# Limits on Neutrino Emission from GRB 221009A from MeV to PeV using the
IceCube Neutrino Observatory

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
N. Aggarwal  Dept. of Physics, University of Alberta, Edmonton, Alberta,
Canada T6G 2E1  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, 41296
Gothenburg, Sweden  Fakultät für Physik & Astronomie, Ruhr-Universität Bochum,
D-44780 Bochum, Germany  J. Beise Dept. of Physics and Astronomy, Uppsala
University, Box 516, SE-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  J. Borowka  III. Physikalisches
Institut, RWTH Aachen University, D-52056 Aachen, Germany  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, SE-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  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  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 and
Astronomy, Michigan State University, East Lansing, MI 48824, 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, SE-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  C. Dappen  III. Physikalisches Institut, RWTH Aachen University, D-52056
Aachen, Germany  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 Karlsruhe Institute of
Technology, Institute for Astroparticle Physics, D-76021 Karlsruhe, Germany
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  III. Physikalisches Institut, RWTH Aachen University,
D-52056 Aachen, Germany  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  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, SE-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, SE-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, SE-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  Dept. of Physics and Wisconsin IceCube Particle Astrophysics Center,
University of Wisconsin–Madison, Madison, WI 53706, 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. 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  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. 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  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  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,
SE-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, SE-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, SE-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  K. Upshaw  Dept. of
Physics, Southern University, Baton Rouge, LA 70813, USA  N. Valtonen-Mattila
Dept. of Physics and Astronomy, Uppsala University, Box 516, SE-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 Dept. of Physics and
Wisconsin IceCube Particle Astrophysics Center, University of
Wisconsin–Madison, Madison, WI 53706, USA  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

(March 29, 2023)

###### Abstract

Gamma-ray bursts (GRBs) have long been considered a possible source of high-
energy neutrinos. While no correlations have yet been detected between high-
energy neutrinos and GRBs, the recent observation of GRB 221009A — the
brightest GRB observed by Fermi-GBM to date and the first one to be observed
above an energy of 10 TeV — provides a unique opportunity to test for hadronic
emission. In this paper, we leverage the wide energy range of the IceCube
Neutrino Observatory to search for neutrinos from GRB 221009A. We find no
significant deviation from background expectation across event samples ranging
from MeV to PeV energies, placing stringent upper limits on the neutrino
emission from this source.

Neutrino telescopes – Gamma-ray bursts – Particle astrophysics

##  1 Introduction

On October 9th 2022 at 13:16:59.99 UT, the Gamma-ray Burst Monitor (GBM) on
board the Fermi satellite triggered and located the exceptionally bright long-
duration Gamma-Ray Burst GRB 221009A (Veres et al., 2022; Lesage et al.,
2022). This source was also observed by Swift (Dichiara et al., 2022; Kennea &
Williams, 2022), Fermi-LAT (Bissaldi et al., 2022), INTEGRAL (SPI-ACS), Konus-
Wind and triangulated by the InterPlanetary Network (IPN; Svinkin et al.,
2022). A highlight among the many multiwavelength and multimessenger follow-up
searches§§§see https://gcn.gsfc.nasa.gov/ &
http://www.astronomerstelegram.org/ of GRB 221009A has been the first
detection of $\gamma$-rays above an energy of $10$ TeV from a GRB as observed
by LHAASO (Huang et al., 2022).

The GBM light curve consists of an initial $17$ s long pulse after the GBM
trigger (T0), followed by an extraordinarily bright episode starting $221.1$ s
after T0. The duration (T90) that contains the central 90% of emission from
the GRB has a length of $(325.8\pm 6.8)$ s. Given that this GRB saturated the
Fermi-GBM instrument, it is possible that this is an overestimation of the
T90. The time-integrated energy flux in the range 10–1000 keV is reported as
$(2.912\pm 0.001)\times 10^{-2}\,{\rm erg}\,{\rm cm}^{-2}$ with a $1.024$ s
peak photon flux at the level of $(2385\pm 3)\,{\rm cm}^{-2}\,{\rm s}^{-1}$,
making this the most fluent and intense GRB detected by Fermi-GBM (Lesage et
al., 2022).

