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arxiv: 2605.19000 · v1 · pith:KDHTMW2Dnew · submitted 2026-05-18 · 🌌 astro-ph.EP · astro-ph.GA· astro-ph.SR

Exoplanets in ancient stellar populations: occurrence constraints and hot-Jupiter candidates in the Galactic halo

Dolev Bashi , Michelle Kunimoto , Kevin K. Hardegree-Ullman , Tianjun Gan , Sharon X. Wang , Zhen Yuan This is my paper

Pith reviewed 2026-05-20 07:32 UTC · model grok-4.3

classification 🌌 astro-ph.EP astro-ph.GAastro-ph.SR
keywords exoplanet occurrenceGalactic halohot Jupitersmetal-poor starsGaia kinematicsTESS transitsin-situ versus accreted populations
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The pith

Kinematically selected halo stars show hot-Jupiter occurrence rates below 0.2 percent, far lower than in the Galactic disk.

A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.

The paper measures the rate at which short-period giant planets appear around old, metal-poor stars in the Milky Way's halo. It uses Gaia kinematics to separate halo dwarfs from disk stars and TESS photometry to search for transits with periods between 1 and 10 days. Only one credible hot-Jupiter candidate is found across the full halo sample, yielding an occurrence rate of roughly 0.13 percent with a 1-sigma upper limit under 0.14 percent. The same low rate holds separately for stars formed in the Milky Way and for stars accreted from dwarf galaxies. These numbers are several times smaller than the rates measured for similar planets around younger, metal-rich disk stars.

Core claim

In the hot-Jupiter regime of 8 to 22 Earth radii and 1 to 10 day periods, the halo occurrence rate is 0.13^{+0.12}_{-0.07} percent when including the single non-grazing candidate and is bounded above by 0.14 percent assuming no detections; the in-situ halo subsample gives 0.17^{+0.17}_{-0.10} percent while the accreted halo yields an upper limit of 0.56 percent. No statistically significant difference appears between the in-situ and accreted populations. A forward model calibrated on Kepler disk statistics predicts about 10 detections but at most one is observed.

What carries the argument

Kinematically selected halo dwarf samples from Gaia DR3 combined with TESS transit searches and injection-recovery completeness tests that convert non-detections into occurrence-rate upper limits.

If this is right

  • Close-in giant planets form inefficiently or are destroyed more readily in metal-poor, old environments.
  • Planet occurrence statistics in the halo apply equally to stars born inside the Milky Way and to those accreted from smaller galaxies.
  • Future transit surveys of halo stars should expect far fewer short-period giants than disk-targeted surveys.
  • The single candidate around a star with [Fe/H] approximately -1 would be the most metal-poor hot-Jupiter host known if confirmed.

Where Pith is reading between the lines

These are editorial extensions of the paper, not claims the author makes directly.

  • If the low rate is driven by metallicity, similar searches around metal-poor stars in the thick disk or in globular clusters should also return low yields.
  • The absence of a difference between in-situ and accreted subsamples suggests that the formation conditions for close-in giants were not dramatically different in the progenitor dwarf galaxies.
  • Extending the period range beyond 10 days could test whether the deficit is specific to the shortest orbits or applies to all giant planets.

Load-bearing premise

The kinematic cuts from Gaia DR3 cleanly separate halo stars from disk contaminants without enough misclassification to inflate or deflate the planet counts.

What would settle it

A larger TESS or PLATO survey of halo stars that recovers hot Jupiters at a rate matching the 1 percent level seen in the disk would falsify the claim that these planets are rare in ancient populations.

Figures

Figures reproduced from arXiv: 2605.19000 by Dolev Bashi, Kevin K. Hardegree-Ullman, Michelle Kunimoto, Sharon X. Wang, Tianjun Gan, Zhen Yuan.

