# Constraining High-Energy Neutrino Emission from Supernovae with IceCube

R. Abbasi Department of Physics, Loyola University Chicago, Chicago, IL 60660,
USA  M. Ackermann Deutsches Elektronen-Synchrotron DESY, Platanenallee 6,
15738 Zeuthen, Germany  J. Adams  Dept. of Physics and Astronomy, University
of Canterbury, Private Bag 4800, Christchurch, New Zealand  S. K. Agarwalla
also at Institute of Physics, Sachivalaya Marg, Sainik School Post,
Bhubaneswar 751005, India  Dept. of Physics and Wisconsin IceCube Particle
Astrophysics Center, University of Wisconsin–Madison, Madison, WI 53706, USA
J. A. Aguilar Université Libre de Bruxelles, Science Faculty CP230, B-1050
Brussels, Belgium  M. Ahlers Niels Bohr Institute, University of Copenhagen,
DK-2100 Copenhagen, Denmark  J.M. Alameddine Dept. of Physics, TU Dortmund
University, D-44221 Dortmund, Germany  N. M. Amin  Bartol Research Institute
and Dept. of Physics and Astronomy, University of Delaware, Newark, DE 19716,
USA  K. Andeen  Department of Physics, Marquette University, Milwaukee, WI,
53201, USA  G. Anton Erlangen Centre for Astroparticle Physics, Friedrich-
Alexander-Universität Erlangen-Nürnberg, D-91058 Erlangen, Germany  C.
Argüelles Department of Physics and Laboratory for Particle Physics and
Cosmology, Harvard University, Cambridge, MA 02138, USA  Y. Ashida  Dept. of
Physics and Wisconsin IceCube Particle Astrophysics Center, University of
Wisconsin–Madison, Madison, WI 53706, USA  S. Athanasiadou  Deutsches
Elektronen-Synchrotron DESY, Platanenallee 6, 15738 Zeuthen, Germany  S. N.
Axani Bartol Research Institute and Dept. of Physics and Astronomy, University
of Delaware, Newark, DE 19716, USA  X. Bai Physics Department, South Dakota
School of Mines and Technology, Rapid City, SD 57701, USA  A. Balagopal V.
Dept. of Physics and Wisconsin IceCube Particle Astrophysics Center,
University of Wisconsin–Madison, Madison, WI 53706, USA  M. Baricevic  Dept.
of Physics and Wisconsin IceCube Particle Astrophysics Center, University of
Wisconsin–Madison, Madison, WI 53706, USA  S. W. Barwick Dept. of Physics and
Astronomy, University of California, Irvine, CA 92697, USA  V. Basu Dept. of
Physics and Wisconsin IceCube Particle Astrophysics Center, University of
Wisconsin–Madison, Madison, WI 53706, USA  R. Bay  Dept. of Physics,
University of California, Berkeley, CA 94720, USA  J. J. Beatty Dept. of
Astronomy, Ohio State University, Columbus, OH 43210, USA  Dept. of Physics
and Center for Cosmology and Astro-Particle Physics, Ohio State University,
Columbus, OH 43210, USA  K.-H. Becker  Dept. of Physics, University of
Wuppertal, D-42119 Wuppertal, Germany  J. Becker Tjus also at Department of
Space, Earth and Environment, Chalmers University of Technology, 412 96
Gothenburg, Sweden  Fakultät für Physik & Astronomie, Ruhr-Universität Bochum,
D-44780 Bochum, Germany  J. Beise Dept. of Physics and Astronomy, Uppsala
University, Box 516, S-75120 Uppsala, Sweden  C. Bellenghi  Physik-department,
Technische Universität München, D-85748 Garching, Germany  S. BenZvi Dept. of
Physics and Astronomy, University of Rochester, Rochester, NY 14627, USA  D.
Berley  Dept. of Physics, University of Maryland, College Park, MD 20742, USA
E. Bernardini Dipartimento di Fisica e Astronomia Galileo Galilei, Università
Degli Studi di Padova, 35122 Padova PD, Italy  D. Z. Besson  Dept. of Physics
and Astronomy, University of Kansas, Lawrence, KS 66045, USA  G. Binder  Dept.
of Physics, University of California, Berkeley, CA 94720, USA  Lawrence
Berkeley National Laboratory, Berkeley, CA 94720, USA  D. Bindig  Dept. of
Physics, University of Wuppertal, D-42119 Wuppertal, Germany  E. Blaufuss
Dept. of Physics, University of Maryland, College Park, MD 20742, USA  S. Blot
Deutsches Elektronen-Synchrotron DESY, Platanenallee 6, 15738 Zeuthen, Germany
F. Bontempo  Karlsruhe Institute of Technology, Institute for Astroparticle
Physics, D-76021 Karlsruhe, Germany  J. Y. Book Department of Physics and
Laboratory for Particle Physics and Cosmology, Harvard University, Cambridge,
MA 02138, USA  C. Boscolo Meneguolo Dipartimento di Fisica e Astronomia
Galileo Galilei, Università Degli Studi di Padova, 35122 Padova PD, Italy  S.
Böser Institute of Physics, University of Mainz, Staudinger Weg 7, D-55099
Mainz, Germany  O. Botner Dept. of Physics and Astronomy, Uppsala University,
Box 516, S-75120 Uppsala, Sweden  J. Böttcher  III. Physikalisches Institut,
RWTH Aachen University, D-52056 Aachen, Germany  E. Bourbeau  Niels Bohr
Institute, University of Copenhagen, DK-2100 Copenhagen, Denmark  J. Braun
Dept. of Physics and Wisconsin IceCube Particle Astrophysics Center,
University of Wisconsin–Madison, Madison, WI 53706, USA  B. Brinson  School of
Physics and Center for Relativistic Astrophysics, Georgia Institute of
Technology, Atlanta, GA 30332, USA  J. Brostean-Kaiser  Deutsches Elektronen-
Synchrotron DESY, Platanenallee 6, 15738 Zeuthen, Germany  R. T. Burley
Department of Physics, University of Adelaide, Adelaide, 5005, Australia  R.
S. Busse  Institut für Kernphysik, Westfälische Wilhelms-Universität Münster,
D-48149 Münster, Germany  D. Butterfield  Dept. of Physics and Wisconsin
IceCube Particle Astrophysics Center, University of Wisconsin–Madison,
Madison, WI 53706, USA  M. A. Campana Dept. of Physics, Drexel University,
3141 Chestnut Street, Philadelphia, PA 19104, USA  K. Carloni  Department of
Physics and Laboratory for Particle Physics and Cosmology, Harvard University,
Cambridge, MA 02138, USA  E. G. Carnie-Bronca  Department of Physics,
University of Adelaide, Adelaide, 5005, Australia  S. Chattopadhyay  also at
Institute of Physics, Sachivalaya Marg, Sainik School Post, Bhubaneswar
751005, India  Dept. of Physics and Wisconsin IceCube Particle Astrophysics
Center, University of Wisconsin–Madison, Madison, WI 53706, USA  C. Chen
School of Physics and Center for Relativistic Astrophysics, Georgia Institute
of Technology, Atlanta, GA 30332, USA  Z. Chen  Dept. of Physics and
Astronomy, Stony Brook University, Stony Brook, NY 11794-3800, USA  D. Chirkin
Dept. of Physics and Wisconsin IceCube Particle Astrophysics Center,
University of Wisconsin–Madison, Madison, WI 53706, USA  S. Choi  Dept. of
Physics, Sungkyunkwan University, Suwon 16419, Korea  B. A. Clark Dept. of
Physics, University of Maryland, College Park, MD 20742, USA  L. Classen
Institut für Kernphysik, Westfälische Wilhelms-Universität Münster, D-48149
Münster, Germany  A. Coleman Dept. of Physics and Astronomy, Uppsala
University, Box 516, S-75120 Uppsala, Sweden  G. H. Collin  Dept. of Physics,
Massachusetts Institute of Technology, Cambridge, MA 02139, USA  A. Connolly
Dept. of Astronomy, Ohio State University, Columbus, OH 43210, USA  Dept. of
Physics and Center for Cosmology and Astro-Particle Physics, Ohio State
University, Columbus, OH 43210, USA  J. M. Conrad Dept. of Physics,
Massachusetts Institute of Technology, Cambridge, MA 02139, USA  P. Coppin
Vrije Universiteit Brussel (VUB), Dienst ELEM, B-1050 Brussels, Belgium  P.
Correa Vrije Universiteit Brussel (VUB), Dienst ELEM, B-1050 Brussels, Belgium
S. Countryman  Columbia Astrophysics and Nevis Laboratories, Columbia
University, New York, NY 10027, USA  D. F. Cowen  Dept. of Astronomy and
Astrophysics, Pennsylvania State University, University Park, PA 16802, USA
Dept. of Physics, Pennsylvania State University, University Park, PA 16802,
USA  P. Dave School of Physics and Center for Relativistic Astrophysics,
Georgia Institute of Technology, Atlanta, GA 30332, USA  C. De Clercq Vrije
Universiteit Brussel (VUB), Dienst ELEM, B-1050 Brussels, Belgium  J. J.
DeLaunay Dept. of Physics and Astronomy, University of Alabama, Tuscaloosa, AL
35487, USA  D. Delgado López Department of Physics and Laboratory for Particle
Physics and Cosmology, Harvard University, Cambridge, MA 02138, USA  H.
Dembinski Bartol Research Institute and Dept. of Physics and Astronomy,
University of Delaware, Newark, DE 19716, USA  K. Deoskar  Oskar Klein Centre
and Dept. of Physics, Stockholm University, SE-10691 Stockholm, Sweden  A.
Desai Dept. of Physics and Wisconsin IceCube Particle Astrophysics Center,
University of Wisconsin–Madison, Madison, WI 53706, USA  P. Desiati Dept. of
Physics and Wisconsin IceCube Particle Astrophysics Center, University of
Wisconsin–Madison, Madison, WI 53706, USA  K. D. de Vries Vrije Universiteit
Brussel (VUB), Dienst ELEM, B-1050 Brussels, Belgium  G. de Wasseige Centre
for Cosmology, Particle Physics and Phenomenology - CP3, Université catholique
de Louvain, Louvain-la-Neuve, Belgium  T. DeYoung Dept. of Physics and
Astronomy, Michigan State University, East Lansing, MI 48824, USA  A. Diaz
Dept. of Physics, Massachusetts Institute of Technology, Cambridge, MA 02139,
USA  J. C. Díaz-Vélez Dept. of Physics and Wisconsin IceCube Particle
Astrophysics Center, University of Wisconsin–Madison, Madison, WI 53706, USA
M. Dittmer  Institut für Kernphysik, Westfälische Wilhelms-Universität
Münster, D-48149 Münster, Germany  A. Domi  Erlangen Centre for Astroparticle
Physics, Friedrich-Alexander-Universität Erlangen-Nürnberg, D-91058 Erlangen,
Germany  H. Dujmovic Dept. of Physics and Wisconsin IceCube Particle
Astrophysics Center, University of Wisconsin–Madison, Madison, WI 53706, USA
M. A. DuVernois Dept. of Physics and Wisconsin IceCube Particle Astrophysics
Center, University of Wisconsin–Madison, Madison, WI 53706, USA  T. Ehrhardt
Institute of Physics, University of Mainz, Staudinger Weg 7, D-55099 Mainz,
Germany  P. Eller Physik-department, Technische Universität München, D-85748
Garching, Germany  R. Engel  Karlsruhe Institute of Technology, Institute for
Astroparticle Physics, D-76021 Karlsruhe, Germany  Karlsruhe Institute of
Technology, Institute of Experimental Particle Physics, D-76021 Karlsruhe,
Germany  H. Erpenbeck  Dept. of Physics and Wisconsin IceCube Particle
Astrophysics Center, University of Wisconsin–Madison, Madison, WI 53706, USA
J. Evans  Dept. of Physics, University of Maryland, College Park, MD 20742,
USA  P. A. Evenson  Bartol Research Institute and Dept. of Physics and
Astronomy, University of Delaware, Newark, DE 19716, USA  K. L. Fan  Dept. of
Physics, University of Maryland, College Park, MD 20742, USA  K. Fang  Dept.
of Physics and Wisconsin IceCube Particle Astrophysics Center, University of
Wisconsin–Madison, Madison, WI 53706, USA  A. R. Fazely Dept. of Physics,
Southern University, Baton Rouge, LA 70813, USA  A. Fedynitch Institute of
Physics, Academia Sinica, Taipei, 11529, Taiwan  N. Feigl  Institut für
Physik, Humboldt-Universität zu Berlin, D-12489 Berlin, Germany  S.
Fiedlschuster  Erlangen Centre for Astroparticle Physics, Friedrich-Alexander-
Universität Erlangen-Nürnberg, D-91058 Erlangen, Germany  C. Finley Oskar
Klein Centre and Dept. of Physics, Stockholm University, SE-10691 Stockholm,
Sweden  L. Fischer  Deutsches Elektronen-Synchrotron DESY, Platanenallee 6,
15738 Zeuthen, Germany  D. Fox Dept. of Astronomy and Astrophysics,
Pennsylvania State University, University Park, PA 16802, USA  A. Franckowiak
Fakultät für Physik & Astronomie, Ruhr-Universität Bochum, D-44780 Bochum,
Germany  E. Friedman  Dept. of Physics, University of Maryland, College Park,
MD 20742, USA  A. Fritz  Institute of Physics, University of Mainz, Staudinger
Weg 7, D-55099 Mainz, Germany  P. Fürst  III. Physikalisches Institut, RWTH
Aachen University, D-52056 Aachen, Germany  T. K. Gaisser Bartol Research
Institute and Dept. of Physics and Astronomy, University of Delaware, Newark,
DE 19716, USA  J. Gallagher  Dept. of Astronomy, University of
Wisconsin–Madison, Madison, WI 53706, USA  E. Ganster III. Physikalisches
Institut, RWTH Aachen University, D-52056 Aachen, Germany  A. Garcia
Department of Physics and Laboratory for Particle Physics and Cosmology,
Harvard University, Cambridge, MA 02138, USA  S. Garrappa Deutsches
Elektronen-Synchrotron DESY, Platanenallee 6, 15738 Zeuthen, Germany  L.
Gerhardt  Lawrence Berkeley National Laboratory, Berkeley, CA 94720, USA  A.
Ghadimi Dept. of Physics and Astronomy, University of Alabama, Tuscaloosa, AL
35487, USA  C. Glaser  Dept. of Physics and Astronomy, Uppsala University, Box
516, S-75120 Uppsala, Sweden  T. Glauch Physik-department, Technische
Universität München, D-85748 Garching, Germany  T. Glüsenkamp Erlangen Centre
for Astroparticle Physics, Friedrich-Alexander-Universität Erlangen-Nürnberg,
D-91058 Erlangen, Germany  Dept. of Physics and Astronomy, Uppsala University,
Box 516, S-75120 Uppsala, Sweden  N. Goehlke  Karlsruhe Institute of
Technology, Institute of Experimental Particle Physics, D-76021 Karlsruhe,
Germany  J. G. Gonzalez  Bartol Research Institute and Dept. of Physics and
Astronomy, University of Delaware, Newark, DE 19716, USA  S. Goswami  Dept. of
Physics and Astronomy, University of Alabama, Tuscaloosa, AL 35487, USA  D.
Grant  Dept. of Physics and Astronomy, Michigan State University, East
Lansing, MI 48824, USA  S. J. Gray Dept. of Physics, University of Maryland,
College Park, MD 20742, USA  S. Griffin  Dept. of Physics and Wisconsin
IceCube Particle Astrophysics Center, University of Wisconsin–Madison,
Madison, WI 53706, USA  S. Griswold Dept. of Physics and Astronomy, University
of Rochester, Rochester, NY 14627, USA  C. Günther  III. Physikalisches
Institut, RWTH Aachen University, D-52056 Aachen, Germany  P. Gutjahr Dept. of
Physics, TU Dortmund University, D-44221 Dortmund, Germany  C. Haack  Physik-
department, Technische Universität München, D-85748 Garching, Germany  A.
Hallgren Dept. of Physics and Astronomy, Uppsala University, Box 516, S-75120
Uppsala, Sweden  R. Halliday  Dept. of Physics and Astronomy, Michigan State
University, East Lansing, MI 48824, USA  L. Halve III. Physikalisches
Institut, RWTH Aachen University, D-52056 Aachen, Germany  F. Halzen Dept. of
Physics and Wisconsin IceCube Particle Astrophysics Center, University of
Wisconsin–Madison, Madison, WI 53706, USA  H. Hamdaoui Dept. of Physics and
Astronomy, Stony Brook University, Stony Brook, NY 11794-3800, USA  M. Ha Minh
Physik-department, Technische Universität München, D-85748 Garching, Germany
K. Hanson  Dept. of Physics and Wisconsin IceCube Particle Astrophysics
Center, University of Wisconsin–Madison, Madison, WI 53706, USA  J. Hardin
Dept. of Physics, Massachusetts Institute of Technology, Cambridge, MA 02139,
USA  A. A. Harnisch  Dept. of Physics and Astronomy, Michigan State
University, East Lansing, MI 48824, USA  P. Hatch  Dept. of Physics,
Engineering Physics, and Astronomy, Queen’s University, Kingston, ON K7L 3N6,
