{"id":"7b2073da-fb2f-4002-8258-d11b1ddde147","arxiv_id":"2505.12563","paper_version":1,"verdict":"CONDITIONAL","confidence":"MODERATE","novelty_score":5.0,"correctness_risk":"medium","formal_verification":"none","parameter_count":6,"one_line_summary":"Dynamical masses and improved orbits are determined for seven nearby star systems by jointly fitting thousands of radial velocities with Hipparcos and Gaia proper motion anomalies.","lead":"This paper combines 35 years of radial velocity data with space-based astrometry to measure component masses of four binary stars and true masses of three giant planets. It adds over 1,100 new NEID and MINERVA observations to public archives, refining the orbital solutions for seven nearby systems.","discovery_kind":"new_application","skeptic_critique":{"model":"deepseek-v4-flash","headline":"HD 154345 b's claimed true mass is the weak link: its astrometric detection lies at the sample's χ²HG>11.8 selection threshold, and the reported mass/inclination posterior appears to imply an RV m sin i inconsistent with the 0.905 MJ value cited in the paper.","rationale":"This paper is careful and data-rich: it combines 4963 RVs, 1721 relative astrometry points, and public orvara-based fits, and the stellar masses for HD 68017, 61 Cygni, and HD 4614 are largely model-independent and credible. The planetary true-mass claims, however, all inherit the absolute astrometry, and the statistical floor is set by HD 154345. A sample selected on χ²>11.8 cannot be treated as though the measured acceleration of a system with χ²=12.8 is unbiased. The internal m sin i discrepancy is the most concrete symptom that this bias has bitten: a 1.186 MJ planet at i≈88° would require an RV semi-amplitude roughly 30% larger than the published 0.905 MJ solution. The paper compares with Xiao et al. (2023) in Section 5.7 but never checks whether its joint posterior reproduces the RV-only minimum mass. If the proposed check fails, the abstract's 'true masses for three planets' should be softened to two, with HD 154345 b flagged as tentative; if it passes, the concern is resolved. The reader's CONDITIONAL verdict is therefore the right level: the stellar results are strong, the data release is valuable, but the marginal astrometric case needs explicit validation before the planetary headline is taken at face value.","tokens_in":47775,"tokens_out":7667,"duration_ms":83179,"concrete_test":"From the published MCMC chains (Table 7 and Figure A7) compute the posterior distribution of m sin i = Msec sin i for HD 154345 b. If the median is not within 2σ of 0.905 MJ, the reported true mass is internally inconsistent with the RV likelihood and the astrometric acceleration is driving an inflated mass. This single check is decisive; an optional injection-recovery test (drawing fake HD 154345 systems, re-applying the χ²HG>11.8 selection, and comparing recovered to injected companion mass) would quantify how much of the 1.186 MJ value is selection bias.","verdict_should_be":"UNCHANGED","load_bearing_attack":"The paper's headline result includes true masses for three planets; the least secure of these is HD 154345 b. Section 2.1 selects targets with χ²HG > 11.8, and HD 154345 sits just above that threshold (χ²HG = 12.8, Table 1). Selecting on a significance threshold biases the measured acceleration amplitude upward, and the paper applies no truncation or injection-recovery correction. Since the astrometric acceleration is the only datum that breaks the m sin i degeneracy, any upward bias in its amplitude maps directly into an upward bias in companion mass. A sharper symptom is internal: Table 7 reports Msec = 1.186+0.095−0.059 MJ with i = 88±20°, which at face value implies m sin i ≈ 1.18 MJ, while Section 3.7 cites the RV-only minimum mass as 0.905 MJ. Unless the new NEID/MINERVA RVs shift the Keplerian amplitude by roughly 30%, the joint posterior cannot simultaneously satisfy the RV likelihood and produce the reported companion mass with a near-edge-on inclination. The paper never reports the joint m sin i posterior, so this consistency check is absent. HD 217107 (χ²=49.2) and HD 190360 (χ²=14.8) are less exposed, but HD 154345 is the marginal case supporting the 'three true masses' summary. The four stellar masses rest mainly on relative astrometry and are not affected by this concern.","agreement_with_reader":"partial"},"referee_report":{"model":"deepseek-v4-flash","summary":"This paper presents joint orbit fits for seven nearby star systems drawn from the NEID Earth Twin Survey that show significant Hipparcos-Gaia proper-motion anomalies. For four binary systems (HD 68017 AB, 61 Cygni AB, HD 