{"id":"6898b609-e8b1-49de-8b26-a2e0b3337f0f","arxiv_id":"hep-ph/0206162","paper_version":1,"verdict":"CONDITIONAL","confidence":"MODERATE","novelty_score":5.0,"correctness_risk":"low","formal_verification":"none","parameter_count":0,"one_line_summary":"A pull-based global fit to 81 solar neutrino observables confirms the LMA oscillation solution, leaves LOW and QVO viable, and disfavors SMA at Delta chi-squared of about 23.5.","lead":"A global fit of 81 solar neutrino measurements against two-flavor oscillation models, recast in a 'pull' form of chi-squared that shows exactly which data points and which systematic errors drive the fit. It confirms the large-mixing (LMA) solution and quantifies how strongly the low-mass and quasi-vacuum alternatives are disfavored.","discovery_kind":"new_method","skeptic_critique":{"model":"selfhosted/deepseek-v4.1-flash","headline":"The reader's SK nadir-correlation concern is real and acknowledged, but relaxing that restriction can only lower chi-squared for LOW/QVO, so it makes the paper's acceptability claims conservative rather than threatened; the central claim survives.","rationale":"The paper's central claim is that LMA is the best fit (chi-squared 73.4 at delta m squared = 5.5e-5 eV squared, tan squared theta = 0.42), LOW (Delta chi-squared 10.4) and QVO (7.8) remain acceptable, and SMA (23.5) is disfavored. The statistical machinery is sound and proved rather than asserted: Appendix A derives the covariance-pull equivalence and the reduction from an 81-by-81 to a 31-by-31 inversion, and the pull tables (II-VI) are internally consistent (e.g., Table III sums to 71.3, Table V to 2.1, Table VI to 73.4). The reader's identified weakest assumption, the fully-correlated-in-nadir SK systematics, is real and acknowledged in Appendix C, but the reader misjudges its direction: relaxing the restriction can only lower chi-squared, so the paper's 'acceptable' statements for LOW and QVO are conservative upper bounds, not consequences of an artificially tight model. The SMA rejection is likewise robust because it is driven by observable residuals (chi-squared_obs = 83.1 versus 71.3 for LMA), not by systematic stretching (chi-squared_sys = 13.8 is below the naive 31). The secondary items the reader lists are legitimate but minor: the Ga winter-summer datum's provenance (a 'to appear' proceeding plus a private communication) and the explicit 'derivation omitted' in Appendix E for the SK ES flux behind Fig. 9. Neither bears on the LMA/LOW/QVO/SMA ranking. I therefore agree with the reader that the paper is a careful methodological contribution rather than a discovery paper, but I do not think the flagged concern lands as load-bearing against the central claim, and I would keep the verdict at CONDITIONAL for the secondary revision items rather than move it. The concrete test above would settle the direction-of-effect question empirically: if per-nadir-bin freedom lowers Delta chi-squared for LOW/QVO (as predicted) and leaves SMA above roughly 15, the central claim is confirmed; if it rescues SMA below roughly 10, the rejection claim weakens. I note one small internal inconsistency worth a copy-edit: Section III.B says the 8B shape uncertainty affects 'all the 81 observables,' while footnote 10 says its effect on the Ga winter-summer difference is neglected, implying 80; this is cosmetic and does not affect any number in the tables.","tokens_in":33042,"tokens_out":11237,"duration_ms":198958,"concrete_test":"Re-run the global fit with the SK nadir bins given independent nuisance parameters (e.g., a per-nadir-bin fractional offset of 2-3%, or the day-night non-cancelling systematics the authors cite from [22, 63, 59]), and report the new Delta chi-squared for LOW, QVO, and SMA relative to LMA. The direction-of-effect argument predicts Delta chi-squared(LOW) and Delta chi-squared(QVO) will decrease, confirming the paper's acceptability claims are conservative. If instead Delta chi-squared(SMA) falls below roughly 10, the SMA rejection would be an artifact