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A shipboard scintillator finds sea-level cosmic-ray rate lowest near 7°N, about 16% below the rate at Trieste.

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2026-07-11 21:00 UTC pith:R5BM7YO7

load-bearing objection Clean modern muon latitude survey on a single instrument; 16% effect and ~7°N minimum are solid, Forbush ratios check out, work is incremental but usable.

arxiv 2607.04197 v1 pith:R5BM7YO7 submitted 2026-07-05 astro-ph.IM astro-ph.SRphysics.ins-det

The Amerigo Vespucci as a traveling laboratory for studying the cosmic-ray fluxes at sea level

Davide Cerasole , Federica Cuna , Gaia De Palma , Riccardo Di Tria , Leonardo Di Venere , Fabio Gargano , Mario Giliberti , Francesco Licciulli
show 8 more authors
Antonio Liguori Pierpaolo Loizzo Francesco Loparco Leonarda Lorusso Mario Nicola Mazziotta Giuliana Panzarini Roberta Pillera Davide Serini
This is my paper
classification astro-ph.IM astro-ph.SRphysics.ins-det PACS 96.50.S-94.20.wq95.55.Vj
keywords cosmic rayssea-level muon rategeomagnetic cutofflatitude effectForbush decreaseplastic scintillatorAmerigo Vespucci
verification ladder T0 review T1 audit T2 compute T3 formal T4 reserved

The pith

A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.

A plastic-scintillator counter rode the Italian Navy tall ship Amerigo Vespucci from Darwin to Trieste (and then through the Mediterranean) and recorded the rate of secondary cosmic rays that reach the sea surface. Across latitudes from 15°S to 45°N the rate is lowest near geographic latitude 7°N—roughly 16% below the value measured at Trieste—exactly where the geomagnetic cutoff rigidity is highest. The same continuous record also registers seven Forbush decreases caused by solar coronal-mass ejections; the muon-sensitive drops are typically a factor of three smaller than the corresponding drops seen by a high-latitude neutron monitor. Because a single instrument operated under stable conditions for many months, the data set cleanly separates the slow geomagnetic latitude effect from the rapid solar-driven transients, confirming the classic latitude surveys of the mid-twentieth century with modern electronics and continuous environmental monitoring.

Core claim

The sea-level cosmic-ray rate measured by a two-tile plastic scintillator on the Vespucci reaches its minimum near geographic latitude 7°N and is about 16% lower there than at Trieste (~45°N); the same data set also captures seven Forbush decreases whose amplitudes are typically a factor of three smaller than those recorded by the Oulu neutron monitor.

What carries the argument

The phenomenological rate model (Eq. 1) that multiplies a sum of Forbush-decrease templates (start times, rise and fall times fixed to the Oulu neutron-monitor fit) by either a simple latitude term L(λ)=1−α cos^γ(λ−λ0) or the Dorman cutoff function R(Rc)=1−exp(−A Rc^−k); the free amplitude parameters then isolate the geomagnetic latitude effect from solar modulation.

Load-bearing premise

The assumption that fixing the Forbush start, rise and fall times to the Oulu neutron-monitor values fully removes solar modulation so that the remaining latitude dependence is purely geomagnetic.

What would settle it

An independent continuous muon-rate measurement spanning the same 7°N–45°N corridor during a period of low solar activity that either recovers a 16% amplitude and λ0≈7.8°N or finds a statistically different minimum location or depth.

Watch this falsifier — get emailed when new claim-graph text bears on it.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit.

Referee Report

0 major / 5 minor

Summary. The paper reports sea-level cosmic-ray rates measured with a two-tile plastic scintillator coincidence detector installed on the Italian Navy tall ship Amerigo Vespucci. Data were collected from Darwin (Oct 2024) to Trieste (Mar 2025) over latitudes 15°S–45°N, then continued on the Mediterranean leg to Genova (Jun 2025). After inclination and barometric corrections, the lowest azimuth-averaged rate occurs near 7°N and is ~16% below the Trieste value. Seven Forbush decreases are identified by fixing start/rise/fall times to the independent Oulu neutron monitor and floating only amplitudes on the Vespucci data; muon amplitudes are typically a factor ~3 smaller than neutron-monitor amplitudes. The same latitude and Forbush patterns are recovered on the Mediterranean leg and with the independent ALBERT muon counter at Bari. Rates are also shown versus IGRF vertical cutoff rigidity and fitted with a Dorman function.

