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28 results on '"Campana MA"'

1. Search for 10–1000 GeV Neutrinos from Gamma-Ray Bursts with IceCube

Author: Abbasi, R, Abbasi, R, Ackermann, M, Adams, J, Agarwalla, SK, Aguilar, JA, Ahlers, M, Alameddine, JM, Amin, NM, Andeen, K, Anton, G, Argüelles, C, Ashida, Y, Athanasiadou, S, Ausborm, L, Axani, SN, Bai, X, V., A Balagopal, Baricevic, M, Barwick, SW, Basu, V, Bay, R, Beatty, JJ, Tjus, J Becker, Beise, J, Bellenghi, C, Benning, C, BenZvi, S, Berley, D, Bernardini, E, Besson, DZ, Blaufuss, E, Blot, S, Bontempo, F, Book, JY, Meneguolo, C Boscolo, Böser, S, Botner, O, Böttcher, J, Braun, J, Brinson, B, Brostean-Kaiser, J, Brusa, L, Burley, RT, Busse, RS, Butterfield, D, Campana, MA, Carloni, K, Carnie-Bronca, EG, Chattopadhyay, S, Chau, N, Chen, C, Chen, Z, Chirkin, D, Choi, S, Clark, BA, Coleman, A, Collin, GH, Connolly, A, Conrad, JM, Coppin, P, Correa, P, Cowen, DF, Dave, P, De Clercq, C, DeLaunay, JJ, Delgado, D, Deng, S, Deoskar, K, Desai, A, Desiati, P, de Vries, KD, de Wasseige, G, DeYoung, T, Diaz, A, Díaz-Vélez, JC, Dittmer, M, Domi, A, Dujmovic, H, DuVernois, MA, Ehrhardt, T, Eimer, A, Eller, P, Ellinger, E, Mentawi, S El, Elsässer, D, Engel, R, Erpenbeck, H, Evans, J, Evenson, PA, Fan, KL, Fang, K, Farrag, K, Fazely, AR, Fedynitch, A, Feigl, N, Fiedlschuster, S, Finley, C, Fischer, L, Fox, D, Franckowiak, A, Abbasi, R, Abbasi, R, Ackermann, M, Adams, J, Agarwalla, SK, Aguilar, JA, Ahlers, M, Alameddine, JM, Amin, NM, Andeen, K, Anton, G, Argüelles, C, Ashida, Y, Athanasiadou, S, Ausborm, L, Axani, SN, Bai, X, V., A Balagopal, Baricevic, M, Barwick, SW, Basu, V, Bay, R, Beatty, JJ, Tjus, J Becker, Beise, J, Bellenghi, C, Benning, C, BenZvi, S, Berley, D, Bernardini, E, Besson, DZ, Blaufuss, E, Blot, S, Bontempo, F, Book, JY, Meneguolo, C Boscolo, Böser, S, Botner, O, Böttcher, J, Braun, J, Brinson, B, Brostean-Kaiser, J, Brusa, L, Burley, RT, Busse, RS, Butterfield, D, Campana, MA, Carloni, K, Carnie-Bronca, EG, Chattopadhyay, S, Chau, N, Chen, C, Chen, Z, Chirkin, D, Choi, S, Clark, BA, Coleman, A, Collin, GH, Connolly, A, Conrad, JM, Coppin, P, Correa, P, Cowen, DF, Dave, P, De Clercq, C, DeLaunay, JJ, Delgado, D, Deng, S, Deoskar, K, Desai, A, Desiati, P, de Vries, KD, de Wasseige, G, DeYoung, T, Diaz, A, Díaz-Vélez, JC, Dittmer, M, Domi, A, Dujmovic, H, DuVernois, MA, Ehrhardt, T, Eimer, A, Eller, P, Ellinger, E, Mentawi, S El, Elsässer, D, Engel, R, Erpenbeck, H, Evans, J, Evenson, PA, Fan, KL, Fang, K, Farrag, K, Fazely, AR, Fedynitch, A, Feigl, N, Fiedlschuster, S, Finley, C, Fischer, L, Fox, D, and Franckowiak, A
Abstract: We present the results of a search for 10-1000 GeV neutrinos from 2268 gamma-ray bursts (GRBs) over 8 yr of IceCube-DeepCore data. This work probes burst physics below the photosphere where electromagnetic radiation cannot escape. Neutrinos of tens of giga electronvolts are predicted in sub-photospheric collision of free-streaming neutrons with bulk-jet protons. In a first analysis, we searched for the most significant neutrino-GRB coincidence using six overlapping time windows centered on the prompt phase of each GRB. In a second analysis, we conducted a search for a group of GRBs, each individually too weak to be detectable, but potentially significant when combined. No evidence of neutrino emission is found for either analysis. The most significant neutrino coincidence is for Fermi-GBM GRB bn 140807500, with a p-value of 0.097 corrected for all trials. The binomial test used to search for a group of GRBs had a p-value of 0.65 after all trial corrections. The binomial test found a group consisting only of GRB bn 140807500 and no additional GRBs. The neutrino limits of this work complement those obtained by IceCube at tera electronvolt to peta electronvolt energies. We compare our findings for the large set of GRBs as well as GRB 221009A to the sub-photospheric neutron-proton collision model and find that GRB 221009A provides the most constraining limit on baryon loading. For a jet Lorentz factor of 300 (800), the baryon loading on GRB 221009A is lower than 3.85 (2.13) at a 90% confidence level.
Published: 2024

2. A Search for IceCube Sub-TeV Neutrinos Correlated with Gravitational-wave Events Detected By LIGO/Virgo

Author: Abbasi, R, Abbasi, R, Ackermann, M, Adams, J, Agarwalla, SK, Aguilar, JA, Ahlers, M, Alameddine, JM, Amin, NM, Andeen, K, Anton, G, Argüelles, C, Ashida, Y, Athanasiadou, S, Axani, SN, Bai, X, V., A Balagopal, Baricevic, M, Barwick, SW, Basu, V, Bay, R, Beatty, JJ, Becker, K-H, Tjus, J Becker, Beise, J, Bellenghi, C, BenZvi, S, Berley, D, Bernardini, E, Besson, DZ, Binder, G, Bindig, D, Blaufuss, E, Blot, S, Bontempo, F, Book, JY, Meneguolo, C Boscolo, Böser, S, Botner, O, Böttcher, J, Bourbeau, E, Braun, J, Brinson, B, Brostean-Kaiser, J, Burley, RT, Busse, RS, Butterfield, D, Campana, MA, Carloni, K, Carnie-Bronca, EG, Chattopadhyay, S, Chau, N, Chen, C, Chen, Z, Chirkin, D, Choi, S, Clark, BA, Classen, L, Coleman, A, Collin, GH, Connolly, A, Conrad, JM, Coppin, P, Correa, P, Countryman, S, Cowen, DF, Dave, P, De Clercq, C, DeLaunay, JJ, López, D Delgado, Dembinski, H, Deoskar, K, Desai, A, Desiati, P, de Vries, KD, de Wasseige, G, DeYoung, T, Diaz, A, Díaz-Vélez, JC, Dittmer, M, Domi, A, Dujmovic, H, DuVernois, MA, Ehrhardt, T, Eller, P, Engel, R, Erpenbeck, H, Evans, J, Evenson, PA, Fan, KL, Fang, K, Fazely, AR, Fedynitch, A, Feigl, N, Fiedlschuster, S, Finley, C, Fischer, L, Fox, D, Franckowiak, A, Friedman, E, Fritz, A, Abbasi, R, Abbasi, R, Ackermann, M, Adams, J, Agarwalla, SK, Aguilar, JA, Ahlers, M, Alameddine, JM, Amin, NM, Andeen, K, Anton, G, Argüelles, C, Ashida, Y, Athanasiadou, S, Axani, SN, Bai, X, V., A Balagopal, Baricevic, M, Barwick, SW, Basu, V, Bay, R, Beatty, JJ, Becker, K-H, Tjus, J Becker, Beise, J, Bellenghi, C, BenZvi, S, Berley, D, Bernardini, E, Besson, DZ, Binder, G, Bindig, D, Blaufuss, E, Blot, S, Bontempo, F, Book, JY, Meneguolo, C Boscolo, Böser, S, Botner, O, Böttcher, J, Bourbeau, E, Braun, J, Brinson, B, Brostean-Kaiser, J, Burley, RT, Busse, RS, Butterfield, D, Campana, MA, Carloni, K, Carnie-Bronca, EG, Chattopadhyay, S, Chau, N, Chen, C, Chen, Z, Chirkin, D, Choi, S, Clark, BA, Classen, L, Coleman, A, Collin, GH, Connolly, A, Conrad, JM, Coppin, P, Correa, P, Countryman, S, Cowen, DF, Dave, P, De Clercq, C, DeLaunay, JJ, López, D Delgado, Dembinski, H, Deoskar, K, Desai, A, Desiati, P, de Vries, KD, de Wasseige, G, DeYoung, T, Diaz, A, Díaz-Vélez, JC, Dittmer, M, Domi, A, Dujmovic, H, DuVernois, MA, Ehrhardt, T, Eller, P, Engel, R, Erpenbeck, H, Evans, J, Evenson, PA, Fan, KL, Fang, K, Fazely, AR, Fedynitch, A, Feigl, N, Fiedlschuster, S, Finley, C, Fischer, L, Fox, D, Franckowiak, A, Friedman, E, and Fritz, A
Abstract: The LIGO/Virgo collaboration published the catalogs GWTC-1, GWTC-2.1, and GWTC-3 containing candidate gravitational-wave (GW) events detected during its runs O1, O2, and O3. These GW events can be possible sites of neutrino emission. In this paper, we present a search for neutrino counterparts of 90 GW candidates using IceCube DeepCore, the low-energy infill array of the IceCube Neutrino Observatory. The search is conducted using an unbinned maximum likelihood method, within a time window of 1000 s, and uses the spatial and timing information from the GW events. The neutrinos used for the search have energies ranging from a few GeV to several tens of TeV. We do not find any significant emission of neutrinos, and place upper limits on the flux and the isotropic-equivalent energy emitted in low-energy neutrinos. We also conduct a binomial test to search for source populations potentially contributing to neutrino emission. We report a nondetection of a significant neutrino-source population with this test.
Published: 2023

3. Search for neutrino lines from dark matter annihilation and decay with IceCube

Author: Abbasi, R, Abbasi, R, Ackermann, M, Adams, J, Agarwalla, SK, Aguilar, JA, Ahlers, M, Alameddine, JM, Amin, NM, Andeen, K, Anton, G, Argüelles, C, Ashida, Y, Athanasiadou, S, Axani, SN, Bai, X, Balagopal, A, Baricevic, M, Barwick, SW, Basu, V, Baur, S, Bay, R, Beatty, JJ, Becker, K-H, Tjus, J Becker, Beise, J, Bellenghi, C, BenZvi, S, Berley, D, Bernardini, E, Besson, DZ, Binder, G, Bindig, D, Blaufuss, E, Blot, S, Bontempo, F, Book, JY, Meneguolo, C Boscolo, Böser, S, Botner, O, Böttcher, J, Bourbeau, E, Braun, J, Brinson, B, Brostean-Kaiser, J, Burley, RT, Busse, RS, Butterfield, D, Campana, MA, Carloni, K, Carnie-Bronca, EG, Chattopadhyay, S, Chau, N, Chen, C, Chen, Z, Chirkin, D, Choi, S, Clark, BA, Classen, L, Coleman, A, Collin, GH, Connolly, A, Conrad, JM, Coppin, P, Correa, P, Countryman, S, Cowen, DF, Dave, P, De Clercq, C, DeLaunay, JJ, López, D Delgado, Dembinski, H, Deoskar, K, Desai, A, Desiati, P, de Vries, KD, de Wasseige, G, DeYoung, T, Diaz, A, Díaz-Vélez, JC, Dittmer, M, Domi, A, Dujmovic, H, DuVernois, MA, Ehrhardt, T, Aisati, C El, Eller, P, Engel, R, Erpenbeck, H, Evans, J, Evenson, PA, Fan, KL, Fang, K, Fazely, AR, Fedynitch, A, Feigl, N, Fiedlschuster, S, Finley, C, Fischer, L, Fox, D, Franckowiak, A, Abbasi, R, Abbasi, R, Ackermann, M, Adams, J, Agarwalla, SK, Aguilar, JA, Ahlers, M, Alameddine, JM, Amin, NM, Andeen, K, Anton, G, Argüelles, C, Ashida, Y, Athanasiadou, S, Axani, SN, Bai, X, Balagopal, A, Baricevic, M, Barwick, SW, Basu, V, Baur, S, Bay, R, Beatty, JJ, Becker, K-H, Tjus, J Becker, Beise, J, Bellenghi, C, BenZvi, S, Berley, D, Bernardini, E, Besson, DZ, Binder, G, Bindig, D, Blaufuss, E, Blot, S, Bontempo, F, Book, JY, Meneguolo, C Boscolo, Böser, S, Botner, O, Böttcher, J, Bourbeau, E, Braun, J, Brinson, B, Brostean-Kaiser, J, Burley, RT, Busse, RS, Butterfield, D, Campana, MA, Carloni, K, Carnie-Bronca, EG, Chattopadhyay, S, Chau, N, Chen, C, Chen, Z, Chirkin, D, Choi, S, Clark, BA, Classen, L, Coleman, A, Collin, GH, Connolly, A, Conrad, JM, Coppin, P, Correa, P, Countryman, S, Cowen, DF, Dave, P, De Clercq, C, DeLaunay, JJ, López, D Delgado, Dembinski, H, Deoskar, K, Desai, A, Desiati, P, de Vries, KD, de Wasseige, G, DeYoung, T, Diaz, A, Díaz-Vélez, JC, Dittmer, M, Domi, A, Dujmovic, H, DuVernois, MA, Ehrhardt, T, Aisati, C El, Eller, P, Engel, R, Erpenbeck, H, Evans, J, Evenson, PA, Fan, KL, Fang, K, Fazely, AR, Fedynitch, A, Feigl, N, Fiedlschuster, S, Finley, C, Fischer, L, Fox, D, and Franckowiak, A
Abstract: Dark matter particles in the Galactic Center and halo can annihilate or decay into a pair of neutrinos producing a monochromatic flux of neutrinos. The spectral feature of this signal is unique and it is not expected from any astrophysical production mechanism. Its observation would constitute a dark matter smoking gun signal. We performed the first dedicated search with a neutrino telescope for such signal, by looking at both the angular and energy information of the neutrino events. To this end, a total of five years of IceCube's DeepCore data has been used to test dark matter masses ranging from 10 GeV to 40 TeV. No significant neutrino excess was found and upper limits on the annihilation cross section, as well as lower limits on the dark matter lifetime, were set. The limits reached are of the order of 10-24 cm3/s for an annihilation and up to 1027 s for decaying dark matter. Using the same data sample we also derive limits for dark matter annihilation or decay into a pair of Standard Model charged particles.
Published: 2023

4. IceCat-1: The IceCube Event Catalog of Alert Tracks

Author: Abbasi, R, Abbasi, R, Ackermann, M, Adams, J, Agarwalla, SK, Aguilar, JA, Ahlers, M, Alameddine, JM, Amin, NM, Andeen, K, Anton, G, Argüelles, C, Ashida, Y, Athanasiadou, S, Axani, SN, Bai, X, Balagopal, A, Baricevic, M, Barwick, SW, Basu, V, Bay, R, Beatty, JJ, Becker, K-H, Tjus, J Becker, Beise, J, Bellenghi, C, BenZvi, S, Berley, D, Bernardini, E, Besson, DZ, Binder, G, Bindig, D, Blaufuss, E, Blot, S, Bontempo, F, Book, JY, Meneguolo, C Boscolo, Böser, S, Botner, O, Böttcher, J, Bourbeau, E, Braun, J, Brinson, B, Brostean-Kaiser, J, Burley, RT, Busse, RS, Butterfield, D, Campana, MA, Carloni, K, Carnie-Bronca, EG, Chattopadhyay, S, Chau, N, Chen, C, Chen, Z, Chirkin, D, Choi, S, Clark, BA, Classen, L, Coleman, A, Collin, GH, Connolly, A, Conrad, JM, Coppin, P, Correa, P, Countryman, S, Cowen, DF, Dave, P, De Clercq, C, DeLaunay, JJ, Delgado, D, Dembinski, H, Deng, S, Deoskar, K, Desai, A, Desiati, P, de Vries, KD, de Wasseige, G, DeYoung, T, Diaz, A, Díaz-Vélez, JC, Dittmer, M, Domi, A, Dujmovic, H, DuVernois, MA, Ehrhardt, T, Eller, P, Engel, R, Erpenbeck, H, Evans, J, Evenson, PA, Fan, KL, Fang, K, Farrag, K, Fazely, AR, Fedynitch, A, Feigl, N, Fiedlschuster, S, Finley, C, Fischer, L, Fox, D, Franckowiak, A, Abbasi, R, Abbasi, R, Ackermann, M, Adams, J, Agarwalla, SK, Aguilar, JA, Ahlers, M, Alameddine, JM, Amin, NM, Andeen, K, Anton, G, Argüelles, C, Ashida, Y, Athanasiadou, S, Axani, SN, Bai, X, Balagopal, A, Baricevic, M, Barwick, SW, Basu, V, Bay, R, Beatty, JJ, Becker, K-H, Tjus, J Becker, Beise, J, Bellenghi, C, BenZvi, S, Berley, D, Bernardini, E, Besson, DZ, Binder, G, Bindig, D, Blaufuss, E, Blot, S, Bontempo, F, Book, JY, Meneguolo, C Boscolo, Böser, S, Botner, O, Böttcher, J, Bourbeau, E, Braun, J, Brinson, B, Brostean-Kaiser, J, Burley, RT, Busse, RS, Butterfield, D, Campana, MA, Carloni, K, Carnie-Bronca, EG, Chattopadhyay, S, Chau, N, Chen, C, Chen, Z, Chirkin, D, Choi, S, Clark, BA, Classen, L, Coleman, A, Collin, GH, Connolly, A, Conrad, JM, Coppin, P, Correa, P, Countryman, S, Cowen, DF, Dave, P, De Clercq, C, DeLaunay, JJ, Delgado, D, Dembinski, H, Deng, S, Deoskar, K, Desai, A, Desiati, P, de Vries, KD, de Wasseige, G, DeYoung, T, Diaz, A, Díaz-Vélez, JC, Dittmer, M, Domi, A, Dujmovic, H, DuVernois, MA, Ehrhardt, T, Eller, P, Engel, R, Erpenbeck, H, Evans, J, Evenson, PA, Fan, KL, Fang, K, Farrag, K, Fazely, AR, Fedynitch, A, Feigl, N, Fiedlschuster, S, Finley, C, Fischer, L, Fox, D, and Franckowiak, A
Abstract: We present a catalog of likely astrophysical neutrino track-like events from the IceCube Neutrino Observatory. IceCube began reporting likely astrophysical neutrinos in 2016, and this system was updated in 2019. The catalog presented here includes events that were reported in real time since 2019, as well as events identified in archival data samples starting from 2011. We report 275 neutrino events from two selection channels as the first entries in the catalog, the IceCube Event Catalog of Alert Tracks, which will see ongoing extensions with additional alerts. The Gold and Bronze alert channels respectively provide neutrino candidates with a 50% and 30% probability of being astrophysical, on average assuming an astrophysical neutrino power-law energy spectral index of 2.19. For each neutrino alert, we provide the reconstructed energy, direction, false-alarm rate, probability of being astrophysical in origin, and likelihood contours describing the spatial uncertainty in the alert's reconstructed location. We also investigate a directional correlation of these neutrino events with gamma-ray and X-ray catalogs, including 4FGL, 3HWC, TeVCat, and Swift-BAT.
Published: 2023

