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10 results on '"[ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph]"'

1. Inferences on mass composition and tests of hadronic interactions from 0.3 to 100 EeV using the water-Cherenkov detectors of the Pierre Auger Observatory

Author

Aab, A., Abreu, P., AGLIETTA, MARCO, Al Samarai, I., Albuquerque, I. F. M., Allekotte, I., Almela, A., Alvarez Castillo, J., Alvarez-Muñiz, J., Anastasi, G. A., Anchordoqui, L., Andrada, B., Andringa, S., Aramo, C., Arqueros, F., Arsene, N., Asorey, H., Assis, P., Aublin, J., Avila, G., Badescu, A. M., Balaceanu, A., Barbato, F., Barreira Luz, R. J., Beatty, J. J., Becker, K. H., Bellido, J. A., Berat, C., Bertaina, M. E., Bertou, X., Biermann, P. L., Biteau, J., Blaess, S. G., Blanco, A., Blazek, J., Bleve, C., Boháčová, M., Boncioli, D., Bonifazi, C., Borodai, N., Botti, A. M., Brack, J., Brancus, I., Bretz, T., Bridgeman, A., Briechle, F. L., Buchholz, P., Bueno, A., Buitink, S., Buscemi, M., Caballero-Mora, K. S., Caccianiga, L., Cancio, A., Canfora, F., Caramete, L., Caruso, R., CASTELLINA, ANTONELLA, Catalani, F., Cataldi, G., Cazon, L., Chavez, A. G., Chinellato, J. A., Chudoba, J., Clay, R. W., Cobos, A., Colalillo, R., Coleman, A., Collica, L., Coluccia, M. R., Conceição, R., Consolati, G., Contreras, F., Cooper, M. J., Coutu, S., Covault, C. E., Cronin, J., D'Amico, S., Daniel, B., Dasso, S., Daumiller, K., Dawson, B. R., de Almeida, R. M., de Jong, S. J., De Mauro, G., de Mello Neto, J. R. T., De Mitri, I., de Oliveira, J., de Souza, V., Debatin, J., Deligny, O., Díaz Castro, M. L., Diogo, F., Dobrigkeit, C., D'Olivo, J. C., Dorosti, Q., dos Anjos, R. C., Dova, M. T., Dundovic, A., Ebr, J., Engel, R., Erdmann, M., Erfani, M., Escobar, C. O., Espadanal, J., Etchegoyen, A., Falcke, H., Farmer, J., Farrar, G., Fauth, A. C., Fazzini, N., Fenu, F., Fick, B., Figueira, J. M., Filipčič, A., Fratu, O., Freire, M. M., Fujii, T., Fuster, A., Gaior, R., García, B., Garcia-Pinto, D., Gaté, F., Gemmeke, H., Gherghel-Lascu, A., Ghia, P. L., Giaccari, U., Giammarchi, M., Giller, M., Głas, D., Glaser, C., Golup, G., Gómez Berisso, M., Gómez Vitale, P. F., González, N., GORGI, Alessio, Gorham, P., Grillo, A. F., Grubb, T. D., Guarino, F., Guedes, G. P., Halliday, R., Hampel, M. R., Hansen, P., Harari, D., Harrison, T. A., Harton, J. L., Haungs, A., Hebbeker, T., Heck, D., Heimann, P., Herve, A. E., Hill, G. C., Hojvat, C., Holt, E., Homola, P., Hörandel, J. R., Horvath, P., Hrabovský, M., Huege, T., Hulsman, J., Insolia, A., Isar, P. G., Jandt, I., Johnsen, J. A., Josebachuili, M., Jurysek, J., Kääpä, A., Kambeitz, O., Kampert, K. H., Keilhauer, B., Kemmerich, N., Kemp, E., Kemp, J., Kieckhafer, R. M., Klages, H. O., Kleifges, M., Kleinfeller, J., Krause, R., Krohm, N., Kuempel, D., Kukec Mezek, G., Kunka, N., Kuotb Awad, A., Lago, B. L., LaHurd, D., Lang, R. G., Lauscher, M., Legumina, R., Leigui de Oliveira, M. A., Letessier-Selvon, A., Lhenry-Yvon, I., Link, K., Lo Presti, D., Lopes, L., López, R., López Casado, A., Lorek, R., Luce, Q., Lucero, A., Malacari, M., Mallamaci, M., Mandat, D., Mantsch, P., Mariazzi, A. G., Mariș, I. C., Marsella, G., Martello, D., Martinez, H., Martínez Bravo, O., Masías Meza, J. J., Mathes, H. J., Mathys, S., Matthews, J., Matthews, J. A. J., Matthiae, G., Mayotte, E., Mazur, P. O., Medina, C., Medina-Tanco, G., Melo, D., Menshikov, A., Merenda, K. -D., Michal, S., Micheletti, M. I., Middendorf, L., Miramonti, L., Mitrica, B., Mockler, D., Mollerach, S., Montanet, F., Morello, C., Mostafá, M., Müller, A. L., Müller, G., Muller, M. A., Müller, S., Mussa, R., Naranjo, I., Nellen, L., Nguyen, P. H., Niculescu-Oglinzanu, M., Niechciol, M., Niemietz, L., Niggemann, T., Nitz, D., Nosek, D., Novotny, V., Nožka, L., Núñez, L. A., Ochilo, L., Oikonomou, F., Olinto, A., Palatka, M., Pallotta, J., Papenbreer, P., Parente, G., Parra, A., Paul, T., Pech, M., Pedreira, F., Pekala, J., Pelayo, R., Peña-Rodriguez, J., Pereira, L. A. S., Perlin, M., Perrone, L., Peters, C., Petrera, S., Phuntsok, J., Piegaia, R., Pierog, T., Pimenta, M., Pirronello, V., Platino, M., Plum, M., Porowski, C., Prado, R. R., Privitera, P., Prouza, M., Quel, E. J., Querchfeld, S., Quinn, S., Ramos-Pollan, R., Rautenberg, J., Ravignani, D., Ridky, J., Riehn, F., Risse, M., Ristori, P., Rizi, V., Rodrigues de Carvalho, W., Rodriguez Fernandez, G., Rodriguez Rojo, J., Rogozin, D., Roncoroni, M. J., Roth, M., Roulet, E., Rovero, A. C., Ruehl, P., Saffi, S. J., Saftoiu, A., Salamida, F., Salazar, H., Saleh, A., Salesa