{"id":"a9a0f36e-740d-4726-b1eb-d591caeb4b06","arxiv_id":"1612.02010","paper_version":2,"verdict":"CONDITIONAL","confidence":"HIGH","novelty_score":5.0,"correctness_risk":"medium","formal_verification":"none","parameter_count":0,"one_line_summary":"Galactic parameter and baryonic-morphology uncertainties shift the local dark matter density by up to a factor of 30, moving direct and indirect detection limits on Singlet Scalar and Inert Doublet dark matter by comparable amounts.","lead":"Varying the Milky Way's baryonic morphology and the Sun's galactocentric distance and circular speed shifts the inferred local dark matter density by up to a factor of 30, which in turn moves direct and indirect detection limits on two simple WIMP models. The paper quantifies how much of a dark matter constraint is astronomy rather than particle physics.","discovery_kind":"new_application","skeptic_critique":{"model":"selfhosted/deepseek-v4.1-flash","headline":"The headline direct-detection effect rests on a factor-32 rho0 range produced by pairing anti-correlated (R0, v0) extremes; the paper's own factor-19 Milky Way mass range suggests the fit is absorbing the mismatch, so the 'largest effect' ordering may be an artifact of the pairing rather than a real","rationale":"The reader's weakest_assumption identifies exactly the load-bearing soft spot: the two (R0, v0) pairs are anti-correlated corners, not a joint credible region, and the resulting rho0 range is an upper bound rather than a best estimate. I agree and would sharpen it in one respect. The reader frames the issue as a pairing choice; the paper's own reported Milky Way mass range (1.2-22.9 x10^11 M_sun, Section 2.1) is independent corroboration that the fit is absorbing the (R0, v0) mismatch into the DM profile rather than reflecting a genuine density uncertainty. A factor-19 total-mass range from a factor-1.3 change in R0 and a factor-1.7 change in v0 is not physically credible, and the paper reports it without flagging it. That strengthens the case that the factor-32 rho0 spread is partly an artifact of the rigid gNFW with fixed Rs = 20 kpc. The consequence is narrow but real: the Section 5 ordering claim that (R0, v0) produces the largest effect is contingent on the inflated rho0 range. Since morphology moves rho0 by only ~20% (0.387 to 0.471 GeV/cm3), a joint propagation giving rho0 within a factor of 2-3 would put (R0, v0) on par with morphology for direct detection rather than ahead of it. The paper's qualitative thesis, that Galactic systematics are first-order in WIMP constraints, is not threatened; the specific ranking and the factor-32 band are. This is why CONDITIONAL is the right verdict and why I would not move it: the concern is about the magnitude and ordering of a stated result, not about whether the pipeline is sound or whether the qualitative conclusion holds. Two secondary points from the reader also stand but are lighter. The IDM statement in Section 4.2 that the shifted region 'is not visible in the figure as it is forbidden by the cosmological constraint' is asserted without showing the shifted points, which is a presentational gap rather than a correctness risk. The absence of a code or data release is a reproducibility limitation but not a load-bearing concern for the central claim, since the pipeline components (galkin, the RC compilation, the LUX maximum-gap reanalysis, the GeV-excess rescaling from [43]) are individually documented and cited. Credit where due: the uncertainty taxonomy in Section 2.1 is clearly organized, the one-at-a-time caveat is stated explicitly, and the GeV-excess contour rescaling follows a published procedure with a stated conservation condition. None of that rescues the specific factor-32 number, which is why the verdict should stay CONDITIONAL rather than ACCEPT, and the concrete test above is the single check that would settle whether the ordering claim survives joint propagation.","tokens_in":23090,"tokens_out":4393,"duration_ms":87017,"concrete_test":"Sample the joint posterior on (R0, v0) from McMillan & Binney (2010) [12], which the paper already cites, rather than taking the two anti-correlated corners. For each draw, refit rho0 with the same gNFW + fixed Rs = 20 kpc pipeline and the same RC compilation, and report the 95% interval of rho0. If that interval is much narrower than [0.055, 1.762] GeV/cm3 (e.g. within a