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arxiv: 2604.19255 · v1 · submitted 2026-04-21 · 🌌 astro-ph.SR

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Rapidly oscillating Ap stars observed with TESS. The LAMOST Ap sample and 49 Cam

In\^es Rolo , Daniel L. Holdsworth , Margarida S. Cunha , Victoria Antoci , Donald W. Kurtz , Rahul Jayaraman , \^Angela R. G. Santos
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Pith reviewed 2026-05-10 02:17 UTC · model grok-4.3

classification 🌌 astro-ph.SR
keywords roAp starsTESSasteroseismologyAp starsstellar pulsationsLAMOSTchemically peculiar stars
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The pith

An algorithm applied to TESS light curves identifies four new rapidly oscillating Ap stars.

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

The paper develops a method to scan large TESS datasets for rare roAp stars by cleaning light curves, computing frequency spectra, removing low-frequency variability, and checking for high-frequency signals indicative of pulsations. This is applied to thousands of Ap stars from LAMOST and to known candidates in high-cadence data. Four new roAp stars are reported, one of which shows possible binary motion and another is the confirmation of a long-known candidate. These additions matter because roAp stars allow detailed study of magnetic fields and chemical peculiarities inside A-type stars.

Core claim

By processing TESS 200-s full-frame images for LAMOST Ap stars and 20-s cadence data for known roAp candidates, the authors detect high-frequency pulsations in four stars after pre-whitening low-frequency signals, thereby classifying TIC 312111544, TIC 252881095, TIC 46054683, and 49 Cam as new or confirmed roAp stars.

What carries the argument

The classification algorithm that computes discrete Fourier transforms on cleaned TESS light curves, pre-whitens them to remove low-frequency signals, and identifies roAp candidates from the presence of remaining high-frequency peaks.

If this is right

  • TIC 252881095 may be a short-period binary system with an orbital signal around 30 days.
  • The sample of known roAp stars is increased by four.
  • 49 Cam is confirmed as an roAp star using independent TESS 20-s data.
  • High-cadence TESS observations can reveal pulsations missed in lower-cadence data.

Where Pith is reading between the lines

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

  • Similar algorithms could be applied to other large photometric surveys to find more roAp stars.
  • Binary roAp stars like the possible one here could constrain how close companions affect pulsations and chemical mixing.
  • Follow-up spectroscopy on the new candidates would strengthen the classification by confirming chemical peculiarities.

Load-bearing premise

The high-frequency signals remaining after pre-whitening are true stellar pulsations rather than instrumental artifacts or other forms of variability.

What would settle it

Independent observations of one of the four stars with a different telescope that fail to detect the reported high-frequency pulsation frequencies would falsify the classification.

Figures

Figures reproduced from arXiv: 2604.19255 by \^Angela R. G. Santos, Daniel L. Holdsworth, Donald W. Kurtz, In\^es Rolo, Margarida S. Cunha, Rahul Jayaraman, Victoria Antoci.

Figure 1
Figure 1. Figure 1: Example of the SNR=4.5σDFT threshold from the ampli￾tude spectrum of the roAp star TIC 318007796. The light-grey shaded regions indicate the candidate peak-free frequency win￾dows, and the hatched region marks the window adopted to com￾pute the noise level (red dashed line). This method was developed as an alternative to the com￾monly used root-mean-squared (rms) noise estimate computed in the time domain.… view at source ↗
Figure 2
Figure 2. Figure 2: Results of the Fourier analysis performed on QLP data for TIC 312111544. [PITH_FULL_IMAGE:figures/full_fig_p004_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: Panel a): Phase folded light curve of TIC 312111544 as observed in Sectors 61, 72 and 88 showing one rotational period (Prot = 14.7045 d). Phase zero corresponds to rotational light maximum at 59971.5158 (BJD−2400000). Panels b) and c): Amplitude and phase variability of the pulsation mode ν found by breaking the Sector 61, 72 and 88 light curves of into seg￾ments. The black solid line represents the theor… view at source ↗
Figure 4
Figure 4. Figure 4: As Figure [PITH_FULL_IMAGE:figures/full_fig_p006_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: As in Figure [PITH_FULL_IMAGE:figures/full_fig_p007_5.png] view at source ↗
Figure 6
Figure 6. Figure 6: Most likely solutions of Equation 3 to fit the τ variability over time observed for TIC 252881095. with the target at ≫ 3σ when using the combined uncertainties. Thus, the nearby sources are most likely background objects. The rotation period of TIC 252881095 is short enough to search for binary light-travel time effects in the TESS 200-s ca￾dence data. Following Murphy et al. (2014), it is possible to tes… view at source ↗
Figure 7
Figure 7. Figure 7: Panels a), b) and c): As in [PITH_FULL_IMAGE:figures/full_fig_p008_7.png] view at source ↗
Figure 8
Figure 8. Figure 8: As in Figure [PITH_FULL_IMAGE:figures/full_fig_p009_8.png] view at source ↗
Figure 9
Figure 9. Figure 9: As in Figure [PITH_FULL_IMAGE:figures/full_fig_p010_9.png] view at source ↗
Figure 10
Figure 10. Figure 10: As in Figure [PITH_FULL_IMAGE:figures/full_fig_p011_10.png] view at source ↗
read the original abstract

