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HD 35843: A Sun-like star hosting a long period sub-Neptune and inner super-Earth

T0 review · 4 major / 5 minor · reviewed 2026-08-16 · deepseek-v4-flash

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Pith's one-line read HD 35843 hosts two planets: a transiting 46.96-day sub-Neptune and a non-transiting 9.90-day super-Earth.

desk verdict HD 35843 c is a solid, well-characterized long-period sub-Neptune; HD 35843 b is plausible but the paper's exclusion of PFS RVs leaves the inner planet less certain than advertised. read the letter →

arxiv 2505.00898 v1 pith:2WVRGP7G submitted 2025-05-01 astro-ph.EP

Katharine Hesse , Ismael Mireles , François Bouchy , Diana Dragomir , Solène Ulmer-Moll , Nora L. Eisner , Keivan G. Stassun , Samuel N. Quinn
show 47 more authors
Hugh P. Osborn Sergio G. Sousa Cristilyn N. Watkins Karen A. Collins Edward M. Bryant Jonathan M. Irwin Coel Hellier Marshall C. Johnson Carl Ziegler Steve B. Howell David R. Anderson Daniel Bayliss Allyson Bieryla César Briceño R. Paul Butler David Charbonneau Ryan Cloutier Jeffrey Crane Jason Dittmann Jason D. Eastman Sebastián A. Freigeiro Benjamin J. Fulton Samuel Gill Maximilian Günther Haedam Im Jon M. Jenkins Michelle Kunimoto Baptiste Lavie Monika Lendl Michael B. Lund Andrew W. Mann Belinda Nicholson David Osip Martin Paegert Nuno C. Santos Richard P. Schwarz Sara Seager Stephen Shectman Johanna Teske Joseph D. Twicken Stéphane Udry Vincent Van Eylen José Vinés López Sharon X. Wang Peter J. Wheatley Joshua N. Winn Edward E. Zuidema
This is my paper · ORCID
classification astro-ph.EP
keywords exoplanetssub-Neptunesuper-EarthtransitphotometryradialvelocitiesTESSplanetvalidationatmosphericcharacterization
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 sets out to establish that the metal-poor Sun-like star HD 35843 hosts two planets: a temperate transiting sub-Neptune on a 46.96-day orbit and an inner, non-transiting super-Earth-mass planet on a 9.90-day orbit. A joint analysis of TESS photometry and high-precision radial velocities gives the outer planet a radius of $2.54\,R_\oplus$, a mass of $11.32\,M_\oplus$, and a slightly eccentric orbit, while the inner signal has a minimum mass of $5.84\,M_\oplus$. If correct, the system joins the small sample of well-characterized long-period, temperate sub-Neptunes bright enough for atmospheric follow-up, and it provides a rare architecture in which the inner planet does not transit.

What carries the argument

The central object is a two-planet Keplerian model constrained by the transits of planet c and the Doppler wobble of both planets. The load-bearing technique is a joint nested-sampling fit of the TESS light curve with the ESPRESSO radial velocities, supported by a Lomb-Scargle periodogram and a stacked periodogram that show the 9.9-day signal grows stronger as more data are added and does not correlate with stellar activity indicators. False-positive scenarios for the transiting planet are excluded with ground-based photometry, high-resolution imaging, and a statistical validator that returns a false-positive probability of about $0.05\%$.

What would settle it

A decisive test is to add more ESPRESSO radial velocities over a longer baseline and include the independent radial-velocity data in a single joint fit: if the 9.9-day signal does not stay phase-coherent with one well-determined period near 9.90 days, or if its amplitude tracks the bisector or line-width activity indicators, then planet b is not established.