of the tight nadir model and the central claim would weaken; if SMA stays above roughly 15, the claim is confirmed.","verdict_should_be":"UNCHANGED","load_bearing_attack":"The reader's weakest_assumption is genuine and the authors flag it themselves in the closing remark of Appendix C: SK systematics are taken as fully correlated in nadir, with no allowance for uncorrelated day-night shape variations, and Earth-density/PREM-local uncertainties are noted but not propagated. However, the direction of the effect matters. Restricting nuisance parameters can only inflate chi-squared; relaxing the nadir correlation would lower chi-squared for every solution, including LOW (83.8) and QVO (81.2), which are already acceptable at NDF = 79. So the paper's 'acceptable' verdicts are upper bounds under the restriction, not artifacts of it. The reader's framing ('the LOW and QVO verdicts rest substantially on mild day-night and spectral distortions') implies the restriction is doing favorable work for the claim; it is doing the opposite. The one prong that could be threatened by a more generous error budget is the SMA rejection (Delta chi-squared = 23.5), but that is driven by chi-squared_obs = 83.1 versus 71.3 for LMA, not by systematic stretching: chi-squared_sys = 13.8 over 31 sources is well below the naive expectation of 31, so the SMA fit is not being propped up by stretched systematics. The genuinely soft spots are secondary: the Ga winter-summer datum rests on a 'to appear' proceeding [4] and a private communication [56], and Appendix E explicitly says 'derivation omitted' for the SK ES flux that Fig. 9 depends on. Neither threatens the LMA/LOW/QVO/SMA ranking.","agreement_with_reader":"partial"},"referee_report":{"model":"selfhosted/deepseek-v4.1-flash","summary":"The paper presents a global two-flavor active oscillation analysis of the then-current solar neutrino data set: 81 observables comprising the Homestake Cl rate, the combined SAGE+GALLEX/GNO Ga rate and its winter-summer difference, 44 Super-Kamiokande energy-nadir spectrum bins, and 34 SNO day-night spectrum bins, together with 31 correlated systematic uncertainties (12 SSM inputs, the 8B shape error, 11 SK and 7 SNO sources). The methodological core is the 'pull' formulation of the chi-squared, in which each systematic is a Gaussian nuisance parameter penalized quadratically and minimized away; Appendix A proves the exact equivalence of this construction to the covariance-matrix approach and shows that it reduces an N-by-N inversion to a K-by-K one. The physics output is a set of local minima: LMA at delta m^2 = 5.5e-5 eV^2, tan^2 theta = 0.42 with chi^2 = 73.4 (NDF = 79), LOW at Delta chi^2 = 10.4, QVO at 7.8, and SMA at 23.5. The paper further decomposes chi^2 into per-observable and per-systematic pulls (Tables II-IV), translates the SSM pulls into preferred flux shifts (Table VII), and closes with a quasi-model-independent SK/SNO comparison in the (Phi_B, <P_ee>) plane (Appendix E).","tokens_in":33279,"tokens_out":7367,"duration_ms":123663,"significance":"The pull decomposition is a genuine and durable methodological contribution: it converts an 81-by-81 covariance inversion into a 31-by-31 one, and, more importantly, it makes the fit auditable, since every observable and every systematic carries a signed residual that a reader can inspect. The equivalence proof in Appendix A is self-contained linear algebra and is correct as written. The itemized error budget, the explicit treatment of the 8B shape uncertainty, and the recalculation of fractional systematic errors at each grid point (Appendix C) are all real services to the field, and the pull tables are the kind of diagnostic that later global fits adopted. The physics conclusions are consistent with the 2002 consensus and are stated with appropriate hedging for LOW and QVO. The paper does not ship code or machine-checked proofs, but the statistical construction is fully specified and reproducible from the text.","major_comments":[{"comment":"The rejection of the SMA