5. Constraining High-energy Neutrino Emission from Supernovae with IceCube

Author: Abbasi, R, Abbasi, R, Ackermann, M, Adams, J, Agarwalla, SK, Aguilar, JA, Ahlers, M, Alameddine, JM, Amin, NM, Andeen, K, Anton, G, Argüelles, C, Ashida, Y, Athanasiadou, S, Axani, SN, Bai, X, V., A Balagopal, Baricevic, M, Barwick, SW, Basu, V, Bay, R, Beatty, JJ, Becker, K-H, Tjus, J Becker, Beise, J, Bellenghi, C, BenZvi, S, Berley, D, Bernardini, E, Besson, DZ, Binder, G, Bindig, D, Blaufuss, E, Blot, S, Bontempo, F, Book, JY, Meneguolo, C Boscolo, Böser, S, Botner, O, Böttcher, J, Bourbeau, E, Braun, J, Brinson, B, Brostean-Kaiser, J, Burley, RT, Busse, RS, Butterfield, D, Campana, MA, Carloni, K, Carnie-Bronca, EG, Chattopadhyay, S, Chen, C, Chen, Z, Chirkin, D, Choi, S, Clark, BA, Classen, L, Coleman, A, Collin, GH, Connolly, A, Conrad, JM, Coppin, P, Correa, P, Countryman, S, Cowen, DF, Dave, P, De Clercq, C, DeLaunay, JJ, López, D Delgado, Dembinski, H, Deoskar, K, Desai, A, Desiati, P, de Vries, KD, de Wasseige, G, DeYoung, T, Diaz, A, Díaz-Vélez, JC, Dittmer, M, Domi, A, Dujmovic, H, DuVernois, MA, Ehrhardt, T, Eller, P, Engel, R, Erpenbeck, H, Evans, J, Evenson, PA, Fan, KL, Fang, K, Fazely, AR, Fedynitch, A, Feigl, N, Fiedlschuster, S, Finley, C, Fischer, L, Fox, D, Franckowiak, A, Friedman, E, Fritz, A, Fürst, P, Abbasi, R, Abbasi, R, Ackermann, M, Adams, J, Agarwalla, SK, Aguilar, JA, Ahlers, M, Alameddine, JM, Amin, NM, Andeen, K, Anton, G, Argüelles, C, Ashida, Y, Athanasiadou, S, Axani, SN, Bai, X, V., A Balagopal, Baricevic, M, Barwick, SW, Basu, V, Bay, R, Beatty, JJ, Becker, K-H, Tjus, J Becker, Beise, J, Bellenghi, C, BenZvi, S, Berley, D, Bernardini, E, Besson, DZ, Binder, G, Bindig, D, Blaufuss, E, Blot, S, Bontempo, F, Book, JY, Meneguolo, C Boscolo, Böser, S, Botner, O, Böttcher, J, Bourbeau, E, Braun, J, Brinson, B, Brostean-Kaiser, J, Burley, RT, Busse, RS, Butterfield, D, Campana, MA, Carloni, K, Carnie-Bronca, EG, Chattopadhyay, S, Chen, C, Chen, Z, Chirkin, D, Choi, S, Clark, BA, Classen, L, Coleman, A, Collin, GH, Connolly, A, Conrad, JM, Coppin, P, Correa, P, Countryman, S, Cowen, DF, Dave, P, De Clercq, C, DeLaunay, JJ, López, D Delgado, Dembinski, H, Deoskar, K, Desai, A, Desiati, P, de Vries, KD, de Wasseige, G, DeYoung, T, Diaz, A, Díaz-Vélez, JC, Dittmer, M, Domi, A, Dujmovic, H, DuVernois, MA, Ehrhardt, T, Eller, P, Engel, R, Erpenbeck, H, Evans, J, Evenson, PA, Fan, KL, Fang, K, Fazely, AR, Fedynitch, A, Feigl, N, Fiedlschuster, S, Finley, C, Fischer, L, Fox, D, Franckowiak, A, Friedman, E, Fritz, A, and Fürst, P
Abstract: Core-collapse supernovae are a promising potential high-energy neutrino source class. We test for correlation between seven years of IceCube neutrino data and a catalog containing more than 1000 core-collapse supernovae of types IIn and IIP and a sample of stripped-envelope supernovae. We search both for neutrino emission from individual supernovae as well as for combined emission from the whole supernova sample, through a stacking analysis. No significant spatial or temporal correlation of neutrinos with the cataloged supernovae was found. All scenarios were tested against the background expectation and together yield an overall p-value of 93%; therefore, they show consistency with the background only. The derived upper limits on the total energy emitted in neutrinos are 1.7 × 1048 erg for stripped-envelope supernovae, 2.8 × 1048 erg for type IIP, and 1.3 × 1049 erg for type IIn SNe, the latter disfavoring models with optimistic assumptions for neutrino production in interacting supernovae. We conclude that stripped-envelope supernovae and supernovae of type IIn do not contribute more than 14.6% and 33.9%, respectively, to the diffuse neutrino flux in the energy range of about [ 103-105] GeV, assuming that the neutrino energy spectrum follows a power-law with an index of −2.5. Under the same assumption, we can only constrain the contribution of type IIP SNe to no more than 59.9%. Thus, core-collapse supernovae of types IIn and stripped-envelope supernovae can both be ruled out as the dominant source of the diffuse neutrino flux under the given assumptions.
Published: 2023

6. Constraints on Populations of Neutrino Sources from Searches in the Directions of IceCube Neutrino Alerts

Author: Abbasi, R, Abbasi, R, Ackermann, M, Adams, J, Aggarwal, N, Aguilar, JA, Ahlers, M, Alameddine, JM, Alves, AA, Amin, NM, Andeen, K, Anderson, T, Anton, G, Argüelles, C, Ashida, Y, Athanasiadou, S, Axani, SN, Bai, X, V., A Balagopal, Baricevic, M, Barwick, SW, Basu, V, Bay, R, Beatty, JJ, Becker, K-H, Tjus, J Becker, Beise, J, Bellenghi, C, Benda, S, BenZvi, S, Berley, D, Bernardini, E, Besson, DZ, Binder, G, Bindig, D, Blaufuss, E, Blot, S, Bontempo, F, Book, JY, Borowka, J, Meneguolo, C Boscolo, Böser, S, Botner, O, Böttcher, J, Bourbeau, E, Braun, J, Brinson, B, Brostean-Kaiser, J, Burley, RT, Busse, RS, Campana, MA, Carnie-Bronca, EG, Chen, C, Chen, Z, Chirkin, D, Choi, K, Clark, BA, Classen, L, Coleman, A, Collin, GH, Connolly, A, Conrad, JM, Coppin, P, Correa, P, Countryman, S, Cowen, DF, Cross, R, Dappen, C, Dave, P, De Clercq, C, DeLaunay, JJ, López, D Delgado, Dembinski, H, Deoskar, K, Desai, A, Desiati, P, de Vries, KD, de Wasseige, G, DeYoung, T, Diaz, A, Díaz-Vélez, JC, Dittmer, M, Dujmovic, H, DuVernois, MA, Ehrhardt, T, Eller, P, Engel, R, Erpenbeck, H, Evans, J, Evenson, PA, Fan, KL, Fazely, AR, Fedynitch, A, Feigl, N, Fiedlschuster, S, Fienberg, AT, Finley, C, Fischer, L, Fox, D, Franckowiak, A, Friedman, E, Abbasi, R, Abbasi, R, Ackermann, M, Adams, J, Aggarwal, N, Aguilar, JA, Ahlers, M, Alameddine, JM, Alves, AA, Amin, NM, Andeen, K, Anderson, T, Anton, G, Argüelles, C, Ashida, Y, Athanasiadou, S, Axani, SN, Bai, X, V., A Balagopal, Baricevic, M, Barwick, SW, Basu, V, Bay, R, Beatty, JJ, Becker, K-H, Tjus, J Becker, Beise, J, Bellenghi, C, Benda, S, BenZvi, S, Berley, D, Bernardini, E, Besson, DZ, Binder, G, Bindig, D, Blaufuss, E, Blot, S, Bontempo, F, Book, JY, Borowka, J, Meneguolo, C Boscolo, Böser, S, Botner, O, Böttcher, J, Bourbeau, E, Braun, J, Brinson, B, Brostean-Kaiser, J, Burley, RT, Busse, RS, Campana, MA, Carnie-Bronca, EG, Chen, C, Chen, Z, Chirkin, D, Choi, K, Clark, BA, Classen, L, Coleman, A, Collin, GH, Connolly, A, Conrad, JM, Coppin, P, Correa, P, Countryman, S, Cowen, DF, Cross, R, Dappen, C, Dave, P, De Clercq, C, DeLaunay, JJ, López, D Delgado, Dembinski, H, Deoskar, K, Desai, A, Desiati, P, de Vries, KD, de Wasseige, G, DeYoung, T, Diaz, A, Díaz-Vélez, JC, Dittmer, M, Dujmovic, H, DuVernois, MA, Ehrhardt, T, Eller, P, Engel, R, Erpenbeck, H, Evans, J, Evenson, PA, Fan, KL, Fazely, AR, Fedynitch, A, Feigl, N, Fiedlschuster, S, Fienberg, AT, Finley, C, Fischer, L, Fox, D, Franckowiak, A, and Friedman, E
Abstract: Beginning in 2016, the IceCube Neutrino Observatory has sent out alerts in real time containing the information of high-energy (E ≳ 100 TeV) neutrino candidate events with moderate to high (≳30%) probability of astrophysical origin. In this work, we use a recent catalog of such alert events, which, in addition to events announced in real time, includes events that were identified retroactively and covers the time period of 2011-2020. We also search for additional, lower-energy neutrinos from the arrival directions of these IceCube alerts. We show how performing such an analysis can constrain the contribution of rare populations of cosmic neutrino sources to the diffuse astrophysical neutrino flux. After searching for neutrino emission coincident with these alert events on various timescales, we find no significant evidence of either minute-scale or day-scale transient neutrino emission or of steady neutrino emission in the direction of these alert events. This study also shows how numerous a population of neutrino sources has to be to account for the complete astrophysical neutrino flux. Assuming that sources have the same luminosity, an E −2.5 neutrino spectrum, and number densities that follow star formation rates, the population of sources has to be more numerous than 7 × 10−9 Mpc−3. This number changes to 3 × 10−7 Mpc−3 if number densities instead have no cosmic evolution.
Published: 2023

7. First all-flavor search for transient neutrino emission using 3-years of IceCube DeepCore data

Author: Abbasi, R, Abbasi, R, Ackermann, M, Adams, J, Aguilar, JA, Ahlers, M, Ahrens, M, Alispach, C, Alves, AA, Amin, NM, Andeen, K, Anderson, T, Ansseau, I, Anton, G, Argüelles, C, Axani, S, Bai, X, Balagopal, VA, Barbano, A, Barwick, SW, Bastian, B, Basu, V, Baum, V, Baur, S, Bay, R, Beatty, JJ, Becker, KH, Becker Tjus, J, Bellenghi, C, Benzvi, S, Berley, D, Bernardini, E, Besson, DZ, Binder, G, Bindig, D, Blaufuss, E, Blot, S, Böser, S, Botner, O, Böttcher, J, Bourbeau, E, Bourbeau, J, Bradascio, F, Braun, J, Bron, S, Brostean-Kaiser, J, Burgman, A, Busse, RS, Campana, MA, Chen, C, Chirkin, D, Choi, S, Clark, BA, Clark, K, Classen, L, Coleman, A, Collin, GH, Conrad, JM, Coppin, P, Correa, P, Cowen, DF, Cross, R, Dave, P, De Clercq, C, Delaunay, JJ, Dembinski, H, Deoskar, K, De Ridder, S, Desai, A, Desiati, P, De Vries, KD, De Wasseige, G, De With, M, Deyoung, T, Dharani, S, Diaz, A, Díaz-Vélez, JC, Dujmovic, H, Dunkman, M, Duvernois, MA, Dvorak, E, Ehrhardt, T, Eller, P, Engel, R, Evans, J, Evenson, PA, Fahey, S, Fazely, AR, Fiedlschuster, S, Fienberg, AT, Filimonov, K, Finley, C, Fischer, L, Fox, D, Franckowiak, A, Friedman, E, Fritz, A, Fürst, P, Gaisser, TK, Gallagher, J, Ganster, E, Abbasi, R, Abbasi, R, Ackermann, M, Adams, J, Aguilar, JA, Ahlers, M, Ahrens, M, Alispach, C, Alves, AA, Amin, NM, Andeen, K, Anderson, T, Ansseau, I, Anton, G, Argüelles, C, Axani, S, Bai, X, Balagopal, VA, Barbano, A, Barwick, SW, Bastian, B, Basu, V, Baum, V, Baur, S, Bay, R, Beatty, JJ, Becker, KH, Becker Tjus, J, Bellenghi, C, Benzvi, S, Berley, D, Bernardini, E, Besson, DZ, Binder, G, Bindig, D, Blaufuss, E, Blot, S, Böser, S, Botner, O, Böttcher, J, Bourbeau, E, Bourbeau, J, Bradascio, F, Braun, J, Bron, S, Brostean-Kaiser, J, Burgman, A, Busse, RS, Campana, MA, Chen, C, Chirkin, D, Choi, S, Clark, BA, Clark, K, Classen, L, Coleman, A, Collin, GH, Conrad, JM, Coppin, P, Correa, P, Cowen, DF, Cross, R, Dave, P, De Clercq, C, Delaunay, JJ, Dembinski, H, Deoskar, K, De Ridder, S, Desai, A, Desiati, P, De Vries, KD, De Wasseige, G, De With, M, Deyoung, T, Dharani, S, Diaz, A, Díaz-Vélez, JC, Dujmovic, H, Dunkman, M, Duvernois, MA, Dvorak, E, Ehrhardt, T, Eller, P, Engel, R, Evans, J, Evenson, PA, Fahey, S, Fazely, AR, Fiedlschuster, S, Fienberg, AT, Filimonov, K, Finley, C, Fischer, L, Fox, D, Franckowiak, A, Friedman, E, Fritz, A, Fürst, P, Gaisser, TK, Gallagher, J, and Ganster, E
Abstract: Since the discovery of a flux of high-energy astrophysical neutrinos, searches for their origins have focused primarily at TeV-PeV energies. Compared to sub-TeV searches, high-energy searches benefit from an increase in the neutrino cross section, improved angular resolution on the neutrino direction, and a reduced background from atmospheric neutrinos and muons. However, the focus on high energy does not preclude the existence of sub-TeV neutrino emission where IceCube retains sensitivity. Here we present the first all-flavor search from IceCube for transient emission of low-energy neutrinos, focusing on the energy region of 5.6-100 GeV using three years of data obtained with the IceCube-DeepCore detector. We find no evidence of transient neutrino emission in the data, thus leading to a constraint on the volumetric rate of astrophysical transient sources in the range of ∼ 705-2301 Gpc-3 yr-1 for sources following a subphotospheric energy spectrum with a mean energy of 100 GeV and a bolometric energy of 1052 erg.
Published: 2022

