{"id":"845704fd-9ae3-41a8-b5a9-51f3464abf0f","arxiv_id":"2607.03943","paper_version":1,"verdict":"ACCEPT","confidence":"HIGH","novelty_score":6.0,"correctness_risk":"low","formal_verification":"none","parameter_count":3,"one_line_summary":"Attenuation of pre-supernova electron antineutrinos by local dark matter yields upper limits on the reduced DM–ν cross section of order 10^{-21} cm^{2}/GeV at detectors such as JUNO, Super-K and KamLAND.","lead":"Pre-supernova neutrinos from a nearby massive star can set upper limits on dark-matter–neutrino scattering via flux attenuation seen as missing inverse-beta-decay events. The limits give an independent MeV-energy cross-check on supernova-neutrino bounds and can test certain early-universe interaction hints.","discovery_kind":"new_application","skeptic_critique":{"model":"grok-4.5","headline":"No significant objection identified","rationale":"The paper is a clean phenomenological sensitivity study. Its strongest claim is simply that the listed detectors would set the quoted upper limits if a nearby pre-supernova flux is observed and attenuated. That claim follows directly from Eqs. (1)–(5) once the fluxes and detector parameters are accepted; both are taken from the literature and cross-checked against published event counts. The reader’s weakest assumption (constant local density, simple attenuation) is real but already acknowledged by the authors and does not invalidate the existence of the sensitivity numbers. Because the limits are independent of d⋆ (N_tot ∝ 1/d⋆^{2} cancels the linear d⋆ in \tau), and because the collapse-phase flux dominates, the numerical results are stable under the O(1) variations the authors themselves quote. No further load-bearing flaw is present, so the reader’s ACCEPT verdict with high confidence stands.","tokens_in":11395,"tokens_out":683,"duration_ms":5810,"concrete_test":"Recompute N_tot for Super-K, KamLAND and JUNO by integrating the tabulated d^{2}N\nu/dE\nu dt spectra of the 15 M⊙ normal-hierarchy model over the collapse-phase window (t < 0.1 s) with the IBD cross section of Eq. (2) and the detector parameters of Table I; verify that the resulting \tau^{2}σ limits on σχν/mχ match the published entries to within ~10 %. If they do, the headline numbers are robust under the paper’s own assumptions.","verdict_should_be":"UNCHANGED","load_bearing_attack":"The central claim is a transparent sensitivity estimate: a 2σ deficit of IBD events from pre-supernova ν̄e yields distance-independent upper limits on σχν/mχ of order (0.5–9)×10^{-21} cm^{2}/GeV (Table I, collapse-phase τ^{2}σ). The calculation rests on standard optical-depth attenuation (Eq. 3) with a constant local density, tabulated preSN fluxes from Ref. [30/47], and the usual IBD cross section. The reader correctly flags the constant-density assumption and the neglect of regeneration or a dark-disk component; the authors themselves already list these as caveats (Introduction points (iii)–(iv) and Sec. III) and quantify O(1) model dependence from progenitor mass and hierarchy. None of these assumptions is load-bearing for the existence of the quoted sensitivity numbers themselves; they only modulate the numerical reach by factors already stated. No internal inconsistency, circular reasoning, or hidden error appears in the derivation of Eqs. (1)–(5) or Table I.","agreement_with_reader":"agree"},"referee_report":{"model":"grok-4.5","summary":"The paper estimates the sensitivity of large-volume, low-threshold detectors (Super-K, KamLAND, JUNO) to dark-matter–neutrino scattering by computing the attenuation of the pre-supernova electron-antineutrino flux from a nearby massive star. Using tabulated fluxes for a 15 M☉ progenitor, the IBD cross section, and a simple optical-depth criterion τ_χ = 2/√N_tot (Eqs. 3–5), the authors derive distance-independent 2σ upper limits on the reduced cross section σ_χν/m_χ of order (0.5–9)×10^{-21} cm^{2}/GeV (Table I, collapse-phase events). They compare these MeV-scale limits with post-bounce SN sensitivities, SN1987A bounds, structure-formation constraints, and a Lyman-α hint, arguing that pre-supernova neutrinos offer a complementary probe of energy-dependent interactions and a cross-check that relies only on the local DM density.","tokens_in":11633,"tokens_out":1005,"duration_ms":21912,"significance":"If the quoted sensitivities are realized, the work supplies the first BSM application of pre-supernova neutrinos and a clean MeV-energy handle on DM–ν scattering that is independent of Galactic