The GRB was also localized using measurements from the Swift Observatory at
right ascension $\alpha=288.2645^{\circ}$ and declination
$\delta=+19.7735^{\circ}$. The 90% containment of this measurement, as
provided by Swift, is $0.61$ arcseconds (Dichiara et al., 2022). The redshift
$z\simeq 0.151$ of the GRB has been inferred from afterglow emission observed
with X-SHOOTER of the Very Large Telescope $11.55$ hr after T0 (de Ugarte
Postigo et al., 2022) corresponding to a luminosity distance of about
$D_{L}\simeq 740$ Mpc (Workman et al., 2022).

Long-duration GRBs are triggered by the death of massive stars. The
gravitational and/or magnetic energy that is released in these events is the
principal power for the observed bright $\gamma$-ray display and has long been
speculated to facilitate cosmic-ray acceleration (Waxman, 1995; Vietri, 1995).
The interaction of these cosmic rays with ambient radiation and/or matter
could yield broadband neutrino emission that, depending on the mechanism, can
even precede the electromagnetic emission. The IceCube Observatory has already
reported upper limits on neutrino emission of GRB 221009A from a Fast Response
Analysis (FRA; Thwaites, 2022) searching for TeV–PeV neutrino emission in the
periods [T0 $-$ 1 hr , T0 + 2 hr] and T0 $\pm$ 1d. An independent search by
the KM3NeT Observatory did not find significant neutrino emission in the
period [T0 $-$ 50 s , T0 + 5000 s] either (Dornic, 2022).

In this Letter, we report the results of four searches for neutrino emission
coincident with GRB 221009A using data collected with the IceCube Observatory.
These searches cover complementary energy ranges from a few MeV up to the PeV
scale, probing neutrino emission from the burst core to high-energy neutrinos
produced in external shocks during the GRB.

##  2 Neutrinos from Gamma-Ray Bursts

One of the leading models for the GRB prompt emission involves a hot and dense
plasma (“fireball”) that is initially opaque to radiation and expands under
its pressure. The kinetic energy of the resulting highly relativistic outflow
is dissipated via internal shocks, which are expected to form from variations
of the bulk Lorentz factor (Rees & Mészáros, 1994; Daigne & Mochkovitch, 1998;
Kobayashi et al., 1997), or via magnetic reconnection in Poynting-flux-
dominated outflows (Mészáros & Rees, 1997). In both cases, electrons are
accelerated and produce the bright $\gamma$-ray prompt display via synchrotron
emission in magnetic fields.

Protons or heavier nuclei entrained in the outflow can also be accelerated by
these mechanisms and produce high-energy TeV–PeV neutrinos on collisions with
background photons (Waxman & Bahcall, 1997; Becker et al., 2006; Murase &
Nagataki, 2006; Hümmer et al., 2012; Bustamante et al., 2015; Biehl et al.,
2018; Pitik et al., 2021; Ai & Gao, 2023; Liu et al., 2023; Rudolph et al.,
2023). Prior to the prompt emission, internal collisions of protons and
neutrons below the photosphere have been considered as a source of GeV
neutrino emission (Murase et al., 2013; Bahcall & Mészáros, 2000; Bartos et
al., 2013; Murase et al., 2022). Furthermore, reverse shocks that form during
the afterglow phase have been considered sites for efficient cosmic-ray
acceleration and would yield extremely high energy neutrinos in the EeV energy
range from interactions with optical–UV photons (Waxman & Bahcall, 2000;
Murase, 2007; Thomas et al., 2017; Murase et al., 2022; Zhang et al., 2022).
Detection of these neutrinos would be a compelling indicator of (ultra-)high-
energy cosmic-ray acceleration in GRBs.

GRBs could also be promising sites of production of thermal neutrino
distributions through different mechanisms, for example, in the standard core-
collapse processes, where neutrinos would arrive before the shock breakout
(Kistler et al., 2013). Neutrino-dominated accretion flows (Liu et al., 2017;
Qi et al., 2022) could form in the case of a supernova with jets, producing
neutrinos in the MeV energy range that would arrive either prior to the GRB
(Wang & Mészáros, 2007; Wei et al., 2019; Liu et al., 2016), or during the
$\gamma$-ray emission (Liu et al., 2016). Finally, the fireball could also be
a potential site of neutrino emission with thermal spectra (Halzen & Jaczko,
1996), where these neutrinos are predicted to arrive shortly before the
photons in a millisecond burst.