factor of ~2-3 of 0.466), the factor-32 band is an upper bound from corner-pairing, and the Section 5 claim that (R0, v0) dominates over morphology for direct detection should be softened. A secondary check: repeat the two extreme fits with Rs free and see whether the rho0 values move toward the standard range, which would confirm the fixed-Rs rigidity is contributing to the spread.","verdict_should_be":"UNCHANGED","load_bearing_attack":"The paper's central quantitative claim (Section 5) is that 'the largest effects on the SSDM and IDM parameter space are obtained as a consequence of varying the Galactic parameters (R0, v0).' For direct detection this reduces almost entirely to the variation of rho0, since vpeak is held fixed at 250 km/s in Section 4. Table 1 rows 2 and 3 give rho0 = 1.762 and 0.055 GeV/cm3 for (R0, v0) = (7.5 kpc, 312 km/s) and (8.5 kpc, 180 km/s). That is a factor of 32, far outside the factor ~2-3 range the same literature (including the review [1] the paper cites) quotes for the local DM density. The pairing is maximally anti-correlated in the well-determined combination v0/R0: 41.6 vs 21.2 km/s/kpc against the standard 28.75. Section 2.1 states the choice ('we take v0 = 180 km/s and 312 km/s as lower and higher estimates') but does not treat the two as corners rather than a joint credible region. A symptom the paper reports without comment: 'When varying Galactic parameters, we obtain the total mass of the MW within 50 kpc to be in the range M(<50 kpc) = (1.2-22.9)x10^11 M_sun' (Section 2.1). A factor-19 total-mass range from a factor-1.3 change in R0 and a factor-1.7 change in v0 is not a credible uncertainty band; it indicates the rigid gNFW with fixed Rs = 20 kpc is being forced to absorb the (R0, v0) mismatch. If the rho0 extremes are artifacts, the ordering claim in Section 5 is at risk: the morphology variation moves rho0 only from 0.387 to 0.471 GeV/cm3 (~20%), so a joint (R0, v0) propagation giving rho0 in, say, [0.3, 0.7] would make the (R0, v0) effect comparable to, not dominant over, morphology for direct detection. The qualitative thesis (astrophysical systematics are first-order) survives; the specific 'largest effect' ranking and the factor-32 band do not obviously survive. The paper's own 'one at a time' caveat in Section 2.1 is acknowledged but is not carried into the Section 5 conclusions.","agreement_with_reader":"agree"},"referee_report":{"model":"selfhosted/deepseek-v4.1-flash","summary":"The manuscript quantifies how uncertainties in the Milky Way's baryonic morphology and in the Galactic parameters (R0, v0) propagate into the determination of new-physics parameters in two minimal dark matter models, the Singlet Scalar (SSDM) and the Inert Doublet (IDM). The method is a global rotation-curve fit: a generalised NFW profile with fixed scale radius Rs = 20 kpc is fitted to the compilation of Iocco, Pato & Bertone using the unbinned chi-squared of Eq. (2.2), over a catalogue of observationally inferred baryonic morphologies assembled by Pato, Iocco & Bertone. The resulting (rho0, gamma) pairs are then fed into a LUX spin-independent exclusion limit computed with the maximum-gap method, and into annihilation J-factors used to rescale the Fermi GeV excess contours and to compare against the dSphs limit. The paper concludes that statistical uncertainties are negligible, that morphology variation matters mainly for indirect detection through the J-factor, and that the variation of (R0, v0) produces the largest effect on the particle-physics parameter space, chiefly through the local density rho0. The stated aim is to prompt similar systematic uncertainty propagation in more complex models.","tokens_in":23482,"tokens_out":5956,"duration_ms":120081,"significance":"The qualitative message is important and, in my view, correct: quoted WIMP limits and GeV-excess interpretations are routinely presented with astrophysical inputs held fixed, and the community would benefit from the kind of bracketing exercise performed here. The paper is well organised, the chain from rotation curve to LUX limit to J-factor is standard and correctly executed, and the use of a data-driven catalogue of baryonic morphologies rather than a single fiducial model is a genuine strength. Propagating the bracket all the way into two concrete models with relic-density consistency (Figs. 8-11) goes beyond most existing