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arxiv: 2604.05570 · v1 · submitted 2026-04-07 · 🌌 astro-ph.EP

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Investigation of Transit Timing and an Optical Transmission Spectrum of the Hot Jupiter WASP-11 b

Napaporn A-thano , Supachai Awiphan , Eamonn Kerins , Akshay Priyadarshi , Iain McDonald , Orarik Tasuya , Ronnakrit Rattanamala , Ing-Guey Jiang
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Yogesh C. Joshi Fan Yang Ida Janiak Patcharawee Munsaket Yasir Abdul Qadir Smanchan Chandaiam Boonyarit Choonhakit Suwanit Wutsang Boonrucksar Soonthornthum Vik S Dhillon
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Pith reviewed 2026-05-10 19:36 UTC · model grok-4.3

classification 🌌 astro-ph.EP
keywords WASP-11 bhot Jupitertransit timing variationstransmission spectroscopyRayleigh scatteringorbital decayTESS
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The pith

Updated transit observations of hot Jupiter WASP-11 b show no orbital decay and no signs of additional planets, while revealing a Rayleigh scattering slope in its transmission spectrum.

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

This paper gathers 31 fresh transit light curves of the inflated hot Jupiter WASP-11 b from a global network and combines them with older ground and space data covering 16 years. The goal is to sharpen the planet's size, orbit, and temperature details while testing whether its period is shortening or if unseen planets are tugging on it. No clear decay appears in the timing residuals, and no repeating patterns suggest companions. The optical colors of the transits show the planet blocking more light at blue wavelengths, pointing to scattering that might come from its own air or from light leaks by the host star or a nearby companion.

Core claim

Combining 31 new ground-based transits with prior observations and TESS data, the timing analysis finds the observed minus calculated transit times consistent with a fixed orbital period, providing no evidence for orbital decay or additional planets through transit timing variations. The transmission spectrum from multi-band photometry displays a pronounced negative slope toward shorter wavelengths, characteristic of Rayleigh scattering that could originate in the planetary atmosphere or arise from contamination by stellar activity or the companion star.

What carries the argument

The O-C diagram tracking transit timing deviations over 16 years to test for period changes, paired with wavelength-dependent transit depth measurements to build an optical transmission spectrum.

If this is right

  • The planet maintains a stable orbit without measurable shrinkage over the 16-year baseline.
  • No periodic signals in timing data rule out detectable additional planets in this system.
  • The strong short-wavelength slope in the spectrum suggests scattering particles that future observations can probe.
  • Contamination from the companion star must be accounted for when interpreting atmospheric features.

Where Pith is reading between the lines

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

  • If the scattering is atmospheric, it implies high-altitude hazes that could be common in hot Jupiters.
  • Longer baseline monitoring could eventually detect very slow orbital changes.
  • High-resolution imaging or spectroscopy might separate the companion's light contribution to confirm the source of the slope.

Load-bearing premise

That the observed wavelength-dependent transit depths primarily reflect the planet after standard corrections for systematics, stellar activity, and companion light.

What would settle it

A measurement of the companion star's contribution to the total flux in each observing band that, when subtracted, removes the observed slope in the transmission spectrum.

Figures

Figures reproduced from arXiv: 2604.05570 by Akshay Priyadarshi, Boonrucksar Soonthornthum, Boonyarit Choonhakit, Eamonn Kerins, Fan Yang, Iain McDonald, Ida Janiak, Ing-Guey Jiang, Napaporn A-thano, Orarik Tasuya, Patcharawee Munsaket, Ronnakrit Rattanamala, Smanchan Chandaiam, Supachai Awiphan, Suwanit Wutsang, Vik S Dhillon, Yasir Abdul Qadir, Yogesh C. Joshi.

