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Astrometric Accelerations of Provisional Targets for the Habitable Worlds Observatory

T0 review · 2 major / 6 minor · reviewed 2026-08-06 · deepseek-v4-flash

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Pith's one-line read Long-baseline astrometry reveals that 54 of 156 provisional HWO target stars are accelerating, 17 with no known cause.

desk verdict Solid precursor science: systematic Hipparcos-Gaia acceleration analysis of the HWO target list; the headline counts are robust, but the error model for the Kervella eta factor deserves a sensitivity check before the 85% claim is quoted. read the letter →

arxiv 2506.21768 v1 pith:6RELJZ6S submitted 2025-06-26 astro-ph.EP astro-ph.IMastro-ph.SR

Katie E. Painter , Brendan P. Bowler , Kyle Franson , Juliette C. Becker , Jennifer A. Burt This is my paper · ORCID
classification astro-ph.EPastro-ph.IMastro-ph.SR
keywords astrometricaccelerationHabitableWorldsObservatoryHipparcos-Gaiaastrometryexoplanetcompanionszonestabilitygiantplanetsbrowndwarfsprecursorscience
verification ladder T0 review T1 audit T2 compute T3 formal

The pith

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

The reading

Most of the 164 provisional Habitable Worlds Observatory targets are the nearest Sun-like stars on which the mission hopes to image Earth-like planets, so hidden stellar or giant-planet companions would either make the habitable zone unstable or block the imaging. The paper tries to establish that Hipparcos-Gaia astrometry can screen this list: it finds 54 of the 156 targets in the acceleration catalog show statistically significant long-term accelerations, implying an unseen companion. It attributes 37 of those accelerations to known planets, stars, white dwarfs, or brown dwarfs, leaving 17 accelerations as likely signals of previously unknown companions. For the 102 non-accelerating stars, the paper argues that large regions of companion mass and separation can be excluded, and that the method is about 85% sensitive to two-Jupiter-mass planets between 4 and 10 AU. If right, this gives mission planners a dynamical-hazard map of the HWO sample and a concrete list of systems needing follow-up before launch.

What carries the argument

The central tool is the Hipparcos-Gaia Catalog of Accelerations (HGCA), which supplies a long-term proper motion measured from the position difference between the two missions; subtracting the Gaia epoch proper motion from this long-term proper motion gives the acceleration $\Delta\mu_G$ of the star in the plane of the sky. A semi-analytical relation adapted from Kervella et al. (2019) converts this acceleration into a joint constraint on companion mass $m_2$ and orbital radius $r$, with correction factors $\gamma$ (Gaia time averaging), $\eta = 0.87$ (orbital projection and phase), and $\zeta(P)$ (orbital-period efficiency). Monte Carlo sampling over the eight input parameters produces the mass-separation curves for accelerating stars, and for non-accelerating stars the same machinery yields upper limits above which companions are excluded. This is what carries the argument from a measured proper-motion difference to statements about which companions exist or are ruled out.

What would settle it

Take the 17 unaccounted accelerating targets and observe them with high-contrast imaging and precision radial velocities at the predicted mass-separation locations; if several of the high-significance cases such as HD 212330 A or kappa Tucanae A show no companion, or show a companion far outside the 2-sigma band, the conversion model or the single-companion assumption would be falsified. Alternatively, recompute the accelerations with Gaia DR4's longer baseline: the strongest unaccounted signals should persist if real, while the 2-3 sigma ones should mostly remain; if most disappear, the 2-sigma threshold is too permissive.

Watch

Extended reading notes

Core claim

Using proper-motion differences between Hipparcos and Gaia EDR3, the authors identify 54 of 156 HWO provisional targets with statistically significant ($>2\sigma$) astrometric accelerations, and for each accelerating star they compute joint mass-separation constraints on the companion that produces the pull. Comparing these constraints with known planets, brown dwarfs, stellar binaries, and white dwarfs, 37 of the accelerations are consistent with a known companion, while 17 are unaccounted for and likely require close-in stellar companions, brown dwarfs, or giant planets. The same machinery applied to the 102 non-accelerating stars is used to rule out wide-orbit companions over large regions of mass and separation, reaching an average sensitivity of about 85% to $2\,M_\mathrm{Jup}$ planets between 4 and 10 AU. The paper further claims that analytical stability estimates flag 13 systems whose known companions are likely to disrupt Earth-mass planets in their habitable zones.

Load-bearing premise

The load-bearing premise is that the measured proper-motion difference reflects the pull of exactly one companion, and that the empirical correction factors used to convert that pull into a companion mass are accurate for these stars; if either fails, the mass-separation curves, the consistent and inconsistent labels, and the sensitivity percentages all shift.

Editorial extensions

If this is right

  • Seventeen accelerating HWO targets now have a concrete follow-up agenda: high-contrast imaging and precision radial velocities aimed at the predicted mass-separation bands should reveal the suspected companions.
  • The 102 non-accelerating stars have large regions of companion mass and separation excluded, so companion searches on those systems can focus on shorter-period and lower-mass regimes where astrometry is insensitive.
  • Thirteen systems are identified as likely to have habitable zones that are dynamically unstable for Earth-mass planets, which could lower their priority for HWO's core science goal.
  • Future Gaia releases should push the same screening down to sub-Jovian planet masses at Solar-System separations, extending the mass-separation constraints to smaller companions.
  • If the derived wide-orbit giant planet occurrence rate of about $12\pm3\%$ for this sample holds, HWO targets look broadly similar to the wider solar neighborhood in their giant-planet demographics.

Reading between the lines

Editorial extensions of the paper, not claims the author makes directly.

  • The paper's single-companion assumption means multi-planet systems such as HD 219134 and HD 115404 A are the most likely to be misclassified; a direct test would be a joint Keplerian fit to the radial velocities and astrometry that allows two companions to contribute to the acceleration.
  • Because the 3$\sigma$ upper limits are tabulated for all 102 non-accelerating stars, the same screening can be applied verbatim to any future revision of the HWO target list or to other nearby-star samples, without new observations.
  • If Gaia DR4 confirms the 17 unaccounted accelerations with a longer baseline, the $\sim12\pm3\%$ wide-orbit giant planet occurrence rate can be checked directly; if several of the low-significance signals vanish, the 2$\sigma$ cutoff and the assumption that most 2-3$\sigma$ signals are real would be the weak link.
  • The stability assessment assumes circular, coplanar orbits, so real eccentric or inclined companions would shrink the stable habitable-zone regions further; the 13 flagged systems are therefore likely a lower bound on the number of targets whose habitable zones are threatened.
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Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, and a circularity audit.

