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An updated catalog of HIRES/Keck radial velocity measurements. Including Ca II H&K measurements

T0 review · 3 major / 6 minor · reviewed 2026-08-05 · deepseek-v4-flash

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Pith's one-line read This paper presents an updated public HIRES/Keck radial-velocity catalog of 78,920 measurements for 1,702 stars, now paired with Ca II H&K activity indicators for roughly 40% of the spectra.

desk verdict The RV half is a solid, community-serving data release that will become standard reference; the new R'HK product is the weak spot because its absolute scale is never cross-calibrated against an external activity indicator. read the letter →

arxiv 2509.06072 v1 pith:BFGNHERW submitted 2025-09-07 astro-ph.EP astro-ph.IMastro-ph.SR

Jerusalem T. Teklu , Volker Perdelwitz , R. Paul Butler , Trifon Trifonov , Steven S. Vogt , Deepa Mukhija , Lev Tal-Or This is my paper · ORCID
classification astro-ph.EPastro-ph.IMastro-ph.SR
keywords radialvelocitycatalogstellaractivityCaIIH&KR'HKindexHIRES/KeckexoplanetdetectionchromosphericemissionPHOENIXspectralrectification
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

This paper claims to deliver the latest public version of the HIRES/Keck precision radial-velocity catalog: 78,920 velocity measurements for 1,702 stars, extending previous releases to March 2023. Its new contribution is pairing those velocities with the chromospheric activity indicator R'HK, derived from Ca II H&K emission in the same spectra for roughly 40% of the measurements, so that stellar-activity wobbles and genuine planetary signals can be told apart within a single dataset. The authors argue this matters because magnetic activity on the stellar surface produces velocity variations that mimic or mask exoplanet signals, and an activity measurement recorded at the same epoch as each velocity lets users test whether a candidate planetary period has a chromospheric counterpart. They also report a 2-3 m/s activity floor for slowly rotating stars, a correlation between activity-driven scatter and projected rotation, and no clear Vaughan-Preston gap in the activity-color diagram.

What carries the argument

The paper rests on two established techniques joined into one pipeline. Precision RVs come from the iodine absorption cell technique, in which iodine lines superimposed on the stellar spectrum supply both the wavelength scale and a measurement of the spectrograph point-spread function at each epoch. The activity indicator R'HK comes from the PHOENIX-rectification method: each spectrum is divided by a synthetic PHOENIX spectrum chosen from the star's Gaia/TESS parameters, using six narrow bands around the Ca II H and K lines to set the continuum, and the photospheric contribution is then subtracted to isolate chromospheric emission. The third piece is the nightly zero-point correction framewo

What would settle it

Take the subset of catalog stars that also appear in published long-term S-index monitoring programs, convert S to R'HK with the standard photospheric corrections, and compare against the values in this catalog as a function of Teff, logg, and metallicity. A systematic offset that scales with any of these parameters would show the PHOENIX photospheric subtraction is biased; agreement within uncertainties would confirm the absolute activity scale. A lighter test: recover the vsin i versus RV-scatter floor trend using only stars whose rotation periods are known from photometry, to confirm the fl

Watch

Extended reading notes

Core claim

The central claim is that the updated HIRES/Keck catalog — 78,920 precision RVs for 1,702 stars, corrected for nightly zero-point and intra-night drift systematics following the earlier release of TO19 — now includes, for the first time at this scale, per-spectrum R'HK activity measurements for about 40% of the spectra. R'HK is derived by rectifying each observed spectrum against PHOENIX synthetic spectra in six narrow bands around the Ca II H and K line cores and subtracting the computed photospheric flux, leaving the chromospheric excess. Individual spectra are flagged for flux calibration problems, unphysical wavelength solutions, and RV discrepancies above 3 km/s, yielding a 'clean sampl

Load-bearing premise

The absolute scale of the R'HK values assumes that PHOENIX synthetic spectra reproduce the true photospheric flux in the six narrow bands around the Ca II H and K lines, so that subtracting the model leaves only the chromospheric emission; if the model or the stellar parameters feeding it are wrong for a given star, the activity measurement is systematically offset, and the paper validates the time series for only three stars against S-index periods, not the absolute scale.

