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REVIEW 2 major objections 5 minor 48 references

IceCube neutrinos map Earth's density shells and recover its mass and moment of inertia via weak interactions alone.

Reviewed by Pith at T0; open to challenge. T0 means a machine referee read the full paper against a public rubric. the ladder, T0–T4 →

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T0 review · grok-4.5

2026-07-12 08:01 UTC pith:4RH5OXHB

load-bearing objection Solid order-of-magnitude upgrade of IceCube Earth tomography; mass and MOI posteriors are new, consistent with PREM/gravity, and the analysis is carefully done. the 2 major comments →

arxiv 2607.02644 v2 pith:4RH5OXHB submitted 2026-07-02 astro-ph.HE astro-ph.EPhep-exphysics.geo-ph

High-Energy Neutrino Tomography of the Earth's Interior with IceCube

The IceCube Collaboration , R. Abbasi , M. Ackermann , J. Adams , J. A. Aguilar , M. Ahlers , J.M. Alameddine , S. Ali
show 412 more authors
N. M. Amin K. Andeen C. Arg\"uelles S. Athanasiadou S. N. Axani R. Babu X. Bai A. Balagopal V. S. W. Barwick V. Basu R. Bay J. J. Beatty J. Becker Tjus P. Behrens J. Beise C. Bellenghi S. Benkel S. BenZvi D. Berley E. Bernardini D. Z. Besson E. Blaufuss L. Bloom S. Blot F. Bontempo J. Y. Book Motzkin C. Boscolo Meneguolo S. B\"oser O. Botner J. B\"ottcher J. Braun B. Brinson Z. Brisson-Tsavoussis L. Brusa R. T. Burley D. Butterfield K. Carloni J. Carpio N. Chau Y. C. Chen Z. Chen D. Chirkin S. Choi A. Chubarov B. A. Clark G. H. Collin D. A. Coloma Borja A. Connolly J. M. Conrad D. F. Cowen C. De Clercq J. J. DeLaunay D. Delgado T. Delmeulle S. Deng P. Desiati K. D. de Vries G. de Wasseige T. DeYoung J. C. D\'iaz-V\'elez S. DiKerby T. Ding M. Dittmer A. Domi L. Draper L. Dueser D. Durnford K. Dutta M. A. DuVernois T. Ehrhardt L. Eidenschink A. Eimer C. Eldridge P. Eller E. Ellinger D. Els\"asser R. Engel H. Erpenbeck W. Esmail S. Eulig J. Evans P. A. Evenson K. L. Fan K. Fang K. Farrag A. Fattorini A. R. Fazely A. Fedynitch N. Feigl C. Finley D. Fox A. Franckowiak S. Fukami P. F\"urst J. Gallagher E. Ganster A. Garcia M. Garcia E. Genton L. Gerhardt A. Ghadimi C. Glaser T. Gl\"usenkamp J. G. Gonzalez S. Goswami A. Granados D. Grant S. J. Gray S. Griffin S. Griswold K. M. Groth D. Guevel C. G\"unther P. Gutjahr C. Ha A. Hallgren L. Halve F. Halzen L. Hamacher M. Handt K. Hanson J. Hardin A. A. Harnisch P. Hatch A. Haungs J. H\"au{\ss}ler K. Helbing J. Hellrung B. Henke L. Hennig F. Henningsen L. Heuermann R. Hewett N. Heyer S. Hickford A. Hidvegi C. Hill G. C. Hill R. Hmaid K. D. Hoffman A. Hollnagel D. Hooper S. Hori K. Hoshina M. Hostert W. Hou M. Hrywniak T. Huber K. Hultqvist K. Hymon A. Ishihara W. Iwakiri M. Jacquart S. Jain O. Janik M. Jansson M. Jin N. Kamp D. Kang W. Kang A. Kappes L. Kardum T. Karg A. Karle A. Katil M. Kauer J. L. Kelley M. Khanal A. Khatee Zathul A. Kheirandish T. Kim H. Kimku F. Kirchner J. Kiryluk C. Klein S. R. Klein Y. Kobayashi S. Koch A. Kochocki R. Koirala H. Kolanoski T. Kontrimas L. K\"opke C. Kopper D. J. Koskinen P. Koundal M. Kowalski T. Kozynets A. Kravka N. Krieger T. Krishnan K. Kruiswijk E. Krupczak E. Kun N. Kurahashi C. Lagunas Gualda L. Lallement Arnaud M. J. Larson F. Lauber J. P. Lazar K. Leonard DeHolton A. Leszczy\'nska C. Li J. Liao C. Lin Q. R. Liu Y. T. Liu M. Liubarska C. Love L. Lu F. Lucarelli W. Luszczak Y. Lyu M. Macdonald E. Magnus Y. Makino E. Manao S. Mancina A. Mand I. C. Mari\c{s} S. Marka Z. Marka L. Marten I. Martinez-Soler R. Maruyama J. Mauro F. Mayhew F. McNally K. Meagher A. Medina M. Meier Y. Merckx L. Merten S. Minji J. Mitchell L. Molchany S. Mondal T. Montaruli R. W. Moore Y. Morii A. Mosbrugger D. Mousadi E. Moyaux T. Mukherjee M. Nakos U. Naumann R. Neshat L. Neste M. Neumann H. Niederhausen M. U. Nisa K. Noda A. Noell A. Novikov A. Obertacke V. O'Dell A. Olivas R. Orsoe J. Osborn E. O'Sullivan B. Owens V. Palusova H. Pandya A. Parenti C. Parisel N. Park V. Parrish E. N. Paudel L. Paul C. P\'erez de los Heros T. Pernice T. C. Petersen J. Peterson S. Pick M. Plum A. Pont\'en V. Poojyam B. Pries R. Procter-Murphy G. T. Przybylski L. Pyras C. Raab J. Rack-Helleis N. Rad M. Ravn K. Rawlins Z. Rechav A. Rehman I. Reistroffer E. Resconi C. D. Rho W. Rhode L. Ricca B. Riedel A. Rifaie E. J. Roberts S. Rodan M. Rongen A. Rosted C. Rott T. Ruhe L. Ruohan D. Ryckbosch J. Saffer D. Salazar-Gallegos P. Sampathkumar A. Sandrock G. Sanger-Johnson M. Santander S. Sarkar M. Scarnera M. Schaufel H. Schieler S. Schindler L. Schlickmann B. Schl\"uter F. Schl\"uter N. Schmeisser T. Schmidt A. Scholz F. G. Schr\"oder S. Schwirn S. Sclafani D. Seckel L. Seen M. Seikh S. Seunarine P. A. Sevle Myhr R. Shah S. Shah S. Shefali N. Shimizu B. Skrzypek R. Snihur J. Soedingrekso D. Soldin P. Soldin G. Sommani D. Song C. Spannfellner G. M. Spiczak C. Spiering J. Stachurska M. Stamatikos T. Stanev T. Stezelberger T. St\"urwald T. Stuttard G. W. Sullivan I. Taboada S. Ter-Antonyan A. Terliuk A. Thakuri M. Thiesmeyer W. G. Thompson J. Thwaites S. Tilav K. Tollefson J. A. Torres S. Toscano D. Tosi K. Upshaw A. Vaidyanathan N. Valtonen-Mattila J. Valverde J. Vandenbroucke T. Van Eeden N. van Eijndhoven L. Van Rootselaar J. van Santen J. Vara F. Varsi M. Velazquez M. Venugopal M. Vereecken S. Vergara Carrasco S. Verpoest D. Veske A. Vijai J. Villarreal C. Walck A. Wang E. H. S. Warrick C. Weaver P. Weigel A. Weindl J. Weldert A. Y. Wen C. Wendt J. Werthebach M. Weyrauch N. Whitehorn C. H. Wiebusch D. R. Williams L. Witthaus G. Wrede X. W. Xu J. P. Yanez Y. Yao E. Yildizci S. Yoshida F. Yu S. Yu T. Yuan S. Yun-C\'arcamo A. Zander Jurowitzki A. Zegarelli S. Zhang Z. Zhang P. Zhelnin P. Zilberman C. Zilleruelo Ca\~nas
This is my paper
classification astro-ph.HE astro-ph.EPhep-exphysics.geo-ph
keywords neutrino tomographyEarth density profileIceCubemuon neutrinosEarth massmoment of inertiaweak interactionPREM
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.