studies of this type, and the public availability of the rotation-curve compilation tool galkin supports reproducibility. If the ordering claim survives scrutiny, it is a useful cautionary result. My reservation is that the headline quantitative ordering rests on a bracketing choice that is not defended and that produces a local-density range far wider than the literature supports, so the specific numbers in the conclusions should be read as an upper bound on the effect rather than a realistic uncertainty band.","major_comments":[{"comment":"The paper's headline ordering claim in Section 5, that 'the largest effects on the SSDM and IDM parameter space are obtained as a consequence of varying the Galactic parameters (R0, v0)', rests on the two extreme rows of Table 1, which pair R0 = 7.5 kpc with v0 = 312 km/s and R0 = 8.5 kpc with v0 = 180 km/s. This is a maximally anti-correlated pairing in the well-measured combination v0/R0 (41.6 and 21.2 km/s/kpc against the standard 28.75), and it yields rho0 = 1.762 and 0.055 GeV/cm3, a factor of 32. That range is far wider than the factor of roughly two to three quoted for the local density in the review [1] that the paper itself cites. Section 2.1 justifies the individual ranges of R0 and v0 but does not justify treating the two as independent corners rather than as a joint credible region. A symptom the paper reports without comment is the total Milky Way mass range M(<50 kpc) = (1.2-22.9) x 10^11 Msun, a factor of 19 from a factor-1.3 change in R0 and a factor-1.7 change in v0; this suggests the rigid gNFW with fixed Rs is absorbing the (R0, v0) mismatch rather than reflecting a credible mass uncertainty. Since the morphology variation moves rho0 only between 0.387 and 0.471 GeV/cm3 (about 20%), the ordering claim is entirely controlled by whether the (R0, v0) bracket is realistic. I would ask the authors either to defend the anti-correlated pairing explicitly, or to present the (R0, v0) result as a deliberately conservative upper bound and to soften the ordering statement in Section 5 accordingly, and in either case to confront the resulting rho0 range with the existing literature determinations and to comment on the factor-19 mass range.","section":"Section 2.1, Table 1 rows 2-3, Section 5","authors_acknowledge":null,"authors_acknowledge_p":null},{"comment":"As written, the second term of the chi-squared in Eq. (2.2) is (xi - xt,i)^2 sigma_{x,i}^2, with the uncertainty multiplying rather than dividing the squared residual. This is dimensionally inconsistent with the first term and would make the statistic essentially insensitive to residuals in the R direction, which is precisely the direction that carries the R0 dependence. I assume this is a transcription error and that the intended form is (xi - xt,i)^2 / sigma_{x,i}^2, but because Eq. (2.2) is the fitting statistic on which every number in Table 1 depends, the correction should be made explicitly and the authors should confirm that the fits reported in Table 1 were performed with the intended expression.","section":"Section 2.1, Eq. (2.2)","authors_acknowledge":null,"authors_acknowledge_p":null},{"comment":"The indirect-detection results in Figs. 5, 9 and 11 depend on rescaling the GeV excess contours of ref. [43] by requiring that the excess flux at 2 GeV and 5 degrees from the Galactic centre be conserved. The justification given is that 'at 5 degrees away from the GC the GeV excess intensity has been shown to be almost independent on the assumption on the gNFW slope used in the data analysis', but no reference is given for that demonstration and no quantitative estimate of the residual dependence is provided. Because the rescaling is the sole bridge between the Galactic fit and the indirect-detection conclusions, and because the choice of a single off-centre angle rather than the full region of interest is a strong assumption, I would ask the authors to cite where the slope-independence at 5 degrees is established and to quantify the systematic by, for example, repeating one of the rescalings with the full region-of-interest integral and reporting the difference in the shifted contours. If the difference is small compared with the morphology-driven shift, a short statement to that effect would settle the point.","section":"Section 2.3, Fig. 5","authors_acknowledge":null,"authors_acknowledge_p":null},{"comment":"The