Watch

Extended reading notes

Core claim

The paper reports the discovery and confirmation of two planets around HD 35843 (TOI 4189), a metal-poor G dwarf. The outer planet, HD 35843 c, transits with period $P=46.9622$ d, radius $R=2.54\,R_\oplus$, mass $M=11.32\,M_\oplus$, and eccentricity $e=0.153$; the inner planet, HD 35843 b, is detected only in radial velocities with period $P=9.8991$ d and minimum mass $M\sin i=5.84\,M_\oplus$. The outer planet's bulk density of $3.80$ g/cm$^3$ places it in the degenerate region between a rocky planet with a substantial hydrogen envelope and a water world, and its equilibrium temperature of about $480$ K makes it one of the coolest sub-Neptunes found by TESS.

Load-bearing premise

The load-bearing premise is that the 9.9-day radial-velocity wobble assigned to HD 35843 b comes from an orbiting planet rather than from stellar activity or an alias of the observing window; the paper's own analysis leaves a residual ~27-day peak with false-alarm probability 0.02, and adding independent radial-velocity data makes the period of planet b bimodal, so this is the premise that would collapse the two-planet claim.

Editorial extensions

If this is right

  • HD 35843 c joins the small set of long-period ($P>40$ d) transiting sub-Neptunes with a well-measured mass orbiting a bright host star, making it a high-value target for atmospheric characterization.
  • The measured density of $3.80$ g/cm$^3$ means the planet's composition is ambiguous between a rocky world with a hydrogen envelope and a water world; only atmospheric spectra can break that degeneracy.
  • If planet b truly does not transit, HD 35843 becomes one of only six known systems with a non-transiting inner planet and a transiting outer sub-Neptune, an architecture that may preserve a record of past dynamical instability.
  • Upcoming TESS re-observations in Sectors 87 and 95 can test whether b transits and can check the apparent transit-timing variations of c.

Reading between the lines

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

  • The bimodal period for planet b that appears when the independent radial-velocity data are included is a warning sign; if future data do not sharpen the 9.9-day period into a single coherent solution, the inner planet could turn out to be activity or an alias, leaving HD 35843 as a one-planet system.
  • If the apparent transit-timing variations in the ground-based partial transits are real, they imply a third body in the system; full transits from Sectors 87 and 95 could confirm this and constrain the perturber's mass.
  • A rocky, non-transiting b with $M\sin i\approx5.8\,M_\oplus$ would put the system on both sides of the radius valley, offering a single-star test bed for how super-Earths and sub-Neptunes form in the same disk.
  • The host's low metallicity suggests that temperate sub-Neptunes can form around metal-poor stars; a targeted search for such planets around other metal-poor FGK stars would test how common this population is.
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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

4 major / 5 minor

Summary. The paper reports the discovery and characterization of two planets around the metal-poor Sun-like star HD 35843 (TOI 4189). The outer planet, HD 35843 c, is a transiting sub-Neptune with P = 46.9622 d, R = 2.54 R⊕, M = 11.32 M⊕, and e = 0.15, validated through TESS photometry, ground-based follow-up, speckle imaging, and ESPRESSO radial velocities, with a triceratops false-positive probability of 0.05%. The inner planet, HD 35843 b, is inferred from ESPRESSO RVs with P = 9.90 d and a minimum mass of 5.84 M⊕, and is not observed to transit. The authors combine TESS and ESPRESSO data in a joint allesfitter fit, explore model scenarios with BIC/AIC, check activity indicators, and discuss composition and atmospheric prospects.

Significance. If both planets are real, the system is valuable: HD 35843 c is a bright (V = 9.4), temperate sub-Neptune with a precise mass and radius, adding to the sparse population of long-period transiting sub-Neptunes with well-measured masses. The validation of planet c is thorough and community-oriented, and the TSM and equilibrium temperature make it a plausible JWST target. Planet b, if confirmed, would make the system one of only a few with a non-transiting inner planet interior to a transiting sub-Neptune, with implications for system architecture and formation. The analysis is generally careful, with explicit activity checks, injection-recovery tests, and an appendix with the alternative fit including PFS. The main weakness is the security of planet b, whose detection rests on a single instrument and the post-hoc exclusion of an independent dataset.