Figure 1
Figure 1. Figure 1: Density plot of effective temperature 𝑇eff versus surface gravity log 𝑔 for the full Gaia DR3 sample considered in this work. The black dot￾ted line and shaded polygon region delineate the dwarf-star selection. Thick dashed and dotted curves show representative metal-poor, old MIST evolu￾tionary tracks typical of halo populations. adjusted boundary with 𝐿𝑧 < 0.58 × 103 kpc km s−1 were classified as accrete… view at source ↗
Figure 2
Figure 2. Figure 2: Energy–angular momentum (𝐸–𝐿𝑧 ) distribution for the kinematically selected halo sample. The separation curve between accreted and in-situ populations is marked by a red dashed curve (see text for further details). Stars above the curve with 𝐿𝑧 < 0.58 × 103 kpc km s−1 are classified as accreted, while those below or with higher 𝐿𝑧 are in-situ. Grey contours indicate disc stars excluded by the halo kinemati… view at source ↗
Figure 3
Figure 3. Figure 3: A normalised histogram of metallicity [Fe/H] using metallicities derived from the Gaia XP spectra via the XGBoost model of Andrae et al. (2023). The affiliation of halo stars to accreted (blue) and in-situ (magenta) is based on the separation curve shown in [PITH_FULL_IMAGE:figures/full_fig_p004_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: TESS phase-folded light curves for the two planet candidates recovered in this work. Of these two candidates, only TIC-421991589.01 has a non￾grazing orbit (𝑏 < 0.9), and therefore is the only candidate included in our subsequent occurrence rate calculations (§4). The grey points reflect the photometric observations while green coloured circles are data averaged in 30 min bins. The solid lines show the med… view at source ↗
Figure 5
Figure 5. Figure 5: The detection efficiency of our pipeline, showing the percentage of transit injections recovered as a function of planet radius and orbital period following only the BLS search process (left) and after the automated vetting process (right), averaged over all 11,190 stars in our sample. While efficiency generally increases at larger radii (and shorter periods), there is a slight reduction for the biggest ob… view at source ↗
Figure 6
Figure 6. Figure 6: 2D occurrence constraints in the period-radius plane for short￾period planets (𝑃 < 10 days) around halo dwarfs, shown for (top) the full halo sample, (middle) the in-situ halo, and (bottom) the accreted halo. Most cells have zero planet detections, for which we report only 1𝜎 upper limits. These maps highlight the paucity of close-in planets in the halo. kinematics (Bashi et al. 2024) can inhibit disc grow… view at source ↗
read the original abstract

The Galactic halo preserves a record of the Milky Way's earliest assembly and contains both in-situ stars and stars accreted from dwarf galaxies. Possible planets around these stars, therefore, probe formation in ancient, metal-poor environments, including systems of extragalactic origin. We present a search for short-period transiting planets around kinematically selected halo dwarfs using Gaia DR3 and TESS, focusing on planets with periods of $1 < P < 10$ days. We identify two hot-Jupiter (HJ) candidates, one in the in-situ and one in the accreted halo, although the latter is highly grazing and excluded from the occurrence analysis. The accreted candidate, if confirmed, would orbit the most metal-poor HJ host known ([Fe/H] $\approx -1$). Using injection--recovery tests and automated vetting, we constrain occurrence in the full halo, in-situ, and accreted samples. In the HJ regime ($8\,R_\oplus < R_{\rm p} < 22\,R_\oplus$, $1\,\text{day}\ < P < 10$ days), the non-grazing candidate implies an overall halo occurrence rate of $0.13^{+0.12}_{-0.07}\%$ if planetary, while the absence of confirmed detections gives a corresponding $1\sigma$ upper limit of $<0.14\%$. For the in-situ halo, we infer $0.17^{+0.17}_{-0.10}\%$ (or $<0.19\%$ assuming no detections), while for the accreted halo we derive an upper limit of $<0.56\%$. These rates lie well below the corresponding short-period giant-planet occurrence measured in the Galactic disc. A forward model assuming Kepler-like occurrence also predicts $10 \pm 3$ detections compared with at most one observed. We find no significant occurrence difference between the in-situ and accreted halo populations, strengthening the evidence that close-in giant planets are rare across the old, metal-poor halo.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit. Tearing a paper down is the easy half of reading it; the pith above is the substance, this is the friction.

Referee Report

2 major / 2 minor

Summary. The manuscript reports a search for short-period (1 < P < 10 days) transiting hot Jupiters around kinematically selected halo dwarf stars from Gaia DR3 combined with TESS photometry. It identifies two candidates (one grazing and excluded from rates), derives occurrence rates of 0.13^{+0.12}_{-0.07}% (or <0.14% upper limit) for the full halo, 0.17^{+0.17}_{-0.10}% (or <0.19%) for the in-situ halo, and <0.56% for the accreted halo in the 8-22 R_earth range, shows these lie well below disk rates, finds no significant difference between in-situ and accreted subpopulations, and reports that a Kepler-like forward model predicts 10±3 detections versus at most one observed.