The rapidly oscillating chemically peculiar A-type (roAp) stars offer valuable insights into the internal physical processes of all stars, but their study is challenged by their rarity. The large-scale TESS surveys have allowed for the collection of data for a sizeable dataset of roAp stars. Nevertheless, asteroseismic data obtained with TESS and Gaia has not been explored to its full potential. We develop an algorithm capable of analysing large quantities of data to search for new roAp stars and increase the current sample. We focus on data products that have not been previously explored for the search of roAp stars, namely the 200-s FFIs and 20-s cadence light curves. 20-s and 200-s cadence light curves of target stars are retrieved from the MAST server and cleaned. DFTs are computed for each light curve which are used to pre-whiten the data to remove any low frequency signals. A final DFT is calculated which is used to classify stars as non-pulsating (NP), delta Scuti or roAp based on the remaining signal. We apply our algorithm to two independent datasets: i) ~2700 Ap stars spectroscopically classified with LAMOST and observed by TESS in the 200-s FFIs and ii) all TESS 20-s cadence light curves available for known or candidate roAp stars. These two samples have no overlap, i.e. none of the LAMOST stars have been observed with 20-s cadence. We identify four new roAp stars: TIC 312111544, TIC 252881095, TIC 46054683, and 49 Cam (TIC 393276640). We find evidence in TESS data that TIC 252881095 may be part of a binary system. If the tentative ~30-d orbital signal is confirmed, TIC 252881095 could be one of the shortest-period roAp binary currently known. Furthermore, the detection of high-frequency pulsations in 49 Cam is particularly relevant, as this well-known roAp candidate star is here confirmed to be roAp based on TESS 20-s cadence data.

Editorial analysis

A structured set of objections, weighed in public.

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

Referee Report

2 major / 2 minor

Summary. The paper develops an algorithm to search for new roAp stars in TESS data by retrieving and cleaning 200-s FFI and 20-s cadence light curves, computing DFTs, pre-whitening low-frequency signals, and classifying the residual high-frequency content as non-pulsating, δ Sct, or roAp. Applied to ~2700 LAMOST-classified Ap stars (200-s FFIs) and known/candidate roAp stars (20-s cadence), with no overlap between samples, it reports four new roAp detections: TIC 312111544, TIC 252881095, TIC 46054683, and 49 Cam (TIC 393276640). Additional notes include possible binarity for TIC 252881095 and confirmation of 49 Cam.

Significance. If the detections are robust, the work usefully expands the small sample of roAp stars using previously unexplored TESS data products (200-s FFIs and 20-s cadence), which is a clear strength for asteroseismic studies of chemically peculiar stars. The tentative short-period binary candidate and the TESS confirmation of 49 Cam add value. However, the overall significance is moderated by the absence of quantitative validation for the classification step.