major comments (4)
  1. [Section 3.4, Appendix D] The exclusion of the PFS radial velocities from the final joint fit is a load-bearing step for the 9.9-day planet b claim. The text states that PFS data are excluded because they 'result in a bimodal posterior for the period of planet b'; Appendix D shows that the joint fit with PFS still yields a bimodal Pb posterior (printed median 9.935 d over a 9.75-10.05 d prior, with two modes). Since PFS is an independent 18-epoch dataset with ~1 m/s precision, the bimodality indicates that the 9.9-day period is not uniquely determined when a second, independent dataset is included. Please provide a periodogram and a joint model of the ESPRESSO and PFS RVs (with and without an activity component), and discuss whether the 9.9-day signal is an alias or is genuinely present in both datasets. The current treatment amounts to removing the dataset that challenges the claimed period, and that is not sufficient support for the discovery claim.
  2. [Section 3.1.1, Section 3.3.1, Section 3.4] A ~25-27 d stellar activity signal is detected in the bisector span (25.49 d, FAP 1e-8) and remains in the RV residuals at 26.95 d with FAP 0.02 after subtracting both planets, yet the RV fits model only white noise (jitter) plus the two Keplerian signals. The 9.9-day signal has K = 1.81 ± 0.25 m/s, only a few times the expected activity-induced RV amplitude for a slowly rotating G star. To secure the planetary interpretation of the 9.9-day signal, the authors should perform a joint fit that includes a quasi-periodic Gaussian-process activity model (or at least a sinusoid at the adopted rotation period) and show that the 9.9-day Keplerian remains stable in period, amplitude, and significance. The checks against activity indicators are useful but do not rule out a non-sinusoidal or harmonic activity signal that could project onto the 9.9-day period.
  3. [Section 3.3.1, Table 2] The model comparison in Table 2 prefers the two-planet flat model over the two-planet linear-trend model by ΔBIC = 2.55 but by only ΔAIC = 0.94, which is marginal evidence against a linear trend; the text states the preference is 'nearly indistinguishable' between the flat and linear two-planet models. This is not itself a problem, but the derived parameter tables and discussion should note that the trend is not strongly constrained and that omitting a trend could slightly bias Kb or Kc. A sentence in Section 3.3.1 or Section 3.4 would suffice.
  4. [Section 4] The discussion states a minimum mass for HD 35843 b of 5.47 ± 0.82 M⊕, which is inconsistent with the abstract, Table 4, and Section 5 (5.84 ± 0.84 M⊕). Because this is the only reported parameter for planet b that appears in multiple places, the inconsistency should be corrected before publication.
minor comments (5)
  1. [Figure 3 caption] The caption says 'Ground-based photometry of HD 35843 b', but the transits shown belong to HD 35843 c; the figure and text refer to the 46.96-day transiting planet. Please correct the caption.
  2. [Abstract] The phrase 'among the coolest ~5% of planets discovered by TESS' lacks a quantitative definition or citation; please specify the comparison sample (e.g., TESS confirmed planets with measured radii) and provide the percentile calculation.
  3. [Section 3.4, Table 3] The inner planet's eccentricity is fixed to zero in the global fit (√eb cosωb = √eb sinωb = 0), but a test with a free eccentricity for planet b is not reported. Given the low Kb, an eccentric solution could affect the period and mass; please report such a test or justify why circularity is a safe assumption.
  4. [Section 3.2] The triceratops FPP is quoted as 0.05 ± 0.01 %, but the sentence immediately before states an NFPP of (2.7 ± 0.7) × 10−8 and then says 'We calculate an FPP of 0.05 ± 0.01 %'. It would be clearer to define FPP and NFPP in the text, since the former is the more standard validation metric.
  5. [Table A1] The PFS RVs are listed as relative velocities with an arbitrary zero point; because the final fit excludes them, the table would benefit from a note stating the zero-point convention and whether the absolute velocities were adjusted to a common barycentric frame.