Greus, F., Salina, G., Sánchez, F., Sanchez-Lucas, P., Santos, E. M., Santos, E., Sarazin, F., Sarmento, R., Sarmiento-Cano, C., Sato, R., Schauer, M., Scherini, V., Schieler, H., Schimp, M., Schmidt, D., Scholten, O., Schovánek, P., Schröder, F. G., Schröder, S., Schulz, A., Schumacher, J., Sciutto, S. J., SEGRETO, ALBERTO, Shadkam, A., Shellard, R. C., Sigl, G., Silli, G., Sima, O., Śmiałkowski, A., Šmída, R., Smith, B., Snow, G. R., Sommers, P., Sonntag, S., Squartini, R., Stanca, D., Stanič, S., Stasielak, J., Stassi, P., Stolpovskiy, M., Strafella, F., Streich, A., Suarez, F., Suarez Durán, M., Sudholz, T., Suomijärvi, T., Supanitsky, A. D., Šupík, J., Swain, J., Szadkowski, Z., Taboada, A., Taborda, O. A., Theodoro, V. M., Timmermans, C., Todero Peixoto, C. J., Tomankova, L., Tomé, B., Torralba Elipe, G., Travnicek, P., Trini, M., Ulrich, R., Unger, M., Urban, M., Valdés Galicia, J. F., Valiño, I., Valore, L., van Aar, G., van Bodegom, P., van den Berg, A. M., van Vliet, A., Varela, E., Vargas Cárdenas, B., Varner, G., Vázquez, R. A., Veberič, D., Ventura, C., Vergara Quispe, I. D., Verzi, V., Vicha, J., Villaseñor, L., Vorobiov, S., Wahlberg, H., Wainberg, O., Walz, D., Watson, A. A., Weber, M., Weindl, A., Wiencke, L., Wilczyński, H., Wileman, C., Wirtz, M., Wittkowski, D., Wundheiler, B., Yang, L., Yushkov, A., Zas, E., Zavrtanik, D., Zavrtanik, M., Zepeda, A., Zimmermann, B., Ziolkowski, M., Zong, Z., Zuccarello, Francesca, Pierre Auger Collaboration, Laboratoire de Physique Nucléaire et de Hautes Énergies ( LPNHE ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Université Paris Diderot - Paris 7 ( UPD7 ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratoire de Physique Subatomique et de Cosmologie ( LPSC ), Université Joseph Fourier - Grenoble 1 ( UJF ) -Institut polytechnique de Grenoble - Grenoble Institute of Technology ( Grenoble INP ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Centre National de la Recherche Scientifique ( CNRS ) -Université Grenoble Alpes ( UGA ), Institut de Physique Nucléaire d'Orsay ( IPNO ), Université Paris-Sud - Paris 11 ( UP11 ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratoire de physique subatomique et des technologies associées ( SUBATECH ), IMT Atlantique Bretagne-Pays de la Loire ( IMT Atlantique ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Centre National de la Recherche Scientifique ( CNRS ) -Université de Nantes ( UN ), Pierre Auger, Research unit Astroparticle Physics, Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE (UMR_7585)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP ), Université Grenoble Alpes (UGA), Institut de Physique Nucléaire d'Orsay (IPNO), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), Laboratoire de physique subatomique et des technologies associées (SUBATECH), Université de Nantes - UFR des Sciences et des Techniques (UN UFR ST), Université de Nantes (UN)-Université de Nantes (UN)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-IMT Atlantique Bretagne-Pays de la Loire (IMT Atlantique), Institut Mines-Télécom [Paris] (IMT)-Institut Mines-Télécom [Paris] (IMT), Physics, Elementary Particle Physics, Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Université de Nantes - Faculté des Sciences et des Techniques, Université de Nantes (UN)-Université de Nantes (UN)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-IMT Atlantique Bretagne-Pays de la Loire (IMT Atlantique), Aab, A., Abreu, P., Aglietta, M., Al Samarai, I., Albuquerque, I. F. M., Allekotte, I., Almela, A., Alvarez Castillo, J., Alvarez-Muñiz, J., Anastasi, G. A., Anchordoqui, L., Andrada, B., Andringa, S., Aramo, C., Arqueros, F., Arsene, N., Asorey, H., Assis, P., Aublin, J., Avila, G., Badescu, A. M., Balaceanu, A., Barbato, F., Barreira Luz, R. J., Beatty, J. J., Becker, K. H., Bellido, J. A., Berat, C., Bertaina, M. E., Bertou, X., Biermann, P. L., Biteau, J., Blaess, S. G., Blanco, A., Blazek, J., Bleve, C., Boháčová, M., Boncioli, D., Bonifazi, C., Borodai, N., Botti, A. M., Brack, J., Brancus, I., Bretz, T., Bridgeman, A., Briechle, F. L., Buchholz, P., Bueno, A., Buitink, S., Buscemi, M., Caballero-Mora, K. S., Caccianiga, L., Cancio, A., Canfora, F., Caramete, L., Caruso, R., Castellina, A., Catalani, F., Cataldi, G., Cazon, L., Chavez, A. G., Chinellato, J. A., Chudoba, J., Clay, R. W., Cobos, A., Colalillo, R., Coleman, A., Collica, L., Coluccia, M. R., Conceição, R., Consolati, G., Contreras, F., Cooper, M. J., Coutu, S., Covault, C. E., Cronin, J., D'Amico, S., Daniel, B., Dasso, S., Daumiller, K., Dawson, B. R., De