density-profile uncertainties. The calculation is transparent, uses publicly available stellar-evolution tables, and yields falsifiable, distance-independent numbers that can be directly compared with a future nearby core-collapse event. The discussion of energy dependence, failed supernovae, and dark-disk scenarios correctly identifies regimes in which pre-supernova limits become uniquely informative. These features make the result a useful addition to the literature even though the numerical reach is weaker than post-bounce SN bounds.","major_comments":[{"comment":"Sec. II.2, Eq. (3): The optical-depth formula assumes a spatially constant local density ρ_χ = 0.4 GeV cm^{-3} and pure attenuation (no regeneration or angular redistribution). For the τ_χ ∼ 1 criterion listed in Table I this approximation can overestimate the observable deficit; a short estimate of the size of regeneration effects, or an explicit statement that the quoted limits are optimistic under pure attenuation, is needed to keep the central claim quantitatively robust.","section":"Sec. II.2, Eq. (3)"},{"comment":"Sec. III and Fig. 2: The illustrative scaling σ_χν ∝ E_ν^{3.8} that is said to test the Lyman-α hint is not derived from any concrete mediator model. Either a brief particle-physics motivation for this power or a clearer disclaimer that the curve is purely phenomenological would prevent the figure from being over-interpreted as a realistic exclusion.","section":"Sec. III, Fig. 2"}],"minor_comments":[{"comment":"Abstract, second sentence: missing capital after the period (“Super-K. which we use”).","section":"Abstract"},{"comment":"Introduction, first paragraph: “apre-supernova” lacks a space; several other compound terms (preSNν, SNν) are introduced without a consistent definition list.","section":"Introduction"},{"comment":"Table I caption and last column: the four τ criteria are listed in braces without an explicit key; a short legend would improve readability.","section":"Table I"},{"comment":"Fig. 1 right panel: the vertical dashed line marking the collapse phase is not defined in the caption; a one-line explanation would help.","section":"Fig. 1"},{"comment":"Sec. II.1: the statement that backgrounds are “negligible” is asserted without a quantitative reference or residual-rate estimate for the time window used.","section":"Sec. II.1"}],"recommendation":"minor_revision","confidential_remarks":"The manuscript is a clean, first-of-its-kind sensitivity study that fits well in hep-ph. The central calculation is sound and the authors already flag the main caveats. Minor revision is sufficient; no deeper conceptual flaw is present."},"author_rebuttal":null,"desk_editor":{"model":"grok-4.5","letter":"This is the first quantitative look at pre-supernova neutrinos as a probe of DM–ν scattering. The authors take public 15 M⊙ flux tables, fold them through IBD at Super-K/KamLAND/JUNO, and convert a 2σ event deficit into distance-independent upper limits on σχν/mχ of order (0.5–9)×10^{-21} cm^{2}/GeV. That is new, correctly done, and useful as an MeV-scale cross-check and energy-dependence diagnostic relative to post-bounce SN and DSNB work.\n\nWhat they do well is keep the calculation transparent. Event rates (Eq. 1), the IBD cross section, and the optical-depth criterion (Eqs. 3–5) are standard and applied without hidden parameters. Systematics are shown to be sub-dominant; progenitor-mass and hierarchy variations are quantified as O(1) and partially offset by local-density uncertainty. They also flag the dark-disk and failed-SN cases where pre-SN could actually become competitive. The Lyman-α toy model (σ ∝ E^{3.8}) is illustrative rather than realistic, but it correctly shows why an MeV window can matter.\n\nSoft spots are minor and already stated by the authors: constant local density 0.4 GeV cm^{-3}, neglect of regeneration, and the practical rarity of a <100 pc progenitor. None of these breaks the existence of the quoted sensitivity numbers; they only shift the numerical reach by factors already discussed. Citation pattern is clean; no circularity.