discussion of Fig. 11 states that the region shifted by Galactic-parameter or morphology variation 'is not visible in the figure as it is forbidden by the cosmological constraint, which henceforth practically sets limits on the DM interpretation of the GC excess, but only for some combinations of the Galactic parameters.' This is a substantive claim about the IDM that is difficult to verify from the figure as presented: the reader cannot see where the shifted region went, which combinations of parameters exclude it, or how the relic-density band itself moves under the same variations. Since this is the one place where the paper reports a qualitative difference between the SSDM and IDM responses, it deserves an explicit panel or a table showing the shifted region together with the relic-density band, and a clearer statement of which parameter combinations are excluded and by how much.","section":"Section 4.2, Fig. 11","authors_acknowledge":null,"authors_acknowledge_p":null}],"minor_comments":[{"comment":"The three BjX rows list different stellar masses, M* = 4.6, 4.2 and 5.1 x 10^10 Msun, for what is described as the same reference morphology. Please explain in the table caption or the text why the baryonic mass changes when only (R0, v0) are varied.","section":"Section 2.1, Table 1","authors_acknowledge":null,"authors_acknowledge_p":null},{"comment":"The check that varying Rs by a factor of two changes rho0 by less than 5% and the J-factor by less than 10% is quoted for the reference configuration. Given the factor-19 spread in total mass reported for the extreme (R0, v0) rows, it would strengthen the paper to state whether the same check was performed for those rows, where the fit has more freedom to absorb the mismatch.","section":"Section 2.1, footnote 1","authors_acknowledge":null,"authors_acknowledge_p":null},{"comment":"The LUX limit used throughout is derived from the 2015 reanalysis of the 2013 exposure (1.4 x 10^4 kg days) rather than the 332-live-day result, for the stated reason that event-level information is not public. This is reasonable, but the abstract and introduction refer to 'current' constraints, so a sentence in Section 2.2 noting that the quoted limits correspond to the 2013 exposure would avoid overstating the currency of the bound.","section":"Section 2.2","authors_acknowledge":null,"authors_acknowledge_p":null},{"comment":"Fig. 3 uses vpeak = v0 while Figs. 8 and 10 fix vpeak = 250 km/s independently of v0. The paper notes this in passing, but it would help to state explicitly that, as a consequence, the direct-detection bands in Figs. 8 and 10 are driven by rho0 alone, so that the reader does not attribute part of the shift to the velocity distribution.","section":"Section 2.2 and Section 4","authors_acknowledge":null,"authors_acknowledge_p":null},{"comment":"The captions of Figs. 7, 10 and 11 refer to left, central and right panels, but the figures as presented appear to be single-panel. The captions should be brought into agreement with the figures actually shown, and the colour coding of the overlaid regions (statistical, Galactic, morphology) should be described in each caption rather than only in the body text.","section":"Figs. 7, 10, 11","authors_acknowledge":null,"authors_acknowledge_p":null},{"comment":"The scan range is stated as 10 GeV < mH0 < 1 TeV, while the horizontal axis of Fig. 7 extends to 10^3 GeV. Please reconcile the stated scan range with the plotted range.","section":"Section 3.2","authors_acknowledge":null,"authors_acknowledge_p":null},{"comment":"The lower integration limit in Eq. (2.4) is printed as 'vmim'; it should read vmin.","section":"Section 2.1, Eq. (2.4)","authors_acknowledge":null,"authors_acknowledge_p":null},{"comment":"Fig. 1 shows the rotation curves for the morphology variations only. Adding the curves for the two extreme (R0, v0) configurations would let the reader see directly how well or badly the fixed-Rs gNFW accommodates those data, which is central to the discussion in my first major comment.","section":"Section 2.1, Fig. 1","authors_acknowledge":null,"authors_acknowledge_p":null},{"comment":"The phrase 'Blobs of different color shading are the regions that explain the GeV excess' is imprecise; please state which colour corresponds to which variation, as is done in the caption of Fig. 11.","section":"Section 