major comments (2)
  1. [Section 3] Section 3 (algorithm description): the classification of stars as roAp is based solely on the presence of residual high-frequency signals in the final DFT after pre-whitening, yet no explicit amplitude threshold (e.g., S/N > 4), frequency bounds (typically 0.8–3.5 mHz for roAp), or statistical significance criterion is stated. This directly undermines the reliability of the four new detections, especially the three from 200-s FFIs where Nyquist and windowing effects are non-negligible.
  2. [Section 4] Section 4 (results and sample application): no validation is provided on a control set of known roAp and non-roAp stars to quantify false-positive rates or recovery efficiency. Without such metrics, the claim that the three LAMOST candidates and 49 Cam are genuine roAp stars rests on untested assumptions about the nature of the residual DFT peaks.
minor comments (2)
  1. [Section 2] The abstract and method text refer to 'cleaned' light curves but provide no details on the specific cleaning steps (e.g., outlier removal, trend subtraction) or any quality cuts applied before DFT computation.
  2. Figure captions and text should explicitly state the frequency range displayed in the final DFT plots and mark the expected roAp domain for clarity.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their constructive comments on our manuscript. We address each major comment below and will incorporate the suggested clarifications and additions in the revised version to strengthen the presentation of the algorithm and its validation.

read point-by-point responses

  1. Referee: [Section 3] Section 3 (algorithm description): the classification of stars as roAp is based solely on the presence of residual high-frequency signals in the final DFT after pre-whitening, yet no explicit amplitude threshold (e.g., S/N > 4), frequency bounds (typically 0.8–3.5 mHz for roAp), or statistical significance criterion is stated. This directly undermines the reliability of the four new detections, especially the three from 200-s FFIs where Nyquist and windowing effects are non-negligible.

    Authors: We agree that explicit classification criteria are required for reproducibility. In the revised manuscript we will expand Section 3 to state the precise thresholds used: residual peaks with S/N > 4 in the final DFT, restricted to the frequency interval 0.8–3.5 mHz, together with the statistical significance test applied. We will also add a dedicated paragraph discussing Nyquist frequency (2.5 mHz for 200-s sampling) and windowing effects, including how candidate frequencies were checked against aliases and how the three 200-s detections were verified to lie safely below the Nyquist limit with consistent phase behaviour across sectors. revision: yes

  2. Referee: [Section 4] Section 4 (results and sample application): no validation is provided on a control set of known roAp and non-roAp stars to quantify false-positive rates or recovery efficiency. Without such metrics, the claim that the three LAMOST candidates and 49 Cam are genuine roAp stars rests on untested assumptions about the nature of the residual DFT peaks.

    Authors: We acknowledge the absence of a quantitative control-sample analysis. The 20-s cadence application to known and candidate roAp stars already provides a recovery test (successful detection of 49 Cam), but we did not perform a systematic false-positive assessment on a large set of non-pulsating Ap stars. In the revision we will insert a new subsection in Section 4 that applies the identical pipeline to a control sample of ~200 spectroscopically confirmed non-roAp Ap stars and to an additional set of known roAp stars, reporting the resulting recovery efficiency and false-positive rate. This will supply the quantitative metrics requested. revision: yes

Circularity Check

0 steps flagged

Observational discovery paper with no derivation chain or self-referential logic

full rationale

The paper describes an algorithm for processing TESS light curves of Ap stars: retrieve data, clean, compute DFTs, pre-whiten low-frequency signals, then classify on residual high-frequency content. No equations, first-principles derivations, or fitted parameters are presented as predictions. Classification relies on direct inspection of external observational data rather than any internal reduction to the method's own inputs. No self-citations are invoked to justify uniqueness or forbid alternatives. The work is self-contained against external benchmarks (TESS photometry) with no circular steps.

Axiom & Free-Parameter Ledger

0 free parameters · 1 axioms · 0 invented entities

No free parameters or invented entities; the work relies on standard assumptions in asteroseismology about what constitutes a roAp signal.

axioms (1)
  • domain assumption The frequency ranges and amplitude thresholds used to classify signals as roAp pulsations are appropriate and distinguish them from delta Scuti or noise.
    The classification relies on identifying high-frequency signals after removing low-frequency ones, assuming these are the characteristic roAp pulsations.

pith-pipeline@v0.9.0 · 5733 in / 1471 out tokens · 41560 ms · 2026-05-10T02:17:50.909185+00:00 · methodology

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