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16 results on '"Clancy W. James"'

1. The Curious Case of Twin Fast Radio Bursts: Evidence for Neutron Star Origin?

Author

Apurba Bera, Clancy W. James, Adam T. Deller, Keith W. Bannister, Ryan M. Shannon, Danica R. Scott, Kelly Gourdji, Lachlan Marnoch, Marcin Glowacki, Ronald D. Ekers, Stuart D. Ryder, and Tyson Dial

Subjects
Time domain astronomy, Radio transient sources, Radio bursts, Astrophysics, QB460-466
Abstract

Fast radio bursts (FRBs) are brilliant short-duration flashes of radio emission originating at cosmological distances. The vast diversity in the properties of currently known FRBs and the fleeting nature of these events make it difficult to understand their progenitors and emission mechanism(s). Here we report high time resolution polarization properties of FRB 20210912A, a highly energetic event detected by the Australian Square Kilometre Array Pathfinder (ASKAP) in the Commensal Real-time ASKAP Fast Transients survey, which show intraburst position angle (PA) variation similar to Galactic pulsars and unusual variation of Faraday rotation measure (RM) across its two sub-bursts. The observed intraburst PA variation and apparent RM variation pattern in FRB 20210912A may be explained by a rapidly spinning neutron star origin, with rest-frame spin periods of ∼1.1 ms. This rotation timescale is comparable to the shortest known rotation period of a pulsar and close to the shortest possible rotation period of a neutron star. Curiously, FRB 20210912A exhibits a remarkable resemblance to the previously reported FRB 20181112A, including similar rest-frame emission timescales and polarization profiles. These observations suggest that these two FRBs may have similar origins.

Published
2024
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2. FLIMFLAM DR1: The First Constraints on the Cosmic Baryon Distribution from Eight Fast Radio Burst Sight Lines

Author

Ilya S. Khrykin, Metin Ata, Khee-Gan Lee, Sunil Simha, Yuxin Huang, J. Xavier Prochaska, Nicolas Tejos, Keith W. Bannister, Jeff Cooke, Cherie K. Day, Adam Deller, Marcin Glowacki, Alexa C. Gordon, Clancy W. James, Lachlan Marnoch, Ryan. M. Shannon, Jielai Zhang, and Lucas Bernales-Cortes

Subjects
Missing mass, Intergalactic gas, Circumgalactic medium, Cosmic web, Redshift surveys, Astrophysics, QB460-466
Abstract

The dispersion measure of fast radio bursts (FRBs), arising from the interactions with free electrons along the propagation path, constitutes a unique probe of the cosmic baryon distribution. Their constraining power is further enhanced in combination with observations of the foreground large-scale structure and intervening galaxies. In this work, we present the first constraints on the partition of the cosmic baryons between the intergalactic medium (IGM) and circumgalactic medium (CGM), inferred from the FLIMFLAM spectroscopic survey. In its first data release, the FLIMFLAM survey targeted galaxies in the foreground of eight localized FRBs. Using Bayesian techniques, we reconstruct the underlying ∼Mpc-scale matter density field that is traced by the IGM gas. Simultaneously, deeper spectroscopy of intervening foreground galaxies (at impact parameters b _⊥ ≲ r _200 ) and the FRB host galaxies constrains the contribution from the CGM. Applying Bayesian parameter inference to our data and assuming a fiducial set of priors, we infer the IGM cosmic baryon fraction to be ${f}_{\mathrm{igm}}={0.59}_{-0.10}^{+0.11}$ and a CGM gas fraction of ${f}_{\mathrm{gas}}={0.55}_{-0.29}^{+0.26}$ for 10 ^10 M _⊙ ≲ M _halo ≲ 10 ^13 M _⊙ halos. The mean FRB host dispersion measure (rest-frame) in our sample is $\langle {\mathrm{DM}}_{\mathrm{host}}\rangle ={90}_{-19}^{+29}\,\mathrm{pc}\ \ {\mathrm{cm}}^{-3}$ , of which $\langle {\mathrm{DM}}_{\mathrm{host}}^{\mathrm{unk}}\rangle ={69}_{-19}^{+28}\,\mathrm{pc}\ \ {\mathrm{cm}}^{-3}$ arises from the host galaxy interstellar medium (ISM) and/or the FRB progenitor environment. While our current f _igm and f _gas uncertainties are too broad to constrain most galactic feedback models, this result marks the first measurement of the IGM and CGM baryon fractions, as well as the first systematic separation of the FRB host dispersion measure into two components: arising from the halo and from the inner ISM/FRB engine.

Published
2024
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3. Mapping Obscured Star Formation in the Host Galaxy of FRB 20201124A

Author

Yuxin Dong, Tarraneh Eftekhari, Wen-fai Fong, Adam T. Deller, Alexandra G. Mannings, Sunil Simha, Navin Sridhar, Marc Rafelski, Alexa C. Gordon, Shivani Bhandari, Cherie K. Day, Kasper E. Heintz, Jason W. T. Hessels, Joel Leja, Clancy W. James, Charles D. Kilpatrick, Elizabeth K. Mahony, Benito Marcote, Ben Margalit, Kenzie Nimmo, J. Xavier Prochaska, Alicia Rouco Escorial, Stuart D. Ryder, Genevieve Schroeder, Ryan M. Shannon, and Nicolas Tejos

Subjects
Magnetars, Star formation, Radio transient sources, Astrophysics, QB460-466
Abstract

