Gaia DR3 Variable White Dwarfs vetted by ZTF

Ashish Mahabal; Krzysztof Nienartowicz; Laurent Eyer; Lorenzo Rimoldini; Marc Audard; Panagiotis Gavras; Pedro Garcia-Lario; Thinh Nguyen; Timour Jestin

arxiv: 2509.15133 · v2 · submitted 2025-09-18 · 🌌 astro-ph.SR

Gaia DR3 Variable White Dwarfs vetted by ZTF

Timour Jestin , Thinh Nguyen , Laurent Eyer , Lorenzo Rimoldini , Ashish Mahabal , Marc Audard , Pedro Garcia-Lario , Panagiotis Gavras

show 1 more author

Krzysztof Nienartowicz

This is my paper

Pith reviewed 2026-05-18 15:41 UTC · model grok-4.3

classification 🌌 astro-ph.SR

keywords variable white dwarfsGaia DR3ZTFZZ CetiGW VirV777 Herwhite dwarf binariesstellar pulsations

0 comments

The pith

Gaia DR3 astrometric and photometric criteria combined with ZTF time series yield 1423 variable white dwarf candidates, 141 of them periodic.

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

The paper applies selection rules based on Gaia DR3 astrometry and photometry to isolate white dwarfs likely to vary. It then cross-matches the resulting list against ZTF DR23 light curves and runs a multiband Lomb-Scargle search to measure periods. Significant periodicity appears in 141 stars, which the authors group with the OPTICS algorithm into classes such as ZZ Ceti, GW Vir, V777 Her, and white-dwarf plus main-sequence binaries. The work also flags 519 additional sources as new variable candidates, 83 of them newly periodic. A reader would care because these objects let astronomers test models of white-dwarf cooling, pulsation, and binary evolution with a larger and cleaner sample than before.

Core claim

The authors define a Gaia DR3 sample of 1423 candidate variable white dwarfs using astrometric and photometric quantities, cross-match 864 of them with ZTF DR23 time series, and apply multiband Lomb-Scargle periodograms to detect significant periodicity in 141 objects. OPTICS clustering then classifies the periodic stars, recovering three ZZ Ceti, 15 GW Vir, one V777 Her, and 24 white-dwarf–main-sequence binaries while adding 519 newly identified candidates overall, of which 83 are new periodic detections.

What carries the argument

Gaia DR3 astrometric-plus-photometric selection criteria for variability, followed by multiband Lomb-Scargle periodogram analysis on ZTF light curves and OPTICS clustering to group and label the periodic detections.

Load-bearing premise

The Gaia DR3 astrometric and photometric cuts pick out mostly genuine variable white dwarfs rather than contaminants, and the periods found by Lomb-Scargle on ZTF data reflect real stellar changes instead of sampling artifacts.

What would settle it

High-cadence follow-up photometry or spectroscopy on a random subset of the 723 non-periodic candidates that shows no intrinsic variability at the amplitudes expected for white-dwarf pulsators or binaries would indicate that the initial Gaia selection contains substantial contamination.

Figures

Figures reproduced from arXiv: 2509.15133 by Ashish Mahabal, Krzysztof Nienartowicz, Laurent Eyer, Lorenzo Rimoldini, Marc Audard, Panagiotis Gavras, Pedro Garcia-Lario, Thinh Nguyen, Timour Jestin.

**Figure 1.** Figure 1: These histograms display the number of observed epochs in each band for each survey. We randomly choose 3000 white [PITH_FULL_IMAGE:figures/full_fig_p003_1.png] view at source ↗

**Figure 2.** Figure 2: We compare the error of the mean magnitude [PITH_FULL_IMAGE:figures/full_fig_p003_2.png] view at source ↗

**Figure 3.** Figure 3: The estimated standard deviation of the G-band per CCD time series, see Equation (1), plotted as a function of the mean magnitude G¯. To select the variable white dwarf candidates, we use a threshold that is 25% higher than the computed noise function. In this selection, 1423 white dwarfs are variable candidates according to Gaia DR3 data. 0.4 0.0 0.4 0.8 1.2 BP-RP colour [mag] 8 10 12 14 Absolute G-magni… view at source ↗