This paper shows that the energy- and zenith-dependent attenuation of high-energy neutrinos that have crossed the Earth can be turned into a measurement of the planet's radial density profile. Using 10.7 years of IceCube muon-track data, the collaboration fits a concentric-shell density model while floating flux, cross-section, detector and ice systematics. From the resulting density posteriors they extract the Earth's total mass and polar moment of inertia as measured by neutrinos. The values are consistent with the seismological PREM model and with gravitational determinations, yet rest on the weak force rather than gravity or elasticity. The result establishes neutrinos as a complementary, independent probe of planetary interiors.

Core claim

From the posterior densities of five (and eight) concentric shells fitted to the zenith- and energy-dependent suppression of upgoing atmospheric and astrophysical neutrinos, the Earth's mass and polar moment of inertia are recovered with the highest precision yet achieved through weak interactions; both quantities are statistically consistent with PREM and gravitational reference values.

What carries the argument

Energy- and zenith-dependent neutrino attenuation through a concentric uniform-density shell model, jointly fitted with 37 nuisance parameters via MCMC; the resulting density samples are integrated to give mass and moment of inertia under spherical symmetry.

Load-bearing premise

The Standard-Model neutrino-nucleon cross section is assumed known to a few percent, so residual energy-dependent biases are absorbed into the shell densities rather than treated as free physics.

What would settle it

A future higher-statistics measurement (or an independent cross-section determination) that drives the neutrino-derived mass or moment of inertia outside the present 95 percent highest-posterior-density intervals while PREM remains fixed would falsify the claim of consistency.

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

2 major / 5 minor

Summary. The paper reports a measurement of the Earth’s radial density profile from the energy- and zenith-dependent attenuation of upgoing muon neutrinos in 10.7 years of IceCube data (500 GeV–100 TeV). The Earth is parametrized as five (or eight) concentric uniform-density shells whose densities are free parameters with flat nonnegative priors; 37 nuisance parameters cover flux, CSMS NLO cross-section, detector, and ice systematics. MCMC sampling of the joint posterior yields shell-density constraints that are statistically consistent with PREM-averaged values. From the same posterior samples the authors derive the Earth’s mass (mode 7.25 imes10^24 kg, 68 % HPD [6.31, 8.31] imes10^24 kg) and polar moment of inertia (mode 1.05 imes10^38 kg m^{2}, 68 % HPD [9.04 imes10^37, 1.24 imes10^38] kg m^{2}), both of which contain the gravitational/PREM reference values inside the 95 % HPD. Blind staged unblinding, a posterior-predictive p-value of 16 %, and an explicit comparison of fits with and without near-horizontal events are used to support the claim that these are the most precise weak-interaction determinations of the two global quantities to date.

Significance. If the result holds, the work supplies an independent, weak-interaction probe of planetary bulk properties that is complementary to gravity and seismology. The order-of-magnitude increase in statistics relative to Donini et al. (2019), the blind analysis protocol, the documented MCMC convergence criteria, and the posterior-predictive goodness-of-fit test constitute a clear methodological advance. The derived mass and moment-of-inertia posteriors are falsifiable against future gravitational or seismic determinations and against next-generation neutrino-telescope data. The measurement therefore strengthens the case that high-energy neutrino attenuation can become a precision geophysical tool once detector and cross-section systematics improve.