8. Search for GeV-scale dark matter annihilation in the Sun with IceCube DeepCore

Author: Abbasi, R, Abbasi, R, Ackermann, M, Adams, J, Aguilar, JA, Ahlers, M, Ahrens, M, Alameddine, JM, Alispach, C, Alves, AA, Amin, NM, Andeen, K, Anderson, T, Anton, G, Argüelles, C, Ashida, Y, Axani, S, Bai, X, Balagopal, A, Barbano, A, Barwick, SW, Bastian, B, Basu, V, Baur, S, Bay, R, Beatty, JJ, Becker, KH, Becker Tjus, J, Bellenghi, C, Benzvi, S, Berley, D, Bernardini, E, Besson, DZ, Binder, G, Bindig, D, Blaufuss, E, Blot, S, Boddenberg, M, Bontempo, F, Borowka, J, Böser, S, Botner, O, Böttcher, J, Bourbeau, E, Bradascio, F, Braun, J, Brinson, B, Bron, S, Brostean-Kaiser, J, Browne, S, Burgman, A, Burley, RT, Busse, RS, Campana, MA, Carnie-Bronca, EG, Chen, C, Chen, Z, Chirkin, D, Choi, K, Clark, BA, Clark, K, Classen, L, Coleman, A, Collin, GH, Conrad, JM, Coppin, P, Correa, P, Cowen, DF, Cross, R, Dappen, C, Dave, P, De Clercq, C, Delaunay, JJ, Delgado López, D, Dembinski, H, Deoskar, K, Desai, A, Desiati, P, De Vries, KD, De Wasseige, G, De With, M, Deyoung, T, Diaz, A, Díaz-Vélez, JC, Dittmer, M, Dujmovic, H, Dunkman, M, Duvernois, MA, Dvorak, E, Ehrhardt, T, Eller, P, Engel, R, Erpenbeck, H, Evans, J, Evenson, PA, Fan, KL, Fazely, AR, Feigl, N, Fiedlschuster, S, Fienberg, AT, Filimonov, K, Abbasi, R, Abbasi, R, Ackermann, M, Adams, J, Aguilar, JA, Ahlers, M, Ahrens, M, Alameddine, JM, Alispach, C, Alves, AA, Amin, NM, Andeen, K, Anderson, T, Anton, G, Argüelles, C, Ashida, Y, Axani, S, Bai, X, Balagopal, A, Barbano, A, Barwick, SW, Bastian, B, Basu, V, Baur, S, Bay, R, Beatty, JJ, Becker, KH, Becker Tjus, J, Bellenghi, C, Benzvi, S, Berley, D, Bernardini, E, Besson, DZ, Binder, G, Bindig, D, Blaufuss, E, Blot, S, Boddenberg, M, Bontempo, F, Borowka, J, Böser, S, Botner, O, Böttcher, J, Bourbeau, E, Bradascio, F, Braun, J, Brinson, B, Bron, S, Brostean-Kaiser, J, Browne, S, Burgman, A, Burley, RT, Busse, RS, Campana, MA, Carnie-Bronca, EG, Chen, C, Chen, Z, Chirkin, D, Choi, K, Clark, BA, Clark, K, Classen, L, Coleman, A, Collin, GH, Conrad, JM, Coppin, P, Correa, P, Cowen, DF, Cross, R, Dappen, C, Dave, P, De Clercq, C, Delaunay, JJ, Delgado López, D, Dembinski, H, Deoskar, K, Desai, A, Desiati, P, De Vries, KD, De Wasseige, G, De With, M, Deyoung, T, Diaz, A, Díaz-Vélez, JC, Dittmer, M, Dujmovic, H, Dunkman, M, Duvernois, MA, Dvorak, E, Ehrhardt, T, Eller, P, Engel, R, Erpenbeck, H, Evans, J, Evenson, PA, Fan, KL, Fazely, AR, Feigl, N, Fiedlschuster, S, Fienberg, AT, and Filimonov, K
Abstract: The Sun provides an excellent target for studying spin-dependent dark matter-proton scattering due to its high matter density and abundant hydrogen content. Dark matter particles from the Galactic halo can elastically interact with Solar nuclei, resulting in their capture and thermalization in the Sun. The captured dark matter can annihilate into Standard Model particles including an observable flux of neutrinos. We present the results of a search for low-energy (<500 GeV) neutrinos correlated with the direction of the Sun using 7 years of IceCube data. This work utilizes, for the first time, new optimized cuts to extend IceCube's sensitivity to dark matter mass down to 5 GeV. We find no significant detection of neutrinos from the Sun. Our observations exclude capture by spin-dependent dark matter-proton scattering with cross section down to a few times 10-41 cm2, assuming there is equilibrium with annihilation into neutrinos/antineutrinos for dark matter masses between 5 GeV and 100 GeV. These are the strongest constraints at GeV energies for dark matter annihilation directly to neutrinos.
Published: 2022

9. Search for High-energy Neutrino Emission from Galactic X-Ray Binaries with IceCube

Author: Abbasi, R, Abbasi, R, Ackermann, M, Adams, J, Aguilar, JA, Ahlers, M, Ahrens, M, Alameddine, JM, Alves, AA, Amin, NM, Andeen, K, Anderson, T, Anton, G, Arguëlles, C, Ashida, Y, Axani, S, Bai, X, V., AB, Barwick, SW, Bastian, B, Basu, V, Baur, S, Bay, R, Beatty, JJ, Becker, KH, Tjus, JB, Beise, J, Bellenghi, C, Benda, S, Benzvi, S, Berley, D, Bernardini, E, Besson, DZ, Binder, G, Bindig, D, Blaufuss, E, Blot, S, Boddenberg, M, Bontempo, F, Borowka, J, Böser, S, Botner, O, Böttcher, J, Bourbeau, E, Bradascio, F, Braun, J, Brinson, B, Bron, S, Brostean-Kaiser, J, Browne, S, Burgman, A, Burley, RT, Busse, RS, Campana, MA, Carnie-Bronca, EG, Chen, C, Chen, Z, Chirkin, D, Choi, K, Clark, BA, Clark, K, Classen, L, Coleman, A, Collin, GH, Conrad, JM, Coppin, P, Correa, P, Cowen, DF, Cross, R, Dappen, C, Dave, P, De Clercq, C, Delaunay, JJ, López, DD, Dembinski, H, Deoskar, K, Desai, A, Desiati, P, De Vries, KD, De Wasseige, G, De With, M, Deyoung, T, Diaz, A, Diáz-Vélez, JC, Dittmer, M, Dujmovic, H, Dunkman, M, Duvernois, MA, Ehrhardt, T, Eller, P, Engel, R, Erpenbeck, H, Evans, J, Evenson, PA, Fan, KL, Fazely, AR, Fedynitch, A, Feigl, N, Fiedlschuster, S, Fienberg, AT, Finley, C, Abbasi, R, Abbasi, R, Ackermann, M, Adams, J, Aguilar, JA, Ahlers, M, Ahrens, M, Alameddine, JM, Alves, AA, Amin, NM, Andeen, K, Anderson, T, Anton, G, Arguëlles, C, Ashida, Y, Axani, S, Bai, X, V., AB, Barwick, SW, Bastian, B, Basu, V, Baur, S, Bay, R, Beatty, JJ, Becker, KH, Tjus, JB, Beise, J, Bellenghi, C, Benda, S, Benzvi, S, Berley, D, Bernardini, E, Besson, DZ, Binder, G, Bindig, D, Blaufuss, E, Blot, S, Boddenberg, M, Bontempo, F, Borowka, J, Böser, S, Botner, O, Böttcher, J, Bourbeau, E, Bradascio, F, Braun, J, Brinson, B, Bron, S, Brostean-Kaiser, J, Browne, S, Burgman, A, Burley, RT, Busse, RS, Campana, MA, Carnie-Bronca, EG, Chen, C, Chen, Z, Chirkin, D, Choi, K, Clark, BA, Clark, K, Classen, L, Coleman, A, Collin, GH, Conrad, JM, Coppin, P, Correa, P, Cowen, DF, Cross, R, Dappen, C, Dave, P, De Clercq, C, Delaunay, JJ, López, DD, Dembinski, H, Deoskar, K, Desai, A, Desiati, P, De Vries, KD, De Wasseige, G, De With, M, Deyoung, T, Diaz, A, Diáz-Vélez, JC, Dittmer, M, Dujmovic, H, Dunkman, M, Duvernois, MA, Ehrhardt, T, Eller, P, Engel, R, Erpenbeck, H, Evans, J, Evenson, PA, Fan, KL, Fazely, AR, Fedynitch, A, Feigl, N, Fiedlschuster, S, Fienberg, AT, and Finley, C
Abstract: We present the first comprehensive search for high-energy neutrino emission from high- A nd low-mass X-ray binaries conducted by IceCube. Galactic X-ray binaries are long-standing candidates for the source of Galactic hadronic cosmic rays and neutrinos. The compact object in these systems can be the site of cosmic-ray acceleration, and neutrinos can be produced by interactions of cosmic rays with radiation or gas, in the jet of a microquasar, in the stellar wind, or in the atmosphere of the companion star. We study X-ray binaries using 7.5 yr of IceCube data with three separate analyses. In the first, we search for periodic neutrino emission from 55 binaries in the Northern Sky with known orbital periods. In the second, the X-ray light curves of 102 binaries across the entire sky are used as templates to search for time-dependent neutrino emission. Finally, we search for time-integrated emission of neutrinos for a list of 4 notable binaries identified as microquasars. In the absence of a significant excess, we place upper limits on the neutrino flux for each hypothesis and compare our results with theoretical predictions for several binaries. In addition, we evaluate the sensitivity of the next generation neutrino telescope at the South Pole, IceCube-Gen2, and demonstrate its power to identify potential neutrino emission from these binary sources in the Galaxy.
Published: 2022

10. Search for GeV-scale dark matter annihilation in the Sun with IceCube DeepCore

Author: Abbasi, R, Abbasi, R, Ackermann, M, Adams, J, Aguilar, JA, Ahlers, M, Ahrens, M, Alameddine, JM, Alispach, C, Alves, AA, Amin, NM, Andeen, K, Anderson, T, Anton, G, Argüelles, C, Ashida, Y, Axani, S, Bai, X, Balagopal, A, Barbano, A, Barwick, SW, Bastian, B, Basu, V, Baur, S, Bay, R, Beatty, JJ, Becker, KH, Becker Tjus, J, Bellenghi, C, Benzvi, S, Berley, D, Bernardini, E, Besson, DZ, Binder, G, Bindig, D, Blaufuss, E, Blot, S, Boddenberg, M, Bontempo, F, Borowka, J, Böser, S, Botner, O, Böttcher, J, Bourbeau, E, Bradascio, F, Braun, J, Brinson, B, Bron, S, Brostean-Kaiser, J, Browne, S, Burgman, A, Burley, RT, Busse, RS, Campana, MA, Carnie-Bronca, EG, Chen, C, Chen, Z, Chirkin, D, Choi, K, Clark, BA, Clark, K, Classen, L, Coleman, A, Collin, GH, Conrad, JM, Coppin, P, Correa, P, Cowen, DF, Cross, R, Dappen, C, Dave, P, De Clercq, C, Delaunay, JJ, Delgado López, D, Dembinski, H, Deoskar, K, Desai, A, Desiati, P, De Vries, KD, De Wasseige, G, De With, M, Deyoung, T, Diaz, A, Díaz-Vélez, JC, Dittmer, M, Dujmovic, H, Dunkman, M, Duvernois, MA, Dvorak, E, Ehrhardt, T, Eller, P, Engel, R, Erpenbeck, H, Evans, J, Evenson, PA, Fan, KL, Fazely, AR, Feigl, N, Fiedlschuster, S, Fienberg, AT, Filimonov, K, Abbasi, R, Abbasi, R, Ackermann, M, Adams, J, Aguilar, JA, Ahlers, M, Ahrens, M, Alameddine, JM, Alispach, C, Alves, AA, Amin, NM, Andeen, K, Anderson, T, Anton, G, Argüelles, C, Ashida, Y, Axani, S, Bai, X, Balagopal, A, Barbano, A, Barwick, SW, Bastian, B, Basu, V, Baur, S, Bay, R, Beatty, JJ, Becker, KH, Becker Tjus, J, Bellenghi, C, Benzvi, S, Berley, D, Bernardini, E, Besson, DZ, Binder, G, Bindig, D, Blaufuss, E, Blot, S, Boddenberg, M, Bontempo, F, Borowka, J, Böser, S, Botner, O, Böttcher, J, Bourbeau, E, Bradascio, F, Braun, J, Brinson, B, Bron, S, Brostean-Kaiser, J, Browne, S, Burgman, A, Burley, RT, Busse, RS, Campana, MA, Carnie-Bronca, EG, Chen, C, Chen, Z, Chirkin, D, Choi, K, Clark, BA, Clark, K, Classen, L, Coleman, A, Collin, GH, Conrad, JM, Coppin, P, Correa, P, Cowen, DF, Cross, R, Dappen, C, Dave, P, De Clercq, C, Delaunay, JJ, Delgado López, D, Dembinski, H, Deoskar, K, Desai, A, Desiati, P, De Vries, KD, De Wasseige, G, De With, M, Deyoung, T, Diaz, A, Díaz-Vélez, JC, Dittmer, M, Dujmovic, H, Dunkman, M, Duvernois, MA, Dvorak, E, Ehrhardt, T, Eller, P, Engel, R, Erpenbeck, H, Evans, J, Evenson, PA, Fan, KL, Fazely, AR, Feigl, N, Fiedlschuster, S, Fienberg, AT, and Filimonov, K
Abstract: The Sun provides an excellent target for studying spin-dependent dark matter-proton scattering due to its high matter density and abundant hydrogen content. Dark matter particles from the Galactic halo can elastically interact with Solar nuclei, resulting in their capture and thermalization in the Sun. The captured dark matter can annihilate into Standard Model particles including an observable flux of neutrinos. We present the results of a search for low-energy (<500 GeV) neutrinos correlated with the direction of the Sun using 7 years of IceCube data. This work utilizes, for the first time, new optimized cuts to extend IceCube's sensitivity to dark matter mass down to 5 GeV. We find no significant detection of neutrinos from the Sun. Our observations exclude capture by spin-dependent dark matter-proton scattering with cross section down to a few times 10-41 cm2, assuming there is equilibrium with annihilation into neutrinos/antineutrinos for dark matter masses between 5 GeV and 100 GeV. These are the strongest constraints at GeV energies for dark matter annihilation directly to neutrinos.
Published: 2022

11. First all-flavor search for transient neutrino emission using 3-years of IceCube DeepCore data

Author: Abbasi, R, Abbasi, R, Ackermann, M, Adams, J, Aguilar, JA, Ahlers, M, Ahrens, M, Alispach, C, Alves, AA, Amin, NM, Andeen, K, Anderson, T, Ansseau, I, Anton, G, Argüelles, C, Axani, S, Bai, X, Balagopal, VA, Barbano, A, Barwick, SW, Bastian, B, Basu, V, Baum, V, Baur, S, Bay, R, Beatty, JJ, Becker, KH, Becker Tjus, J, Bellenghi, C, Benzvi, S, Berley, D, Bernardini, E, Besson, DZ, Binder, G, Bindig, D, Blaufuss, E, Blot, S, Böser, S, Botner, O, Böttcher, J, Bourbeau, E, Bourbeau, J, Bradascio, F, Braun, J, Bron, S, Brostean-Kaiser, J, Burgman, A, Busse, RS, Campana, MA, Chen, C, Chirkin, D, Choi, S, Clark, BA, Clark, K, Classen, L, Coleman, A, Collin, GH, Conrad, JM, Coppin, P, Correa, P, Cowen, DF, Cross, R, Dave, P, De Clercq, C, Delaunay, JJ, Dembinski, H, Deoskar, K, De Ridder, S, Desai, A, Desiati, P, De Vries, KD, De Wasseige, G, De With, M, Deyoung, T, Dharani, S, Diaz, A, Díaz-Vélez, JC, Dujmovic, H, Dunkman, M, Duvernois, MA, Dvorak, E, Ehrhardt, T, Eller, P, Engel, R, Evans, J, Evenson, PA, Fahey, S, Fazely, AR, Fiedlschuster, S, Fienberg, AT, Filimonov, K, Finley, C, Fischer, L, Fox, D, Franckowiak, A, Friedman, E, Fritz, A, Fürst, P, Gaisser, TK, Gallagher, J, Ganster, E, Abbasi, R, Abbasi, R, Ackermann, M, Adams, J, Aguilar, JA, Ahlers, M, Ahrens, M, Alispach, C, Alves, AA, Amin, NM, Andeen, K, Anderson, T, Ansseau, I, Anton, G, Argüelles, C, Axani, S, Bai, X, Balagopal, VA, Barbano, A, Barwick, SW, Bastian, B, Basu, V, Baum, V, Baur, S, Bay, R, Beatty, JJ, Becker, KH, Becker Tjus, J, Bellenghi, C, Benzvi, S, Berley, D, Bernardini, E, Besson, DZ, Binder, G, Bindig, D, Blaufuss, E, Blot, S, Böser, S, Botner, O, Böttcher, J, Bourbeau, E, Bourbeau, J, Bradascio, F, Braun, J, Bron, S, Brostean-Kaiser, J, Burgman, A, Busse, RS, Campana, MA, Chen, C, Chirkin, D, Choi, S, Clark, BA, Clark, K, Classen, L, Coleman, A, Collin, GH, Conrad, JM, Coppin, P, Correa, P, Cowen, DF, Cross, R, Dave, P, De Clercq, C, Delaunay, JJ, Dembinski, H, Deoskar, K, De Ridder, S, Desai, A, Desiati, P, De Vries, KD, De Wasseige, G, De With, M, Deyoung, T, Dharani, S, Diaz, A, Díaz-Vélez, JC, Dujmovic, H, Dunkman, M, Duvernois, MA, Dvorak, E, Ehrhardt, T, Eller, P, Engel, R, Evans, J, Evenson, PA, Fahey, S, Fazely, AR, Fiedlschuster, S, Fienberg, AT, Filimonov, K, Finley, C, Fischer, L, Fox, D, Franckowiak, A, Friedman, E, Fritz, A, Fürst, P, Gaisser, TK, Gallagher, J, and Ganster, E
Abstract: Since the discovery of a flux of high-energy astrophysical neutrinos, searches for their origins have focused primarily at TeV-PeV energies. Compared to sub-TeV searches, high-energy searches benefit from an increase in the neutrino cross section, improved angular resolution on the neutrino direction, and a reduced background from atmospheric neutrinos and muons. However, the focus on high energy does not preclude the existence of sub-TeV neutrino emission where IceCube retains sensitivity. Here we present the first all-flavor search from IceCube for transient emission of low-energy neutrinos, focusing on the energy region of 5.6-100 GeV using three years of data obtained with the IceCube-DeepCore detector. We find no evidence of transient neutrino emission in the data, thus leading to a constraint on the volumetric rate of astrophysical transient sources in the range of ∼ 705-2301 Gpc-3 yr-1 for sources following a subphotospheric energy spectrum with a mean energy of 100 GeV and a bolometric energy of 1052 erg.
Published: 2022

