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The Hot Neptune Initiative (HONEI) II. TOI-5795 b: A hot super-Neptune orbiting a metal-poor star

T0 review · 0 major / 6 minor · reviewed 2026-08-06 · deepseek-v4-flash

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Pith's one-line read TOI-5795 b is a confirmed hot super-Neptune: a 23.66-Earth-mass, 5.62-Earth-radius planet on a 6.14-day, near-circular orbit at the edge of the Neptune desert.

desk verdict A solid super-Neptune confirmation with honest analysis; the RV jitter is the only fragile premise and it holds up. read the letter →

arxiv 2507.23413 v1 pith:SV2NXXBF submitted 2025-07-31 astro-ph.EP

F. Manni , L. Naponiello , L. Mancini , S. Vissapragada , K. Biazzo , A. S. Bonomo , D. Polychroni , D. Turrini
show 26 more authors
D. Locci A. Maggio V. D Orazi M. Damasso C. Briceno D. R. Ciardi C. A. Clark K. A. Collins D. W. Latham N. Law M. Lopez-Morales M. B. Lund L. Malavolta A. W. Mann G. Mantovan D. Nardiello M. Pinamonti D. J. Radford R. P. Schwarz A. Shporer A. Sozzetti C. N. Watkins S. W. Yee C. Ziegler T. Zingales
This is my paper
classification astro-ph.EP
keywords planetarysystemstechniques:radialvelocitiesphotometrystars:individual:TOI-5795hotsuper-NeptuneNeptunedesertTESSatmosphericevaporation
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 confirms and characterizes TOI-5795 b, a planet discovered in TESS photometry around the metal-poor G3 star TOI-5795. Combining 19 HARPS radial-velocity measurements with three sectors of TESS light curves and two ground-based transits, the authors measure a planet mass of $M_p = 23.66^{+4.09}_{-4.60}\ M_\oplus$ and a radius of $R_p = 5.62 \pm 0.11\ R_\oplus$, placing it on a 6.14-day, near-circular orbit at the edge of the Neptune desert. The authors argue that the planet's low density and its host's low metallicity align it with the 'savanna' population rather than with the metal-rich hosts of desert planets, supporting a distinct formation origin. Their pebble-accretion simulations almost never reproduce this planet, and their atmospheric-evolution models indicate it lost 4–9 $M_\oplus$, roughly 14–27% of its initial mass, to photoevaporation while contracting from an initial radius near 10.5–11.2 $R_\oplus$. A well-characterized object like this is a test case for how close-in Neptunes form and evolve.

What carries the argument

The argument is carried by the joint photometry+radial-velocity model, which fits the TESS and ground-based transit light curves together with the 19 HARPS velocities using a nested-sampling Bayesian approach; the HARPS data supply a Keplerian semi-amplitude of $K = 8.97^{+1.51}_{-1.74}$ m s$^{-1}$, from which the planet's mass follows. High-angular-resolution SOAR speckle and Palomar adaptive-optics imaging, reaching contrasts of roughly 3.9 and 7.5 magnitudes within 0.5 arcseconds, exclude contaminating companions that could dilute the transit. Two modeling tools interpret the result: the GroMiT Monte Carlo code, a pebble-accretion growth-and-migration simulator whose synthetic populations only rarely land on the observed mass and orbit, and an atmospheric-evolution code that uses the ATES mass-loss rates, driven by stellar XUV evolutionary tracks, to reconstruct the planet's earlier, larger state.

What would settle it

A new radial-velocity campaign of roughly 30 additional HARPS measurements spread over at least one full year would settle the mass. If a statistically significant periodicity or trend remains after fitting the single Keplerian, and removing it shifts the best-fit semi-amplitude by more than about $1.5$ m s$^{-1}$, the quoted mass and its claimed significance would need revision.