Canada  A. Haungs Karlsruhe Institute of Technology, Institute for
Astroparticle Physics, D-76021 Karlsruhe, Germany  K. Helbing Dept. of
Physics, University of Wuppertal, D-42119 Wuppertal, Germany  J. Hellrung
Fakultät für Physik & Astronomie, Ruhr-Universität Bochum, D-44780 Bochum,
Germany  F. Henningsen Physik-department, Technische Universität München,
D-85748 Garching, Germany  L. Heuermann  III. Physikalisches Institut, RWTH
Aachen University, D-52056 Aachen, Germany  S. Hickford  Dept. of Physics,
University of Wuppertal, D-42119 Wuppertal, Germany  A. Hidvegi  Oskar Klein
Centre and Dept. of Physics, Stockholm University, SE-10691 Stockholm, Sweden
C. Hill Dept. of Physics and The International Center for Hadron Astrophysics,
Chiba University, Chiba 263-8522, Japan  G. C. Hill  Department of Physics,
University of Adelaide, Adelaide, 5005, Australia  K. D. Hoffman  Dept. of
Physics, University of Maryland, College Park, MD 20742, USA  K. Hoshina  also
at Earthquake Research Institute, University of Tokyo, Bunkyo, Tokyo 113-0032,
Japan  Dept. of Physics and Wisconsin IceCube Particle Astrophysics Center,
University of Wisconsin–Madison, Madison, WI 53706, USA  W. Hou Karlsruhe
Institute of Technology, Institute for Astroparticle Physics, D-76021
Karlsruhe, Germany  T. Huber Karlsruhe Institute of Technology, Institute for
Astroparticle Physics, D-76021 Karlsruhe, Germany  K. Hultqvist Oskar Klein
Centre and Dept. of Physics, Stockholm University, SE-10691 Stockholm, Sweden
M. Hünnefeld  Dept. of Physics, TU Dortmund University, D-44221 Dortmund,
Germany  R. Hussain  Dept. of Physics and Wisconsin IceCube Particle
Astrophysics Center, University of Wisconsin–Madison, Madison, WI 53706, USA
K. Hymon  Dept. of Physics, TU Dortmund University, D-44221 Dortmund, Germany
S. In  Dept. of Physics, Sungkyunkwan University, Suwon 16419, Korea  N.
Iovine Université Libre de Bruxelles, Science Faculty CP230, B-1050 Brussels,
Belgium  A. Ishihara  Dept. of Physics and The International Center for Hadron
Astrophysics, Chiba University, Chiba 263-8522, Japan  M. Jacquart  Dept. of
Physics and Wisconsin IceCube Particle Astrophysics Center, University of
Wisconsin–Madison, Madison, WI 53706, USA  M. Jansson  Oskar Klein Centre and
Dept. of Physics, Stockholm University, SE-10691 Stockholm, Sweden  G. S.
Japaridze CTSPS, Clark-Atlanta University, Atlanta, GA 30314, USA  K.
Jayakumar  also at Institute of Physics, Sachivalaya Marg, Sainik School Post,
Bhubaneswar 751005, India  Dept. of Physics and Wisconsin IceCube Particle
Astrophysics Center, University of Wisconsin–Madison, Madison, WI 53706, USA
M. Jeong  Dept. of Physics, Sungkyunkwan University, Suwon 16419, Korea  M.
Jin Department of Physics and Laboratory for Particle Physics and Cosmology,
Harvard University, Cambridge, MA 02138, USA  B. J. P. Jones Dept. of Physics,
University of Texas at Arlington, 502 Yates St., Science Hall Rm 108, Box
19059, Arlington, TX 76019, USA  D. Kang Karlsruhe Institute of Technology,
Institute for Astroparticle Physics, D-76021 Karlsruhe, Germany  W. Kang Dept.
of Physics, Sungkyunkwan University, Suwon 16419, Korea  X. Kang  Dept. of
Physics, Drexel University, 3141 Chestnut Street, Philadelphia, PA 19104, USA
A. Kappes Institut für Kernphysik, Westfälische Wilhelms-Universität Münster,
D-48149 Münster, Germany  D. Kappesser  Institute of Physics, University of
Mainz, Staudinger Weg 7, D-55099 Mainz, Germany  L. Kardum  Dept. of Physics,
TU Dortmund University, D-44221 Dortmund, Germany  T. Karg Deutsches
Elektronen-Synchrotron DESY, Platanenallee 6, 15738 Zeuthen, Germany  M. Karl
Physik-department, Technische Universität München, D-85748 Garching, Germany
A. Karle Dept. of Physics and Wisconsin IceCube Particle Astrophysics Center,
University of Wisconsin–Madison, Madison, WI 53706, USA  U. Katz Erlangen
Centre for Astroparticle Physics, Friedrich-Alexander-Universität Erlangen-
Nürnberg, D-91058 Erlangen, Germany  M. Kauer Dept. of Physics and Wisconsin
IceCube Particle Astrophysics Center, University of Wisconsin–Madison,
Madison, WI 53706, USA  J. L. Kelley Dept. of Physics and Wisconsin IceCube
Particle Astrophysics Center, University of Wisconsin–Madison, Madison, WI
53706, USA  A. Khatee Zathul  Dept. of Physics and Wisconsin IceCube Particle
Astrophysics Center, University of Wisconsin–Madison, Madison, WI 53706, USA
A. Kheirandish Department of Physics & Astronomy, University of Nevada, Las
Vegas, NV, 89154, USA  Nevada Center for Astrophysics, University of Nevada,
Las Vegas, NV 89154, USA  K. Kin  Dept. of Physics and The International
Center for Hadron Astrophysics, Chiba University, Chiba 263-8522, Japan  J.
Kiryluk Dept. of Physics and Astronomy, Stony Brook University, Stony Brook,
NY 11794-3800, USA  S. R. Klein Dept. of Physics, University of California,
Berkeley, CA 94720, USA  Lawrence Berkeley National Laboratory, Berkeley, CA
94720, USA  A. Kochocki Dept. of Physics and Astronomy, Michigan State
University, East Lansing, MI 48824, USA  R. Koirala Bartol Research Institute
and Dept. of Physics and Astronomy, University of Delaware, Newark, DE 19716,
USA  H. Kolanoski Institut für Physik, Humboldt-Universität zu Berlin, D-12489
Berlin, Germany  T. Kontrimas Physik-department, Technische Universität
München, D-85748 Garching, Germany  L. Köpke  Institute of Physics, University
of Mainz, Staudinger Weg 7, D-55099 Mainz, Germany  C. Kopper Dept. of Physics
and Astronomy, Michigan State University, East Lansing, MI 48824, USA  D. J.
Koskinen Niels Bohr Institute, University of Copenhagen, DK-2100 Copenhagen,
Denmark  P. Koundal Karlsruhe Institute of Technology, Institute for
Astroparticle Physics, D-76021 Karlsruhe, Germany  M. Kovacevich Dept. of
Physics, Drexel University, 3141 Chestnut Street, Philadelphia, PA 19104, USA
M. Kowalski Institut für Physik, Humboldt-Universität zu Berlin, D-12489
Berlin, Germany  Deutsches Elektronen-Synchrotron DESY, Platanenallee 6, 15738
Zeuthen, Germany  T. Kozynets  Niels Bohr Institute, University of Copenhagen,
DK-2100 Copenhagen, Denmark  K. Kruiswijk  Centre for Cosmology, Particle
Physics and Phenomenology - CP3, Université catholique de Louvain, Louvain-la-
Neuve, Belgium  E. Krupczak  Dept. of Physics and Astronomy, Michigan State
University, East Lansing, MI 48824, USA  A. Kumar Deutsches Elektronen-
Synchrotron DESY, Platanenallee 6, 15738 Zeuthen, Germany  E. Kun  Fakultät
für Physik & Astronomie, Ruhr-Universität Bochum, D-44780 Bochum, Germany  N.
Kurahashi Dept. of Physics, Drexel University, 3141 Chestnut Street,
Philadelphia, PA 19104, USA  N. Lad  Deutsches Elektronen-Synchrotron DESY,
Platanenallee 6, 15738 Zeuthen, Germany  C. Lagunas Gualda Deutsches
Elektronen-Synchrotron DESY, Platanenallee 6, 15738 Zeuthen, Germany  M.
Lamoureux Centre for Cosmology, Particle Physics and Phenomenology - CP3,
Université catholique de Louvain, Louvain-la-Neuve, Belgium  M. J. Larson
Dept. of Physics, University of Maryland, College Park, MD 20742, USA  F.
Lauber Dept. of Physics, University of Wuppertal, D-42119 Wuppertal, Germany
J. P. Lazar Department of Physics and Laboratory for Particle Physics and
Cosmology, Harvard University, Cambridge, MA 02138, USA  Dept. of Physics and
Wisconsin IceCube Particle Astrophysics Center, University of
Wisconsin–Madison, Madison, WI 53706, USA  J. W. Lee Dept. of Physics,
Sungkyunkwan University, Suwon 16419, Korea  K. Leonard DeHolton Dept. of
Astronomy and Astrophysics, Pennsylvania State University, University Park, PA
16802, USA  Dept. of Physics, Pennsylvania State University, University Park,
PA 16802, USA  A. Leszczyńska Bartol Research Institute and Dept. of Physics
and Astronomy, University of Delaware, Newark, DE 19716, USA  M. Lincetto
Fakultät für Physik & Astronomie, Ruhr-Universität Bochum, D-44780 Bochum,
Germany  Q. R. Liu Dept. of Physics and Wisconsin IceCube Particle
Astrophysics Center, University of Wisconsin–Madison, Madison, WI 53706, USA
M. Liubarska  Dept. of Physics, University of Alberta, Edmonton, Alberta,
Canada T6G 2E1  E. Lohfink  Institute of Physics, University of Mainz,
Staudinger Weg 7, D-55099 Mainz, Germany  C. Love  Dept. of Physics, Drexel
University, 3141 Chestnut Street, Philadelphia, PA 19104, USA  C. J. Lozano
Mariscal  Institut für Kernphysik, Westfälische Wilhelms-Universität Münster,
D-48149 Münster, Germany  L. Lu Dept. of Physics and Wisconsin IceCube
Particle Astrophysics Center, University of Wisconsin–Madison, Madison, WI
53706, USA  F. Lucarelli Département de physique nucléaire et corpusculaire,
Université de Genève, CH-1211 Genève, Switzerland  A. Ludwig Department of
Physics and Astronomy, UCLA, Los Angeles, CA 90095, USA  W. Luszczak Dept. of
Astronomy, Ohio State University, Columbus, OH 43210, USA  Dept. of Physics
and Center for Cosmology and Astro-Particle Physics, Ohio State University,
Columbus, OH 43210, USA  Y. Lyu Dept. of Physics, University of California,
Berkeley, CA 94720, USA  Lawrence Berkeley National Laboratory, Berkeley, CA
94720, USA  W. Y. Ma Deutsches Elektronen-Synchrotron DESY, Platanenallee 6,
15738 Zeuthen, Germany  J. Madsen Dept. of Physics and Wisconsin IceCube
Particle Astrophysics Center, University of Wisconsin–Madison, Madison, WI
53706, USA  K. B. M. Mahn  Dept. of Physics and Astronomy, Michigan State
University, East Lansing, MI 48824, USA  Y. Makino  Dept. of Physics and
Wisconsin IceCube Particle Astrophysics Center, University of
Wisconsin–Madison, Madison, WI 53706, USA  S. Mancina  Dept. of Physics and
Wisconsin IceCube Particle Astrophysics Center, University of
Wisconsin–Madison, Madison, WI 53706, USA  Dipartimento di Fisica e Astronomia
Galileo Galilei, Università Degli Studi di Padova, 35122 Padova PD, Italy  W.
Marie Sainte  Dept. of Physics and Wisconsin IceCube Particle Astrophysics
Center, University of Wisconsin–Madison, Madison, WI 53706, USA  I. C. Mariş
Université Libre de Bruxelles, Science Faculty CP230, B-1050 Brussels, Belgium
S. Marka  Columbia Astrophysics and Nevis Laboratories, Columbia University,
New York, NY 10027, USA  Z. Marka  Columbia Astrophysics and Nevis
Laboratories, Columbia University, New York, NY 10027, USA  M. Marsee  Dept.
of Physics and Astronomy, University of Alabama, Tuscaloosa, AL 35487, USA  I.
Martinez-Soler  Department of Physics and Laboratory for Particle Physics and
Cosmology, Harvard University, Cambridge, MA 02138, USA  R. Maruyama Dept. of
Physics, Yale University, New Haven, CT 06520, USA  F. Mayhew  Dept. of
Physics and Astronomy, Michigan State University, East Lansing, MI 48824, USA
T. McElroy  Dept. of Physics, University of Alberta, Edmonton, Alberta, Canada
T6G 2E1  F. McNally Department of Physics, Mercer University, Macon, GA
31207-0001, USA  J. V. Mead  Niels Bohr Institute, University of Copenhagen,
DK-2100 Copenhagen, Denmark  K. Meagher Dept. of Physics and Wisconsin IceCube
Particle Astrophysics Center, University of Wisconsin–Madison, Madison, WI
53706, USA  S. Mechbal  Deutsches Elektronen-Synchrotron DESY, Platanenallee
6, 15738 Zeuthen, Germany  A. Medina  Dept. of Physics and Center for
Cosmology and Astro-Particle Physics, Ohio State University, Columbus, OH
43210, USA  M. Meier Dept. of Physics and The International Center for Hadron
Astrophysics, Chiba University, Chiba 263-8522, Japan  S. Meighen-Berger
Physik-department, Technische Universität München, D-85748 Garching, Germany
Y. Merckx  Vrije Universiteit Brussel (VUB), Dienst ELEM, B-1050 Brussels,
Belgium  L. Merten  Fakultät für Physik & Astronomie, Ruhr-Universität Bochum,
D-44780 Bochum, Germany  J. Micallef  Dept. of Physics and Astronomy, Michigan
State University, East Lansing, MI 48824, USA  D. Mockler  Université Libre de
Bruxelles, Science Faculty CP230, B-1050 Brussels, Belgium  T. Montaruli
Département de physique nucléaire et corpusculaire, Université de Genève,
CH-1211 Genève, Switzerland  R. W. Moore Dept. of Physics, University of
Alberta, Edmonton, Alberta, Canada T6G 2E1  Y. Morii  Dept. of Physics and The
International Center for Hadron Astrophysics, Chiba University, Chiba
263-8522, Japan  R. Morse  Dept. of Physics and Wisconsin IceCube Particle
Astrophysics Center, University of Wisconsin–Madison, Madison, WI 53706, USA
M. Moulai Dept. of Physics and Wisconsin IceCube Particle Astrophysics Center,
University of Wisconsin–Madison, Madison, WI 53706, USA  T. Mukherjee
Karlsruhe Institute of Technology, Institute for Astroparticle Physics,
D-76021 Karlsruhe, Germany  R. Naab Deutsches Elektronen-Synchrotron DESY,
Platanenallee 6, 15738 Zeuthen, Germany  R. Nagai Dept. of Physics and The
International Center for Hadron Astrophysics, Chiba University, Chiba
263-8522, Japan  M. Nakos  Dept. of Physics and Wisconsin IceCube Particle
Astrophysics Center, University of Wisconsin–Madison, Madison, WI 53706, USA
U. Naumann  Dept. of Physics, University of Wuppertal, D-42119 Wuppertal,
Germany  J. Necker Deutsches Elektronen-Synchrotron DESY, Platanenallee 6,
15738 Zeuthen, Germany  M. Neumann  Institut für Kernphysik, Westfälische
Wilhelms-Universität Münster, D-48149 Münster, Germany  H. Niederhausen Dept.
of Physics and Astronomy, Michigan State University, East Lansing, MI 48824,
USA  M. U. Nisa Dept. of Physics and Astronomy, Michigan State University,
East Lansing, MI 48824, USA  A. Noell  III. Physikalisches Institut, RWTH
Aachen University, D-52056 Aachen, Germany  S. C. Nowicki  Dept. of Physics
and Astronomy, Michigan State University, East Lansing, MI 48824, USA  A.
Obertacke Pollmann Dept. of Physics, University of Wuppertal, D-42119
Wuppertal, Germany  V. O’Dell  Dept. of Physics and Wisconsin IceCube Particle
Astrophysics Center, University of Wisconsin–Madison, Madison, WI 53706, USA
M. Oehler  Karlsruhe Institute of Technology, Institute for Astroparticle
Physics, D-76021 Karlsruhe, Germany  B. Oeyen Dept. of Physics and Astronomy,
University of Gent, B-9000 Gent, Belgium  A. Olivas  Dept. of Physics,
University of Maryland, College Park, MD 20742, USA  R. Orsoe  Physik-
department, Technische Universität München, D-85748 Garching, Germany  J.
Osborn  Dept. of Physics and Wisconsin IceCube Particle Astrophysics Center,
University of Wisconsin–Madison, Madison, WI 53706, USA  E. O’Sullivan Dept.
of Physics and Astronomy, Uppsala University, Box 516, S-75120 Uppsala, Sweden
H. Pandya Bartol Research Institute and Dept. of Physics and Astronomy,
University of Delaware, Newark, DE 19716, USA  N. Park Dept. of Physics,
Engineering Physics, and Astronomy, Queen’s University, Kingston, ON K7L 3N6,