Circularity Check

0 steps flagged · score 1.0 of 10

No significant circularity; planet parameters are measured from independent TESS photometry and ESPRESSO RVs, and self-citations are contextual corrections, not load-bearing.

full rationale

This is an observational discovery paper, and its central claims are fits to independent data rather than conclusions forced by the model inputs. HD 35843 c is validated with triceratops (FPP 0.05±0.01%) using TESS, ground-based photometry, speckle imaging, and reconnaissance spectra; its orbital period and radius come from TESS transits, while its mass comes from ESPRESSO RVs fitted jointly with the transits. HD 35843 b is detected as a ~9.9 d GLS peak in the ESPRESSO RVs after subtracting the 46.96 d signal; the two-planet model is preferred over one-planet models by ΔBIC≈30, activity-indicator periodograms show no 9.9 d peak, and residual RVs are not correlated with activity indices. These are standard, falsifiable data-analysis steps. The only self-citations are to Eisner et al. (2021), the Planet Hunters identification and the earlier SB2 misclassification; the paper expressly corrects the SB2 claim with CHIRON, NRES, CORALIE, PFS, and ESPRESSO spectra, so that citation is contextual rather than load-bearing. Disclosed limitations — exclusion of PFS RVs because they produce a bimodal Pb posterior (Section 3.4, Appendix D), a residual 26.95 d activity peak with FAP 0.02 (Section 3.1.1), and possibly unreal TTVs (Section 3.5) — are correctness/robustness concerns, not circularity. The ExoMDN composition inference is explicitly acknowledged to be degenerate and to require atmospheric observations. No equation or derived quantity is equivalent to an input by construction.

Assumptions & free parameters 9 free parameters · 5 assumptions · 0 invented entities

The central claim rests on standard exoplanet analysis assumptions: Keplerian orbits, the planetary interpretation of the RV signal, a single-star model, and a non-transiting circular inner planet. The fitted parameters are the usual orbital and noise parameters. No new physical entities are introduced.

free parameters (9)
  • Orbital period of planet b (Pb) = 9.8991 +0.0557/-0.0574 d
    Fitted to ESPRESSO RVs; a free parameter of the two-planet Keplerian model.
  • Orbital period of planet c (Pc) = 46.9622 ± 0.0002 d
    Fitted jointly to TESS transits and RVs.
  • RV semi-amplitude of planet b (Kb) = 1.81 ± 0.25 m/s
    Fitted to ESPRESSO RVs; determines minimum mass.
  • RV semi-amplitude of planet c (Kc) = 2.13 ± 0.24 m/s
    Fitted to ESPRESSO RVs; determines mass of c.
  • Eccentricity of planet c (ec) = 0.153 +0.070/-0.064
    Fitted via sqrt(e) cos ω and sqrt(e) sin ω.
  • Radius ratio Rc/R* = 0.02603 ± 0.00061
    Fitted to TESS transit depth.
  • cos i_c = 0.0074 +0.0016/-0.0030
    Fitted to transit shape; gives impact parameter.
  • RV jitter of ESPRESSO datasets = ln σ = -6.60 +0.10/-0.09 (km/s)
    Fitted per-instrument jitter; affects mass uncertainties.
  • TESS white noise scaling (ln σ_TESS) = -7.535 ± 0.015
    Fitted noise term for TESS photometry.
assumptions (5)
  • standard math Keplerian orbital motion: the RV signal of each planet is described by a Keplerian orbit, and the two planets do not interact significantly.
    Used in all RV fits (radvel, allesfitter); the TTV analysis is a separate check.
  • domain assumption The 9.9-day RV signal is generated by a planet, not by stellar activity or an instrumental window-function alias.
    Section 3.3.1: activity indicators show no correlation, but a ~27-day residual peak (FAP 0.02) remains.
  • ad hoc to paper Planet b is non-transiting and its orbit is circular.
    Section 3.4: eccentricity of b fixed to 0; non-transiting assumed from lack of TESS transits and the injection-recovery limit.
  • domain assumption The star is a single, slowly rotating G dwarf with the spectroscopically measured parameters (T_eff=5666 K, [Fe/H]=-0.27).
    Section 3.1: from ESPRESSO spectra, SED fit, and high-resolution imaging.
  • ad hoc to paper PFS radial velocities are excluded from the final joint fit.
    Section 3.4: including them yields a bimodal posterior for Pb; an alternative fit is shown in Appendix D.