Figure 1
Figure 1. Figure 1: The normalized transit light curve of WASP-11 b/HAT-P-10 b was obtained with the 0.7 m TRT-GAO telescope in the R filter on 22 December 2016, during an observation graciously conducted remotely by Her Royal Highness Princess Maha Chakri Sirindhorn while visiting the Thai National Observatory. The best-fit model from TransitFit is shown as a solid line, and the residuals after model subtraction are displaye… view at source ↗
Figure 2
Figure 2. Figure 2: The normalized transit light curves of WASP-11 b/HAT-P-10 b observed with the 2.4-m telescope of the SPEARNET network (gray dots, upper panel). The best-fit model from TransitFit is shown as a solid line, and the residuals after model subtraction are displayed in the lower panel. 4.4. Line-of-Sight Acceleration Furthermore, orbital decay can be investigated by measuring line-of-sight acceleration, a phenom… view at source ↗
Figure 3
Figure 3. Figure 3: The normalized transit light curves of WASP-11 b/HAT-P-10 b observed by TESS (gray dots, upper panel), with the best-fit model from TransitFit shown as solid lines. The residuals after model subtraction are displayed in the lower panel. where Pq represents the orbital period from the orbital decay model (Porb,din [PITH_FULL_IMAGE:figures/full_fig_p009_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: The O − C diagram and best-fit model for WASP-11 b/HAT-P-10 b, showing data from Bakos et al. (2009) (gray dots), Mancini et al. (2015) (pink dots), Maciejewski et al. (2023) (blue dots), Yal¸cınkaya et al. (2024) (green dots), TESS (purple dots), and this study (red dots). Timing residuals for the orbital decay and apsidal precession models are shown as brown and orange curves, respectively. system. The t… view at source ↗
Figure 5
Figure 5. Figure 5: The GLS periodogram of the timing residuals from 50 mid-transit times derived with TransitFit. The false-alarm probability (FAP) levels are indicated by dashed lines. contribute to the effect. Since the host star of WASP￾11 b/HAT-P-10 b is a K-type star in a binary system, the observed scattering signature could potentially be influenced by stellar activity or contamination from the companion star, as disc… view at source ↗
Figure 6
Figure 6. Figure 6: Top panel: Retrieved transmission spectrum of WASP-11 b/HAT-P-10 b with forward models generated using PLATON. Bottom panel: Band-pass filter profiles for u ′ , g ′ , V , r ′ , R, i ′ , I, T ESS, and z ′ (from left to right). WASP-11 b/HAT-P-10 b a promising target for future observations. We thank the referee for their comments and sugges￾tions, which have improved the quality of this work. This work is s… view at source ↗
read the original abstract

WASP-11~b/HAT-P-10~b is an inflated hot Jupiter, which has a low density that makes it a good target for atmospheric studies using the transmission spectroscopy technique. In this work, we present 31 new transit light curves of WASP-11~b/HAT-P-10~b, obtained through the SPEARNET network. These data were analyzed along with previously published ground-based observations and space-based data from \texttt{TESS}. We refine the planetary parameters of WASP-11~b/HAT-P-10~b and perform a transit timing analysis using data spanning 16 years. The updated ($O-C$) diagram shows no significant evidence of orbital decay. The TTV analysis reveals no significant signals indicative of additional planets. Atmospheric analysis using multi-band optical observations indicates a strong Rayleigh scattering slope in the transmission spectra, which may originate from the planetary atmosphere itself or be influenced by contamination such as stellar activity or light from the companion star.

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

1 major / 2 minor

Summary. The manuscript reports 31 new ground-based transit light curves of the hot Jupiter WASP-11 b/HAT-P-10 b obtained via the SPEARNET network. Combined with prior observations and TESS data spanning 16 years, the authors refine the system parameters, construct an O-C diagram showing no significant orbital decay, perform TTV analysis finding no evidence for additional planets, and derive a multi-band optical transmission spectrum exhibiting a strong Rayleigh scattering slope whose origin is attributed possibly to the planetary atmosphere or to contamination from stellar activity or the unresolved companion star.