Canada  G. K. Parker  Dept. of Physics, University of Texas at Arlington, 502
Yates St., Science Hall Rm 108, Box 19059, Arlington, TX 76019, USA  E. N.
Paudel Bartol Research Institute and Dept. of Physics and Astronomy,
University of Delaware, Newark, DE 19716, USA  L. Paul  Department of Physics,
Marquette University, Milwaukee, WI, 53201, USA  C. Pérez de los Heros Dept.
of Physics and Astronomy, Uppsala University, Box 516, S-75120 Uppsala, Sweden
J. Peterson  Dept. of Physics and Wisconsin IceCube Particle Astrophysics
Center, University of Wisconsin–Madison, Madison, WI 53706, USA  S. Philippen
III. Physikalisches Institut, RWTH Aachen University, D-52056 Aachen, Germany
S. Pieper  Dept. of Physics, University of Wuppertal, D-42119 Wuppertal,
Germany  A. Pizzuto Dept. of Physics and Wisconsin IceCube Particle
Astrophysics Center, University of Wisconsin–Madison, Madison, WI 53706, USA
M. Plum Physics Department, South Dakota School of Mines and Technology, Rapid
City, SD 57701, USA  Y. Popovych  Institute of Physics, University of Mainz,
Staudinger Weg 7, D-55099 Mainz, Germany  M. Prado Rodriguez  Dept. of Physics
and Wisconsin IceCube Particle Astrophysics Center, University of
Wisconsin–Madison, Madison, WI 53706, USA  B. Pries Dept. of Physics and
Astronomy, Michigan State University, East Lansing, MI 48824, USA  R. Procter-
Murphy  Dept. of Physics, University of Maryland, College Park, MD 20742, USA
G. T. Przybylski  Lawrence Berkeley National Laboratory, Berkeley, CA 94720,
USA  C. Raab Université Libre de Bruxelles, Science Faculty CP230, B-1050
Brussels, Belgium  J. Rack-Helleis  Institute of Physics, University of Mainz,
Staudinger Weg 7, D-55099 Mainz, Germany  K. Rawlins  Dept. of Physics and
Astronomy, University of Alaska Anchorage, 3211 Providence Dr., Anchorage, AK
99508, USA  Z. Rechav  Dept. of Physics and Wisconsin IceCube Particle
Astrophysics Center, University of Wisconsin–Madison, Madison, WI 53706, USA
A. Rehman Bartol Research Institute and Dept. of Physics and Astronomy,
University of Delaware, Newark, DE 19716, USA  P. Reichherzer  Fakultät für
Physik & Astronomie, Ruhr-Universität Bochum, D-44780 Bochum, Germany  G.
Renzi  Université Libre de Bruxelles, Science Faculty CP230, B-1050 Brussels,
Belgium  E. Resconi Physik-department, Technische Universität München, D-85748
Garching, Germany  S. Reusch  Deutsches Elektronen-Synchrotron DESY,
Platanenallee 6, 15738 Zeuthen, Germany  W. Rhode Dept. of Physics, TU
Dortmund University, D-44221 Dortmund, Germany  M. Richman  Dept. of Physics,
Drexel University, 3141 Chestnut Street, Philadelphia, PA 19104, USA  B.
Riedel Dept. of Physics and Wisconsin IceCube Particle Astrophysics Center,
University of Wisconsin–Madison, Madison, WI 53706, USA  E. J. Roberts
Department of Physics, University of Adelaide, Adelaide, 5005, Australia  S.
Robertson  Dept. of Physics, University of California, Berkeley, CA 94720, USA
Lawrence Berkeley National Laboratory, Berkeley, CA 94720, USA  S. Rodan
Dept. of Physics, Sungkyunkwan University, Suwon 16419, Korea  G. Roellinghoff
Dept. of Physics, Sungkyunkwan University, Suwon 16419, Korea  M. Rongen
Institute of Physics, University of Mainz, Staudinger Weg 7, D-55099 Mainz,
Germany  C. Rott Department of Physics and Astronomy, University of Utah, Salt
Lake City, UT 84112, USA  Dept. of Physics, Sungkyunkwan University, Suwon
16419, Korea  T. Ruhe  Dept. of Physics, TU Dortmund University, D-44221
Dortmund, Germany  L. Ruohan  Physik-department, Technische Universität
München, D-85748 Garching, Germany  D. Ryckbosch  Dept. of Physics and
Astronomy, University of Gent, B-9000 Gent, Belgium  S.Athanasiadou  Deutsches
Elektronen-Synchrotron DESY, Platanenallee 6, 15738 Zeuthen, Germany  I. Safa
Department of Physics and Laboratory for Particle Physics and Cosmology,
Harvard University, Cambridge, MA 02138, USA  Dept. of Physics and Wisconsin
IceCube Particle Astrophysics Center, University of Wisconsin–Madison,
Madison, WI 53706, USA  J. Saffer  Karlsruhe Institute of Technology,
Institute of Experimental Particle Physics, D-76021 Karlsruhe, Germany  D.
Salazar-Gallegos Dept. of Physics and Astronomy, Michigan State University,
East Lansing, MI 48824, USA  P. Sampathkumar  Karlsruhe Institute of
Technology, Institute for Astroparticle Physics, D-76021 Karlsruhe, Germany
S. E. Sanchez Herrera  Dept. of Physics and Astronomy, Michigan State
University, East Lansing, MI 48824, USA  A. Sandrock Dept. of Physics, TU
Dortmund University, D-44221 Dortmund, Germany  M. Santander Dept. of Physics
and Astronomy, University of Alabama, Tuscaloosa, AL 35487, USA  S. Sarkar
Dept. of Physics, University of Alberta, Edmonton, Alberta, Canada T6G 2E1  S.
Sarkar Dept. of Physics, University of Oxford, Parks Road, Oxford OX1 3PU, UK
J. Savelberg  III. Physikalisches Institut, RWTH Aachen University, D-52056
Aachen, Germany  P. Savina  Dept. of Physics and Wisconsin IceCube Particle
Astrophysics Center, University of Wisconsin–Madison, Madison, WI 53706, USA
M. Schaufel  III. Physikalisches Institut, RWTH Aachen University, D-52056
Aachen, Germany  H. Schieler  Karlsruhe Institute of Technology, Institute for
Astroparticle Physics, D-76021 Karlsruhe, Germany  S. Schindler Erlangen
Centre for Astroparticle Physics, Friedrich-Alexander-Universität Erlangen-
Nürnberg, D-91058 Erlangen, Germany  B. Schlüter  Institut für Kernphysik,
Westfälische Wilhelms-Universität Münster, D-48149 Münster, Germany  T.
Schmidt  Dept. of Physics, University of Maryland, College Park, MD 20742, USA
J. Schneider Erlangen Centre for Astroparticle Physics, Friedrich-Alexander-
Universität Erlangen-Nürnberg, D-91058 Erlangen, Germany  F. G. Schröder
Karlsruhe Institute of Technology, Institute for Astroparticle Physics,
D-76021 Karlsruhe, Germany  Bartol Research Institute and Dept. of Physics and
Astronomy, University of Delaware, Newark, DE 19716, USA  L. Schumacher
Physik-department, Technische Universität München, D-85748 Garching, Germany
G. Schwefer  III. Physikalisches Institut, RWTH Aachen University, D-52056
Aachen, Germany  S. Sclafani Dept. of Physics, Drexel University, 3141
Chestnut Street, Philadelphia, PA 19104, USA  D. Seckel  Bartol Research
Institute and Dept. of Physics and Astronomy, University of Delaware, Newark,
DE 19716, USA  S. Seunarine  Dept. of Physics, University of Wisconsin, River
Falls, WI 54022, USA  A. Sharma  Dept. of Physics and Astronomy, Uppsala
University, Box 516, S-75120 Uppsala, Sweden  S. Shefali  Karlsruhe Institute
of Technology, Institute of Experimental Particle Physics, D-76021 Karlsruhe,
Germany  N. Shimizu  Dept. of Physics and The International Center for Hadron
Astrophysics, Chiba University, Chiba 263-8522, Japan  M. Silva Dept. of
Physics and Wisconsin IceCube Particle Astrophysics Center, University of
Wisconsin–Madison, Madison, WI 53706, USA  B. Skrzypek  Department of Physics
and Laboratory for Particle Physics and Cosmology, Harvard University,
Cambridge, MA 02138, USA  B. Smithers Dept. of Physics, University of Texas at
Arlington, 502 Yates St., Science Hall Rm 108, Box 19059, Arlington, TX 76019,
USA  R. Snihur  Dept. of Physics and Wisconsin IceCube Particle Astrophysics
Center, University of Wisconsin–Madison, Madison, WI 53706, USA  J.
Soedingrekso  Dept. of Physics, TU Dortmund University, D-44221 Dortmund,
Germany  A. Søgaard  Niels Bohr Institute, University of Copenhagen, DK-2100
Copenhagen, Denmark  D. Soldin Karlsruhe Institute of Technology, Institute of
Experimental Particle Physics, D-76021 Karlsruhe, Germany  G. Sommani Fakultät
für Physik & Astronomie, Ruhr-Universität Bochum, D-44780 Bochum, Germany  C.
Spannfellner  Physik-department, Technische Universität München, D-85748
Garching, Germany  G. M. Spiczak Dept. of Physics, University of Wisconsin,
River Falls, WI 54022, USA  C. Spiering Deutsches Elektronen-Synchrotron DESY,
Platanenallee 6, 15738 Zeuthen, Germany  M. Stamatikos  Dept. of Physics and
Center for Cosmology and Astro-Particle Physics, Ohio State University,
Columbus, OH 43210, USA  T. Stanev  Bartol Research Institute and Dept. of
Physics and Astronomy, University of Delaware, Newark, DE 19716, USA  R. Stein
Deutsches Elektronen-Synchrotron DESY, Platanenallee 6, 15738 Zeuthen, Germany
T. Stezelberger Lawrence Berkeley National Laboratory, Berkeley, CA 94720, USA
T. Stürwald  Dept. of Physics, University of Wuppertal, D-42119 Wuppertal,
Germany  T. Stuttard Niels Bohr Institute, University of Copenhagen, DK-2100
Copenhagen, Denmark  G. W. Sullivan Dept. of Physics, University of Maryland,
College Park, MD 20742, USA  I. Taboada School of Physics and Center for
Relativistic Astrophysics, Georgia Institute of Technology, Atlanta, GA 30332,
USA  S. Ter-Antonyan Dept. of Physics, Southern University, Baton Rouge, LA
70813, USA  W. G. Thompson Department of Physics and Laboratory for Particle
Physics and Cosmology, Harvard University, Cambridge, MA 02138, USA  J.
Thwaites  Dept. of Physics and Wisconsin IceCube Particle Astrophysics Center,
University of Wisconsin–Madison, Madison, WI 53706, USA  S. Tilav  Bartol
Research Institute and Dept. of Physics and Astronomy, University of Delaware,
Newark, DE 19716, USA  K. Tollefson Dept. of Physics and Astronomy, Michigan
State University, East Lansing, MI 48824, USA  C. Tönnis  Dept. of Physics,
Sungkyunkwan University, Suwon 16419, Korea  S. Toscano Université Libre de
Bruxelles, Science Faculty CP230, B-1050 Brussels, Belgium  D. Tosi  Dept. of
Physics and Wisconsin IceCube Particle Astrophysics Center, University of
Wisconsin–Madison, Madison, WI 53706, USA  A. Trettin  Deutsches Elektronen-
Synchrotron DESY, Platanenallee 6, 15738 Zeuthen, Germany  C. F. Tung School
of Physics and Center for Relativistic Astrophysics, Georgia Institute of
Technology, Atlanta, GA 30332, USA  R. Turcotte  Karlsruhe Institute of
Technology, Institute for Astroparticle Physics, D-76021 Karlsruhe, Germany
J. P. Twagirayezu  Dept. of Physics and Astronomy, Michigan State University,
East Lansing, MI 48824, USA  B. Ty  Dept. of Physics and Wisconsin IceCube
Particle Astrophysics Center, University of Wisconsin–Madison, Madison, WI
53706, USA  M. A. Unland Elorrieta Institut für Kernphysik, Westfälische
Wilhelms-Universität Münster, D-48149 Münster, Germany  A. K. Upadhyay  also
at Institute of Physics, Sachivalaya Marg, Sainik School Post, Bhubaneswar
751005, India  Dept. of Physics and Wisconsin IceCube Particle Astrophysics
Center, University of Wisconsin–Madison, Madison, WI 53706, USA  K. Upshaw
Dept. of Physics, Southern University, Baton Rouge, LA 70813, USA  N.
Valtonen-Mattila Dept. of Physics and Astronomy, Uppsala University, Box 516,
S-75120 Uppsala, Sweden  J. Vandenbroucke Dept. of Physics and Wisconsin
IceCube Particle Astrophysics Center, University of Wisconsin–Madison,
Madison, WI 53706, USA  N. van Eijndhoven Vrije Universiteit Brussel (VUB),
Dienst ELEM, B-1050 Brussels, Belgium  D. Vannerom  Dept. of Physics,
Massachusetts Institute of Technology, Cambridge, MA 02139, USA  J. van Santen
Deutsches Elektronen-Synchrotron DESY, Platanenallee 6, 15738 Zeuthen, Germany
J. Vara  Institut für Kernphysik, Westfälische Wilhelms-Universität Münster,
D-48149 Münster, Germany  J. Veitch-Michaelis  Dept. of Physics and Wisconsin
IceCube Particle Astrophysics Center, University of Wisconsin–Madison,
Madison, WI 53706, USA  M. Venugopal  Karlsruhe Institute of Technology,
Institute for Astroparticle Physics, D-76021 Karlsruhe, Germany  S. Verpoest
Dept. of Physics and Astronomy, University of Gent, B-9000 Gent, Belgium  D.
Veske  Columbia Astrophysics and Nevis Laboratories, Columbia University, New
York, NY 10027, USA  C. Walck  Oskar Klein Centre and Dept. of Physics,
Stockholm University, SE-10691 Stockholm, Sweden  T. B. Watson Dept. of
Physics, University of Texas at Arlington, 502 Yates St., Science Hall Rm 108,
Box 19059, Arlington, TX 76019, USA  C. Weaver Dept. of Physics and Astronomy,
Michigan State University, East Lansing, MI 48824, USA  P. Weigel  Dept. of
Physics, Massachusetts Institute of Technology, Cambridge, MA 02139, USA  A.
Weindl  Karlsruhe Institute of Technology, Institute for Astroparticle
Physics, D-76021 Karlsruhe, Germany  J. Weldert  Dept. of Astronomy and
Astrophysics, Pennsylvania State University, University Park, PA 16802, USA
Dept. of Physics, Pennsylvania State University, University Park, PA 16802,
USA  C. Wendt Dept. of Physics and Wisconsin IceCube Particle Astrophysics
Center, University of Wisconsin–Madison, Madison, WI 53706, USA  J. Werthebach
Dept. of Physics, TU Dortmund University, D-44221 Dortmund, Germany  M.
Weyrauch  Karlsruhe Institute of Technology, Institute for Astroparticle
Physics, D-76021 Karlsruhe, Germany  N. Whitehorn Dept. of Physics and
Astronomy, Michigan State University, East Lansing, MI 48824, USA  Department
of Physics and Astronomy, UCLA, Los Angeles, CA 90095, USA  C. H. Wiebusch
III. Physikalisches Institut, RWTH Aachen University, D-52056 Aachen, Germany
N. Willey  Dept. of Physics and Astronomy, Michigan State University, East
Lansing, MI 48824, USA  D. R. Williams  Dept. of Physics and Astronomy,
University of Alabama, Tuscaloosa, AL 35487, USA  M. Wolf Physik-department,
Technische Universität München, D-85748 Garching, Germany  G. Wrede  Erlangen
Centre for Astroparticle Physics, Friedrich-Alexander-Universität Erlangen-
Nürnberg, D-91058 Erlangen, Germany  J. Wulff  Fakultät für Physik &
Astronomie, Ruhr-Universität Bochum, D-44780 Bochum, Germany  X. W. Xu  Dept.
of Physics, Southern University, Baton Rouge, LA 70813, USA  J. P. Yanez
Dept. of Physics, University of Alberta, Edmonton, Alberta, Canada T6G 2E1  E.
Yildizci  Dept. of Physics and Wisconsin IceCube Particle Astrophysics Center,
University of Wisconsin–Madison, Madison, WI 53706, USA  S. Yoshida Dept. of
Physics and The International Center for Hadron Astrophysics, Chiba
University, Chiba 263-8522, Japan  F. Yu  Department of Physics and Laboratory
for Particle Physics and Cosmology, Harvard University, Cambridge, MA 02138,
USA  S. Yu  Dept. of Physics and Astronomy, Michigan State University, East
Lansing, MI 48824, USA  T. Yuan Dept. of Physics and Wisconsin IceCube
Particle Astrophysics Center, University of Wisconsin–Madison, Madison, WI
53706, USA  Z. Zhang  Dept. of Physics and Astronomy, Stony Brook University,
Stony Brook, NY 11794-3800, USA  P. Zhelnin  Department of Physics and
Laboratory for Particle Physics and Cosmology, Harvard University, Cambridge,
MA 02138, USA