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Cite this review

Pith. "Pith review of HD 35843: A Sun-like star hosting a long period sub-Neptune and inner super-Earth." pith.science (2026). https://pith.science/paper/2WVRGP7G

@misc{pith2026250500898,
  author       = {Pith},
  title        = {Pith review of: HD 35843: A Sun-like star hosting a long period sub-Neptune and inner super-Earth},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/2WVRGP7G}},
  note         = {Machine review of arXiv:2505.00898}
}
abstract

We report the discovery and confirmation of two planets orbiting the metal-poor Sun-like star, HD 35843 (TOI 4189). HD 35843 c is a temperate sub-Neptune transiting planet with an orbital period of 46.96 days that was first identified by Planet Hunters TESS. We combine data from TESS and follow-up observations to rule out false-positive scenarios and validate the planet. We then use ESPRESSO radial velocities to confirm the planetary nature and characterize the planet's mass and orbit. Further analysis of these RVs reveals the presence of an additional planet, HD 35843 b, with a period of 9.90 days and a minimum mass of $5.84\pm0.84$ $M_{\oplus}$. For HD 35843 c, a joint photometric and spectroscopic analysis yields a radius of $2.54 \pm 0.08 R_{\oplus}$, a mass of $11.32 \pm 1.60 M_{\oplus}$, and an orbital eccentricity of $e = 0.15\pm0.07$. With a bulk density of $3.80 \pm 0.70$ g/cm$^3$, the planet might be rocky with a substantial H$_2$ atmosphere or it might be a ``water world". With an equilibrium temperature of $\sim$480 K, HD 35843 c is among the coolest $\sim 5\%$ of planets discovered by TESS. Combined with the host star's relative brightness (V= 9.4), HD 35843 c is a promising target for atmospheric characterization that will probe this sparse population of temperate sub-Neptunes.

Figures

Figures reproduced from arXiv: 2505.00898 by the authors.