solution is one of the paper's headline claims, and roughly half of its statistical weight comes from stretched systematics rather than from the data residuals: Delta chi^2_SMA = 23.5 splits into Delta chi^2_obs = 11.8 and Delta chi^2_sys = 11.7. The systematic part is dominated by SNO scale (-1.48), SNO vertex (-1.42), SNO neutron capture (+0.94), SNO low-energy background (+0.87) and the 8B shape (-1.56), all pulling in a direction that reduces the spectral difference between theory and data. Because these are treated as independent zero-centered Gaussians, the SMA penalty is a sum of squares of individually order-one-sigma offsets, and the paper's own remark that it is 'quite unlikely that future, possible recalibrations of systematics may just happen to cancel out all these offsets' is an assertion rather than a demonstrated result. A sensitivity statement is needed: what is Delta chi^2_SMA if, for instance, the SNO energy scale and the 8B shape are allowed a common fully correlated component, or if the SNO scale prior is doubled? If the SMA Delta chi^2 falls to about 12, the language 'safely ruled out' in Section IV C and 'could be recovered only by ad hoc recalibrations' in the abstract would need softening.","section":"Section IV C, Table IV","authors_acknowledge":null,"authors_acknowledge_p":null},{"comment":"The twelve SSM inputs enter as zero-centered Gaussian pulls, so the posterior flux shifts obtained from Eq. (17) are shrunk toward zero by construction; the conclusion that the LMA solution 'basically confirms' all solar neutrino fluxes is therefore partly a property of the prior rather than an independent measurement. The authors acknowledge this explicitly for Phi_B, noting that SNO already determines it better than the SSM, but the same logic applies with more force to Phi_Be, Phi_N and Phi_O, where the SSM prior is far tighter than the data. The 'striking LMA agreement with all standard solar model fluxes' claimed in Section V would be made testable, rather than guaranteed, by repeating the fit with at least Phi_Be (and ideally Phi_N, Phi_O) free, or by quoting the shifts obtained with the SSM priors inflated by a stated factor. As written, Table VII cannot distinguish agreement from prior shrinkage.","section":"Section IV D, Table VII","authors_acknowledge":null,"authors_acknowledge_p":null},{"comment":"The Ga winter-summer difference R_W - R_S = -11 +/- 9 SNU is introduced here for the first time in an oscillation analysis, and it rests on a conference contribution listed as 'to appear' in the reference list [4] plus a private communication [56] for the statement that systematics largely cancel in the difference. Section IV A states that including this datum lowers the likelihood of the LOW solution, so the LOW acceptability verdict depends on a number whose final published value and error are not yet fixed. The authors should quote Delta chi^2_LOW with and without this datum, so that a reader can see how much of the LOW result is carried by an unpublished input. The direction of the effect appears conservative for the LOW claim, but that should be shown rather than inferred.","section":"Section III A and Appendix B, Eq. (B1)","authors_acknowledge":null,"authors_acknowledge_p":null}],"minor_comments":[{"comment":"The SK ES flux estimate and its three error components are given with the parenthetical 'derivation omitted'. Since the 2-sigma band in Fig. 9 depends on this number and on the propagation of the 8B shape error into it, a short derivation or a pointer to the intermediate quantities would let the reader check the error budget.","section":"Appendix E, Eq. (E4)","authors_acknowledge":null,"authors_acknowledge_p":null},{"comment":"The differences between the SNO contours in Fig. 2 and the official SNO analysis in Fig. 4a of [9] are attributed in part to 'the (numerically delicate) averaging of the oscillating terms in the energy or time domain' in the SNO analysis. This is a claim about another collaboration's numerics made without demonstration; it