We present high-resolution 1.5–6 GHz Karl G. Jansky Very Large Array and Hubble Space Telescope (HST) optical and infrared observations of the extremely active repeating fast radio burst (FRB) FRB 20201124A and its barred spiral host galaxy. We constrain the location and morphology of star formation in the host and search for a persistent radio source (PRS) coincident with FRB 20201124A. We resolve the morphology of the radio emission across all frequency bands and measure a star formation rate (SFR) ≈ 8.9 M _⊙ yr ^−1 , approximately ≈2.5–6 times larger than optically inferred SFRs, demonstrating dust-obscured star formation throughout the host. Compared to a sample of all known FRB hosts with radio emission, the host of FRB 20201124A has the most significantly obscured star formation. While HST observations show the FRB to be offset from the bar or spiral arms, the radio emission extends to the FRB location. We propose that the FRB progenitor could have formed in situ (e.g., a magnetar born from a massive star explosion). It is still plausible, although less likely, that the progenitor of FRB 20201124A migrated from the central bar of the host. We further place a limit on the luminosity of a putative PRS at the FRB position of L _6.0GHz ≲ 1.8 ×10 ^27 erg s ^−1 Hz ^−1 , among the deepest PRS luminosity limits to date. However, this limit is still broadly consistent with both magnetar nebulae and hypernebulae models assuming a constant energy injection rate of the magnetar and an age of ≳10 ^5 yr in each model, respectively.

Published
2024
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4. Is the M81 Fast Radio Burst Host Globular Cluster Special?

Author

Kristen C. Dage, Arash Bahramian, Clancy W. James, Arunav Kundu, Katherine L. Rhode, Jay Strader, Enrico Vesperini, and Stephen E. Zepf

Subjects
Globular star clusters, Radio transient sources, Low-mass x-ray binary stars, Astrophysics, QB460-466
Abstract

We use multiband archival Hubble Space Telescope (HST) observations to measure the photometric and structural parameters of the M81 globular cluster (GC) that hosts the fast radio burst FRB 20200120E. Our best-fitting King model has an effective radius r _h = 3.06 pc with a moderate King model concentration of c = 53, and an inferred core radius of 0.81 pc. We revisit the exact astrometric location of the FRB within the cluster, and find that FRB 20200120E is located 1.92 pc from the center, but within the projected half-light radius. We estimate the relative encounter rate of the FRB host, along with the corresponding rates of 210 other GCs in M81, and compare these values with the encounter rates of Galactic GCs. The FRB resides in a GC with an encounter rate that is moderately higher than the median stellar encounter rate in our two comparison samples. While the estimated encounter rate of the FRB host cluster (e.g., ∼50% of a cluster like 47 Tuc) is sufficient to allow the possibility that the FRB formed dynamically, our results do not place strong constraints on this scenario due to the limitations of the available HST data and the possible systematic uncertainties and selection effects in the comparison data.

Published
2023
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5. Calculation and Uncertainty of Fast Radio Burst Structure Based on Smoothed Data

Author

Adrian T. Sutinjo, Danica R. Scott, Clancy W. James, Marcin Glowacki, Keith W. Bannister, Hyerin Cho, Cherie K. Day, Adam T. Deller, Timothy P. Perrett, and Ryan M. Shannon

Subjects
Radio transient sources, Astrophysics, QB460-466
Abstract

Studies of the time-domain structure of fast radio bursts (FRBs) require an accurate estimate of the FRB dispersion measure in order to recover the intrinsic burst shape. Furthermore, the exact dispersion measure is itself of interest when studying the time evolution of the medium through which multiple bursts from repeating FRBs propagate. A commonly used approach to obtain the dispersion measure is to take the value that maximizes the FRB structure in the time domain. However, various authors use differing methods to obtain this structure parameter and do not document the smoothing method used. Furthermore, there are no quantitative estimates of the error in this procedure in the FRB literature. In this article, we present a smoothing filter based on the discrete cosine transform, and show that computing the structure parameter by summing the squares of the derivatives and taking the square root (that is, the 2-norm, $\sqrt{{\rm{\Sigma }}{(d/{dt})}^{2}}$ ) immediately lends itself to the calculation of the uncertainty of the structure parameter. We illustrate this with FRB 20181112A and FRB 20210117A data, which were detected by the Australian Square Kilometre Array Pathfinder, and for which high-time-resolution data are available.

Published
2023
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6. A Nonrepeating Fast Radio Burst in a Dwarf Host Galaxy

Author

Shivani Bhandari, Alexa C. Gordon, Danica R. Scott, Lachlan Marnoch, Navin Sridhar, Pravir Kumar, Clancy W. James, Hao Qiu, Keith W. Bannister, Adam T. Deller, Tarraneh Eftekhari, Wen-fai Fong, Marcin Glowacki, J. Xavier Prochaska, Stuart D. Ryder, Ryan M. Shannon, and Sunil Simha

Subjects
Radio transient sources, Dwarf galaxies, High time resolution astrophysics, High energy astrophysics, Astrophysics, QB460-466
Abstract

We present the discovery of an as yet nonrepeating fast radio burst (FRB), FRB 20210117A, with the Australian Square Kilometre Array Pathfinder (ASKAP), as a part of the Commensal Real-time ASKAP Fast Transients Survey. The subarcsecond localization of the burst led to the identification of its host galaxy at z = 0.214(1). This redshift is much lower than what would be expected for a source dispersion measure (DM) of 729 pc cm ^−3 , given typical contributions from the intergalactic medium and the host galaxy. Optical observations reveal the host to be a dwarf galaxy with little ongoing star formation—very different to the dwarf host galaxies of the known repeating FRBs 20121102A and 20190520B. We find an excess DM contribution from the host and attribute it to the FRB’s local environment. We do not find any radio emission from the FRB site or host galaxy. The low magnetized environment and the lack of a persistent radio source indicate that the FRB source is older than those found in other dwarf host galaxies, establishing the diversity of FRB sources in dwarf galaxy environments. We find our observations to be fully consistent with the “hypernebula” model, where the FRB is powered by an accretion jet from a hyperaccreting black hole. Finally, our high time resolution analysis reveals burst characteristics similar to those seen in repeating FRBs. We encourage follow-up observations of FRB 20210117A to establish any repeating nature.

