{"id":"7b7cb5ae-8f9d-4ae4-aee7-083d04dea9d1","arxiv_id":"1908.10295","paper_version":1,"verdict":"CONDITIONAL","confidence":"HIGH","novelty_score":6.0,"correctness_risk":"low","formal_verification":"none","parameter_count":5,"one_line_summary":"A homogeneous Fabry-Perot Hα kinematic survey of 152 Herschel Reference Survey galaxies yields rotation curves, Tully-Fisher relations, baryonic-to-dynamical mass scaling, and the first dynamical mass main sequence.","lead":"This paper presents new high-resolution measurements of gas motion inside 152 nearby galaxies, delivering rotation curves and velocity maps for a complete reference sample. It uses them to test and extend standard galaxy scaling relations, including a new star-forming main sequence based on total dynamical mass.","discovery_kind":"new_application","skeptic_critique":{"model":"deepseek-v4-flash","headline":"Fixed spherical α=1.0 in Eq. (9) is not propagated; if α is mass-dependent, the headline slopes and baryon-fraction trend shift beyond quoted errors.","rationale":"The paper's real deliverable is an homogeneous Hα kinematic catalog and validation via TF relations; those parts are independently supported by the HI Vmax comparison (§5.1) and by agreement with literature TF slopes, and they do not depend on α. The genuinely new claims — the Mbar-Mdyn slope and the dynamical main sequence — inherit their x-axis from Eq. (9), so the fixed-α choice is the most load-bearing assumption. The reader's weakest_assumption identifies exactly this, and I find no separate flaw of comparable weight. The concern is not that α=1 is wrong for every galaxy; it is that the paper provides no evidence that α is mass-independent, and plausible morphology trends imply a mass-dependent α that would alter the quoted slopes and the baryon-fraction trend. This warrants a robustness test but not rejection, because the published data and public products allow the test to be run without new observations. Verdict unchanged: conditional acceptance pending the α-propagation check.","tokens_in":55685,"tokens_out":4943,"duration_ms":54869,"concrete_test":"Refit the Section 5.4/5.5 relations (Tables 6 and 7, Figs 12 and 14) using per-galaxy α estimated from available HRS photometry: assign α=0.6 to disk-dominated (low bulge-to-total, B/T<0.2) galaxies, α=1.0 to bulge-dominated (B/T>0.5), interpolating between, or preferably fit a two-component disk+bulge mass model to derive α for each galaxy. If the Mbar-Mdyn slope or the dynamical main-sequence slope shifts by more than the quoted 1σ uncertainties (0.12 and 0.19 respectively), the published values need a propagated systematic term. A constant-α=0.6 rerun alone would isolate the zero-point shift but would not test the mass-dependence that is the actual threat to the slopes.","verdict_should_be":"UNCHANGED","load_bearing_attack":"Section 5.4 computes every dynamical mass with Eq. (9), Mdyn = α ropt Vmax^2/G, fixing α=1.0 (spherical) and only plotting the 0.6≤α≤1.0 range as a shaded band. This choice is load-bearing because Mdyn is the x-axis in the main-sequence fits (Table 7, Fig. 14) and the independent variable in the Mbar-Mdyn fit (Table 6, Fig. 12). A constant α would only shift zero points, but the paper gives no argument that α is constant across the sample. The Lequeux coefficient is meant to interpolate between flat (disk, α≈0.6) and spherical (α≈1.0) mass distributions. The low-mass, gas-rich, late-type galaxies that dominate the low-Mdyn end are exactly the systems expected to be disk-dominated, while massive bulge-dominated galaxies should be closer to spherical. If α therefore increases with Mdyn, the quoted slope 1.11±0.12 is biased: the measured log Mdyn = log Mdyn_true − log α introduces a term that decreases with true mass. The same mechanism biases the SFR-Mdyn main-sequence slope 0.87±0.19. It also changes the baryon-fraction trend: Fig. 13 reports ~20–25% baryon fractions at log Mdyn < 10.5; if those galaxies have α≈0.6, their true fractions are ~1.7 times larger, potentially erasing the reported rise with mass. The text acknowledges these as rough approximations but does not propagate the 0.6≤α≤1.0 systematic into any quoted parameter.","agreement_with_reader":"agree"},"referee_report":{"model":"deepseek-v4-flash","summary":"Gómez-López et al. present Fabry-Perot Hα datacubes, velocity fields, and rotation curves for 152 HRS star-forming galaxies