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1 Erratum to: Eur. Phys. J. C https://doi.org/10.1140/epjc/s10052-014-2938-8
In the analyses, published in Ref. [1], the exclusion limits are calculated in dependence of the mean free path of the magnetic monopole - nucleon catalysis interaction \(\lambda _{\mathrm {cat}}\). The values of the latter are set as defined point of measurement for the analyses. For comparison with previous limits, the mean free path is converted to the catalysis cross section \(\sigma _{\mathrm {cat}}\) via
where n is the number density of contributing targets, the nucleons of the water molecule \(\mathrm {H}_{2}\mathrm {O}\).
Nucleons bound in various nuclei contribute differently to the total catalysis cross section which can be expressed by the following calculation of the catalysis cross section \(\sigma _{\rm cat}\)
where \(\sigma _{0}\) is the speed independent cross section (introduced in Ref. [4], \(\beta \) is the speed as fraction of the speed of light, and \(f_{i}\) is the form factor accounting for the contribution of nucleons bound in a nucleus i to the cross section. An exemplary calculation of the form factor f can be found in Ref. [2].
In Ref. [1] the number of hydrogen nucleons
is used as target density instead of the valid number density of nucleons
required in Eq. 1 where \(N_{A}\) is the Avogadro constant, \(\rho \) is the mass density of the ice and m is the molar mass of two hydrogen nucleons or all nucleons. Therefore the exclusion limits apply to a factor 9 smaller catalysis cross section as depicted in Fig. 1.
The analyses are based on the detection and reconstruction of light produced by magnetic monopoles. Increasing speed or increasing cross section result in brighter signatures. Thus, an exclusion limit implicitly not only excludes higher rates but also larger cross sections. Therefore the corrected limits still exclude the same flux vs. cross section area as published before. However, it extends by a factor of 9 to smaller cross sections. In comparison to the MACRO limits, which is also shown in Fig. 1, the originally published limit in Ref. [1] is weaker than the corrected limit which is calculated using the nucleon density \(n_{n}\).
All values of the cross section given in descriptions and captions of Ref. [1] have to be divided by a factor of 9 throughout the paper. Thus, the IC86-DC analysis of Ref. [1] improves the flux limits published previously above \(\sigma _{\rm cat}=10^{-25}\,\mathrm {cm}^{2}\) corresponding to \(\lambda _{\rm cat}<3\,\mathrm {m}\) by more than one order of magnitude. The IC-59 analysis is sensitive for bright monopoles with \(\sigma _{\rm cat}=1.9\cdot 10^{-24}\,\mathrm {cm}^{2}\).
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Acknowledgements
USA – U.S. National Science Foundation-Office of Polar Programs, U.S. National Science Foundation-Physics Division, Wisconsin Alumni Research Foundation, Center for High Throughput Computing (CHTC) at the University of Wisconsin-Madison, Open Science Grid (OSG), Extreme Science and Engineering Discovery Environment (XSEDE), 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; 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, Danish National Research Foundation (DNRF); 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).
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III. Physikalisches Institut, RWTH Aachen University, 52056, Aachen, Germany
J. Auffenberg, M. Bissok, J. Blumenthal, P. Gretskov, C. Haack, P. Hallen, D. Heinen, K. Jagielski, A. Kriesten, K. Krings, M. Leuermann, L. Paul, L. Rädel, R. Reimann, S. Schoenen, A. Schukraft, M. Vehring, M. Wallraff, C. H. Wiebusch & S. Zierke
School of Chemistry and Physics, University of Adelaide, Adelaide, SA, 5005, Australia
M. G. Aartsen, G. C. Hill, S. Robertson & B. J. Whelan
Department of Physics and Astronomy, University of Alaska Anchorage, 3211 Providence Dr., Anchorage, AK, 99508, USA
K. Rawlins
CTSPS, Clark-Atlanta University, Atlanta, GA, 30314, USA
G. S. Japaridze
School of civistic Astrophysics, Georgia Institute of Technology, Atlanta, GA, 30332, USA
J. Casey, J. Daughhetee & I. Taboada
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A. R. Fazely, S. Ter-Antonyan & X. W. Xu
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R. Bay, G. Binder, K. Filimonov, L. Gerhardt, C. Ha, S. R. Klein, S. Miarecki, P. B. Price & K. Woschnagg
Lawrence Berkeley National Laboratory, Berkeley, CA, 94720, USA
G. Binder, L. Gerhardt, A. Goldschmidt, C. Ha, S. R. Klein, H. S. Matis, S. Miarecki, D. R. Nygren, G. T. Przybylski, T. Stezelberger & R. G. Stokstad
Institut für Physik, Humboldt-Universität zu Berlin, 12489, Berlin, Germany
M. de With & H. Kolanoski
Fakultät für Physik & Astronomie, Ruhr-Universität Bochum, 44780, Bochum, Germany
J. Becker Tjus, B. Eichmann, A. Fedynitch, S. M. Saba, S. Schöneberg & E. Unger
Physikalisches Institut, Universität Bonn, Nussallee 12, 53115, Bonn, Germany
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Université Libre de Bruxelles, Science Faculty CP230, 1050, Brussels, Belgium
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Department of Astronomy, University of Wisconsin, Madison, WI, 53706, USA
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T.U. Munich, 85748, Garching, Germany
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Correspondence to M. L. Benabderrahmane or S. Schoenen.
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Aartsen, M.G., Abbasi, R., Ackermann, M. et al. Erratum to: Search for non-relativistic magnetic monopoles with IceCube. Eur. Phys. J. C 79, 124 (2019). https://doi.org/10.1140/epjc/s10052-019-6582-1
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DOI: https://doi.org/10.1140/epjc/s10052-019-6582-1
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