12. Density of GeV muons in air showers measured with IceTop.

Author: Abbasi, R, Abbasi, R, Ackermann, M, Adams, J, Aguilar, JA, Ahlers, M, Ahrens, M, Alameddine, JM, Alves, AA, Amin, NM, Andeen, K, Anderson, T, Anton, G, Argüelles, C, Ashida, Y, Axani, S, Bai, X, Balagopal V, A, Barwick, SW, Bastian, B, Basu, V, Baur, S, Bay, R, Beatty, JJ, Becker, KH, Becker Tjus, J, Beise, J, Bellenghi, C, Benda, S, Benzvi, S, Berley, D, Bernardini, E, Besson, DZ, Binder, G, Bindig, D, Blaufuss, E, Blot, S, Boddenberg, M, Bontempo, F, Borowka, J, Böser, S, Botner, O, Böttcher, J, Bourbeau, E, Bradascio, F, Braun, J, Brinson, B, Bron, S, Brostean-Kaiser, J, Browne, S, Burgman, A, Burley, RT, Busse, RS, Campana, MA, Carnie-Bronca, EG, Chen, C, Chen, Z, Chirkin, D, Choi, K, Clark, BA, Clark, K, Classen, L, Coleman, A, Collin, GH, Conrad, JM, Coppin, P, Correa, P, Cowen, DF, Cross, R, Dappen, C, Dave, P, De Clercq, C, Delaunay, JJ, Delgado López, D, Dembinski, H, Deoskar, K, Desai, A, Desiati, P, De Vries, KD, De Wasseige, G, De With, M, Deyoung, T, Diaz, A, Díaz-Vélez, JC, Dittmer, M, Dujmovic, H, Dunkman, M, Duvernois, MA, Ehrhardt, T, Eller, P, Engel, R, Erpenbeck, H, Evans, J, Evenson, PA, Fan, KL, Fazely, AR, Fedynitch, A, Feigl, N, Fiedlschuster, S, Fienberg, AT, Finley, C, Abbasi, R, Abbasi, R, Ackermann, M, Adams, J, Aguilar, JA, Ahlers, M, Ahrens, M, Alameddine, JM, Alves, AA, Amin, NM, Andeen, K, Anderson, T, Anton, G, Argüelles, C, Ashida, Y, Axani, S, Bai, X, Balagopal V, A, Barwick, SW, Bastian, B, Basu, V, Baur, S, Bay, R, Beatty, JJ, Becker, KH, Becker Tjus, J, Beise, J, Bellenghi, C, Benda, S, Benzvi, S, Berley, D, Bernardini, E, Besson, DZ, Binder, G, Bindig, D, Blaufuss, E, Blot, S, Boddenberg, M, Bontempo, F, Borowka, J, Böser, S, Botner, O, Böttcher, J, Bourbeau, E, Bradascio, F, Braun, J, Brinson, B, Bron, S, Brostean-Kaiser, J, Browne, S, Burgman, A, Burley, RT, Busse, RS, Campana, MA, Carnie-Bronca, EG, Chen, C, Chen, Z, Chirkin, D, Choi, K, Clark, BA, Clark, K, Classen, L, Coleman, A, Collin, GH, Conrad, JM, Coppin, P, Correa, P, Cowen, DF, Cross, R, Dappen, C, Dave, P, De Clercq, C, Delaunay, JJ, Delgado López, D, Dembinski, H, Deoskar, K, Desai, A, Desiati, P, De Vries, KD, De Wasseige, G, De With, M, Deyoung, T, Diaz, A, Díaz-Vélez, JC, Dittmer, M, Dujmovic, H, Dunkman, M, Duvernois, MA, Ehrhardt, T, Eller, P, Engel, R, Erpenbeck, H, Evans, J, Evenson, PA, Fan, KL, Fazely, AR, Fedynitch, A, Feigl, N, Fiedlschuster, S, Fienberg, AT, and Finley, C
Abstract: We present a measurement of the density of GeV muons in near-vertical air showers using three years of data recorded by the IceTop array at the South Pole. Depending on the shower size, the muon densities have been measured at lateral distances between 200 and 1000 m. From these lateral distributions, we derive the muon densities as functions of energy at reference distances of 600 and 800 m for primary energies between 2.5 and 40 PeV and between 9 and 120 PeV, respectively. The muon densities are determined using, as a baseline, the hadronic interaction model Sibyll 2.1 together with various composition models. The measurements are consistent with the predicted muon densities within these baseline interaction and composition models. The measured muon densities have also been compared to simulations using the post-LHC models EPOS-LHC and QGSJet-II.04. The result of this comparison is that the post-LHC models together with any given composition model yield higher muon densities than observed. This is in contrast to the observations above 1 EeV where all model simulations yield for any mass composition lower muon densities than the measured ones. The post-LHC models in general feature higher muon densities so that the agreement with experimental data at the highest energies is improved but the muon densities are not correct in the energy range between 2.5 and about 100 PeV.
Published: 2022

13. Search for High-energy Neutrino Emission from Galactic X-Ray Binaries with IceCube

Author: Abbasi, R, Abbasi, R, Ackermann, M, Adams, J, Aguilar, JA, Ahlers, M, Ahrens, M, Alameddine, JM, Alves, AA, Amin, NM, Andeen, K, Anderson, T, Anton, G, Arguëlles, C, Ashida, Y, Axani, S, Bai, X, V., AB, Barwick, SW, Bastian, B, Basu, V, Baur, S, Bay, R, Beatty, JJ, Becker, KH, Tjus, JB, Beise, J, Bellenghi, C, Benda, S, Benzvi, S, Berley, D, Bernardini, E, Besson, DZ, Binder, G, Bindig, D, Blaufuss, E, Blot, S, Boddenberg, M, Bontempo, F, Borowka, J, Böser, S, Botner, O, Böttcher, J, Bourbeau, E, Bradascio, F, Braun, J, Brinson, B, Bron, S, Brostean-Kaiser, J, Browne, S, Burgman, A, Burley, RT, Busse, RS, Campana, MA, Carnie-Bronca, EG, Chen, C, Chen, Z, Chirkin, D, Choi, K, Clark, BA, Clark, K, Classen, L, Coleman, A, Collin, GH, Conrad, JM, Coppin, P, Correa, P, Cowen, DF, Cross, R, Dappen, C, Dave, P, De Clercq, C, Delaunay, JJ, López, DD, Dembinski, H, Deoskar, K, Desai, A, Desiati, P, De Vries, KD, De Wasseige, G, De With, M, Deyoung, T, Diaz, A, Diáz-Vélez, JC, Dittmer, M, Dujmovic, H, Dunkman, M, Duvernois, MA, Ehrhardt, T, Eller, P, Engel, R, Erpenbeck, H, Evans, J, Evenson, PA, Fan, KL, Fazely, AR, Fedynitch, A, Feigl, N, Fiedlschuster, S, Fienberg, AT, Finley, C, Abbasi, R, Abbasi, R, Ackermann, M, Adams, J, Aguilar, JA, Ahlers, M, Ahrens, M, Alameddine, JM, Alves, AA, Amin, NM, Andeen, K, Anderson, T, Anton, G, Arguëlles, C, Ashida, Y, Axani, S, Bai, X, V., AB, Barwick, SW, Bastian, B, Basu, V, Baur, S, Bay, R, Beatty, JJ, Becker, KH, Tjus, JB, Beise, J, Bellenghi, C, Benda, S, Benzvi, S, Berley, D, Bernardini, E, Besson, DZ, Binder, G, Bindig, D, Blaufuss, E, Blot, S, Boddenberg, M, Bontempo, F, Borowka, J, Böser, S, Botner, O, Böttcher, J, Bourbeau, E, Bradascio, F, Braun, J, Brinson, B, Bron, S, Brostean-Kaiser, J, Browne, S, Burgman, A, Burley, RT, Busse, RS, Campana, MA, Carnie-Bronca, EG, Chen, C, Chen, Z, Chirkin, D, Choi, K, Clark, BA, Clark, K, Classen, L, Coleman, A, Collin, GH, Conrad, JM, Coppin, P, Correa, P, Cowen, DF, Cross, R, Dappen, C, Dave, P, De Clercq, C, Delaunay, JJ, López, DD, Dembinski, H, Deoskar, K, Desai, A, Desiati, P, De Vries, KD, De Wasseige, G, De With, M, Deyoung, T, Diaz, A, Diáz-Vélez, JC, Dittmer, M, Dujmovic, H, Dunkman, M, Duvernois, MA, Ehrhardt, T, Eller, P, Engel, R, Erpenbeck, H, Evans, J, Evenson, PA, Fan, KL, Fazely, AR, Fedynitch, A, Feigl, N, Fiedlschuster, S, Fienberg, AT, and Finley, C
Abstract: We present the first comprehensive search for high-energy neutrino emission from high- A nd low-mass X-ray binaries conducted by IceCube. Galactic X-ray binaries are long-standing candidates for the source of Galactic hadronic cosmic rays and neutrinos. The compact object in these systems can be the site of cosmic-ray acceleration, and neutrinos can be produced by interactions of cosmic rays with radiation or gas, in the jet of a microquasar, in the stellar wind, or in the atmosphere of the companion star. We study X-ray binaries using 7.5 yr of IceCube data with three separate analyses. In the first, we search for periodic neutrino emission from 55 binaries in the Northern Sky with known orbital periods. In the second, the X-ray light curves of 102 binaries across the entire sky are used as templates to search for time-dependent neutrino emission. Finally, we search for time-integrated emission of neutrinos for a list of 4 notable binaries identified as microquasars. In the absence of a significant excess, we place upper limits on the neutrino flux for each hypothesis and compare our results with theoretical predictions for several binaries. In addition, we evaluate the sensitivity of the next generation neutrino telescope at the South Pole, IceCube-Gen2, and demonstrate its power to identify potential neutrino emission from these binary sources in the Galaxy.
Published: 2022

14. Searches for Neutrinos from Gamma-Ray Bursts Using the IceCube Neutrino Observatory

Author: Abbasi, R, Abbasi, R, Ackermann, M, Adams, J, Aguilar, JA, Ahlers, M, Ahrens, M, Alameddine, JM, Alves, AA, Amin, NM, Andeen, K, Anderson, T, Anton, G, Argüelles, C, Ashida, Y, Athanasiadou, S, Axani, S, Bai, X, V., A Balagopal, Barwick, SW, Basu, V, Baur, S, Bay, R, Beatty, JJ, Becker, K-H, Tjus, J Becker, Beise, J, Bellenghi, C, Benda, S, BenZvi, S, Berley, D, Bernardini, E, Besson, DZ, Binder, G, Bindig, D, Blaufuss, E, Blot, S, Boddenberg, M, Bontempo, F, Book, JY, Borowka, J, Böser, S, Botner, O, Böttcher, J, Bourbeau, E, Bradascio, F, Braun, J, Brinson, B, Bron, S, Brostean-Kaiser, J, Burley, RT, Busse, RS, Campana, MA, Carnie-Bronca, EG, Chen, C, Chen, Z, Chirkin, D, Choi, K, Clark, BA, Clark, K, Classen, L, Coleman, A, Collin, GH, Connolly, A, Conrad, JM, Coppin, P, Correa, P, Cowen, DF, Cross, R, Dappen, C, Dave, P, De Clercq, C, DeLaunay, JJ, López, D Delgado, Dembinski, H, Deoskar, K, Desai, A, Desiati, P, de Vries, KD, de Wasseige, G, DeYoung, T, Diaz, A, Díaz-Vélez, JC, Dittmer, M, Dujmovic, H, DuVernois, MA, Ehrhardt, T, Eller, P, Engel, R, Erpenbeck, H, Evans, J, Evenson, PA, Fan, KL, Fazely, AR, Fedynitch, A, Feigl, N, Fiedlschuster, S, Fienberg, AT, Finley, C, Fischer, L, Fox, D, Abbasi, R, Abbasi, R, Ackermann, M, Adams, J, Aguilar, JA, Ahlers, M, Ahrens, M, Alameddine, JM, Alves, AA, Amin, NM, Andeen, K, Anderson, T, Anton, G, Argüelles, C, Ashida, Y, Athanasiadou, S, Axani, S, Bai, X, V., A Balagopal, Barwick, SW, Basu, V, Baur, S, Bay, R, Beatty, JJ, Becker, K-H, Tjus, J Becker, Beise, J, Bellenghi, C, Benda, S, BenZvi, S, Berley, D, Bernardini, E, Besson, DZ, Binder, G, Bindig, D, Blaufuss, E, Blot, S, Boddenberg, M, Bontempo, F, Book, JY, Borowka, J, Böser, S, Botner, O, Böttcher, J, Bourbeau, E, Bradascio, F, Braun, J, Brinson, B, Bron, S, Brostean-Kaiser, J, Burley, RT, Busse, RS, Campana, MA, Carnie-Bronca, EG, Chen, C, Chen, Z, Chirkin, D, Choi, K, Clark, BA, Clark, K, Classen, L, Coleman, A, Collin, GH, Connolly, A, Conrad, JM, Coppin, P, Correa, P, Cowen, DF, Cross, R, Dappen, C, Dave, P, De Clercq, C, DeLaunay, JJ, López, D Delgado, Dembinski, H, Deoskar, K, Desai, A, Desiati, P, de Vries, KD, de Wasseige, G, DeYoung, T, Diaz, A, Díaz-Vélez, JC, Dittmer, M, Dujmovic, H, DuVernois, MA, Ehrhardt, T, Eller, P, Engel, R, Erpenbeck, H, Evans, J, Evenson, PA, Fan, KL, Fazely, AR, Fedynitch, A, Feigl, N, Fiedlschuster, S, Fienberg, AT, Finley, C, Fischer, L, and Fox, D
Abstract: Gamma-ray bursts (GRBs) are considered as promising sources of ultra-high-energy cosmic rays (UHECRs) due to their large power output. Observing a neutrino flux from GRBs would offer evidence that GRBs are hadronic accelerators of UHECRs. Previous IceCube analyses, which primarily focused on neutrinos arriving in temporal coincidence with the prompt gamma-rays, found no significant neutrino excess. The four analyses presented in this paper extend the region of interest to 14 days before and after the prompt phase, including generic extended time windows and targeted precursor searches. GRBs were selected between 2011 May and 2018 October to align with the data set of candidate muon-neutrino events observed by IceCube. No evidence of correlation between neutrino events and GRBs was found in these analyses. Limits are set to constrain the contribution of the cosmic GRB population to the diffuse astrophysical neutrino flux observed by IceCube. Prompt neutrino emission from GRBs is limited to 21% of the observed diffuse neutrino flux, and emission on timescales up to 104 s is constrained to 24% of the total diffuse flux.
Published: 2022