should be softened or supported with a concrete comparison.","section":"Section IV B","authors_acknowledge":null,"authors_acknowledge_p":null},{"comment":"The no-oscillation normalization of 556 events/kty is described as 'graphically derived from [59]', a conference slide. Even though the authors note that only the ratios in the third column matter in practice, a citable number or an explicit statement of the insensitivity would be preferable.","section":"Table VIII, footnote a","authors_acknowledge":null,"authors_acknowledge_p":null},{"comment":"The LMA 3-sigma range for the Ga winter-summer pull is quoted as [-1.23, -1.22], essentially constant across the entire allowed LMA region. This indicates that the datum is uncorrelated with the oscillation parameters there, so the pull is a fixed roughly 1.2-sigma offset contributing about 1.5 to every chi^2 in that region; a sentence noting this would help the reader interpret the entry.","section":"Table II, pull 3","authors_acknowledge":null,"authors_acknowledge_p":null},{"comment":"The cross-section error prescription (linear sum within the low- and high-energy clusters, quadratic between them) and the Ga recipe of taking one third of the variation induced by the plus-or-minus 3-sigma perturbed cross sections are both hand-chosen. They are disclosed, which is good practice, but a sentence on how sensitive the fit is to these choices would strengthen the error-budget discussion.","section":"Section III A, Eq. (14)","authors_acknowledge":null,"authors_acknowledge_p":null},{"comment":"The statement that the highest allowed delta m^2 values 'hit the region independently disfavored by CHOOZ data' is made without showing the CHOOZ bound used or where it lies in Fig. 1. A line stating the CHOOZ contour adopted would make the comparison checkable.","section":"Section IV A","authors_acknowledge":null,"authors_acknowledge_p":null}],"recommendation":"minor_revision","confidential_remarks":"The paper is a methods-plus-reanalysis contribution with substantial overlap with the authors' own earlier work ([37], [39], [58]), which is properly cited. The statistical machinery is sound and the equivalence proof is correct. The one claim most likely to be revisited is the SMA rejection, which is the only place where the conclusion depends materially on the assumed independence and normalization of the SNO and 8B shape systematics; the requested sensitivity check is the item I would most want to see before the paper is cited as settling that question."},"author_rebuttal":null,"desk_editor":{"model":"selfhosted/deepseek-v4.1-flash","letter":"The thing worth your time here is the bookkeeping, not the headline. Fogli and collaborators redo the 2002 solar neutrino global fit in the pull formalism: 81 observables, 31 correlated systematics, and — this is the useful part — they publish the full pull tables. Table II gives you the residual of every SK and SNO bin at each solution; Table IV does the same for every systematic. You can audit the fit yourself instead of taking a chi-squared on faith. That is rare and it is the paper's real contribution. The equivalence of pull and covariance is not new and they say so plainly in footnote 3 and Appendix A, crediting Stump et al. from the parton-fitting literature. Appendix A's derivation of the K-by-K reduction is clean and self-contained. The first inclusion of the GALLEX/GNO winter-summer difference in an oscillation analysis is a genuine addition, and Table VII's flux shifts are a nice byproduct of the pull bookkeeping — the SSM pulls translate directly into preferred flux variations, which the covariance approach does not hand you for free. The physics conclusions (LMA at 73.4, LOW at +10.4, QVO at +7.8, SMA at +23.5) follow from the numbers as printed, and the SMA rejection is driven by chi-squared_obs, not by stretched systematics — chi-squared_sys = 13.8 over 31 sources is well under expectation, so SMA is not being rescued or propped up by nuisance parameters. On the SK nadir-correlation worry: I think