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arxiv: 2606.04685 · v1 · pith:2OWZB7VCnew · submitted 2026-06-03 · 🌌 astro-ph.EP · astro-ph.SR

Upper limits on exosatellites around β Pictoris b

M.A. Kenworthy , R. Landman , A. Vanderburg , J.E. Rodriguez , J.L. Birkby , I. Macias , D. Gonz\'alez Picos , S.A. Jenkins
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E. Kleisioti T. Stolker I. Koutalios
This is my paper

Pith reviewed 2026-06-28 04:06 UTC · model grok-4.3

classification 🌌 astro-ph.EP astro-ph.SR
keywords exomoonsradial velocitybeta Pictoris bdirectly imaged exoplanetsexoplanet atmospheresCRIRES+
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The pith

No exomoon is detected around β Pictoris b, but radial velocity data set upper limits of 80 Earth masses at 1-day periods and 1 Jupiter mass at 200 days.

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

The paper measures the radial velocity of the directly imaged exoplanet β Pictoris b by cross-correlating a template spectrum with absorption lines in its atmosphere, reaching a mean precision of 160 m/s across epochs from October 2024 to March 2025. A periodogram analysis of these velocities finds no periodic signal from a possible exomoon. The non-detection is converted into mass upper limits that vary with orbital period. These limits are comparable to those obtained in other radial velocity searches for exomoons around substellar companions. Additional observing time with the same instrument is projected to reach lower masses, including a Neptune-mass moon at large separations.

Core claim

Although we do not detect an exomoon signal in our data, our detection limits for a single moon are 80 Earth masses at P=1 day and 1 Jupiter at P=200 days, comparable to RV exomoon searches around other substellar companions.

What carries the argument

Cross-correlation of a template spectrum with the planet's atmospheric absorption lines to extract radial velocities, followed by periodogram analysis to search for periodic signals from an exomoon.

If this is right

  • The radial velocity mass limits are comparable to the astrometric exomoon limit of 150 Earth masses at a 7-day period.
  • For periods longer than about 7 days the astrometric method provides tighter mass limits than the radial velocity data.
  • One additional observing season with CRIRES+ can reach a planet-to-moon mass ratio of 10^{-3}, or 4 Earth masses, at periods up to one day.
  • The same additional data can detect a Neptune-mass moon at orbital distances of hundreds of Jupiter radii.

Where Pith is reading between the lines

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

  • Tighter future limits could begin to test whether massive moons can form or be captured around young, directly imaged gas giants.
  • Joint radial velocity and astrometric monitoring may cover a wider range of orbital periods than either technique alone.
  • The achieved precision suggests that similar radial velocity campaigns on other directly imaged planets could yield comparable exomoon constraints.

Load-bearing premise

The scatter and sampling of the derived radial velocities are sufficient to turn a non-detection in the periodogram into quantitative mass upper limits as a function of period.

What would settle it

A future radial velocity measurement that reveals a periodic signal whose amplitude corresponds to a moon mass above the reported limits at a given period.

Figures

Figures reproduced from arXiv: 2606.04685 by A. Vanderburg, D. Gonz\'alez Picos, E. Kleisioti, I. Koutalios, I. Macias, J.E. Rodriguez, J.L. Birkby, M.A. Kenworthy, R. Landman, S.A. Jenkins, T. Stolker.

Figure 1
Figure 1. Figure 1: A section of the spectrum of 𝛽 Pictoris b from CRIRES+, showing one night of data and the fitted model. The template spectra of water and carbon monoxide are shown above, indicating their relative contributions. § lists for water (H2O; Polyansky et al. 2018) and carbon monoxide (CO; Rothman et al. 2010; Li et al. 2015). The atmospheric composi￾tion is parameterised using constant-with-altitude abundances, … view at source ↗
Figure 3
Figure 3. Figure 3: Radial velocity measurements of 𝛽 Pictoris b from CRIRES+ with the González Picos et al. (2024) formulation [PITH_FULL_IMAGE:figures/full_fig_p004_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: Results of the blind search for exosatellites in the RV time series listed in [PITH_FULL_IMAGE:figures/full_fig_p004_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: The upper limits on exosatellites around 𝛽 Pictoris b. The blue line represents the radial velocity limits for 50% retrieval of injected edge-on circular orbits. The red line is the outermost stable prograde orbit for an exosatellite around 𝛽 Pictoris b. The pale green line corresponds to astrometric limits from Macias et al. (2026). The Roche limits for rigid and fluid exosatellite bodies are shown in gra… view at source ↗
read the original abstract

$\beta$ Pictoris b is one of the closest known directly-imaged gas giant exoplanets with an orbit that is almost edge-on to our line of sight, making it an ideal target for radial velocity monitoring to search for massive exomoons. We measure the radial velocity of $\beta$ Pictoris b over several epochs between October 2024 and March 2025 by using the cross-correlation of a template spectrum with absorption lines in the planet's atmosphere, giving a mean precision of 160 m s$^{-1}$. The resultant set of radial velocities is analysed with a periodogram to search for candidate RV signals indicating a massive exomoon. Although we do not detect an exomoon signal in our data, our detection limits for a single moon are 80 Earth masses at P=1 day and 1 Jupiter at P=200 days, comparable to RV exomoon searches around other substellar companions. The RV limit is comparable with the astrometric exomoon limit at a period of 7 days and a mass of 150 Earth masses, where for longer periods the astrometric searches have lower mass limits. With an additional observing season, CRIRES+ can detect a planet/moon mass ratio of $10^{-3}$ (4 Earth masses) with a period of up to one day, and can detect a Neptune-mass moon at hundreds of Jupiter radii.

