer, B., Kemp, J., Khakurdikar, A., Kizakke Covilakam, V. V., Klages, H. O., Kleifges, M., Kleinfeller, J., Köpke, M., Kunka, N., Lago, B. L., Lang, R. G., Langner, N., Leigui Oliveira, M. A., Lenok, V., Letessier-Selvon, A., Lhenry-Yvon, I., Lo Presti, D., Lopes, L., López, R., Lu, L., Luce, Q., Lundquist, J. P., Machado Payeras, A., Mancarella, G., Mandat, D., Manning, B. C., Manshanden, J., Mantsch, P., Marafico, S., Mariazzi, A. G., Mariş, I. C., Marsella, G., Martello, D., Martinelli, S., Martínez Bravo, O., Mastrodicasa, M., Mathes, H. J., Matthews, J., Matthiae, G., Mayotte, E., Mazur, P. O., Medina-Tanco, G., Melo, D., Menshikov, A., Merenda, K. -D, Michal, S., Micheletti, M. I., Miramonti, L., Mollerach, S., Montanet, F., Morello, C., Mostafá, M., Müller, A. L., Muller, M. A., Mulrey, K., Mussa, R., Muzio, M., Namasaka, W. M., Nasr-Esfahani, A., Nellen, L., Niculescu-Oglinzanu, M., Niechciol, M., Nitz, D., Nosek, D., Novotny, V., Nožka, L., Nucita, A., Núñez, L. A., Palatka, M., Pallotta, J., Papenbreer, P., Parente, G., Parra, A., Pawlowsky, J., Pech, M., Pedreira, F., Pȩkala, J., Pelayo, R., Peña-Rodriguez, J., Pereira Martins, E. E., Perez Armand, J., Pérez Bertolli, C., Perlin, M., Perrone, L., Petrera, S., Pierog, T., Pimenta, M., Pirronello, V., Platino, M., Pont, B., Pothast, M., Privitera, P., Prouza, M., Puyleart, A., Querchfeld, S., Rautenberg, J., Ravignani, D., Reininghaus, M., Ridky, J., Riehn, F., Risse, M., Rizi, V., Rodrigues Carvalho, W., Rodriguez Rojo, J., Roncoroni, M. J., Rossoni, S., Roth, M., Roulet, E., Rovero, A. C., Ruehl, P., Saftoiu, A., Salamida, F., Salazar, H., Salina, G., Sanabria Gomez, J. D., Sánchez, F., Santos, E. M., Santos, E., Sarazin, F., Sarmento, R., Sarmiento-Cano, C., Sato, R., Savina, P., Schäfer, C. M., Scherini, V., Schieler, H., Schimassek, M., Schimp, M., Schlüter, F., Schmidt, D., Scholten, O., Schovánek, P., Schröder, F. G., Schröder, S., Schulte, J., Sciutto, S. J., Scornavacche, M., Segreto, A., Sehgal, S., Shellard, R. C., Sigl, G., Silli, G., Sima, O., Šmída, R., Sommers, P., Soriano, J. F., Souchard, J., Squartini, R., Stadelmaier, M., Stanca, D., Stanič, S., Stasielak, J., Stassi, P., Streich, A., Suárez-Durán, M., Sudholz, T., Suomijärvi, T., Supanitsky, A. D., Szadkowski, Z., Tapia, A., Taricco, C., Timmermans, C., Tkachenko, O., Tobiska, P., Todero Peixoto, C. J., Tomé, B., Torrès, Z., Travaini, A., Travnicek, P., Trimarelli, C., Tueros, M., Ulrich, R., Unger, M., Vaclavek, L., Vacula, M., Valdés Galicia, J. F., Valore, L., Varela, E., Vásquez-Ramírez, A., Veberič, D., Ventura, C., Vergara Quispe, I. D., Verzi, V., Vicha, J., Vink, J., Vorobiov, S., Wahlberg, H., Watanabe, C., Watson, A. A., Weber, M., Weindl, A., Wiencke, L., Wilczyński, H., Wirtz, M., Wittkowski, D., Wundheiler, B., Yushkov, A., Zapparrata, O., Zas, E., Zavrtanik, D., Zavrtanik, M., Zehrer, L., Colalillo, Roberta, Abreu, Pedro, Aglietta, Marco, Albury, Justin M., Allekotte, Ingomar, Almela, Alejandro, Alvarez-Muniz, Jaime, Alves Batista, Rafael, Anastasi, Gioacchino Alex, Anchordoqui, Luis A., Andrada, Belén, Andringa, Sofia, Aramo, Carla, Araújo Ferreira, Paulo Ricardo, Arteaga Velazquez, Juan Carlo, Asorey, Hernán Gonzalo, Assis, Pedro, Avila, Gualberto, Badescu, Alina Mihaela, Bakalova, Alena, Balaceanu, Alexandru, Barbato, Felicia, Barreira Luz, Ricardo Jorge, Becker, Karl-Heinz, Bellido, Jose A., Berat, Corinne, Bertaina, Mario Edoardo, Bertou, Xavier, Biermann, Peter