it is backwards. The authors flag in Appendix C that SK systematics are taken as fully correlated in nadir, and they are right that this is a restriction. But restricting nuisance parameters can only inflate chi-squared. Relaxing it would lower chi-squared for LOW and QVO too, so the acceptability verdicts are conservative, not artifacts. The genuinely soft items are smaller: the Ga winter-summer datum rests on a proceeding listed as 'to appear' plus a private communication, and Appendix E says 'derivation omitted' for the SK ES flux that Fig. 9 depends on. The paper also explains its SNO contour disagreement by speculating about SNO's numerical averaging without demonstrating it — that should have been shown or dropped. None of this touches the ranking. For anyone doing global fits with correlated systematics, this is worth reading as a template. Send it out.","headline":"A careful, well-documented pull-based global solar neutrino fit whose real value is the audit trail — per-observable and per-systematic pull tables — not the LMA confirmation, which the field already expected.","tokens_in":34006,"tokens_out":829,"would_cite":true,"duration_ms":12451,"reading_group":"yes","serious_thinker":"yes","would_accept_peer_review":true},"pith_extraction":{"msc":[],"pacs":["26.65.+t","13.15.+g","14.60.Pq","91.35.-x"],"model":"selfhosted/deepseek-v4.1-flash","headline":"A pull-based global fit to 81 solar neutrino observables confirms large mixing as the best solution while keeping low-mass and quasi-vacuum solutions statistically viable and disfavoring small mixing.","keywords":["solar neutrinos","neutrino oscillations","LMA solution","pull method","correlated systematic uncertainties","chi-squared analysis","Super-Kamiokande","Sudbury Neutrino Observatory"],"falsifier":"A reanalysis of the same SK and SNO spectra that allows independent per-nadir-bin shape systematics, or a future day-night measurement with smaller errors, would settle it: if the LOW and QVO $Δχ^2$ values move substantially above the LMA value, the paper's acceptability ranking fails; if they stay near 8–10, it holds.","tokens_in":34318,"feed_emoji":"☀️","tokens_out":4461,"duration_ms":82855,"temperature":0.7,"pith_summary":"The paper asks how to extract the most information from a global fit to solar neutrino data when there are many observables and many correlated uncertainties. It advocates the pull method, in which each systematic uncertainty gets a Gaussian parameter that is fitted away, and proves that this is numerically identical to the covariance-matrix method while yielding a clean split into observable and systematic contributions. Applied to 81 observables from chlorine, gallium, Super-Kamiokande, and SNO, together with 31 correlated systematics, the fit puts the large-mixing LMA solution first but leaves LOW and QVO acceptable and makes SMA hard to recover. The practical payoff is a diagnostic table of pulls that shows which measurements and which systematics drive the fit, and a way to read off preferred shifts of the solar neutrino fluxes from their standard-solar-model values.","feed_headline":"Pull method keeps LMA on top of solar neutrino fits","feed_subtitle":"An 81-observable global fit leaves LOW and QVO viable and finds no stretched systematics at LMA.","key_machinery":"The pull method replaces each correlated systematic source $k$ with a Gaussian variable $ξ_k$ that shifts every affected prediction by $ξ_k c_{kn}$, then minimizes $χ^2_{pull} = Σ_n [(R_{expt,n} - R_{theo,n} - Σ_k ξ_k c_{kn})/u_n]^2 + Σ_k ξ_k^2$. At the minimum the $ξ_k$ solve $K$ linear equations, so one inverts a $K × K$ matrix instead of the $N × N$ covariance matrix, and the result splits exactly into $χ^2_{obs} = Σ_n x_n^2$ and $χ^2_{sys} = Σ_k ξ_k^2$. The same $ξ_k$ values, fed through the standard-solar-model log-derivatives $α_{ik}$, give the preferred fractional flux shifts $ΔΦ_i/Φ_i = Σ_k ξ_k α_{ik} Δ ln X_k$, which is how the paper turns statistical pulls into statements about the Sun.","core_discovery":"The central