Editorial extensions

If this is right

  • Users can now check, for the same nights and the same stars, whether a candidate exoplanet period in the RVs also shows up in the R'HK time series — the standard test for an activity-induced false positive.
  • The 2-3 m/s scatter floor for slowly rotating stars quantifies the activity-limited precision of HIRES and clarifies which stars can still host detectable low-mass planets.
  • The empirical relation between RV scatter and projected rotational velocity offers a way to predict the minimum expected velocity jitter of a target star from its rotation alone.
  • The absence of a clear Vaughan-Preston gap in the activity-color diagram supports the view that chromospheric activity is a continuum rather than two distinct states.
  • The clean sample of 1,285 stars provides a ready-made, uniformly processed subset for population studies of activity cycles and rotation periods.

Reading between the lines

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

  • The absolute scale of the new R'HK values is not directly calibrated: if the PHOENIX photospheric subtraction is systematically wrong for some temperature or gravity range, relative activity variations would remain useful while absolute activity levels would be biased. A cross-check against S-index-calibrated R'HK over the full stellar-parameter range would settle this.
  • Because the R'HK extraction runs on archival pipeline-reduced spectra, the same pipeline could in principle be applied to the public archives of other echelle spectrographs with blue coverage, producing homogeneous activity indicators across surveys.
  • Providing per-measurement R'HK simultaneously with RVs invites a joint modeling approach in which activity indicators and velocities are fitted together, potentially recovering planets at amplitudes below the scatter that velocity-only fits would treat as noise.
  • The per-star median uncertainties tabulated for R'HK could serve as a quantitative prior on activity jitter amplitude for stars lacking long activity time series — an application the paper does not itself pursue.
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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

3 major / 6 minor

Summary. The paper presents an updated HIRES/Keck precision RV catalog, extending the Tal-Or et al. (2019) data through March 2023. The new product contains 78,920 RVs for 1,702 stars (14,440 spectra added) and, for the first time for this catalog, Ca II H&K R'HK measurements for 31,218 spectra (~40%). RVs are derived with the iodine-cell technique and corrected for nightly zero-point and intra-night drift; both corrected and uncorrected values are provided. R'HK is derived by rectifying spectra with PHOENIX synthetic models and subtracting the photospheric contribution, following Perdelwitz et al. (2021, 2024), with custom quality flags. The authors validate the NZP correction by Keplerian fits to 71 planet-hosting stars (mean ΔlogL=0.09, std=3.01) and demonstrate activity-cycle detections for three stars. They also analyze RV scatter versus vsini and R'HK versus color.

Significance. If the R'HK product is reliable, this will be a valuable public resource for disentangling stellar activity from planetary signals, providing uniform activity indicators for a large, long-baseline RV sample. The RV catalog is built on a mature pipeline; the internal counts are consistent, flags are documented, and the NZP validation is reported honestly, including its marginal improvement. The paper's main gap is the lack of absolute calibration of R'HK: the only external check is relative period recovery for three stars. Because the abstract and Sect. 3 use R'HK values for cross-star comparisons and call them high-quality, the absence of a comparison with published activity indices is a substantive weakness that should be fixed before publication.

major comments (3)
  1. [Sect. 2.4 / Fig. 7 / Sect. 3.3] The absolute R'HK scale is not validated. R'HK is obtained by subtracting a PHOENIX synthetic photospheric flux in six narrow bands; any bias in the model or in the Gaia/TESS stellar parameters propagates directly into the zero point and scale. The only external check is the recovery of activity-cycle periods for three stars (Sect. 3.3), which tests time variability, not absolute values. No comparison with published S-index or R'HK measurements (e.g., B17, Isaacson & Fischer 2010) is made. Since the abstract calls these 'high-quality' and Fig. 7 uses them for cross-star activity comparisons, this missing calibration is load-bearing. Please add a validation sample spanning Teff, logg, and [M/H] and report offsets/scatter.
  2. [Sect. 2.4 vs. Sect. 3] The 'clean sample' definition is internally inconsistent. Sect. 2.4 says it comprises approximately 21% of R'HK measurements, while Sect. 3 says it comprises 1,285 stars out of 1,702 (75.5%). The abstract states 'High-quality R'HK measurements are provided for ~40% of the HIRES catalog,' but Sect. 3 reports 31,218 spectra (40% of spectra, not stars). Please reconcile these numbers: how many stars have at least one unflagged R'HK value, and how many spectra are in the clean sample? This affects the central claim.
  3. [Sect. 3.3 / Table 2] The claimed agreement of activity-cycle periods with B17 is not quantified. The text reports 2817, 5522, and 4214 d for HD 7924, HD 219134, and HD 156668, but does not give the B17 S-index periods or their uncertainties, so 'closely match' cannot be evaluated. Since this is the only validation of the R'HK time series, provide a direct comparison (periods, uncertainties, FAPs) or otherwise demonstrate the agreement.
minor comments (6)
  1. [Sect. 3.3] The selection of the 'top three stars based on two criteria' is unclear; specify how stars were ranked (e.g., by number of observations? by R'HK?).
  2. [Fig. 8] The fitted periods are only in the text; include period values and B17 values in the figure panel or caption for readability.
  3. [Sect. 2.3 / Fig. 4] The 50-day moving-average window is mentioned only in the figure caption; define it in the text.
  4. [Sect. 3.1] Typo: 'it is is ~2.3 m/s' should be 'it is ~2.3 m/s'.
  5. [Sect. 3.1 / Fig. 6] The lower-envelope and median-uncertainty fits are based on only six stars; no uncertainties or goodness-of-fit are reported. If this relation is presented as a predictive framework, report fit parameters and scatter.
  6. [Sect. 2.2] The absolute RV derivation via PHOENIX-template CCF is summarized in one paragraph; if these values are part of the release, describe the validation (e.g., comparison with Gaia RVs) and flag any outliers.