Which (if any) of these mechanisms leads to detectable neutrino emission is
uncertain, so it is imperative to consider different time windows and energy
spectra of GRB neutrino emission in dedicated searches. Previous searches of
high-energy neutrino emission carried out by IceCube have so far yielded upper
limits that imposed constraints on optimistic neutrino emission models (Abbasi
et al., 2009a, 2012a; Aartsen et al., 2015, 2016a; Abbott et al., 2017;
Aartsen et al., 2017a; Abbasi et al., 2022c); see also Lucarelli et al.
(2022).

##  3 The IceCube Observatory

The IceCube Observatory (Aartsen et al., 2017b) is a multicomponent facility
located at the geographic South Pole. Its main component consists of an in-ice
array that utilizes one cubic kilometer of the deep ultraclear glacial ice as
its detector medium. The fiducial volume is instrumented with 5,160 Digital
Optical Modules (DOMs; Abbasi et al., 2009b), each hosting one downward-facing
photomultiplier tube (PMT), that register the Cherenkov light emitted by
relativistic charged particles passing through the detector (Abbasi et al.,
2010). The DOMs are distributed on 86 readout and support cables (“strings”)
and are deployed between 1.45 km and 2.45 km below the surface. Most strings
follow a triangular grid with a width of 125 m, evenly spaced over the volume.

Eight strings are placed in the center of the array and are instrumented with
a denser DOM spacing and typical interstring separation of 55 m. They are
equipped with PMTs with 35% higher quantum efficiency. These strings, along
with the nearest layer of the surrounding standard strings, form the DeepCore
low-energy subarray (Abbasi et al., 2012b). While the original IceCube array
has a neutrino energy threshold of about 100 GeV, the addition of the denser
infill lowers the energy threshold to about 1 GeV. An additional component of
IceCube is the surface air shower array, IceTop (Abbasi et al., 2013), whose
data were not used in the analyses presented in this Letter.

Neutrino interactions with matter in the vicinity of the in-ice array create
energetic charged particles that are visible via Cherenkov emission. Several
triggers are active in IceCube that are designed for the selection of these
and other interesting physics events. The principal challenges of
astrophysical neutrino observations with IceCube are the large background
generated by cosmic-ray interactions in the atmosphere and reconstruction of
neutrino direction. The better the direction of the neutrino is known, the
more background from directions not compatible with the GRB can be reduced. At
high energies ($\gtrsim$ 100 GeV), enough light is deposited, in particular by
energetic muons that are individually reconstructable in both direction and
energy, to provide half-degree typical angular resolution. At lower energies
($\sim$ 10–100 GeV), only enough light is collected to reconstruct directions
within uncertainties of several to tens of degrees, forcing higher reliance on
time correlations with the GRB to reject background. At the lowest energies
($\lesssim$ 10 GeV), individual neutrino interactions are not reconstructable,
forcing a complete reliance on timing information.

The analyses described in the following section use different strategies to
search for neutrino emission from astrophysical transients of a wide variety
of energy and time scales. Each analysis is optimized for the detection of
neutrino emission in a different energy range, where it surpasses the
sensitivity of other analyses. In combination, this allows us to probe
neutrino emission of GRB 221009A over nine orders of magnitude in neutrino
energy, from MeV to PeV.

Table 1: Models for the time-integrated neutrino flux $F(E)$ and energy ranges
probed by different datasets. While the analyses based on GFU, GRECO and
ELOWEN test broad power-law fluxes the analysis based on SNDAQ probes peaked
quasi-thermal fluxes motivated by core-collapse supernovae.

Dataset | Time-Integrated Neutrino Flux Model
---|---
| Power-law : $F(E)\propto E^{-\gamma}$ for $E_{\rm min}\leq E\leq E_{\rm
max}$
| $\gamma$ | $E_{\rm min}$ | $E_{\rm max}$
GFU⋆ | 1.5 |  $6.8$ TeV |  $9.9$ PeV
2.0 |  $0.83$ TeV |  $0.96$ PeV
2.5 |  $0.23$ TeV |  $0.086$ PeV
3.0 |  $0.13$ TeV |  $0.013$ PeV
GRECO⋆ | 1.5 |  $40$ GeV |  $1.5$ TeV
2.0 |  $26$ GeV |  $1.2$ TeV
2.5 |  $15$ GeV |  $0.70$ TeV
3.0 |  $11$ GeV |  $0.35$ TeV
ELOWEN | 2.0 $-$ 3.0 |  $0.5$ GeV |  $5.0$ GeV
| Quasi-thermal : $F_{\bar{\nu}_{e}}(E)\propto E^{2}\exp(-3E/\langle
E\rangle)$
SNDAQ | $E\simeq\langle E\rangle\simeq(10-20)\,{\rm MeV}$

Note. — ⋆Central 90% energy range depends on spectral index $\gamma$.