4.1","authors_acknowledge":null,"authors_acknowledge_p":null},{"comment":"There are several typographical and language slips that should be cleaned up, among them 'the target in object' in the abstract, 'elusivedark' in the introduction, 'respect to previous similar studies' (missing 'with'), 'countours' in the caption of Fig. 5, and the broken 'Table' in the caption of Table 1.","section":"General","authors_acknowledge":null,"authors_acknowledge_p":null}],"recommendation":"major_revision","confidential_remarks":"Two disclosure points for the editor. First, the GeV excess contours that underpin the indirect-detection half of the paper are taken from ref. [43], which shares a co-author with this manuscript; the rescaling procedure is the authors' own and is only lightly justified, which is why I have raised it as a major comment rather than treating it as a cited result. Second, the paper's central ordering claim is, in my reading, defensible in spirit but overstated in its present quantitative form; I would expect a revised version to retain the qualitative message while presenting the (R0, v0) bracket explicitly as a conservative upper bound. Neither point bears on the authors' integrity, and both are fixable within the present scope."},"author_rebuttal":null,"desk_editor":{"model":"selfhosted/deepseek-v4.1-flash","letter":"Worth your time, with one number you should not quote as-is. The paper's real contribution is the taxonomy: it separates statistical uncertainty, Galactic-parameter uncertainty, and baryonic-morphology uncertainty, and propagates each into the Singlet Scalar and Inert Doublet parameter spaces via LUX limits and J-factors. That is a clean, honest piece of bookkeeping, and the qualitative conclusion — that morphology and (R0, v0) move the constrained region by amounts comparable to the particle physics effect being constrained — holds up. The morphology result for indirect detection is the more robust half: the J-factor shifts by more than an order of magnitude inside a few degrees, and that is a real, useful warning for anyone interpreting the GC excess against dSphs. The pipeline itself is standard and correctly run: gNFW fit to the rotation curve with the unbinned chi-squared of Eq. 2.2, then propagation. Nothing is circular; the GeV excess contours are rescaled from Calore et al. with a stated procedure, and the relic density is computed from the model. The authors are also upfront in Section 2.1 that they vary one source at a time, and that the scale radius is held fixed at 20 kpc — both acknowledged, both fair caveats. Where I part company is the Section 5 ranking. The claim that (R0, v0) variation dominates comes almost entirely from rho0 = 1.762 and 0.055 GeV/cm3 in Table 1, which is a factor of 32. Those two rows pair 7.5 kpc with 312 km/s and 8.5 kpc with 180 km/s — maximally anti-correlated in v0/R0, which is the combination the rotation curve actually pins down. The paper's own reported Milky Way mass range, (1.2–22.9) x 10^11 solar masses, is the tell: a factor-19 spread from a factor-1.3 change in R0 and a factor-1.7 change in v0 means the rigid gNFW is absorbing the mismatch, not measuring an uncertainty. Read those rows as corners of a scan, not a credible band. A joint propagation would likely put the (R0, v0) effect at roughly the morphology level for direct detection, not above it. Two smaller things: the IDM claim in Section 4.2 that the shifted region fails the relic-density constraint is asserted without showing the shifted points, and no code or data accompanies the fitting, the LUX reanalysis, or the scans. Neither is fatal. Who should read it: anyone who quotes WIMP limits or excess interpretations without an astrophysical error bar, and anyone working on the GC excess. Send it out. The referees should press hard on the (R0, v0) pairing and ask for the joint propagation, but the paper deserves the review.","headline":"A useful, correctly executed demonstration that Galactic systematics are first-order in WIMP constraints — but the headline 'largest effect' ranking rests on an anti-correlated (R0, v0) pairing that inflates the local-density band by roughly an order of magnitude.","tokens_in":24322,"tokens_out":948,"would_cite":true,"duration_ms":20686,"reading_group":"yes","serious_thinker":"yes","would_accept_peer_review":true},"pith_extraction":{"msc":[],"pacs":["95.35.+d","98.35.Gi","14.80.