Referee Report

2 major / 6 minor

Summary. The manuscript crossmatches the 164-star provisional HWO target list against the Hipparcos-Gaia Catalog of Accelerations, identifying 156 targets with HGCA entries. Using the HGCA proper-motion differences and the Kervella et al. (2019, 2022) semi-analytical conversion, it computes joint companion mass–separation constraints for every target, flags 54 stars with >2σ accelerations, compares these predictions with a compiled catalog of known planets and stellar companions, and attributes 37 of the accelerations to known companions. The remaining 102 non-accelerating targets are used to build average sensitivity maps and exclusion limits, leading to the headline ~85% sensitivity to 2 M_Jup planets between 4 and 10 AU. A final analytical stability assessment identifies 13 systems in which known companions may disrupt habitable-zone planets.

Significance. The primary value is a community resource: per-target mass–separation constraints, upper limits, and sensitivity maps for the HWO precursor target list, with machine-readable tables. The central numbers are derived from an external catalog and an external model rather than fitted, and the authors explicitly flag the single-companion assumption and the circular-orbit stability limits. If the error-distribution issue raised below is resolved, the 54/37/17 accounting and the 85% sensitivity figure are useful and falsifiable inputs to HWO target selection, and the 17 unaccounted accelerators provide a concrete follow-up list.

major comments (2)
  1. [§2.1, Eq. (2)] The Monte Carlo description states that all eight parameters are drawn from normal distributions, but the paper reports η = 0.87^{+0.12}_{-0.32} without specifying which σ is used for η. Because m2 is inversely proportional to η, a symmetric normal with σ = 0.12 under-represents the large negative tail and narrows the 3σ upper limits for non-accelerating stars and the 2σ credible intervals for accelerating stars; a symmetric normal with σ = 0.32 would draw negative η values and hence negative masses unless truncated. This uncertainty propagates directly into the ~85% sensitivity claim in the abstract and Section 3, the Table 3 fractions, and the Table 1 consistent/inconsistent labels. Please specify the adopted η distribution and test robustness to the asymmetric error, for example using a log-normal or skew-normal distribution or resampling the reported asymmetric interval.
  2. [§2.2, Table 1] The consistent/inconsistent assignment assumes that a single companion produces the full measured acceleration, as the paper notes. The headline 37/17 count nonetheless includes multi-companion systems such as HD 219134, Lalande 21185, υ Andromedae A, and HD 115404 A, where the acceleration could be a superposition of several companions; in such systems a companion lying below the 2σ curve is not necessarily excluded as a contributor. Please quantify, or at least explicitly list, the systems for which the single-companion assumption affects the classification, and adjust the abstract's '37 accounted for' wording accordingly.
minor comments (6)
  1. [Section 1 vs Sections 2–3] The introduction says '154 of the 164 targets ... have entries in the HGCA', but Sections 2 and 3 use 156 throughout (54 accelerating + 102 non-accelerating = 156). This is an internal inconsistency that should be fixed.
  2. [Section 3, bullet list] The sentence 'The other 8 without previously confirmed companions are ...' lists nine stars and includes ι Pavonis, which was already listed among the two disputed binaries (104 Tauri and ι Pavonis). Correct the list or the count.
  3. [Section 4, stability paragraph] The text says '15 known planets do fall within the region that would affect the stability of an Earth-mass planet', but the following list contains 13 system names; clarify whether the count refers to planets or systems and reconcile the number.
  4. [Tables 4 and 5] The excerpt for HIP 104214 shows identical 1σ, 2σ, and 3σ values (0.68 M⊙) across many rows. If this is a truncated or degenerate distribution, explain it in the table notes; if it is a formatting artifact, confirm that the machine-readable version is correct.
  5. [Abstract and Section 3] The phrase 'the remaining 17 accelerating stars' could be read as 17 confirmed unknown companions; since 11 of the 17 have significance between 2σ and 3σ, consider wording such as '17 targets with significant accelerations not accounted for by known companions' to avoid overclaiming.
  6. [Introduction, paragraph 3] The word 'complimenting' should be 'complementing' when describing how astrometry complements radial velocities and direct imaging.

Circularity Check

1 steps flagged · score 6.0 of 10

Several planet accelerators are classified as 'consistent' using the same Hipparcos-Gaia acceleration that went into their measured masses, partially forcing the 37/17 split.

  1. fitted input called prediction [Section 2.2 (consistent-companion definition) and Section 4.1 (π Mensae, ε Indi A notes)]
    "If the companion falls within 2σ of the joint mass and separation constraints predicted from an acceleration, we deem it as being 'consistent' with being the source of the observed acceleration. ... π Mensae b was found by Jones et al. (2002) through RVs, and its most updated parameters from a combination of astrometry, RVs, and imaging are M = 12.33+1.19−1.38 MJup and a = 3.31+0.13−0.15 AU (Feng et al. 2022)."

    The HGCA proper-motion difference ΔvT,G is the input to Eq. 2, which produces the mass-separation curves used to define 'consistent'. For π Mensae b and ε Indi Ab, the cited parameters come from a combination of astrometry, RVs, and imaging; the astrometry is the same Hipparcos-Gaia acceleration signal used in this paper. Their masses and semi-major axes are therefore fitted to the same observable that Eq. 2 predicts. Declaring these companions 'consistent' with, and 'accounting for', the measured acceleration is a restatement of that fit rather than an independent test. The same issue applies to HD 140901 c, HD 115404 Ac, and ε Eridani b.

full rationale

The paper's core astrometric measurements come from the external HGCA catalog, and its mass-separation conversion comes from Kervella et al. (2019, 2022). No parameter is fitted to reproduce the 54/37/17 counts or the 85% sensitivity; these are derived from the measured accelerations and the external model. Non-detection upper limits and sensitivity maps are standard uses of non-detections, not circular. The dynamical stability analysis uses independent literature companions and external stability criteria. However, a subset of the 'known companions' used to 'account for' accelerations were themselves characterized with the same Hipparcos-Gaia astrometric signal. For example, π Mensae b's mass and orbit are given from a combination of astrometry, RVs, and imaging; the astrometry is the same HGCA acceleration used to build the prediction curve. Classifying such planets as 'consistent' is a re-use of the same data, so part of the 37/17 accounting is forced. The skeptical concern about asymmetric η uncertainties is a robustness/correctness issue, not circularity. Because the circular subset affects the headline accounting claim but most companions (stellar binaries, RV-only planets) are independent, the overall circularity is partial.