##  4 Analyses and Results

In the following, we summarize the methodology and results of four
complementary IceCube analyses of neutrino emission of GRB 221009A. Three of
these are based on neutrino event samples that have been developed for
previous IceCube analyses: the Gamma-ray Follow-Up (GFU) sample has been
optimized for IceCube’s real-time program (Aartsen et al., 2016b); the GeV
Reconstructed Events with Containment for Oscillations (GRECO) sample was
originally developed for oscillation studies with atmospheric neutrinos
(Aartsen et al., 2019) and has since been used for low-energy neutrino
transients (GRECO Astronomy; Abbasi et al., 2022d); the Extremely Low-Energy
(ELOWEN) event sample was developed for the search of low-energy neutrino
emission during solar flares (Abbasi et al., 2021a). In addition, IceCube is
able to observe a significant burst of MeV neutrinos through an increased
level of single-photon hit rates in DOMs across the entire detector. This
search is based on a real-time data stream called the Supernova Data
Acquisition (SNDAQ) that was developed to detect MeV neutrinos from supernovae
(Abbasi et al., 2011).

Table 1 summarizes the test hypotheses for the time-integrated neutrino flux
$F(E)\equiv d^{2}N/dE/dA$ (neutrinos per area $A$ and energy $E$) and
corresponding neutrino energy scales accessible by these different datasets.
The energy-dependent effective areas from the direction of GRB 221009A can be
found in Appendix A. For the GFU and GRECO datasets the energy interval
$[E_{\rm min},E_{\rm max}]$ corresponds to the central 90% energy range of
predicted events for a power-law emission with spectral index $\gamma$ at the
location of GRB 221009A; harder (softer) indices will shift this energy range
to higher (lower) values. Table 1 shows the wide MeV–PeV bandwidth covered in
the following analyses.

Figure 1: Gamma-ray observations and upper limits on the time-integrated
neutrino flux of GRB 221009A. We show the $\gamma$-ray observations from
Fermi-GBM (Lesage et al., 2022) and Fermi-LAT (Bissaldi et al., 2022) as well
as upper limits from HAWC (Ayala, 2022). The Fermi-GBM result covering the
prompt phase (“peak 2”) had no reported spectral fit, so it is shown here at
$\gamma=2.0$ for visualization purposes. The upper limits on the time-
integrated neutrino flux are shown for various spectral indices as indicated
by the numbers. The right axis shows the differential isotropic equivalent
energy $d\mathcal{E}_{\rm iso}/dE$.

###  4.1 Fast Response Analysis: ¿ 100 GeV

The FRA (Abbasi et al., 2021b, 2022a) is a framework established to rapidly
follow up interesting transients or multimessenger events in real time with
the IceCube Neutrino Observatory. The FRA requires a real-time data stream,
with low-latency access to data from the South Pole, in order to follow up
interesting transients in real time. This GFU sample uses events triggered by
causally connected single-photon hits on eight or more neighboring IceCube
DOMs and employs a faster event reconstruction at the expense of some angular
resolution available for offline reconstructions (Aartsen et al., 2016b). At
final filter level, the stream has an all-sky rate that varies between
approximately 6 and 7 mHz owing to seasonal variations (Abbasi et al., 2021b).
Figure 2 in Appendix A shows the effective area of the GFU sample for the
direction of GRB 221009A.

The FRA uses an unbinned maximum likelihood method to identify significant
neutrino emission following an $E^{-2}$ spectrum on top of background events.
The method has been used in other searches for short-timescale neutrino
emission from potential sources (Aartsen et al., 2020; Abbasi et al., 2023,
2022c). We initiated an FRA of GRB 221009A in response to the observations
reported by Swift and Fermi-GBM using the time windows (a) [T0 $-$ 1 hr , T0 +
2 hr] (3 hours in total) and (b) T0 $\pm$ 1 d (2 days in total) to cover
extended emission periods before and after the Fermi-GBM trigger, as
summarized in Thwaites (2022).