Circularity Check

0 steps flagged · score 0.0 of 10

No circularity: RVs and R'HK are produced by applied pipelines with no fitted quantity renamed as prediction; the B17 cycle comparisons are independent.

full rationale

The paper's main deliverable is an updated RV catalog and R'HK activity measurements. The RV derivation uses the standard iodine-cell pipeline (Butler et al. 1996) and the NZP correction follows TO19; neither is fitted to the catalog results being claimed. The R'HK values are obtained by applying the published Perdelwitz et al. (2021, 2024) method, which uses PHOENIX synthetic spectra and fixed narrow passbands; no parameter in that method is fitted to the HIRES R'HK output, so the output is not an input by construction. The only validation shown (Sect. 3.3) compares three R'HK cycle periods with B17 S-index periods; these are independent time series, so the agreement is evidence rather than a tautology. The skeptic's concern is that the absolute R'HK scale is not calibrated against published absolute activity values (e.g., Isaacson & Fischer 2010) and therefore 'high-quality' is not fully substantiated. That is a missing-validation/correctness-risk point, not circularity. No equation reduces to another, no fitted parameter is renamed as a prediction, and no load-bearing claim rests solely on a self-citation. Score 0.

Assumptions & free parameters 2 free parameters · 4 assumptions · 0 invented entities

The central catalog and R'HK values rest on domain assumptions about instrument stability and model fidelity, but no physical constants are invented and no new entities are postulated. The only tunable choices, the NZP smoothing window and the six-star envelope fit, are processing or descriptive parameters rather than free parameters fitted to the claimed result.

free parameters (2)
  • NZP 50-day moving average smoothing window = 50 days (adopted from TO19)
    The 50-day window for the nightly zero-point model is a smoothing timescale adopted from TO19, not refit here; it affects the corrected RVs but not the raw catalog.
  • Lower-envelope RV std versus vsini linear fit = Not quoted in text (slope and intercept shown in Figure 6)
    A descriptive linear fit to six selected stars outlining the lower envelope of RV scatter versus rotational velocity; it is illustrative, not used for prediction, and does not affect the catalog.
assumptions (4)
  • domain assumption PHOENIX synthetic spectra provide an accurate photospheric flux model in the Ca II H and K passbands after rectification.
    Invoked in Section 2.4; any mismatch between model and star propagates directly into the R'HK values, especially for stars with uncertain Teff, logg, or [M/H].
  • domain assumption The iodine absorption cell provides a stable, decade-long wavelength and PSF reference.
    Section 2.2; the relative RV accuracy and the long-term zero-point stability of the catalog rest on the iodine cell being unchanged since 1996.
  • domain assumption The RV-quiet star definition (more than five measurements and RV std below 10 m/s) supports the NZP correction.
    Section 2.3; the nightly zero-point correction assumes these stars are dynamically quiet and that their RV scatter reflects instrumental systematics.
  • domain assumption Gaia DR3 and TESS Input Catalog stellar parameters are sufficiently accurate for selecting PHOENIX templates.
    Section 2.1; template mismatch biases both the absolute RVs from CCF and the R'HK photospheric subtraction.