Assumptions & free parameters 4 free parameters · 6 assumptions · 0 invented entities

The analysis relies on external astrometric data (HGCA), external conversion factors (Kervella et al.), and external companion catalogs. The authors choose several practical thresholds and assumptions, but no free parameter is fitted to make the headline results come out as desired.

free parameters (4)
  • Host star mass uncertainty (10 percent)
    Adopted because Mamajek and Stapelfeldt (2023) do not report uncertainties; used as an input to the Monte Carlo but stated to have little effect on results (Section 2.1).
  • Assumed stellar age of 3 Gyr for MIST companion masses = 3 Gyr
    Used to infer masses of F/G/K stellar companions; individual system ages are not measured (Section 2.2).
  • 2-sigma significance cutoff for acceleration detection = 2 sigma (chi-squared = 6.16)
    Chosen to balance completeness and false positives; affects the 54 and 17 counts (Section 2).
  • 3-sigma threshold for sensitivity map = 3 sigma
    Assumed as a hard cutoff to compute the fraction of parameter space ruled out by non-detections (Section 3).
assumptions (6)
  • domain assumption HGCA proper motion differences and chi-squared values are accurate.
    All acceleration detections and upper limits derive from the HGCA catalog (Brandt 2018, 2021); if the catalog is systematically biased, the 54/37/17 breakdown and sensitivity estimates shift. Invoked throughout Section 2.
  • domain assumption The Kervella et al. conversion factors eta and zeta provide an unbiased mapping from Delta-mu-G to companion mass and separation.
    Section 2.1 adopts Eq. 2 with eta = 0.87 and zeta from Fig. 3 of Kervella et al. (2019); these are calibrated on orbital simulations, not on HWO targets. A mis-calibration would bias all mass-separation curves and the 85 percent sensitivity claim.
  • domain assumption Only one massive companion is accelerating the host star.
    Stated in Section 2: 'this analysis assumes that only one massive companion is accelerating the host star.' If multiple companions contribute, inferred masses and consistency classifications can change.
  • domain assumption Known companion catalogs are complete for the purpose of classification.
    Section 2.2 compiles companions from the NASA Exoplanet Archive, WDS, and literature; missing or incorrect entries change the number of accounted-for accelerations.
  • domain assumption Projected separation to semi-major axis conversion via the Dupuy and Liu (2011) uniform-eccentricity factor is valid.
    Section 2.2 converts projected separations at epoch about 2009.8 to semi-major axes; individual eccentricities and inclinations are not known.
  • domain assumption Quarles et al. (2018, 2020) stability limits and the Hill stability criterion apply to HZ stability for circular coplanar orbits.
    Section 4 uses these analytical limits to flag 13 systems; the paper notes eccentricity and mutual inclination are not captured.

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Pith. "Pith review of Astrometric Accelerations of Provisional Targets for the Habitable Worlds Observatory." pith.science (2026). https://pith.science/paper/6RELJZ6S

@misc{pith2026250621768,
  author       = {Pith},
  title        = {Pith review of: Astrometric Accelerations of Provisional Targets for the Habitable Worlds Observatory},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/6RELJZ6S}},
  note         = {Machine review of arXiv:2506.21768}
}
abstract

NASA's Habitable Worlds Observatory (HWO) will be the first space telescope capable of directly imaging Earth-like planets in the habitable zones of Sun-like stars to probe their atmospheres for signs of life. Now in its early stages of design, a list of the 164 most promising targets for HWO has been released to the community to carry out precursor science. Massive companions in these systems--stars, brown dwarfs, or giant planets--could preclude the existence of Earth-sized planets in the habitable zone by impacting their long-term dynamical stability. Here, we use astrometry from Hipparcos and Gaia EDR3 to identify stars in the HWO preliminary target list that exhibit astrometric accelerations and determine joint constraints on the expected mass and separation of these companions. We find that 54 HWO targets have significant astrometric accelerations, 37 of which are accounted for by known giant planets and stellar companions. Follow-up efforts are required to clarify the specific nature of the suspected companions around the remaining 17 accelerating stars. Stars without significant accelerations are used to rule out large regions of companion mass and separation down to planetary masses. We find that with Hipparcos and Gaia EDR3 we are $\sim$85$\%$ sensitive to 2 $M_\mathrm{Jup}$ planets between 4 and 10 AU. Future Gaia releases will provide sensitivity to sub-Jovian mass planets on Solar System scales for provisional HWO targets. Finally, using analytical estimates of dynamical stability, we find that 13 HWO targets have known stellar or planetary companions that are likely to disrupt habitable-zone planets.

Figures

Figures reproduced from arXiv: 2506.21768 by the authors.

Figure 1
Figure 1. Top: HGCA acceleration measurements for HWO preliminary targets. Bottom: Significance of HGCA accel￾eration measurements for HWO targets, calculated from χ 2 values for constant proper motion model fits (see Section 2 for details). We adopt a cutoff for significance at 2σ. The significant (> 2σ) accelerations are shown in red in both the top and bottom panels. There are three multiplicative correction factors in thi… view at source ↗
Figure 2
Figure 2. Examples of companion mass-separation predictions calculated using Hipparcos-Gaia astrometry from HGCA. For stars with significant accelerations, such as 10 Canum Venaticorum (left panel), 1 and 2σ confidence intervals are computed to identify the joint constraints on companion mass and separation consistent with the measured acceleration of the host star. For non-accelerating stars, such as HD 193664 (right panel),… view at source ↗
Figure 3
Figure 3. HZ limits in physical (top) and angular (bottom) separation for all HWO targets following the prescription from Kopparapu et al. (2014). These display the separations that HWO will need to resolve. Optimistic bounds, defined by “recent Venus” and “early Mars” empirical constraints, are shown on the far left and right, respectively. Conservative bounds, defined by “runaway greenhouse” and “maximum greenhouse” calcula… view at source ↗
Figures from the paper (5 more)
Figure 4
Figure 4. Figure 4: Left: Significance of acceleration (s) for all HWO targets in the HGCA. Middle: Of the 54 accelerating HWO targets, 37 have companions that are consistent with the acceleration and 17 have unknown accelerators. Right: Of the 37 accelerations that are consistent with a …
Figure 5
Figure 5. Figure 5: Fraction of parameter space (in companion mass and separation) that the HGCA method is sensitive to, to within at least 99.7% confidence. Each panel is calculated in different mass ranges—stellar (m2 > 75 MJup), brown dwarf (13 MJup < m2 < 75 MJup), and giant planet (5…
Figure 6
Figure 6. Figure 6: Average sensitivity of HGCA astrometric acceleration method to companions across mass and separation space, calculated from non-significant accelerations. 90%, 50%, and 10% contours are shown. All known companions of HWO targets in the HGCA are plotted. Red circles and…
Figure 7
Figure 7. Figure 7: Left: Dynamical stability analysis of habitable zones. Known planets (green circles) and companions in the stellar/brown dwarf mass-range (yellow stars) are shown relative to the region of physical instability for an Earth-mass planet situated in the HZ (gray contours)…
Figure 8
Figure 8. Figure 8: Companion mass versus separation for all targets in the HGCA as shown in [PITH_FULL_IMAGE:figures/full_fig_p024_8.png]