observed at OHP, and combine these with 40 literature galaxies to reach 192/261 (73.6%) of the HRS late-type sample. The data reduction includes Voronoi adaptive binning, sky-line subtraction, FSR corrections, and a Monte-Carlo residual-field method for parameter uncertainties. Kinematic parameters are derived from a modified Zhao model, and Vmax from a modified Courteau profile. The internal validation is thorough: Vmax,Hα versus Vmax,HI has slope 0.9975±0.01 for Flag A objects, and the i-band, 3.6 μm, stellar, and baryonic Tully-Fisher relations agree with literature samples (Masters et al. 2006, Sorce et al. 2014, McGaugh et al. 2000, Bell & de Jong 2001) and with EAGLE predictions. The paper then uses Mdyn = α ropt Vmax^2/G, fixing α = 1.0 (with 0.6 ≤ α ≤ 1.0 shown as a shaded band), to derive the Mbar-Mdyn relation (slope 1.11±0.12), baryon-fraction trends, and the baryonic and dynamical main sequences (SFR-Mdyn slope 0.87±0.19).","tokens_in":56040,"tokens_out":8378,"duration_ms":88781,"significance":"The survey products are a valuable community resource, and the kinematic pipeline is careful: parameters carry Monte-Carlo uncertainties, quality flags are assigned by an automatic procedure, and the external HI and Tully-Fisher cross-checks are convincing. Public availability through HeDAM and the Fabry-Perot database further strengthens the contribution. If the α systematic is properly propagated, the Mbar-Mdyn relation and the first dynamical main sequence on a representative local sample would be useful constraints for galaxy formation models and simulations. The key validations are against independent external data and published calibrations, so I do not see a circularity problem. The main weakness is that the dynamical-mass-based relations depend on a single fixed α with no propagated systematic error.","major_comments":[{"comment":"The dynamical masses used in the Mbar-Mdyn relation and in the Mdyn main sequence are computed with Mdyn = α ropt Vmax^2/G adopting α = 1.0 for every galaxy, with the 0.6 ≤ α ≤ 1.0 range shown only as a shaded band. This is load-bearing: α is meant to interpolate between disk-like (α ≈ 0.6) and spherical (α ≈ 1.0) mass distributions, and the low-mass, gas-rich galaxies at the low-Mdyn end are exactly the systems expected to be disk-dominated, whereas massive bulge-dominated galaxies should be closer to spherical. If α therefore increases with Mdyn, the slope 1.11±0.12 of the Mbar-Mdyn relation and the slope 0.87±0.19 of the SFR-Mdyn main sequence are biased, and the reported rising baryon fraction with Mdyn in Fig. 13 could be weakened or erased because low-mass galaxies with α ≈ 0.6 would have true baryon fractions roughly 1.7 times larger. I request a quantitative treatment: either propagate a per-galaxy α prior (for example based on morphology or bulge-to-total light ratio), or at minimum quote all fit parameters for both α = 0.6 and α = 1.0 and add a systematic error term to the headline slopes and baryon fractions.","section":"Section 5.4, Eq. (9), Tables 6-7, Figs. 12-14"},{"comment":"After defining the quality flags, the analysis deliberately excludes Flag B and HI-deficient (HI-Def > 0.4) galaxies. These objects are preferentially cluster members with truncated gas discs, so the resulting 123-object sample is not the full HRS and may be biased at the low-mass, high-environment end. Since the abstract and conclusions claim representative local-universe relations, the paper should either qualify the claims as applying to unperturbed systems or show that re-including these galaxies (with appropriate weights or as a robustness test) does not change the fitted slopes and zero points. At minimum, the paper should quantify what fraction of the HRS star-forming population is excluded and discuss the possible selection effect on the reported slopes.","section":"Section 5.1 and Tables 6-7"}],"minor_comments":[{"comment":"There are several typographical errors, including “constitue,” “avalibale,” “gouverned,” and “OSL” where “OLS” is intended; a careful proofreading pass is needed.","section":"Throughout"},{"comment":"The sentence “the SFR is studied considering the mean value derived using the three tracers Mdyn, Mbar and Mstar” should read “the three mass estimators,” since SFR is a single physical quantity and the three quantities are galaxy mass tracers.","section":"Section 5.5"},{"comment":"The baryonic mass