major comments (2)
  1. Methods and §I: the claim that nuclear shadowing and non-isoscalarity are “adequately described” by the two attenuation nuisance parameters (νAtt, ν̄Att) rests on a single EPPS21 study whose quantitative impact on the final mass and MOI posteriors is not shown. A short table or figure quantifying the shift in the mass and MOI modes when the nuclear-PDF correction is turned on (or when a non-isoscalar target is used) would make the residual systematic fully transparent and would strengthen the central consistency claim.
  2. Fig. 3 and Table I: the posterior modes for mass and MOI lie ~20–30 % above the gravitational/PREM references, with only 6–9 % of the posterior mass below those values. While the 95 % HPD still covers the references, the paper should state more explicitly whether this mild upward bias is expected from the violin ensembles of PREM-based pseudo-data or whether it could indicate a residual energy-dependent cross-section or flux mismodelling that is partially absorbed into the outer-shell densities.
minor comments (5)
  1. Fig. 1 caption: the phrase “exaggerated by a factor of 10 for illustrative purposes” should specify whether the exaggeration is applied to the rate difference or to the absolute rate; the present wording is ambiguous.
  2. Table I: the PREM densities used for normalization are given only in parentheses in the row labels; a separate column would improve readability.
  3. Supplementary Fig. 9: the caption states that mass or MOI is fixed to the reference values, but the numerical values used are not restated; adding them would make the figure self-contained.
  4. Eq. (1): the structure-function definitions in Eq. (2) are given only for neutrinos at leading order; a brief note that the NLO CSMS calculation used for the actual attenuation includes the corresponding antineutrino and higher-order terms would avoid confusion.
  5. Methods: the statement that tau regeneration is “negligibly small compared to uncertainties on the inferred Earth densities” would be more convincing if a one-sentence quantitative bound (e.g., “<2 % on column depth for E < 100 TeV”) were supplied.

Circularity Check

0 steps flagged

No significant circularity: shell densities are free parameters with flat priors; mass and MOI are derived posteriors, not inputs; PREM is used only for comparison and pseudo-data ensembles.

full rationale

The central claim is an inference of Earth's radial density profile from the energy- and zenith-dependent attenuation of IceCube upgoing muon tracks, followed by derivation of mass and polar moment of inertia from those density posteriors. The paper parametrizes the Earth as concentric uniform-density shells with nonnegative uniform priors, jointly samples them with 37 nuisance parameters (flux, CSMS cross-section scalings, ice/DOM systematics) via MCMC, and reports posterior modes and HPD intervals. PREM densities appear only as a comparison curve, as the mean of the statistical-ensemble violins generated from PREM-averaged shells, and as a normalization reference in Table I; they are not imposed as constraints on the primary fit (the constrained-mass/MOI exercise of Fig. 9 is presented separately as a diagnostic). Mass and MOI are computed after the fact from the free density samples under spherical symmetry and are compared to independent gravitational/PREM values; the gravitational mass and PREM MOI lie inside the 95 % HPDs. The CSMS NLO cross section is an external Standard-Model input whose residual nuclear effects are shown (via EPPS21 tests) to be absorbed by the two attenuation nuisance parameters; this is ordinary model dependence, not circularity. Self-citations to earlier IceCube flux, cross-section, and reconstruction papers supply the data sample and nuisance model but do not force the density result. Blind staging, posterior-predictive p = 16 %, and the order-of-magnitude statistics gain over Donini et al. further confirm that the result is data-driven rather than definitional. No step reduces a claimed prediction to a fitted input or to a self-citation uniqueness theorem by construction.

Axiom & Free-Parameter Ledger

3 free parameters · 4 axioms · 0 invented entities

The central claim rests on the Standard-Model DIS cross section, a concentric-shell density parametrization, and a large set of floated nuisance parameters that absorb flux, ice, and detector uncertainties. No new physical entities are postulated; the free parameters are the shell densities themselves plus the 37 systematics.

free parameters (3)
  • five (or eight) shell densities
    Uniform non-negative priors; posterior modes and 68 % HPD intervals are the primary result (Table I, Fig. 2).
  • 37 nuisance parameters (Norm, DOMeff, Ice A0-4, Ice Phs1-4, Hole Ice, DaemonFlux hadronic and GSF parameters, astrophysi
    Floated simultaneously with densities; priors listed in Table II; dominate the systematic budget.
  • astrophysical flux normalization and spectral indices
    Broken power-law parameters with Gaussian priors taken from orthogonal IceCube samples; largest single systematic contribution according to the text.
axioms (4)
  • domain assumption CSMS NLO neutrino-nucleon cross section (HERA PDFs) is accurate to a few percent in the 0.5-100 TeV range
    Used as the baseline attenuation kernel; nuclear corrections tested and claimed sub-dominant (Methods).
  • ad hoc to paper Earth density can be approximated by concentric uniform-density spherical shells
    Five- and eight-shell models with boundaries at core-mantle and equal radial spacing; mass and MOI derived under spherical symmetry.
  • domain assumption Atmospheric and astrophysical neutrino fluxes are adequately described by DaemonFlux + broken power law once nuisance parameters are floated
    Standard IceCube modeling; priors informed by external measurements.
  • domain assumption Fixed nuclear composition (isoscalar nucleons) for converting mass density to nucleon number density
    Stated in Methods; non-isoscalarity noted as future work.