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Works this paper leans on

138 extracted references · 10 canonical work pages

  1. [1]

    - [1] #1 = = ^ ^ ^ .\!\!^ d .\!\!^ h .\!\!^ m .\!\!^ s .\!\!^ @mss

    thebibliography [1] 20pt to REFERENCES 6pt =0pt -12pt 10pt plus 3pt =0pt =0pt =1pt plus 1pt =0pt =0pt -12pt =13pt plus 1pt =20pt =13pt plus 1pt \@M =10000 =-1.0em =0pt =0pt 0pt =0pt =1.0em @enumiv\@empty 10000 10000 `\.\@m \@noitemerr \@latex@warning Empty `thebibliography' environment \@ifnextchar \@reference \@latexerr Missing key on reference command E...

    2021

  2. [2]

    , " * write output.state after.block = add.period write newline

    ENTRY address author booktitle chapter edition editor howpublished institution journal key month note number organization pages publisher school series title type volume year label extra.label sort.label short.list INTEGERS output.state before.all mid.sentence after.sentence after.block FUNCTION init.state.consts #0 'before.all := #1 'mid.sentence := #2 '...

  3. [3]

    write newline

    " write newline "" before.all 'output.state := FUNCTION n.dashify 't := "" t empty not t #1 #1 substring "-" = t #1 #2 substring "--" = not "--" * t #2 global.max substring 't := t #1 #1 substring "-" = "-" * t #2 global.max substring 't := while if t #1 #1 substring * t #2 global.max substring 't := if while FUNCTION word.in bbl.in " " * FUNCTION format....

  4. [4]

    Abt , H. A. 2009, , 180, 117, 10.1088/0067-0049/180/1/117

    doi:10.1088/0067-0049/180/1/117 2009

  5. [5]

    T., Maddison , S

    Agnew , M. T., Maddison , S. T., Horner , J., & Kane , S. R. 2019, , 485, 4703, 10.1093/mnras/stz345

    doi:10.1093/mnras/stz345 2019

  6. [6]

    J., Morales , J

    Alonso-Floriano , F. J., Morales , J. C., Caballero , J. A., et al. 2015, , 577, A128, 10.1051/0004-6361/201525803

    doi:10.1051/0004-6361/201525803 2015

  7. [7]

    2012, Journal of Double Star Observations, 8, 15

    Anton , R. 2012, Journal of Double Star Observations, 8, 15

    2012

  8. [8]

    2019, Journal of Double Star Observations, 15, 336

    ---. 2019, Journal of Double Star Observations, 15, 336

    2019

Show all 138 references
  1. [9]

    H., Fletcher , J

    Batten , A. H., Fletcher , J. M., & Mann , P. J. 1978, Publications of the Dominion Astrophysical Observatory Victoria, 15, 121

    1978

  2. [10]

    P., Endl , M., Cochran , W

    Bowler , B. P., Endl , M., Cochran , W. D., et al. 2021, , 913, L26, 10.3847/2041-8213/abfec8

    2021 doi

  3. [11]

    Brandt , T. D. 2018, , 239, 31, 10.3847/1538-4365/aaec06

    2018 doi

  4. [12]

    2021, , 254, 42, 10.3847/1538-4365/abf93c

    ---. 2021, , 254, 42, 10.3847/1538-4365/abf93c

    2021 doi

  5. [13]

    D., Dupuy , T

    Brandt , T. D., Dupuy , T. J., & Bowler , B. P. 2019, , 158, 140, 10.3847/1538-3881/ab04a8

    2019 doi

  6. [14]

    D., Dupuy , T

    Brandt , T. D., Dupuy , T. J., Li , Y., et al. 2021, , 162, 186, 10.3847/1538-3881/ac042e

    2021 doi

  7. [15]

    R., Quirion , P

    Bruntt , H., Bedding , T. R., Quirion , P. O., et al. 2010, , 405, 1907, 10.1111/j.1365-2966.2010.16575.x

    2010

  8. [16]

    K., et al

    Bryson , S., Kunimoto , M., Kopparapu , R. K., et al. 2021, , 161, 36, 10.3847/1538-3881/abc418

    2021 doi

  9. [17]

    J., Kirkpatrick , J

    Burgasser , A. J., Kirkpatrick , J. D., Cutri , R. M., et al. 2000, , 531, L57, 10.1086/312522

    2000 doi

  10. [18]

    J., Christiansen , J

    Burke , C. J., Christiansen , J. L., Mullally , F., et al. 2015, , 809, 8, 10.1088/0004-637X/809/1/8

    2015 doi

  11. [19]

    P., Marcy , G

    Butler , R. P., Marcy , G. W., Fischer , D. A., et al. 1999, , 526, 916, 10.1086/308035

    1999 doi

  12. [20]

    P., Marcy , G

    Butler , R. P., Marcy , G. W., Williams , E., Hauser , H., & Shirts , P. 1997, , 474, L115, 10.1086/310444

    1997 doi

  13. [21]

    P., Vogt , S

    Butler , R. P., Vogt , S. S., Laughlin , G., et al. 2017, , 153, 208, 10.3847/1538-3881/aa66ca