Figure 1
Figure 1. TESS target pixel files of HD 35843 (TIC 7422496) for all 5 sectors of observations made using tpfplotter Aller et al. (2020). The SPOC photometric aperture is highlighted in each panel. 4096 × 4096 SINISTRO camera having an image scale of 0. ′′389 per pixel, resulting in a 26′ × 26′ field of view and the images were calibrated by the standard LCOGT BANZAI pipeline (McCully et al. 2018), and differen￾tial photometri… view at source ↗
Figure 2
Figure 2. Top: Full TESS PDCSAP lightcurve of HD 35843. Transits of HD 35843 c are marked with dashed magenta lines. Bottom: Zoom-in of the 3 individual transits from Sectors 6, 32, and 33 along with the best-fit transit light curve. Further follow-up observations targeting better-placed transit windows were therefore scheduled. 2.2.3. Next Generation Transit Survey (NGTS) The Next Generation Transit Survey (NGTS; Wheat￾ley e… view at source ↗
Figure 3
Figure 3. Ground-based photometry of HD 35843 b from LCOGT, MEarth, and NGTS along with the best-fit transit light curve from the joint TESS+ESPRESSO fit in red. Blue curves account for the potential TTVs discussed in Section 3.5. with the custom NGTS filter (520 – 890 nm). The NGTS observations were reduced and the light curves were ex￾tracted using a custom aperture photometry pipeline using a photometric aperture with a ra… view at source ↗
Figures from the paper (14 more)
Figure 4
Figure 4. Figure 4 [PITH_FULL_IMAGE:figures/full_fig_p006_4.png]
Figure 5
Figure 5. Figure 5: ESPRESSO RVs for HD 35843 and best-fit RV curve for the 2-planet system. 0.0 0.2 0.4 0.6 0.8 1.0 1.2 angular separation (arcsec) 0 1 2 3 4 5 6 7 8 m 562 nm 832 nm TOI 4189 1" 562 nm 1" 832 nm 0.0 0.5 1.0 1.5 2.0 2.5 3.0 ¢arcsec 0 1 2 3 4 5 6 7 ¢ m a g nit u d e (I-b a …
Figure 6
Figure 6. Figure 6: Left: Gemini speckle imaging contrast curves of HD 35843 (TOI 4189), with insets showing the images for each filter. Right: High resolution speckle imaging and contrast curve from SOAR. lowing the same procedure as described in Sousa et al. (2021). The obtained value (…
Figure 7
Figure 7. Figure 7: Spectral energy distribution of TOI-4189. Red symbols represent the observed photometric measurements, where the horizontal bars represent the effective width of the passband. Blue symbols are the model fluxes from the best￾fit Kurucz atmosphere model (black). applied;…
Figure 8
Figure 8. Figure 8: Transit injection and recovery for the TESS light curve of HD 35843 made using matrix (D´evora-Pajares & Pozuelos 2022) showing that an additional transiting planet at a period shorter than 20 days or a radius larger than 1.5 R⊕ should have been detected if present. In…
Figure 9
Figure 9. Figure 9: Generalized Lomb-Scargle periodogram for the ESPRESSO RVs before (top) and after subtracting out the 46.96 day planet (middle) and both planets (bottom). The peak near 10 days becomes more significant after this sub￾traction. The peaks near 1 day and the past 100 days …
Figure 11
Figure 11. Figure 11: ESPRESSO residual RVs (46.96 d planet subtracted) vs various activity indicators showing no significant correla￾tions. The plots show the Pearson correlation coefficient and corresponding p-value [PITH_FULL_IMAGE:figures/full_fig_p013_11.png]
Figure 12
Figure 12. Figure 12: Top row: From left to right, we create stacked periodograms for 1) the full set of ESPRESSO RV points, 2) the ESPRESSO RV points with the 47 day signal removed, 3) the RV points with both the 47 day and 10 day signals removed. The color scale corresponds to logarithm …
Figure 13
Figure 13. Figure 13: Phase folded TESS transit data with the mod￾eled best-fit allesfitter light curve, and residuals plot on the bottom. In addition to the joint fit, we also ran a fit to deter￾mine if HD 35843 c exhibited any transit timing vari￾ations that might indicate the presence o…
Figure 14
Figure 14. Figure 14: Phase folded and offset-subtracted ESPRESSO RVs with the modeled best-fit allesfitter RV curve for HD 35843 b (left) and HD 35843 c (right), with residuals plotted on the bottom. Stellar jitter has been added in quadrature with measurement uncertainties. epoch and per…
Figure 15
Figure 15. Figure 15: Period-radius diagram of confirmed and vali￾dated sub-Neptunes as of this writing. Magenta diamonds denote long period (P > 40 days) planets with upper limits on their masses, masses from transit timing variations, or radial velocities masses that are loosely constrai…
Figure 16
Figure 16. Figure 16: Mass-radius diagram made using mr-plotter (Castro-Gonz´alez et al. 2023) of sub-Neptunes with mea￾sured masses as well as theoretical models from Zeng et al. (2019). Only planets with 5-σ mass and radius measure￾ments are shown for clarity. HD 35843 c lies in the over…
Figure 17
Figure 17. Figure 17: Left: Mass fractions for the core, mantle, water, and gas layers calculated using ExoMDN. Right: Radius fractions for the same layers. tial Photometric Precision (CDPP) of ∼150 ppm across the existing 5 sectors of TESS data. Using the period and ephemeris from the RVs…
Figure 18
Figure 18. Figure 18: Left:Eccentricity measurements of transiting sub-Neptune systems vs. orbital periods. Empty markers denote upper limits on eccentricity. HD 35843 c has the highest eccentricity of the 6 sub-Neptunes. Right: HD 35843 and the 5 other sub-Neptune systems with a non-trans…

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Pith tools

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