claim is that the pull formulation of $χ^2$ is not merely a computational convenience but the right way to organize a large solar neutrino fit. The authors prove $χ^2_{covar} ≡ χ^2_{pull}$ and then apply the pull form to 81 observables and 31 systematics. At the best-fit LMA point, $δm^2 = 5.5 × 10^{-5}$ eV$^2$ and $tan^2 θ_{12} = 0.42$, they find $χ^2 = 73.4$, with $χ^2_{obs} = 71.3$ and $χ^2_{sys} = 2.1$; LOW has $Δχ^2 = 10.4$, QVO 7.8, and SMA 23.5. No observable pull exceeds about $2.2σ$ at LMA, and no correlated systematic is stretched significantly there, while SMA requires offsets of order $1σ$ in several SNO systematics and about $1.5σ$ in the $^8$B shape.","pith_inferences":["The paper's own caveat about nadir-correlated SK systematics is a ready-made stress test: redoing the fit with independent day-night shape parameters would show whether the LOW and QVO verdicts are robust or are artifacts of the correlation assumption.","Because the pull split is exact, the same diagnostic can be transplanted to reactor and accelerator oscillation fits where dozens of spectral bins share a handful of detector systematics.","The near-zero SSM pulls at LMA suggest that the solar flux and oscillation parameters are not compensating each other; a precise KamLAND $δm^2$ measurement would convert the remaining flux shifts into a clean test of the standard solar model.","The historical SMA detour was driven by a small chlorine pull; the pull table makes that kind of single-observable accident visible in advance, which is a general lesson for global fits."],"forward_implications":["If LMA is the true solution, the fitted flux shifts are near zero for all components, so the standard solar model's pp, pep, Be, B, N, and O fluxes are confirmed at the percent-to-few-percent level; the paper's Table VII gives the numbers.","If LOW or QVO is true, the fit prefers a cooler Sun, with negative shifts in Be, B, N, and O fluxes and a B flux about 12–22 percent below the standard value.","The pull decomposition predicts that removing SK would weaken the preference for LMA and revive some small-mixing or vacuum regions, while removing SNO would mainly weaken the rejection of SMA.","SMA cannot be rescued without coordinated recalibrations of several SNO systematics and the $^8$B shape, so a future measurement that moves those systematics in the required direction would reopen it.","The method gives a per-observable residual table, so any future data set that produces a pull above about $3σ$ would flag a specific inconsistency rather than a global bad fit."],"supporting_citations":[{"why":"Supplies the covariance-matrix approach to solar neutrino data that the pull method is proved equivalent to.","marker":"[21]"},{"why":"Provides the standard-solar-model input uncertainties and log-derivatives used to propagate SSM systematics into the flux shifts.","marker":"[37]"},{"why":"Supplies the 44-bin Super-Kamiokande energy-nadir spectrum and the 11 SK systematic error sources.","marker":"[6]"},{"why":"Supplies the 34-bin SNO day-night spectrum used in the global fit.","marker":"[8]"},{"why":"Supplies the $^8$B neutrino energy-spectrum shape uncertainty that affects all observables.","marker":"[46]"},{"why":"Supplies the standard solar model central fluxes and the updated metallicity uncertainty.","marker":"[41]"},{"why":"Documents an earlier discussion of the covariance-pull equivalence in parton-density fitting, which the paper cites for the identity.","marker":"[25]"},{"why":"Supplies the calculation of the winter-summer gallium rate difference induced by Earth matter effects.","marker":"[39]"},{"why":"Supplies the SNO forward-fitting procedure, background treatment, and several SNO systematic uncertainties.","marker":"[40]"},{"why":"Supplies the prescription for treating chlorine and gallium cross-section errors in the uncorrelated error budget.","marker":"[33]"}],"fun_headline_variants":["Pull form of chi-squared organizes 81-observable solar neutrino fit","Solar neutrino fit: pull method equals covariance, LMA