    2017 doi

  14. [22]

    Carr , M. H. 1996, Water on Mars

    1996

  15. [23]

    2004, , 601, 289, 10.1086/380442

    Chanam \'e , J., & Gould , A. 2004, , 601, 289, 10.1086/380442

    2004 doi

  16. [24]

    D., et al

    Chen , M., Li , Y., Brandt , T. D., et al. 2022, , 163, 288, 10.3847/1538-3881/ac66d2

    2022 doi

  17. [25]

    2014, , 437, 879, 10.1093/mnras/stt1953

    Chini , R., Fuhrmann , K., Barr , A., et al. 2014, , 437, 879, 10.1093/mnras/stt1953

    2014 doi

  18. [26]

    2016, , 823, 102, 10.3847/0004-637X/823/2/102

    Choi , J., Dotter , A., Conroy , C., et al. 2016, , 823, 102, 10.3847/0004-637X/823/2/102

    2016 doi

  19. [27]

    R., Bean , J., Burt , J., et al

    Ciardi , D. R., Bean , J., Burt , J., et al. 2019, arXiv e-prints, arXiv:1903.05665, 10.48550/arXiv.1903.05665

    2019 doi arXiv

  20. [28]

    Corbally , C. J. 1984, , 55, 657, 10.1086/190973

    1984 doi

  21. [29]

    S., Leifer , S., et al

    Crass , J., Gaudi , B. S., Leifer , S., et al. 2021, arXiv e-prints, arXiv:2107.14291, 10.48550/arXiv.2107.14291

    2021 doi arXiv

  22. [30]

    M., Brandt , T

    Currie , T., Brandt , G. M., Brandt , T. D., et al. 2023, Science, 380, 198, 10.1126/science.abo6192

    2023 doi

  23. [31]

    2011, Journal of Double Star Observations, 7, 104

    Daley , J. 2011, Journal of Double Star Observations, 7, 104

    2011

  24. [32]

    V., Fatuzzo , M., & Adams , F

    David , E.-M., Quintana , E. V., Fatuzzo , M., & Adams , F. C. 2003, , 115, 825, 10.1086/376395

    2003 doi

  25. [33]

    J., Nielsen , E

    De Rosa , R. J., Nielsen , E. L., Wahhaj , Z., et al. 2023, , 672, A94, 10.1051/0004-6361/202345877

    2023 doi

  26. [34]

    2016, , 222, 8, 10.3847/0067-0049/222/1/8

    Dotter , A. 2016, , 222, 8, 10.3847/0067-0049/222/1/8

    2016 doi

  27. [35]

    J., & Liu , M

    Dupuy , T. J., & Liu , M. C. 2011, , 733, 122, 10.1088/0004-637X/733/2/122

    2011 doi

  28. [36]

    El-Badry , K., Rix , H.-W., & Heintz , T. M. 2021, , 506, 2269, 10.1093/mnras/stab323

    2021 doi

  29. [37]

    2002, , 392, 671, 10.1051/0004-6361:20020937

    Endl , M., K \"u rster , M., Els , S., et al. 2002, , 392, 671, 10.1051/0004-6361:20020937

    2002 doi

  30. [38]

    2019, , 490, 5002, 10.1093/mnras/stz2912

    Feng , F., Anglada-Escud \'e , G., Tuomi , M., et al. 2019, , 490, 5002, 10.1093/mnras/stz2912

    2019 doi

  31. [39]

    P., Vogt , S

    Feng , F., Butler , R. P., Vogt , S. S., et al. 2022, , 262, 21, 10.3847/1538-4365/ac7e57

    2022 doi

  32. [40]

    1999, , 351, 619, 10.48550/arXiv.astro-ph/9909342

    Forveille , T., Beuzit , J.-L., Delfosse , X., et al. 1999, , 351, 619, 10.48550/arXiv.astro-ph/9909342

    1999 doi arXiv

  33. [41]

    P., Zhou , Y., et al

    Franson , K., Bowler , B. P., Zhou , Y., et al. 2023, , 950, L19, 10.3847/2041-8213/acd6f6

    2023 doi

  34. [42]

    2015, , 809, 107, 10.1088/0004-637X/809/1/107

    Fuhrmann , K., & Chini , R. 2015, , 809, 107, 10.1088/0004-637X/809/1/107

    2015 doi

  35. [43]

    2017, , 836, 139, 10.3847/1538-4357/836/1/139

    Fuhrmann , K., Chini , R., Kaderhandt , L., & Chen , Z. 2017, , 836, 139, 10.3847/1538-4357/836/1/139

    2017 doi

  36. [44]

    J., Rosenthal , L

    Fulton , B. J., Rosenthal , L. J., Hirsch , L. A., et al. 2021, , 255, 14, 10.3847/1538-4365/abfcc1

    2021 doi

  37. [45]

    2022, VizieR Online Data Catalog: Gaia DR3 Part 1

    Gaia Collaboration . 2022, VizieR Online Data Catalog: Gaia DR3 Part 1. Main source (Gaia Collaboration, 2022) , VizieR On-line Data Catalog: I/355. Originally published in: Astron. Astrophys., in prep. (2022), 10.26093/cds/vizier.1355

    2022 doi

  38. [46]

    Gaia Collaboration , Prusti , T., de Bruijne , J. H. J., et al. 2016, , 595, A1, 10.1051/0004-6361/201629272

    2016 doi

  39. [47]

    Gaia Collaboration , Vallenari , A., Brown , A. G. A., et al. 2023, , 674, A1, 10.1051/0004-6361/202243940

    2023 doi

  40. [48]

    H., et al

    Gandolfi , D., Barrag \'a n , O., Livingston , J. H., et al. 2018, , 619, L10, 10.1051/0004-6361/201834289

    2018 doi

  41. [49]

    Gianninas , A., Bergeron , P., & Ruiz , M. T. 2011, , 743, 138, 10.1088/0004-637X/743/2/138

    2011 doi

  42. [50]

    2017, Nature Astronomy, 1, 0056, 10.1038/s41550-017-0056

    Gillon , M., Demory , B.-O., Van Grootel , V., et al. 2017, Nature Astronomy, 1, 0056, 10.1038/s41550-017-0056

    2017 doi

  43. [51]