In addition to this initial real-time FRA, we also searched for neutrino
emission using the same data sample for an extended set of time windows
following the method of a previous archival search for neutrinos coincident
with GRBs (Abbasi et al., 2022c). This analysis used three time windows in
order to search for neutrinos (c) during the T90 phase as given by Fermi-GBM,
(d) during the period [T0 $-$ 200 s , T0 + 2000 s] to include times
corresponding to the high-energy photons observed by LHAASO (Huang et al.,
2022) as well as potential precursor emission, and (e) during the extended
period [T0 $-$ 1 d , T0 + 14 d] covering precursor-to-afterglow emission. We
scanned over a circle of radius of $1^{\circ}$, centered on the location of
GRB 221009A in order to find the location with highest significance, which is
consistent with the previous method. Both these analyses assumed an $E^{-2}$
spectrum as in the initial FRA.

None of these analyses — the initial FRA and its application to an extended
set of time windows — found indications for neutrino emission above background
expectations, with $p$-values being close to 1. These results allow us to set
upper limits on the energy-scaled time-integrated neutrino flux, $E^{2}F(E)$,
which are summarized in Tab. 2 at a reference energy $E_{0}=100\,{\rm TeV}$.
In the case of the standard FRA time windows of 3 hours and 2 days, we provide
upper limits for four different power-law indices $\gamma$ based on Monte
Carlo injections following $F(E)\propto E^{-\gamma}$.

Figure 1 shows the upper limits on the time-integrated neutrino flux for the
T90 phase and the time window [T0 $-$ 1 hr , T0 + 2 hr]. These upper limits
can be translated into limits on the differential isotropic equivalent energy
$d\mathcal{E}_{\rm iso}/dE$ of GRB 221009A at redshift $z$ and luminosity
distance $D_{L}$ via the relation $E^{2}F(E)=Ed\mathcal{E}_{\rm
iso}/dE\times(1+z)/(4\pi D_{L}^{2})$. This quantity is indicated by the right
axis in Fig. 1.

Table 2: Upper limits (UL) on the time-integrated neutrino flux of GRB 221009A
for different time windows♯. The three analyses based on GFU, GRECO and ELOWEN
assume a per-flavor time-integrated power-law flux $F(E)\propto E^{-\gamma}$
with variable spectral index $\gamma$. The results are given for the energy-
scaled time-integrated per-flavor neutrino flux, $E^{2}F(E)$, at a reference
energy $E_{0}$ depending on the dataset. The analysis based on the SNDAQ
assumes an electron antineutrino spectrum following a quasi-thermal spectrum
peaked at $\langle E\rangle=15$ MeV. Results are shown for the total and peak
time-integrated $\bar{\nu}_{e}$ flux.