15. Graph Neural Networks for low-energy event classification & reconstruction in IceCube

Author: Abbasi, R, Abbasi, R, Ackermann, M, Adams, J, Aggarwal, N, Aguilar, JA, Ahlers, M, Ahrens, M, Alameddine, JM, Alves, AA, Amin, NM, Andeen, K, Anderson, T, Anton, G, Argüelles, C, Ashida, Y, Athanasiadou, S, Axani, S, Bai, X, V., A Balagopal, Baricevic, M, Barwick, SW, Basu, V, Bay, R, Beatty, JJ, Becker, K-H, Tjus, J Becker, Beise, J, Bellenghi, C, Benda, S, BenZvi, S, Berley, D, Bernardini, E, Besson, DZ, Binder, G, Bindig, D, Blaufuss, E, Blot, S, Bontempo, F, Book, JY, Borowka, J, Meneguolo, C Boscolo, Böser, S, Botner, O, Böttcher, J, Bourbeau, E, Braun, J, Brinson, B, Brostean-Kaiser, J, Burley, RT, Busse, RS, Campana, MA, Carnie-Bronca, EG, Chen, C, Chen, Z, Chirkin, D, Choi, K, Clark, BA, Classen, L, Coleman, A, Collin, GH, Connolly, A, Conrad, JM, Coppin, P, Correa, P, Countryman, S, Cowen, DF, Cross, R, Dappen, C, Dave, P, De Clercq, C, DeLaunay, JJ, López, D Delgado, Dembinski, H, Deoskar, K, Desai, A, Desiati, P, de Vries, KD, de Wasseige, G, DeYoung, T, Diaz, A, Díaz-Vélez, JC, Dittmer, M, Dujmovic, H, DuVernois, MA, Ehrhardt, T, Eller, P, Engel, R, Erpenbeck, H, Evans, J, Evenson, PA, Fan, KL, Fazely, AR, Fedynitch, A, Feigl, N, Fiedlschuster, S, Fienberg, AT, Finley, C, Fischer, L, Fox, D, Franckowiak, A, Abbasi, R, Abbasi, R, Ackermann, M, Adams, J, Aggarwal, N, Aguilar, JA, Ahlers, M, Ahrens, M, Alameddine, JM, Alves, AA, Amin, NM, Andeen, K, Anderson, T, Anton, G, Argüelles, C, Ashida, Y, Athanasiadou, S, Axani, S, Bai, X, V., A Balagopal, Baricevic, M, Barwick, SW, Basu, V, Bay, R, Beatty, JJ, Becker, K-H, Tjus, J Becker, Beise, J, Bellenghi, C, Benda, S, BenZvi, S, Berley, D, Bernardini, E, Besson, DZ, Binder, G, Bindig, D, Blaufuss, E, Blot, S, Bontempo, F, Book, JY, Borowka, J, Meneguolo, C Boscolo, Böser, S, Botner, O, Böttcher, J, Bourbeau, E, Braun, J, Brinson, B, Brostean-Kaiser, J, Burley, RT, Busse, RS, Campana, MA, Carnie-Bronca, EG, Chen, C, Chen, Z, Chirkin, D, Choi, K, Clark, BA, Classen, L, Coleman, A, Collin, GH, Connolly, A, Conrad, JM, Coppin, P, Correa, P, Countryman, S, Cowen, DF, Cross, R, Dappen, C, Dave, P, De Clercq, C, DeLaunay, JJ, López, D Delgado, Dembinski, H, Deoskar, K, Desai, A, Desiati, P, de Vries, KD, de Wasseige, G, DeYoung, T, Diaz, A, Díaz-Vélez, JC, Dittmer, M, Dujmovic, H, DuVernois, MA, Ehrhardt, T, Eller, P, Engel, R, Erpenbeck, H, Evans, J, Evenson, PA, Fan, KL, Fazely, AR, Fedynitch, A, Feigl, N, Fiedlschuster, S, Fienberg, AT, Finley, C, Fischer, L, Fox, D, and Franckowiak, A
Abstract: IceCube, a cubic-kilometer array of optical sensors built to detect atmospheric and astrophysical neutrinos between 1 GeV and 1 PeV, is deployed 1.45 km to 2.45 km below the surface of the ice sheet at the South Pole. The classification and reconstruction of events from the in-ice detectors play a central role in the analysis of data from IceCube. Reconstructing and classifying events is a challenge due to the irregular detector geometry, inhomogeneous scattering and absorption of light in the ice and, below 100 GeV, the relatively low number of signal photons produced per event. To address this challenge, it is possible to represent IceCube events as point cloud graphs and use a Graph Neural Network (GNN) as the classification and reconstruction method. The GNN is capable of distinguishing neutrino events from cosmic-ray backgrounds, classifying different neutrino event types, and reconstructing the deposited energy, direction and interaction vertex. Based on simulation, we provide a comparison in the 1 GeV-100 GeV energy range to the current state-of-the-art maximum likelihood techniques used in current IceCube analyses, including the effects of known systematic uncertainties. For neutrino event classification, the GNN increases the signal efficiency by 18% at a fixed background rate, compared to current IceCube methods. Alternatively, the GNN offers a reduction of the background (i.e. false positive) rate by over a factor 8 (to below half a percent) at a fixed signal efficiency. For the reconstruction of energy, direction, and interaction vertex, the resolution improves by an average of 13%-20% compared to current maximum likelihood techniques in the energy range of 1 GeV-30 GeV. The GNN, when run on a GPU, is capable of processing IceCube events at a rate nearly double of the median IceCube trigger rate of 2.7 kHz, which opens the possibility of using low energy neutrinos in online searches for transient events.
Published: 2022

16. Search for quantum gravity using astrophysical neutrino flavour with IceCube

Author: Abbasi, R, Abbasi, R, Ackermann, M, Adams, J, Aguilar, JA, Ahlers, M, Ahrens, M, Alameddine, JM, Alispach, C, Alves, AA, Amin, NM, Andeen, K, Anderson, T, Anton, G, Argüelles, C, Ashida, Y, Axani, S, Bai, X, Balagopal V, A, Barbano, A, Barwick, SW, Bastian, B, Basu, V, Baur, S, Bay, R, Beatty, JJ, Becker, KH, Tjus, JB, Bellenghi, C, BenZvi, S, Berley, D, Bernardini, E, Besson, DZ, Binder, G, Bindig, D, Blaufuss, E, Blot, S, Boddenberg, M, Bontempo, F, Borowka, J, Böser, S, Botner, O, Böttcher, J, Bourbeau, E, Bradascio, F, Braun, J, Brinson, B, Bron, S, Brostean-Kaiser, J, Browne, S, Burgman, A, Burley, RT, Busse, RS, Campana, MA, Carnie-Bronca, EG, Chen, C, Chen, Z, Chirkin, D, Choi, K, Clark, BA, Clark, K, Classen, L, Coleman, A, Collin, GH, Conrad, JM, Coppin, P, Correa, P, Cowen, DF, Cross, R, Dappen, C, Dave, P, Clercq, CD, DeLaunay, JJ, López, DD, Dembinski, H, Deoskar, K, Desai, A, Desiati, P, Vries, KDD, Wasseige, GD, With, MD, DeYoung, T, Diaz, A, Díaz-Vélez, JC, Dittmer, M, Dujmovic, H, Dunkman, M, DuVernois, MA, Dvorak, E, Ehrhardt, T, Eller, P, Engel, R, Erpenbeck, H, Evans, J, Evenson, PA, Fan, KL, Farrag, K, Fazely, AR, Feigl, N, Fiedlschuster, S, Fienberg, AT, Abbasi, R, Abbasi, R, Ackermann, M, Adams, J, Aguilar, JA, Ahlers, M, Ahrens, M, Alameddine, JM, Alispach, C, Alves, AA, Amin, NM, Andeen, K, Anderson, T, Anton, G, Argüelles, C, Ashida, Y, Axani, S, Bai, X, Balagopal V, A, Barbano, A, Barwick, SW, Bastian, B, Basu, V, Baur, S, Bay, R, Beatty, JJ, Becker, KH, Tjus, JB, Bellenghi, C, BenZvi, S, Berley, D, Bernardini, E, Besson, DZ, Binder, G, Bindig, D, Blaufuss, E, Blot, S, Boddenberg, M, Bontempo, F, Borowka, J, Böser, S, Botner, O, Böttcher, J, Bourbeau, E, Bradascio, F, Braun, J, Brinson, B, Bron, S, Brostean-Kaiser, J, Browne, S, Burgman, A, Burley, RT, Busse, RS, Campana, MA, Carnie-Bronca, EG, Chen, C, Chen, Z, Chirkin, D, Choi, K, Clark, BA, Clark, K, Classen, L, Coleman, A, Collin, GH, Conrad, JM, Coppin, P, Correa, P, Cowen, DF, Cross, R, Dappen, C, Dave, P, Clercq, CD, DeLaunay, JJ, López, DD, Dembinski, H, Deoskar, K, Desai, A, Desiati, P, Vries, KDD, Wasseige, GD, With, MD, DeYoung, T, Diaz, A, Díaz-Vélez, JC, Dittmer, M, Dujmovic, H, Dunkman, M, DuVernois, MA, Dvorak, E, Ehrhardt, T, Eller, P, Engel, R, Erpenbeck, H, Evans, J, Evenson, PA, Fan, KL, Farrag, K, Fazely, AR, Feigl, N, Fiedlschuster, S, and Fienberg, AT
Abstract: Along their long propagation from production to detection, neutrinos undergo flavour conversions that convert their types or flavours1,2. High-energy astrophysical neutrinos propagate unperturbed over a billion light years in vacuum3 and are sensitive to small effects caused by new physics. Effects of quantum gravity4 are expected to appear at the Planck energy scale. Such a high-energy universe would have existed only immediately after the Big Bang and is inaccessible by human technologies. On the other hand, quantum gravity effects may exist in our low-energy vacuum5–8, but are suppressed by inverse powers of the Planck energy. Measuring the coupling of particles to such small effects is difficult via kinematic observables, but could be observable through flavour conversions. Here we report a search with the IceCube Neutrino Observatory, using astrophysical neutrino flavours9,10 to search for new space–time structure. We did not find any evidence of anomalous flavour conversion in the IceCube astrophysical neutrino flavour data. We apply the most stringent limits of any known technologies, down to 10−42 GeV−2 with Bayes factor greater than 10 on the dimension-six operators that parameterize the space–time defects. We thus unambiguously reach the parameter space of quantum-gravity-motivated physics.
Published: 2022

17. Searching for High-energy Neutrino Emission from Galaxy Clusters with IceCube

Author: Abbasi, R, Abbasi, R, Ackermann, M, Adams, J, Aguilar, JA, Ahlers, M, Ahrens, M, Alameddine, JM, Alves, AA, Amin, NM, Andeen, K, Anderson, T, Anton, G, Argüelles, C, Ashida, Y, Athanasiadou, S, Axani, S, Bai, X, V., A Balagopal, Baricevic, M, Barwick, SW, Basu, V, Bay, R, Beatty, JJ, Becker, K-H, Tjus, J Becker, Beise, J, Bellenghi, C, Benda, S, BenZvi, S, Berley, D, Bernardini, E, Besson, DZ, Binder, G, Bindig, D, Blaufuss, E, Blot, S, Bontempo, F, Book, JY, Borowka, J, Böser, S, Botner, O, Böttcher, J, Bourbeau, E, Bradascio, F, Braun, J, Brinson, B, Bron, S, Brostean-Kaiser, J, Burley, RT, Busse, RS, Campana, MA, Carnie-Bronca, EG, Chen, C, Chen, Z, Chirkin, D, Choi, K, Clark, BA, Clark, K, Classen, L, Coleman, A, Collin, GH, Connolly, A, Conrad, JM, Coppin, P, Correa, P, Cowen, DF, Cross, R, Dappen, C, Dave, P, De Clercq, C, DeLaunay, JJ, López, D Delgado, Dembinski, H, Deoskar, K, Desai, A, Desiati, P, de Vries, KD, de Wasseige, G, DeYoung, T, Diaz, A, Díaz-Vélez, JC, Dittmer, M, Dujmovic, H, DuVernois, MA, Ehrhardt, T, Eller, P, Engel, R, Erpenbeck, H, Evans, J, Evenson, PA, Fan, KL, Fazely, AR, Fedynitch, A, Feigl, N, Fiedlschuster, S, Fienberg, AT, Finley, C, Fischer, L, Fox, D, Franckowiak, A, Abbasi, R, Abbasi, R, Ackermann, M, Adams, J, Aguilar, JA, Ahlers, M, Ahrens, M, Alameddine, JM, Alves, AA, Amin, NM, Andeen, K, Anderson, T, Anton, G, Argüelles, C, Ashida, Y, Athanasiadou, S, Axani, S, Bai, X, V., A Balagopal, Baricevic, M, Barwick, SW, Basu, V, Bay, R, Beatty, JJ, Becker, K-H, Tjus, J Becker, Beise, J, Bellenghi, C, Benda, S, BenZvi, S, Berley, D, Bernardini, E, Besson, DZ, Binder, G, Bindig, D, Blaufuss, E, Blot, S, Bontempo, F, Book, JY, Borowka, J, Böser, S, Botner, O, Böttcher, J, Bourbeau, E, Bradascio, F, Braun, J, Brinson, B, Bron, S, Brostean-Kaiser, J, Burley, RT, Busse, RS, Campana, MA, Carnie-Bronca, EG, Chen, C, Chen, Z, Chirkin, D, Choi, K, Clark, BA, Clark, K, Classen, L, Coleman, A, Collin, GH, Connolly, A, Conrad, JM, Coppin, P, Correa, P, Cowen, DF, Cross, R, Dappen, C, Dave, P, De Clercq, C, DeLaunay, JJ, López, D Delgado, Dembinski, H, Deoskar, K, Desai, A, Desiati, P, de Vries, KD, de Wasseige, G, DeYoung, T, Diaz, A, Díaz-Vélez, JC, Dittmer, M, Dujmovic, H, DuVernois, MA, Ehrhardt, T, Eller, P, Engel, R, Erpenbeck, H, Evans, J, Evenson, PA, Fan, KL, Fazely, AR, Fedynitch, A, Feigl, N, Fiedlschuster, S, Fienberg, AT, Finley, C, Fischer, L, Fox, D, and Franckowiak, A
Abstract: Galaxy clusters have the potential to accelerate cosmic rays (CRs) to ultrahigh energies via accretion shocks or embedded CR acceleration sites. The CRs with energies below the Hillas condition will be confined within the cluster and eventually interact with the intracluster medium gas to produce secondary neutrinos and gamma rays. Using 9.5 yr of muon neutrino track events from the IceCube Neutrino Observatory, we report the results of a stacking analysis of 1094 galaxy clusters with masses ≳1014 Me and redshifts between 0.01 and ∼1 detected by the Planck mission via the Sunyaev–Zel’dovich effect. We find no evidence for significant neutrino emission and report upper limits on the cumulative unresolved neutrino flux from massive galaxy clusters after accounting for the completeness of the catalog up to a redshift of 2, assuming three different weighting scenarios for the stacking and three different power-law spectra. Weighting the sources according to mass and distance, we set upper limits at a 90% confidence level that constrain the flux of neutrinos from massive galaxy clusters (≳1014 Me) to be no more than 4.6% of the diffuse IceCube observations at 100 TeV, assuming an unbroken E−2.5 power-law spectrum.
Published: 2022

18. Search for Astrophysical Neutrinos from 1FLE Blazars with IceCube

Author: Abbasi, R, Abbasi, R, Ackermann, M, Adams, J, Aguilar, JA, Ahlers, M, Ahrens, M, Alameddine, JM, Alves, AA, Amin, NM, Andeen, K, Anderson, T, Anton, G, Argüelles, C, Ashida, Y, Athanasiadou, S, Axani, S, Bai, X, V., A Balagopal, Baricevic, M, Barwick, SW, Basu, V, Bay, R, Beatty, JJ, Becker, K-H, Tjus, J Becker, Beise, J, Bellenghi, C, Benda, S, BenZvi, S, Berley, D, Bernardini, E, Besson, DZ, Binder, G, Bindig, D, Blaufuss, E, Blot, S, Bontempo, F, Book, JY, Borowka, J, Böser, S, Botner, O, Böttcher, J, Bourbeau, E, Bradascio, F, Braun, J, Brinson, B, Bron, S, Brostean-Kaiser, J, Burley, RT, Busse, RS, Campana, MA, Carnie-Bronca, EG, Chen, C, Chen, Z, Chirkin, D, Choi, K, Clark, BA, Classen, L, Coleman, A, Collin, GH, Connolly, A, Conrad, JM, Coppin, P, Correa, P, Cowen, DF, Cross, R, Dappen, C, Dave, P, De Clercq, C, DeLaunay, JJ, López, D Delgado, Dembinski, H, Deoskar, K, Desai, A, Desiati, P, de Vries, KD, de Wasseige, G, DeYoung, T, Diaz, A, Díaz-Vélez, JC, Dittmer, M, Dujmovic, H, DuVernois, MA, Ehrhardt, T, Eller, P, Engel, R, Erpenbeck, H, Evans, J, Evenson, PA, Fan, KL, Fazely, AR, Fedynitch, A, Feigl, N, Fiedlschuster, S, Fienberg, AT, Finley, C, Fischer, L, Fox, D, Franckowiak, A, Friedman, E, Abbasi, R, Abbasi, R, Ackermann, M, Adams, J, Aguilar, JA, Ahlers, M, Ahrens, M, Alameddine, JM, Alves, AA, Amin, NM, Andeen, K, Anderson, T, Anton, G, Argüelles, C, Ashida, Y, Athanasiadou, S, Axani, S, Bai, X, V., A Balagopal, Baricevic, M, Barwick, SW, Basu, V, Bay, R, Beatty, JJ, Becker, K-H, Tjus, J Becker, Beise, J, Bellenghi, C, Benda, S, BenZvi, S, Berley, D, Bernardini, E, Besson, DZ, Binder, G, Bindig, D, Blaufuss, E, Blot, S, Bontempo, F, Book, JY, Borowka, J, Böser, S, Botner, O, Böttcher, J, Bourbeau, E, Bradascio, F, Braun, J, Brinson, B, Bron, S, Brostean-Kaiser, J, Burley, RT, Busse, RS, Campana, MA, Carnie-Bronca, EG, Chen, C, Chen, Z, Chirkin, D, Choi, K, Clark, BA, Classen, L, Coleman, A, Collin, GH, Connolly, A, Conrad, JM, Coppin, P, Correa, P, Cowen, DF, Cross, R, Dappen, C, Dave, P, De Clercq, C, DeLaunay, JJ, López, D Delgado, Dembinski, H, Deoskar, K, Desai, A, Desiati, P, de Vries, KD, de Wasseige, G, DeYoung, T, Diaz, A, Díaz-Vélez, JC, Dittmer, M, Dujmovic, H, DuVernois, MA, Ehrhardt, T, Eller, P, Engel, R, Erpenbeck, H, Evans, J, Evenson, PA, Fan, KL, Fazely, AR, Fedynitch, A, Feigl, N, Fiedlschuster, S, Fienberg, AT, Finley, C, Fischer, L, Fox, D, Franckowiak, A, and Friedman, E
Abstract: The majority of astrophysical neutrinos have undetermined origins. The IceCube Neutrino Observatory has observed astrophysical neutrinos but has not yet identified their sources. Blazars are promising source candidates, but previous searches for neutrino emission from populations of blazars detected in ≳ GeV gamma rays have not observed any significant neutrino excess. Recent findings in multimessenger astronomy indicate that high-energy photons, coproduced with high-energy neutrinos, are likely to be absorbed and reemitted at lower energies. Thus, lower-energy photons may be better indicators of TeV-PeV neutrino production. This paper presents the first time-integrated stacking search for astrophysical neutrino emission from MeV-detected blazars in the first Fermi Large Area Telescope low energy (1FLE) catalog using ten years of IceCube muon-neutrino data. The results of this analysis are found to be consistent with a background-only hypothesis. Assuming an E-2 neutrino spectrum and proportionality between the blazars MeV gamma-ray fluxes and TeV-PeV neutrino flux, the upper limit on the 1FLE blazar energy-scaled neutrino flux is determined to be 1.64 × 10-12 TeV cm-2 s-1 at 90% confidence level. This upper limit is approximately 1% of IceCube's diffuse muon-neutrino flux measurement.
Published: 2022