###### 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, and 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. The overall deviation of all tested scenarios from the
background expectation yields a p-value of $93\%$ which is fully compatible
with background. The derived upper limits on the total energy emitted in
neutrinos are $1.7\times 10^{48}$ erg for stripped-envelope supernovae,
$2.8\times 10^{48}$ erg for type IIP, and $1.3\times 10^{49}$ erg for type IIn
SNe, the latter disfavouring 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 $10^{3}-10^{5}\,\mathrm{GeV}$,
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.

neutrino astronomy, IceCube, core-collapse supernovae

††journal: ApJ Letters††facilities: HST(STIS), Swift(XRT and UVOT), AAVSO,
CTIO:1.3m, CTIO:1.5m,CXO††software: flarestack (Stein et al., 2022a)

##  1 Introduction

IceCube has detected a diffuse flux of high-energy astrophysical neutrinos
(Aartsen et al., 2015, 2013). The majority of the high-energy neutrinos
follows an isotropic distribution which suggests an extra-galactic origin. The
active galaxy NGC 1068 was recently reported to be the first extra-galactic
point-source of high-energy neutrinos beyond the $4\sigma$ level (IceCube
Collaboration et al., 2022). While there is evidence that gamma-ray blazars
and tidal disruption events (TDEs) produce high-energy neutrinos (Aartsen et
al., 2018a, b; Stein et al., 2021; Reusch et al., 2022), the rate of observed
coincidences constrain the overall diffuse flux contribution of resolved
gamma-ray blazars and tidal disruption events to no more than $30\%$ (Aartsen
et al., 2017a) and $26\%$ (Stein, 2019) respectively, leaving the majority of
the diffuse flux unexplained.

In general, high-energy neutrinos are created through interactions of high-
energy protons with ambient matter or photon fields. Charged and neutral pions
produced in those interactions decay to neutrinos and gamma rays,
respectively. While gamma rays can also be produced in leptonic processes such
as Inverse Compton scattering, neutrinos are considered to be the clear
signature for hadronic interactions, and thus also cosmic-ray acceleration.

