A DECam Search for Explosive Optical Transients Associated with IceCube Neutrino Alerts

R. Morgan, K. Bechtol, R. Kessler, M. Sako, K. Herner, Z. Doctor, D. Scolnic, I. Sevilla-Noarbe, A. Franckowiak, K. N. Neilson, M. Kowalski, A. Palmese, E. Swann, B. P. Thomas, A. K. Vivas, A. Drlica-Wagner, A. Garcia, D. Brout, F. Paz-Chinchón, E. NeilsenH. T. Diehl, M. Soares-Santos, T. M.C. Abbott, S. Avila, E. Bertin, D. Brooks, E. Buckley-Geer, A. Carnero Rosell, M. Carrasco Kind, J. Carretero, R. Cawthon, M. Costanzi, J. De Vicente, S. Desai, P. Doel, B. Flaugher, P. Fosalba, J. Frieman, J. García-Bellido, E. Gaztanaga, D. W. Gerdes, D. Gruen, R. A. Gruendl, J. Gschwend, G. Gutierrez, D. L. Hollowood, K. Honscheid, D. J. James, N. Kuropatkin, M. Lima, M. A.G. Maia, J. L. Marshall, F. Menanteau, C. J. Miller, R. Miquel, A. A. Plazas, E. Sanchez, V. Scarpine, M. Schubnell, S. Serrano, M. Smith, F. Sobreira, E. Suchyta, M. E.C. Swanson, G. Tarle, V. Vikram, A. R. Walker, J. Weller

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Abstract

In this work, we investigate the likelihood of association between real-time, neutrino alerts with teraelectronvolt to petaelectronvolt energy from IceCube and optical counterparts in the form of core-collapse supernovae (CC SNe). The optical follow-up of IceCube alerts requires two main instrumental capabilities: (1) deep imaging, since 73% of neutrinos would come from CC SNe at redshifts z > 0.3, and (2) a large field of view (FoV), since typical IceCube muon neutrino pointing accuracy is on the order of ∼1 deg. With Blanco/DECam (gri to 24th magnitude and 2.2 deg diameter FoV), we performed a triggered optical follow-up observation of two IceCube alerts, IC170922A and IC171106A, on six nights during the three weeks following each alert. For the IC170922A (IC171106A) follow-up observations, we expect that 12.1% (9.5%) of coincident CC SNe at z ≲ 0.3 are detectable, and that, on average, 0.23 (0.07) unassociated SNe in the neutrino 90% containment regions also pass our selection criteria. We find two candidate CC SNe that are temporally coincident with the neutrino alerts in the FoV, but none in the 90% containment regions, a result that is statistically consistent with expected rates of background CC SNe for these observations. If CC SNe are the dominant source of teraelectronvolt to petaelectronvolt neutrinos, we would expect an excess of coincident CC SNe to be detectable at the 3σ confidence level using DECam observations similar to those of this work for ∼60 (∼200) neutrino alerts with (without) redshift information for all candidates.

Original languageEnglish
Article number125
JournalAstrophysical Journal
Volume883
Issue number2
DOIs
StatePublished - Oct 1 2019