19. A search for time-dependent astrophysical neutrino emission with icecube data from 2012 to 2017

Author: Abbasi, R, Abbasi, R, Ackermann, M, Adams, J, Aguilar, JA, Ahlers, M, Ahrens, M, Alispach, C, Alves, JA, Amin, NM, Andeen, K, Anderson, T, Ansseau, I, Anton, G, Argüelles, C, Axani, S, Bai, X, Balagopal V, A, Barbano, A, Barwick, SW, Bastian, B, Basu, V, Baum, V, Baur, S, Bay, R, Beatty, JJ, Becker, KH, Becker Tjus, J, Bellenghi, C, BenZvi, S, Berley, D, Bernardini, E, Besson, DZ, Binder, G, Bindig, D, Blaufuss, E, Blot, S, Böser, S, Botner, O, Böttcher, J, Bourbeau, E, Bourbeau, J, Bradascio, F, Braun, J, Bron, S, Brostean-Kaiser, J, Burgman, A, Busse, RS, Campana, MA, Chen, C, Chirkin, D, Choi, S, Clark, BA, Clark, K, Classen, L, Coleman, A, Collin, GH, Conrad, JM, Coppin, P, Correa, P, Cowen, DF, Cross, R, Dave, P, De Clercq, C, DeLaunay, JJ, Dembinski, H, Deoskar, K, De Ridder, S, Desai, A, Desiati, P, de Vries, KD, de Wasseige, G, de With, M, DeYoung, T, Dharani, S, Diaz, A, Díaz-Vélez, JC, Dujmovic, H, Dunkman, M, DuVernois, MA, Dvorak, E, Ehrhardt, T, Eller, P, Engel, R, Evans, J, Evenson, PA, Fahey, S, Fazely, AR, Fiedlschuster, S, Fienberg, AT, Filimonov, K, Finley, C, Fischer, L, Fox, D, Franckowiak, A, Friedman, E, Fritz, A, Fürst, P, Gaisser, TK, Gallagher, J, Ganster, E, Abbasi, R, Abbasi, R, Ackermann, M, Adams, J, Aguilar, JA, Ahlers, M, Ahrens, M, Alispach, C, Alves, JA, Amin, NM, Andeen, K, Anderson, T, Ansseau, I, Anton, G, Argüelles, C, Axani, S, Bai, X, Balagopal V, A, Barbano, A, Barwick, SW, Bastian, B, Basu, V, Baum, V, Baur, S, Bay, R, Beatty, JJ, Becker, KH, Becker Tjus, J, Bellenghi, C, BenZvi, S, Berley, D, Bernardini, E, Besson, DZ, Binder, G, Bindig, D, Blaufuss, E, Blot, S, Böser, S, Botner, O, Böttcher, J, Bourbeau, E, Bourbeau, J, Bradascio, F, Braun, J, Bron, S, Brostean-Kaiser, J, Burgman, A, Busse, RS, Campana, MA, Chen, C, Chirkin, D, Choi, S, Clark, BA, Clark, K, Classen, L, Coleman, A, Collin, GH, Conrad, JM, Coppin, P, Correa, P, Cowen, DF, Cross, R, Dave, P, De Clercq, C, DeLaunay, JJ, Dembinski, H, Deoskar, K, De Ridder, S, Desai, A, Desiati, P, de Vries, KD, de Wasseige, G, de With, M, DeYoung, T, Dharani, S, Diaz, A, Díaz-Vélez, JC, Dujmovic, H, Dunkman, M, DuVernois, MA, Dvorak, E, Ehrhardt, T, Eller, P, Engel, R, Evans, J, Evenson, PA, Fahey, S, Fazely, AR, Fiedlschuster, S, Fienberg, AT, Filimonov, K, Finley, C, Fischer, L, Fox, D, Franckowiak, A, Friedman, E, Fritz, A, Fürst, P, Gaisser, TK, Gallagher, J, and Ganster, E
Abstract: High-energy neutrinos are unique messengers of the high-energy universe, tracing the processes of cosmic ray acceleration. This paper presents analyses focusing on time-dependent neutrino point-source searches. A scan of the whole sky, making no prior assumption about source candidates, is performed, looking for a space and time clustering of high-energy neutrinos in data collected by the IceCube Neutrino Observatory between 2012 and 2017. No statistically significant evidence for a time-dependent neutrino signal is found with this search during this period, as all results are consistent with the background expectation. Within this study period, the blazar 3C 279, showed strong variability, inducing a very prominent gamma-ray flare observed in 2015 June. This event motivated a dedicated study of the blazar, which consists of searching for a time-dependent neutrino signal correlated with the gamma-ray emission. No evidence for a time-dependent signal is found. Hence, an upper limit on the neutrino fluence is derived, allowing us to constrain a hadronic emission model.
Published: 2021

20. Measurement of the high-energy all-flavor neutrino-nucleon cross section with IceCube

Author: Abbasi, R, Abbasi, R, Ackermann, M, Adams, J, Aguilar, JA, Ahlers, M, Ahrens, M, Alispach, C, Alves, AA, Amin, NM, Andeen, K, Anderson, T, Ansseau, I, Anton, G, Argüelles, C, Axani, S, Bai, X, Balagopal V., A, Barbano, A, Barwick, SW, Bastian, B, Basu, V, Baum, V, Baur, S, Bay, R, Beatty, JJ, Becker, KH, Becker Tjus, J, Bellenghi, C, Benzvi, S, Berley, D, Bernardini, E, Besson, DZ, Binder, G, Bindig, D, Blaufuss, E, Blot, S, Böser, S, Botner, O, Böttcher, J, Bourbeau, E, Bourbeau, J, Bradascio, F, Braun, J, Bron, S, Brostean-Kaiser, J, Burgman, A, Busse, RS, Campana, MA, Chen, C, Chirkin, D, Choi, S, Clark, BA, Clark, K, Classen, L, Coleman, A, Collin, GH, Conrad, JM, Coppin, P, Correa, P, Cowen, DF, Cross, R, Dave, P, De Clercq, C, Delaunay, JJ, Dembinski, H, Deoskar, K, De Ridder, S, Desai, A, Desiati, P, De Vries, KD, De Wasseige, G, De With, M, Deyoung, T, Dharani, S, Diaz, A, Díaz-Vélez, JC, Dujmovic, H, Dunkman, M, Duvernois, MA, Dvorak, E, Ehrhardt, T, Eller, P, Engel, R, Evans, J, Evenson, PA, Fahey, S, Fazely, AR, Fiedlschuster, S, Fienberg, AT, Filimonov, K, Finley, C, Fischer, L, Fox, D, Franckowiak, A, Friedman, E, Fritz, A, Fürst, P, Gaisser, TK, Gallagher, J, Ganster, E, Abbasi, R, Abbasi, R, Ackermann, M, Adams, J, Aguilar, JA, Ahlers, M, Ahrens, M, Alispach, C, Alves, AA, Amin, NM, Andeen, K, Anderson, T, Ansseau, I, Anton, G, Argüelles, C, Axani, S, Bai, X, Balagopal V., A, Barbano, A, Barwick, SW, Bastian, B, Basu, V, Baum, V, Baur, S, Bay, R, Beatty, JJ, Becker, KH, Becker Tjus, J, Bellenghi, C, Benzvi, S, Berley, D, Bernardini, E, Besson, DZ, Binder, G, Bindig, D, Blaufuss, E, Blot, S, Böser, S, Botner, O, Böttcher, J, Bourbeau, E, Bourbeau, J, Bradascio, F, Braun, J, Bron, S, Brostean-Kaiser, J, Burgman, A, Busse, RS, Campana, MA, Chen, C, Chirkin, D, Choi, S, Clark, BA, Clark, K, Classen, L, Coleman, A, Collin, GH, Conrad, JM, Coppin, P, Correa, P, Cowen, DF, Cross, R, Dave, P, De Clercq, C, Delaunay, JJ, Dembinski, H, Deoskar, K, De Ridder, S, Desai, A, Desiati, P, De Vries, KD, De Wasseige, G, De With, M, Deyoung, T, Dharani, S, Diaz, A, Díaz-Vélez, JC, Dujmovic, H, Dunkman, M, Duvernois, MA, Dvorak, E, Ehrhardt, T, Eller, P, Engel, R, Evans, J, Evenson, PA, Fahey, S, Fazely, AR, Fiedlschuster, S, Fienberg, AT, Filimonov, K, Finley, C, Fischer, L, Fox, D, Franckowiak, A, Friedman, E, Fritz, A, Fürst, P, Gaisser, TK, Gallagher, J, and Ganster, E
Abstract: The flux of high-energy neutrinos passing through the Earth is attenuated due to their interactions with matter. The interaction rate is determined by the neutrino interaction cross section and affects the flux arriving at the IceCube Neutrino Observatory, a cubic-kilometer neutrino detector embedded in the Antarctic ice sheet. We present a measurement of the neutrino cross section between 60 TeV and 10 PeV using the high-energy starting event (HESE) sample from IceCube with 7.5 years of data. The result is binned in neutrino energy and obtained using both Bayesian and frequentist statistics. We find it compatible with predictions from the Standard Model. While the cross section is expected to be flavor independent above 1 TeV, additional constraints on the measurement are included through updated experimental particle identification (PID) classifiers, proxies for the three neutrino flavors. This is the first such measurement to use a ternary PID observable and the first to account for neutrinos from tau decay.
Published: 2021

21. Search for GeV neutrino emission during intense gamma-ray solar flares with the IceCube Neutrino Observatory

Author: Abbasi, R, Abbasi, R, Ackermann, M, Adams, J, Aguilar, JA, Ahlers, M, Ahrens, M, Alispach, C, Alves, AA, Amin, NM, An, R, Andeen, K, Anderson, T, Ansseau, I, Anton, G, Argüelles, C, Axani, S, Bai, X, Balagopal V., A, Barbano, A, Barwick, SW, Bastian, B, Basu, V, Baum, V, Baur, S, Bay, R, Beatty, JJ, Becker, KH, Becker Tjus, J, Bellenghi, C, Benzvi, S, Berley, D, Bernardini, E, Besson, DZ, Binder, G, Bindig, D, Blaufuss, E, Blot, S, Böser, S, Botner, O, Böttcher, J, Bourbeau, E, Bourbeau, J, Bradascio, F, Braun, J, Bron, S, Brostean-Kaiser, J, Burgman, A, Busse, RS, Campana, MA, Chen, C, Chirkin, D, Choi, S, Clark, BA, Clark, K, Classen, L, Coleman, A, Collin, GH, Conrad, JM, Coppin, P, Correa, P, Cowen, DF, Cross, R, Dave, P, De Clercq, C, Delaunay, JJ, Dembinski, H, Deoskar, K, De Ridder, S, Desai, A, Desiati, P, De Vries, KD, De Wasseige, G, De With, M, Deyoung, T, Dharani, S, Diaz, A, Díaz Vélez, JC, Dujmovic, H, Dunkman, M, Duvernois, MA, Dvorak, E, Ehrhardt, T, Eller, P, Engel, R, Evans, J, Evenson, PA, Fahey, S, Fazely, AR, Fiedlschuster, S, Fienberg, AT, Filimonov, K, Finley, C, Fischer, L, Fox, D, Franckowiak, A, Friedman, E, Fritz, A, Fürst, P, Gaisser, TK, Gallagher, J, Abbasi, R, Abbasi, R, Ackermann, M, Adams, J, Aguilar, JA, Ahlers, M, Ahrens, M, Alispach, C, Alves, AA, Amin, NM, An, R, Andeen, K, Anderson, T, Ansseau, I, Anton, G, Argüelles, C, Axani, S, Bai, X, Balagopal V., A, Barbano, A, Barwick, SW, Bastian, B, Basu, V, Baum, V, Baur, S, Bay, R, Beatty, JJ, Becker, KH, Becker Tjus, J, Bellenghi, C, Benzvi, S, Berley, D, Bernardini, E, Besson, DZ, Binder, G, Bindig, D, Blaufuss, E, Blot, S, Böser, S, Botner, O, Böttcher, J, Bourbeau, E, Bourbeau, J, Bradascio, F, Braun, J, Bron, S, Brostean-Kaiser, J, Burgman, A, Busse, RS, Campana, MA, Chen, C, Chirkin, D, Choi, S, Clark, BA, Clark, K, Classen, L, Coleman, A, Collin, GH, Conrad, JM, Coppin, P, Correa, P, Cowen, DF, Cross, R, Dave, P, De Clercq, C, Delaunay, JJ, Dembinski, H, Deoskar, K, De Ridder, S, Desai, A, Desiati, P, De Vries, KD, De Wasseige, G, De With, M, Deyoung, T, Dharani, S, Diaz, A, Díaz Vélez, JC, Dujmovic, H, Dunkman, M, Duvernois, MA, Dvorak, E, Ehrhardt, T, Eller, P, Engel, R, Evans, J, Evenson, PA, Fahey, S, Fazely, AR, Fiedlschuster, S, Fienberg, AT, Filimonov, K, Finley, C, Fischer, L, Fox, D, Franckowiak, A, Friedman, E, Fritz, A, Fürst, P, Gaisser, TK, and Gallagher, J
Abstract: Solar flares convert magnetic energy into thermal and nonthermal plasma energy, the latter implying particle acceleration of charged particles such as protons. Protons are injected out of the coronal acceleration region and can interact with dense plasma in the lower solar atmosphere, producing mesons that subsequently decay into gamma rays and neutrinos at O(MeV-GeV) energies. We present the results of the first search for GeV neutrinos emitted during solar flares carried out with the IceCube Neutrino Observatory. While the experiment was originally designed to detect neutrinos with energies between 10 GeV and a few PeV, a new approach allowing for a O(GeV) energy threshold will be presented. The resulting limits allow us to constrain some of the theoretical estimates of the expected neutrino flux.
Published: 2021