pith-pipeline@v1.1.0-grok45 · 29986 in / 2354 out tokens · 27657 ms · 2026-07-12T08:01:12.592173+00:00 · methodology

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read the original abstract

The Earth's interior reflects its geological evolution, from accretion to present-day dynamics. Its structure drives the geodynamo in the outer core, generating the magnetic field that shields the surface from charged cosmic radiation. The primary observables of the Earth's interior are its radial density distribution and derived quantities such as its mass and moment of inertia. These have traditionally been inferred from gravity and seismic wave propagation, which probe the macroscopic response of matter to gravitational and elastic forces. Here we instead constrain the Earth's density profile using high-energy neutrinos observed by the IceCube Neutrino Observatory at the South Pole. We analyze 10.7 years of predominantly muon-neutrino data spanning 500 GeV--100 TeV, including atmospheric neutrinos produced by cosmic-ray interactions in the Earth's atmosphere and the diffuse astrophysical neutrino flux. Neutrino attenuation depends on both the traversed column density and neutrino energy. By measuring the zenith- and energy-dependent flux suppression, we infer the Earth's radial density profile by fitting a concentric uniform-density shell model that incorporates neutrino fluxes, interaction cross sections, detector response, and glacial-ice systematic uncertainties. From the resulting density posteriors, we derive the Earth's mass and polar moment of inertia as measured by neutrinos. These are the most precise weak-interaction measurements of these quantities to date and are consistent with the Preliminary Reference Earth Model and independent gravitational determinations. Our results demonstrate that neutrinos provide a novel probe of planetary interiors via a distinct physical interaction, complementing gravity and seismology. With improved detectors and precision, neutrinos will further contribute to a multifaceted understanding of the Earth's structure.

