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HWO Target Stars and Systems: Activity and Rotation Catalog (ARC) of Potential Target Stars for the Habitable Worlds Observatory

T0 review · 2 major / 5 minor · reviewed 2026-08-02 · deepseek-v4-flash

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Pith's one-line read Activity and rotation are measured for most high-priority exoplanet-imaging targets, but activity cycles are known for under 20%, so cycle monitoring must begin now.

desk verdict Solid, transparent HWO activity/rotation catalog with an abstract that overstates its own Table 1 completeness. read the letter →

arxiv 2605.22618 v2 pith:OBWY6GKX submitted 2026-05-21 astro-ph.SR astro-ph.EP

Tara Fetherolf , Arvind F. Gupta , Elisabeth R. Newton , Andrea P. Buccino , Jennifer A. Burt , Jose A. Caballero , Sebastian Carrazco-Gaxiola , Mariela C. Vieytes
show 2 more authors
Natalie R. Hinkel Eric E. Mamajek
This is my paper · ORCID
classification astro-ph.SRastro-ph.EP
keywords stellaractivityrotationperiodscycleschromospherichabitableworldsobservatorytargetselectioninclinationmagnetic
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

The paper aims to show that target preparation for the Habitable Worlds Observatory — a planned mission to directly image and characterize Earth-like exoplanets — is uneven: single-epoch measures of stellar activity and rotation are largely on record for the highest-priority stars, while the long-baseline measurement that actually matters for scheduling (the activity cycle) is almost entirely missing. To do this, the authors compile thousands of published measurements into a new catalog, the ARC, and count how many stars in each target-priority tier have each property. They find at least 70% of high-interest systems have some activity/rotation measurement, but fewer than 20% have a measured activity cycle. The reader should care because a star that is quiet today can be at cycle maximum during planned observations, and measuring a cycle takes decades of monitoring — so the window to start is now.

What carries the argument

The central object is the Activity and Rotation Catalog (ARC), a compiled list of adopted, ranked literature values for vsini, S-index, R'HK, rotation period, activity cycle, and photometric jitter for 7,981 of 12,944 potential HWO target stars. The argument runs on the completeness fractions this catalog enables: by counting how many stars per priority tier have each property, the paper isolates the temporal gap between snapshot measurements (activity, rotation) and the cycle measurement that requires decades of baseline. A second load-bearing piece is the inclination check, v sin i = (2πR*/P_rot) sin i, whose forbidden sin i>1 outcomes expose internal inconsistencies in the adopted single-

What would settle it

Recompute the completeness fractions from the catalog's Table 1 counting a star as characterized only if its activity indicator is measured at two or more epochs separated by at least a year; if that ≥70% single-epoch coverage drops to near the <20% activity-cycle coverage, the readiness gap is real but the 70% number is a snapshot, not a temporal characterization.

Watch

Extended reading notes

Core claim

The paper's central claim is a readiness gap: for the 164 highest-priority target stars (Tier 1) and the 495 next-tier stars, projected rotational velocity is measured for more than ~90% of stars, S-index and log R'HK activity metrics for roughly 60–90%, and rotation periods for ~60–70%, but activity cycles are measured for fewer than 20% of high-interest targets at every tier. The catalog also reveals that combining adopted vsini and Prot yields a biased inclination distribution and a subset of stars with sin i>1, so the authors caution against using the catalog for stellar inclinations without per-star vetting. They further find that a literature S-index to R'HK conversion produces wide sc

Load-bearing premise

The 70% readiness claim assumes a star counts as 'characterized' when any archival catalog lists a measurement for it, even if that measurement is from a single epoch, decades old, or inconsistent with another measurement of the same star.

Editorial extensions

If this is right

  • If the completeness fractions are right, target-selection work for HWO should shift from measuring rotation and activity once to building long-baseline cycle records for Tier 1 and 2 stars.
  • The <20% activity-cycle coverage means that without new monitoring programs starting now, the mission could fly without knowing which quiet-looking stars will be at cycle maximum.
  • The biased inclination distribution implies that population-level spin-orbit alignment studies should not rely on the ARC's vsini/Prot pairs until the sources of the sin i>1 outliers are resolved.
  • The wide scatter between literature R'HK values and uniformly recalculated ones indicates that activity levels in the literature are not on a homogeneous scale, so cross-star activity comparisons should use the recalculated values.
  • The shallow slopes of cycle-versus-rotation relations are consistent with previous work; a larger cycle sample would sharpen or revise those dynamo constraints.