22. LeptonInjector and LeptonWeighter: A neutrino event generator and weighter for neutrino observatories

Author: Abbasi, R, Abbasi, R, Ackermann, M, Adams, J, Aguilar, JA, Ahlers, M, Ahrens, M, Alispach, C, Alves, AA, Amin, NM, An, R, Andeen, K, Anderson, T, Ansseau, I, Anton, G, Argüelles, C, Axani, S, Bai, X, Balagopal, A, Barbano, A, Barwick, SW, Bastian, B, Basu, V, Baum, V, Baur, S, Bay, R, Beatty, JJ, Becker, KH, Becker Tjus, J, Bellenghi, C, BenZvi, S, Berley, D, Bernardini, E, Besson, DZ, Binder, G, Bindig, D, Blaufuss, E, Blot, S, Böser, S, Botner, O, Böttcher, J, Bourbeau, E, Bourbeau, J, Bradascio, F, Braun, J, Bron, S, Brostean-Kaiser, J, Burgman, A, Busse, RS, Campana, MA, Chen, C, Chirkin, D, Choi, S, Clark, BA, Clark, K, Classen, L, Coleman, A, Collin, GH, Conrad, JM, Coppin, P, Correa, P, Cowen, DF, Cross, R, Dave, P, De Clercq, C, DeLaunay, JJ, Dembinski, H, Deoskar, K, De Ridder, S, Desai, A, Desiati, P, de Vries, KD, de Wasseige, G, de With, M, DeYoung, T, Dharani, S, Diaz, A, Díaz-Vélez, JC, Dujmovic, H, Dunkman, M, DuVernois, MA, Dvorak, E, Ehrhardt, T, Eller, P, Engel, R, Evans, J, Evenson, PA, Fahey, S, Fazely, AR, Fiedlschuster, S, Fienberg, AT, Filimonov, K, Finley, C, Fischer, L, Fox, D, Franckowiak, A, Friedman, E, Fritz, A, Fürst, P, Gaisser, TK, Gallagher, J, Abbasi, R, Abbasi, R, Ackermann, M, Adams, J, Aguilar, JA, Ahlers, M, Ahrens, M, Alispach, C, Alves, AA, Amin, NM, An, R, Andeen, K, Anderson, T, Ansseau, I, Anton, G, Argüelles, C, Axani, S, Bai, X, Balagopal, A, Barbano, A, Barwick, SW, Bastian, B, Basu, V, Baum, V, Baur, S, Bay, R, Beatty, JJ, Becker, KH, Becker Tjus, J, Bellenghi, C, BenZvi, S, Berley, D, Bernardini, E, Besson, DZ, Binder, G, Bindig, D, Blaufuss, E, Blot, S, Böser, S, Botner, O, Böttcher, J, Bourbeau, E, Bourbeau, J, Bradascio, F, Braun, J, Bron, S, Brostean-Kaiser, J, Burgman, A, Busse, RS, Campana, MA, Chen, C, Chirkin, D, Choi, S, Clark, BA, Clark, K, Classen, L, Coleman, A, Collin, GH, Conrad, JM, Coppin, P, Correa, P, Cowen, DF, Cross, R, Dave, P, De Clercq, C, DeLaunay, JJ, Dembinski, H, Deoskar, K, De Ridder, S, Desai, A, Desiati, P, de Vries, KD, de Wasseige, G, de With, M, DeYoung, T, Dharani, S, Diaz, A, Díaz-Vélez, JC, Dujmovic, H, Dunkman, M, DuVernois, MA, Dvorak, E, Ehrhardt, T, Eller, P, Engel, R, Evans, J, Evenson, PA, Fahey, S, Fazely, AR, Fiedlschuster, S, Fienberg, AT, Filimonov, K, Finley, C, Fischer, L, Fox, D, Franckowiak, A, Friedman, E, Fritz, A, Fürst, P, Gaisser, TK, and Gallagher, J
Abstract: We present a high-energy neutrino event generator, called LeptonInjector, alongside an event weighter, called LeptonWeighter. Both are designed for large-volume Cherenkov neutrino telescopes such as IceCube. The neutrino event generator allows for quick and flexible simulation of neutrino events within and around the detector volume, and implements the leading Standard Model neutrino interaction processes relevant for neutrino observatories: neutrino-nucleon deep-inelastic scattering and neutrino-electron annihilation. In this paper, we discuss the event generation algorithm, the weighting algorithm, and the main functions of the publicly available code, with examples. Program summary: Program Titles: LeptonInjector and LeptonWeighter CPC Library link to program files: https://doi.org/10.17632/662gkpjfd9.1 Developer's repository links: https://github.com/icecube/LeptonInjector and https://github.com/icecube/LeptonWeighter Licensing provisions: GNU Lesser General Public License, version 3. Programming Language: C++11 External Routines: • Boost • HDF5 • nuflux (https://github.com/icecube/nuflux) • nuSQuIDS (https://github.com/arguelles/nuSQuIDS) • Photospline (https://github.com/icecube/photospline) • SuiteSparse (https://github.com/DrTimothyAldenDavis/SuiteSparse) Nature of problem: LeptonInjector: Generate neutrino interaction events of all possible topologies and energies throughout and around a detector volume. LeptonWeighter: Reweight Monte Carlo events, generated by a set of LeptonInjector Generators, to any desired physical neutrino flux or cross section. Solution method: LeptonInjector: Projected ranges of generated leptons and the extent of the detector, in terms of column depth, are used to inject events in and around the detector volume. Event kinematics follow distributions provided in cross section files. LeptonWeighter: Event generation probabilities are calculated for each Generator, which are then combined into a generation weight and used to calculate
Published: 2021

23. Measurement of the high-energy all-flavor neutrino-nucleon cross section with IceCube

Author: Abbasi, R, Abbasi, R, Ackermann, M, Adams, J, Aguilar, JA, Ahlers, M, Ahrens, M, Alispach, C, Alves, AA, Amin, NM, Andeen, K, Anderson, T, Ansseau, I, Anton, G, Argüelles, C, Axani, S, Bai, X, Balagopal V., A, Barbano, A, Barwick, SW, Bastian, B, Basu, V, Baum, V, Baur, S, Bay, R, Beatty, JJ, Becker, KH, Becker Tjus, J, Bellenghi, C, Benzvi, S, Berley, D, Bernardini, E, Besson, DZ, Binder, G, Bindig, D, Blaufuss, E, Blot, S, Böser, S, Botner, O, Böttcher, J, Bourbeau, E, Bourbeau, J, Bradascio, F, Braun, J, Bron, S, Brostean-Kaiser, J, Burgman, A, Busse, RS, Campana, MA, Chen, C, Chirkin, D, Choi, S, Clark, BA, Clark, K, Classen, L, Coleman, A, Collin, GH, Conrad, JM, Coppin, P, Correa, P, Cowen, DF, Cross, R, Dave, P, De Clercq, C, Delaunay, JJ, Dembinski, H, Deoskar, K, De Ridder, S, Desai, A, Desiati, P, De Vries, KD, De Wasseige, G, De With, M, Deyoung, T, Dharani, S, Diaz, A, Díaz-Vélez, JC, Dujmovic, H, Dunkman, M, Duvernois, MA, Dvorak, E, Ehrhardt, T, Eller, P, Engel, R, Evans, J, Evenson, PA, Fahey, S, Fazely, AR, Fiedlschuster, S, Fienberg, AT, Filimonov, K, Finley, C, Fischer, L, Fox, D, Franckowiak, A, Friedman, E, Fritz, A, Fürst, P, Gaisser, TK, Gallagher, J, Ganster, E, Abbasi, R, Abbasi, R, Ackermann, M, Adams, J, Aguilar, JA, Ahlers, M, Ahrens, M, Alispach, C, Alves, AA, Amin, NM, Andeen, K, Anderson, T, Ansseau, I, Anton, G, Argüelles, C, Axani, S, Bai, X, Balagopal V., A, Barbano, A, Barwick, SW, Bastian, B, Basu, V, Baum, V, Baur, S, Bay, R, Beatty, JJ, Becker, KH, Becker Tjus, J, Bellenghi, C, Benzvi, S, Berley, D, Bernardini, E, Besson, DZ, Binder, G, Bindig, D, Blaufuss, E, Blot, S, Böser, S, Botner, O, Böttcher, J, Bourbeau, E, Bourbeau, J, Bradascio, F, Braun, J, Bron, S, Brostean-Kaiser, J, Burgman, A, Busse, RS, Campana, MA, Chen, C, Chirkin, D, Choi, S, Clark, BA, Clark, K, Classen, L, Coleman, A, Collin, GH, Conrad, JM, Coppin, P, Correa, P, Cowen, DF, Cross, R, Dave, P, De Clercq, C, Delaunay, JJ, Dembinski, H, Deoskar, K, De Ridder, S, Desai, A, Desiati, P, De Vries, KD, De Wasseige, G, De With, M, Deyoung, T, Dharani, S, Diaz, A, Díaz-Vélez, JC, Dujmovic, H, Dunkman, M, Duvernois, MA, Dvorak, E, Ehrhardt, T, Eller, P, Engel, R, Evans, J, Evenson, PA, Fahey, S, Fazely, AR, Fiedlschuster, S, Fienberg, AT, Filimonov, K, Finley, C, Fischer, L, Fox, D, Franckowiak, A, Friedman, E, Fritz, A, Fürst, P, Gaisser, TK, Gallagher, J, and Ganster, E
Abstract: The flux of high-energy neutrinos passing through the Earth is attenuated due to their interactions with matter. The interaction rate is determined by the neutrino interaction cross section and affects the flux arriving at the IceCube Neutrino Observatory, a cubic-kilometer neutrino detector embedded in the Antarctic ice sheet. We present a measurement of the neutrino cross section between 60 TeV and 10 PeV using the high-energy starting event (HESE) sample from IceCube with 7.5 years of data. The result is binned in neutrino energy and obtained using both Bayesian and frequentist statistics. We find it compatible with predictions from the Standard Model. While the cross section is expected to be flavor independent above 1 TeV, additional constraints on the measurement are included through updated experimental particle identification (PID) classifiers, proxies for the three neutrino flavors. This is the first such measurement to use a ternary PID observable and the first to account for neutrinos from tau decay.
Published: 2021

24. A search for time-dependent astrophysical neutrino emission with icecube data from 2012 to 2017

Author: Abbasi, R, Abbasi, R, Ackermann, M, Adams, J, Aguilar, JA, Ahlers, M, Ahrens, M, Alispach, C, Alves, JA, Amin, NM, Andeen, K, Anderson, T, Ansseau, I, Anton, G, Argüelles, C, Axani, S, Bai, X, Balagopal V, A, Barbano, A, Barwick, SW, Bastian, B, Basu, V, Baum, V, Baur, S, Bay, R, Beatty, JJ, Becker, KH, Becker Tjus, J, Bellenghi, C, BenZvi, S, Berley, D, Bernardini, E, Besson, DZ, Binder, G, Bindig, D, Blaufuss, E, Blot, S, Böser, S, Botner, O, Böttcher, J, Bourbeau, E, Bourbeau, J, Bradascio, F, Braun, J, Bron, S, Brostean-Kaiser, J, Burgman, A, Busse, RS, Campana, MA, Chen, C, Chirkin, D, Choi, S, Clark, BA, Clark, K, Classen, L, Coleman, A, Collin, GH, Conrad, JM, Coppin, P, Correa, P, Cowen, DF, Cross, R, Dave, P, De Clercq, C, DeLaunay, JJ, Dembinski, H, Deoskar, K, De Ridder, S, Desai, A, Desiati, P, de Vries, KD, de Wasseige, G, de With, M, DeYoung, T, Dharani, S, Diaz, A, Díaz-Vélez, JC, Dujmovic, H, Dunkman, M, DuVernois, MA, Dvorak, E, Ehrhardt, T, Eller, P, Engel, R, Evans, J, Evenson, PA, Fahey, S, Fazely, AR, Fiedlschuster, S, Fienberg, AT, Filimonov, K, Finley, C, Fischer, L, Fox, D, Franckowiak, A, Friedman, E, Fritz, A, Fürst, P, Gaisser, TK, Gallagher, J, Ganster, E, Abbasi, R, Abbasi, R, Ackermann, M, Adams, J, Aguilar, JA, Ahlers, M, Ahrens, M, Alispach, C, Alves, JA, Amin, NM, Andeen, K, Anderson, T, Ansseau, I, Anton, G, Argüelles, C, Axani, S, Bai, X, Balagopal V, A, Barbano, A, Barwick, SW, Bastian, B, Basu, V, Baum, V, Baur, S, Bay, R, Beatty, JJ, Becker, KH, Becker Tjus, J, Bellenghi, C, BenZvi, S, Berley, D, Bernardini, E, Besson, DZ, Binder, G, Bindig, D, Blaufuss, E, Blot, S, Böser, S, Botner, O, Böttcher, J, Bourbeau, E, Bourbeau, J, Bradascio, F, Braun, J, Bron, S, Brostean-Kaiser, J, Burgman, A, Busse, RS, Campana, MA, Chen, C, Chirkin, D, Choi, S, Clark, BA, Clark, K, Classen, L, Coleman, A, Collin, GH, Conrad, JM, Coppin, P, Correa, P, Cowen, DF, Cross, R, Dave, P, De Clercq, C, DeLaunay, JJ, Dembinski, H, Deoskar, K, De Ridder, S, Desai, A, Desiati, P, de Vries, KD, de Wasseige, G, de With, M, DeYoung, T, Dharani, S, Diaz, A, Díaz-Vélez, JC, Dujmovic, H, Dunkman, M, DuVernois, MA, Dvorak, E, Ehrhardt, T, Eller, P, Engel, R, Evans, J, Evenson, PA, Fahey, S, Fazely, AR, Fiedlschuster, S, Fienberg, AT, Filimonov, K, Finley, C, Fischer, L, Fox, D, Franckowiak, A, Friedman, E, Fritz, A, Fürst, P, Gaisser, TK, Gallagher, J, and Ganster, E
Abstract: High-energy neutrinos are unique messengers of the high-energy universe, tracing the processes of cosmic ray acceleration. This paper presents analyses focusing on time-dependent neutrino point-source searches. A scan of the whole sky, making no prior assumption about source candidates, is performed, looking for a space and time clustering of high-energy neutrinos in data collected by the IceCube Neutrino Observatory between 2012 and 2017. No statistically significant evidence for a time-dependent neutrino signal is found with this search during this period, as all results are consistent with the background expectation. Within this study period, the blazar 3C 279, showed strong variability, inducing a very prominent gamma-ray flare observed in 2015 June. This event motivated a dedicated study of the blazar, which consists of searching for a time-dependent neutrino signal correlated with the gamma-ray emission. No evidence for a time-dependent signal is found. Hence, an upper limit on the neutrino fluence is derived, allowing us to constrain a hadronic emission model.
Published: 2021

25. Search for GeV neutrino emission during intense gamma-ray solar flares with the IceCube Neutrino Observatory

Author: Abbasi, R, Abbasi, R, Ackermann, M, Adams, J, Aguilar, JA, Ahlers, M, Ahrens, M, Alispach, C, Alves, AA, Amin, NM, An, R, Andeen, K, Anderson, T, Ansseau, I, Anton, G, Argüelles, C, Axani, S, Bai, X, Balagopal V., A, Barbano, A, Barwick, SW, Bastian, B, Basu, V, Baum, V, Baur, S, Bay, R, Beatty, JJ, Becker, KH, Becker Tjus, J, Bellenghi, C, Benzvi, S, Berley, D, Bernardini, E, Besson, DZ, Binder, G, Bindig, D, Blaufuss, E, Blot, S, Böser, S, Botner, O, Böttcher, J, Bourbeau, E, Bourbeau, J, Bradascio, F, Braun, J, Bron, S, Brostean-Kaiser, J, Burgman, A, Busse, RS, Campana, MA, Chen, C, Chirkin, D, Choi, S, Clark, BA, Clark, K, Classen, L, Coleman, A, Collin, GH, Conrad, JM, Coppin, P, Correa, P, Cowen, DF, Cross, R, Dave, P, De Clercq, C, Delaunay, JJ, Dembinski, H, Deoskar, K, De Ridder, S, Desai, A, Desiati, P, De Vries, KD, De Wasseige, G, De With, M, Deyoung, T, Dharani, S, Diaz, A, Díaz Vélez, JC, Dujmovic, H, Dunkman, M, Duvernois, MA, Dvorak, E, Ehrhardt, T, Eller, P, Engel, R, Evans, J, Evenson, PA, Fahey, S, Fazely, AR, Fiedlschuster, S, Fienberg, AT, Filimonov, K, Finley, C, Fischer, L, Fox, D, Franckowiak, A, Friedman, E, Fritz, A, Fürst, P, Gaisser, TK, Gallagher, J, Abbasi, R, Abbasi, R, Ackermann, M, Adams, J, Aguilar, JA, Ahlers, M, Ahrens, M, Alispach, C, Alves, AA, Amin, NM, An, R, Andeen, K, Anderson, T, Ansseau, I, Anton, G, Argüelles, C, Axani, S, Bai, X, Balagopal V., A, Barbano, A, Barwick, SW, Bastian, B, Basu, V, Baum, V, Baur, S, Bay, R, Beatty, JJ, Becker, KH, Becker Tjus, J, Bellenghi, C, Benzvi, S, Berley, D, Bernardini, E, Besson, DZ, Binder, G, Bindig, D, Blaufuss, E, Blot, S, Böser, S, Botner, O, Böttcher, J, Bourbeau, E, Bourbeau, J, Bradascio, F, Braun, J, Bron, S, Brostean-Kaiser, J, Burgman, A, Busse, RS, Campana, MA, Chen, C, Chirkin, D, Choi, S, Clark, BA, Clark, K, Classen, L, Coleman, A, Collin, GH, Conrad, JM, Coppin, P, Correa, P, Cowen, DF, Cross, R, Dave, P, De Clercq, C, Delaunay, JJ, Dembinski, H, Deoskar, K, De Ridder, S, Desai, A, Desiati, P, De Vries, KD, De Wasseige, G, De With, M, Deyoung, T, Dharani, S, Diaz, A, Díaz Vélez, JC, Dujmovic, H, Dunkman, M, Duvernois, MA, Dvorak, E, Ehrhardt, T, Eller, P, Engel, R, Evans, J, Evenson, PA, Fahey, S, Fazely, AR, Fiedlschuster, S, Fienberg, AT, Filimonov, K, Finley, C, Fischer, L, Fox, D, Franckowiak, A, Friedman, E, Fritz, A, Fürst, P, Gaisser, TK, and Gallagher, J
Abstract: Solar flares convert magnetic energy into thermal and nonthermal plasma energy, the latter implying particle acceleration of charged particles such as protons. Protons are injected out of the coronal acceleration region and can interact with dense plasma in the lower solar atmosphere, producing mesons that subsequently decay into gamma rays and neutrinos at O(MeV-GeV) energies. We present the results of the first search for GeV neutrinos emitted during solar flares carried out with the IceCube Neutrino Observatory. While the experiment was originally designed to detect neutrinos with energies between 10 GeV and a few PeV, a new approach allowing for a O(GeV) energy threshold will be presented. The resulting limits allow us to constrain some of the theoretical estimates of the expected neutrino flux.
Published: 2021

26. All-flavor constraints on nonstandard neutrino interactions and generalized matter potential with three years of IceCube DeepCore data