Almeida, R. M., De Jong, S. J., De Mauro, G., De Mello Neto, J. R. T., De Mitri, I., De Oliveira, J., De Souza, V., Debatin, J., Deligny, O., Díaz Castro, M. L., Diogo, F., Dobrigkeit, C., D'Olivo, J. C., Dorosti, Q., Dos Anjos, R. C., Dova, M. T., Dundovic, A., Ebr, J., Engel, R., Erdmann, M., Erfani, M., Escobar, C. O., Espadanal, J., Etchegoyen, A., Falcke, H., Farmer, J., Farrar, G., Fauth, A. C., Fazzini, N., Fenu, F., Fick, B., Figueira, J. M., Filipčič, A., Fratu, O., Freire, M. M., Fujii, T., Fuster, A., Gaior, R., García, B., Garcia-Pinto, D., Gaté, F., Gemmeke, H., Gherghel-Lascu, A., Ghia, P. L., Giaccari, U., Giammarchi, M., Giller, M., Głas, D., Glaser, C., Golup, G., Gómez Berisso, M., Gómez Vitale, P. F., González, N., Gorgi, A., Gorham, P., Grillo, A. F., Grubb, T. D., Guarino, Fausto., Guedes, G. P., Halliday, R., Hampel, M. R., Hansen, P., Harari, D., Harrison, T. A., Harton, J. L., Haungs, A., Hebbeker, T., Heck, D., Heimann, P., Herve, A. E., Hill, G. C., Hojvat, C., Holt, E., Homola, P., Hörandel, J. R., Horvath, P., Hrabovský, M., Huege, T., Hulsman, J., Insolia, A., Isar, P. G., Jandt, I., Johnsen, J. A., Josebachuili, M., Jurysek, J., Kääpä, A., Kambeitz, O., Kampert, K. H., Keilhauer, B., Kemmerich, N., Kemp, E., Kemp, J., Kieckhafer, R. M., Klages, H. O., Kleifges, M., Kleinfeller, J., Krause, R., Krohm, N., Kuempel, D., Kukec Mezek, G., Kunka, N., Kuotb Awad, A., Lago, B. L., Lahurd, D., Lang, R. G., Lauscher, M., Legumina, R., Leigui De Oliveira, M. A., Letessier-Selvon, A., Lhenry-Yvon, I., Link, K., Lo Presti, D., Lopes, L., López, R., López Casado, A., Lorek, R., Luce, Q., Lucero, A., Malacari, M., Mallamaci, M., Mandat, D., Mantsch, P., Mariazzi, A. G., Mariş, I. C., Marsella, G., Martello, D., Martinez, H., Martínez Bravo, O., Masías Meza, J. J., Mathes, H. J., Mathys, S., Matthews, J., Matthews, J. A. J., Matthiae, G., Mayotte, E., Mazur, P. O., Medina, C., Medina-Tanco, G., Melo, D., Menshikov, A., Merenda, K. -D., Michal, S., Micheletti, M. I., Middendorf, L., Miramonti, L., Mitrica, B., Mockler, D., Mollerach, S., Montanet, F., Morello, C., Mostafá, M., Müller, A. L., Müller, G., Muller, M. A., Müller, S., Mussa, R., Naranjo, I., Nellen, L., Nguyen, P. H., Niculescu-Oglinzanu, M., Niechciol, M., Niemietz, L., Niggemann, T., Nitz, D., Nosek, D., Novotny, V., Nožka, L., Núñez, L. A., Ochilo, L., Oikonomou, F., Olinto, A., Palatka, M., Pallotta, J., Papenbreer, P., Parente, G., Parra, A., Paul, T., Pech, M., Pedreira, F., Pȩkala, J., Pelayo, R., Peña-Rodriguez, J., Pereira, L. A. S., Perlin, M., Perrone, L., Peters, C., Petrera, S., Phuntsok, J., Piegaia, R., Pierog, T., Pimenta, M., Pirronello, V., Platino, M., Plum, M., Porowski, C., Prado, R. R., Privitera, P., Prouza, M., Quel, E. J., Querchfeld, S., Quinn, S., Ramos-Pollan, R., Rautenberg, J., Ravignani, D., Ridky, J., Riehn, F., Risse, M., Ristori, P., Rizi, V., Rodrigues De Carvalho, W., Rodriguez Fernandez, G., Rodriguez Rojo, J., Rogozin, D., Roncoroni, M. J., Roth, M., Roulet, E., Rovero, A. C., Ruehl, P., Saffi, S. J., Saftoiu, A., Salamida, F., Salazar, H., Saleh, A., Salesa Greus, F., Salina, G., Sánchez, F., Sanchez-Lucas, P., Santos, E. M., Santos, E., Sarazin, F., Sarmento, R., Sarmiento-Cano, C., Sato, R., Schauer, M., Scherini, V., Schieler, H., Schimp, M., Schmidt, D., Scholten, O., Schovánek, P., Schröder, F. G., Schröder, S., Schulz, A., Schumacher, J., Sciutto, S. J., Segreto, A., Shadkam, A., Shellard, R. C., Sigl, G., Silli, G., Sima, O., Śmiałkowski, A., Šmída, R., Smith, B., Snow, G. R., Sommers, P., Sonntag, S., Squartini, R., Stanca, D., Stanič, S., Stasielak, J., Stassi, P., Stolpovskiy, M., Strafella, F., Streich, A., Suarez, F., Suarez Durán, M., Sudholz, T., Suomijärvi, T., Supanitsky, A. D., Šupík, J., Swain, J., Szadkowski, Z., Taboada, A., Taborda, O. A., Theodoro, V. M., Timmermans, C., Todero Peixoto, C. J., Tomankova, L., Tomé, B., Torralba Elipe, G., Travnicek, P., Trini, M., Ulrich, R., Unger, M., Urban, M., Valdés Galicia, J. F., Valiño, I., Valore, L., Van Aar, G., Van Bodegom, P., Van Den Berg, A. M., Van Vliet, A., Varela, E., Vargas Cárdenas, B., Varner, G., Vázquez, R. A., Veberič, D., Ventura, C., Vergara Quispe, I. D., Verzi, V., Vicha, J., Villaseñor, L., Vorobiov, S., Wahlberg, H., Wainberg, O., Walz, D., Watson, A. A., Weber, M., Weindl, A., Wiencke, L., Wilczyński, H., Wileman, C., Wirtz, M., Wittkowski, D., Wundheiler, B., Yang, L., Yushkov, A., Zas, E., Zavrtanik, D., Zavrtanik, M., Zepeda, A., Zimmermann, B., Ziolkowski, M., Zong, Z., and Zuccarello, F.