Watch

Extended reading notes

Core claim

TOI-5795 b is a genuine hot super-Neptune: a transiting planet with $M_p = 23.66^{+4.09}_{-4.60}\ M_\oplus$, $R_p = 5.62 \pm 0.11\ R_\oplus$, bulk density $0.73 \pm 0.13$ g cm$^{-3}$, and equilibrium temperature $1136 \pm 18$ K, orbiting a $10.2^{+2.5}_{-3.3}$-Gyr-old, metal-poor ($[\mathrm{Fe/H}] = -0.27 \pm 0.07$) G3 V star every $6.1406325 \pm 0.0000054$ days on an orbit compatible with circular. The detection rests on a joint fit of TESS and ground-based photometry with HARPS radial velocities, and high-angular-resolution speckle and adaptive-optics imaging excludes blended eclipsing binaries as the source of the signal. The paper further claims that standard pebble-accretion formation models fail to produce this planet (one match in $4 \times 10^5$ simulations under the native disk, and one more across alternative disk configurations), and that its atmosphere has been stripped and compressed over roughly 10 Gyr, with an inferred mass loss of 4–9 $M_\oplus$ and a contraction from radii near 10.5–11.2 $R_\oplus$ at 10 Myr to its current size. With a transmission spectroscopy metric near 100, the authors present it as a promising target for atmospheric follow-up.

Load-bearing premise

That the scatter left over after subtracting the planet's signal from the 19 radial-velocity measurements is genuine white noise, so the fitted jitter of $3.75$ m s$^{-1}$ does not conceal a second signal that would change the measured mass.

Editorial extensions

If this is right

  • TOI-5795 b joins the small sample of well-characterized planets at the desert–savanna boundary; if the measured mass and radius hold, it becomes one of the few benchmarks for testing that boundary's physical origin.
  • The planet's low density and the host's low metallicity reinforce the demographic case that savanna Neptunes are not stripped gas giants, since the top-down pathway predicts metal-rich hosts.
  • The near-total failure of the pebble-accretion simulations implies that close-in super-Neptunes around 20–30 $M_\oplus$ require either a different accretion mode, a more efficient migration channel, or a stochastic dynamical origin such as mergers or high-eccentricity tidal migration.
  • With a transmission spectroscopy metric near 100 and a bright host, the planet is a viable target for atmospheric spectroscopy; measuring its atmospheric metallicity would test whether the envelope is primordial or was accreted after a dynamical rearrangement.

Reading between the lines

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

  • Editorial: The elevated radial-velocity jitter ($3.75$ m s$^{-1}$, roughly 40% of the planet's semi-amplitude) is itself a clue; an outer companion revealed by a longer baseline would supply the natural trigger for the dynamical scattering the authors invoke.
  • Editorial: The evaporation models imply that at 10 Myr the planet had a radius near 10.5–11.2 $R_\oplus$ and a mass of about 28–33 $M_\oplus$; a survey of young clusters might catch such inflated progenitors and test this mass-loss history directly.
  • Editorial: Because the host is metal-poor and roughly 10 Gyr old, this system cleanly separates the two main desert-shaping mechanisms (photoevaporation versus top-down stripping); the planet's survival at 1136 K favors evaporation-and-migration models over primordial gas-giant stripping.
  • Editorial: Re-running the same planetary seeds with a high-eccentricity migration prescription added to the GroMiT pebble-accretion tracks, rather than smooth inward migration, is a direct computational test of the authors' post-formation-shaping hypothesis.
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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

0 major / 6 minor

Summary. The paper reports the confirmation and characterization of the transiting super-Neptune TOI-5795 b. Using 12 TESS transits from three sectors, two ground-based transits, and 19 HARPS radial velocities, the authors derive an orbital period of 6.1406 d, a mass of 23.66 M⊕, a radius of 5.62 R⊕, and a bulk density of 0.73 g cm^-3, orbiting a metal-poor G3 V star. High-resolution speckle and AO imaging exclude significant blends. The planet lies at the edge of the Neptune desert / beginning of the savanna in the period-radius diagram. The paper also presents Monte Carlo pebble-accretion formation simulations, which fail to reproduce the planet's mass and orbit in the vast majority of trials, and an atmospheric-evolution study suggesting that the planet has lost 4-9 M⊕ of its initial atmosphere.