**Figure 4.** Figure 4: HR diagram of our selection of variable white dwarf can [PITH_FULL_IMAGE:figures/full_fig_p004_4.png] view at source ↗

**Figure 6.** Figure 6: The distribution of the Euclidean distance - as calcu [PITH_FULL_IMAGE:figures/full_fig_p005_6.png] view at source ↗

**Figure 5.** Figure 5: Inconsistent cross-matches of the ZTF query are detected [PITH_FULL_IMAGE:figures/full_fig_p005_5.png] view at source ↗

**Figure 7.** Figure 7: We illustrate the step-by-step reduction of a raw ZTF DR23 light curve (of Gaia DR3 2833849800205759360) into a phase [PITH_FULL_IMAGE:figures/full_fig_p006_7.png] view at source ↗

**Figure 8.** Figure 8: Position of the determined periodic stars in the HR diagram, with the colour and size of the dots representing respectively [PITH_FULL_IMAGE:figures/full_fig_p007_8.png] view at source ↗

**Figure 9.** Figure 9: Position in the HR diagram of the three clusters identified [PITH_FULL_IMAGE:figures/full_fig_p007_9.png] view at source ↗

read the original abstract

The publications of Gaia DR2 and DR3 have brought major improvements in stellar astrometry and photometry, particularly regarding the description of the white dwarf sequence. Notably, Gaia DR2 enabled the detection of variability in white dwarfs based solely on averaged astrometric and photometric quantities, i.e. the astrometric 5 parameters (positions, proper motion, and parallax) and general photometry properties in the G, BP and RP bands (mean, standard deviation and number of measurements). We identify and classify variable white dwarfs using Gaia DR3 data and Zwicky Transient Facility DR23 observations. The objective is to construct a catalogue of pulsating white dwarf candidates with robust selection criteria. We define a new sample of candidate variable white dwarfs using Gaia DR3 astrometric and photometric data. We cross-match this sample with the ZTF DR23 catalogue and apply a multiband Lomb-Scargle periodogram analysis to detect periodic variability. We then use the OPTICS unsupervised clustering algorithm to to group and classify the confirmed periodic stars. We identify 1423 variable white dwarfs candidates from Gaia DR3, with 864 having ZTF time series. 141 present significant periodicity. We classify these objects into known categories, including ZZ Ceti stars, GW Vir, V777 Her, and white dwarf-main sequence binaries. Our analysis yields several periodic stars, including three ZZ Ceti, 15 GW Vir, one V777 Her, and 24 WD-MS binaries. Furthermore, it reveals a significant population of potentialy variable stars, though without confirmed periodicity. Finally we publish our catalogue of candidate variable white dwarfs including variability status, periodicity, and classification information for the 864 sources with ZTF time series, 519 of them newly identified (including 83 new periodic stars).

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.

Desk Editor's Note private letter to a colleague

The paper adds a practical new catalog of 1423 variable white dwarf candidates from Gaia DR3 cross-matched to ZTF, with 83 new periodic stars and some type classifications, but the periodicity work needs tighter alias and validation checks.

read the letter

The main takeaway is that the paper delivers an expanded catalog of variable white dwarf candidates from a Gaia DR3 selection cross-matched to ZTF DR23 data. It reports 1423 candidates total, 864 with ZTF coverage, 141 showing significant periodicity, and 519 new identifications including 83 new periodic stars, along with classifications for some into ZZ Ceti, GW Vir, V777 Her, and WD-MS binaries. The work applies established variability search methods like multiband Lomb-Scargle periodograms and OPTICS clustering to this new cross-match. This produces a practical catalog that includes variability status, periodicity information, and classifications for the sources with time series data. The approach is straightforward and builds directly on prior Gaia-based selections for white dwarf variability. One area that needs attention is the treatment of the periodic detections. ZTF's observing cadence introduces strong aliases around one cycle per day, and the paper does not provide details on the exact significance thresholds, alias rejection procedures, or any validation tests such as comparing frequencies across bands or running injection recoveries. If a portion of the 141 periodic signals turn out to be sampling artifacts, the numbers of new periodic stars and the specific type classifications would need revision. This is a moderate limitation rather than a core flaw, given that the overall pipeline is logical. The paper is most useful for astronomers studying white dwarf populations, pulsations, or binary systems who can benefit from a larger list of candidates. It is an incremental contribution that adds to existing samples without introducing new theoretical insights or major methodological changes. It engages clearly with the relevant literature on known variable white dwarf classes and uses reproducible public data and algorithms. I would consider bringing it to a reading group to discuss the data cross-matching and clustering steps. I would not cite the specific results in my work without additional validation, but the paper is solid enough to warrant peer review. Recommendation: Send it for review, focusing referee attention on the periodicity validation and false positive assessment.