stays best","LMA survives 81 observables and 31 systematics in solar neutrino fit","Pull method shows LMA best while LOW and QVO remain viable","No pull exceeds 2.2 sigma at LMA in solar neutrino analysis"],"cache_read_input_tokens":0,"weakest_assumption_plain":"The empirical ranking of solutions depends on treating all Super-Kamiokande systematic errors as fully correlated across nadir bins, with no independent day-night shape freedom; the authors acknowledge this in Appendix C but do not quantify its effect.","fun_headline_variants_meta":{"raw":{"variants":["Pull form of chi-squared organizes 81-observable solar neutrino fit","Solar neutrino fit: pull method equals covariance, LMA stays best","LMA survives 81 observables and 31 systematics in solar neutrino fit","Pull method shows LMA best while LOW and QVO remain viable","No pull exceeds 2.2 sigma at LMA in solar neutrino analysis"]},"model":"selfhosted/deepseek-v4.1-flash","effort":"low","attempts":1,"cost_usd":0.0,"raw_usage":{"total_tokens":1669,"prompt_tokens":1032,"completion_tokens":637,"prompt_tokens_details":null,"completion_tokens_details":{"reasoning_tokens":553}},"tokens_in":1032,"tokens_out":637,"duration_ms":11463,"image_pages":[],"temperature":1.0,"reasoning_budget":50,"reasoning_tokens":553,"transport_provider":"selfhosted","cache_read_input_tokens":0,"cache_creation_input_tokens":0},"cache_creation_input_tokens":0},"created_at":"2026-10-29T17:31:41.544789+00:00","model_set":{"reader":"selfhosted/deepseek-v4.1-flash"},"falsifier":"A reanalysis of the same SK and SNO spectra that allows independent per-nadir-bin shape systematics, or a future day-night measurement with smaller errors, would settle it: if the LOW and QVO $Δχ^2$ values move substantially above the LMA value, the paper's acceptability ranking fails; if they stay near 8–10, it holds.","supporting_citations":[{"cited_title":"Astropart. Phys. 3, 185","cited_arxiv_id":null,"evidence_quote":"Supplies the covariance-matrix approach to solar neutrino data that the pull method is proved equivalent to."},{"cited_title":"Phys. Rev. D 62, 013002","cited_arxiv_id":null,"evidence_quote":"Provides the standard-solar-model input uncertainties and log-derivatives used to propagate SSM systematics into the flux shifts."},{"cited_title":"Determination of Solar Neutrino Oscillation Parameters using 1496 Days of Super-Kamiokande-I Data","cited_arxiv_id":"hep-ex/0205075","evidence_quote":"Supplies the 44-bin Super-Kamiokande energy-nadir spectrum and the 11 SK systematic error sources."},{"cited_title":"Direct Evidence for Neutrino Flavor Transformation from Neutral-Current Interactions in the Sudbury Neutrino Observatory","cited_arxiv_id":"nucl-ex/0204008","evidence_quote":"Supplies the 34-bin SNO day-night spectrum used in the global fit."},{"cited_title":"L. De Braeckeleer , S. J. Freedman, and J. Napolitano, Phys. Rev. C 54, 411","cited_arxiv_id":null,"evidence_quote":"Supplies the $^8$B neutrino energy-spectrum shape uncertainty that affects all observables."},{"cited_title":"Astrophy s. J. 555, 990","cited_arxiv_id":null,"evidence_quote":"Supplies the standard solar model central fluxes and the updated metallicity uncertainty."},{"cited_title":null,"cited_arxiv_id":null,"evidence_quote":"Documents an earlier discussion of the covariance-pull equivalence in parton-density fitting, which the paper cites for the identity."},{"cited_title":"Phys. Rev. D 61, 073009","cited_arxiv_id":null,"evidence_quote":"Supplies the calculation of the winter-summer gallium rate difference induced by Earth matter effects."},{"cited_title":null,"cited_arxiv_id":null,"evidence_quote":"Supplies the SNO forward-fitting procedure, background treatment, and several SNO systematic uncertainties."},{"cited_title":"If sterile neutrinos exist, how can one determine the total solar neutrino fluxes?","cited_arxiv_id":"hep-ph/0204194","evidence_quote":"Supplies the prescription for treating chlorine and gallium cross-section errors in the uncorrelated error budget."}],"review_version":1}