Several source classes have been proposed as candidate neutrino (and cosmic-
ray) sources. Among the most promising are Active Galactic Nuclei (AGN),
Gamma-Ray Bursts (GRBs) and Supernovae (SNe) – see Kurahashi et al. (2022) for
a recent review. While gamma-bright GRBs are strongly disfavored as the main
contributor to the measured diffuse neutrino flux (Aartsen et al., 2017b), a
large population of nearby low-luminosity bursts could still contribute
significantly. The discovery of a connection between GRBs and type Ic-BL SNe
implies that (mildly) relativistic jets should also exist in a fraction of
core-collapse SNe (Senno et al., 2016; Ando & Beacom, 2005; Razzaque et al.,
2004; Denton & Tamborra, 2018), where such jets might be choked inside the
envelope of the star. In this scenario, the gamma rays would be absorbed but
the neutrinos could still escape. A short neutrino burst ($\sim 100$ s) would
be expected, in coincidence with the explosion time of the SNe (Senno et al.,
2016).

Another possibility for producing high-energy neutrinos in core-collapse
supernovae (CCSN) is through interactions of the SN ejecta with a dense
circumstellar medium (CSM). Strong stellar winds in the star’s late evolution
stages or pre-outburst could produce a sufficiently-dense CSM (Ofek et al.,
2013; Strotjohann et al., 2021). When the supernova shock front reaches this
dense medium, efficient acceleration of charged particles on timescales
ranging from a few tens of seconds to $\sim 1000$ days may occur (Murase et
al., 2011; Zirakashvili & Ptuskin, 2016; Sarmah et al., 2022). CSM
interactions can be revealed through the detection of a combination of narrow
and broad emission lines (as observed in type IIn SNe). The narrow component
of the spectral lines is produced by circumstellar gas, which is ionised as
the shock breaks out of the star. The intermediate and broad components are
produced by shocked, high-velocity SN ejecta, arising as a result of the
collision of the ejecta with circumstellar gas. Another indication might be a
long plateau in the SN light curve (as seen in Type IIP SNe), which could be
partly powered by SN shock breakout interaction with dense CSM (Moriya et al.,
2011, 2012). Some IIP SNe show direct observational evidence for interactions
(Mauerhan et al., 2013; Faran et al., 2014; Yaron et al., 2017; Nakaoka et
al., 2018). Pitik et al. (2022) found the high-energy neutrino IC200530A in
spatial coincidence with the optical transient AT2019fdr, which they interpret
as a Type IIn superluminous supernova.

Optical follow-up campaigns of IceCube high-energy neutrino alerts (Stein et
al., 2022b; Necker et al., 2022) are close to constraining the brightest
observed superluminous supernovae.

Here, for the first time, we probe different SN classes as potential neutrino
sources and calculate their possible contribution to the observed diffuse
neutrino flux. To search for cross-correlation between neutrinos and optically
observed SNe, we utilize data recorded by the IceCube Neutrino Observatory.

This paper is organized as follows: Section 2 describes the relevant data
sets, followed by a discussion of the analysis methods in Section 3 and the
presentation of the results in Section 4. Section 5 presents the constraints
on the contribution of CCSNe to the diffuse neutrino flux. Section 6
summarizes the paper. Upper limits on the total energy released in neutrinos
from individual SNe can be found in the Appendix C.

##  2 The Data

IceCube is a cubic-kilometer-sized neutrino detector, located in the
transparent ice of the 2.8 km-thick glacier covering the bedrock at the
geographical South Pole (Aartsen et al., 2017a). Neutrino-nucleon interactions
in the ice are detected indirectly, via Cherenkov light emission from
secondary particles, by 5160 photomultiplier tubes. While charged-current
interactions of muon neutrinos produce track-like signatures with sub-degree
angular resolution, both charged-current interactions of electron and tau
neutrinos, and neutral-current interactions, have angular resolutions of
several degrees. This analysis utilizes a selection of seven years of IceCube
muon-track data that was optimised for point-source searches (Aartsen et al.,
2017b), with roughly 700,000 events from years 2008 to 2014.

The CCSN catalog for this analysis was compiled using publicly available
records of optical detections of SNe. The primary sources were the WiseREP SN
catalog (Yaron & Gal-Yam, 2012) and the OpenSupernovaCatalog (Guillochon et
al., 2017). In total, the compiled source sample contains 339 SN type IIn, 198
SN type IIP, 503 type Ib/c and type IIb SNe. The latter are referred to as
stripped-envelope supernovae. Both type IIn and type IIP SN are candidates for
CSM interaction, while stripped-envelope supernovae might host choked jets. In
Figure 1 the distance distribution of the two sub-samples is shown. Note that
while we did include many supernovae in the analysis, we list only those of a
smaller subsample in Tables A, A and A as explained below.

Figure 1: Distance distribution of CSM SN sample and the stripped-envelope SN
sample. The decrease at large distance is a result of limited detection
sensitivity and a selection bias towards brighter objects, which are easier to
classify spectroscopically.

The distance was taken from the previously-cited catalogs. For cases in which
entries were missing in the catalogs, the distances were estimated using
redshift measurements. The $\Lambda$CDM model, with cosmological parameters
measured by Planck (Ade et al., 2016), were used to convert from redshift to
luminosity distance. We have assumed a peculiar motion of
$300\,\mathrm{km\,s^{-1}}$, which also provides a lower distance limit for SNe
with very small redshifts. SNe with neither distance nor redshift measurements
were excluded from the catalog. The distance distribution peaks at about
$100\,\mathrm{Mpc}$, as can be seen in Fig. 1.

##  3 Analysis Method

To find an excess of neutrinos from the given SN positions and times, a time
dependent point source likelihood method (Braun et al., 2010) is used. The
likelihood function is given by

$\mathcal{L}=\prod_{i=1}^{N}\left(\frac{n_{\text{s}}}{N}\mathcal{S}(\nu_{i})+\left(1-\frac{n_{\text{s}}}{N}\right)\mathcal{B}(\nu_{i})\right)$
(1)

where $N$ is the number of neutrino events, $\nu_{i}$ the $i$th neutrino and
$n_{\text{s}}$ is the number of signal events. $\mathcal{S}$ and $\mathcal{B}$
are signal and background probability distribution functions (PDFs). Each PDF
is a product of a spatial term $\mathcal{N}$, an energy term $\mathcal{E}$ and
a time term $\mathcal{T}$, which gives for the signal PDF:

$\mathcal{S}=\mathcal{N}_{\mathcal{S}}\times\mathcal{E}_{\mathcal{S}}(\gamma)\times\mathcal{T}_{\mathcal{S}}$
(2)

and similarly for the background PDF $\mathcal{B}$ (Braun et al., 2010). The
signal time PDF $\mathcal{T}_{\mathcal{S}}$ corresponds to the expected
neutrino flux as a function of time (light curve) and the background time PDF
$\mathcal{T}_{\mathcal{B}}$ assumes a constant background rate.

The energy term $\mathcal{E}$ describes the expected neutrino energy spectrum.
As the dataset is highly background-dominated 111For an astrophysical signal
component in the dataset with a spectral index of $\gamma=2.5$, we expect
$\mathcal{O}(10^{3})$ signal events and $\mathcal{O}(10^{5})$ atmospheric
background events, amounting to a signal contribution of $<1\%$ , we can
safely assume that the signal contribution is negligible. The background
energy proxy distribution is thus assumed to follow the distribution observed
in the data. The signal neutrino energy distribution is described as a power-
law function, $E^{-\gamma}$, where $\gamma$ is the spectral index. For similar
reasons, the background spatial PDF as a function of declination is chosen to
match the distribution of declinations found in data. We assume that the
background spatial PDF is uniform in right ascension, leading to
$\mathcal{N}_{\mathcal{B}}(\delta,\phi)=\frac{1}{2\pi}\times\mathcal{N}_{\mathcal{B},\text{dec}}(\delta)$
for source declination $\delta$ and right ascension $\phi$. The signal spatial
PDF, $\mathcal{N}_{\mathcal{S}}$, is assumed to follow a 2D-Gaussian
distribution.

The likelihood function is maximized with respect to $n_{\text{s}}$ and
$\gamma$. The best fitted value $n_{\text{s}}$ gives an estimate of the number
of signal-like events, i.e., those that are likely to originate from a given
SN.

In addition to probing the neutrino fluxes from single SNe, we combine the
signal of a sample of SNe with a stacking analysis. Such a source stacking is
implemented through a weighted sum of the signal PDFs $\mathcal{S}_{j}$ of
individual SNe $j$:

$\mathcal{S}=\sum_{j}w_{j}\mathcal{S}_{j}$ (3)

where the weights $w_{j}$ represent the expected signal strength of the
sources. In this analysis, the weights are assumed to be proportional to:

$\displaystyle w_{j}$
$\displaystyle\propto\underbrace{\frac{\Phi_{0}}{D_{\text{p}}^{2}}}_{\begin{subarray}{c}\text{Source}\\\
\text{Properties}\end{subarray}}\times\underbrace{\int_{t_{\text{start}}}^{t_{\text{end}}}\int_{E_{\text{min}}}^{E_{\text{max}}}\,L_{j}^{\nu}\,E^{-\gamma}\,A_{\mathrm{eff}}\,\mathrm{d}t\mathrm{d}E}_{\text{Time
Dependence}}$ (4)

with $\Phi_{0}$ as the intrinsic neutrino power of the sources, $D_{\text{p}}$
as the proper distance (Hogg, 1999) of the SN, $L_{j}^{\nu}(t)$ the estimated
neutrino light curve, $E^{-\gamma}$ the neutrino energy spectrum and
$A_{\mathrm{eff}}(t,\delta_{j},E)$ the effective area, the energy $E$ and the
declination of the source $\delta$. The effective area is time-dependent,
because the dataset covers several distinct phases of detector construction.
The weighting scheme assumes a standard candle ansatz, since we assume the
same $\Phi_{0}$ for each source. It is very sensitive to the estimated source
distances, which can have large uncertainties.

A more detailed investigation of the Supernova light curves could mitigate
these uncertainties but the optical lightcurves of the supernovae in our
catalogue are typically sparse and make detailed modeling complicated. Wrongly
estimated weights will impact the sensitivity of the analysis so for the first
time in an IceCube analysis we use a novel method of directly fitting the
weights $w_{j}$. Adding the flux per source as an additional free parameter to
the maximum likelihood removes the standard candle assumption and also the
dependence on the SN distance estimate, but requires a more advanced numerical
procedure to maximize the likelihood function. To test the power of this
method, we simulated five sources with random positions on the sky and
respective weights. We then perturbed the weights according to a log-normal
distribution and used them to compute the sensitivity of the standard, fixed-
weights likelihood. Comparing to this, we find an improvement of up to 40%
when using the fitting-weights likelihood. We applied this method in addition
to the traditional standard-candle one, yielding two separate results.

We define the test statistic (TS) by

$\lambda=2\times\log\left(\frac{\mathcal{L}(\hat{n}_{\text{s}},\hat{\gamma})}{\mathcal{L}(0)}\right)$
(5)

where $\mathcal{L}(\hat{n}_{\text{s}},\hat{\gamma})$ corresponds to the
maximum of the likelihood function and $\mathcal{L}(0)$ to the null
hypothesis, i.e., the case of neither spatial nor temporal correlation of
neutrinos and SNe (Braun et al., 2008, 2010). The TS distribution is estimated
by generating background-only datasets and maximizing the likelihood function
with respect to $n_{\text{s}}$ and $\gamma$. Repeating this procedure many
times gives a numerical estimate of the TS distribution. Given an experimental
outcome $\lambda_{\text{exp}}$ and the TS distribution $P(\lambda)$, the
p-value is computed as
$p=\int_{\lambda_{\text{exp}}}^{\infty}P(\lambda)\mathrm{d}\lambda$.

##  4 Constraints on supernova subclasses

In the following we present results for selected individual CCSNe, as well as
for different subclasses of CCSNe.

Stripped-envelope SNe, which might have choked jets, are expected to emit a
short burst of neutrinos in coincidence with the SN explosion time (Senno et
al., 2016). Motivated by theoretical uncertainties in the duration of the
expected neutrino emission, and even larger uncertainties in the SNe explosion
time due to sparse optical light curve data, we used a box function starting
at 20 days before and extending up to the first available optical data. This
ensures the inclusion of the explosion time for a typical SN even if the first
detection happened at peak time.

All SN types were tested with box function PDFs of length $100$, $300$ and
$1000$ days, starting at the first available optical data, since longer
neutrino emission would be expected under the scenario of CSM interaction. In
addition, for SNe IIn and IIP light curves were tested of the form:

$\mathcal{T}(t)\propto\left(1+\nicefrac{{t}}{{t_{\text{pp}}}}\right)^{-1}$ (6)

where values of $0.02$, $0.2$ and $2$ years were used for the characteristic
time scale constant $t_{\text{pp}}$, as proposed by Zirakashvili & Ptuskin
(2016).

We first applied the maximum likelihood method described above to a selection
of individual SNe, which were identified based on their expected relative
signal strength $w_{j}$ as promising. We did not find a statistically
significant excess for any of the selected sources.

The resulting upper limits on the total energy emitted in neutrinos between
$10^{2}\,\mathrm{GeV}$ and $10^{7}\,\mathrm{GeV}$, assuming an $E^{-2}$ power-
law spectrum, are presented in Appendix C. In the conversion from the number
of neutrino events to flux, the systemic uncertainty is estimated to be about
$11\%$, mainly arising from uncertainties in the optical properties of the ice
and detector effects (Coenders, 2016).