Funding

R. Morgan K. Bechtol R. Kessler M. Sako K. Herner Z. Doctor D. Scolnic I. Sevilla-Noarbe A. Franckowiak K. N. Neilson M. Kowalski A. Palmese E. Swann B. P. Thomas A. K. Vivas A. Drlica-Wagner A. Garcia D. Brout F. Paz-Chinch\uFFFDn E. Neilsen H. T. Diehl M. Soares-Santos T. M. C. Abbott S. Avila E. Bertin D. Brooks E. Buckley-Geer A. Carnero Rosell M. Carrasco Kind J. Carretero R. Cawthon M. Costanzi J. De Vicente S. Desai P. Doel B. Flaugher P. Fosalba J. Frieman J. Garc\uFFFDa-Bellido E. Gaztanaga D. W. Gerdes D. Gruen R. A. Gruendl J. Gschwend G. Gutierrez D. L. Hollowood K. Honscheid D. J. James N. Kuropatkin M. Lima M. A. G. Maia J. L. Marshall F. Menanteau C. J. Miller R. Miquel A. A. Plazas E. Sanchez V. Scarpine M. Schubnell S. Serrano M. Smith F. Sobreira E. Suchyta M. E. C. Swanson G. Tarle V. Vikram A. R. Walker J. Weller R. Morgan K. Bechtol R. Kessler M. Sako K. Herner Z. Doctor D. Scolnic I. Sevilla-Noarbe A. Franckowiak K. N. Neilson M. Kowalski A. Palmese E. Swann B. P. Thomas A. K. Vivas A. Drlica-Wagner A. Garcia D. Brout F. Paz-Chinch\uFFFDn E. Neilsen H. T. Diehl M. Soares-Santos T. M. C. Abbott S. Avila E. Bertin D. Brooks E. Buckley-Geer A. Carnero Rosell M. Carrasco Kind J. Carretero R. Cawthon M. Costanzi J. De Vicente S. Desai P. Doel B. Flaugher P. Fosalba J. Frieman J. Garc\uFFFDa-Bellido E. Gaztanaga D. W. Gerdes D. Gruen R. A. Gruendl J. Gschwend G. Gutierrez D. L. Hollowood K. Honscheid D. J. James N. Kuropatkin M. Lima M. A. G. Maia J. L. Marshall F. Menanteau C. J. Miller R. Miquel A. A. Plazas E. Sanchez V. Scarpine M. Schubnell S. Serrano M. Smith F. Sobreira E. Suchyta M. E. C. Swanson G. Tarle V. Vikram A. R. Walker J. Weller Physics Department, University of Wisconsin-Madison, 1150 University Avenue Madison, WI 53706, USA Large Synoptic Survey Telescope Corporation Data Science Fellowship Program, USA Large Synoptic Survey Telescope, 933 North Cherry Avenue, Tucson, AZ 85721, USA Department of Astronomy and Astrophysics, University of Chicago, Chicago, IL 60637, USA Kavli Institute for Cosmological Physics, University of Chicago, Chicago, IL 60637, USA Department of Physics and Astronomy, University of Pennsylvania, Philadelphia, PA 19104, USA Fermi National Accelerator Laboratory, P.O. Box 500, Batavia, IL 60510, USA Centro de Investigaciones Energ\uFFFDticas, Medioambientales y Tecnol\uFFFDgicas (CIEMAT), Madrid, Spain Deutsches Elektronen Synchrotron DESY, D-15738 Zeuthen, Germany Department of Physics, Drexel University, 3141 Chestnut St, Philadelphia, PA 19104, USA Institute of Physics, Humboldt-Universit\uFFFDt zu Berlin, Newtonstr. 15, D-12489 Berlin, Germany Deutsches Elektronen-Synchrotron, D-15735 Zeuthen, Germany Institute of Cosmology and Gravitation, University of Portsmouth, Portsmouth, PO1 3FX, UK Cerro Tololo Inter-American Observatory, National Optical Astronomy Observatory, Casilla 603, La Serena, Chile Brandeis University, Physics Department, 415 South Street, Waltham MA 02453, USA National Center for Supercomputing Applications, 1205 West Clark St., Urbana, IL 61801, USA Instituto de Fisica Teorica UAM/CSIC, Universidad Autonoma de Madrid, E-28049 Madrid, Spain CNRS, UMR 7095, Institut d\u2019Astrophysique de Paris, F-75014, Paris, France Sorbonne Universit\uFFFDs, UPMC Univ Paris 06, UMR 7095, Institut d\u2019Astrophysique de Paris, F-75014, Paris, France Department of Physics & Astronomy, University College London, Gower Street, London, WC1E 6BT, UK Laborat\uFFFDrio Interinstitucional de e-Astronomia\u2014LIneA, Rua Gal. Jos\uFFFD Cristino 77, Rio de Janeiro, RJ\u201420921-400, Brazil Department of Astronomy, University of Illinois at Urbana-Champaign, 1002 W. Green Street, Urbana, IL 61801, USA Institut de F\uFFFDsica d\u2019Altes Energies (IFAE), The Barcelona Institute of Science and Technology, Campus UAB, E-08193 Bellaterra (Barcelona), Spain Physics Department, 2320 Chamberlin Hall, University of Wisconsin-Madison, 1150 University Avenue Madison, WI 53706-1390, USA Universit\uFFFDts-Sternwarte, Fakult\uFFFDt f\uFFFDr Physik, Ludwig-Maximilians Universit\uFFFDt M\uFFFDnchen, Scheinerstr. 