    M., Beust , H., et al

    Grandjean , A., Lagrange , A. M., Beust , H., et al. 2019, , 627, L9, 10.1051/0004-6361/201935044

    2019 doi

  44. [52]

    O., Corbally , C

    Gray , R. O., Corbally , C. J., Garrison , R. F., et al. 2006, , 132, 161, 10.1086/504637

    2006 doi

  45. [53]

    O., Corbally , C

    Gray , R. O., Corbally , C. J., Garrison , R. F., McFadden , M. T., & Robinson , P. E. 2003, , 126, 2048, 10.1086/378365

    2003 doi

  46. [54]

    O., Napier , M

    Gray , R. O., Napier , M. G., & Winkler , L. I. 2001, , 121, 2148, 10.1086/319956

    2001 doi

  47. [55]

    K., Dressing , C

    Harada , C. K., Dressing , C. D., Kane , S. R., & Ardestani , B. A. 2024 a , , 272, 30, 10.3847/1538-4365/ad3e81

    2024 doi

  48. [56]

    K., Dressing , C

    Harada , C. K., Dressing , C. D., Kane , S. R., et al. 2024 b , arXiv e-prints, arXiv:2409.10679, 10.48550/arXiv.2409.10679

    2024 doi

  49. [57]

    P., Cochran , W

    Hatzes , A. P., Cochran , W. D., McArthur , B., et al. 2000, , 544, L145, 10.1086/317319

    2000 doi

  50. [58]

    P., Gandolfi , D., Korth , J., et al

    Hatzes , A. P., Gandolfi , D., Korth , J., et al. 2022, , 163, 223, 10.3847/1538-3881/ac5dcb

    2022 doi

  51. [59]

    1998, , 129, 431, 10.1051/aas:1998195

    Hauck , B., & Mermilliod , M. 1998, , 129, 431, 10.1051/aas:1998195

    1998 doi

  52. [60]

    1785, Philosophical Transactions of the Royal Society of London Series I, 75, 40

    Herschel , W. 1785, Philosophical Transactions of the Royal Society of London Series I, 75, 40

  53. [61]

    D., et al

    Hinkley , S., Lacour , S., Marleau , G. D., et al. 2023, , 671, L5, 10.1051/0004-6361/202244727

    2023 doi

  54. [62]

    A., Rosenthal , L., Fulton , B

    Hirsch , L. A., Rosenthal , L., Fulton , B. J., et al. 2021, , 161, 134, 10.3847/1538-3881/abd639

    2021 doi

  55. [63]

    X., Burt , J., Vanderburg , A., et al

    Huang , C. X., Burt , J., Vanderburg , A., et al. 2018, , 868, L39, 10.3847/2041-8213/aaef91

    2018 doi

  56. [64]

    A., Fulton , B., Isaacson , H., et al

    Hurt , S. A., Fulton , B., Isaacson , H., et al. 2022, , 163, 218, 10.3847/1538-3881/ac5c47

    2022 doi

  57. [65]

    2015, Journal of Double Star Observations, 11, 91

    Iverson , E., & Nugent , R. 2015, Journal of Double Star Observations, 11, 91

    2015

  58. [66]

    G., Pichardo , B., & Aguilar , L

    Jaime , L. G., Pichardo , B., & Aguilar , L. 2012, , 427, 2723, 10.1111/j.1365-2966.2012.21839.x

    2012

  59. [67]

    C., Endl , M., Cochran , W

    Johnson , M. C., Endl , M., Cochran , W. D., et al. 2016, , 821, 74, 10.3847/0004-637X/821/2/74

    2016 doi

  60. [68]

    Jones , H. R. A., Paul Butler , R., Tinney , C. G., et al. 2002, , 333, 871, 10.1046/j.1365-8711.2002.05459.x

    2002

  61. [69]

    2017, , 55, 433, 10.1146/annurev-astro-082214-122238

    Kaltenegger , L. 2017, , 55, 433, 10.1146/annurev-astro-082214-122238

    2017 doi

  62. [70]

    R., & Blunt , S

    Kane , S. R., & Blunt , S. 2019, , 158, 209, 10.3847/1538-3881/ab4c3e

    2019 doi

  63. [71]

    R., Li , Z., Turnbull , M

    Kane , S. R., Li , Z., Turnbull , M. C., Dressing , C. D., & Harada , C. K. 2024, , 168, 195, 10.3847/1538-3881/ad6a50

    2024 doi

  64. [72]

    F., Whitmire , D

    Kasting , J. F., Whitmire , D. P., & Reynolds , R. T. 1993, , 101, 108, 10.1006/icar.1993.1010

    1993

  65. [73]

    C., & McNeil , R

    Keenan , P. C., & McNeil , R. C. 1989, , 71, 245, 10.1086/191373

    1989 doi

  66. [74]

    O., Castanheira , B

    Kepler , S. O., Castanheira , B. G., Costa , A. F. M., & Koester , D. 2006, , 372, 1799, 10.1111/j.1365-2966.2006.10992.x

    2006

  67. [75]

    2019, , 623, A72, 10.1051/0004-6361/201834371

    Kervella , P., Arenou , F., Mignard , F., & Th \'e venin , F. 2019, , 623, A72, 10.1051/0004-6361/201834371

    2019 doi

  68. [76]

    2022, , 657, A7, 10.1051/0004-6361/202142146

    Kervella , P., Arenou , F., & Th \'e venin , F. 2022, , 657, A7, 10.1051/0004-6361/202142146

    2022 doi

  69. [77]

    Kharchenko , N. V. 2001, Kinematika i Fizika Nebesnykh Tel, 17, 409

    2001

  70. [78]

    R., McCaughrean , M

    King , R. R., McCaughrean , M. J., Homeier , D., et al. 2010, , 510, A99, 10.1051/0004-6361/200912981

    2010 doi

  71. [79]

    D., Henry , T

    Kirkpatrick , J. D., Henry , T. J., & McCarthy , Jr., D. W. 1991, , 77, 417, 10.1086/191611

    1991 doi

  72. [80]

    D., Kellogg , K., Schneider , A

    Kirkpatrick , J. D., Kellogg , K., Schneider , A. C., et al. 2016, , 224, 36, 10.3847/0067-0049/224/2/36

    2016 doi

  73. [81]

    K., & Barnes , R

    Kopparapu , R. K., & Barnes , R. 2010, , 716, 1336, 10.1088/0004-637X/716/2/1336

    2010 doi

  74. [82]