Significance. If the characterization holds, TOI-5795 b is a valuable addition to the small sample of well-characterized hot super-Neptunes at the Neptune desert/savanna boundary. The precise mass and radius (both at the roughly 5-10% level) and the metal-poor host star make it an important test case for formation and evolution models. The paper's strengths include the multi-dataset joint analysis, explicit exclusion of blends with high-angular-resolution imaging, injection-recovery simulations for the RV detection sensitivity, and the use of independent formation simulations that yield a genuine negative result for pebble accretion. The atmospheric-evolution analysis is clearly hedged against the large uncertainty in the star's high-energy history. The TSM of ~100 also makes this a promising target for future atmospheric follow-up.

minor comments (6)
  1. [Table 2] The value log gp = 7.33±1.29 cgs in Table 2 is inconsistent with the quoted Mp = 23.66 M⊕ and Rp = 5.62 R⊕, which imply log gp ≈ 2.87 cgs; please correct this typographical error.
  2. [Sect. 4.2] The text reports 'e = 0.15±0.06' and states that the eccentricity is compatible with zero at 95.5% confidence, while Table 2 gives a 2σ upper limit of e < 0.25; these statements should be reconciled, for example by quoting the median and 68% credible interval together with the upper limit and noting that the posterior is non-Gaussian.
  3. [Abstract and Sect. 7] The abstract describes TOI-5795 b as 'at the edge of the Neptune desert', but the paper adopts the Castro-González et al. (2024a) definitions in which the desert is P_orb < 3.2 d, the ridge is 3.2–5.7 d, and the savanna is 5.7–100 d; with P_orb = 6.14 d the planet is actually at the beginning of the savanna, so the wording should be aligned.
  4. [Table 1] The column 'δ(J2010)' should read 'δ(J2000)'.
  5. [Sect. 2.4.1] The TRES RVs are described as having an average precision of 27.7 m/s, but the listed values show a scatter of about ±50 m/s; reporting the RMS of the TRES RVs would help the reader gauge the sensitivity to long-period companions.
  6. [Sect. 4.2] Given that the fitted jitter (3.75 m/s) is a sizable fraction of the RV semi-amplitude (8.97 m/s), it would be informative to state explicitly the resulting detection significance of the Keplerian signal after the jitter is included, beyond the >5σ claim, and to note whether a model with a correlated noise component changes the inferred mass.

Circularity Check

0 steps flagged · score 1.0 of 10

No circular derivation: the planet's mass and radius are measured quantities from an independent joint RV/photometry fit, and the formation and evaporation analyses are forward models with literature-based inputs.

full rationale

The central claims (orbital period, mass, radius) come from a joint fit of TESS photometry, ground-based transit photometry, and 19 HARPS radial velocities (Sect. 4.2, Table 2); no claimed quantity is used to calibrate the model that produces it. The Keplerian semi-amplitude and transit depth are independent observables, and the quoted uncertainties already include the fitted HARPS jitter, which the authors explicitly flag as elevated and recommend monitoring. The formation analysis (Sect. 5) is a forward pebble-accretion simulation whose disk parameters are drawn from literature surveys (disk mass 1–10% of Mstar, R0 = 40/90 au, pebble sizes, viscosity ranges) and then compared to the observed planet; the low match rate (only 1–14 synthetic objects in 3 sigma) is a genuine negative result, not a refit. The atmospheric evolution analysis (Sect. 6) is a forward calculation anchored to measured stellar parameters and literature XUV evolution tracks; it back-propagates the current mass and radius to infer initial conditions, which is model-dependent extrapolation rather than a circular prediction. The paper's self-references (Naponiello et al. 2022, 2023, 2025a; Mantovan et al. 2024b; Polychroni et al. 2023) are methodological citations and do not carry the key inference. A typographical inconsistency in Table 2 (log gp = 7.33 cgs versus the roughly 2.87 cgs implied by the quoted Mp and Rp) is an internal error, not evidence of circularity. Overall, no load-bearing circular step is present.

Assumptions & free parameters 2 free parameters · 5 assumptions · 0 invented entities

The planet confirmation itself uses only standard transit and RV nuisance parameters plus domain assumptions about the star and the single-planet interpretation. The secondary formation and atmospheric-evolution sections introduce additional hand-chosen disk parameters and model assumptions that do not affect the central mass and radius result.