Published
2023
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7. The most probable host of CHIME FRB 190425A, associated with binary neutron star merger GW190425, and a late-time transient search

Author

Fiona H Panther, Gemma E Anderson, Shivani Bhandari, Adelle J Goodwin, Natasha Hurley-Walker, Clancy W James, Adela Kawka, Shunke Ai, Manoj Kovalam, Alexandra Moroianu, Linqing Wen, and Bing Zhang

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Space and Planetary Science, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics - High Energy Astrophysical Phenomena
Abstract

The identification and localization of Fast Radio Bursts to their host galaxies has revealed important details about the progenitors of these mysterious, millisecond-long bursts of coherent radio emission. In this work we study the most probable host galaxy of the apparently non-repeating CHIME/FRB event FRB 20190425A -- a particularly high luminosity, low dispersion measure event that was demonstrated by Moroianu et al. 2022 to be temporally and spatially coincident with the LIGO-Virgo-KAGRA binary neutron star merger GW190425, suggesting an astrophysical association (p-value 0.0052). In this paper we remain agnostic to this result, and we confirm UGC10667 as the most probable host galaxy of FRB 20190425A, demonstrating that the host galaxies of low dispersion measure, one-off CHIME FRBs can be plausibly identified. We then perform multi-wavelength observations to characterize the galaxy and search for any afterglow emission associated with the FRB and its putative GW counterpart. We find no radio or optical transient emission in our observations $2.5\,\mathrm{yr}$ post-burst. UGC10667 is a spiral galaxy at $z\sim0.03$, dominated by an old stellar population. We find no evidence of a large population of young stars, with nebular emission dominated by star formation at a rate of $1-2\,\mathrm{M_\odot\,yr^{-1}}$. While we cannot rule out a young magnetar as the origin of FRB 20190425A, our observations are consistent with an origin in a long delay-time neutron star binary merger as posited by Moroianu et al. 2022., 17 pages, 11 figures, accepted for publication in Monthly Notices of the Royal Astronomical Society

Published
2022

9. A non-repeating fast radio burst in a dwarf host galaxy

Author

Shivani Bhandari, Alexa C. Gordon, Danica R. Scott, Lachlan Marnoch, Navin Sridhar, Pravir Kumar, Clancy W. James, Hao Qiu, Keith W. Bannister, Adam T. Deller, Tarraneh Eftekhari, Wen-fai Fong, Marcin Glowacki, J. Xavier Prochaska, Stuart D. Ryder, Ryan M. Shannon, and Sunil Simha

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Astrophysics of Galaxies
Abstract

We present the discovery of as-of-yet non-repeating Fast Radio Burst (FRB), FRB 20210117A, with the Australian Square Kilometer Array Pathfinder (ASKAP) as a part of the Commensal Real-time ASKAP Fast Transients (CRAFT) Survey. The sub-arcsecond localization of the burst led to the identification of its host galaxy at a $z=0.214(1)$. This redshift is much lower than what would be expected for a source dispersion measure (DM) of 729 pc cm$^{-3}$, given typical contributions from the intergalactic medium and the host galaxy. Optical observations reveal the host to be a dwarf galaxy with little on-going star formation, very different to the dwarf host galaxies of known repeating FRBs 20121102A, and 20190520B. We find an excess DM contribution from the host and attribute it to the FRB's local environment. We do not find any radio emission from the FRB site or host galaxy. The low magnetized environment and lack of a persistent radio source (PRS) indicate that the FRB source is older than those found in other dwarf host galaxies, and establish the diversity of FRB sources in dwarf galaxy environments. We find our observations to be fully consistent with the hypernebula model, where the FRB is powered by accretion-jet from a hyper-accreting black hole. Finally, our high-time resolution analysis reveals burst characteristics similar to those seen in repeating FRBs. We encourage follow-up observations of FRB 20210117A to establish any repeating nature., 15 pages, 9 figures, 2 Tables

Published
2022

10. Characterizing the Fast Radio Burst Host Galaxy Population and its Connection to Transients in the Local and Extragalactic Universe

Author

Shivani Bhandari, Kasper E. Heintz, Kshitij Aggarwal, Lachlan Marnoch, Cherie K. Day, Jessica Sydnor, Sarah Burke-Spolaor, Casey J. Law, J. Xavier Prochaska, Nicolas Tejos, Keith W. Bannister, Bryan J. Butler, Adam T. Deller, R. D. Ekers, Chris Flynn, Wen-fai Fong, Clancy W. James, T. Joseph W. Lazio, Rui Luo, Elizabeth K. Mahony, Stuart D. Ryder, Elaine M. Sadler, Ryan M. Shannon, JinLin Han, Kejia Lee, and Bing Zhang

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), ENVIRONMENT, 010308 nuclear & particles physics, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, MASS, 01 natural sciences, DWARF, Astrophysics - Astrophysics of Galaxies, STAR-FORMATION, STELLAR, GLOBULAR-CLUSTER SYSTEM, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), 0103 physical sciences, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