-j"],"model":"selfhosted/deepseek-v4.1-flash","headline":"The bounds physicists place on dark matter particles move when the Milky Way's own uncertain size and rotation speed are varied, and the paper argues those shifts are large enough that they should be quoted alongside every WIMP limit.","keywords":["dark matter direct detection","dark matter indirect detection","Milky Way dark matter density","Galactic rotation curve","astrophysical uncertainties","singlet scalar dark matter","inert doublet model","WIMP parameter space"],"falsifier":"A joint fit of the Milky Way rotation curve that treats the Solar galactocentric distance and the circular speed with their measured correlation, and marginalises over the full baryonic model space, would yield a credible interval on the local dark matter density. If that interval turns out far narrower than 0.055 to 1.762 GeV/cm$^3$, the size of the reported shifts in the Singlet Scalar and Inert Doublet parameter spaces shrinks in proportion, and the paper's headline claim weakens accordingly.","tokens_in":24369,"feed_emoji":"🌌","tokens_out":2971,"duration_ms":59698,"temperature":0.7,"pith_summary":"Every limit on a dark matter particle rests on a number nobody has measured precisely: how much dark matter sits near the Sun, and how it is distributed toward the Galactic Centre. This paper takes the current spread in the Sun's distance from the Galactic Centre, the local circular speed, and the shape of the stellar bulge and disk, refits the Milky Way's dark matter profile for each choice, and carries the resulting spread all the way through to the parameter space of two concrete particle models, the Singlet Scalar and the Inert Doublet. The result is that the quoted statistical error on the local density is nearly irrelevant, while the disagreements between plausible Galactic geometries and parameters move the exclusion regions and the favoured regions by amounts comparable to, and sometimes larger than, the particle-physics effects being constrained. The practical message is that a WIMP limit quoted without an astrophysical error band is understating its own uncertainty, and that a claimed tension between a Galactic Centre excess and dwarf-galaxy limits can be created or dissolved by choices that have nothing to do with particle physics.","feed_headline":"WIMP limits swing with the Milky Way's uncertain size and speed","feed_subtitle":"Changing the Sun's distance from the galactic centre and the circular speed moves dark matter bounds by factors.","key_machinery":"The machinery is a two-stage propagation. First, a global rotation-curve fit: for each combination of stellar bulge, stellar disk and gaseous disk models, the authors scan the local density $rho_0$ and the inner slope $gamma$ of a generalised NFW profile with fixed scale radius $R_s = 20$ kpc, comparing the total baryon-plus-dark-matter rotation curve to a compilation of observed data through an unbinned two-dimensional $chi^2$ built on the reduced variables $x = R/R_0$ and $y = w/w_0 - 1$, where $w = v_c/R$ is the angular velocity. Second, the fitted profiles are inserted into the two observables that carry astrophysics: the combination $rho_0 eta(v_{min})$ entering the spin-independent direct-detection rate, and the line-of-sight integral $J_{annih} = int rho_{DM}^2 , dl$ entering the gamma-ray flux. Those two numbers then rescale the LUX exclusion curve and the GeV-excess contours, and the rescaled curves are projected onto the $(m_S, lambda_{HS})$ and $(|lambda_L|, m_{H^0})$ planes of the two benchmark models.","core_discovery":"The paper's central claim is that Galactic uncertainties propagate into new-physics parameter determination at a level that matters. Working with a generalised NFW profile, the authors fit the observed rotation curve for a catalogue of baryonic morphologies and for extreme choices of the Solar galactocentric distance and circular speed, obtaining local dark matter densities spanning $0.055$ to $1.762$ GeV/cm$^3$ against a reference value of $0.466$ GeV/cm$^3$. Feeding these into a reanalysis of the 2013 LUX exposure, they find the spin-independent exclusion curve in the mass–cross-section plane shifts by more than the statistical band, with the largest shift coming from the Galactic-parameter variation rather than from morphology. Feeding them instead into the annihilation $J$-factor, they find that within