L., Binet, Virginia, Bismark, Kathrin, Bister, Teresa, Biteau, Jonathan, Blazek, Jiri, Bleve, Carla, Bohacova, Martina, Boncioli, Denise, Bonifazi, Carla, Bonneau Arbeletche, Luan, Borodai, Nataliia, Botti, Ana Martina, Brack, Jeffrey, Bretz, Thoma, Brichetto Orchera, P. Gabriel, Briechle, Florian Luka, Buchholz, Peter, Bueno, Antonio, Buitink, Stijn, Buscemi, Mario, Büsken, Max, Caballero-Mora, Karen S., Caccianiga, Lorenzo, Canfora, Fabrizia, Caracas, Ioana, Carceller, Juan Miguel, Caruso, Rossella, Castellina, Antonella, Catalani, Fernando, Cataldi, Gabriella, Cazon, Lorenzo, Cerda, Marco, Chinellato, Jose Augusto, Chudoba, Jiří, Chytka, Ladislav, Clay, Roger W, Cobos Cerutti, Agustín, Coleman, Alan, Coluccia, Maria Rita, Conceição, Rúben, Condorelli, Antonio, Consolati, Giovanni, Contreras, Fernando, Convenga, Fabio, Correia dos Santos, Diego, Covault, Corbin, Dasso, Sergio, Daumiller, Kai, Dawson, Bruce R., Day, Jarryd A., de Almeida, Rogerio M., de Jesús, Joaquín, de Jong, Sijbrand J., De Mauro, Giuseppe, de Mello Neto, João, De Mitri, Ivan, de Oliveira, Jaime, de Oliveira Franco, Danelise, de Palma, Francesco, de Souza, Vitor, De Vito, Emanuele, del Río, Mariano, Deligny, Olivier, Deval, Luca, di Matteo, Armando, Dobrigkeit, Carola, D'Olivo, Juan Carlo, Domingues Mendes, Luis Miguel, dos Anjos, Rita, dos Santos, Diego, Dova, Maria Teresa, Ebr, Jan, Engel, Ralph, Epicoco, Italo, Erdmann, Martin, Escobar, Carlos O., Etchegoyen, Alberto, Falcke, Heino, Farmer, John, Farrar, Glennys R., Fauth, Anderson, Fazzini, Norberto, Feldbusch, Fridtjof, Fenu, Francesco, Fick, Brian, Figueira, Juan Manuel, Filipcic, Andrej, Fitoussi, Thoma, Fodran, Tomáš, Freire, Martín Miguel, Fujii, Toshihiro, Fuster, Alan, Galea, Cristina, Galelli, Claudio, García, Beatriz, García Vegas, Adrianna Luz, Gemmeke, Hartmut, Gesualdi, Flavia, Gherghel-Lascu, Alexandru, Ghia, Piera Luisa, Giaccari, Ugo, Giammarchi, Marco, Glombitza, Jona, Gobbi, Fabian, Gollan, Fernando, Golup, Geraldina, Gómez Berisso, Mariano, Gómez Vitale, Primo F., Gongora, Juan Pablo, González, Juan Manuel, Gonzalez, Nicolas Martin, Goos, Isabel, Gora, Dariusz, Gorgi, Alessio, Gottowik, Marvin, Grubb, Trent D., Guarino, Fausto, Guedes, Germano, Guido, Eleonora, Hahn, Steffen, Hamal, Petr, Hampel, Matías Rolf, Hansen, Patricia María, Harari, Diego, Harvey, Violet M., Haungs, Andrea, Hebbeker, Thoma, Heck, Dieter, Hill, Gary C., Hojvat, Carlo, Hörandel, Jörg, Horvath, Pavel, Hrabovsky, Miroslav, Huege, Tim, Insolia, Antonio, Isar, Paula Gina, Janecek, Petr, Johnsen, Jeffrey A., Juryšek, Jakub, Kääpä, Alex, Kampert, Karl-Heinz, Karastathis, Nikolao, Keilhauer, Bianca, Kemp, Julian, Khakurdikar, Abha, Kizakke Covilakam, Varada Varma, Klages, Han, Kleifges, Matthia, Kleinfeller, Jonny, Köpke, Marcel, Kunka, Norbert, Lago, Bruno L., Lang, Rodrigo Guede, Langner, Nikla, Leigui de Oliveira, Marcelo Augusto, Lenok, Vladimir, Letessier-Selvon, Antoine, Lhenry-Yvon, Isabelle, Lo Presti, Domenico, Lopes, Lui, López, Rebeca, Lu, Lu, Luce, Quentin, Lundquist, Jon Paul, Machado Payeras, Allan, Mancarella, Giovanni, Mandat, Dusan, Manning, Bradley C., Manshanden, Julien, Mantsch, Paul, Marafico, Sullivan, Mariazzi, Analisa, Maris, Ioana Codrina, Marsella, Giovanni, Martello, Daniele, Martinelli, Sara, Martínez Bravo, Oscar, Mastrodicasa, Massimo, Mathes, Hermann-Josef, Matthews, Jame, Matthiae, Giorgio, Mayotte, Eric, Mazur, Peter, Medina-Tanco, Gustavo, Melo, Diego, Menshikov, Alexander, Merenda, Kevin-Drui, Michal, Stanislav, Micheletti, Maria