24496 AB, HD 4614 AB) the authors combine up to ~200 years of relative astrometry, absolute astrometry from the HGCA, and RVs including newly published NEID and MINERVA measurements. For three planetary systems (HD 217107, HD 190360, HD 154345) they combine RVs with the Hipparcos-Gaia acceleration to constrain companion inclinations and report true masses. The paper claims four stellar masses with ≲1% relative precision, true masses for three planets whose masses were previously entangled with inclination, an improved orbit for HD 24496 AB (the first published for that system), and refined ephemerides for all seven systems. The modeling is carried out with orvara, using Gaussian mass priors for the planet hosts and for HD 24496 A, while the other three binary systems are fit without mass priors.","tokens_in":47983,"tokens_out":9068,"duration_ms":94447,"significance":"If the results hold, this is a valuable contribution to the small set of benchmark stellar and planetary masses. The sub-percent dynamical masses for 61 Cygni A, HD 4614 A/B, and HD 68017 B, the first orbital solution for HD 24496 AB, the public release of over 900 new RVs, and the careful treatment of 19th-century relative astrometry are concrete strengths. The comparisons with photometric mass relations and with independent model masses are useful, and the residual periodogram searches add value beyond the headline masses. However, the central claim of 'true masses for three planets' is currently too strong: the HD 154345 b solution appears internally inconsistent with the RV minimum mass, HD 190360 b retains a broad/bimodal inclination, and all three planetary targets sit close to the χ²HG selection threshold where acceleration measurements can be biased. The paper is likely correct in its broad conclusions, but the planetary mass claims need targeted verification and re-scoping before they can be accepted as stated.","major_comments":[{"comment":"The reported posterior for HD 154345 b is internally inconsistent with the RV minimum mass quoted earlier in the paper. Table 7 lists Msec = 1.186+0.095−0.059 MJ with i = 88±20°, which implies m sin i ≈ 1.18 MJ; Section 3.7 quotes the RV-only minimum mass as 0.905+0.071−0.089 MJ from Rosenthal et al. (2021), whose HIRES data are included in the joint fit. Since the joint posterior must satisfy the RV likelihood, the fitted Keplerian semi-amplitude would need to be about 30% larger than the well-established value, which is implausible unless the new NEID/MINERVA data drastically alter the RV solution. The paper does not report the joint m sin i posterior or the best-fit K, so this consistency check is absent. Because HD 154345 b is one of the three headline 'true mass' results, the authors should verify the MCMC solution, report the implied K, and reconcile these numbers.","section":"Section 5.7 / Table 7 / Section 3.7"},{"comment":"The sample is selected on χ²HG > 11.8, and HD 154345 sits just above this threshold with χ²HG = 12.8. For a significance-based cut, the measured proper-motion anomaly of a marginal source is an upward-biased estimate of the true acceleration, and no truncation correction or injection-recovery test is presented. Because the astrometric acceleration is the only datum that breaks the m sin i degeneracy for HD 154345 b, this bias propagates directly into the inferred companion mass. The direction and approximate magnitude of the bias are consistent with the discrepancy raised in the previous comment. I request a quantitative test, such as injecting synthetic accelerations at the χ²HG threshold and fitting the same model, or a re-analysis with a selection-aware prior, before the true mass is claimed for this planet.","section":"Section 2.1 / Table 1 / Section 5.7"},{"comment":"The claim of a 'true mass' for HD 190360 b is not supported by the reported posterior. The inclination is given as i = 69+42−17°, and the text states that the distribution is bimodal with modes near 60° and 120°, so the m sin i degeneracy remains essentially unbroken. The quoted Msec = 1.68+0.26−0.16 MJ is therefore strongly prior-driven rather than a direct dynamical measurement. The abstract's statement of 'true masses for three planets' overstates the result for this system. I recommend either restricting the 'true mass' claim to the cases where the inclination is actually constrained, or demonstrating explicitly that the mass posterior is insensitive to the inclination prior.","section":"Section 5.6 / Table 7 / Figure A6"}],"minor_comments":[{"comment":"The abstract states 'over 1100 previously unpublished measurements,' but the totals given in the text sum to 960 (543 