Figures

Figures reproduced from arXiv: 2607.02644 by A. A. Harnisch, A. Balagopal V., A. Chubarov, A. Connolly, A. Domi, A. Eimer, A. Fattorini, A. Fedynitch, A. Franckowiak, A. Garcia, A. Ghadimi, A. Granados, A. Hallgren, A. Haungs, A. Hidvegi, A. Hollnagel, A. Ishihara, A. Kappes, A. Karle, A. Katil, A. Khatee Zathul, A. Kheirandish, A. Kochocki, A. Kravka, A. Leszczy\'nska, A. Mand, A. Medina, A. Mosbrugger, A. Noell, A. Novikov, A. Obertacke, A. Olivas, A. Parenti, A. Pont\'en, A. Rehman, A. R. Fazely, A. Rifaie, A. Rosted, A. Sandrock, A. Scholz, A. Terliuk, A. Thakuri, A. Vaidyanathan, A. Vijai, A. Wang, A. Weindl, A. Y. Wen, A. Zander Jurowitzki, A. Zegarelli, B. A. Clark, B. Brinson, B. Henke, B. Owens, B. Pries, B. Riedel, B. Schl\"uter, B. Skrzypek, C. Arg\"uelles, C. Bellenghi, C. Boscolo Meneguolo, C. De Clercq, C. D. Rho, C. Eldridge, C. Finley, C. Glaser, C. G\"unther, C. Ha, C. Hill, C. H. Wiebusch, C. Klein, C. Kopper, C. Lagunas Gualda, C. Li, C. Lin, C. Love, C. Parisel, C. P\'erez de los Heros, C. Raab, C. Rott, C. Spannfellner, C. Spiering, C. Walck, C. Weaver, C. Wendt, C. Zilleruelo Ca\~nas, D. A. Coloma Borja, D. Berley, D. Butterfield, D. Chirkin, D. Delgado, D. Durnford, D. Els\"asser, D. F. Cowen, D. Fox, D. Grant, D. Guevel, D. Hooper, D. J. Koskinen, D. Kang, D. Mousadi, D. R. Williams, D. Ryckbosch, D. Salazar-Gallegos, D. Seckel, D. Soldin, D. Song, D. Tosi, D. Veske, D. Z. Besson, E. Bernardini, E. Blaufuss, E. Ellinger, E. Ganster, E. Genton, E. H. S. Warrick, E. J. Roberts, E. Krupczak, E. Kun, E. Magnus, E. Manao, E. Moyaux, E. N. Paudel, E. O'Sullivan, E. Resconi, E. Yildizci, F. Bontempo, F. G. Schr\"oder, F. Halzen, F. Henningsen, F. Kirchner, F. Lauber, F. Lucarelli, F. Mayhew, F. McNally, F. Schl\"uter, F. Varsi, F. Yu, G. C. Hill, G. de Wasseige, G. H. Collin, G. M. Spiczak, G. Sanger-Johnson, G. Sommani, G. T. Przybylski, G. Wrede, G. W. Sullivan, H. Erpenbeck, H. Kimku, H. Kolanoski, H. Niederhausen, H. Pandya, H. Schieler, I. C. Mari\c{s}, I. Martinez-Soler, I. Reistroffer, I. Taboada, J. A. Aguilar, J. Adams, J. A. Torres, J. Becker Tjus, J. Beise, J. B\"ottcher, J. Braun, J. Carpio, J. C. D\'iaz-V\'elez, J. Evans, J. Gallagher, J. G. Gonzalez, J. Hardin, J. H\"au{\ss}ler, J. Hellrung, J. J. Beatty, J. J. DeLaunay, J. Kiryluk, J. Liao, J. L. Kelley, J.M. Alameddine, J. Mauro, J. M. Conrad, J. Mitchell, J. Osborn, J. Peterson, J. P. Lazar, J. P. Yanez, J. Rack-Helleis, J. Saffer, J. Soedingrekso, J. Stachurska, J. Thwaites, J. Valverde, J. Vandenbroucke, J. van Santen, J. Vara, J. Villarreal, J. Weldert, J. Werthebach, J. Y. Book Motzkin, K. Andeen, K. Carloni, K. D. de