a few degrees of the Galactic Centre the astrophysical uncertainty on $J$ exceeds a factor of ten, and that the region of the Singlet Scalar parameter space able to explain the Galactic Centre GeV excess moves in and out of tension with the dwarf-spheroidal limits. For the Inert Doublet, the shifted regions often land where the relic-abundance constraint forbids them, so the cosmological bound rather than the Galactic one ends up doing the excluding. The authors are explicit that they vary one source of uncertainty at a time rather than constructing a joint statistical interval.","pith_inferences":["The paper's own framing suggests a discipline for the field: report every limit as a band whose width is set by the Galactic inputs, in the same way experimental collaborations already report detector systematics. A limit quoted as a single curve is, on this argument, an incomplete result.","The anti-correlated pairing of the extreme parameters, with the smallest Solar radius against the fastest circular speed and the largest radius against the slowest, maximises the spread in local density. A joint fit with realistic correlations between the two would give a narrower band, so the headline numbers here are best read as an upper bound on the astrophysical systematic rather than a credi","The same propagation applies to any channel whose signal scales with density or density squared, including antiprotons, neutrinos from the Sun, and charged cosmic-ray sources, so the qualitative conclusion should transfer even though only gamma rays are computed here.","Because the morphology choice dominates the $J$-factor but not the local density, a future analysis that measures the bulge and disk geometry independently would tighten indirect constraints without touching direct-detection uncertainties, and vice versa."],"forward_implications":["Published WIMP exclusion limits and Galactic Centre excess interpretations should carry an explicit astrophysical error band, since the Galactic-parameter spread alone moves them by more than their statistical uncertainty.","A tension between a Galactic Centre signal and dwarf-spheroidal limits is not by itself evidence against a dark matter interpretation, because the $J$-factor uncertainty near the Galactic Centre exceeds a factor of ten.","For the Inert Doublet, some combinations of Galactic parameters push the GeV-excess region into conflict with the relic-abundance constraint, so the cosmological bound can do the excluding that was attributed to direct or indirect searches.","Because morphology dominates the $J$-factor uncertainty while Galactic parameters dominate the local-density uncertainty, the two detection channels need different error budgets rather than a single shared one.","Improved determinations of the Oort constants and of the Solar galactocentric distance, of the kind expected from Gaia, would shrink the dominant systematic without any new dark matter data."],"supporting_citations":[{"why":"Supplies the global rotation-curve methodology and the catalogue of data-driven baryonic morphologies that the whole fit is built on.","marker":"[2]"},{"why":"Provides the observed rotation-curve compilation and the unbinned two-dimensional chi-square statistic used to fit the dark matter profile.","marker":"[6]"},{"why":"Motivates the adopted Maxwellian peak-speed range of 223 to 289 km/s, decoupled from the local circular speed, for the direct-detection analysis.","marker":"[7]"},{"why":"The 2013 LUX reanalysis whose published event selection and efficiency are reproduced to derive the exclusion curve that is then rescaled.","marker":"[37]"},{"why":"Supplies the local Galactic escape speed of 533 km/s used to truncate the velocity distribution.","marker":"[36]"},{"why":"Provides the dwarf-spheroidal annihilation limits against which the rescaled Galactic Centre excess contours are compared.","marker":"[41]"},{"why":"Supplies the GeV-excess contours and the rescaling prescription at 5 degrees from the Galactic Centre that fixes the excess flux.","marker":"[43]"},{"why":"The Planck relic-abundance measurement that defines which parameter points survive in both benchmark models.","marker":"[64]"}],"fun_headline_variants":["Galactic parameter shifts move dark matter exclusion curves","Milky Way inputs shift LUX limits beyond statistical band","J-factor uncertainty exceeds tenfold near