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 / 1 minor

Summary. The manuscript reports radial velocity monitoring of the directly imaged exoplanet β Pictoris b using cross-correlation of a template spectrum against atmospheric absorption lines, yielding a mean precision of 160 m s^{-1} across several epochs spanning October 2024 to March 2025. A periodogram search finds no significant periodic signal from an exomoon. The resulting upper limits are 80 Earth masses at a 1-day period and 1 Jupiter mass at a 200-day period; these are compared to existing astrometric limits, and projections for improved sensitivity with an additional observing season are presented.

Significance. If the noise model and sampling assumptions hold, the work supplies competitive RV-based exomoon mass limits around a young, directly imaged giant planet and illustrates the complementarity between RV and astrometric techniques. The reported precision on a substellar companion and the explicit mass-period limits constitute a concrete observational benchmark for future exomoon searches.

major comments (2)
  1. [RV measurement and periodogram analysis] The section on RV measurement and periodogram analysis does not specify the number of epochs, the precise temporal sampling, the false-alarm probability threshold adopted, or the procedure (injection-recovery or analytic) used to translate the non-detection into the quoted mass limits of 80 M_⊕ (P=1 d) and 1 M_Jup (P=200 d). These details are load-bearing because the ~5-month baseline and the assumption that the 160 m s^{-1} scatter is measurement-dominated directly determine whether the stated limits are robust or optimistic.
  2. [RV measurement and periodogram analysis] The conversion from observed RV scatter to companion mass via barycentric motion assumes negligible contribution from atmospheric dynamics or template mismatch; no quantitative test (e.g., residual analysis or red-noise model) is described to support this assumption, which underpins the entire set of upper limits.
minor comments (1)
  1. [Abstract] The abstract refers to 'several epochs' without giving the exact count or dates; the main text should list them explicitly for reproducibility.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for the constructive comments, which highlight areas where the manuscript can be strengthened for clarity and robustness. We address each major comment below.

read point-by-point responses

  1. Referee: [RV measurement and periodogram analysis] The section on RV measurement and periodogram analysis does not specify the number of epochs, the precise temporal sampling, the false-alarm probability threshold adopted, or the procedure (injection-recovery or analytic) used to translate the non-detection into the quoted mass limits of 80 M_⊕ (P=1 d) and 1 M_Jup (P=200 d). These details are load-bearing because the ~5-month baseline and the assumption that the 160 m s^{-1} scatter is measurement-dominated directly determine whether the stated limits are robust or optimistic.

    Authors: We agree these details are essential. The revised manuscript will add a table of all observation epochs with precise MJD sampling, state the adopted FAP threshold of 0.1%, and describe the injection-recovery procedure used to derive the mass limits from the periodogram non-detection. The ~5-month baseline will be explicitly noted along with the justification that the scatter is measurement-dominated. revision: yes

  2. Referee: [RV measurement and periodogram analysis] The conversion from observed RV scatter to companion mass via barycentric motion assumes negligible contribution from atmospheric dynamics or template mismatch; no quantitative test (e.g., residual analysis or red-noise model) is described to support this assumption, which underpins the entire set of upper limits.

    Authors: The referee correctly identifies that no such test was presented. We will add a new subsection with residual analysis after periodogram subtraction, a comparison of observed vs. expected uncertainties, and a simple red-noise assessment to support (or qualify) the assumption of negligible atmospheric/template contributions to the scatter. revision: yes

Circularity Check

0 steps flagged

No circularity: observational upper limits from RV non-detection

full rationale

The paper derives exomoon mass upper limits (80 M_earth at P=1 d; 1 M_Jup at P=200 d) directly from a non-detection in the periodogram of measured radial velocities obtained via template cross-correlation on CRIRES+ data. This is standard observational analysis: the reported limits follow from the observed RV scatter, temporal sampling, and periodogram sensitivity, without any equation or step that reduces the output masses to quantities defined by the fit itself or to a self-citation chain. No self-definitional, fitted-input-called-prediction, or ansatz-smuggled patterns appear in the derivation chain.

Axiom & Free-Parameter Ledger

0 free parameters · 0 axioms · 0 invented entities

No free parameters, axioms, or invented entities are identifiable from the abstract alone.

pith-pipeline@v0.9.1-grok · 5838 in / 1179 out tokens · 44506 ms · 2026-06-28T04:06:31.858747+00:00 · methodology

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Forward citations

Cited by 1 Pith paper

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score.

  1. The carbon isotope ratio of \beta\ Pic b with high-resolution spectroscopy

    astro-ph.EP 2026-06 unverdicted novelty 6.0

    Measured 12C/13C = 58+18-15 in β Pic b atmosphere via CRIRES+ spectroscopy and Bayesian retrieval, consistent with ISM value.

Reference graph

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