Subjects
Hadronic interaction, Physics and Astronomy (miscellaneous), interaction: model, Astronomy, [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], 01 natural sciences, UHE, Auger, mass spectrum, 98.70.Sa, Observatory, 010303 astronomy & astrophysics, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Astrophysics::Instrumentation and Methods for Astrophysics, observatory, ComputingMethodologies_DOCUMENTANDTEXTPROCESSING, fluorescence, Astrophysics - High Energy Astrophysical Phenomena, 96.50.S, air, Astrophysics::High Energy Astrophysical Phenomena, water, FOS: Physical sciences, Cosmic ray, energy dependence, Nuclear physics, Cosmic ray composition, muon, 0103 physical sciences, Calibration, 96.50.sd, High Energy Physics, Cherenkov radiation, Ciencias Exactas, 96.50.sb, Pierre Auger Observatory, Muon, showers: atmosphere, 010308 nuclear & particles physics, Física, ASTROFÍSICA, calibration, Cherenkov counter, electromagnetic, 13. Climate action, Cosmic ray spectra, Experimental High Energy Physics, Mass spectrum, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], statistical
Abstract

We present a new method for probing the hadronic interaction models at ultrahigh energy and extracting details about mass composition. This is done using the time profiles of the signals recorded with the water-Cherenkov detectors of the Pierre Auger Observatory. The profiles arise from a mix of the muon and electromagnetic components of air showers. Using the risetimes of the recorded signals, we define a new parameter, which we use to compare our observations with predictions from simulations. We find, first, inconsistencies between our data and predictions over a greater energy range and with substantially more events than in previous studies. Second, by calibrating the new parameter with fluorescence measurements from observations made at the Auger Observatory, we can infer the depth of shower maximum Xmax for a sample of over 81,000 events extending from 0.3 to over 100 EeV. Above 30 EeV, the sample is nearly 14 times larger than what is currently available from fluorescence measurements and extending the covered energy range by half a decade. The energy dependence of ❬Xmax❭ is compared to simulations and interpreted in terms of the mean of the logarithmic mass. We find good agreement with previous work and extend the measurement of the mean depth of shower maximum to greater energies than before, reducing significantly the statistical uncertainty associated with the inferences about mass composition., La lista completa de autores que integran el documento puede consultarse en el archivo asociado., Instituto de Física La Plata