Reading between the lines

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

  • A fair reading suggests the ≥70% figure is an upper bound on readiness: if 'characterized' requires temporal coverage rather than any archival entry, the true readiness level is closer to the <20% activity-cycle fraction.
  • A concrete next step the paper leaves implicit is a dedicated, multi-year monitoring program targeting the ~100 highest-priority stars that lack cycles, using any spectrograph able to measure Ca II H&K emission; this is feasible with modest facilities.
  • The sin i>1 tension hints that several adopted rotation periods are likely harmonic aliases of the true periods (and some vsini values may be inflated by macroturbulence); resolving this could turn the catalog into a genuine inclination tool.
  • One testable prediction of the paper's framing: recomputing completeness with only measurements taken within, say, the last five years will lower the single-epoch completeness, while the activity-cycle fraction stays near 20%.
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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 / 5 minor

Summary. The paper compiles archival measurements of stellar activity (S-index, R'HK) and rotation (vsini, Prot), plus activity cycles and photometric jitter, for the prioritized Habitable Worlds Observatory target lists HPIC/TSS25 (Tiers 1–3). The authors document their source ranking per property, present the resulting Activity and Rotation Catalog (ARC), recalculate R'HK with two uniform calibrations, and assess completeness by tier. They report that at least 70% of high-interest (Tier 1+2) systems have activity and rotation measurements, but fewer than 20% have measured activity cycles. They also use the catalog to examine inclination distributions, rotation-activity-age relations, and the activity-cycle/rotation relation, concluding that the inclination inference is unreliable and that long-baseline activity-cycle monitoring should begin now.

Significance. If the central claims hold, the ARC is a valuable planning resource for HWO target selection: it is one of the first comprehensive gap assessments for activity and rotation characterization of potential HWO targets, and the <20% activity-cycle completeness finding is a clear, actionable result. The paper is unusually transparent about source ranking, exclusions, and caveats; Appendix A provides cross-match verification, and the catalog is machine-readable. The internally generated R'HK values are explicitly labeled as recalculations from external calibrations, not independent measurements. The main uncertainty is the headline completeness figure, which the paper's own Table 1 does not fully support as stated.

major comments (2)
  1. [Abstract; §4.2, Table 1] The abstract's central quantitative claim that 'stellar activity (S-index and R'HK) and rotation (vsini and Prot) properties have been measured for at least 70% systems' is not supported for the combined Tier 1+2 sample. Summing Table 1: vsini = (160+444)/659 = 91.7%, S-index = (147+392)/659 = 81.8%, R'HK = (123+308)/659 = 65.4%, and Prot = (118+325)/659 = 67.2%. Two of the four named properties fall below 70%, and the fraction with all four measured is at most 65.4%. The text in §4.2 gives per-property ranges that are consistent with these numbers, but the abstract overstates the result. Please revise the abstract to report per-property completeness, or explicitly define the combined criterion used.
  2. [§4.2, §3, §5.1, Fig. 3, Fig. A1] The completeness fractions count a star as 'measured' if it appears in any adopted archival catalog, regardless of epoch, baseline, or mutual consistency. The paper itself documents that measurements for a given star are not necessarily contemporaneous (§3), that adopted vsini and Prot pairs yield forbidden sin i > 1 values and a biased inclination distribution (§5.1, Fig. 3), and that some vsini sources show systematic offsets at low vsini (Fig. A1). Under a stricter 'characterized' definition—one requiring time-resolved or contemporaneous coverage—the ≥70% figure is an upper bound. This should be stated explicitly in the abstract or in §4.2, and the completeness discussion should distinguish 'presence of any measurement' from 'characterization sufficient for mission planning.' The <20% activity-cycle finding is not affected by this concern.
minor comments (5)
  1. [Appendix A, Fig. A2 caption] The caption reads 'Same as Figure A2' but should be 'Same as Figure A1'.
  2. [§4.2] The sentence 'The S-index and log R'HK activity metrics are generally well measured across Tiers 1 and 2 (60–90%)' is consistent with Table 1, but the phrase '(60–90%)' should be reconciled with the abstract's 'at least 70%' claim to avoid apparent inconsistency.
  3. [§6] The text uses 'EPR V community'; the standard abbreviation is 'EPRV'. Please correct.
  4. [§5.3, Figs. 7–8] The 'best-fit linear relationship' is reported with slopes and 3σ uncertainties, but the fitting method, sample selection, and treatment of upper limits or outliers are not described. A sentence specifying the fitting procedure would improve reproducibility.
  5. [Table 1] The column header row appears as 'N1 N2 N3' and the table caption lists 'N1, N2, and N3' but the table body is split across lines; consider clarifying the tier-count definitions directly in the caption.