free parameters (2)
  • HARPS RV jitter = 3.75 +1.23/-1.08 m/s
    Fitted in the joint RV model to absorb unmodeled noise; its large value contributes to the mass uncertainty and is the most important nuisance parameter.
  • GP hyperparameters for TESS photometry = sigma_GP = 0.00160 ± 0.00014, rho_GP = 0.98 ± 0.09
    Fitted to red noise in the photometric model; they do not drive the transit depth but affect the reported uncertainties.
assumptions (5)
  • domain assumption The transit and RV signals are produced by the same planet, not by a blended eclipsing binary.
    The confirmation rests on matching the 6.14-day period in both photometry and RVs; high-resolution imaging and the absence of activity-correlated signals support this, but it is an interpretive step rather than an independent proof.
  • domain assumption The stellar parameters from SED fitting with EXOFASTv2 and MIST isochrones are accurate within the quoted uncertainties.
    Planet radius, equilibrium temperature, and the planet's mass depend on stellar radius and luminosity; errors in stellar parameters propagate directly to the planet.
  • domain assumption Earth-like core composition (rock and iron) for TOI-5795 b's interior.
    Used in Section 6 to split the measured mass and radius into a core (16.5 M_Earth, 2 R_Earth) and an atmospheric fraction of about 30%; a different interior composition would change the inferred mass-loss and initial mass.
  • domain assumption The disk fully dissipated at 10 Myr, setting the initial condition for backward atmospheric evolution.
    Section 6 assumes the planet reached its final orbit at 10 Myr; changing this epoch alters the time-integrated irradiation and the estimated initial mass.
  • domain assumption The adopted XUV luminosity evolutionary tracks bracket the star's past high-energy output.
    No X-ray detection exists; the tracks rely on activity-rotation-age relations, and the three scenarios give a wide range of mass loss, so the specific mass-loss numbers are model-dependent.

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Cite this review

Pith. "Pith review of The Hot Neptune Initiative (HONEI) II. TOI-5795 b: A hot super-Neptune orbiting a metal-poor star." pith.science (2026). https://pith.science/paper/SV2NXXBF

@misc{pith2026250723413,
  author       = {Pith},
  title        = {Pith review of: The Hot Neptune Initiative (HONEI) II. TOI-5795 b: A hot super-Neptune orbiting a metal-poor star},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/SV2NXXBF}},
  note         = {Machine review of arXiv:2507.23413}
}
abstract

The formation of Neptune planets with orbital periods less than 10\,days remains uncertain. They might have developed similarly to longer-period counterparts, emerged from rare collisions between smaller planets, or could be the remnant cores of stripped giant planets. Characterizing a large number of them is important to advance our understanding of how they form and evolve. We aimed at confirming the planetary nature and characterizing the properties of a close-in Neptune-type transiting exoplanet candidate revealed by TESS around the star TOI-5795 (V = 10.7 mag), 162 pc away from the Sun. We monitored TOI-5795 with the HARPS spectrograph for two months to quantify periodic variations in radial velocity (RV) to estimate the mass of the smaller companion. We combined these RV and TESS photometry. High-angular-resolution speckle and adaptive optics imaging excluded contamination from nearby sources. We found that the parent star is a metal-poor (${\rm [Fe/H]}=-0.27\pm0.07$), G3\,V star ($T_{\rm eff}=5718\pm50$\,K), with $R_{\star}=1.082\pm0.026\,R_{\sun}$, $M_{\star}=0.901^{+0.055}_{-0.037}\,M_{\sun}$ and $10.2^{+2.5}_{-3.3}$\,Gyr. We estimated that the planet has an orbital period of $P_{\rm orb}=6.1406325 \pm 0.0000054$ days and an orbital eccentricity compatible with zero. Having a mass of $23.66^{+4.09}_{-4.60}\,M_{\oplus}$, a radius of $5.62\pm 0.11\,R_{\oplus}$ and an equilibrium temperature of $1136\pm18$\,K, it can be considered as a hot super-Neptune at the edge of the Neptune desert. We simulated planet-formation processes but found almost no successful matches to the observed planet's mass and orbit, suggesting that post-formation dynamical events may have shaped its current state.

Figures

Figures reproduced from arXiv: 2507.23413 by the authors.