MINERVA RVs in Section 2.3.9 plus 417 NEID RVs in Section 2.3.10). Please reconcile the count.","section":"Abstract / Section 2.3.9 / Section 2.3.10"},{"comment":"The text 'HD 190630 is in a wide (178″) orbit' appears to be a typo for HD 190360 B; the following sentence correctly refers to HD 190360 B.","section":"Section 3.6"},{"comment":"The bottom panel of Figure 5 labels the system as 'HD 217017'; this should be HD 217107.","section":"Section 5.5 / Figure 5"},{"comment":"The reported primary mass 'MA = 0.6772± +0.0051' contains a stray plus sign and should read 'MA = 0.6772+0.0051−0.0051' or use the symmetric notation.","section":"Section 5.2"},{"comment":"The phrase 'one of the longest-period super-Earths (m<20 M⊕)' should be formatted as 'M < 20 M⊕' to avoid confusion between mass and the planet designation.","section":"Section 7.5"}],"recommendation":"major_revision","confidential_remarks":"The paper is a good fit for AJ and the binary-star results are likely robust, but the headline 'three true masses' currently rests on an internally inconsistent solution for HD 154345 b and an overbroad claim for HD 190360 b. The χ²HG selection-bias concern raised by the stress-test analysis is real and should be addressed with an injection-recovery test or an explicit selection correction. I would be willing to review a revision that fixes the HD 154345 consistency check, re-scopes the true-mass language, and quantifies the selection effect."},"author_rebuttal":null,"desk_editor":{"model":"deepseek-v4-flash","letter":"Dear Colleague,\n\nThis is a data-rich paper that earns its place: over 1,100 new NEID/MINERVA RVs, the first orbital solution for HD 24496 AB, and model-independent dynamical masses for 61 Cygni AB and HD 4614 AB that are precise to about 1% and rest on roughly two centuries of relative astrometry. Those binary results look solid, and the full data release is genuinely useful. I also credit the authors for flagging the blended-photocenter caveat in HD 68017 and for comparing against photometric mass relations rather than overclaiming.\n\nThe soft spots are concentrated in the three planetary \"true masses,\" and the reader's conditional verdict is right. HD 217107 c is secure: strong acceleration, near-edge-on, consistent with previous RV minimum mass. HD 190360 b is reasonable but less sharp—broad bimodal inclination and only a ~12% mass constraint. HD 154345 b is the real problem. The paper selects targets on χ²HG>11.8, and HD 154345 sits at 12.8, just above threshold. That selection biases the measured acceleration upward, and no truncation or injection-recovery correction is applied. More damaging, the reported posterior (Msec=1.186 MJ, i=88±20°) implies m sin i ≈ 1.18 MJ, while the RV minimum mass the authors cite is 0.905 MJ. The paper never reports the joint m sin i posterior, so the reader cannot check whether the new NEID data really moved the Keplerian amplitude by ~30%. I'd want that resolved before accepting the mass as a headline result.\n\nAlso, the abstract's \"true masses for three planets whose measurements were previously entangled with inclinations\" overstates novelty: HD 190360 b and HD 154345 b already had true masses from Feng et al. (2021) and Xiao et al. (2023), which the paper cites. The genuinely new one is HD 217107 c.\n\nI don't think any of this sinks the core stellar-mass work. The four binary solutions are valuable, and the data release alone is worth a referee's time. But the presentational claim of three secure planetary masses should be softened, and HD 154345 b needs a re-analysis or a tentative flag.\n\nRecommendation: send to peer review; ask for a revision that addresses the χ² selection bias (or justifies ignoring it for these amplitudes) and that reports the joint m sin i posterior for all three planets.\n\nBest,\n[your name]","headline":"Solid stellar-mass work with a valuable data release, but the three true planetary masses are overstated—HD 154345 b needs re-examination before it is quoted as a secure mass.","tokens_in":48877,"tokens_out":3919,"would_cite":true,"duration_ms":41822,"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 reports true dynamical masses for three planets and four stars by combining 35 years of radial velocities with Hipparcos-Gaia astrometry, breaking the inclination degeneracy in Doppler-only surveys.","keywords":["dynamical masses","binary stars","exoplanets","radial velocities","astrometric acceleration","orbit fitting","proper motion anomaly","cold Jupiters"],"falsifier":"Re-derive the HD 154345 acceleration using the epoch astrometry in Gaia DR4 rather than the two-epoch proper-motion difference; if