Dataset | Time Window & Index♯ | 90% C.L. Upper Limits (ULs) on the Time-integrated Neutrino Flux $F(E)$
---|---|---
|  |  | Power-law $F(E)\propto E^{-\gamma}$: per-flavor ULs show $E^{2}F(E)$ [GeV cm-2] at $E_{0}$
|  |  | $E_{0}$ | $\gamma=1.5$ | $\gamma=2.0$ | $\gamma=2.5$ | $\gamma=3.0$
GFU | [T0 $-$ 1 hr , T0 + 2 hr] | (a) | $100$ TeV | 0.0359 | 0.0393⋆ | 0.0143 | 0.00240
T0 $\pm$ 1 d | (b) | 0.0370 | 0.0410⋆ | 0.0176 | 0.00345
T90 phase | (c) |  $\cdots$ | 0.0364 |  $\cdots$ |  $\cdots$
[T0 $-$ 200 s , T0 + 2000 s] | (d) |  $\cdots$ | 0.0369 |  $\cdots$ |  $\cdots$
[T0 $-$ 1 d , T0 + 14 d] | (e) |  $\cdots$ | 0.0471 |  $\cdots$ |  $\cdots$
GRECO | T90 phase | (c) | $1$ TeV | 1.052 | 1.015 | 0.561 | 0.174
[T0 $-$ 200 s , T0 + 2000 s] | (d) | 1.387 | 1.338 | 0.740 | 0.229
ELOWEN | T0 $\pm$ 500 s | (f) | $1$ GeV |  $\cdots$ | $5.3\times 10^{3}$ | $8.7\times 10^{3}$ | $1.4\times 10^{4}$
[T0 $-$ 200 s , T0 + 2000 s] | (d) |  $\cdots$ | $7.9\times 10^{3}$ | $1.3\times 10^{4}$ | $2.0\times 10^{4}$
|  |  | Quasi-thermal $F_{\bar{\nu}_{e}}(E)\propto E^{2}\exp(-3E/\langle E\rangle)$ : ${\bar{\nu}_{e}}$ UL on total and peak flux
|  |  | $\langle E\rangle$ | Total ${\bar{\nu}_{e}}$ Flux [cm-2] |  $E^{2}F_{\bar{\nu}_{e}}(E)$ [GeV cm-2] at $\langle E\rangle$
SNDAQ | [T0 $-$ 100 s , T0] | (g) | $15$ MeV | $7.98\times 10^{8}$ | $8.05\times 10^{6}$
[T0 $-$ 1 s , T0] | (h) | $1.81\times 10^{9}$ | $1.82\times 10^{7}$
[T0 , T0 + 17 s] | (i) | $8.00\times 10^{8}$ | $8.07\times 10^{6}$
[T0 + 18 s , T0 + 174 s] | (j) | $3.08\times 10^{8}$ | $3.11\times 10^{6}$
[T0 + 174 s , T0 + 175 s] | (k) | $1.35\times 10^{9}$ | $1.36\times 10^{7}$
[T0 + 175 s , T0 + 547 s] | (l) | $4.00\times 10^{8}$ | $4.03\times 10^{6}$

Note. — ♯The different time windows are discussed in section 4 and are
referenced by their inline text indices.

Note. — ⋆Values corresponding to the real-time FRA results published in
Thwaites (2022).

###  4.2 GRECO Astronomy Analysis: 10–1000 GeV

This analysis focuses on the low-energy GRECO Astronomy dataset, which is
optimized for neutrinos between 10 GeV and 1 TeV (Abbasi et al., 2022b). This
sample is based on events with at least three coincident hits in DeepCore DOMs
and has an average event rate of about 4 mHz at final filter level (Aartsen et
al., 2019). The effective area for GRB 221009A is shown in Fig. 2. In order to
test for neutrino emission from GRB 221009A, we use an extended unbinned
maximum-likelihood outlined in Abbasi et al. (2022c) combined with a spatial
prior to account for the source localization uncertainty. The signal
hypothesis assumes an $E^{-2.5}$ neutrino spectrum with equal contributions
from all flavors.

To account for the fact that angular uncertainties for the low-energy events
used in the GRECO Astronomy dataset are relatively large, a Kent distribution
(Kent, 1982) is assumed for the spatial likelihood. The localization prior is
a $1^{\circ}$ radius top-hat distribution centered at the localization
provided by Swift. This is done for computational reasons, and the size of the
prior does not affect the result given that angular uncertainties used in
GRECO Astronomy are relatively large.

The analysis of GRB 221009A focused on two time windows, matching those of
other analyses at different energy ranges. We searched for neutrino emission
${\it(c)}$ coincident with the central 90% emission from the GRB as reported
as the T90 phase by Fermi-GBM and ${\it(d)}$ the 2,200 second window [T0 $-$
200 s , T0 + 2000 s] including potential precursor emission and coinciding
with high-energy photons observed by LHAASO. Though even longer time windows
are desirable too, this is prevented by computational constraints.

We did not find significant deviations from a background distribution in
either of the two time windows, with $p$-values being close to 1 in this
analysis. The corresponding upper limits on the energy-scaled time-integrated
neutrino flux, $E^{2}F(E)$, at a reference energy of $E_{0}=1$ TeV for each
time window and four different spectral indices can be found in Tab. 2.
Similar to the previous analysis, we provide upper limits for different power-
law indices $\gamma$ derived from the corresponding Monte-Carlo injections.
Figure 1 shows the upper limits on the time-integrated neutrino flux for the
T90 phase.