We present the localization and host galaxies of one repeating and two apparently non-repeating Fast Radio Bursts. FRB20180301A was detected and localized with the Karl G. Jansky Very Large Array to a star-forming galaxy at $z=0.3304$. FRB20191228A, and FRB20200906A were detected and localized by the Australian Square Kilometre Array Pathfinder to host galaxies at $z=0.2430$ and $z=0.3688$, respectively. We combine these with 13 other well-localized FRBs in the literature, and analyze the host galaxy properties. We find no significant differences in the host properties of repeating and apparently non-repeating FRBs. FRB hosts are moderately star-forming, with masses slightly offset from the star-forming main-sequence. Star formation and low-ionization nuclear emission-line region (LINER) emission are major sources of ionization in FRB host galaxies, with the former dominant in repeating FRB hosts. FRB hosts do not track stellar mass and star formation as seen in field galaxies (more than 95% confidence). FRBs are rare in massive red galaxies, suggesting that progenitor formation channels are not solely dominated by delayed channels which lag star formation by Gigayears. The global properties of FRB hosts are indistinguishable from core-collapse supernovae (CCSNe) and short gamma-ray bursts (SGRBs) hosts, and the spatial offset (from galaxy centers) of FRBs is mostly inconsistent with that of the Galactic neutron star population (95% confidence). The spatial offsets of FRBs (normalized to the galaxy effective radius) also differ from those of globular clusters (GCs) in late- and early-type galaxies with 95% confidence., 27 pages, 12 figures, 8 tables. Accepted for publication in the Astrophysical Journal

Published
2022

11. An assessment of the Association Between a Fast Radio Burst and Binary Neutron Star Merger

Author

Alexandra Moroianu, Linqing Wen, Clancy W. James, Shunke Ai, Manoj Kovalam, Fiona H. Panther, and Bing Zhang

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics - High Energy Astrophysical Phenomena
Abstract

Fast radio bursts (FRBs) are mysterious bright millisecond-duration radio bursts at cosmological distances. While young magnetars have been put forward as the leading source candidate, recent observations suggest there may be multiple FRB progenitor classes. It has long been theorised that FRBs could be emitted from compact object mergers - cataclysmic events such as binary neutron star (BNS) mergers that may be detectable in gravitational waves (GWs) by the ground-based Laser Interferometer Gravitational Wave Observatory (LIGO)and Virgo. Here we report a potential coincidence between the only BNS merger event GW190425 out of 21 GW sources detected during the first six months of LIGO-Virgo's 3rd Science Run and a bright, non-repeating FRB event, FRB 20190425A, from a search using public GW and CHIME FRB data. The FRB is located within the GW's sky localization area, occurred 2.5 hours after the GW event, and has a dispersion measure consistent with the distance inferred from GW parameter estimation. The chance probability of a coincidence between unrelated FRB and GW events in the databases is estimated to be 0.0052 ($2.8 σ$). We estimate the chance of CHIME detecting such an event to range from 0.4% for a beam-centre detection to 68% if a bright burst is detectable in a far sidelobe. This potential association is consistent with the theory that the BNS merger leaves behind a supramassive, highly magnetized compact object, which collapses to form a black hole after losing angular momentum due to spindown and makes an FRB through ejecting the magnetosphere. If such a physical association is established, the equation of state of the post-merger compact object is likely stiff, with a Tolman-Oppenheimer-Volkoff non-spinning maximum mass $M_{TOV} > 2.63_{-0.23}^{+0.39} M_\odot$ for a neutron star remnant, or $M_{TOV} > 2.31_{-0.08}^{+0.24} M_\odot$ for a quark star remnant., 53 pages, 7 figures, 2 tables

Published
2022
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13. KM3NeT front-end and readout electronics system: hardware, firmware and software