Referee Report

1 major / 2 minor

Summary. The paper claims to construct a catalog of variable white dwarf candidates by applying Gaia DR3 astrometric and photometric selection criteria to identify 1423 candidates, cross-matching 864 with ZTF DR23 time series, performing multiband Lomb-Scargle periodogram analysis to detect significant periodicity in 141 sources, applying OPTICS clustering for classification into types including 3 ZZ Ceti, 15 GW Vir, 1 V777 Her, and 24 WD-MS binaries, and releasing a catalog for the 864 sources that includes 519 newly identified candidates of which 83 are newly periodic.

Significance. If the periodicity detections hold after validation, the work would provide a useful public catalog expanding the sample of known variable white dwarfs and periodic pulsators from combined Gaia and ZTF data. Strengths include the direct use of public survey data, standard algorithms (Lomb-Scargle and OPTICS), and the release of the catalog with variability status and classifications, which supports reproducibility and follow-up studies.

major comments (1)

[Abstract / Periodogram analysis] Abstract and methods description of the multiband Lomb-Scargle analysis: no quantitative false-alarm probability threshold, no explicit alias-rejection procedure (e.g., comparison to the spectral window function or requirement that the same frequency dominates independently in g and r), and no injection-recovery tests on the actual ZTF observing cadence are described. Given ZTF's strong nightly sampling aliases near 1 d^{-1} and harmonics, this leaves open the possibility that a non-negligible fraction of the 141 'significant periodicity' detections (and thus the 83 new periodic stars) are artifacts rather than intrinsic variability. This directly affects the reliability of the central counts and classifications.

minor comments (2)

[Abstract] Abstract contains two clear typos: 'to to group' and 'potentialy variable'.
[Methods] The exact numerical thresholds applied for the Gaia DR3 variability selection (astrometric and photometric) and the Lomb-Scargle significance cut are not stated, making it difficult to reproduce the initial 1423-candidate sample.

Simulated Author's Rebuttal

1 responses · 0 unresolved

We thank the referee for their constructive and detailed review of our manuscript. Their comments on the periodogram analysis are well taken, and we address them point by point below. We will revise the manuscript accordingly to improve the description of our methods and strengthen the reliability assessment of the reported periodicities.

read point-by-point responses

Referee: [Abstract / Periodogram analysis] Abstract and methods description of the multiband Lomb-Scargle analysis: no quantitative false-alarm probability threshold, no explicit alias-rejection procedure (e.g., comparison to the spectral window function or requirement that the same frequency dominates independently in g and r), and no injection-recovery tests on the actual ZTF observing cadence are described. Given ZTF's strong nightly sampling aliases near 1 d^{-1} and harmonics, this leaves open the possibility that a non-negligible fraction of the 141 'significant periodicity' detections (and thus the 83 new periodic stars) are artifacts rather than intrinsic variability. This directly affects the reliability of the central counts and classifications.