Published
2017
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2. Fourier domain gravitational waveforms for precessing eccentric binaries

Author

Achamveedu Gopakumar, Antoine Klein, Philippe Jetzer, Lorenzo De Vittori, Y. Boetzel, Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), University of Zurich, Institut d'Astrophysique de Paris ( IAP ), and Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS )

Subjects
data analysis method, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Orbital plane, Physics and Astronomy (miscellaneous), 530 Physics, General relativity, [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], binary, FOS: Physical sciences, alternative theories of gravity, General Relativity and Quantum Cosmology (gr-qc), 10192 Physics Institute, 01 natural sciences, General Relativity and Quantum Cosmology, [ PHYS.GRQC ] Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], symbols.namesake, precession, binary: spin, numerical methods, 0103 physical sciences, Waveform, 3101 Physics and Astronomy (miscellaneous), numerical calculations, 010303 astronomy & astrophysics, orbit, Physics, 010308 nuclear & particles physics, Gravitational wave, gravitational radiation, Computational physics, Fourier transform, Amplitude, gravitational radiation: emission, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], Precession, symbols, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Eccentricity (mathematics), Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We build two families of inspiral waveforms for precessing binaries on eccentric orbits in the Fourier domain. To achieve this, we use a small eccentricity expansion of the waveform amplitudes in order to separate the periastron precession timescale from the orbital timescale, and use a shifted uniform asymptotics transformation to compute the Fourier transform in the presence of spin-induced precession. We show that the resulting waveforms can yield a median faithfulness above 0.993 when compared to an equivalent time domain waveform with an initial eccentricity of $e_0 \approx 0.3$. We also show that when the spins are large, using a circular waveform can potentially lead to significant biases in the recovery of the parameters, even when the system has fully circularized, particularly when the accumulated number of cycles is large. This is an effect of the residual eccentricity present when the objects forming the binary have nonvanishing spin components in the orbital plane., 23 pages, 13 figures

Published
2018
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3. Vector disformal transformation of cosmological perturbations

Author

Vassilis Papadopoulos, Hassan Firouzjahi, Moslem Zarei, Shinji Mukohyama, École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL), Laboratoire de Mathématiques et Physique Théorique (LMPT), Centre National de la Recherche Scientifique (CNRS)-Université de Tours, École normale supérieure - Paris ( ENS Paris ), Laboratoire de Mathématiques et Physique Théorique ( LMPT ), and Université de Tours-Centre National de la Recherche Scientifique ( CNRS )

Subjects
High Energy Physics - Theory, neutron star: binary, Cosmology and Nongalactic Astrophysics (astro-ph.CO), [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], media_common.quotation_subject, FOS: Physical sciences, General Relativity and Quantum Cosmology (gr-qc), 01 natural sciences, General Relativity and Quantum Cosmology, [ PHYS.HTHE ] Physics [physics]/High Energy Physics - Theory [hep-th], [ PHYS.GRQC ] Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], matter: coupling, 0103 physical sciences, Invariant (mathematics), 010306 general physics, Mathematical physics, media_common, Physics, [PHYS.HTHE]Physics [physics]/High Energy Physics - Theory [hep-th], 010308 nuclear & particles physics, Gravitational wave, gravitational radiation, Observable, Gauge (firearms), Universe, Neutron star, Transformation (function), High Energy Physics - Theory (hep-th), gravitational radiation: emission, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], gauge field theory: U(1), field theory: vector, curvature: perturbation, Vector field, transformation: gauge, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We study disformal transformations of cosmological perturbations by vector fields in theories invariant under U(1) gauge transformations. Three types of vector disformal transformations are considered: (i) disformal transformations by a single timelike vector; (ii) disformal transformations by a single spacelike vector; and (iii) disformal transformations by three spacelike vectors. We show that transformations of type (i) do not change either curvature perturbation or gravitational waves; that those of type (ii) do not change curvature perturbation but change gravitational waves; and that those of type (iii) change both curvature perturbation and gravitational waves. Therefore, coupling matter fields to the metric after disformal transformations of type (ii) or (iii) in principle have observable consequences. While the recent multi-messenger observation of binary neutron stars has singled out a proper disformal frame at the present epoch with a high precision, the result of the present paper may thus help distinguishing disformal frames in the early universe., Comment: 16 pages

Published
2018
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4. Perturbed redshifts from N -body simulations

Author

Julian Adamek, Laboratoire Univers et Théories (LUTH (UMR_8102)), Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7), Laboratoire Univers et Théories ( LUTH ), Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Centre National de la Recherche Scientifique ( CNRS ), and PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Length scale, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Scale (ratio), [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], FOS: Physical sciences, General Relativity and Quantum Cosmology (gr-qc), Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Astronomical survey, 01 natural sciences, General Relativity and Quantum Cosmology, [ PHYS.GRQC ] Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], symbols.namesake, 0103 physical sciences, 010303 astronomy & astrophysics, Physics, 010308 nuclear & particles physics, Redshift survey, Redshift, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], symbols, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Relativistic quantum chemistry, Doppler effect, Astrophysics - Cosmology and Nongalactic Astrophysics, Gravitational redshift
Abstract