    K., Ramirez , R

    Kopparapu , R. K., Ramirez , R. M., SchottelKotte , J., et al. 2014, , 787, L29, 10.1088/2041-8205/787/2/L29

    2014 doi

  75. [83]

    K., Ramirez , R., Kasting , J

    Kopparapu , R. K., Ramirez , R., Kasting , J. F., et al. 2013, , 765, 131, 10.1088/0004-637X/765/2/131

    2013 doi

  76. [84]

    L., Ireland , M

    Kraus , A. L., Ireland , M. J., Huber , D., Mann , A. W., & Dupuy , T. J. 2016, , 152, 8, 10.3847/0004-6256/152/1/8

    2016 doi

  77. [85]

    Lada , C. J. 2006, , 640, L63, 10.1086/503158

    2006 doi

  78. [86]

    A., Mamajek , E

    Laliotis , K., Burt , J. A., Mamajek , E. E., et al. 2023, , 165, 176, 10.3847/1538-3881/acc067

    2023 doi

  79. [87]

    D., Brandt , G

    Li , Y., Brandt , T. D., Brandt , G. M., et al. 2021, , 162, 266, 10.3847/1538-3881/ac27ab

    2021 doi

  80. [88]

    J., Ruffio , J.-B., et al

    Llop-Sayson , J., Wang , J. J., Ruffio , J.-B., et al. 2021, , 162, 181, 10.3847/1538-3881/ac134a

    2021 doi

  81. [89]

    2010, Observations et Travaux, 75, 17

    Losse , F. 2010, Observations et Travaux, 75, 17

    2010

  82. [90]

    J., Kirkpatrick , J

    Lowrance , P. J., Kirkpatrick , J. D., & Beichman , C. A. 2002, , 572, L79, 10.1086/341554

    2002 doi

  83. [91]

    2023, NASA ExEP Mission Star List for the Habitable Worlds Observatory

    Mamajek , E., & Stapelfeldt , K. 2023, NASA ExEP Mission Star List for the Habitable Worlds Observatory

    2023

  84. [92]

    W., Dupuy , T., Kraus , A

    Mann , A. W., Dupuy , T., Kraus , A. L., et al. 2019, , 871, 63, 10.3847/1538-4357/aaf3bc

    2019 doi

  85. [93]

    1982, Celestial Mechanics, 26, 311, 10.1007/BF01230725

    Marchal , C., & Bozis , G. 1982, Celestial Mechanics, 26, 311, 10.1007/BF01230725

    1982 doi

  86. [94]

    2013, , 551, A90, 10.1051/0004-6361/201219639

    Marmier , M., S \'e gransan , D., Udry , S., et al. 2013, , 551, A90, 10.1051/0004-6361/201219639

    2013 doi

  87. [95]

    D., Hartkopf , W

    Mason , B. D., Hartkopf , W. I., & Miles , K. N. 2017, , 154, 200, 10.3847/1538-3881/aa803e

    2017 doi

  88. [96]

    D., Williams , S

    Mason , B. D., Williams , S. J., Matson , R. A., et al. 2021, , 162, 53, 10.3847/1538-3881/abfaa2

    2021 doi

  89. [97]

    D., Wycoff , G

    Mason , B. D., Wycoff , G. L., Hartkopf , W. I., Douglass , G. G., & Worley , C. E. 2001, , 122, 3466, 10.1086/323920

    2001 doi

  90. [98]

    S., Carter , Carter, A

    Matthews , E. S., Carter , Carter, A. L., Pathak , P., & Morley , C. V. 2024, Nature, 10.1038/s41586-024-07837-8

    2024 doi

  91. [99]

    J., et al

    Mawet , D., Hirsch , L., Lee , E. J., et al. 2019, , 157, 33, 10.3847/1538-3881/aaef8a

    2019 doi

  92. [100]

    2003, The Messenger, 114, 20

    Mayor , M., Pepe , F., Queloz , D., et al. 2003, The Messenger, 114, 20

    2003

  93. [101]

    J., Close , L

    McCaughrean , M. J., Close , L. M., Scholz , R. D., et al. 2004, , 413, 1029, 10.1051/0004-6361:20034292

    2004 doi

  94. [102]

    Mermilliod , J. C. 1997, VizieR Online Data Catalog: Homogeneous Means in the UBV System (Mermilliod 1991) , VizieR On-line Data Catalog: II/168. Originally published in: Institut d'Astronomie, Universite de Lausanne (1991)

    1991

  95. [103]

    2023, , 672, A93, 10.1051/0004-6361/202345865

    Mesa , D., Gratton , R., Kervella , P., et al. 2023, , 672, A93, 10.1051/0004-6361/202345865

    2023 doi

  96. [104]

    2015, , 584, A72, 10.1051/0004-6361/201526822

    Motalebi , F., Udry , S., Gillon , M., et al. 2015, , 584, A72, 10.1051/0004-6361/201526822

    2015 doi

  97. [105]

    G., et al

    Naef , D., Mayor , M., Korzennik , S. G., et al. 2003, , 410, 1051, 10.1051/0004-6361:20031341

    2003 doi

  98. [106]

    2025, Planetary Systems, Version: 2025-03-31 11:50, NExScI-Caltech/IPAC, 10.26133/NEA12

    NASA Exoplanet Archive . 2025, Planetary Systems, Version: 2025-03-31 11:50, NExScI-Caltech/IPAC, 10.26133/NEA12

    2025 doi

  99. [107]

    2021, Pathways to Discovery in Astronomy and Astrophysics for the 2020s , 10.17226/26141

    National Academies of Sciences , E., & Medicine. 2021, Pathways to Discovery in Astronomy and Astrophysics for the 2020s , 10.17226/26141

    2021 doi

  100. [108]

    D., Plavchan , P., Burt , J

    Newman , P. D., Plavchan , P., Burt , J. A., et al. 2023, , 165, 151, 10.3847/1538-3881/acad07

    2023 doi

  101. [109]

    L., De Rosa , R

    Nielsen , E. L., De Rosa , R. J., Macintosh , B., et al. 2019, , 158, 13, 10.3847/1538-3881/ab16e9

    2019 doi

  102. [110]

    2011, , 192, 3, 10.1088/0067-0049/192/1/3

    Paxton , B., Bildsten , L., Dotter , A., et al. 2011, , 192, 3, 10.1088/0067-0049/192/1/3

