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COUNTESS I: A Uniformly Vetted Catalog of Known and New Transiting Exoplanets in the TESS Northern Continuous Viewing Zone

T0 review · reviewed 2026-08-04 · deepseek-v4-flash

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Pith's one-line read A multi-cadence TESS pipeline recovers 72% of known northern-CVZ TOIs and delivers 10 new planet candidates, including two statistically validated sub-Neptunes.

arxiv 2606.13789 v2 pith:UTSHVEEU submitted 2026-06-11 astro-ph.EP astro-ph.IMastro-ph.SR

Andrew Hotnisky , Rachel B. Fernandes , Kevin K. Hardegree-Ullman , Steven Giacalone , Kiersten M. Boley , Kristo Ment , Michelle Kunimoto , Galen J. Bergsten
show 4 more authors
Sakhee Bhure Jessie L. Christiansen Brandon Radzom Suvrath Mahadevan
This is my paper
classification astro-ph.EPastro-ph.IMastro-ph.SR
keywords tessdayscountessoplusplanetsstarstexttransiting
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 TESS satellite stares at most of the sky for only about 27 days at a time, so standard searches mostly find planets with orbits shorter than ~10 days. But near the north and south ecliptic poles — the Continuous Viewing Zones — overlapping observations give stretches of months to years of coverage. COUNTESS combines those long light curves, even though the data arrive at two different cadences (30-minute images in the primary mission, 10-minute in the first extended mission), by binning the faster data down to 30 minutes.

The pipeline detrends the stitched light curves with a 'biweight' filter, searches for repeating transit dips with a fast-folding Box Least Squares code called GERBLS, fits transit shapes with EXOTIC, removes false alarms with the LEOVetter suite, and finally runs surviving signals through triceratops, which computes the probability that a signal is a false positive versus a real planet.

On 26,114 stars with TESS-SPOC light curves, COUNTESS recovered 115 of 159 previously known planet signals (72%) and found 38 new transit signals, 10 of which survived all vetting. Two — TIC 219893931b and TIC 237254473b — have false-positive probabilities below 1.5% and are designated statistically validated sub-Neptunes. Caveats: one of those two was already reported as a community candidate in 2023, the pipeline's planet radii come out systematically smaller than published values, and the 'likely planet' list uses a looser nearby false-positive threshold (10^-1) than the one stated in the methods (10^-3).

Extended reading notes

Core claim

The central load-bearing assertion is that COUNTESS 'recovers 115 out of 159 known TESS Objects of Interest' and that its blind search produced '10 new exoplanet candidates... including two new statistically validated sub-Neptunes, TIC 219893931b and TIC 237254473b' (Abstract; §4.2–4.4). If the paper is correct, the pipeline genuinely stitches heterogeneous-cadence CVZ light curves into a sensitive long-baseline search, the 72% recovery rate reflects real performance, and the two 'b' designations are statistically validated planets (with the caveat that TIC 219893931b was previously reported by Montalto 2023).

Load-bearing premise

The step-function detrending window w(P) = 0.5 days for P ≤ 100 days and 1.75 days for P > 100 days (§3.2, 'our window length w as a function of period P is...'). Every transit depth — and hence every recovered planet radius and the sub-Neptune classifications — passes through this filter, and the 100-day boundary was chosen by hand to maximize recovery of the known TOI sample (the same sample later used to report the 72% recovery). The paper itself demonstrates that the 0.5-day window removes part of the transit depth for long-duration transits (Figure 10). The re-processing at 1.75 days only triggers after the first-pass search has returned P > 100 days, so any long-duration signal that the short window over-detrends in the first pass is lost before the longer window is applied. If the window function is wrong for some period/duration range, the candidate list — and the completeness the pipeline needs for its stated demographic goal — is biased in a way the paper does not quantify (n

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Editorial analysis

A structured set of objections, weighed in public.