In order to keep pace with the increasing data quality of astronomical surveys the observed source redshift has to be modeled beyond the well-known Doppler contribution. In this letter I want to examine the gauge issue that is often glossed over when one assigns a perturbed redshift to simulated data generated with a Newtonian N-body code. A careful analysis reveals the presence of a correction term that has so far been neglected. It is roughly proportional to the observed length scale divided by the Hubble scale and therefore suppressed inside the horizon. However, on gigaparsec scales it can be comparable to the gravitational redshift and hence amounts to an important relativistic effect., 5 pages; v2: minor revision, accepted version

Published
2018
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5. Stable cosmology in chameleon bigravity

Author

Michele Oliosi, Yota Watanabe, Antonio De Felice, Shinji Mukohyama, Laboratoire de Mathématiques et Physique Théorique (LMPT), Centre National de la Recherche Scientifique (CNRS)-Université de Tours, Laboratoire de Mathématiques et Physique Théorique ( LMPT ), Centre National de la Recherche Scientifique ( CNRS ) -Université de Tours, and Université de Tours (UT)-Centre National de la Recherche Scientifique (CNRS)

Subjects
High Energy Physics - Theory, chameleon, cosmological model, Cosmology and Nongalactic Astrophysics (astro-ph.CO), media_common.quotation_subject, [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], FOS: Physical sciences, Astrophysics, General Relativity and Quantum Cosmology (gr-qc), Parameter space, gravitation: potential, 01 natural sciences, Stability (probability), Cosmology, General Relativity and Quantum Cosmology, [ PHYS.HTHE ] Physics [physics]/High Energy Physics - Theory [hep-th], [ PHYS.GRQC ] Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], Theoretical physics, De Sitter universe, de Sitter, 0103 physical sciences, strong coupling, bimetric, 010306 general physics, media_common, Physics, 010308 nuclear & particles physics, Gravitational wave, background, [PHYS.HTHE]Physics [physics]/High Energy Physics - Theory [hep-th], Graviton, gravitational radiation, solar system, stability, Universe, boundary condition, Vainshtein, field theory: scalar, High Energy Physics - Theory (hep-th), graviton, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Scalar field, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

The recently proposed chameleonic extension of bigravity theory, by including a scalar field dependence in the graviton potential, avoids several fine-tunings found to be necessary in usual massive bigravity. In particular it ensures that the Higuchi bound is satisfied at all scales, that no Vainshtein mechanism is needed to satisfy solar-system experiments, and that the strong coupling scale is always above the scale of cosmological interest all the way up to the early universe. This paper extends the previous work by presenting a stable example of cosmology in the chameleon bigravity model. We find a set of initial conditions and parameters such that the derived stability conditions on general flat Friedmann background are satisfied at all times. The evolution goes through radiation dominated, matter dominated, and de Sitter eras. We argue that the parameter space allowing for such a stable evolution may be large enough to encompass an observationally viable evolution. We also argue that our model satisfies all known constraints due to gravitational wave observations so far and thus can be considered as a unique testing ground of gravitational wave phenomenologies in bimetric theories of gravity., Comment: 15 pages, 5 figures, v2 matches published version

Published
2018
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6. Primordial black hole dark matter from single field inflation

Author

M. Taoso, Guillermo Ballesteros, Institut de Physique Théorique - UMR CNRS 3681 (IPHT), Centre National de la Recherche Scientifique (CNRS)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Institut de Physique Théorique - UMR CNRS 3681 ( IPHT ), Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Université Paris-Saclay-Centre National de la Recherche Scientifique ( CNRS ), and Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)

Subjects
High Energy Physics - Theory, Cosmology and Nongalactic Astrophysics (astro-ph.CO), [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], Dark matter, Scalar field dark matter, FOS: Physical sciences, Primordial black hole, General Relativity and Quantum Cosmology (gr-qc), cosmic background radiation, dark matter: density, Astrophysics::Cosmology and Extragalactic Astrophysics, spectrum: tensor, effective potential: model, 01 natural sciences, General Relativity and Quantum Cosmology, [ PHYS.GRQC ] Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], [ PHYS.HTHE ] Physics [physics]/High Energy Physics - Theory [hep-th], mass spectrum, Theoretical physics, High Energy Physics - Phenomenology (hep-ph), fluctuation: scalar, 0103 physical sciences, spectrum: scalar, 010306 general physics, black hole: production, Physics, Inflation (cosmology), mass: solar, [PHYS.HTHE]Physics [physics]/High Energy Physics - Theory [hep-th], 010308 nuclear & particles physics, Hot dark matter, inflation: slow-roll approximation, deceleration, Inflaton, inflaton, inflation: model, Black hole, High Energy Physics - Phenomenology, High Energy Physics - Theory (hep-th), space-time, curvature, [PHYS.HPHE]Physics [physics]/High Energy Physics - Phenomenology [hep-ph], [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], [ PHYS.HPHE ] Physics [physics]/High Energy Physics - Phenomenology [hep-ph], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], black hole: primordial, Dark fluid, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We propose a model of inflation capable of generating a population of light black holes (about $10^{-16}$ - $10^{-14}$ solar masses) that might account for a significant fraction of the dark matter in the Universe. The effective potential of the model features an approximate inflection point arising from two-loop order logarithmic corrections in well-motivated and perturbative particle physics examples. This feature decelerates the inflaton before the end of inflation, enhancing the primordial spectrum of scalar fluctuations and triggering efficient black hole production with a peaked mass distribution. At larger field values, inflation occurs thanks to a generic small coupling between the inflaton and the curvature of spacetime. We compute accurately the peak mass and abundance of the primordial black holes using the Press-Schechter and Mukhanov-Sasaki formalisms, showing that the slow-roll approximation fails to reproduce the correct results by orders of magnitude. We study as well a qualitatively similar implementation of the idea, where the approximate inflection point is due to competing terms in a generic polynomial potential. In both models, requiring a significant part of the dark matter abundance to be in the form of black holes implies a small blue scalar tilt with a sizable negative running and a tensor spectrum that may be detected by the next-generation probes of the cosmic microwave background. We also comment on previous works on the topic., minor changes, references added, to appear in PRD