Circularity Check

0 steps flagged · score 0.0 of 10

No circularity: ARC is a literature compilation; completeness counts and recalculated R'HK values derive from external data and published calibrations, not from the paper's own fitted outputs.

full rationale

The paper's derivation chain is catalog construction, not a fitted model. The completeness fractions in §4.2/Table 1 are tallies of whether a measurement exists in external literature catalogs; no parameter is fitted to those tallies and then renamed a prediction. The internally generated quantities are the recalculated R'HK values (§4.1), but the paper explicitly says "we re-calculate R'HK values from the adopted S-index values using two different calibrations" (Eq. 1, using C_cf from Rutten 1984, R_phot from Noyes 1984, and Marvin et al. 2023); these are labeled as recalculations and compared with literature values, not presented as independent measurements. The rotation/activity and cycle/rotation regressions in §5.2–5.3 are descriptive fits to the compiled data, not first-principles predictions. Self-citations such as Fetherolf et al. (2023) TESS-SVC and Tuchow et al. (2024, 2025) HPIC/TSS25 provide input data or target lists, and no load-bearing argument reduces to an unverified self-citation or an imported uniqueness theorem. The paper itself flags the counting caveats: in §5.1, adopted vsini+Prot pairs yield sin i > 1 and "we therefore advise that this catalog not be used to compute stellar inclinations without more careful vetting of the source data for individual stars"; in §3, "measurements for a given star are not necessarily collected at the same time and may reflect different levels of magnetic activity." These are internal-consistency limitations, not circular reductions. The only in-prep citation (Peralta & Vieytes) is motivational, not load-bearing. The abstract's "at least 70%" is numerically loose if read over all Tier 1+2 (Table 1 gives RHK 431/659=65.4% and Prot 443/659=67.2%), though it holds for Tier 1 alone; this is an overstatement/ambiguity, not a circularity.

Assumptions & free parameters 5 free parameters · 6 assumptions · 0 invented entities

The ARC's central claim rests on trusting thousands of compiled literature values and on the transferability of calibrations (Mount Wilson S-index scale, Noyes/Rutten B−V-based R'HK conversions, Cranmer-Saar turnover timescales). No new physical entities are introduced. The paper itself demonstrates that one joint-usage assumption (rigid-rotation vsini–Prot consistency, Eq. 2) is violated for a subset of adopted values (§5.1), which is a useful self-limitation but also marks the weakest joint-inference premise.

free parameters (5)
  • ASAS-SN long-period exclusion threshold = >180 d excluded
    Rotation periods above 180 d from the ASAS-SN catalog were excluded as implausible for dwarf stars (§3.4). This hand-chosen cutoff shapes the adopted Prot distribution.
  • PyAstronomy R'HK recalculation range = B−V 0.44–1.2; Teff > 4000 K
    Limits imposed in §4.1 for recomputing R'HK from adopted S-index; stars outside this range receive no updated value, affecting which stars appear in Figures 4–5.
  • Unphysical S-index cutoff = S > 2 excluded
    §3.2 excludes stars with S>2 in source catalogs as unphysical; a handful of stars affected.
  • Rice & Brewer vsini valid range = 0.0044–18.71 km/s
    §3.1 adopts only vsini measurements inside this 'reliable range' defined by Rice & Brewer (2020); imported, not fitted here, but it restricts adopted values.
  • Per-property catalog ranking orders
    The adopted value for each star is the top of a hand-chosen ranking of source catalogs (§3). Not numeric fits, but a selection rule that fully determines the catalog's entries.
assumptions (6)
  • domain assumption Mount Wilson S-index calibration transfers to all compiled instruments
    The paper adopts catalog values ranked by whether they are 'calibrated to the Mount Wilson scale' (§3.2); cross-instrument systematics are assumed removed, with no independent check for most sources.
  • domain assumption R'HK conversion via Noyes et al. (1984) B−V relations applies to the target stars
    Used to recompute R'HK from S-index (§4.1); the paper restricts B−V 0.44–1.2 and Teff>4000 K for the PyAstronomy route, acknowledging limited calibration range.
  • domain assumption vsini = (2πR*/Prot) sin i with negligible oblateness and differential rotation
    Equation (2) in §5.1, used to test inclination distributions; the paper shows it fails for a subset (sin i>1), so this assumption is explicitly violated for some adopted values.
  • standard math Isotropic spin-axis distribution as the expected reference
    Equation (3) from Masuda & Winn (2020) used as the null distribution for the inclination comparison in §5.1.
  • domain assumption Cranmer & Saar (2011) convective turnover timescale relation
    Eqn. 36 of Cranmer & Saar (2011) used to compute Rossby numbers in §5.2; quoted as a formula but not re-derived.
  • domain assumption HPIC ages are reliable enough for age-activity relations
    §5.2 uses ages from Tuchow et al. (2024), which the paper notes are inhomogeneous and available for only 33.4% of stars.