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

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

No new physical entities are introduced (no new particles, forces, or dimensions); COUNTESS is a software pipeline. The central claims rest on 5 tuned processing parameters and 5 domain assumptions, mostly inherited from the Kepler/K2/TESS toolchain rather than independently validated here. The most consequential choices are the detrending window function and the NFPP threshold inconsistency.

free parameters (5)
  • Detrending window function w(P) = 0.5 d for P ≤ 100 d; 1.75 d for P > 100 d
    Chosen in §3.2 by maximizing known-TOI recovery; the 100-day breakpoint is a hand-set boundary, and the paper shows the 0.5-d window over-detrends long transits (Figure 10).
  • Minimum transit count = 3 transits
    COUNTESS requires ≥3 transits for candidate status (§4.1); this hard cut excludes part of the long-period regime the pipeline is designed to explore and caused misses like TOI-4600.02 (P=482.8 d, only two clear transits).
  • GERBLS BLS SNR threshold = S/N ≥ 6 (MES ≥ 6.2)
    Adopted from prior TESS surveys (§3.3); sets which TCEs proceed to fitting; 29 of 46 missed TOIs failed at this stage.
  • triceratops NFPP threshold = 10^-3 stated (§3.5, §5 bullet); 10^-1 applied for 8 candidates (§4.3)
    Inconsistent application: the two 'b' planets meet 10^-3, but the '10 likely planet candidates' list uses NFPP < 10^-1.
  • EM1 cadence binning = 10-min → 30-min
    Choice to homogenize cadence (§3.1); removes sensitivity to short-duration transits, acknowledged in the text.
assumptions (5)
  • domain assumption TESS-SPOC PDC-SAP FFI light curves are adequately corrected for instrumental systematics
    Used as input without independent verification (§3.1); the Skye excess metric (§3.1.1) shows residual systematics in sectors 14, 16-19, 22 that required masking.
  • domain assumption Stellar radius/mass derivation (color-Teff relation, random-forest [Fe/H]/log g on LAMOST, MIST isochrones, Mann/Torres relations) is accurate
    Planet radii scale linearly with R_star; the method is borrowed from Hardegree-Ullman et al. 2025 (§2.2) and its errors propagate directly into the candidate sizes.
  • domain assumption triceratops FPP/NFPP correctly represent the false-positive probability given the modeled scenarios
    Validation rests on this external tool (§3.5); its scenario list is assumed complete, and the paper uses the median of 20 runs without independent checks.
  • domain assumption RUWE < 1.4 plus Gaia non-single-star flag = 0 isolates single stars
    Used to build the target sample (§2.1); unresolved multiples can mimic or dilute transits, and the cut is imperfect.
  • standard math Standard transit-search statistical machinery (BLS significance, MES thresholds, Kepler vetting thresholds) is valid without recalibration for CVZ data
    LEOVetter thresholds in Table 3 are adopted wholesale from Kepler/K2 literature (§3.5) and applied to multi-sector stitched TESS light curves.

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Pith. "Pith review of COUNTESS I: A Uniformly Vetted Catalog of Known and New Transiting Exoplanets in the TESS Northern Continuous Viewing Zone." pith.science (2026). https://pith.science/paper/UTSHVEEU

@misc{pith2026260613789,
  author       = {Pith},
  title        = {Pith review of: COUNTESS I: A Uniformly Vetted Catalog of Known and New Transiting Exoplanets in the TESS Northern Continuous Viewing Zone},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/UTSHVEEU}},
  note         = {Machine review of arXiv:2606.13789}
}
abstract

The Transiting Exoplanet Survey Satellite (TESS) has transformed the study of nearby exoplanetary systems; however, its nominal observing strategy limits sensitivity to planets with orbital periods shorter than $\sim$10 days for most parts of the sky. The two TESS Continuous Viewing Zones (CVZs) provide extended temporal baselines that help overcome this limitation, enabling the detection of longer-period ($>$10 days) transiting planets around nearby stars. Here, we present COUNTESS, a transit-search pipeline optimized for long-baseline TESS observations that combines multi-sector light curves with heterogeneous cadences, and implements fast-folding BLS period detection, vetting, and statistical validation. As a first application of the pipeline, we conducted a search on the primary and first extended mission photometry in the TESS northern CVZ. For this analysis, we used Gaia DR3 and 2MASS photometry to homogeneously derive a stellar catalog of FGKM stars for the TESS northern CVZ, resulting in a sample of 391,059 stars. We used COUNTESS to search for transiting planets around 26,114 of these stars with TESS-SPOC light curves and assessed its performance, recovering 115 out of 159 known TESS Objects of Interest (TOIs; $0.85\ \text{days} < P <124.72\ \text{days}$; $1.03\ R_\oplus < R_p < 16.35\ R_\oplus$). Additionally, we identified 10 new exoplanet candidates ($1.20\ \text{days} < P <34.62\ \text{days}$; $1.73\ R_\oplus < R_p < 4.19\ R_\oplus$) that passed vetting tests, including two new statistically validated sub-Neptunes, TIC 219893931b and TIC 237254473b. COUNTESS enables extended-baseline TESS analyses and identification of longer-period planets, establishing a foundation for future exoplanet demographic studies, including comparisons with Kepler and K2.