Author

Sebastiano Aiello, Annarita Margiotta, Antonio Marinelli, Christos Markou, Gregory Martignac, Lilian Martin, Juan A. Martínez-Mora, Agnese Martini, Fabio Marzaioli, Safaa Mazzou, Rosa Mele, Karel W. Melis, Pasquale Migliozzi, Emilio Migneco, Piotr Mijakowski, Luis S. Miranda, Carlos M. Mollo, Mauro Morganti, Michael Moser, Abdelilah Moussa, Rasa Muller, Paolo Musico, Mario Musumeci, Lodewijk Nauta, Sergio Navas, Carlo A. Nicolau, Christine Nielsen, Brian Ó Fearraigh, Mukharbek Organokov, Angelo Orlando, Gogita Papalashvili, Riccardo Papaleo, Cosimo Pastore, Gabriela E. Păvălaş, Giuliano Pellegrini, Carmelo Pellegrino, Mathieu Perrin-Terrin, Paolo Piattelli, Camiel Pieterse, Konstantinos Pikounis, Ofelia Pisanti, Chiara Poirè, Georgia Polydefki, Vlad Popa, Maarten Post, Thierry Pradier, Gerd Pühlhofer, Sara Pulvirenti, Liam Quinn, Fabrizio Raffaelli, Nunzio Randazzo, Antonio Rapicavoli, Soebur Razzaque, Diego Real, Stefan Reck, Jonas Reubelt, Giorgio Riccobene, Marc Richer, Louis Rigalleau, Alberto Rovelli, Ilenia Salvadori, Dorothea F. E. Samtleben, Agustin Sánchez Losa, Matteo Sanguineti, Andrea Santangelo, Domenico Santonocito, Piera Sapienza, Jan-Willem Schmelling, Jutta Schnabel, Virginia Sciacca, Jordan Seneca, Irene Sgura, Rezo Shanidze, Ankur Sharma, Francesco Simeone, Anna Sinopoulou, Bernardino Spisso, Maurizio Spurio, Dimitris Stavropoulos, Jos Steijger, Simona M. Stellacci, Bruno Strandberg, Dominik Stransky, Mauro Taiuti, Yahya Tayalati, Enrique Tenllado, Tarak Thakore, Paul Timmer, Steven Tingay, Ekaterini Tzamariudaki, Dimitrios Tzanetatos, Veronique Van Elewyck, Federico Versari, Salvo Viola, Daniele Vivolo, Gwenhael de Wasseige, Joern Wilms, Rafał Wojaczyński, Els de Wolf, Dmitry Zaborov, Angela Zegarelli, Juan D. Zornoza, Juan Zúñiga, Vasilis Panagopoulos, Fabrizio Ameli, Michel Andre, Giorgos Androulakis, Marco Anghinolfi, Gisela Anton, Miquel Ardid, Julien Aublin, Christos Bagatelas, Giancarlo Barbarino, Bruny Baret, Suzan Basegmez du Pree, Anastasios Belias, Meriem Bendahman, Edward Berbee, Ad M. van den Berg, Vincent Bertin, Vincent van Beveren, Simone Biagi, Andrea Biagioni, Matthias Bissinger, Pascal Bos, Jihad Boumaaza, Simon Bourret, Mohammed Bouta, Gilles Bouvet, Mieke Bouwhuis, Cristiano Bozza, Horea Brânzaş, Max M. Briel, Marc Bruchner, Ronald Bruijn, Jurgen Brunner, Ernst-Jan Buis, Raffaele Buompane, Jose Busto, David Calvo, Antonio Capone, Silvia Celli, Mohamed Chabab, Nhan Chau, Silvio Cherubini, Vitaliano Chiarella, Tommaso Chiarusi, Marco Circella, Rosanna Cocimano, Joao A. B. Coelho, Alexis Coleiro, Marta C. Molla, Stephane Colonges, Rosa Coniglione, Paschal Coyle, Alexandre Creusot, Giacomo Cuttone, Antonio D’Amico, Antonio D’Onofrio, Richard Dallier, Mauro De Palma, Irene Di Palma, Antonio F. Díaz, Didac Diego-Tortosa, Carla Distefano, Alba Domi, Roberto Donà, Corinne Donzaud, Damien Dornic, Manuel Dörr, Mora Durocher, Thomas Eberl, Thijs van Eeden, Imad El Bojaddaini, Hassnae Eljarrari, Dominik Elsaesser, Alexander Enzenhöfer, Paolo Fermani, Giovanna Ferrara, Miroslav D. Filipović, Luigi A. Fusco, Deepak Gajanana, Tamas Gal, Alfonso Garcia Soto, Fabio Garufi, Lucio Gialanella, Emidio Giorgio, Sara R. Gozzini, Rodrigo Gracia, Kay Graf, Dario Grasso, Timothee Grégoire, Giuseppe Grella, Daniel Guderian, Carlo Guidi, Steffen Hallmann, Hassane Hamdaoui, Hans van Haren, Aart Heijboer, Amar Hekalo, Juan J. Hernández-Rey, Jannik Hofestädt, Feifei Huang, Enrique H. Santiago, Giulia Illuminati, Clancy W. James, Peter Jansweijer, Martijn Jongen, Maarten de Jong, Paul de Jong, Matthias Kadler, Piotr Kalaczyński, Oleg Kalekin, Uli F. Katz, Nafis R. Khan Chowdhury, Frits van der Knaap, Els N. Koffeman, Paul Kooijman, Antoine Kouchner, Michael Kreter, Vladimir Kulikovskiy, Robert Lahmann, Giuseppina Larosa, Remy Le Breton, Francesco Leone, Emanuele Leonora, Giuseppe Levi, Massimiliano Lincetto, Miles Lindsey Clark, Alessandro Lonardo, Fabio Longhitano, Daniel Lopez-Coto, Giuliano Maggi, Jerzy Mańczak, Karl Mannheim, AstroParticule et Cosmologie (APC (UMR_7164)), 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), Centre de Physique des Particules de Marseille (CPPM), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Aix Marseille Université (AMU), Laboratoire de physique subatomique et des technologies associées (SUBATECH), Université de Nantes - Faculté des Sciences et des Techniques, 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), Institut de Recherches Subatomiques (IReS), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Cancéropôle du Grand Est-Centre National de la Recherche Scientifique (CNRS), Institut Universitaire de France (IUF), Ministère de l'Education nationale, de l’Enseignement supérieur et de la Recherche (M.E.N.E.S.R.), KM3NeT, 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), Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-IMT Atlantique (IMT Atlantique), Institut Mines-Télécom [Paris] (IMT)-Institut Mines-Télécom [Paris] (IMT)-Nantes université - UFR des Sciences et des Techniques (Nantes univ - UFR ST), Nantes Université - pôle Sciences et technologie, Nantes Université (Nantes Univ)-Nantes Université (Nantes Univ)-Nantes Université - pôle Sciences et technologie, Nantes Université (Nantes Univ)-Nantes Université (Nantes Univ), Institut Pluridisciplinaire Hubert Curien (IPHC), Université de Strasbourg (UNISTRA)-Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA))-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Aiello, Sebastiano, Margiotta, Annarita, Marinelli, Antonio, Markou, Christo, Martignac, Gregory, Martin, Lilian, Martínez-Mora, Juan A., Martini, Agnese, Marzaioli, Fabio, Mazzou, Safaa, Mele, Rosa, Melis, Karel W., Migliozzi, Pasquale, Migneco, Emilio, Mijakowski, Piotr, Miranda, Luis S., Mollo, Carlos M., Morganti, Mauro, Moser, Michael, Moussa, Abdelilah, Muller, Rasa, Musico, Paolo, Musumeci, Mario, Nauta, Lodewijk, Navas, Sergio, Nicolau, Carlo A., Nielsen, Christine, Fearraigh, Brian Ó, Organokov, Mukharbek, Orlando, Angelo, Papalashvili, Gogita, Papaleo, Riccardo, Pastore, Cosimo, Păvălaş, Gabriela E., Pellegrini, Giuliano, Pellegrino, Carmelo, Perrin-Terrin, Mathieu, Piattelli, Paolo, Pieterse, Camiel, Pikounis, Konstantino, Pisanti, Ofelia, Poirè, Chiara, Polydefki, Georgia, Popa, Vlad, Post, Maarten, Pradier, Thierry, Pühlhofer, Gerd, Pulvirenti, Sara, Quinn, Liam, Raffaelli, Fabrizio, Randazzo, Nunzio, Rapicavoli, Antonio, Razzaque, Soebur, Real, Diego, Reck, Stefan, Reubelt, Jona, Riccobene, Giorgio, Richer, Marc, Rigalleau, Loui, Rovelli, Alberto, Salvadori, Ilenia, Samtleben, Dorothea F. E., Sánchez Losa, Agustin, Sanguineti, Matteo, Santangelo, Andrea, Santonocito, Domenico, Sapienza, Piera, Schmelling, Jan-Willem, Schnabel, Jutta, Sciacca, Virginia, Seneca, Jordan, Sgura, Irene, Shanidze, Rezo, Sharma, Ankur, Simeone, Francesco, Sinopoulou, Anna, Spisso, Bernardino, Spurio, Maurizio, Stavropoulos, Dimitri, Steijger, Jo, Stellacci, Simona M., Strandberg, Bruno, Stransky, Dominik, Taiuti, Mauro, Tayalati, Yahya, Tenllado, Enrique, Thakore, Tarak, Timmer, Paul, Tingay, Steven, Tzamariudaki, Ekaterini, Tzanetatos, Dimitrio, Van