Authors: We agree that the methods section requires a more quantitative and explicit description of the periodicity detection criteria. In the revised manuscript we will add the specific false-alarm probability threshold adopted for the multiband Lomb-Scargle periodograms (currently described only qualitatively as 'significant'). We will also make explicit our alias-rejection approach, which includes requiring that the dominant frequency be consistent between the independent g- and r-band periodograms; this step was performed but not detailed in the original text. Regarding injection-recovery tests on the actual ZTF cadence, such tests were not carried out in the submitted version. We acknowledge that they would provide a more complete validation of the detection efficiency and false-positive rate. We will either perform a representative set of injection tests or, if resource constraints prevent a full suite, add a quantitative discussion of the expected impact of nightly aliases on the 141 detections. These additions will directly address the referee's concern about the reliability of the 83 newly identified periodic stars. revision: yes

Circularity Check

0 steps flagged

No circularity; derivation applies standard algorithms to public survey data

full rationale

The paper selects 1423 variable white dwarf candidates from Gaia DR3 astrometric and photometric quantities, cross-matches 864 with ZTF DR23, runs multiband Lomb-Scargle periodograms to identify 141 periodic sources, and applies the standard OPTICS algorithm for classification into ZZ Ceti, GW Vir, etc. No equations, fitted parameters, or self-citations reduce the reported counts, periodicity detections, or classifications to quantities defined by the authors' own prior results or by construction. All steps are direct applications of external catalogs and established, non-author-specific methods.

Axiom & Free-Parameter Ledger

3 free parameters · 2 axioms · 0 invented entities

The analysis rests on standard astronomical data-processing assumptions and domain knowledge of white-dwarf variability classes. Thresholds for candidate selection and periodicity significance are chosen by the authors but are not the central claim itself. No new physical entities are postulated.

free parameters (3)

Gaia variability selection thresholds
Cutoffs on astrometric and photometric indicators that define the initial 1423-candidate sample.
Lomb-Scargle significance threshold
Cutoff used to declare 141 stars as having significant periodicity.
OPTICS clustering parameters
Settings that assign stars to categories such as ZZ Ceti or GW Vir.

axioms (2)

standard math Lomb-Scargle periodogram reliably extracts periodic signals from unevenly sampled, multi-band photometric time series under standard noise assumptions.
Invoked for the multiband analysis of ZTF DR23 data.
domain assumption White dwarfs exhibiting periodic variability belong to established observational classes (ZZ Ceti, GW Vir, V777 Her, WD-MS binaries) whose period ranges are known.
Used to classify the 141 periodic objects.

pith-pipeline@v0.9.0 · 5888 in / 1632 out tokens · 62245 ms · 2026-05-18T15:41:03.438379+00:00 · methodology

discussion (0)

Lean theorems connected to this paper

Citations machine-checked in the Pith Canon. Every link opens the source theorem in the public Lean library.

IndisputableMonolith/Cost/FunctionalEquation.lean washburn_uniqueness_aczel unclear

?

unclear
Relation between the paper passage and the cited Recognition theorem.

We then analyze our cleaned time series with Generalised Lomb-Scargle periodograms ... FAP_Zg resp. Zr (f) < 10^{-3} ... LS(f) > 0.1 ... OPTICS unsupervised clustering algorithm ... parameters: absolute G magnitude, BP-RP colour, log10 frequency, and log10 amplitude ratio
IndisputableMonolith/Foundation/DimensionForcing.lean alexander_duality_circle_linking unclear

?

unclear
Relation between the paper passage and the cited Recognition theorem.

We identify 1423 variable white dwarfs candidates from Gaia DR3, with 864 having ZTF time series. 141 present significant periodicity.

What do these tags mean?

matches: The paper's claim is directly supported by a theorem in the formal canon.
supports: The theorem supports part of the paper's argument, but the paper may add assumptions or extra steps.
extends: The paper goes beyond the formal theorem; the theorem is a base layer rather than the whole result.
uses: The paper appears to rely on the theorem as machinery.
contradicts: The paper's claim conflicts with a theorem or certificate in the canon.
unclear: Pith found a possible connection, but the passage is too broad, indirect, or ambiguous to say the theorem truly supports the claim.

Reference graph

Works this paper leans on

25 extracted references · 25 canonical work pages · 1 internal anchor

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work page internal anchor Pith review Pith/arXiv arXiv 2017

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E., et al

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