Vries, K. D. Hoffman, K. Dutta, K. Fang, K. Farrag, K. Hanson, K. Helbing, K. Hoshina, K. Hultqvist, K. Hymon, K. Kruiswijk, K. Leonard DeHolton, K. L. Fan, K. Meagher, K. M. Groth, K. Noda, K. Rawlins, K. Tollefson, K. Upshaw, L. Bloom, L. Brusa, L. Draper, L. Dueser, L. Eidenschink, L. Gerhardt, L. Halve, L. Hamacher, L. Hennig, L. Heuermann, L. Kardum, L. K\"opke, L. Lallement Arnaud, L. Lu, L. Marten, L. Merten, L. Molchany, L. Neste, L. Paul, L. Pyras, L. Ricca, L. Ruohan, L. Schlickmann, L. Seen, L. Van Rootselaar, L. Witthaus, M. Ackermann, M. A. DuVernois, M. Ahlers, M. Dittmer, M. Garcia, M. Handt, M. Hostert, M. Hrywniak, M. Jacquart, M. Jansson, M. Jin, M. J. Larson, M. Kauer, M. Khanal, M. Kowalski, M. Liubarska, M. Macdonald, M. Meier, M. Nakos, M. Neumann, M. Plum, M. Ravn, M. Rongen, M. Santander, M. Scarnera, M. Schaufel, M. Seikh, M. Stamatikos, M. Thiesmeyer, M. U. Nisa, M. Velazquez, M. Venugopal, M. Vereecken, M. Weyrauch, N. Chau, N. Feigl, N. Heyer, N. Kamp, N. Krieger, N. Kurahashi, N. M. Amin, N. Park, N. Rad, N. Schmeisser, N. Shimizu, N. Valtonen-Mattila, N. van Eijndhoven, N. Whitehorn, O. Botner, O. Janik, P. A. Evenson, P. A. Sevle Myhr, P. Behrens, P. Desiati, P. Eller, P. F\"urst, P. Gutjahr, P. Hatch, P. Koundal, P. Sampathkumar, P. Soldin, P. Weigel, P. Zhelnin, P. Zilberman, Q. R. Liu, R. Abbasi, R. Babu, R. Bay, R. Engel, R. Hewett, R. Hmaid, R. Koirala, R. Maruyama, R. Neshat, R. Orsoe, R. Procter-Murphy, R. Shah, R. Snihur, R. T. Burley, R. W. Moore, S. Ali, S. Athanasiadou, S. Benkel, S. BenZvi, S. Blot, S. B\"oser, S. Choi, S. Deng, S. DiKerby, S. Eulig, S. Fukami, S. Goswami, S. Griffin, S. Griswold, S. Hickford, S. Hori, S. Jain, S. J. Gray, S. Koch, S. Mancina, S. Marka, S. Minji, S. Mondal, S. N. Axani, S. Pick, S. R. Klein, S. Rodan, S. Sarkar, S. Schindler, S. Schwirn, S. Sclafani, S. Seunarine, S. Shah, S. Shefali, S. Ter-Antonyan, S. Tilav, S. Toscano, S. Vergara Carrasco, S. Verpoest, S. W. Barwick, S. Yoshida, S. Yu, S. Yun-C\'arcamo, S. Zhang, T. C. Petersen, T. Delmeulle, T. DeYoung, T. Ding, T. Ehrhardt, T. Gl\"usenkamp, The IceCube Collaboration, T. Huber, T. Karg, T. Kim, T. Kontrimas, T. Kozynets, T. Krishnan, T. Montaruli, T. Mukherjee, T. Pernice, T. Ruhe, T. Schmidt, T. Stanev, T. Stezelberger, T. St\"urwald, T. Stuttard, T. Van Eeden, T. Yuan, U. Naumann, V. Basu, V. O'Dell, V. Palusova, V. Parrish, V. Poojyam, W. Esmail, W. G. Thompson, W. Hou, W. Iwakiri, W. Kang, W. Luszczak, W. Rhode, X. Bai, X. W. Xu, Y. C. Chen, Y. Kobayashi, Y. Lyu, Y. Makino, Y. Merckx, Y. Morii, Y. T. Liu, Y. Yao, Z. Brisson-Tsavoussis, Z. Chen, Z. Marka, Z. Rechav, Z. Zhang.