Elewyck, Veronique, Versari, Federico, Viola, Salvo, Vivolo, Daniele, de Wasseige, Gwenhael, Wilms, Joern, Wojaczyński, Rafał, de Wolf, El, Zaborov, Dmitry, Zegarelli, Angela, Zornoza, Juan D., Zúñiga, Juan, Panagopoulos, Vasili, Ameli, Fabrizio, Andre, Michel, Androulakis, Giorgo, Anghinolfi, Marco, Anton, Gisela, Ardid, Miquel, Aublin, Julien, Bagatelas, Christo, Barbarino, Giancarlo, Baret, Bruny, Basegmez du Pree, Suzan, Belias, Anastasio, Bendahman, Meriem, Berbee, Edward, van den Berg, Ad M., Bertin, Vincent, van Beveren, Vincent, Biagi, Simone, Biagioni, Andrea, Bissinger, Matthia, Bos, Pascal, Boumaaza, Jihad, Bourret, Simon, Bouta, Mohammed, Bouvet, Gille, Bouwhuis, Mieke, Bozza, Cristiano, Brânzaş, Horea, Briel, Max M., Bruchner, Marc, Bruijn, Ronald, Brunner, Jurgen, Buis, Ernst-Jan, Buompane, Raffaele, Busto, Jose, Calvo, David, Capone, Antonio, Celli, Silvia, Chabab, Mohamed, Chau, Nhan, Cherubini, Silvio, Chiarella, Vitaliano, Chiarusi, Tommaso, Circella, Marco, Cocimano, Rosanna, Coelho, Joao A. B., Coleiro, Alexi, Molla, Marta C., Colonges, Stephane, Coniglione, Rosa, Coyle, Paschal, Creusot, Alexandre, Cuttone, Giacomo, D’Amico, Antonio, D’Onofrio, Antonio, Dallier, Richard, De Palma, Mauro, Di Palma, Irene, Díaz, Antonio F., Diego-Tortosa, Didac, Distefano, Carla, Domi, Alba, Donà, Roberto, Donzaud, Corinne, Dornic, Damien, Dörr, Manuel, Durocher, Mora, Eberl, Thoma, van Eeden, Thij, El Bojaddaini, Imad, Eljarrari, Hassnae, Elsaesser, Dominik, Enzenhöfer, Alexander, Fermani, Paolo, Ferrara, Giovanna, Filipović, Miroslav D., Fusco, Luigi A., Gajanana, Deepak, Gal, Tama, Garcia Soto, Alfonso, Garufi, Fabio, Gialanella, Lucio, Giorgio, Emidio, Gozzini, Sara R., Gracia, Rodrigo, Graf, Kay, Grasso, Dario, Grégoire, Timothee, Grella, Giuseppe, Guderian, Daniel, Guidi, Carlo, Hallmann, Steffen, Hamdaoui, Hassane, van Haren, Han, Heijboer, Aart, Hekalo, Amar, Hernández-Rey, Juan J., Hofestädt, Jannik, Huang, Feifei, Santiago, Enrique H., Illuminati, Giulia, James, Clancy W., Jansweijer, Peter, Jongen, Martijn, de Jong, Maarten, de Jong, Paul, Kadler, Matthia, Kalaczyński, Piotr, Kalekin, Oleg, Katz, Uli F., Khan Chowdhury, Nafis R., van der Knaap, Frit, Koffeman, Els N., Kooijman, Paul, Kouchner, Antoine, Kreter, Michael, Kulikovskiy, Vladimir, Lahmann, Robert, Larosa, Giuseppina, Le Breton, Remy, Leone, Francesco, Leonora, Emanuele, Levi, Giuseppe, Lincetto, Massimiliano, Lindsey Clark, Mile, Lonardo, Alessandro, Longhitano, Fabio, Lopez-Coto, Daniel, Maggi, Giuliano, Mańczak, Jerzy, Mannheim, Karl, Centre Tecnològic de Vilanova i la Geltrú, Universitat Politècnica de Catalunya. LAB - Laboratori d'Aplicacions Bioacústiques, Sebastiano Aiello, Fabrizio Ameli, Michel Andre, Giorgos Androulaki, Marco Anghinolfi, Gisela Anton, Miquel Ardid, Julien Aublin, Christos Bagatela, Giancarlo Barbarino, Bruny Baret, Suzan Basegmez du Pree, Anastasios Belia, Meriem Bendahman, Edward Berbee, Ad M. van den Berg, Vincent Bertin, Vincent van Beveren, Simone Biagi, Andrea Biagioni, Matthias Bissinger, Pascal Bo, Jihad Boumaaza, Simon Bourret, Mohammed Bouta, Gilles Bouvet, Mieke Bouwhui, Cristiano Bozza, Horea Brânza, Max M. Briel, Marc Bruchner, Ronald Bruijn, Jurgen Brunner, Ernst-Jan Bui, Raffaele Buompane, Jose Busto, David Calvo, Antonio Capone, Silvia Celli, Mohamed Chabab, Nhan Chau, Silvio Cherubini, Vitaliano Chiarella, Tommaso Chiarusi, Marco Circella, Rosanna Cocimano, Joao A. B. Coelho, Alexis Coleiro, Marta C. Molla, Stephane Colonge, Rosa Coniglione, Paschal Coyle, Alexandre Creusot, Giacomo Cuttone, Antonio D’Amico, Antonio D’Onofrio, Richard Dallier, Mauro De Palma, Irene Di Palma, Antonio F. Díaz, Didac Diego-Tortosa, Carla Distefano, Alba Domi, Roberto Donà, Corinne Donzaud, Damien Dornic, Manuel Dörr, Mora Durocher, Thomas Eberl, Thijs van Eeden, Imad El Bojaddaini, Hassnae Eljarrari, Dominik Elsaesser, Alexander Enzenhöfer, Paolo Fermani, Giovanna Ferrara, Miroslav D. Filipovic ́, Luigi A. Fusco, Deepak Gajanana, Tamas Gal, Alfonso Garcia Soto, Fabio Garufi, Lucio Gialanella, Emidio Giorgio, Sara R. Gozzini, Rodrigo Gracia, Kay Graf, Dario Grasso, Timothee Grégoire, Giuseppe Grella, Daniel Guderian, Carlo Guidi, Steffen Hallmann, Hassane Hamdaoui, Hans van Haren, Aart Heijboer, Amar Hekalo, Juan J. Hernández-Rey, Jannik Hofestädt, Feifei Huang, Enrique H. Santiago, Giulia Illuminati, Clancy W. Jame, Peter Jansweijer, Martijn Jongen, Maarten de Jong, Paul de Jong, Matthias Kadler, Piotr Kalaczynski, Oleg Kalekin, Uli F. Katz, Nafis R. Khan Chowdhury, Frits van der Knaap, Els N. Koffeman, Paul Kooijman, Antoine Kouchner, Michael Kreter, Vladimir Kulikovskiy, Robert Lahmann, Giuseppina Larosa, Remy Le Breton, Francesco Leone, Emanuele Leonora, Giuseppe Levi, Massimiliano Lincetto, Miles Lindsey Clark, Alessandro Lonardo, Fabio Longhitano, Daniel Lopez-Coto, Giuliano Maggi, Jerzy Ma ́nczak, Karl Mannheim, Annarita Margiotta, Antonio Marinelli, Christos Markou, Gregory Martignac, Lilian Martin, Juan A. Martínez-Mora, Agnese Martini, Fabio Marzaioli, Safaa Mazzou, Rosa MeleKarel W. Meli, Pasquale Migliozzi, Emilio Migneco, Piotr Mijakowski, Luis S. Miranda, Carlos M. Mollo, Mauro Morganti, Michael Moser, Abdelilah Moussa, Rasa Muller, Paolo Musico, Mario Musumeci, Lodewijk Nauta, Sergio Nava, Carlo A. Nicolau, Christine Nielsen, Brian Ó Fearraigh, Mukharbek Organokov, Angelo Orlando, Vasilis Panagopoulo, Gogita Papalashvili, Riccardo Papaleo, Cosimo Pastore, Gabriela E. Păvăla ̧, Giuliano Pellegrini, Carmelo Pellegrino, Mathieu Perrin-Terrin, Paolo Piattelli, Camiel Pieterse, Konstantinos Pikouni, Ofelia Pisanti, Chiara Poirè, Georgia Polydefki, Vlad Popa, Maarten Post, Thierry Pradier, Gerd Pühlhofer, Sara Pulvirenti, Liam Quinn, Fabrizio Raffaelli, Nunzio Randazzo, Antonio Rapicavoli, Soebur Razzaque, Diego Real, Stefan Reck, Jonas Reubelt, Giorgio Riccobene, Marc Richer, Louis Rigalleau, Alberto Rovelli, Ilenia Salvadori, Dorothea F. E. Samtleben, Agustin Sánchez Losa, Matteo Sanguineti, Andrea Santangelo, Domenico Santonocito, Piera Sapienza, Jan-Willem Schmelling, Jutta Schnabel, Virginia Sciacca, Jordan Seneca, Irene Sgura, Rezo Shanidze, Ankur Sharma, Francesco Simeone, Anna Sinopoulou, Bernardino Spisso, Maurizio Spurio, Dimitris Stavropoulo, Jos Steijger, Simona M. Stellacci, Bruno Strandberg, Dominik Stransky, Mauro Taiuti, Yahya Tayalati, Enrique Tenllado, Tarak Thakore, Paul Timmer, Steven Tingay, Ekaterini Tzamariudaki, Dimitrios Tzanetato, Veronique Van Elewyck, Federico Versari, Salvo Viola, Daniele Vivolo, Gwenhael de Wasseige, Joern Wilm, Rafał Wojaczy ́nski, Els de Wolf, Dmitry Zaborov, Angela Zegarelli, Juan D. Zornoza, Juan Zúñiga, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Université de Nantes - UFR des Sciences et des Techniques (UN UFR ST), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Strasbourg (UNISTRA)-Centre National de la Recherche Scientifique (CNRS), Ministerio de Economía y Competitividad (España), Ministerio de Ciencia, Innovación y Universidades (España), 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), 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), Research unit Astroparticle Physics, and 33379009 - Kreter, Michael