Figures

Figures reproduced from arXiv: 2606.13789 by the authors.

Figure 1
Figure 1. H-R diagram of the TESS northern CVZ stellar sample. The colors on the diagram indicate the number den￾sity of stars in our sample. 3. COUNTESS We focused on the TESS northern CVZ, combining PM and EM1 FFI data, which provide longer baselines but heterogeneous cadences (PM: 30-minute; EM1: 10- minute) and differing noise properties. To address these challenges, we developed COUNTESS a unified end-to￾end workflow opt… view at source ↗
Figure 2
Figure 2. The schematic flow chart of how a target is processed through COUNTESS. derived planetary radius for long-period signals while maintaining recovery of shorter-period signals. 3.3. GERBLS Period Search We searched the detrended light curves for periodic, transit-like signals using the Greatly Expedited Ro￾bust Box Least Squares (GERBLS; Ment et al. submit￾ted)6 code. Like a traditional Box-Least Squares (BLS), GERBLS… view at source ↗
Figure 3
Figure 3. A sector-by-sector detrending of TIC 441765914 (TOI-2088). The top panel of each sector shows the raw flux (black) from the TESS-SPOC FFIs with a detrending curve (orange). The bottom panel shows the detrended light curve. The transits computed from the ExoFOP epoch and from the period recovered by COUNTESS are displayed as vertical bars in green (ExoFOP) and blue (COUNTESS) [PITH_FULL_IMAGE:figures/full_fig_p007_3.png] view at source ↗
Figures from the paper (7 more)
Figure 4
Figure 4. Figure 4: The upper panel shows a phase-folded light curve of TOI-2088 b, with the best-fit model in red from EXOTIC. The lower panel shows the residuals in %. ter estimates consistent with those obtained from the other fitting methods. We passed the phase, flux, period, transit…
Figure 5
Figure 5. Figure 5: The comparison plots of recovered TOIs for the ExoFOP measured orbital periods compared to the COUNTESS discovered periods. FOP10 (J. L. Christiansen et al. 2025), to train and test the planet recovery, vetting, and statistical validation modules of COUNTESS. Of these …
Figure 6
Figure 6. Figure 6: The comparison plot of recovered TOIs for the ExoFOP measured planet radii compared to the COUNTESS discovered planet radii. Note that the planetary parameters from ExoFOP are not homogeneously determined, resulting in expected scatter in the radius fit. but also ident…
Figure 7
Figure 7. Figure 7 [PITH_FULL_IMAGE:figures/full_fig_p013_7.png]
Figure 8
Figure 8. Figure 8: The distribution of planetary radius and orbital period of TOIs and new false positives and planet candidates. COUNTESS discovered 38 new planetary signals, with 28 of them being FPs through triceratops validation and LEOVetter pixel-vetting. Note that the square symbo…
Figure 9
Figure 9. Figure 9: shows the Skye Excess Metric (SEM) for all flagged sectors in our blind search, which we outlined in Section 3.1.1. All timestamps above the corresponding sector’s 3σ threshold were removed from the overall search. 1685 1690 1695 1700 1705 1710 TJD (days) 100 200 300 #…
Figure 10
Figure 10. Figure 10: shows the comparison between using a short window length (w = 0.5 days) versus a longer window length (w = 1.75 days) to detrend a light curve with a transit that has a long duration. If we use a window length where w ∼ tdur, the detrending will remove a portion of th…

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