Figure 1
Figure 1. Figure 1: FIG. 1 [PITH_FULL_IMAGE:figures/full_fig_p006_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: also shows a violin plot of expected statistical fluctuations, constructed by fitting to 50 realizations of the model given the nominal density profile (based on the average PREM density in each shell) and superimposing the resulting posteriors (with the violins representing the KDE of the superposition). This indicates the size and frequency of statistical fluctuations given a model consistent with the PR… view at source ↗
Figure 3
Figure 3. Figure 3: FIG. 3 [PITH_FULL_IMAGE:figures/full_fig_p010_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: FIG. 4 [PITH_FULL_IMAGE:figures/full_fig_p015_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: FIG. 5 [PITH_FULL_IMAGE:figures/full_fig_p020_5.png] view at source ↗
Figure 6
Figure 6. Figure 6: FIG. 6 [PITH_FULL_IMAGE:figures/full_fig_p021_6.png] view at source ↗
Figure 7
Figure 7. Figure 7: FIG. 7 [PITH_FULL_IMAGE:figures/full_fig_p022_7.png] view at source ↗
Figure 8
Figure 8. Figure 8: FIG. 8 [PITH_FULL_IMAGE:figures/full_fig_p022_8.png] view at source ↗
Figure 9
Figure 9. Figure 9: FIG. 9 [PITH_FULL_IMAGE:figures/full_fig_p023_9.png] view at source ↗
Figure 10
Figure 10. Figure 10: FIG. 10 [PITH_FULL_IMAGE:figures/full_fig_p023_10.png] view at source ↗
Figure 11
Figure 11. Figure 11: FIG. 11 [PITH_FULL_IMAGE:figures/full_fig_p024_11.png] view at source ↗

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