Subjects
Astrofísica, data acquisition, Computer science, Physics::Instrumentation and Detectors, readout electronics, sensors, Astrophysics, Neutrino telescope, computer.software_genre, 7. Clean energy, 01 natural sciences, Signal, Synchronization (alternating current), Front and back ends, Front-end electronics, readout electronics, neutrino telescope, KM3NeT, Front-end electronics, KM3NeT, Readout electronics, 010303 astronomy & astrophysics, Instrumentation, field programmable gate arrays, Firmware, electronics, 4. Education, Electrical engineering, Astrophysics::Instrumentation and Methods for Astrophysics, front-end electronics, Electronic, Optical and Magnetic Materials, Astrophysics - Instrumentation and Methods for Astrophysics, Photomultiplier, clocks, front-end electronic, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Partícules (Física nuclear), 010309 optics, 0103 physical sciences, Neutrins, readout electronic, 14. Life underwater, Electronics, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], Instrumentation and Methods for Astrophysics (astro-ph.IM), Cherenkov radiation, Particles (Nuclear physics), Detectors òptics, logic, Optical detectors, Física [Àrees temàtiques de la UPC], Telescopis, business.industry, Mechanical Engineering, neutrino telescope, Astronomy and Astrophysics, Space and Planetary Science, Control and Systems Engineering, FISICA APLICADA, business, computer, Telescopes
Abstract