The individual upper limits range from $10^{49}$ to $6.5\times 10^{50}$
erg222Calculated by integrating over time., which corresponds to 1-65% of the
typical bolometric electromagnetic energy released in SNe. As the individual
stripped-envelope and IIP SNe are typically closer than the IIn, we generally
obtain more stringent limits for these objects.

In order to improve our sensitivity we performed a stacking analysis, looking
for a combined excess from a catalogue instead of individual sources. As
explained above we separate supernovae into types IIn, IIP and stripped-
envelope SNe. Note that we decided to treat the types IIn and IIP separately
because the presence of CSM interaction in IIP is less certain.

Each of the three sub-catalogs was split into two samples, a bright sample of
nearby sources, containing about $70\%$ of the expected signal, and a larger
sample, containing the remaining dimmer sources. The bright samples include
about 10 SN each, depending on the SN class and the model. The catalogues of
the bright samples are listed in Tables A, A and A. Testing both independent
samples allowed us to benefit from the better optical observations of the
nearby sources in the small sample, but also utilize the larger statistics in
the large sample. Because each source adds a free parameter in the likelihood
maximisation when fitting the weights, this was only feasible for the smaller
bright sample. This sample contains $\mathcal{O}(10)$ sources which is a
manageable amount of fit parameters. For the large sample the standard candle
ansatz was applied instead.

The p-values are given in Appendix B. The most significant pre-trial p-value
is $0.62\%$, and is found in the search for neutrinos from the large sample of
type IIP SNe in a 1000-day-long box-shaped light curve. This however
corresponds to a post-trial p-value of $19.5\%$, after accounting for the
multiple tested scenarios through simulated pseudo-experiments of the ensemble
of p-values, and is thus consistent with background expectations. If this
excess were due to astrophysical neutrinos, one would expect a corresponding
excess in the sample of nearby type IIP SNe, where we do not find such an
excess. The second smallest p-value of $6.3\%$ is found for the nearby type
IIn SNe in case of the fitted weights for the box-shaped lightcurve model. The
overall deviation of all tested scenarios from the background expectation
using a Kolmogorov-Smirnov-test leads to a p-value of $29\%$.

To be conservative we use the result from the fitting weights analysis in the
rest of the paper as it resulted in weaker upper limits on the total emitted
neutrino energy. Including systematic uncertainties, those are shown in Fig. 2
for both models of the neutrino light curve. These limits assume that SNe
within each category behave as neutrino standard candles.

Figure 2: Upper limits on total neutrino ($\nu_{\mu}+\bar{\nu}_{\mu}$) energy
assuming a box-like neutrino light curve (upper panel) and assuming a
$L_{\nu}\propto(1+\nicefrac{{t}}{{t_{\text{pp}}}})^{-1}$ neutrino light curve
as predicted by Zirakashvili & Ptuskin (2016). The energy ranges are the same
as indicated in Figure 3. The model predictions by Murase et al. (2011) and
Zirakashvili & Ptuskin (2016) are shown as red squares for comparison.

The stacking result provides us with stronger limits than individual source
limits. We find that SNe type IIn emit less than $1.3\times 10^{49}$ erg and
type IIP less than $2.4\times 10^{48}$ erg, while the strongest limits for
stripped-envelope SNe of $4.5\times 10^{48}$ erg are obtained from the ckoked-
jet scenario. If the longer box models that are associated with CSM
interaction are assumed, then the strongest limit becomes $2.7\times 10^{48}$
erg. In general, the box time window provides tighter constraints for CSM
interacting SNe compared to the specific light curve model by Zirakashvili &
Ptuskin (2016).

##  5 Diffuse Neutrino Flux

Using the limits on neutrino energy obtained in the stacking analysis (shown
in Fig. 2) we can estimate the maximal contribution from the entire
cosmological population of SNe to the measured diffuse neutrino flux (Aartsen
et al., 2015). Using the CCSNe rate by Strolger et al. (2015), $\rho(z)$, the
diffuse flux is computed following the procedure in Ahlers & Halzen (2014)
assuming a 1:1:1 ($\nu_{e}:\nu_{\mu}:\nu_{\tau}$) neutrino flavour ratio at
Earth. Note that we assume that the rate for the individual subclasses scales
according to the corresponding percentage in the local universe (Li et al.,
2011). The diffuse flux is given by

$\phi(E)=\int_{0}^{\infty}\frac{\rho(z)}{1+z}\frac{dN}{dE}\frac{c}{H(z)}dz,$
(7)

where $dN/dE$ is the time integrated flux upper limit for each SN subclass,
assuming that the subclass behaves as a neutrino standard candle class with an
$E^{-2.5}$ energy spectrum as motivated by the central value of the global fit
diffuse neutrino flux (Aartsen et al., 2015) and that the power law holds over
our sensitive energy range. This energy range is calculated by finding the
energy bound for selecting simulated signal events. We find the values where
our sensitivity drops by 5% for the lower and upper bounds separately. The
range between both values is our 90% energy range.

The resulting upper limits on the contribution of different SN types to the
diffuse neutrino flux are shown in Fig. 3. Assuming the choked-jet scenario,
stripped-envelope SNe can not contribute more than $14.6\%$ of the observed
diffuse neutrino flux. Assuming interaction with the CSM, stripped-envelope
SNe and SNe type IIn can explain not more than $26.6\%$ and $33.9\%$,
respectively. We mildly constrain the contribution of SNe type IIP to be less
than $59.9\%$. Note that the limit for type IIP SNe seem weaker when
translating it to a component of the diffuse flux because they are the most
abundant supernova type (Li et al., 2011).

Figure 3:  Upper limit on the contribution of different SN types to the
diffuse neutrino flux ($\nu_{\mu}+\bar{\nu}_{\mu}$) assuming an $E^{-2.5}$
energy spectrum compared with the measured diffuse astrophysical neutrino flux
(gray band). The limits are derived from the corresponding strictest limit in
Figure 2. The choked-jet model refers to the 20-day box model as explained in
Section 4. The energy range plotted here is the central $90\%$ energy range of
the analyzed neutrino sample.

This analysis has different sensitivities for different energy ranges, see
Fig. 4. The region of greatest sensitivity is around 10-100 TeV. It can reach
to higher energies as well, depending on the source declination. This broadly
overlaps with the energy range in which the diffuse IceCube neutrino flux
global fit was measured. The quoted upper limits to the diffuse flux
contribution are thus not strongly dependent on the extrapolation of the
measured diffuse flux to lower energies, where the flux has not yet been
measured due to large atmospheric background.

Figure 4: Differential sensitivity as a function of energy for different
source declinations $\delta$ with one year of experimental data. One can see
the maximum sensitivity is achieved around $10^{5}\,\mathrm{GeV}$ for sources
located in the northern sky and close to the equator. For sources located in
the southern sky, the overall sensitivity is much worse, but also peaks at
higher energies of $10^{6}\,\mathrm{GeV}$.

##  6 Conclusion

We have presented a search for neutrinos from certain types of CCSNe with
IceCube. In a stacking analysis we correlated more than 1000 SNe from optical
surveys with roughly 700,000 muon-track events recorded by IceCube. The
standard stacking method was extended to allow for fitting of individual
weights for each source, in order to account for expected variation in the
neutrino flux from individual sources. SNe type IIn, IIP and stripped-envelope
SNe were tested individually with various neutrino emission time models. No
significant temporal and spatial correlation of neutrinos and the cataloged
SNe was found, allowing us to set upper limits on the contribution of those
SNe to the diffuse neutrino flux.

CCSNe of type IIn, IIP and stripped-envelope SNe contribute less than $34\%$,
$60\%$ and $27\%$ ,respectively, to the diffuse neutrino flux at the $90\%$
confidence level, assuming CSM interaction and an extrapolation of the diffuse
neutrino spectrum to low energies following an unbroken power law with index
-2.5. Assuming a choked-jet, stripped-envelope SNe can not contribute more
than $15\%$.

Upper limits on the total neutrino energy emitted by a single CSM interacting
source are at levels comparable to model predictions by Murase et al. (2011)
(see Fig. 2) while model predictions from Zirakashvili & Ptuskin (2016) are
strongly disfavored. Note that the model prediction could easily be adjusted
to lower neutrino flux predictions by assuming a lower CSM density or a lower
kinetic SN energy.

Improvements to the presented limits are expected in the near future with
optical survey instruments such as the Zwicky Transient Factory (Graham et
al., 2019) which is able to undertake a high-cadence survey across a large
fraction of the sky, providing SN catalogs with much greater completeness. In
combination with next-generation neutrino telescopes, this will significantly
boost the sensitivity of this type of analysis, allowing us to probe dimmer
neutrino emitters and smaller contributions of CCSNe to the diffuse neutrino
flux.

## Acknowledgments

The IceCube Collaboration designed, constructed and now operates the IceCube
Neutrino Observatory. Data processing and calibration, Monte Carlo simulations
of the detector and of theoretical models, and data analyses were performed by
a large number of collaboration members, who also discussed and approved the
scientific results presented here. The IceCube collaboration acknowledges the
significant contributions to this manuscript from Jannis Necker, Alexander
Stasik and Robert Stein. It was reviewed by the entire collaboration before
publication, and all authors approved the final version of the manuscript. We
acknowledge support from the following agencies:

USA – U.S. National Science Foundation-Office of Polar Programs, U.S. National
Science Foundation-Physics Division, U.S. National Science Foundation-EPSCoR,
Wisconsin Alumni Research Foundation, Center for High Throughput Computing
(CHTC) at the University of Wisconsin–Madison, Open Science Grid (OSG),
Advanced Cyberinfrastructure Coordination Ecosystem: Services & Support
(ACCESS), Frontera computing project at the Texas Advanced Computing Center,
U.S. Department of Energy-National Energy Research Scientific Computing
Center, Particle astrophysics research computing center at the University of
Maryland, Institute for Cyber-Enabled Research at Michigan State University,
and Astroparticle physics computational facility at Marquette University;
Belgium – Funds for Scientific Research (FRS-FNRS and FWO), FWO Odysseus and
Big Science programmes, and Belgian Federal Science Policy Office (Belspo);
Germany – Bundesministerium für Bildung und Forschung (BMBF), Deutsche
Forschungsgemeinschaft (DFG), Helmholtz Alliance for Astroparticle Physics
(HAP), Initiative and Networking Fund of the Helmholtz Association, Deutsches
Elektronen Synchrotron (DESY), and High Performance Computing cluster of the
RWTH Aachen; Sweden – Swedish Research Council, Swedish Polar Research
Secretariat, Swedish National Infrastructure for Computing (SNIC), and Knut
and Alice Wallenberg Foundation; European Union – EGI Advanced Computing for
research; Australia – Australian Research Council; Canada – Natural Sciences
and Engineering Research Council of Canada, Calcul Québec, Compute Ontario,
Canada Foundation for Innovation, WestGrid, and Compute Canada; Denmark –
Villum Fonden, Carlsberg Foundation, and European Commission; New Zealand –
Marsden Fund; Japan – Japan Society for Promotion of Science (JSPS) and
Institute for Global Prominent Research (IGPR) of Chiba University; Korea –
National Research Foundation of Korea (NRF); Switzerland – Swiss National
Science Foundation (SNSF); United Kingdom – Department of Physics, University
of Oxford.