Author: Abbasi, R, Abbasi, R, Ackermann, M, Adams, J, Aguilar, JA, Ahlers, M, Ahrens, M, Alispach, C, Alves, AA, Amin, NM, An, R, Andeen, K, Anderson, T, Ansseau, I, Anton, G, Argüelles, C, Ashida, Y, Axani, S, Bai, X, Balagopal V., A, Barbano, A, Barwick, SW, Bastian, B, Basu, V, Baur, S, Bay, R, Beatty, JJ, Becker, KH, Becker Tjus, J, Bellenghi, C, BenZvi, S, Berley, D, Bernardini, E, Besson, DZ, Binder, G, Bindig, D, Blaufuss, E, Blot, S, Bontempo, F, Borowka, J, Böser, S, Botner, O, Böttcher, J, Bourbeau, E, Bradascio, F, Braun, J, Bron, S, Brostean-Kaiser, J, Browne, S, Burgman, A, Busse, RS, Campana, MA, Chen, C, Chirkin, D, Choi, K, Clark, BA, Clark, K, Classen, L, Coleman, A, Collin, GH, Conrad, JM, Coppin, P, Correa, P, Cowen, DF, Cross, R, Dave, P, De Clercq, C, DeLaunay, JJ, Dembinski, H, Deoskar, K, De Ridder, S, Desai, A, Desiati, P, de Vries, KD, de Wasseige, G, de With, M, DeYoung, T, Dharani, S, Diaz, A, Díaz-Vélez, JC, Dujmovic, H, Dunkman, M, DuVernois, MA, Dvorak, E, Ehrhardt, T, Eller, P, Engel, R, Erpenbeck, H, Evans, J, Evenson, PA, Fazely, AR, Fiedlschuster, S, Fienberg, AT, Filimonov, K, Finley, C, Fischer, L, Fox, D, Franckowiak, A, Friedman, E, Fritz, A, Fürst, P, Abbasi, R, Abbasi, R, Ackermann, M, Adams, J, Aguilar, JA, Ahlers, M, Ahrens, M, Alispach, C, Alves, AA, Amin, NM, An, R, Andeen, K, Anderson, T, Ansseau, I, Anton, G, Argüelles, C, Ashida, Y, Axani, S, Bai, X, Balagopal V., A, Barbano, A, Barwick, SW, Bastian, B, Basu, V, Baur, S, Bay, R, Beatty, JJ, Becker, KH, Becker Tjus, J, Bellenghi, C, BenZvi, S, Berley, D, Bernardini, E, Besson, DZ, Binder, G, Bindig, D, Blaufuss, E, Blot, S, Bontempo, F, Borowka, J, Böser, S, Botner, O, Böttcher, J, Bourbeau, E, Bradascio, F, Braun, J, Bron, S, Brostean-Kaiser, J, Browne, S, Burgman, A, Busse, RS, Campana, MA, Chen, C, Chirkin, D, Choi, K, Clark, BA, Clark, K, Classen, L, Coleman, A, Collin, GH, Conrad, JM, Coppin, P, Correa, P, Cowen, DF, Cross, R, Dave, P, De Clercq, C, DeLaunay, JJ, Dembinski, H, Deoskar, K, De Ridder, S, Desai, A, Desiati, P, de Vries, KD, de Wasseige, G, de With, M, DeYoung, T, Dharani, S, Diaz, A, Díaz-Vélez, JC, Dujmovic, H, Dunkman, M, DuVernois, MA, Dvorak, E, Ehrhardt, T, Eller, P, Engel, R, Erpenbeck, H, Evans, J, Evenson, PA, Fazely, AR, Fiedlschuster, S, Fienberg, AT, Filimonov, K, Finley, C, Fischer, L, Fox, D, Franckowiak, A, Friedman, E, Fritz, A, and Fürst, P
Abstract: We report constraints on nonstandard neutrino interactions (NSI) from the observation of atmospheric neutrinos with IceCube, limiting all individual coupling strengths from a single dataset. Furthermore, IceCube is the first experiment to constrain flavor-violating and nonuniversal couplings simultaneously. Hypothetical NSI are generically expected to arise due to the exchange of a new heavy mediator particle. Neutrinos propagating in matter scatter off fermions in the forward direction with negligible momentum transfer. Hence the study of the matter effect on neutrinos propagating in the Earth is sensitive to NSI independently of the energy scale of new physics. We present constraints on NSI obtained with an all-flavor event sample of atmospheric neutrinos based on three years of IceCube DeepCore data. The analysis uses neutrinos arriving from all directions, with reconstructed energies between 5.6 GeV and 100 GeV. We report constraints on the individual NSI coupling strengths considered singly, allowing for complex phases in the case of flavor-violating couplings. This demonstrates that IceCube is sensitive to the full NSI flavor structure at a level competitive with limits from the global analysis of all other experiments. In addition, we investigate a generalized matter potential, whose overall scale and flavor structure are also constrained.
Published: 2021

27. Measurement of the high-energy all-flavor neutrino-nucleon cross section with IceCube

Author: Abbasi, R, Abbasi, R, Ackermann, M, Adams, J, Aguilar, JA, Ahlers, M, Ahrens, M, Alispach, C, Alves, AA, Amin, NM, Andeen, K, Anderson, T, Ansseau, I, Anton, G, Argüelles, C, Axani, S, Bai, X, Balagopal V., A, Barbano, A, Barwick, SW, Bastian, B, Basu, V, Baum, V, Baur, S, Bay, R, Beatty, JJ, Becker, KH, Becker Tjus, J, Bellenghi, C, Benzvi, S, Berley, D, Bernardini, E, Besson, DZ, Binder, G, Bindig, D, Blaufuss, E, Blot, S, Böser, S, Botner, O, Böttcher, J, Bourbeau, E, Bourbeau, J, Bradascio, F, Braun, J, Bron, S, Brostean-Kaiser, J, Burgman, A, Busse, RS, Campana, MA, Chen, C, Chirkin, D, Choi, S, Clark, BA, Clark, K, Classen, L, Coleman, A, Collin, GH, Conrad, JM, Coppin, P, Correa, P, Cowen, DF, Cross, R, Dave, P, De Clercq, C, Delaunay, JJ, Dembinski, H, Deoskar, K, De Ridder, S, Desai, A, Desiati, P, De Vries, KD, De Wasseige, G, De With, M, Deyoung, T, Dharani, S, Diaz, A, Díaz-Vélez, JC, Dujmovic, H, Dunkman, M, Duvernois, MA, Dvorak, E, Ehrhardt, T, Eller, P, Engel, R, Evans, J, Evenson, PA, Fahey, S, Fazely, AR, Fiedlschuster, S, Fienberg, AT, Filimonov, K, Finley, C, Fischer, L, Fox, D, Franckowiak, A, Friedman, E, Fritz, A, Fürst, P, Gaisser, TK, Gallagher, J, Ganster, E, Abbasi, R, Abbasi, R, Ackermann, M, Adams, J, Aguilar, JA, Ahlers, M, Ahrens, M, Alispach, C, Alves, AA, Amin, NM, Andeen, K, Anderson, T, Ansseau, I, Anton, G, Argüelles, C, Axani, S, Bai, X, Balagopal V., A, Barbano, A, Barwick, SW, Bastian, B, Basu, V, Baum, V, Baur, S, Bay, R, Beatty, JJ, Becker, KH, Becker Tjus, J, Bellenghi, C, Benzvi, S, Berley, D, Bernardini, E, Besson, DZ, Binder, G, Bindig, D, Blaufuss, E, Blot, S, Böser, S, Botner, O, Böttcher, J, Bourbeau, E, Bourbeau, J, Bradascio, F, Braun, J, Bron, S, Brostean-Kaiser, J, Burgman, A, Busse, RS, Campana, MA, Chen, C, Chirkin, D, Choi, S, Clark, BA, Clark, K, Classen, L, Coleman, A, Collin, GH, Conrad, JM, Coppin, P, Correa, P, Cowen, DF, Cross, R, Dave, P, De Clercq, C, Delaunay, JJ, Dembinski, H, Deoskar, K, De Ridder, S, Desai, A, Desiati, P, De Vries, KD, De Wasseige, G, De With, M, Deyoung, T, Dharani, S, Diaz, A, Díaz-Vélez, JC, Dujmovic, H, Dunkman, M, Duvernois, MA, Dvorak, E, Ehrhardt, T, Eller, P, Engel, R, Evans, J, Evenson, PA, Fahey, S, Fazely, AR, Fiedlschuster, S, Fienberg, AT, Filimonov, K, Finley, C, Fischer, L, Fox, D, Franckowiak, A, Friedman, E, Fritz, A, Fürst, P, Gaisser, TK, Gallagher, J, and Ganster, E
Abstract: The flux of high-energy neutrinos passing through the Earth is attenuated due to their interactions with matter. The interaction rate is determined by the neutrino interaction cross section and affects the flux arriving at the IceCube Neutrino Observatory, a cubic-kilometer neutrino detector embedded in the Antarctic ice sheet. We present a measurement of the neutrino cross section between 60 TeV and 10 PeV using the high-energy starting event (HESE) sample from IceCube with 7.5 years of data. The result is binned in neutrino energy and obtained using both Bayesian and frequentist statistics. We find it compatible with predictions from the Standard Model. While the cross section is expected to be flavor independent above 1 TeV, additional constraints on the measurement are included through updated experimental particle identification (PID) classifiers, proxies for the three neutrino flavors. This is the first such measurement to use a ternary PID observable and the first to account for neutrinos from tau decay.
Published: 2021

28. LeptonInjector and LeptonWeighter: A neutrino event generator and weighter for neutrino observatories

Author: Abbasi, R, Abbasi, R, Ackermann, M, Adams, J, Aguilar, JA, Ahlers, M, Ahrens, M, Alispach, C, Alves, AA, Amin, NM, An, R, Andeen, K, Anderson, T, Ansseau, I, Anton, G, Argüelles, C, Axani, S, Bai, X, Balagopal, A, Barbano, A, Barwick, SW, Bastian, B, Basu, V, Baum, V, Baur, S, Bay, R, Beatty, JJ, Becker, KH, Becker Tjus, J, Bellenghi, C, BenZvi, S, Berley, D, Bernardini, E, Besson, DZ, Binder, G, Bindig, D, Blaufuss, E, Blot, S, Böser, S, Botner, O, Böttcher, J, Bourbeau, E, Bourbeau, J, Bradascio, F, Braun, J, Bron, S, Brostean-Kaiser, J, Burgman, A, Busse, RS, Campana, MA, Chen, C, Chirkin, D, Choi, S, Clark, BA, Clark, K, Classen, L, Coleman, A, Collin, GH, Conrad, JM, Coppin, P, Correa, P, Cowen, DF, Cross, R, Dave, P, De Clercq, C, DeLaunay, JJ, Dembinski, H, Deoskar, K, De Ridder, S, Desai, A, Desiati, P, de Vries, KD, de Wasseige, G, de With, M, DeYoung, T, Dharani, S, Diaz, A, Díaz-Vélez, JC, Dujmovic, H, Dunkman, M, DuVernois, MA, Dvorak, E, Ehrhardt, T, Eller, P, Engel, R, Evans, J, Evenson, PA, Fahey, S, Fazely, AR, Fiedlschuster, S, Fienberg, AT, Filimonov, K, Finley, C, Fischer, L, Fox, D, Franckowiak, A, Friedman, E, Fritz, A, Fürst, P, Gaisser, TK, Gallagher, J, Abbasi, R, Abbasi, R, Ackermann, M, Adams, J, Aguilar, JA, Ahlers, M, Ahrens, M, Alispach, C, Alves, AA, Amin, NM, An, R, Andeen, K, Anderson, T, Ansseau, I, Anton, G, Argüelles, C, Axani, S, Bai, X, Balagopal, A, Barbano, A, Barwick, SW, Bastian, B, Basu, V, Baum, V, Baur, S, Bay, R, Beatty, JJ, Becker, KH, Becker Tjus, J, Bellenghi, C, BenZvi, S, Berley, D, Bernardini, E, Besson, DZ, Binder, G, Bindig, D, Blaufuss, E, Blot, S, Böser, S, Botner, O, Böttcher, J, Bourbeau, E, Bourbeau, J, Bradascio, F, Braun, J, Bron, S, Brostean-Kaiser, J, Burgman, A, Busse, RS, Campana, MA, Chen, C, Chirkin, D, Choi, S, Clark, BA, Clark, K, Classen, L, Coleman, A, Collin, GH, Conrad, JM, Coppin, P, Correa, P, Cowen, DF, Cross, R, Dave, P, De Clercq, C, DeLaunay, JJ, Dembinski, H, Deoskar, K, De Ridder, S, Desai, A, Desiati, P, de Vries, KD, de Wasseige, G, de With, M, DeYoung, T, Dharani, S, Diaz, A, Díaz-Vélez, JC, Dujmovic, H, Dunkman, M, DuVernois, MA, Dvorak, E, Ehrhardt, T, Eller, P, Engel, R, Evans, J, Evenson, PA, Fahey, S, Fazely, AR, Fiedlschuster, S, Fienberg, AT, Filimonov, K, Finley, C, Fischer, L, Fox, D, Franckowiak, A, Friedman, E, Fritz, A, Fürst, P, Gaisser, TK, and Gallagher, J
Abstract: We present a high-energy neutrino event generator, called LeptonInjector, alongside an event weighter, called LeptonWeighter. Both are designed for large-volume Cherenkov neutrino telescopes such as IceCube. The neutrino event generator allows for quick and flexible simulation of neutrino events within and around the detector volume, and implements the leading Standard Model neutrino interaction processes relevant for neutrino observatories: neutrino-nucleon deep-inelastic scattering and neutrino-electron annihilation. In this paper, we discuss the event generation algorithm, the weighting algorithm, and the main functions of the publicly available code, with examples. Program summary: Program Titles: LeptonInjector and LeptonWeighter CPC Library link to program files: https://doi.org/10.17632/662gkpjfd9.1 Developer's repository links: https://github.com/icecube/LeptonInjector and https://github.com/icecube/LeptonWeighter Licensing provisions: GNU Lesser General Public License, version 3. Programming Language: C++11 External Routines: • Boost • HDF5 • nuflux (https://github.com/icecube/nuflux) • nuSQuIDS (https://github.com/arguelles/nuSQuIDS) • Photospline (https://github.com/icecube/photospline) • SuiteSparse (https://github.com/DrTimothyAldenDavis/SuiteSparse) Nature of problem: LeptonInjector: Generate neutrino interaction events of all possible topologies and energies throughout and around a detector volume. LeptonWeighter: Reweight Monte Carlo events, generated by a set of LeptonInjector Generators, to any desired physical neutrino flux or cross section. Solution method: LeptonInjector: Projected ranges of generated leptons and the extent of the detector, in terms of column depth, are used to inject events in and around the detector volume. Event kinematics follow distributions provided in cross section files. LeptonWeighter: Event generation probabilities are calculated for each Generator, which are then combined into a generation weight and used to calculate
Published: 2021

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28 results on '"Campana MA"'

1. Search for 10–1000 GeV Neutrinos from Gamma-Ray Bursts with IceCube

2. A Search for IceCube Sub-TeV Neutrinos Correlated with Gravitational-wave Events Detected By LIGO/Virgo

3. Search for neutrino lines from dark matter annihilation and decay with IceCube

4. IceCat-1: The IceCube Event Catalog of Alert Tracks

5. Constraining High-energy Neutrino Emission from Supernovae with IceCube

6. Constraints on Populations of Neutrino Sources from Searches in the Directions of IceCube Neutrino Alerts

7. First all-flavor search for transient neutrino emission using 3-years of IceCube DeepCore data

8. Search for GeV-scale dark matter annihilation in the Sun with IceCube DeepCore

9. Search for High-energy Neutrino Emission from Galactic X-Ray Binaries with IceCube

10. Search for GeV-scale dark matter annihilation in the Sun with IceCube DeepCore

11. First all-flavor search for transient neutrino emission using 3-years of IceCube DeepCore data

12. Density of GeV muons in air showers measured with IceTop.

13. Search for High-energy Neutrino Emission from Galactic X-Ray Binaries with IceCube

14. Searches for Neutrinos from Gamma-Ray Bursts Using the IceCube Neutrino Observatory

15. Graph Neural Networks for low-energy event classification & reconstruction in IceCube

16. Search for quantum gravity using astrophysical neutrino flavour with IceCube

17. Searching for High-energy Neutrino Emission from Galaxy Clusters with IceCube

18. Search for Astrophysical Neutrinos from 1FLE Blazars with IceCube

19. A search for time-dependent astrophysical neutrino emission with icecube data from 2012 to 2017

20. Measurement of the high-energy all-flavor neutrino-nucleon cross section with IceCube

21. Search for GeV neutrino emission during intense gamma-ray solar flares with the IceCube Neutrino Observatory

22. LeptonInjector and LeptonWeighter: A neutrino event generator and weighter for neutrino observatories

23. Measurement of the high-energy all-flavor neutrino-nucleon cross section with IceCube

24. A search for time-dependent astrophysical neutrino emission with icecube data from 2012 to 2017

25. Search for GeV neutrino emission during intense gamma-ray solar flares with the IceCube Neutrino Observatory

26. All-flavor constraints on nonstandard neutrino interactions and generalized matter potential with three years of IceCube DeepCore data

27. Measurement of the high-energy all-flavor neutrino-nucleon cross section with IceCube

28. LeptonInjector and LeptonWeighter: A neutrino event generator and weighter for neutrino observatories

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28 results on '"Campana MA"'

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