[EN] The KM3NeT research infrastructure being built at the bottom of the Mediterranean Sea will host water-Cherenkov telescopes for the detection of cosmic neutrinos. The neutrino telescopes will consist of large volume three-dimensional grids of optical modules to detect the Cherenkov light from charged particles produced by neutrino-induced interactions. Each optical module houses 31 3-in. photomultiplier tubes, instrumentation for calibration of the photomultiplier signal and positioning of the optical module, and all associated electronics boards. By design, the total electrical power consumption of an optical module has been capped at seven Watts. We present an overview of the front-end and readout electronics system inside the optical module, which has been designed for a 1-ns synchronization between the clocks of all optical modules in the grid during a life time of at least 20 years., The authors acknowledge financial support from the funding agencies: Agence Nationale de la Recherche (Grant No. ANR-15-CE31-0020), Centre National de la Recherche Scientifique (CNRS), Commission Europeenne (FEDER fund and Marie Curie Program), Institut Universitaire de France (IUF), IdEx program and UnivEarthS Labex program at Sorbonne Paris Cite (Grant Nos. ANR-10-LABX-0023 and ANR-11-IDEX-0005-02), Paris Ile-de-France Region, France; Shota Rustaveli National Science Foundation of Georgia (SRNSFG, Grant No. FR-18-1268), Georgia; Deutsche Forschungsgemeinschaft (DFG), Germany; The General Secretariat of Research and Technology (GSRT), Greece; Istituto Nazionale di Fisica Nucleare (INFN), Ministero dell'Istruzione, dell'Universita e della Ricerca (MIUR), PRIN 2017 program (Grant NAT-NET 2017W4HA7S) Italy; Ministry of Higher Education, Scientific Research and Professional Training, Morocco; Nederlandse organisatie voor Wetenschappelijk Onderzoek (NWO), the Netherlands; The National Science Centre, Poland (2015/18/E/ST2/00758); National Authority for Scientific Research (ANCS), Romania; Plan Estatal de Investigacion [refs. FPA2015-65150-C3-1-P, -2-P and -3-P, (MINECO/FEDER)], Severo Ochoa Centre of Excellence program (MINECO), Red Consolider MultiDark (ref. FPA2017-90566-REDC, MINECO), and Prometeo and Grisolia programs (Generalitat Valenciana), "la Caixa" Foundation (ID 100010434) through the fellowship LCF/BQ/IN17/11620019, and the European Union's Horizon 2020 research and innovation programme under the Marie Sklodowska-Curie Grant Agreement No. 713673, Spain.

Published
2019

14. Studies of intrinsic resolution of low energy electron and muon neutrino events with neutrino telescopes

Author

Clancy W. James and J. Hofestädt

Subjects
Physics, Particle physics, Photon, Muon, Physics::Instrumentation and Detectors, Astrophysics::High Energy Astrophysical Phenomena, Detector, Electron, Nuclear physics, KM3NeT, Neutrino detector, High Energy Physics::Experiment, Muon neutrino, Neutrino
Abstract

Existing large-volume neutrino telescopes such as ANTARES and IceCube, as well as the future KM3NeT/ARCA, investigate neutrinos at characteristic particle energies of 10 TeV, whereas KM3NeT/ORCA and PINGU will operate around 10 GeV to determine the neutrino mass hierarchy by measuring the energy and direction of atmospheric neutrinos. In this energy regime, intrinsic fluctuations in particle behaviour become important. These intrinsic fluctuations are investigated to answer two basic questions. Firstly: How do intrinsic fluctuations limit the reconstruction accuracy of an perfect detector, i.e. if every single photon is detected? While this requires making some basic assumptions about the methods used in the reconstruction, the answer to this question will indicate the optimum that could be achieved by any detector. Secondly: Given that only a finite number of photons will be detected, what is the best possible reconstruction accuracy in the case of a ideal use of the information carried by these photons? For this study the baseline design of the KM3NeT/ORCA detector is used. This investigation separately considers muon tracks, and electromagnetic and hadronic cascades. By combining these results limits on the best possible reconstruction accuracy in energy and direction for the initial neutrinos achievable with an ORCA-type detector are derived.

Published
2016

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