Isabel, Miramonti, Lino, Mollerach, Silvia, Montanet, Françoi, Morello, Carlo, Mostafa, Miguel, Müller, Ana L., Muller, Marcio Aparecido, Mulrey, Katharine, Mussa, Roberto, Muzio, Marco Stein, Namasaka, Wilson M., Nasr-Esfahani, Alina, Nellen, Luka, Niculescu-Oglinzanu, Mihai, Niechciol, Marcu, Nitz, Dave, Nosek, Dalibor, Novotný, Vladimír, Nozka, Libor, Nucita, Achille, Nunez, Luis A., Palatka, Miroslav, Pallotta, Juan, Papenbreer, Philipp, Parente, Gonzalo, Parra, Alejandra, Pawlowsky, Janni, Pech, Miroslav, Pedreira, Francisco, Pękala, Jan, Pelayo, Rodrigo, Peña-Rodríguez, Jesú, Pereira Martins, Edyvania Emily, Perez Armand, Johnnier, Pérez Bertolli, Carmina, Perlin, Matía, Perrone, Lorenzo, Petrera, Sergio, Pierog, Tanguy, Pimenta, Mário, Pirronello, Valerio, Platino, Manuel, Pont, Bjarni, Pothast, Mart, Privitera, Paolo, Prouza, Michael, Puyleart, Andrew, Querchfeld, Sven, Rautenberg, Julian, Ravignani, Diego, Reininghaus, Maximilian, Ridky, Jan, Riehn, Felix, Risse, Marku, Rizi, Vincenzo, Rodrigues de Carvalho, Washington, Rodriguez Rojo, Jorge Rubén, Roncoroni, Matías J., Rossoni, Simone, Roth, Marku, Roulet, Esteban, Rovero, Adrian, Ruehl, Philip, Saftoiu, Alexandra, Salamida, Francesco, Salazar, Humberto Ibarguen, Salina, Gaetano, Sanabria Gomez, Jose, Sánchez, Federico André, Santos, Edivaldo Moura, Santos, Eva, Sarazin, Fred, Sarmento, Raul, Sarmiento-Cano, Christian, Sato, Ricardo, Savina, Pierpaolo, Schäfer, Christoph M., Scherini, Viviana, Schieler, Harald, Schimassek, Martin, Schimp, Michael, Schlüter, Felix, Schmidt, David, Scholten, Olaf, Schovanek, Petr, Schröder, Frank G., Schröder, Sonja, Schulte, Josina, Sciutto, Sergio, Scornavacche, Marina, Segreto, Alberto, Sehgal, Srijan, Shellard, Ronald C., Sigl, Guenter, Silli, Gaia, Sima, Octavian, Smida, Radomir, Sommers, Paul, Soriano, Jorge F., Souchard, Julien, Squartini, Ruben, Stadelmaier, Maximilian, Stanca, Deni, Stanič, Samo, Stasielak, Jaroslaw, Stassi, Patrick, Streich, Alexander, Suárez-Durán, Mauricio, Sudholz, Tristan, Suomijarvi, Tiina, Supanitsky, A. Daniel, Szadkowski, Zbigniew, Tapia, Alex, Taricco, Carla, Timmermans, Charle, Tkachenko, Olena, Tobiska, Petr, Todero Peixoto, Carlos J., Tomé, Bernardo, Torrès, Zoé, Travaini, Andre, Travnicek, Petr, Trimarelli, Caterina, Tueros, Matia, Ulrich, Ralf, Unger, Michael, Vaclavek, Lukáš, Vacula, Martin, Valdés Galicia, Jose F., Valore, Laura, Varela, Enrique, Vásquez-Ramírez, Adriana, Veberic, Darko, Ventura, Cynthia, Vergara Quispe, Indira D., Verzi, Valerio, Vicha, Jakub, Vink, Jacco, Vorobiov, Serguei, Wahlberg, Hernan, Watanabe, Clara Keiko Oliveira, Watson, Alan, Weber, Marc, Weindl, Andrea, Wiencke, Lawrence, Wilczyński, Henryk, Wirtz, Marcu, Wittkowski, David, Wundheiler, Brian, Yushkov, Alexey, Zapparrata, Orazio, Zas, Enrique, Zavrtanik, Danilo, Zavrtanik, Marko, and Zehrer, Lukas
Subjects: Physics, Pierre Auger Observatory, Astronomy, Astrophysics::High Energy Astrophysical Phenomena, Gamma ray, Cosmic ray, Electron, Astrophysics, Lightning, Experimental High Energy Physics, Thunderstorm, High Energy Physics, Atmospheric electricity, ddc:620, Event (particle physics), Engineering & allied operations