Published
2018
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7. CMB bounds on disk-accreting massive primordial black holes

Author

Vivian Poulin, Pasquale D. Serpico, Kazunori Kohri, Sebastien Clesse, Francesca Calore, Laboratoire d'Annecy-le-Vieux de Physique Théorique (LAPTH), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Annecy-le-Vieux de Physique Théorique ( LAPTH ), and Université Savoie Mont Blanc ( USMB [Université de Savoie] [Université de Chambéry] ) -Centre National de la Recherche Scientifique ( CNRS )

Subjects
matter: accretion, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Photon, [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], Astrophysics::High Energy Astrophysical Phenomena, Dark matter, Cosmic microwave background, binary, FOS: Physical sciences, Primordial black hole, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, dark matter: parametrization, thermal, Binary black hole, Ionization, ionization, 0103 physical sciences, conservation law, numerical calculations, 010306 general physics, Astrophysics::Galaxy Astrophysics, Physics, 010308 nuclear & particles physics, Astronomy, Accretion (astrophysics), Dark Ages, nonlinear, Astrophysics::Earth and Planetary Astrophysics, history, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], statistical, black hole: primordial, Astrophysics - Cosmology and Nongalactic Astrophysics, cosmic background radiation: anisotropy
Abstract

Stellar-mass Primordial Black Holes (PBH) have been recently reconsidered as a Dark Matter (DM) candidate, after the aLIGO discovery of several binary BH mergers with masses of tens of $M_\odot$. Matter accretion on such massive objects leads to the emission of high-energy photons, capable of altering the ionization and thermal history of the universe. This in turn affects the statistical properties of the cosmic microwave background (CMB) anisotropies. Previous analyses have assumed spherical accretion. We argue that this approximation likely breaks down and that an accretion disk should form in the dark ages. Using the most up-to-date tools to compute the energy deposition in the medium, we derive constraints on the fraction of DM in PBH. Provided that disks form early on, even under conservative assumptions for accretion, these constraints exclude a monochromatic distribution of PBH with masses above $\sim 2\, M_\odot$ as the dominant form of DM. The bound on the median PBH mass gets more stringent if a broad, log-normal mass function is considered. A deepened understanding of non-linear clustering properties and BH accretion disk physics would permit an improved treatment and possibly lead to more stringent constraints., Comment: 13 pages, 5 figures

Published
2017
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8. Minimal model for extragalactic cosmic rays and neutrinos

Author

M. Kachelrieß, Dmitri Semikoz, Oleg Kalashev, S. Ostapchenko, AstroParticule et Cosmologie (APC (UMR_7164)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), AstroParticule et Cosmologie ( APC - UMR 7164 ), Centre National de la Recherche Scientifique ( CNRS ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ), and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP)

Subjects
Photon, accelerator, gamma ray: background, air, [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], Astrophysics::High Energy Astrophysical Phenomena, cosmic radiation: energy, FOS: Physical sciences, Cosmic ray, Astrophysics, 01 natural sciences, 7. Clean energy, neutrino: flux, Spectral line, IceCube, gas, 0103 physical sciences, cosmic radiation: UHE, hadron hadron: interaction, 010303 astronomy & astrophysics, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, showers: atmosphere, 010308 nuclear & particles physics, photon, nucleus, Astrophysics::Instrumentation and Methods for Astrophysics, Gamma ray, Order (ring theory), 13. Climate action, galaxy, Neutrino, Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Maxima, cosmic radiation: flux, model: minimal, Energy (signal processing)
Abstract

