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astro-ph.SR · Solar and Stellar Astrophysicsastro-ph.GA · Astrophysics of Galaxiesastro-ph.EP · Earth and Planetary Astrophysics

Two local velocity models favor the thin disk for ASASSN-24fw if its Gaia radial velocity is systemic

ASASSN-24fw is a long-eclipse system with a possible disk around a companion. One published study assigns its star to the Galactic thick disk. We test that claim with the public Gaia DR3 source row, its full astrometric covariance, and two published local Gaussian velocity models. If the Gaia radial velocity is systemic, the thick-to-thin disk odds are 0.03118 and 0.03553. Equal disk weights give thin disk scores of 0.672 and 0.679. Thus, the large weighted preference depends strongly on the assumed population fractions. At nominal astrometry, equal odds on the positive radial velocity branch occur at 98.56 and 126.48 km/s. The Gaia value is 36.87 km/s. We also find that the published tangential speeds are about 4.74 times smaller than the speeds implied by the distance and proper motions. A stated circular-motion example gives a random speed of 36.56 km/s. This agrees with an earlier low-speed interpretation; that interpretation is not new here. The contribution is the numerical population comparison, its conditional limits, and the unit audit. The local models omit spatial population densities, selection effects, chemical data, and model uncertainty. They do not determine a stellar age or confirm a planet. The package includes data provenance, code, results, figures, and independent numerical checks.

ASASSN-24fw · J0705+0612 · Gaia DR3 · Galactic kinematics · thin disk · thick disk · systemic radial velocity · velocity units · reproducible research

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References

10
  1. usesdoi:10.5270/esa-qa4lep3

    The public Gaia DR3 source row, errors, and astrometric correlations provide the input data.

  2. usesdoi:10.1051/0004-6361/202243940

    This paper describes the Gaia DR3 release used for the source measurements.

  3. challengesdoi:10.1093/mnras/staf2251

    The tested local velocity models favor the thin disk if the Gaia radial velocity is systemic. The stated Table 1 tangential speeds also disagree with the distance and proper motions. This challenge is limited to the kinematic claim and table units. It does not test the ring fit or the authors' orbit code.

  4. supportsdoi:10.3847/1538-3881/ae1fd9

    A stated circular-motion example gives a random speed near the prior value of 37 km/s. The earlier preprint already discussed a thin disk interpretation. This work adds model scores and sensitivity limits.

  5. supportsdoi:10.48550/arXiv.2507.05367

    Version 1, Section II.2 already gives a thin disk interpretation. We do not claim that interpretation as a first result.

  6. usesdoi:10.1051/0004-6361:20031213

    Table 1 defines the first local Gaussian velocity model. The calculation retains its solar correction and 6 percent thick disk weight.

  7. usesdoi:10.1051/0004-6361:20040332

    Appendix A checks the velocity dispersions and drift speeds and documents the change to a 10 percent thick disk weight.

  8. usesdoi:10.1111/j.1365-2966.2006.10148.x

    Table 1 and Section 2.1 define the second local Gaussian velocity model and its solar correction.

  9. usesdoi:10.1111/j.1365-2966.2010.16253.x

    The solar velocity defines the modern reference-frame example. The scale of its stated errors also guides a solar-scatter sensitivity test.

  10. usesdoi:10.3847/1538-4357/ac7c74

    Astropy supplies an independent coordinate conversion for the numerical checks.

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