Erratum to: Sensitivity of multi-PMT optical modules in Antarctic ice to supernova neutrinos of MeV energy

We found an error in the code for calculating the CCSN detection range that led to double counting of signal events and thus to ranges that were too large by a factor of about

• The values for the detection ranges decrease as shown in the corrected Table 4. Figures 8, 9, 10 change accordingly. Correspondingly, the numbers change in: -Abstract: We find that exploiting temporal coincidences between signals in different photocathode segments, a 27 M progenitor mass CCSN can be detected up to a distance of (341 kpc → 269 kpc) with a false detection rate of 0.01 year −1 with a detector consisting of 10,000 sensors. -Section 4.2: The trigger condition (m ≥ 7, N ν ≥ 7) can be used to send supernova alerts with very high confidence (about one false detection per century), and identify CCSN at a distance of (341 kpc → 269 kpc) with 50% probability. -Section 4.2: With a relaxed set of conditions of (m ≥ 7, N ν ≥ 6), SNe up to (370 kpc → 291 kpc) can be detected with less than one false CCSN detection per year. -Section 4.2: For example, for a number of detected events N ν = 5 a background origin can be excluded at 3.2 σ , while at least a corresponding number of events will be detected in 50% of cases from a 27 M CCSNe at a distance of (407 kpc → 322 kpc). .9] σ certainty that the signal was not produced by background.
• Change in the 5σ detection horizons, in case the arrival time of the burst is known exactly: -Section 4.2: The 5σ discovery horizon in this scenario reaches (400 kpc → 315 kpc) for a 27 M CCSN using m ≥ 7, and (300 kpc → 234 kpc) for the 9.6 M model.
• To reach a detection of one CCSN about every decade doubling the number of modules, the necessary noise reduction changes from a factor ∼ 70 to a factor ∼ 140: -Abstract: Increasing the number of sensors to 20,000 and reducing the optical background by a factor of (∼ 70 → ∼ 140) expands the range such that a CCSN detection rate of (0.    Table 4 -Conclusions: Increasing the number of installed modules to 20,000 and using pressure vessels with significantly reduced optical background could extend the range such that one CCSN (per decade → every ∼ 12 years) can be observed.
The conclusion from this work remains unchanged despite the reduced detection range: exploiting coincidences between detected photons within a segmented photosensor will significantly increase the sensitivity of sparsely instrumented neutrino telescopes to distant CCSNe.
Open Access This article is licensed under a Creative Commons Attribution 4.0 International License, which permits use, sharing, adaptation, distribution and reproduction in any medium or format, as long as you give appropriate credit to the original author(s) and the source, provide a link to the Creative Commons licence, and indicate if changes were made. The images or other third party material in this article (upper) and 20,000 (lower) mDOMs as a function of the false SN detection rate and a reduction in radioactive noise compared to standard mDOMs. The CCSN detection rates have been calculated using the estimated CCSNe population from [16] based on actual observations and scaled to the star formation rate are included in the article's Creative Commons licence, unless indicated otherwise in a credit line to the material. If material is not included in the article's Creative Commons licence and your intended use is not permitted by statutory regulation or exceeds the permitted use, you will need to obtain permission directly from the copyright holder. To view a copy of this licence, visit http://creativecomm ons.org/licenses/by/4.0/. Funded by SCOAP 3 . SCOAP 3 supports the goals of the International Year of Basic Sciences for Sustainable Development.