We aim to explain in a unified way the experimental data on ultrahigh energy cosmic rays (UHECR) and neutrinos, using a single source class and obeying limits on the extragalactic diffuse gamma-ray background (EGRB). If UHECRs only interact hadronically with gas around their sources, the resulting diffuse CR flux can be matched well to the observed one, providing at the same time large neutrino fluxes. However, air showers in the Earth's atmosphere induced by UHECRs with energies $E>3\times 10^{18}$ eV would reach in such a case their maxima too high. Therefore additional photo-hadronic interactions of UEHCRs close to the accelerator have to be present, in order to modify the nuclear composition of CRs in a relatively narrow energy interval. We include thus both photon and gas backgrounds, and combine the resulting CR spectra with the high-energy part of the Galactic CR fluxes predicted by the escape model. As result, we find a good description of experimental data on the total CR flux, the mean shower depth $X_\max$ and its width $RMS(X_\max)$ in the whole energy range above $E\simeq 10^{17}$ eV. The predicted high-energy neutrino flux matches IceCube measurements, while the contribution to the EGRB is of order 30%., v2: 7 pages, 6 eps figures; slightly extended version to appear in PRD

Published
2017
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9. Where does curvaton reside? Differences between bulk and brane frames

Author

Ryo Namba, François Larrouturou, Shinji Mukohyama, Yota Watanabe, École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL), and École normale supérieure - Paris ( ENS Paris )

Subjects
High Energy Physics - Theory, Cosmology and Nongalactic Astrophysics (astro-ph.CO), [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], Cosmic microwave background, FOS: Physical sciences, D-brane, General Relativity and Quantum Cosmology (gr-qc), Astrophysics::Cosmology and Extragalactic Astrophysics, power spectrum, Curvature, String theory, 01 natural sciences, General Relativity and Quantum Cosmology, [ PHYS.HTHE ] Physics [physics]/High Energy Physics - Theory [hep-th], [ PHYS.GRQC ] Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], membrane model, Standard Model, Theoretical physics, conformal, 0103 physical sciences, 010306 general physics, Physics, Inflation (cosmology), curvaton, [PHYS.HTHE]Physics [physics]/High Energy Physics - Theory [hep-th], 010308 nuclear & particles physics, inflation: slow-roll approximation, Observable, Inflaton, inflaton, inflation: model, Classical mechanics, High Energy Physics - Theory (hep-th), gravitation, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], curvature: perturbation, Brane, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Some classes of inflationary models naturally introduce two distinct metrics/frames, and their equivalence in terms of observables has often been put in question. D-brane inflation proposes candidates for an inflaton embedded in the string theory and possesses descriptions on the brane and bulk metrics/frames, which are connected by a conformal/disformal transformation that depends on the inflaton and its derivatives. It has been shown that curvature perturbations generated by the inflaton are identical in both frames, meaning that observables such as the spectrum of cosmic microwave background (CMB) anisotropies are independent of whether matter fields---including those in the standard model of particle physics---minimally couple to the brane or the bulk metric/frame. This is true despite the fact that the observables are eventually measured by the matter fields and that the total action including the matter fields is different in the two cases. In contrast, in curvaton scenarios, the observables depend on the frame to which the curvaton minimally couples. Among all inflationary scenarios, we focus on two models motivated by the KKLMMT fine-tuning problem: a slow-roll inflation with an inflection-point potential and a model of a rapidly rolling inflaton that conformally couples to gravity. In the first model, the difference between the frames in which the curvaton resides is encoded in the spectral index of the curvature perturbations, depicting the nature of the frame transformation. In the second model, the curvaton on the brane induces a spectral index significantly different from that in the bulk and is even falsified by the observations. This work thus demonstrates that two frames connected by a conformal/disformal transformation lead to different physical observables such as CMB anisotropies in curvaton models., 16 pages, v2: published version

Published
2017
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10. Atomic interferometry test of dark energy

Author

Brax, Philippe, Davis, Anne-Christine, Service de Physique Théorique (SPhT), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Centre National de la Recherche Scientifique (CNRS), Service de Physique Théorique ( SPhT ), and Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Centre National de la Recherche Scientifique ( CNRS )

Subjects
chameleon, cosmological model, Gravity (chemistry), Cosmology and Nongalactic Astrophysics (astro-ph.CO), gravitation: model, [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], interferometer, FOS: Physical sciences, Scale (descriptive set theory), Curvature, 01 natural sciences, statistical analysis, Quantum mechanics, 0103 physical sciences, [ PHYS.PHYS.PHYS-GEN-PH ] Physics [physics]/Physics [physics]/General Physics [physics.gen-ph], dark energy, 010306 general physics, Complement (set theory), Physics, Quantum Physics, 010308 nuclear & particles physics, [PHYS.PHYS.PHYS-GEN-PH]Physics [physics]/Physics [physics]/General Physics [physics.gen-ph], Interferometry, curvature, Quantum electrodynamics, Dark energy, Dilaton, Quantum Physics (quant-ph), [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], dilaton, Dark fluid, Astrophysics - Cosmology and Nongalactic Astrophysics, experimental results, symmetron
Abstract

Atomic interferometry can be used to probe dark energy models coupled to matter. We consider the constraints coming from recent experimental results on models generalising the inverse power law chameleons such as $f(R)$ gravity in the large curvature regime, the environmentally dependent dilaton and symmetrons. Using the tomographic description of these models, we find that only symmetrons with masses smaller than the dark energy scale can be efficiently tested. In this regime, the resulting constraints complement the bounds from the E\"otwash experiment and exclude small values of the symmetron self-coupling., Comment: 26 pages, 3 figures

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