definition in the Table 5 note, Mbar = Mstar + 1.4(MHI + MH2) + Mz + Mdust, appears inconsistent with Eqs. (6)-(7), where the factor 1/(1-Y-Z) already accounts for both helium and metals; please clarify whether Mz is double-counted.","section":"Table 5 note"},{"comment":"The text reports an “intrinsic scatter” of 0.82 for the full sample and 0.11 for Flag A galaxies; the units and definition of this scatter should be stated explicitly, since it does not have the usual dex units of a log-log relation.","section":"Section 5.1, Fig. 7"}],"recommendation":"major_revision","confidential_remarks":"Recommendation: major revision. The observational core and kinematic pipeline are solid, and the external HI and Tully-Fisher validations are convincing. The main obstacle is the unpropagated α systematic in Section 5.4, which directly affects the headline Mbar-Mdyn slope, the dynamical main-sequence slope, and the baryon-fraction trend. The exclusion of Flag B and HI-deficient galaxies also needs explicit qualification of the “representative” claim. I do not see circularity or data-integrity concerns; the paper fits the journal's scope."},"author_rebuttal":null,"desk_editor":{"model":"deepseek-v4-flash","letter":"The HRS kinematic dataset is the real deliverable; the derived scaling relations need one robustness pass on the α coefficient before their slopes are quoted.\n\nWhat is actually new: 152 Fabry-Perot datacubes and rotation curves for HRS galaxies, combined with 40 literature objects to give 192 systems (73.6% of the star-forming sample). The pipeline is careful—Voronoi binning, Monte Carlo uncertainties from residual power spectra, and the HI cross-check (slope 1.00 ± 0.01 for Flag A) is convincing. The TF comparisons against luminosity-matched subsamples of Masters et al. and Sorce et al. are well done. The baryonic mass with directly measured dust and metals is a first for a sample this size. The data are public through HeDAM; that is reproducible evidence and worth real credit.\n\nSoft spots: the stress-test concern is correct. The paper fixes α=1.0 in Mdyn = α ropt Vmax²/G and shows a 0.6–1.0 shaded band, but it does not propagate that range into any fitted result. Since Mdyn is the x-axis of the main sequence and the independent variable in the Mbar–Mdyn fit, a mass-dependent α (disks at low mass, spheroids at high mass) can shift the slopes and the baryon-fraction trend beyond the quoted 1σ. The paper acknowledges the approximation in words but not in numbers. That is fixable: run the fits with α=0.6 and with a simple α(Mdyn), and report both. The sample restriction to non-HI-deficient, non-Flag B objects is defensible for unperturbed systems, but it does mean the claim of a 'representative sample' should be phrased relative to that cut. The three main-sequence fits use different subsamples depending on which mass tracer is available; the text says the slopes are comparable, but the samples are not identical, so that comparison is a bit looser than Table 7 suggests.\n\nCitation pattern looks fine: heavy use of their own earlier pipeline papers is normal here, and the external checks (HI, TF, EAGLE) are genuine benchmarks. No circularity.\n\nBottom line: the survey is a valuable, well-executed dataset that deserves peer review. The scaling relations need a robustness test on α. Send it to a referee; ask for that test in the first round. Would I cite it? Yes, for the rotation curves and the TF comparisons.","headline":"The HRS kinematic dataset is the real deliverable; the derived scaling relations need a robustness pass on the α coefficient before their slopes are quoted.","tokens_in":56667,"tokens_out":3555,"would_cite":true,"duration_ms":38797,"reading_group":"yes","serious_thinker":"yes","would_accept_peer_review":true},"rs_alignment":null,"lean_confirmation":null,"pith_extraction":{"msc":[],"pacs":[],"model":"deepseek-v4-flash","headline":"This paper builds a homogeneous Hα kinematic sample of 152 nearby star-forming galaxies and uses it to tie baryonic mass to dynamical mass and to define the first dynamical main sequence.","keywords":["galaxy kinematics","rotation curves","Tully-Fisher relation","dynamical mass","baryonic mass","star-forming galaxies","Fabry-Perot spectroscopy","Herschel Reference Survey"],"falsifier":"Take a subset of roughly twenty HRS galaxies with resolved H I rotation curves extending beyond the optical radius, fit