Figure 1
Figure 1. The light curve of TOI-5795 obtained by TESS by monitoring the Sectors 54 (top panel), 81 (middle panel), and Sector 92 (bottom panel) with a 2-min cadence, as extracted by the SAP pipeline. No sig￾nificant rotational modulation can be appreciated. The black line repre￾sents our best-fit transit model, while the white points are binned data. The residuals of the best-fit model are shown in parts per million in both … view at source ↗
Figure 2
Figure 2. High-resolution sensitivity curves. Final sensitivity of SOAR (top panel) and Palomar Hale (bottom panel), plotted as a function of angular separation from the host star. Insets in the respective panels dis￾play images of the central region of the data. derived RVs have an average precision of 27.7 m s−1 (see Ta￾ble A.1), consistent with no detectable RV variation due to the TESS planet candidate or other external l… view at source ↗
Figure 3
Figure 3. Stellar spectral energy distribution (SED). The broad band mea￾surements from the Tycho, APASS Johnson and Sloan, 2MASS and WISE magnitudes are shown in red, and the corresponding theoretical values with blue circles. The non-averaged best-fit model is displayed with a black solid line [PITH_FULL_IMAGE:figures/full_fig_p005_3.png] view at source ↗
Figures from the paper (10 more)
Figure 4
Figure 4. Figure 4: GLS periodogram of TOI-5795 HARPS RVs, with the main peak correctly identified at ∼ 6 days. 2009), using the Python package astropy v.5.2.2 (Astropy Col￾laboration et al. 2018). The orbital period of the planet candidate TOI 5795.01 was clearly identified as the highes…
Figure 5
Figure 5. Figure 5: Top panel: HARPS RV measurements of TOI-5795 in blue and the preferred model fit in black. Bottom panel: RV residuals over the model fit. pinoza et al. 2019), which makes use of batman5 (Kreidberg 2015) and RadVel6 (Fulton et al. 2018), for the modelling of transit and…
Figure 7
Figure 7. Figure 7: Global fit result for TESS and the ground-based observations. The superimposed points correspond to phase-bins of 22 minutes, 18 minutes, and 17 minutes for TESS, LCO and Brierfield, respectively. The error bars include both the data uncertainty and the jitter derived …
Figure 8
Figure 8. Figure 8: Radius-period diagram of close-in exoplanets with mass and radius known with an accuracy of at least 5σ. The data were col￾lected from the NASA Exoplanet Archive on 13/02/2025. The error bars have been suppressed for clarity. The position of TOI-5795 b is high￾lighted …
Figure 9
Figure 9. Figure 9: Synthetic population of 4×105 exoplanets generated by a plau￾sible native protoplanetary disk of TOI-5795 b. The synthetic planets are plotted in the final semi-major axis versus planet mass plane. The color-scale traces the initial formation region of the planetary se…
Figure 10
Figure 10. Figure 10: Synthetic populations of 7.9×105 exoplanets generated sam￾pling different initial circumstellar disk configurations (disk mass: 1, 5, 10% of the stellar mass; R0: 40 and 90 au; pebble size: cm, mm and sub-mm). Planet TOI-5795 b and its 3σ uncertainty range are shown i…
Figure 12
Figure 12. Figure 12 [PITH_FULL_IMAGE:figures/full_fig_p009_12.png]
Figure 13
Figure 13. Figure 13: Temporal evolution of mass, radius, and mass-loss rate of TOI-5795 b. The left panel shows the evolution of planetary mass, the middle panel the evolution of the radius, and the right panel the evolution of the mass-loss rate. The colors refers to the different high e…
Figure 14
Figure 14. Figure 14: ). The characteristics of the TOI-5795 planetary system sup￾port the idea that planets in the savanna are unlikely to have formed through the top-down mechanism and likely have a dis￾tinct origin and evolution history compared to the hottest Nep￾tunes in the desert. I…
Figure 15
Figure 15. Figure 15: Frequency distribution of parent-star metallicity for transiting exoplanets with 10 M⊕<Mp<100 M⊕ (Vissapragada & Behmard 2025). The histograms are shown with a 0.1 bin and for the three different pop￾ulations pointed out by Castro-González et al. (2024a). “Desert” ref…

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    " write newline "" before.all 'output.state := FUNCTION n.dashify 't := "" t empty not t #1 #1 substring "-" = t #1 #2 substring "--" = not "--" * t #2 global.max substring 't := t #1 #1 substring "-" = "-" * t #2 global.max substring 't := while if t #1 #1 substring * t #2 gl...

Pith tools

Reviewed August 6, 2026 · model on record in the stance chip above.