Galactic Centre","Galactic shifts outweigh morphology in LUX dark matter limits","One-at-a-time Galactic shifts move new-physics bounds"],"cache_read_input_tokens":0,"weakest_assumption_plain":"The load-bearing premise is that the two extreme pairs, a Solar radius of 7.5 kpc with a circular speed of 312 km/s and a radius of 8.5 kpc with 180 km/s, bracket the credible Galactic uncertainty, so that the resulting local densities of 1.762 and 0.055 GeV/cm$^3$ represent an uncertainty band rather than two deliberately anti-correlated corners of parameter space; the authors do acknowledge that they vary one source of uncertainty at a time instead of building a joint statistical interval.","fun_headline_variants_meta":{"raw":{"variants":["Galactic parameter shifts move dark matter exclusion curves","Milky Way inputs shift LUX limits beyond statistical band","J-factor uncertainty exceeds tenfold near Galactic Centre","Galactic shifts outweigh morphology in LUX dark matter limits","One-at-a-time Galactic shifts move new-physics bounds"]},"model":"selfhosted/deepseek-v4.1-flash","effort":"low","attempts":1,"cost_usd":0.0,"raw_usage":{"total_tokens":2328,"prompt_tokens":1060,"completion_tokens":1268,"prompt_tokens_details":null,"completion_tokens_details":{"reasoning_tokens":1204}},"tokens_in":1060,"tokens_out":1268,"duration_ms":29245,"image_pages":[],"temperature":1.0,"reasoning_budget":50,"reasoning_tokens":1204,"transport_provider":"selfhosted","cache_read_input_tokens":0,"cache_creation_input_tokens":0},"cache_creation_input_tokens":0},"created_at":"2026-11-09T12:52:51.360563+00:00","model_set":{"reader":"selfhosted/deepseek-v4.1-flash"},"falsifier":"A joint fit of the Milky Way rotation curve that treats the Solar galactocentric distance and the circular speed with their measured correlation, and marginalises over the full baryonic model space, would yield a credible interval on the local dark matter density. If that interval turns out far narrower than 0.055 to 1.762 GeV/cm$^3$, the size of the reported shifts in the Singlet Scalar and Inert Doublet parameter spaces shrinks in proportion, and the paper's headline claim weakens accordingly.","supporting_citations":[{"cited_title":"Dynamical constraints on the dark matter distribution in the Milky Way","cited_arxiv_id":"1504.06324","evidence_quote":"Supplies the global rotation-curve methodology and the catalogue of data-driven baryonic morphologies that the whole fit is built on."},{"cited_title":"Evidence for dark matter in the inner Milky Way","cited_arxiv_id":"1502.03821","evidence_quote":"Provides the observed rotation-curve compilation and the unbinned two-dimensional chi-square statistic used to fit the dark matter profile."},{"cited_title":"Simulated Milky Way analogues: implications for dark matter direct searches","cited_arxiv_id":"1601.04707","evidence_quote":"Motivates the adopted Maxwellian peak-speed range of 223 to 289 km/s, decoupled from the local circular speed, for the direct-detection analysis."},{"cited_title":"Improved Limits on Scattering of Weakly Interacting Massive Particles from Reanalysis of 2013 LUX data","cited_arxiv_id":"1512.03506","evidence_quote":"The 2013 LUX reanalysis whose published event selection and efficiency are reproduced to derive the exclusion curve that is then rescaled."},{"cited_title":"The RAVE survey: the Galactic escape speed and the mass of the Milky Way","cited_arxiv_id":"1309.4293","evidence_quote":"Supplies the local Galactic escape speed of 533 km/s used to truncate the velocity distribution."},{"cited_title":"SEARCHING FOR DARK MATTER ANNIHILATION IN RECENTLY DISCOVERED MILKY WAY SATELLITES WITH FERMI-LAT","cited_arxiv_id":"1611.03184","evidence_quote":"Provides the dwarf-spheroidal annihilation limits against which the rescaled Galactic Centre excess contours are compared."},{"cited_title":"A Tale of Tails: Dark Matter Interpretations of the Fermi GeV Excess in Light of Background Model Systematics","cited_arxiv_id":"1411.4647","evidence_quote":"Supplies the GeV-excess contours and the rescaling prescription at 5 degrees from the Galactic Centre that fixes the excess flux."},{"cited_title":"Planck 2015 results. XIII. Cosmological parameters","cited_arxiv_id":"1502.01589","evidence_quote":"The Planck relic-abundance measurement that defines which parameter points survive in both benchmark models."}],"review_version":1}