\n\nThis is for people already working on DM–ν interactions or SN neutrino phenomenology. It will not re-shape the field, but it is a solid, self-contained sensitivity study that deserves a serious referee rather than a desk reject. I would accept it for peer review and expect only light revision.","headline":"First clean pre-SN neutrino sensitivity to DM–ν scattering; transparent calculation, limited but real novelty, ready for referees.","tokens_in":12175,"tokens_out":476,"would_cite":true,"duration_ms":3936,"reading_group":"maybe","serious_thinker":"yes","would_accept_peer_review":true},"rs_alignment":null,"lean_confirmation":null,"pith_extraction":{"msc":[],"pacs":[],"model":"grok-4.5","headline":"Pre-supernova neutrinos can set MeV limits on dark-matter scattering through a simple deficit of inverse-beta-decay events.","keywords":["pre-supernova neutrinos","dark matter-neutrino scattering","inverse beta decay","optical depth","MeV neutrinos","attenuation","Lyman-alpha"],"falsifier":"If a nearby massive star collapses and the observed inverse-beta-decay counts at Super-K, KamLAND or JUNO match the no-dark-matter prediction within the quoted statistical errors, the claimed optical-depth limits are ruled out.","tokens_in":12316,"feed_emoji":"💥","tokens_out":612,"duration_ms":4742,"temperature":0.7,"pith_summary":"Massive stars emit a steady stream of MeV neutrinos for roughly a day before they collapse. If those neutrinos scatter off intervening dark matter, some of them leave the line of sight and never reach Earth, producing a measurable shortfall of inverse-beta-decay events in large, low-threshold detectors. The paper turns that shortfall into upper limits on the reduced dark-matter–neutrino cross section that sit near 10^{-21} cm^{2}/GeV. Although the numbers are weaker than the corresponding post-bounce supernova limits, they are independent of distance, rest only on the well-measured local dark-matter density, and probe a lower energy window where resonant or light-mediator models can look completely different. The same data can also test a reported cosmological hint that dark-matter–neutrino scattering suppresses small-scale structure.","feed_headline":"Pre-supernova neutrinos set MeV limits on dark-matter scatter","feed_subtitle":"A simple event deficit at Super-K, KamLAND and JUNO probes cross sections near 10^{-21} cm^{2}/GeV","key_machinery":"Optical depth for attenuation: τχ = ρχ (σχν/mχ) d⋆, set equal to twice the fractional statistical uncertainty of the expected event count; the resulting bound on σχν/mχ is then independent of distance because the event rate scales as 1/d⋆^{2}.","core_discovery":"A 2σ deficit of inverse-beta-decay events from pre-supernova electron antineutrinos yields upper limits on the reduced cross section σχν/mχ of order (0.5–9)×10^{-21} cm^{2}/GeV that are independent of progenitor distance and that uniquely sample the MeV energy band.","pith_inferences":[],"forward_implications":[],"fun_headline_variants":["Pre-supernova neutrinos limit DM-neutrino scatter via MeV event deficit","IBD shortfall from pre-collapse neutrinos bounds dark matter cross section","KamLAND and Super-K deficits probe MeV dark matter-neutrino interactions","Pre-SN neutrino attenuation sets σχν/mχ limits near 10^{-21} cm²/GeV","Unique MeV probe of DM-neutrino scattering from pre-supernova flux"],"cache_read_input_tokens":128,"weakest_assumption_plain":"The calculation assumes a perfectly uniform local dark-matter density of 0.4 GeV per cubic centimetre and pure exponential attenuation, with no regeneration or dark-disk contribution.","fun_headline_variants_meta":{"raw":{"variants":["Pre-supernova neutrinos limit DM-neutrino scatter via MeV event deficit","IBD shortfall from pre-collapse neutrinos bounds dark matter cross section","KamLAND and Super-K deficits probe MeV dark matter-neutrino interactions","Pre-SN neutrino attenuation sets σχν/mχ limits near 10^{-21} cm²/GeV","Unique MeV probe of DM-neutrino scattering from pre-supernova flux"]},"model":"grok-4.5","effort":"low","cost_usd":0.006328,"raw_usage":{"total_tokens":1598,"prompt_tokens":719,"num_sources_used":0,"completion_tokens":94,"cost_in_usd_ticks":63280000,"prompt_tokens_details":{"text_tokens":719,"audio_tokens":0,"image_tokens":0,"cached_tokens":256},"completion_tokens_details":{"audio_tokens":0,"reasoning_tokens":785,"accepted_prediction_tokens":0,"rejected_prediction_tokens":0}},"tokens_in":719,"tokens_out":94,"duration_ms":5608,"temperature":1.0,"reasoning_tokens":785,"cache_read_input_tokens":256,"cache_creation_input_tokens":0},"cache_creation_input_tokens":0},"created_at":"2026-07-11T22:49:48.566605+00:00","model_set":{"reader":"grok-4.5"},"falsifier":"If a nearby massive star collapses and the observed inverse-beta-decay counts at Super-K, KamLAND or JUNO match the no-dark-matter prediction within the quoted statistical errors, the claimed optical-depth limits are ruled out.","supporting_citations":[],"review_version":1}