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Cite this review

Pith. "Pith review of An updated catalog of HIRES/Keck radial velocity measurements. Including Ca II H&K measurements." pith.science (2026). https://pith.science/paper/BFGNHERW

@misc{pith2026250906072,
  author       = {Pith},
  title        = {Pith review of: An updated catalog of HIRES/Keck radial velocity measurements. Including Ca II H&K measurements},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/BFGNHERW}},
  note         = {Machine review of arXiv:2509.06072}
}
abstract

The first HIRES/Keck precision radial velocity (RV) catalog was released in 2017; it was followed by a second release in 2019, which incorporated corrections for small but significant systematic errors. The manifestation of stellar activity accompanied by systematic errors could affect the detection of exoplanets via the RV method. We expanded the HIRES catalog to March 2023 using publicly available spectra. Furthermore, we included the chromospheric emission line Ca II H&K indicator ($R_{\mathrm{HK}}^\prime$), which is among the most prominent tracers of stellar activity. The precision RVs were obtained using an iodine gas absorption cell and corrected for minor systematic errors. $R_{\mathrm{HK}}^\prime$ measurements were derived by rectifying the observed spectra with PHOENIX synthetic spectra models in six narrow bands surrounding the H and K lines, then subtracting the photospheric contribution. We present an updated HIRES/Keck precision RV catalog featuring 78,920 RV measurements for 1,702 stars. High-quality $R_{\mathrm{HK}}^\prime$ measurements are provided for ~ 40% of the HIRES catalog. The updated catalog can help distinguish stellar activity effects from planetary signals in RV time series, thereby corroborating previously detected planetary candidates and aiding in the detection of new ones.

Figures

Figures reproduced from arXiv: 2509.06072 by the authors.

Figure 1
Figure 1. Distribution of HIRES target stars (black) compared to that of Gaia DR3 stars (red). Perdelwitz et al. (2021) introduced a method for directly measur￾ing the relative chromospheric flux in the H&K lines, rectifying spectra using PHOENIX stellar atmospheres and synthetic spec￾tra (Husser et al. 2013) and narrow passbands centered around the emission line cores. We used this method to derive R ′ HK for the entire publ… view at source ↗
Figure 2
Figure 2. Distribution of the overall stellar parameters for the entire catalog: Teff (left), log g (center), and [M/H] (right). This emphasizes the need for caution when interpreting vari￾ability in poorly sampled stars. Beyond about 7 RV measure￾ments, the lower envelope of the distribution (i.e., the minimum RVstd across NRV) represents the external HIRES noise floor of ∼ 2 m s−1 . The bottom panel of [PITH_FULL_IMAGE:fig… view at source ↗
Figure 3
Figure 3. Representation of RV measurements color-coded by RV-quiet threshold criteria: quiet in red and non-quiet in blue. Top: Standard de￾viation of the (NZP-corrected) RVs as a function of the number of RV observations (NRV ). Bottom: Ratio between the median RV uncertainty and the standard deviation of the corrected RVs, providing a measure of how well the RV precision accounts for the observed scatter. 2.3. Systematic v… view at source ↗
Figures from the paper (4 more)
Figure 4
Figure 4. Figure 4: Systematic variability of the HIRES instrument. Individual RVs of RV-quiet stars are denoted in cyan, and nightly weighted average RVs (NZPs) in black. NZPs enclosed in red boxes represent those derived from fewer than three RV measurements, while the green line indica…
Figure 5
Figure 5. Figure 5: Distribution of the ∆ log L difference of fitting the HIRES RV data of 71 stars known to host a single massive planet with a Keplerian model. We repeated the fit twice, once with the original (uncorrected) RVs and once with the corrected RVs, and calculated the differe…
Figure 7
Figure 7. Figure 7: GBP − GRP vs. the median of log(R ′ HK) per star, with logarithmic surface gravity represented as a color map for the clean sample. Only R ′ HK measurements that are > 3σ away from 0 are included. 3.2. R ′ HK and color index In [PITH_FULL_IMAGE:figures/full_fig_p007_7.png]
Figure 8
Figure 8. Figure 8: Example of the R ′ HK time series (black dots in the upper panel) and the corresponding GLS power spectrum (red line in the lower panel), for HD 7924, HD 219134, and HD 156668. Prominent periodicities in the R ′ HK data appear as peaks in the GLS plot. The 1% and 0.1% …

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