##  Appendix A Catalogs

Name | RA | Dec | Discovery Date | Redshift | Distance | Source
---|---|---|---|---|---|---
| [rad] | [rad] |  |  | [Mpc] |
SN1999bw | 2.70 | 0.79 | 1999-00-20 | 0.0032 | 9.80 | 1, 2
SN2002bu | 3.22 | 0.80 | 2002-00-28 | 0.0030 | 8.90 | 1, 2, 3
SN2008S | 5.39 | 1.05 | 2008-00-01 | 0.0012 | 5.60 | 4
SN2009kr | 1.36 | -0.27 | 2009-00-06 | 0.0075 | 16.00 | 5
SN2010jl | 2.54 | 0.17 | 2010-00-03 | 0.0117 | 49.00 | 6
SN2011an | 2.09 | 0.29 | 2011-00-01 | 0.0170 | 73.00 | 7
SN2011ht | 2.65 | 0.90 | 2011-00-29 | 0.0046 | 19.20 | 8
SN2012ab | 3.24 | 0.10 | 2012-00-31 | 0.0190 | 81.00 | 9
SN2013by | 4.29 | -1.05 | 2013-00-23 | 0.0038 | 14.80 | 10, 11
SN2013gc | 2.13 | -0.49 | 2013-00-07 | 0.0044 | 15.10 | 12
PSN J14041297-0938168 | 3.68 | -0.17 | 2013-00-20 | 0.0038 | 12.55 | 13
CSS140111:060437-123740 | 1.59 | -0.22 | 2013-00-24 | 0.0084 | 32.88 | 13
SN2014G | 2.86 | 0.95 | 2014-00-14 | 0.0045 | 20.00 | 14
MASTER OT J044212.20+230616.7 | 1.23 | 0.40 | 2014-00-21 | 0.0170 | 72.00 | 15
SN2015da | 3.63 | 0.69 | 2015-00-09 | 0.0079 | 32.14 | 16, 17
Table 1: Interacting supernovae catalogue. References: (1) Kochanek et al.
(2012), (2) Smith et al. (2011), (3) Szczygieł et al. (2012), (4) Stanishev et
al. (2008), (5) Steele et al. (2009a), (6) Benetti et al. (2010), (7) Marion &
Calkins (2011), (8) Prieto et al. (2011), (9) Bilinski et al. (2018), (10)
Margutti et al. (2013), (11) Parker et al. (2013), (12) Antezana et al.
(2013), (13) Challis (2013), (14) Denisenko et al. (2014), (15) Shivvers et
al. (2014), (16) Zhang & Wang (2015), (17) Tartaglia et al. (2020) Table 2:
IIP catalog. References: (1) Jha et al. (1999), (2) Patat et al. (2004), (3)
Zwitter et al. (2004), (4) Li et al. (2005), (5) Modjaz et al. (2005), (6)
Pastorello et al. (2009), (7) Li et al. (2007), (8) Morrell & Stritzinger
(2008), (9) Gandhi et al. (2013), (10) Sollerman et al. (2009), (11) Steele et
al. (2009b), (12) Valenti & Benetti (2011), (13) Stanishev & Pursimo (2012),
(14) Quadri et al. (2012), (15) Cellier-Holzem et al. (2012), (16) Monard et
al. (2012), (17) Bose et al. (2015), (18) Benetti et al. (2013), (19) Itagaki
et al. (2013), (20) Dhungana et al. (2016), (21) Andrews et al. (2016), (22)
Ochner et al. (2014) Table 3: Stripped-envelope supernovae catalogue.
References: (1) Chornock et al. (2007), (2) Valenti et al. (2008), (3)
Chornock et al. (2008), (4) Pastorello et al. (2008), (5) Silverman et al.
(2008), (6) Anderson et al. (2009), (7) Stockdale et al. (2009), (8) Chornock
& Berger (2009), (9) Marples & Drescher (2009), (10) Stritzinger et al.
(2010), (11) Maxwell et al. (2010), (12) Yamanaka et al. (2010), (13) Foley &
Fong (2011), (14) Borsato et al. (2012), (15) Fremling et al. (2016), (16)
Itagaki et al. (2012), (17) Wang et al. (2012), (18) Johnson et al. (2017),
(19) Takaki et al. (2012), (20) Tomasella et al. (2012), (21) Ciabattari et
al. (2013), (22) Van Dyk et al. (2014), (23) Cao et al. (2013), (24)
Milisavljevic et al. (2013), (25) Srivastav et al. (2014a), (26) Chandra et
al. (2019), (27) Singh et al. (2019), (28) Srivastav et al. (2014b), (29)
Drout et al. (2016), (30) Nakano et al. (2013), (31) Kim et al. (2014), (32)
Milisavljevic et al. (2015), (33) Tinyanont et al. (2016)

##  Appendix B p-values [%]

Table 4: Pre-trial p-values of the fitted weights scenario given as
percentages for a box shaped light curve model of different length and for the
CSM model of Zirakashvili & Ptuskin (2016) for different choices of $t_{pp}$.

##  Appendix C Upper Limits on Individual Sources

This section shows upper limits on individual SNe. Sources were selected based
on their expected neutrino signal. Here we assume a generic neutrino energy
spectrum of $E^{-2}$ rather than tying them to the observed diffuse spectral
shape and an emission time window of 100 days.

Name | ra | dec | discovery date | distance | Energy Upper Limit
---|---|---|---|---|---
| [rad] | [rad] |  | [Mpc] | $[10^{49}\,\mathrm{erg}]$
CSS140111:060437-123740 | 1.59 | -0.22 | 2013-12-24 | 31.8 | 49.8
PSN J13522411+3941286 | 3.63 | 0.693 | 2015-01-09 | 32.1 | 16.8
PSN J14041297-0938168 | 3.68 | -0.168 | 2013-12-20 | 12.5 | 4.8
PTF10aaxf | 2.54 | 0.166 | 2010-11-03 | 52.3 | 29.5
SN2008S | 5.39 | 1.049 | 2008-02-01 | 5.6 | 5.3
SN2009kr | 1.36 | -0.274 | 2009-11-06 | 16.0 | 19.1
SN2011an | 2.09 | 0.287 | 2011-03-01 | 73.0 | 65.3
SN2011ht | 2.65 | 0.905 | 2011-09-29 | 19.2 | 6.6
SN2012ab | 3.24 | 0.098 | 2012-01-31 | 81.0 | 64.18
SN2013gc | 2.13 | -0.49 | 2013-11-07 | 15.1 | 28.4
Table 5: Upper limits on selected SNe type IIn. Name | ra | dec | discovery date | distance | Energy Upper Limit
---|---|---|---|---|---
| [rad] | [rad] |  | [Mpc] | $[10^{49}\,\mathrm{erg}]$
iPTF13aaz | 2.96 | 0.228 | 2013-03-21 | 16.4 | 1.0
SN2012A | 2.73 | 0.299 | 2012-01-07 | 9.0 | 1.0
SN2012aw | 2.81 | 0.204 | 2012-03-16 | 9.6 | 1.0
SN2014bc | 3.22 | 0.826 | 2014-05-19 | 7.6 | 3.0
Table 6: Upper limits on selected SNe type IIP. Name | ra | dec | discovery date | distance | Energy Upper Limit
---|---|---|---|---|---
| [rad] | [rad] |  | [Mpc] | $[10^{49}\,\mathrm{erg}]$
iPTF13bvn | 3.93 | 0.033 | 2013-06-17 | 25.8 | 4.0
MASTER OT J120451.50 | 3.16 | 0.471 | 2014-10-28 | 15.0 | 1.0
PTF11eon | 3.53 | 0.823 | 2011-06-01 | 8.0 | 1.1
SN2008ax | 3.28 | 0.727 | 2008-03-03 | 5.1 | 1.6
SN2008dv | 0.95 | 1.267 | 2008-07-01 | 10.6 | 1.2
SN2010br | 3.16 | 0.777 | 2010-04-10 | 9.9 | 4.1
SN2011jm | 3.38 | 0.046 | 2011-12-24 | 14.0 | 1.8
SN2012cw | 2.68 | 0.06 | 2012-06-14 | 31.3 | 4.3
SN2012fh | 2.81 | 0.434 | 2012-10-18 | 8.6 | 1.1
SN2013df | 3.26 | 0.545 | 2013-06-07 | 10.6 | 1.7
SN2014C | 5.92 | 0.601 | 2014-01-05 | 12.1 | 2.3
Table 7: Upper limits on selected stripped-envelope SNe (Ib/c and IIb).