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Cite this review

Pith. "Pith review of HWO Target Stars and Systems: Activity and Rotation Catalog (ARC) of Potential Target Stars for the Habitable Worlds Observatory." pith.science (2026). https://pith.science/paper/OBWY6GKX

@misc{pith2026260522618,
  author       = {Pith},
  title        = {Pith review of: HWO Target Stars and Systems: Activity and Rotation Catalog (ARC) of Potential Target Stars for the Habitable Worlds Observatory},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/OBWY6GKX}},
  note         = {Machine review of arXiv:2605.22618}
}
read the original abstract

A major goal of the Habitable Worlds Observatory (HWO) is to precisely characterize exoplanets and their atmospheres. However, magnetic activity from an exoplanet's host star can complicate measurements of both the stellar and planetary properties, and stellar activity can be an important factor in our interpretation of the evolutionary history of an exoplanet. In this work, we assess the extent to which magnetic activity has been characterized for potential HWO target stars by collating archival measurements of relevant observables as published in a broad range of photometric and spectroscopic datasets. We describe our data collection strategy, provide an overview of currently known activity and rotation properties in the Activity and Rotation Catalog (ARC) for potential HWO target stars, and briefly review known relationships between stellar inclination, rotation, activity, and age. Overall, we find that stellar activity (S-index and R'HK) and rotation (v sin i and Prot) properties have been measured for at least 70% systems that are currently of high interest as potential HWO atmospheric characterization targets. However, stellar activity is temporal in nature, such that activity properties should be regularly monitored in order to remain up-to-date for informing future observations. In particular, we find that stellar activity cycles are measured for fewer than 20% of high interest potential HWO target stars. Measuring a star's activity cycle is critical for anticipating times when higher levels of magnetic activity may occur during planned HWO observations, which may interfere with measuring precise exoplanet atmospheric characteristics.

Figures

Figures reproduced from arXiv: 2605.22618 by the authors.

Figure 1
Figure 1. Comparison in R ′ HK values from the literature (Section 3.3) and re-calculated using Marvin et al. (2023), in comparison to R ′ HK values recalculated using PyAstronomy. The points are colored by stellar effective temperatures and the one-to-one relationship is shown by a solid red line. Be￾cause of the limits of the calibrations in the method from PyAstronomy, M dwarfs are not included in these plots. 4.2. Catalog… view at source ↗
Figure 2
Figure 2. Completeness fractions for each of the stellar parameters included in the ARC. These are broken down by priority tier to highlight the relative sizes of the gaps in our knowledge between the highest priority (Tier 1) and lowest priority (Tier 3) stellar samples. The decline of stellar activity and rotation with age was established in Wilson & Skumanich (1964) and Sku￾manich (1972). The relations have been the subjec… view at source ↗
Figure 3
Figure 3. Upper panels: Equatorial rotational velocity (veq) vs. projected rotational velocity (v sin i) for stars in Tiers 1, 2, and 3. The v sin i values are taken directly from the ARC and the veq values are calculated using Prot from the ARC and R⋆ from the HPIC. Several stars in each tier fall in a region of parameter space that is mathematically forbidden, i.e., requiring sin i > 1. Lower Panels: Expected and observed i… view at source ↗
Figures from the paper (5 more)
Figure 4
Figure 4. Figure 4: Chromospheric activity log R ′ HK colored by ef￾fective temperature. The gray points represent stars with temperatures less than 5000 K. The red stars show medi￾ans in 1 Gyr bins, after data in the high-activity group is clipped. Ages are derived from Tuchow et al. (20…
Figure 6
Figure 6. Figure 6: Stellar activity cycle period versus rotation period with points colored by effective temperature for stars with these measurements available in the ARC. The active and inactive branch relationships from B¨ohm-Vitense (2007) are shown by the dashed and dash-dotted line…
Figure 5
Figure 5. Figure 5: Chromospheric activity log R ′ HK versus Rossby number, colored by effective temperature. Large Rossby numbers are slower rotators. The gray points represent stars with period measurements from Fetherolf et al. (2023), which uses TESS data and is therefore limited to P…
Figure 7
Figure 7. Figure 7: Ratio of stellar activity cycles to rotation pe￾riod versus rotation period with points colored by effective temperature. The best-fit linear relationship and its 3σ un￾certainty are shown by the dashed gray line and gray shaded region, respectively, with slope of 0.85…
Figure 8
Figure 8. Figure 8: Ratio of stellar activity cycles to rotation period versus the inverse of the Rossby number with points colored by effective temperature. The best-fit linear relationship and its 3σ uncertainty are shown by the dashed gray line and gray shaded region, respectively, wit…

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