disk-plus-bulge-plus-dark-halo mass models, and recover Mdyn independently of the α prescription; if the implied α is systematically below 1 or varies with mass, the reported Mbar-Mdyn slope and the dynamical main sequence will not reproduce.","tokens_in":55464,"feed_emoji":"🌌","tokens_out":7306,"duration_ms":74766,"temperature":0.7,"pith_summary":"Using Fabry-Perot Hα observations of 152 star-forming galaxies from the Herschel Reference Survey, the paper constructs a homogeneous set of 2D velocity fields and rotation curves; combined with 40 galaxies from the literature, this covers 73.6% of the HRS star-forming sample. The paper argues these data are accurate enough that maximum velocities from Hα and H I agree, and that the sample reproduces the i-band, near-infrared, stellar, and baryonic Tully-Fisher relations found from much larger heterogeneous samples. From the same data it derives a baryonic-to-dynamical mass relation with slope 1.11 ± 0.12 and, for the first time, baryonic and dynamical mass main sequences for a representative local sample. A reader should care because this turns the HRS into a local reference anchor for scaling relations connecting gas, stars, and dark matter on a statistical basis.","feed_headline":"152 galaxies yield homogeneous rotation curves and mass relations","feed_subtitle":"The first dynamical main sequence connects star formation to total mass on a representative local sample.","key_machinery":"The load-bearing machinery is the combination of Voronoi-tessellation adaptive binning that preserves spatial resolution in bright H II regions while recovering faint diffuse emission; a tilted-ring kinematical model in which the observed velocity is $V_{\\mathrm{obs}}(r) = V_{\\mathrm{sys}} + V_{\\mathrm{rot}}(r)\\cos\\theta\\,\\sin i$ with $V_{\\mathrm{rot}}(r)$ given by a modified Zhao function, fitted by Levenberg-Marquardt $\\chi^2$ minimization; a modified Courteau profile $v(r) = v_c (1 + r_t/r)^\\beta (1 + (r_t/r)^\\gamma)^{1/\\gamma}$ with $\\beta=0$ to define $V_{\\mathrm{max}}$ from the rotation curve; Monte-Carlo uncertainty estimates from the power spectrum of residual velocity fields; and the dynamical-mass estimator $M_{\\mathrm{dyn}} = \\alpha\\, r_{\\mathrm{opt}} V_{\\mathrm{max}}^2 / G$ with $\\alpha = 1.0$ for all galaxies, the $0.6 \\le \\alpha \\le 1.0$ range being shown as a shaded band. The machinery converts several thousand independent velocity measurements per galaxy into one robust $V_{\\mathrm{max}}$ and one $M_{\\mathrm{dyn}}$ per galaxy.","core_discovery":"On the paper's own terms, the discovery is that a complete, K-band-selected local sample can yield homogeneous Hα kinematics with quality sufficient to measure global scaling relations: the maximum rotation velocity Vmax derived from a Courteau-profile fit to the Hα rotation curve is statistically indistinguishable from Vmax measured from H I line widths for unperturbed galaxies, and the resulting i-band and 3.6 µm Tully-Fisher relations match literature templates once luminosity distributions are matched. Combining these kinematics with directly measured baryonic components (stars, atomic and molecular gas, helium, metals, dust), the paper finds Mbar ∝ $Mdyn^{1}$.11±0.12 with roughly 0.12 dex scatter and a baryon fraction that rises with dynamical mass; it then introduces the baryonic and dynamical main sequences, where star formation rate scales with baryonic and dynamical mass with nearly the same slope and scatter as the stellar main sequence. The intended significance is that galaxy evolution can be phrased in dynamical rather than stellar mass terms on a statistically representative local sample.","pith_inferences":["I infer that if a disc-like correction (α ≈ 0.6) applies, the zero point of the baryonic-to-dynamical mass relation shifts by about 0.22 dex and the reported baryon fractions roughly double; the qualitative trend that low-mass systems are more gas-dominated would likely survive, but the absolute baryon fractions should not be read as model-independent.","I infer that a mass-dependent α would change the slope of the dynamical main sequence, so fitting resolved mass models (disk plus bulge plus dark halo) on a subsample is a direct test the paper leaves open.","I infer that the homogeneous Vmax catalog is a natural local anchor for high-redshift kinematic surveys, provided they adopt the same Vmax definition, namely