## References

  * Aartsen et al. (2013) Aartsen, M. G., et al. 2013, Science, 342, 1242856, doi: 10.1126/science.1242856
  * Aartsen et al. (2015) —. 2015, Astrophys. J., 809, 98, doi: 10.1088/0004-637X/809/1/98
  * Aartsen et al. (2017a) Aartsen, M. G., Abraham, K., Ackermann, M., et al. 2017a, ApJ, 835, 45, doi: 10.3847/1538-4357/835/1/45
  * Aartsen et al. (2017b) Aartsen, M. G., Ackermann, M., Adams, J., et al. 2017b, ApJ, 843, 112, doi: 10.3847/1538-4357/aa7569
  * Aartsen et al. (2017a) Aartsen, M. G., et al. 2017a, JINST, 12, P03012, doi: 10.1088/1748-0221/12/03/P03012
  * Aartsen et al. (2017b) —. 2017b, Astrophys. J., 835, 151, doi: 10.3847/1538-4357/835/2/151
  * Aartsen et al. (2018a) —. 2018a, Science, 361, X
  * Aartsen et al. (2018b) —. 2018b, Science, 361, 147
  * Ade et al. (2016) Ade, P. A. R., et al. 2016, Astron. Astrophys., 594, A13, doi: 10.1051/0004-6361/201525830
  * Ahlers & Halzen (2014) Ahlers, M., & Halzen, F. 2014, Phys. Rev., D90, 043005, doi: 10.1103/PhysRevD.90.043005
  * Anderson et al. (2009) Anderson, J., Morrell, N., Folatelli, G., & Stritzinger, M. 2009, Central Bureau Electronic Telegrams, 1789, 1
  * Ando & Beacom (2005) Ando, S., & Beacom, J. F. 2005, Physical Review Letters, 95, 061103, doi: 10.1103/PhysRevLett.95.061103
  * Andrews et al. (2016) Andrews, J. E., Krafton, K. M., Clayton, G. C., et al. 2016, Monthly Notices of the Royal Astronomical Society, 457, 3241, doi: 10.1093/mnras/stw164
  * Antezana et al. (2013) Antezana, R., Hamuy, M., Gonzalez, L., et al. 2013, Central Bureau Electronic Telegrams, 3699, 1
  * Benetti et al. (2010) Benetti, S., Bufano, F., Vinko, J., et al. 2010, Central Bureau Electronic Telegrams, 2536, 1
  * Benetti et al. (2013) Benetti, S., Tomasella, L., Pastorello, A., et al. 2013, The Astronomer’s Telegram, 4909, 1
  * Bilinski et al. (2018) Bilinski, C., Smith, N., Williams, G. G., et al. 2018, Monthly Notices of the Royal Astronomical Society, 475, 1104, doi: 10.1093/mnras/stx3214
  * Borsato et al. (2012) Borsato, L., Nascimbeni, V., Benetti, S., et al. 2012, Central Bureau Electronic Telegrams, 2993, 2
  * Bose et al. (2015) Bose, S., Valenti, S., Misra, K., et al. 2015, Monthly Notices of the Royal Astronomical Society, 450, 2373, doi: 10.1093/mnras/stv759
  * Braun et al. (2010) Braun, J., Baker, M., Dumm, J., et al. 2010, Astroparticle Physics, 33, 175, doi: 10.1016/j.astropartphys.2010.01.005
  * Braun et al. (2008) Braun, J., Dumm, J., De Palma, F., et al. 2008, Astropart. Phys., 29, 299, doi: 10.1016/j.astropartphys.2008.02.007
  * Cao et al. (2013) Cao, Y., Kasliwal, M. M., Arcavi, I., et al. 2013, The Astrophysical Journal, 775, L7, doi: 10.1088/2041-8205/775/1/L7
  * Cellier-Holzem et al. (2012) Cellier-Holzem, F., Smartt, S. J., Inserra, C., et al. 2012, The Astronomer’s Telegram, 4300, 1
  * Challis (2013) Challis, P. 2013, The Astronomer’s Telegram, 5700, 1
  * Chandra et al. (2019) Chandra, P., Nayana, A. J., Björnsson, C. I., et al. 2019, The Astrophysical Journal, 877, 79, doi: 10.3847/1538-4357/ab1900
  * Chornock & Berger (2009) Chornock, R., & Berger, E. 2009, Central Bureau Electronic Telegrams, 2086, 1
  * Chornock et al. (2007) Chornock, R., Filippenko, A. V., Li, W., et al. 2007, Central Bureau Electronic Telegrams, 1036, 1
  * Chornock et al. (2008) —. 2008, Central Bureau Electronic Telegrams, 1298, 1
  * Ciabattari et al. (2013) Ciabattari, F., Mazzoni, E., Donati, S., et al. 2013, Central Bureau Electronic Telegrams, 3557, 1
  * Coenders (2016) Coenders, S. 2016, Dissertation, Technische Universität München, München
  * Denisenko et al. (2014) Denisenko, D., Lipunov, V., Gorbovskoy, E., et al. 2014, Central Bureau Electronic Telegrams, 3787, 2
  * Denton & Tamborra (2018) Denton, P. B., & Tamborra, I. 2018, ApJ, 855, 37, doi: 10.3847/1538-4357/aaab4a
  * Dhungana et al. (2016) Dhungana, G., Kehoe, R., Vinko, J., et al. 2016, The Astrophysical Journal, 822, 6, doi: 10.3847/0004-637X/822/1/6
  * Drout et al. (2016) Drout, M. R., Milisavljevic, D., Parrent, J., et al. 2016, The Astrophysical Journal, 821, 57, doi: 10.3847/0004-637X/821/1/57
  * Faran et al. (2014) Faran, T., Poznanski, D., Filippenko, A. V., et al. 2014, MNRAS, 442, 844, doi: 10.1093/mnras/stu955
  * Foley & Fong (2011) Foley, R. J., & Fong, W. 2011, Central Bureau Electronic Telegrams, 2962, 2
  * Fremling et al. (2016) Fremling, C., Sollerman, J., Taddia, F., et al. 2016, Astronomy and Astrophysics, 593, A68, doi: 10.1051/0004-6361/201628275
  * Gandhi et al. (2013) Gandhi, P., Yamanaka, M., Tanaka, M., et al. 2013, The Astrophysical Journal, 767, 166, doi: 10.1088/0004-637X/767/2/166
  * Graham et al. (2019) Graham, M. J., Kulkarni, S. R., Bellm, E. C., et al. 2019, arXiv e-prints, arXiv:1902.01945.  https://arxiv.org/abs/1902.01945
  * Guillochon et al. (2017) Guillochon, J., Parrent, J., Kelley, L. Z., & Margutti, R. 2017, ApJ, 835, 64, doi: 10.3847/1538-4357/835/1/64
  * Hogg (1999) Hogg, D. W. 1999, arXiv e-prints, astro.  https://arxiv.org/abs/astro-ph/9905116
  * IceCube Collaboration et al. (2022) IceCube Collaboration, Abbasi, R., Ackermann, M., et al. 2022, Science, 378, 538, doi: 10.1126/science.abg3395
  * Itagaki et al. (2012) Itagaki, K., Noguchi, T., Nakano, S., et al. 2012, Central Bureau Electronic Telegrams, 3148, 1
  * Itagaki et al. (2013) —. 2013, Central Bureau Electronic Telegrams, 3498, 1
  * Jha et al. (1999) Jha, S., Challis, P., Garnavich, P., et al. 1999, International Astronomical Union Circular, 7296, 2
  * Johnson et al. (2017) Johnson, S. A., Kochanek, C. S., & Adams, S. M. 2017, Monthly Notices of the Royal Astronomical Society, 472, 3115, doi: 10.1093/mnras/stx2170
  * Kim et al. (2014) Kim, M., Zheng, W., Li, W., et al. 2014, Central Bureau Electronic Telegrams, 3777, 1
  * Kochanek et al. (2012) Kochanek, C. S., Szczygieł, D. M., & Stanek, K. Z. 2012, The Astrophysical Journal, 758, 142, doi: 10.1088/0004-637X/758/2/142
  * Kurahashi et al. (2022) Kurahashi, N., Murase, K., & Santander, M. 2022, arXiv e-prints, arXiv:2203.11936.  https://arxiv.org/abs/2203.11936
  * Li et al. (2011) Li, W., Leaman, J., et al. 2011, Monthly Notices of the Royal Astronomical Society, 412, 1441, doi: 10.1111/j.1365-2966.2011.18160.x
  * Li et al. (2005) Li, W., Van Dyk, S. D., Filippenko, A. V., & Cuillandre, J.-C. 2005, Publications of the Astronomical Society of the Pacific, 117, 121, doi: 10.1086/428278
  * Li et al. (2007) Li, W., Wang, X., Van Dyk, S. D., et al. 2007, The Astrophysical Journal, 661, 1013, doi: 10.1086/516747
  * Margutti et al. (2013) Margutti, R., Soderberg, A., & Milisavljevic, D. 2013, The Astronomer’s Telegram, 5106, 1
  * Marion & Calkins (2011) Marion, G. H., & Calkins, M. 2011, Central Bureau Electronic Telegrams, 2668, 2
  * Marples & Drescher (2009) Marples, P., & Drescher, C. 2009, Central Bureau Electronic Telegrams, 2080, 1
  * Mauerhan et al. (2013) Mauerhan, J. C., Smith, N., Silverman, J. M., et al. 2013, MNRAS, 431, 2599, doi: 10.1093/mnras/stt360
  * Maxwell et al. (2010) Maxwell, A. J., Graham, M. L., Parker, A., et al. 2010, Central Bureau Electronic Telegrams, 2245, 2
  * Milisavljevic et al. (2013) Milisavljevic, D., Fesen, R., Pickering, T., et al. 2013, The Astronomer’s Telegram, 5142, 1
  * Milisavljevic et al. (2015) Milisavljevic, D., Margutti, R., Kamble, A., et al. 2015, The Astrophysical Journal, 815, 120, doi: 10.1088/0004-637X/815/2/120
  * Modjaz et al. (2005) Modjaz, M., Kirshner, R., Challis, P., & Hutchins, R. 2005, International Astronomical Union Circular, 8555, 1
  * Monard et al. (2012) Monard, L. A. G., Childress, M., Scalzo, R., Yuan, F., & Schmidt, B. 2012, Central Bureau Electronic Telegrams, 3201, 1
  * Moriya et al. (2011) Moriya, T., Tominaga, N., Blinnikov, S. I., Baklanov, P. V., & Sorokina, E. I. 2011, MNRAS, 415, 199, doi: 10.1111/j.1365-2966.2011.18689.x
  * Moriya et al. (2012) Moriya, T. J., Tominaga, N., Blinnikov, S. I., Baklanov, P. V., & Sorokina, E. I. 2012, in IAU Symposium, Vol. 279, Death of Massive Stars: Supernovae and Gamma-Ray Bursts, ed. P. Roming, N. Kawai, & E. Pian, 54–57, doi: 10.1017/S1743921312012689
  * Morrell & Stritzinger (2008) Morrell, N., & Stritzinger, M. 2008, Central Bureau Electronic Telegrams, 1335, 1
  * Murase et al. (2011) Murase, K., Thompson, T. A., Lacki, B. C., & Beacom, J. F. 2011, Phys. Rev., D84, 043003, doi: 10.1103/PhysRevD.84.043003
  * Nakano et al. (2013) Nakano, S., Kiyota, S., Masi, G., et al. 2013, Central Bureau Electronic Telegrams, 3701, 1
  * Nakaoka et al. (2018) Nakaoka, T., Kawabata, K. S., Maeda, K., et al. 2018, The Astrophysical Journal, 859, 78.  http://stacks.iop.org/0004-637X/859/i=2/a=78
  * Necker et al. (2022) Necker, J., de Jaeger, T., Stein, R., et al. 2022, Monthly Notices of the Royal Astronomical Society, 516, 2455, doi: 10.1093/mnras/stac2261
  * Ochner et al. (2014) Ochner, P., Tomasella, L., Benetti, S., et al. 2014, The Astronomer’s Telegram, 6160, 1
  * Ofek et al. (2013) Ofek, E. O., et al. 2013, Nature, 494, 65, doi: 10.1038/nature11877
  * Parker et al. (2013) Parker, S., Kiyota, S., Morrell, N., et al. 2013, Central Bureau Electronic Telegrams, 3506, 1
  * Pastorello et al. (2008) Pastorello, A., Kasliwal, M. M., Crockett, R. M., et al. 2008, Monthly Notices of the Royal Astronomical Society, 389, 955, doi: 10.1111/j.1365-2966.2008.13618.x
  * Pastorello et al. (2009) Pastorello, A., Valenti, S., Zampieri, L., et al. 2009, Monthly Notices of the Royal Astronomical Society, 394, 2266, doi: 10.1111/j.1365-2966.2009.14505.x
  * Patat et al. (2004) Patat, F., Benetti, S., Pastorello, A., Filippenko, A. V., & Aceituno, J. 2004, International Astronomical Union Circular, 8378, 1
  * Pitik et al. (2022) Pitik, T., Tamborra, I., Angus, C. R., & Auchettl, K. 2022, ApJ, 929, 163, doi: 10.3847/1538-4357/ac5ab1
  * Prieto et al. (2011) Prieto, J. L., McMillan, R., Bakos, G., & Grennan, D. 2011, Central Bureau Electronic Telegrams, 2903, 1
  * Quadri et al. (2012) Quadri, U., Strabla, L., Girelli, R., et al. 2012, Central Bureau Electronic Telegrams, 3054, 1
  * Razzaque et al. (2004) Razzaque, S., Mészáros, P., & Waxman, E. 2004, Physical Review Letters, 93, 181101, doi: 10.1103/PhysRevLett.93.181101
  * Reusch et al. (2022) Reusch, S., Stein, R., Kowalski, M., et al. 2022, Physical Review Letters, 128, 221101, doi: 10.1103/PhysRevLett.128.221101
  * Sarmah et al. (2022) Sarmah, P., Chakraborty, S., Tamborra, I., & Auchettl, K. 2022, Journal of Cosmology and Astroparticle Physics, 2022, 011, doi: 10.1088/1475-7516/2022/08/011
  * Senno et al. (2016) Senno, N., Murase, K., & Meszaros, P. 2016, Phys. Rev., D93, 083003, doi: 10.1103/PhysRevD.93.083003
  * Shivvers et al. (2014) Shivvers, I., Kelly, P. L., Clubb, K. I., & Filippenko, A. V. 2014, The Astronomer’s Telegram, 6487, 1
  * Silverman et al. (2008) Silverman, J. M., Griffith, C. V., Filippenko, A. V., Chornock, R., & Li, W. 2008, Central Bureau Electronic Telegrams, 1447, 1
  * Singh et al. (2019) Singh, M., Misra, K., Sahu, D. K., et al. 2019, Monthly Notices of the Royal Astronomical Society, 485, 5438, doi: 10.1093/mnras/stz752
  * Smith et al. (2011) Smith, N., Li, W., Silverman, J. M., Ganeshalingam, M., & Filippenko, A. V. 2011, Monthly Notices of the Royal Astronomical Society, 415, 773, doi: 10.1111/j.1365-2966.2011.18763.x
  * Sollerman et al. (2009) Sollerman, J., Ergon, M., Inserra, C., et al. 2009, Central Bureau Electronic Telegrams, 2068, 1
  * Srivastav et al. (2014a) Srivastav, S., Anupama, G. C., & Sahu, D. K. 2014a, Monthly Notices of the Royal Astronomical Society, 445, 1932, doi: 10.1093/mnras/stu1878
  * Srivastav et al. (2014b) Srivastav, S., Sahu, D. K., & Anupama, G. C. 2014b, The Astronomer’s Telegram, 6639, 1
  * Stanishev et al. (2008) Stanishev, V., Pastorello, A., & Pursimo, T. 2008, Central Bureau Electronic Telegrams, 1235, 1
  * Stanishev & Pursimo (2012) Stanishev, V., & Pursimo, T. 2012, Central Bureau Electronic Telegrams, 2974, 3
  * Steele et al. (2009a) Steele, T. N., Cobb, B., & Filippenko, A. V. 2009a, Central Bureau Electronic Telegrams, 2011, 1
  * Steele et al. (2009b) Steele, T. N., Kandrashoff, M. T., & Filippenko, A. V. 2009b, Central Bureau Electronic Telegrams, 2070, 1
  * Stein (2019) Stein, R. 2019, in Proceedings of 36th International Cosmic Ray Conference — PoS(ICRC2019), Vol. 358, 1016, doi: 10.22323/1.358.1016
  * Stein et al. (2022a) Stein, R., Necker, J., Bradascio, F., & Garrappa, S. 2022a, icecube/flarestack: Titan v2.4.2, v2.4.2, Zenodo, doi: 10.5281/zenodo.6425740
  * Stein et al. (2021) Stein, R., et al. 2021, Nature Astron., 5, 510, doi: 10.1038/s41550-020-01295-8
  * Stein et al. (2022b) Stein, R., Reusch, S., Franckowiak, A., et al. 2022b, arXiv e-prints, arXiv:2203.17135
  * Stockdale et al. (2009) Stockdale, C. J., Rentz, B., Vandrevala, C. M., et al. 2009, International Astronomical Union Circular, 9056, 1
  * Stritzinger et al. (2010) Stritzinger, M., Folatelli, G., & Pignata, G. 2010, Central Bureau Electronic Telegrams, 2116, 1
  * Strolger et al. (2015) Strolger, L.-G., Dahlen, T., Rodney, S. A., et al. 2015, Astrophys. J., 813, 93, doi: 10.1088/0004-637X/813/2/93
  * Strotjohann et al. (2021) Strotjohann, N. L., Ofek, E. O., Gal-Yam, A., et al. 2021, ApJ, 907, 99, doi: 10.3847/1538-4357/abd032
  * Szczygieł et al. (2012) Szczygieł, D. M., Kochanek, C. S., & Dai, X. 2012, The Astrophysical Journal, 760, 20, doi: 10.1088/0004-637X/760/1/20
  * Takaki et al. (2012) Takaki, K., Itoh, R., Ueno, I., et al. 2012, Central Bureau Electronic Telegrams, 3263, 3
  * Tartaglia et al. (2020) Tartaglia, L., Pastorello, A., Sollerman, J., et al. 2020, Astronomy and Astrophysics, 635, A39, doi: 10.1051/0004-6361/201936553
  * Tinyanont et al. (2016) Tinyanont, S., Kasliwal, M. M., Fox, O. D., et al. 2016, The Astrophysical Journal, 833, 231, doi: 10.3847/1538-4357/833/2/231
  * Tomasella et al. (2012) Tomasella, L., Turatto, M., Benetti, S., et al. 2012, Central Bureau Electronic Telegrams, 3263, 2
  * Valenti & Benetti (2011) Valenti, S., & Benetti, S. 2011, Central Bureau Electronic Telegrams, 2749, 2
  * Valenti et al. (2008) Valenti, S., Elias-Rosa, N., Taubenberger, S., et al. 2008, The Astrophysical Journal, 673, L155, doi: 10.1086/527672
  * Van Dyk et al. (2014) Van Dyk, S. D., Zheng, W., Fox, O. D., et al. 2014, The Astronomical Journal, 147, 37, doi: 10.1088/0004-6256/147/2/37
  * Wang et al. (2012) Wang, X. F., Liu, Q., Zhang, J. J., Zhang, T. M., & Brimacombe, J. 2012, Central Bureau Electronic Telegrams, 3148, 2
  * Yamanaka et al. (2010) Yamanaka, M., Arai, A., Sakimoto, K., Okushima, T., & Kawabata, K. S. 2010, Central Bureau Electronic Telegrams, 2384, 1
  * Yaron & Gal-Yam (2012) Yaron, O., & Gal-Yam, A. 2012, Publications of the Astronomical Society of the Pacific, 124, 668.  http://stacks.iop.org/1538-3873/124/i=917/a=668
  * Yaron et al. (2017) Yaron, O., et al. 2017, Nature Phys., 13, 510, doi: 10.1038/nphys4025
  * Zhang & Wang (2015) Zhang, J., & Wang, X. 2015, The Astronomer’s Telegram, 6939, 1
  * Zirakashvili & Ptuskin (2016) Zirakashvili, V. N., & Ptuskin, V. S. 2016, Astropart. Phys., 78, 28, doi: 10.1016/j.astropartphys.2016.02.004
  * Zwitter et al. (2004) Zwitter, T., Munari, U., & Moretti, S. 2004, International Astronomical Union Circular, 8413, 1