###  4.3 ELOWEN Analysis: 0.5–5 GeV

The selection of events below 10 GeV at IceCube is challenging owing to the
presence of large atmospheric backgrounds and the lack of directional
reconstruction in this energy range. However, relying on temporal coincidence
makes it possible to search for potential neutrino emission in the GeV energy
range. Here we follow the methods used in a previous analysis in this energy
range (Abbasi et al., 2021c), which are briefly summarized here. Two short
time windows were chosen based on archival electromagnetic data from GRBs
(Baret et al., 2011) while minimizing the impact of the background for our
neutrino search: (f) a 1,000 second window T0 $\pm$ 500 s centered on the
Fermi-GBM trigger and (d) the 2,200 second window [T0 $-$ 200 s , T0 + 2000 s]
also used in other analyses.

Because of the reliance on timing in this analysis, we require a precise model
of the background event rate as the key component of the search. To determine
this, we examined a large number of time windows of the same lengths during
time periods where no transient events were detected (GRBs, gravitational
waves, or — for the longer window — classical novae). The rates in these
windows, as well as in the 8-hour period immediately before the GRB, were
statistically compatible with the expected background data rate of 0.2 Hz,
validating our background model.

Like GRECO, the dataset is based on events with at least three coincident hits
in DeepCore DOMs. The filtering process for ELOWEN, which is explained in more
detail in Abbasi et al. (2021a), keeps 40% of the initial sample of neutrinos
following an $E^{-2}$ spectrum from 0.5 GeV to 5 GeV, simulated with GENIE
2.8.6 (Andreopoulos et al., 2010), while reducing the background from
atmospheric muons and detector noise (Abbasi et al., 2010, 2009b; Larson,
2013) by $>$99.9%. We show the ELOWEN effective area in comparison to the
previously discussed samples in Fig. 2.

The significance of any excess observed during the on-time phase can then be
calculated by comparison to the off-time phase with the methods described in
Li & Ma (1983). None of the tested time windows showed indications for
neutrino emission in the 0.5 $-$ 5 GeV energy range; we find $p$-values larger
than $0.7$. The corresponding upper limits on the energy-scaled time-
integrated neutrino flux, $E^{2}F(E)$, at a reference energy of $E_{0}=1$ GeV
can be found in Tab. 2 for three different spectral indices of the simulated
power-law spectrum. Figure 1 shows the upper limits on the time-integrated
flux for the 1,000 second time window.

###  4.4 MeV Neutrino Burst Analysis: ¡ 1 GeV

IceCube can observe a significant burst of sub-GeV neutrinos through an
increased level of single-photon hit rates on the PMTs across the entire
detector, predominantly from the reaction $\bar{\nu}_{e}+p\to e^{+}+n$,
compared to the uncorrelated single-PMT noise rate at the level of about $0.5$
kHz (Abbasi et al., 2010). In this analysis, we use the SNDAQ data stream
designed for the detection of supernovae (Abbasi et al., 2011) to search for
MeV neutrinos from GRB 221009A. We divide the search into six time windows
covering from 100 s prior to T0 up to the end of T90 for a total of 647
seconds. These time windows, shown at the bottom of Tab. 2, were selected to
search for MeV neutrino emission (g) 100 s and (h) 1 s prior to the precursor,
(i) during the precursor phase, (j) during the phase between precursor and
prompt emission, (k) 1 s prior to the prompt phase, and (l) during the T90
phase. To find the excess rates in the different time windows, we use a
sliding 1 s search window to identify the highest rate during each of the
longer time periods. For the shortest time windows spanning 1 s, we instead
use a 0.5 s sliding search window.

To calculate the significance of the observed number of hits at the time of
the GRB compared to what is expected from the background, we repeat the search
method described above for each time window on 2 weeks of off-time data: 1
week prior to the GRB and 1 week after. The upper limit on the observed hits
is obtained using the method of Feldman & Cousins (1998) for a 90% C.L. These
hit upper limits are then used to obtain an upper limit on the time-integrated
flux through A Supernova Test Routine for IceCube Analysis (ASTERIA; Griswold
et al., 2020). ASTERIA is a fast supernova neutrino simulation designed to
model the detector response for IceCube.