the resulting acceleration is consistent with zero or notably smaller than the $\\chi^2_{\\rm HG}$-selected value, the reported $1.186\\,M_{\\rm Jup}$ dynamical mass is inflated by the selection cut. The same check on HD 217107 and HD 190360 would reveal whether the bias affects all three planet masses.","tokens_in":47426,"feed_emoji":"🪐","tokens_out":13039,"duration_ms":112942,"temperature":0.7,"pith_summary":"Radial-velocity surveys measure only a planet's minimum mass, because the orbit's tilt is unknown. This paper argues that the gap can be closed by adding a second, independent measurement: the tiny change in a star's sky motion between the Hipparcos and Gaia epochs, which records the star's acceleration toward its companion over roughly 25 years. Applying this to seven nearby accelerated systems, the paper reports true dynamical masses for three planets — HD 217107 c ($4.37$ Jupiter masses), HD 190360 b ($1.68$), and HD 154345 b ($1.186$) — and stellar masses with sub-percent precision for several binary components, together with improved or first orbital solutions. These results matter because model-independent masses anchor stellar evolution and photometric mass calibration, and because the planets' true masses and ephemerides make them concrete targets for direct imaging.","feed_headline":"True masses for three exoplanets via 35-year RV and astrometry fits","feed_subtitle":"Combining Doppler data with Hipparcos-Gaia acceleration breaks the inclination degeneracy and sharpens four stellar masses to ~1%.","key_machinery":"The load-bearing observable is the proper-motion anomaly: the difference between the star's proper motion measured at the Hipparcos epoch and at the Gaia epoch, quantified by the paper's $\\chi^2_{\\rm HG}$ statistic. This difference is a direct measurement of the star's plane-of-sky acceleration over roughly 25 years. When combined with the line-of-sight acceleration from radial velocities and the distance from the Gaia parallax, the resulting three-dimensional acceleration, together with Kepler's laws, fixes the companion mass without knowing the orbit's inclination. For the four binaries, relative astrometry spanning up to about 200 years additionally traces the orbital arc directly. The fits use a parallel-tempered Markov chain Monte Carlo orbit code that simultaneously models absolute astrometry, radial velocities, and relative astrometry, with Gaussian stellar-mass priors applied only where the data cannot supply the mass alone (HD 24496 AB and the three planet hosts).","core_discovery":"By jointly fitting radial velocities spanning more than 35 years with the proper-motion difference between Hipparcos (epoch 1991.25) and Gaia (epoch 2016.0), plus century-long relative astrometry for the resolved binaries, the paper determines the full three-dimensional acceleration of each host star. For the three planetary systems this disentangles mass from inclination for the first time: HD 217107 c has a true mass of $4.37^{+0.13}_{-0.10}\\,M_{\\rm Jup}$ with an orbit close to edge-on ($i = 88^{+14}_{-12}$ degrees); HD 190360 b has $1.68^{+0.26}_{-0.16}\\,M_{\\rm Jup}$ with a bimodal inclination near 60 or 120 degrees; HD 154345 b has $1.186^{+0.095}_{-0.059}\\,M_{\\rm Jup}$ at $i = 88\\pm20$ degrees. For the four binaries, the fit yields masses with relative uncertainties of about 1% or better for HD 68017 B ($0.1548\\pm0.0014\\,M_\\odot$), 61 Cygni A ($0.6772^{+0.0051}_{-0.0051}\\,M_\\odot$), HD 4614 A ($1.0258^{+0.0070}_{-0.0069}\\,M_\\odot$) and HD 4614 B ($0.5487\\pm0.0056\\,M_\\odot$); it also produces the first orbital solution for the 600-year binary HD 24496 AB. The paper states these solutions agree with previous estimates while improving their precision.","pith_inferences":["Because the seven systems were selected on $\\chi^2_{\\rm HG}>11.8$, the measured accelerations for the weakest detections are likely overestimated; a selection-bias correction or a re-fit of stars with $\\chi^2_{\\rm HG}$ between 6 and 11.8 would indicate how much the reported masses, especially that of HD 154345 b, should be discounted.","The two unclassified residual signals — the 2.4-year period around HD 4614 and the 90-day signal around HD 190360 — would, if confirmed as Keplerians, show that this joint-fitting approach can uncover low-mass companions that pure Doppler searches would struggle to validate; the paper's own checks leave both as open questions.","The method's lever arm is the roughly 25-year Hipparcos–Gaia baseline, so systems with periods much longer than that, like HD 24496 AB, still need stellar-mass priors; applying the same fit after Gaia epoch astrometry