    2011 doi

  103. [111]

    2013, , 208, 4, 10.1088/0067-0049/208/1/4

    Paxton , B., Cantiello , M., Arras , P., et al. 2013, , 208, 4, 10.1088/0067-0049/208/1/4

    2013 doi

  104. [112]

    2015, , 220, 15, 10.1088/0067-0049/220/1/15

    Paxton , B., Marchant , P., Schwab , J., et al. 2015, , 220, 15, 10.1088/0067-0049/220/1/15

    2015 doi

  105. [113]

    B., et al

    Paxton , B., Schwab , J., Bauer , E. B., et al. 2018, , 234, 34, 10.3847/1538-4365/aaa5a8

    2018 doi

  106. [114]

    Perryman , M. A. C., Lindegren , L., Kovalevsky , J., et al. 1997, , 323, L49

    1997

  107. [115]

    M., Rubini , P., Kiefer , F., & Chomez , A

    Philipot , F., Lagrange , A. M., Rubini , P., Kiefer , F., & Chomez , A. 2023, , 670, A65, 10.1051/0004-6361/202245396

    2023 doi

  108. [116]

    2020, , 159, 80, 10.3847/1538-3881/ab64fa

    Quarles , B., Li , G., Kostov , V., & Haghighipour , N. 2020, , 159, 80, 10.3847/1538-3881/ab64fa

    2020 doi

  109. [117]

    2018, , 856, 150, 10.3847/1538-4357/aab264

    Quarles , B., Satyal , S., Kostov , V., Kaib , N., & Haghighipour , N. 2018, , 856, 150, 10.3847/1538-4357/aab264

    2018 doi

  110. [118]

    A., Henry , T

    Raghavan , D., McAlister , H. A., Henry , T. J., et al. 2010, , 190, 1, 10.1088/0067-0049/190/1/1

    2010 doi

  111. [119]

    2022, in The 21st Cambridge Workshop on Cool Stars, Stellar Systems, and the Sun, Cambridge Workshop on Cool Stars, Stellar Systems, and the Sun, 218, 10.5281/zenodo.7669746

    Reyl \'e , C., Jardine , K., Fouqu \'e , P., et al. 2022, in The 21st Cambridge Workshop on Cool Stars, Stellar Systems, and the Sun, Cambridge Workshop on Cool Stars, Stellar Systems, and the Sun, 218, 10.5281/zenodo.7669746

    2022 doi

  112. [120]

    L., Matthews , E., Ceva , W., et al

    Rickman , E. L., Matthews , E., Ceva , W., et al. 2022, , 668, A140, 10.1051/0004-6361/202244633

    2022 doi

  113. [121]

    L., Ceva , W., Matthews , E

    Rickman , E. L., Ceva , W., Matthews , E. C., et al. 2024, arXiv e-prints, arXiv:2401.10058, 10.48550/arXiv.2401.10058

    2024 doi arXiv

  114. [122]

    R., Duch \^e ne , G., Tom , H., et al

    Rodriguez , D. R., Duch \^e ne , G., Tom , H., et al. 2015, , 449, 3160, 10.1093/mnras/stv483

    2015 doi

  115. [123]

    J., Fulton , B

    Rosenthal , L. J., Fulton , B. J., Hirsch , L. A., et al. 2021, , 255, 8, 10.3847/1538-4365/abe23c

    2021 doi

  116. [124]

    D., McCaughrean , M

    Scholz , R. D., McCaughrean , M. J., Lodieu , N., & Kuhlbrodt , B. 2003, , 398, L29, 10.1051/0004-6361:20021847

    2003 doi

  117. [125]

    C., & Head , J

    Solomon , S. C., & Head , J. W. 1991, Science, 252, 252, 10.1126/science.252.5003.252

    1991 doi

  118. [126]

    B., Sills , A., et al

    Takeda , G., Ford , E. B., Sills , A., et al. 2007, , 168, 297, 10.1086/509763

    2007 doi

  119. [127]

    2021, , 161, 144, 10.3847/1538-3881/abda42

    Tokovinin , A. 2021, , 161, 144, 10.3847/1538-3881/abda42

    2021 doi

  120. [128]

    Torres , C. A. O., Quast , G. R., da Silva , L., et al. 2006, , 460, 695, 10.1051/0004-6361:20065602

    2006 doi

  121. [129]

    W., Stark , C

    Tuchow , N. W., Stark , C. C., & Mamajek , E. 2024, , 167, 139, 10.3847/1538-3881/ad25ec

    2024 doi

  122. [130]

    2007, , 474, 653, 10.1051/0004-6361:20078357

    van Leeuwen , F. 2007, , 474, 653, 10.1051/0004-6361:20078357

    2007 doi

  123. [131]

    Van Zandt , J., & Petigura , E. A. 2024, , 167, 250, 10.3847/1538-3881/ad390b

    2024 doi

  124. [132]

    Venner , A., Vanderburg , A., & Pearce , L. A. 2021, , 162, 12, 10.3847/1538-3881/abf932

    2021 doi

  125. [133]

    S., Butler , R

    Vogt , S. S., Butler , R. P., Marcy , G. W., et al. 2005, , 632, 638, 10.1086/432901

    2005 doi

  126. [134]

    S., Allen , S

    Vogt , S. S., Allen , S. L., Bigelow , B. C., et al. 1994, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol. 2198, Instrumentation in Astronomy VIII, ed. D. L. Crawford & E. R. Craine , 362, 10.1117/12.176725

    1994 doi

  127. [135]

    S., Burt , J., Meschiari , S., et al

    Vogt , S. S., Burt , J., Meschiari , S., et al. 2015, , 814, 12, 10.1088/0004-637X/814/1/12

    2015 doi

  128. [136]

    2003, , 8188, 2

    Volk , K., Blum , R., Walker , G., & Puxley , P. 2003, , 8188, 2

    2003

  129. [137]

    W., & Wyatt , M

    Xuan , J. W., & Wyatt , M. C. 2020, , 497, 2096, 10.1093/mnras/staa2033

    2020 doi

  130. [138]

    K., Oswalt , T

    Zhao , J. K., Oswalt , T. D., Rudkin , M., Zhao , G., & Chen , Y. Q. 2011, , 141, 107, 10.1088/0004-6256/141/4/107

    2011 doi

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