Significance. A continuous, single-instrument sea-level muon survey spanning a wide latitude range during Solar Cycle 25 maximum is rare and valuable. The work cleanly separates geomagnetic latitude effects from solar modulation by anchoring Forbush timing to an independent neutron monitor, recovers a CR-equator location (~7°N) consistent with historical surveys, and quantifies the weaker muon response relative to neutrons both for latitude and for Forbush events. Cross-checks with the Mediterranean leg and with ALBERT strengthen the observational claim. The data set is a useful modern reference for geomagnetic cutoff and solar-modulation studies.

minor comments (5)
  1. Methods, barometric coefficient: β = (1.52 ± 0.48) × 10^{-3} hPa^{-1} has a large relative uncertainty. A short statement on how this uncertainty propagates into the final rates (or into the 16% amplitude) would help the reader assess residual systematics.
  2. Eq. (3) and surrounding text: the latitude term is correctly described as phenomenological; a one-sentence note that it is used only for description (not for physical inference of cutoff) would further clarify its role relative to the Dorman fit of Eq. (5).
  3. Results, Mediterranean tour: the ~3% rate drop after relocating the detector in Trieste is attributed to additional overburden. A brief estimate of the material thickness or a comparison of the two positions would make this correction more transparent.
  4. Fig. 11 bottom panel: the Sense HAT vertical geomagnetic field shows a constant offset relative to IGRF. Mentioning that the offset does not affect the rate analysis (which uses IGRF cutoffs) would avoid reader confusion.
  5. Abstract and Introduction: a few minor typographical inconsistencies (e.g., spacing around degree symbols, “Thelowestrate”) should be cleaned in production.

Circularity Check

1 steps flagged

No significant circularity: observational latitude effect and Forbush amplitudes are measured data, not forced by construction; phenomenological fits are descriptive only.

specific steps
  1. self citation load bearing [Mediterranean Tour section; Fig. 8 and surrounding text]
    "In Fig. 8 we also show the rate measured with the CR detector “ALBERT” [13] installed at the INFN Bari. In this case we find that the amplitude decrease coefficient associated to the Forbush event is of about 0.08, similar to the result achieved with the Vespucci data."

    ALBERT is the authors’ own portable muon counter (Pillera et al., ICRC 2023). Its use as a contemporaneous cross-check for the June 2025 Forbush amplitude is a minor self-citation. It is not load-bearing for the world-tour 16% latitude claim or the location of the minimum at ~7°N, which rest on the Vespucci data alone and on comparison with the independent Oulu NM.

full rationale

The central claims (minimum rate at ~7°N, ~16% lower than Trieste; seven Forbush decreases with amplitudes ~1/3 of Oulu NM) are direct measurements of the Vespucci scintillator rates after standard inclination and barometric corrections. Forbush start/rise/fall times are taken from the independent Oulu neutron monitor and held fixed while only amplitudes are floated on Vespucci data—an ordinary multi-instrument procedure that does not force the reported 16% latitude amplitude. The latitude term L(λ)=1−α cos^γ(λ−λ0) and the Dorman cutoff function are explicitly phenomenological fits to the same rates; they organize the data but are not presented as first-principles predictions. The Mediterranean leg and the independent ALBERT Bari counter recover consistent latitude and Forbush ratios, providing external cross-checks. Minor self-reference to ALBERT is not load-bearing. Residuals are Gaussian with zero mean. Score 1 reflects only the trivial self-citation of the authors’ own ALBERT instrument, which does not underwrite the primary result.

Axiom & Free-Parameter Ledger

7 free parameters · 4 axioms · 0 invented entities

The central claims rest on standard geomagnetic and atmospheric physics plus a small set of free parameters introduced to describe the observed rate. No new physical entities are postulated. The phenomenological latitude and Dorman functions are ad-hoc functional forms fitted to the data; their parameters are therefore free. The IGRF model and the Oulu neutron-monitor time series are external domain inputs treated as given.

free parameters (7)
  • latitude amplitude α = 0.170 ± 0.001
    Fitted amplitude of the phenomenological latitude term (Eq. 3); best-fit value 0.170±0.001.
  • latitude of minimum λ0 = 7.80 ± 0.09 deg N
    Fitted geographic latitude of the rate minimum; best-fit 7.80±0.09°N.
  • latitude plateau exponent γ = 7.95 ± 0.16
    Fitted exponent controlling the width of the latitude plateau; best-fit 7.95±0.16.
  • Dorman A = 9.21 ± 0.22
    Amplitude parameter of the Dorman cutoff function (Eq. 5); best-fit 9.21±0.22.
  • Dorman k = 0.575 ± 0.007
    Exponent of the Dorman cutoff function; best-fit 0.575±0.007.
  • barometric coefficient β = (1.52 ± 0.48)×10^-3 hPa^-1
    Measured in Darwin before departure; used to correct all rates (Eq. 6).
  • Forbush amplitudes a_j (7 events) = range ~1.1% to ~4%
    Seven free amplitudes floated on the Vespucci data after fixing start/rise/fall times to Oulu.
axioms (4)
  • domain assumption The geomagnetic field is adequately described by the IGRF model at epoch 2024.9 for computing vertical cutoff rigidities at 20 km altitude.
    Used to produce the cutoff map (Fig. 5) and the rate-versus-cutoff plot (Fig. 6).
  • domain assumption The Oulu neutron-monitor count rate provides an independent, latitude-independent monitor of solar modulation (Forbush decreases).
    Start times, rise times and fall times of the seven Forbush events are fixed to the Oulu fit before fitting Vespucci amplitudes.
  • domain assumption Secondary particles reaching sea level are predominantly muons (plus a reduced electron/positron fraction) whose rate is proportional to the primary flux above the local geomagnetic cutoff.
    Stated in the Introduction and Methods; underpins the interpretation of the scintillator coincidence rate as a proxy for primary CR intensity.
  • ad hoc to paper The phenomenological forms L(λ)=1-α cos^γ(λ-λ0) and the Dorman function adequately capture the latitude and cutoff dependence after Forbush subtraction.
    Explicitly introduced in Eqs. 3 and 5; the paper notes that the latitude term 'is just a phenomenological model … not based on any physical consideration.'