Abstract: At the Pierre Auger Observatory, designed primarily to study ultra-high-energy cosmic rays, phenomena related to atmospheric electricity are also observed. Particularly, events have been detected with the surface detector, characterized by long-lasting signals (tens of microseconds) and event footprints much larger (up to 200 km$^2$) than those produced by the highest energy cosmic rays. Moreover, some of them appear to be accompanied by smaller events occurring in the same area within about 1 ms and probably produced by the same phenomenon. A previously reported correlation with the World Wide Lightning Location Network, as well as the observation of very low-altitude clouds, confirm that such events are related to thunderstorms. An ad-hoc reconstruction points to high-energy particles being produced very close to the ground, suggesting that they originate from electrons accelerated to relativistic energies in strong electric fields inside low clouds, as is the case for terrestrial gamma-ray flashes above thunderstorms. A clear explanation of the observed phenomenon is hindered by two facts. One is that the rate of such events, detected serendipitously, is very small (less than 2 events/year) and decreases further after optimization of the surface detector trigger for low-energy shower-events. The second is that most events show a puzzling lack of signals in the central part of the footprint. We have studied in detail both effects and will present such studies here. We developed a strategy for a dedicated trigger to enhance the detection efficiency for these events associated with atmospheric-electricity events.

50. Astrophysical constraints on a possible neutrino ball at the Galactic Center

Author: D. Orlando, A. A. Nucita, Gerardo Iovane, G. Ingrosso, F. De Paolis, Salvatore Capozziello, F., De Paoli, G., Ingrosso, A. A., Nucita, D., Orlando, Capozziello, Salvatore, G., Iovane, DE PAOLIS, Francesco, Ingrosso, Gabriele, Nucita, Achille, Orlando, Daniela, Capozziello, S., and Iovane, G.
Subjects: Physics, Astrophysics::High Energy Astrophysical Phenomena, Galactic Center, Astrophysics (astro-ph), FOS: Physical sciences, Astronomy and Astrophysics, Fermion, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Galaxy, Black hole, Space and Planetary Science, Electron degeneracy pressure, Ball (mathematics), Neutrino, Galactic center (Sgr A*), Astrophysics::Galaxy Astrophysics
Abstract: The nature of the massive object at the Galactic Center (Sgr A$^{*}$) is still unclear even if various observational campaigns led many authors to believe that our Galaxy hosts a super-massive black hole with mass $M\simeq 2.6\times 10^6$ M$_{\odot}$. However, the black hole hypothesis, which theoretically implies a luminosity $\simeq 10^{41}$ erg s$^{-1}$, runs into problems if one takes into account that the observed luminosity, from radio to $\gamma$-ray wavelengths, is below $10^{37}$ erg s$^{-1}$. In order to solve this blackness problem, alternative models have been recently proposed. In particular, it has been suggested that the Galactic Center hosts a ball made up by non-baryonic matter (e.g. massive neutrinos and anti-neutrinos) in which the degeneracy pressure of fermions balances their self-gravity. Requiring to be consistent with all the available observations towards the Galactic Center allows us to put severe astrophysical constraints on the neutrino ball parameters. The presence of such an object in the Galactic Center may be excluded if the constituent neutrino mass $m_{\nu}$ is $\ut> 24$ keV, while if $m_{\nu}\ut< 24$ keV observations can not give a definite answer., Comment: 9 pages, 3 figures, in press on Astronomy and Astrophysics

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