becomes available should remove those priors and test whether the 600-year orbit solution is biased by them.","For HD 68017, the unresolved photocentric motion in both catalogs could bias the primary's proper motion; if a future Gaia release resolves the pair, the secondary mass of $0.1548\\,M_\\odot$ can be checked against an independent orbit."],"forward_implications":["The three cold Jupiters now have unambiguous masses and ephemerides, so their predicted 2025–2035 angular separations and contrasts can be used to decide whether existing space coronagraphs can image them.","The roughly 1% stellar masses provide model-independent anchor points for testing stellar evolutionary tracks and calibrating photometric mass–luminosity relations.","The first orbital solution for HD 24496 AB demonstrates that a moderate set of high-precision radial velocities plus astrometry can pin down a 600-year orbit, extending the method to very long-period binaries.","The more than 35-year radial-velocity baselines assembled here open the search for ultra-long-period and low-amplitude companions; the residual periodicity at 2.4 years around HD 4614 (a possible $22\\,M_\\oplus$ planet) and at 90 days around HD 190360 (a possible $10\\,M_\\oplus$ planet) are flagged for follow-up.","Future Gaia epoch astrometry should tighten every mass reported here and can extend the same technique to the remaining accelerating targets in the parent survey."],"supporting_citations":[{"why":"Supplies the Hipparcos–Gaia proper-motion anomaly catalog and the chi-squared statistic used to select the seven accelerating stars.","marker":"Brandt 2021"},{"why":"Provides the Bayesian orbit-fitting framework that jointly models radial velocities, absolute astrometry, and relative astrometry.","marker":"Brandt et al. 2021c"},{"why":"Source of the archival HIRES, Hamilton, and APF radial velocities that form the multi-decade baseline.","marker":"Rosenthal et al. 2021"},{"why":"Supplies the spectral stellar-mass priors used for HD 24496 A and the three planet hosts, plus the companion survey used to interpret the HD 4614 mass difference.","marker":"Hirsch et al. 2021"},{"why":"Earlier dynamical mass estimate for HD 154345 b from the same astrometric acceleration, providing the comparison that anchors the planet mass reported here.","marker":"Xiao et al. 2023"},{"why":"The Washington Double Star catalog is the main source of the 1721 relative-astrometry measurements that trace the binary orbits.","marker":"Mason et al. 2001"},{"why":"Prior joint astrometry and radial-velocity orbit for HD 68017 AB whose masses are updated and compared against in this work.","marker":"Brandt et al. 2019"}],"fun_headline_variants":["True masses for 3 exoplanets from 35-year RV + astrometry","Astrometry breaks inclination degeneracy for 3 planet masses","First dynamical mass for HD 24496 AB from Hipparcos-Gaia","Seven systems get precise masses via Hipparcos-Gaia acceleration"],"cache_read_input_tokens":3200,"weakest_assumption_plain":"Every reported mass assumes the measured kink in the star's sky motion between the Hipparcos and Gaia epochs comes entirely from the modeled companion's orbit, and that choosing stars because that kink was unusually large did not inflate the measured accelerations.","fun_headline_variants_meta":{"raw":{"variants":["True masses for 3 exoplanets from 35-year RV + astrometry","Astrometry breaks inclination degeneracy for 3 planet masses","First dynamical mass for HD 24496 AB from Hipparcos-Gaia","Seven systems get precise masses via Hipparcos-Gaia acceleration"]},"model":"deepseek-v4-flash","effort":"low","cost_usd":0.000203,"raw_usage":{"total_tokens":1518,"prompt_tokens":1211,"completion_tokens":307,"prompt_tokens_details":{"cached_tokens":384},"prompt_cache_hit_tokens":384,"prompt_cache_miss_tokens":827,"completion_tokens_details":{"reasoning_tokens":227}},"tokens_in":827,"tokens_out":307,"duration_ms":3961,"temperature":1.0,"reasoning_tokens":227,"cache_read_input_tokens":384,"cache_creation_input_tokens":0},"cache_creation_input_tokens":0},"created_at":"2026-08-15T20:34:08.354836+00:00","model_set":{"reader":"deepseek-v4-flash"},"falsifier":"Re-derive the HD 154345 acceleration using the epoch astrometry in Gaia DR4 rather than the two-epoch proper-motion difference; if the resulting acceleration is consistent with zero or notably smaller than the $\\chi^2_{\\rm HG}$-selected value, the reported $1.186\\,M_{\\rm Jup}$ dynamical mass is inflated by the selection cut. The same check on HD 217107 and HD 190360 would reveal whether the bias affects all three planet masses.","supporting_citations":[],"review_version":1}