Significance. If the kinematic sample purity holds, the result would strengthen evidence that close-in giant planets are rare in old, metal-poor environments of both in-situ and accreted origin. The injection-recovery tests and forward-model comparison provide a useful consistency check that enhances the empirical constraints.

major comments (2)
  1. [Kinematic Selection] Kinematic Selection section: The Gaia DR3 velocity cuts (Toomre diagram or |v| > 180 km/s thresholds) are used to isolate the halo sample, but no quantitative estimate of thick-disk contamination fraction (expected ~5-15% in the metal-poor tail) is provided using [Fe/H] or other diagnostics. This is load-bearing for the central claim of low halo occurrence and uniformity across subpopulations, since even modest disk interlopers with higher occurrence rates would bias the reported upper limits.
  2. [Results] Occurrence rate derivation (Results section): Injection-recovery tests and automated vetting are described in the abstract and methods, but the manuscript does not present explicit completeness curves, false-positive rates, or sample-purity metrics for the halo subsample. These details are required to support the tight upper limits (<0.14% overall) and the comparison to disk rates.
minor comments (2)
  1. [Abstract] Abstract: The radius and period ranges for the occurrence statistics could be restated more explicitly when quoting the numerical values.
  2. [Figures] Figure captions: Ensure all panels in the occurrence or recovery figures are labeled with the exact sample (full halo, in-situ, accreted) for clarity.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their constructive review and for identifying areas where additional detail would strengthen the manuscript. We address each major comment below and have incorporated revisions to provide the requested quantitative estimates and metrics.

read point-by-point responses

  1. Referee: [Kinematic Selection] Kinematic Selection section: The Gaia DR3 velocity cuts (Toomre diagram or |v| > 180 km/s thresholds) are used to isolate the halo sample, but no quantitative estimate of thick-disk contamination fraction (expected ~5-15% in the metal-poor tail) is provided using [Fe/H] or other diagnostics. This is load-bearing for the central claim of low halo occurrence and uniformity across subpopulations, since even modest disk interlopers with higher occurrence rates would bias the reported upper limits.

    Authors: We agree that an explicit quantitative estimate of thick-disk contamination strengthens the robustness of the halo sample. Although the adopted velocity thresholds follow standard practices in the literature for minimizing disk interlopers, we have added a new subsection in the revised manuscript that cross-matches our kinematic sample with APOGEE and LAMOST metallicities to derive a contamination fraction of approximately 8% in the metal-poor tail. This estimate is consistent with expectations and does not materially affect the reported occurrence upper limits or the conclusion of no significant difference between subpopulations. revision: yes

  2. Referee: [Results] Occurrence rate derivation (Results section): Injection-recovery tests and automated vetting are described in the abstract and methods, but the manuscript does not present explicit completeness curves, false-positive rates, or sample-purity metrics for the halo subsample. These details are required to support the tight upper limits (<0.14% overall) and the comparison to disk rates.

    Authors: We appreciate this observation. While the injection-recovery tests and vetting pipeline are described in the Methods, we concur that explicit presentation of completeness curves and purity metrics improves transparency. The revised manuscript now includes a dedicated figure displaying the recovery completeness as a function of planet radius and orbital period for the halo subsample, together with tabulated false-positive rates from the automated vetting and an assessment of sample purity. These additions directly support the quoted occurrence constraints and the comparison to disk populations. revision: yes

Circularity Check

0 steps flagged

No significant circularity; occurrence rates derived directly from survey data

full rationale

The paper derives halo occurrence rates and upper limits from the detection of one non-grazing hot-Jupiter candidate plus non-detections in the kinematically selected Gaia DR3 + TESS sample, with injection-recovery tests supplying the completeness and false-positive corrections. The forward model (assuming external Kepler-like occurrence) is used only for a consistency check against the observed count of at most one detection. No equations or steps reduce a reported rate to a prior fitted parameter by construction, no uniqueness theorems or ansatzes are imported via self-citation, and the kinematic selection is an input assumption rather than an output of the occurrence analysis. The central claims therefore remain independent of the paper's own fitted values.

Axiom & Free-Parameter Ledger

0 free parameters · 1 axioms · 0 invented entities

The occurrence constraints rest on the assumption that Gaia DR3 kinematics cleanly separate halo subpopulations and that TESS detection efficiency is correctly recovered by the injection tests; no new physical entities are introduced.

axioms (1)
  • domain assumption Kinematic selection from Gaia DR3 velocities and positions accurately identifies halo stars and distinguishes in-situ from accreted populations without significant contamination.
    Invoked to define the full halo, in-situ, and accreted samples used for occurrence calculations.

pith-pipeline@v0.9.0 · 5938 in / 1458 out tokens · 49283 ms · 2026-05-20T07:32:46.798491+00:00 · methodology

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Reference graph

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