pith-pipeline@v1.1.0-grok45 · 19464 in / 3609 out tokens · 26606 ms · 2026-07-11T21:00:47.719514+00:00 · methodology

0 comments
read the original abstract

We have installed and operated a plastic scintillator detector counter to measure the flux of cosmic radiation during the 2023-2025 tour of the historical vessel Amerigo Vespucci. The Vespucci is the oldest ship of the Italian Navy and serves as a training vessel for Navy cadets. During its tour, some experiments were hosted onboard the vessel, providing unique opportunities for scientists working in different fields. We installed our detector upon the Vespucci's departure from Darwin in early October 2024. The detector collected cosmic-ray data during the journey from Darwin to Trieste, where the worldwide tour ended in March 2025. After about one month of stop in Trieste, the ship continued its tour in the Mediterranean sea, and arrived in Genova on June 10, 2025. We performed measurements of the cosmic radiation reaching the sea level across a wide latitude range, from 15{\deg} S to about 45{\deg} N. The lowest rate (averaged over all azimuth angles) was measured at a geographic latitude of about 7{\deg} N, and was about 16% less than the highest value, which was measured at Trieste, the northernmost location of the journey. Latitude effects on the cosmic radiation flux at sea level are due to the quasi-dipole geomagnetic field configuration, tilted by an angle of about 11{\deg} with respect to Earth's rotational axis.

Figures

Figures reproduced from arXiv: 2607.04197 by Antonio Liguori, Davide Cerasole, Davide Serini, Fabio Gargano, Federica Cuna, Francesco Licciulli, Francesco Loparco, Gaia De Palma, Giuliana Panzarini, Leonarda Lorusso, Leonardo Di Venere, Mario Giliberti, Mario Nicola Mazziotta, Pierpaolo Loizzo, Riccardo Di Tria, Roberta Pillera.

Figure 1
Figure 1. Figure 1: Cosmic-ray rate map measured on board the Vespucci vessel [PITH_FULL_IMAGE:figures/full_fig_p006_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: Top panel: Cosmic-ray rates measured by the detector on board [PITH_FULL_IMAGE:figures/full_fig_p007_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: Cosmic-ray rates measured by the Oulu detector as a function of [PITH_FULL_IMAGE:figures/full_fig_p008_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: Distributions of fractional residual (in units of %) between the [PITH_FULL_IMAGE:figures/full_fig_p009_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: Vertical cutoff rigidity evaluated from the IGRF geomagnetic field [PITH_FULL_IMAGE:figures/full_fig_p010_5.png] view at source ↗
Figure 6
Figure 6. Figure 6: Cosmic-ray rate measured by the Vespucci detector as a function [PITH_FULL_IMAGE:figures/full_fig_p011_6.png] view at source ↗
Figure 7
Figure 7. Figure 7: Cosmic-ray rate map measured on board the Vespucci vessel during [PITH_FULL_IMAGE:figures/full_fig_p013_7.png] view at source ↗
Figure 8
Figure 8. Figure 8: Top panels: CR rates measured by the Oulu NM, by the [PITH_FULL_IMAGE:figures/full_fig_p014_8.png] view at source ↗
Figure 9
Figure 9. Figure 9: Cosmic-ray rate measured by the Vespucci detector from Trieste [PITH_FULL_IMAGE:figures/full_fig_p015_9.png] view at source ↗
Figure 9
Figure 9. Figure 9: The observed data rate are still fitted with the Dorman function in [PITH_FULL_IMAGE:figures/full_fig_p016_9.png] view at source ↗
Figure 10
Figure 10. Figure 10: Left panel: the detector box installed on a desk in the Vespucci [PITH_FULL_IMAGE:figures/full_fig_p019_10.png] view at source ↗
Figure 11
Figure 11. Figure 11: Pressure, temperature and vertical geomagnetic field component [PITH_FULL_IMAGE:figures/full_fig_p020_11.png] view at source ↗

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