a Courteau-profile fit within the optical radius.","I infer that because the sample is K-band-selected and volume-limited, the baryonic and dynamical main sequences could separate mass-driven from environment-driven quenching by comparing Virgo and field galaxies at fixed Mdyn."],"forward_implications":["The remaining 26.4% of the HRS without Fabry-Perot data can be added to statistical studies using H I line widths, since Vmax,Hα matches Vmax,HI for unperturbed objects.","The HRS can serve as a local reference for Tully-Fisher calibrations, giving i-band and 3.6 µm slopes consistent with larger samples once luminosity selection is matched.","Baryonic masses assembled from direct measurements of stars, atomic and molecular gas, helium, metals, and dust make baryon fractions an observable function of dynamical mass rather than an assumed input.","The main sequence of star formation can be expressed in terms of dynamical mass, extending the classic SFR-stellar-mass relation to a mass tracer closer to the total halo scale.","The roughly unit slope of the baryonic-to-dynamical mass relation and its small scatter give local constraints for models of galaxy formation that predict how baryons are distributed within dark-matter halos."],"supporting_citations":[{"why":"Defines the Herschel Reference Survey sample and its completeness.","marker":"Boselli et al. (2010)"},{"why":"Supplies the kinematical modelling and rotation-curve extraction method adapted here.","marker":"Epinat et al. (2008b)"},{"why":"Provides the residual power-spectrum and Monte-Carlo uncertainty estimation.","marker":"Epinat et al. (2008a)"},{"why":"Provides the homogenised H I line widths and gas masses used for comparison and baryonic mass assembly.","marker":"Boselli et al. (2014a)"},{"why":"Supplies stellar masses, morphological parameters, and optical radii used in the fits.","marker":"Cortese et al. (2012)"},{"why":"Provides Hα photometry used to flux-calibrate the Fabry-Perot datacubes.","marker":"Boselli et al. (2015)"},{"why":"Supplies dust masses from SED fitting used in the baryonic mass budget.","marker":"Ciesla et al. (2014)"},{"why":"Supplies metallicities used to compute the metal mass component.","marker":"Hughes et al. (2013)"},{"why":"Provides the i-band Tully-Fisher template and comparison sample.","marker":"Masters et al. (2006)"},{"why":"Provides the dynamical-mass formula Mdyn = α ropt Vmax^2 / G used throughout.","marker":"Lequeux (1983)"}],"fun_headline_variants":["First dynamical main sequence ties mass and star formation","Baryon fraction rises with dynamical mass in 152 galaxies","Dynamical main sequence: star formation scales with total mass","Baryonic and dynamical main sequences from 152 galaxies","Mass relations from 152 Hα velocity fields"],"cache_read_input_tokens":3200,"weakest_assumption_plain":"Dynamical masses are computed with a single spherical-mass coefficient α = 1.0 for every galaxy; if galaxies instead behave like flattened discs (α ≈ 0.6), every dynamical mass shrinks by 40% and the quoted scaling relations shift.","fun_headline_variants_meta":{"raw":{"variants":["First dynamical main sequence ties mass and star formation","Baryon fraction rises with dynamical mass in 152 galaxies","Dynamical main sequence: star formation scales with total mass","Baryonic and dynamical main sequences from 152 galaxies","Mass relations from 152 Hα velocity fields"]},"model":"deepseek-v4-flash","effort":"low","cost_usd":0.001362,"raw_usage":{"total_tokens":5563,"prompt_tokens":1018,"completion_tokens":4545,"prompt_tokens_details":{"cached_tokens":384},"prompt_cache_hit_tokens":384,"prompt_cache_miss_tokens":634,"completion_tokens_details":{"reasoning_tokens":4466}},"tokens_in":634,"tokens_out":4545,"duration_ms":35165,"temperature":1.0,"reasoning_tokens":4466,"cache_read_input_tokens":384,"cache_creation_input_tokens":0},"cache_creation_input_tokens":0},"created_at":"2026-08-14T10:47:58.274146+00:00","model_set":{"reader":"deepseek-v4-flash"},"falsifier":"Take a subset of roughly twenty HRS galaxies with resolved H I rotation curves extending beyond the optical radius, fit disk-plus-bulge-plus-dark-halo mass models, and recover Mdyn independently of the α prescription; if the implied α is systematically below 1 or varies with mass, the reported Mbar-Mdyn slope and the dynamical main sequence will not reproduce.","supporting_citations":[],"review_version":1}