1, D-81679 M\uFFFDnchen, Germany Department of Physics, IIT Hyderabad, Kandi, Telangana 502285, India Institut d\u2019Estudis Espacials de Catalunya (IEEC), E-08034 Barcelona, Spain Institute of Space Sciences (ICE, CSIC), Campus UAB, Carrer de Can Magrans, s/n, 08193 Barcelona, Spain Department of Astronomy, University of Michigan, Ann Arbor, MI 48109, USA Department of Physics, University of Michigan, Ann Arbor, MI 48109, USA Department of Physics, Stanford University, 382 Via Pueblo Mall, Stanford, CA 94305, USA Kavli Institute for Particle Astrophysics & Cosmology, P.O. Box 2450, Stanford University, Stanford, CA 94305, USA SLAC National Accelerator Laboratory, Menlo Park, CA 94025, USA Observat\uFFFDrio Nacional, Rua Gal. Jos\uFFFD Cristino 77, Rio de Janeiro, RJ\u201420921-400, Brazil Santa Cruz Institute for Particle Physics, Santa Cruz, CA 95064, USA Center for Cosmology and Astro-Particle Physics, The Ohio State University, Columbus, OH 43210, USA Department of Physics, The Ohio State University, Columbus, OH 43210, USA Center for Astrophysics, Harvard & Smithsonian, 60 Garden Street, Cambridge, MA 02138, USA Departamento de F\uFFFDsica Matem\uFFFDtica, Instituto de F\uFFFDsica, Universidade de S\uFFFDo Paulo, CP 66318, S\uFFFDo Paulo, SP, 05314-970, Brazil George P. and Cynthia Woods Mitchell Institute for Fundamental Physics and Astronomy, and Department of Physics and Astronomy, Texas A&M University, College Station, TX 77843, USA Instituci\uFFFD Catalana de Recerca i Estudis Avan\uFFFDats, E-08010 Barcelona, Spain Department of Astrophysical Sciences, Princeton University, Peyton Hall, Princeton, NJ 08544, USA School of Physics and Astronomy, University of Southampton, Southampton, SO17 1BJ, UK Instituto de F\uFFFDsica Gleb Wataghin, Universidade Estadual de Campinas, 13083-859, Campinas, SP, Brazil Computer Science and Mathematics Division, Oak Ridge National Laboratory, Oak Ridge, TN 37831, USA Argonne National Laboratory, 9700 South Cass Avenue, Lemont, IL 60439, USA Excellence Cluster Origins, Boltzmannstr. 2, 85748 Garching, Germany Max Planck Institute for Extraterrestrial Physics, Giessenbachstrasse, 85748 Garching, Germany R. Morgan, K. Bechtol, R. Kessler, M. Sako, K. Herner, Z. Doctor, D. Scolnic, I. Sevilla-Noarbe, A. Franckowiak, K. N. Neilson, M. Kowalski, A. Palmese, E. Swann, B. P. Thomas, A. K. Vivas, A. Drlica-Wagner, A. Garcia, D. Brout, F. Paz-Chinch\uFFFDn, E. Neilsen, H. T. Diehl, M. Soares-Santos, T. M. C. Abbott, S. Avila, E. Bertin, D. Brooks, E. Buckley-Geer, A. Carnero Rosell, M. Carrasco Kind, J. Carretero, R. Cawthon, M. Costanzi, J. De Vicente, S. Desai, P. Doel, B. Flaugher, P. Fosalba, J. Frieman, J. Garc\uFFFDa-Bellido, E. Gaztanaga, D. W. Gerdes, D. Gruen, R. A. Gruendl, J. Gschwend, G. Gutierrez, D. L. Hollowood, K. Honscheid, D. J. James, N. Kuropatkin, M. Lima, M. A. G. Maia, J. L. Marshall, F. Menanteau, C. J. Miller, R. Miquel, A. A. Plazas, E. Sanchez, V. Scarpine, M. Schubnell, S. Serrano, M. Smith, F. Sobreira, E. Suchyta, M. E. C. Swanson, G. Tarle, V. Vikram, A. R. Walker and J. Weller 2019-10-01 2019-09-26 14:30:56 cgi/release: Article released bin/incoming: New from .zip National Science Foundation AST-1138766 National Science Foundation AST-1536171 yes In this work, we investigate the likelihood of association between real-time, neutrino alerts with teraelectronvolt to petaelectronvolt energy from IceCube and optical counterparts in the form of core-collapse supernovae (CC SNe). The optical follow-up of IceCube alerts requires two main instrumental capabilities: (1) deep imaging, since 73% of neutrinos would come from CC SNe at redshifts z \uFFFD>\uFFFD0.3, and (2) a large field of view (FoV), since typical IceCube muon neutrino pointing accuracy is on the order of \u223C1\uFFFDdeg. With Blanco/DECam ( gri to 24th magnitude and 2.2 deg diameter FoV), we performed a triggered optical follow-up observation of two IceCube alerts, IC170922A and IC171106A, on six\uFFFDnights during the three\uFFFDweeks following each alert. For the IC170922A (IC171106A) follow-up observations, we expect that 12.1% (9.5%) of coincident CC SNe at z \uFFFD\u2272\uFFFD0.3 are detectable, and that, on average, 0.23 (0.07) unassociated SNe in the neutrino 90% containment regions also pass our selection criteria. We find two candidate CC SNe that are temporally coincident with the neutrino alerts in the FoV, but none in the 90% containment regions, a result that is statistically consistent with expected rates of background CC SNe for these observations. If CC SNe are the dominant source of teraelectronvolt to petaelectronvolt neutrinos, we would expect an excess of coincident CC SNe to be detectable at the 3 \u03C3 confidence level using DECam observations similar to those of this work for \u223C60 (\u223C200) neutrino alerts with (without) redshift information for all candidates. \uFFFD 2019. The American Astronomical Society. All rights reserved. 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FundersFunder number
Kavli Institute for Theoretical Physics, University of California, Santa Barbara
University of Wisconsin-Madison
Synoptic Survey Telescope Corporation
University of Chicago
Deutsches Elektronen-Synchrotron
Data Science Fellowship Program
University of Pennsylvania
Drexel University
Science and Technology Facilities CouncilST/P006892/1
Seventh Framework Programme1138766, 240672, 306478, 1829740
National Science Foundation1138766, 1829740, 291329

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