The neutrino spectra of core-collapse supernovae are expected to evolve in
time. For simplicity, all tested time windows in this analysis assume the
emission of electron antineutrinos ($\bar{\nu}_{e}$) following a generic
quasi-thermal spectrum inferred from simulations of core-collapse supernovae
(Keil et al., 2003) approximated as a Maxwell–Boltzmann distribution
$F_{\bar{\nu}_{e}}(E)\propto E^{2}\exp(-3E/\langle E\rangle)$ with mean energy
of $\langle E\rangle=15$ MeV (Tamborra et al., 2012). Since the on-time data
are consistent with the background for all six time windows ($p>0.3$), we set
a 90% C.L. upper limit for the total time-integrated flux of electron
antineutrinos and the energy-scaled time-integrated flux,
$E^{2}F_{\bar{\nu}_{e}}(E)$, at the peak $\langle E\rangle$ for each time
window in Tab. 2.

##  5 Conclusions

Our searches did not find significant neutrino emission in an energy range
from MeV to PeV, before, during, or after the electromagnetic emission,
resulting in upper limits on the time-integrated neutrino flux of GRB 221009A.
These upper limits allow constraints on neutrino emission models from this
source, as discussed by Ai & Gao (2023), Murase et al. (2022), Liu et al.
(2023), and Rudolph et al. (2023). Previous IceCube searches for the joint
neutrino emission of GRBs showed that high-energy neutrino emission during the
prompt phase (or during $10^{4}$ s) of GRBs is limited to $\leq 1\%$ (or $\leq
24\%$) of the high-energy diffuse neutrino flux observed by IceCube (Abbasi et
al., 2022c).

Future upgrades and proposed extensions of IceCube could provide a crucial
step toward neutrino detection from GRBs. The IceCube-Upgrade (Ishihara, 2021)
will enhance the detection of 1-10 GeV neutrino events with respect to the
GRECO Astronomy and ELOWEN samples and will improve the angular reconstruction
above $10$ GeV. The proposed multicomponent extension IceCube-Gen2 (Aartsen et
al., 2021) would significantly increase the sensitivity to high-energy
neutrino transients, e.g., increasing the observable volume within our
universe by one order of magnitude for TeV–PeV neutrinos compared to IceCube.

## Acknowledgments

The IceCube Collaboration acknowledges Eric Burns for valuable discussions of
public Fermi-GBM results. The authors gratefully acknowledge the support from
the following agencies and institutions: 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 Effective Area

The complementary energy coverage of the different data sets used in this
Letter can be appreciated by a comparison of the respective neutrino effective
areas. The declination and energy-dependent all-flavor effective area $A_{\rm
eff}(\delta,E_{\nu})$ is defined via the relation:

$N_{\rm events}=\int dE_{\nu}A_{\rm eff}(\delta,E_{\nu})F(E_{\nu})\,,$ (A1)

where $N_{\rm events}$ is the analysis-specific number of signal events and
$F(E_{\nu})$ the per-flavor time-integrated neutrino flux (assuming identical
flux for each flavor) for a source at declination $\delta$. Figure 2 shows
these effective areas for the ELOWEN, GRECO, and GFU samples for the
declination $\delta\simeq+19.8^{\circ}$ of GRB 221009A. Starting at low
energy, the ELOWEN sample contributes the most up to neutrino energies of 5
GeV; the GRECO selection performs best in the 10-100 GeV range; the GFU sample
dominates beyond a few 100 GeV. The GFU data sample used for our analysis is
described in full by Aartsen et al. (2016b). Note that the effective area of
this GFU selection is substantially larger, especially at low energies, than
the small subsample of GFU events used to trigger alerts (Blaufuss et al.,
2020) and is similar to those from other neutrino source searches at high
energy. The SNDAQ effective area is not shown, as it is does not work with
individual neutrino events and so its effective area is not comparable to the
other analyses and is not a good guide to sensitivity. The SNDAQ analysis
instead searches for a sudden increase of the overall background rate in the
detector induced by a burst of sub-GeV neutrinos. The figure of merit is not
the total number of signal events, as in Eq. (A1), but rather the rate of
correlated single-photon hits across the detector, which is a function of both
flux and energy spectrum. More details on SNDAQ sensitivity can be found in
Abbasi et al. (2011).

Figure 2: The all-flavor effective area for neutrinos from the direction of
GRB 221009A for various datasets used in this Letter. The GRECO and ELOWEN
samples are sensitive to all neutrino flavors, while the GFU sample only
includes muon-neutrino-induced muons that traverse the detector as signal
events.

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