Significance. If the timing results hold, the 16-year baseline strengthens constraints on orbital stability for this inflated hot Jupiter and adds to the sample of systems without detectable TTVs or decay. The optical transmission spectrum contributes to the catalog of Rayleigh-like slopes in hot Jupiters. The long ground-based temporal coverage is a clear strength for the O-C and TTV portions of the work.

major comments (1)
  1. [Transmission spectrum analysis] Transmission spectrum analysis (abstract and corresponding results section): The reported strong Rayleigh scattering slope is presented with an explicit caveat that it 'may originate from the planetary atmosphere itself or be influenced by contamination such as stellar activity or light from the companion star,' yet no quantitative modeling, dilution corrections, or upper limits on the wavelength-dependent contributions from the companion or spot-induced variability are provided. Standard differential photometry and limb-darkening corrections alone do not isolate these effects; if companion dilution or activity reaches a few percent in the blue, it can produce or erase a slope of the reported magnitude. This renders the atmospheric attribution ambiguous and load-bearing for the central atmospheric claim.
minor comments (2)
  1. [Abstract] Abstract: The phrase 'strong Rayleigh scattering slope' is used without quoting the measured slope value (e.g., in units of scale heights per 1000 Å), its uncertainty, or the wavelength range over which it is detected.
  2. [Methods/Observations] The manuscript would benefit from a brief statement in the methods or results on whether simultaneous activity monitoring or resolved photometry of the companion was obtained or used in the transmission-spectrum reduction.

Simulated Author's Rebuttal

1 responses · 0 unresolved

We thank the referee for their constructive review and positive assessment of the significance of the timing analysis and long-baseline coverage. We address the single major comment below.

read point-by-point responses

  1. Referee: Transmission spectrum analysis (abstract and corresponding results section): The reported strong Rayleigh scattering slope is presented with an explicit caveat that it 'may originate from the planetary atmosphere itself or be influenced by contamination such as stellar activity or light from the companion star,' yet no quantitative modeling, dilution corrections, or upper limits on the wavelength-dependent contributions from the companion or spot-induced variability are provided. Standard differential photometry and limb-darkening corrections alone do not isolate these effects; if companion dilution or activity reaches a few percent in the blue, it can produce or erase a slope of the reported magnitude. This renders the atmospheric attribution ambiguous and load-bearing for the central atmospheric claim.

    Authors: We agree that the current presentation leaves the origin of the slope ambiguous without quantitative constraints. In the revised manuscript we will add a new subsection to the transmission-spectrum analysis that (1) estimates the dilution contribution from the known unresolved companion using its reported magnitude difference and assumed spectral type, (2) derives the maximum wavelength-dependent slope that could be produced by plausible levels of stellar activity (spot coverage and temperature contrast), and (3) places upper limits on the fractional contamination required to fully explain or erase the observed slope. These calculations will be performed with the same photometric bands used for the spectrum and will be presented alongside the existing data so that readers can directly assess the robustness of an atmospheric interpretation. revision: yes

Circularity Check

0 steps flagged

No circularity: results are direct empirical outputs from transit photometry and timing data

full rationale

The paper collects 31 new ground-based transit light curves, combines them with archival data spanning 16 years including TESS, and applies standard timing (O-C) and multi-band photometric analysis. The reported absence of orbital decay, lack of TTV signals, and presence of a Rayleigh slope are direct measurements from the data fits; no equations, parameters, or claims are shown to reduce to their own inputs by construction, nor do any self-citations serve as load-bearing premises for the central results. The noted ambiguity in slope origin is an interpretive caveat, not a circular step.

Axiom & Free-Parameter Ledger

0 free parameters · 1 axioms · 0 invented entities

The central claims rest on conventional assumptions of transit photometry and orbital dynamics without introducing new entities or ad-hoc parameters beyond standard model fits.

axioms (1)
  • domain assumption Standard assumptions of spherical planet, quadratic limb darkening, and Keplerian orbit in transit modeling
    Implicit in all ground-based and TESS transit photometry analyses described.

pith-pipeline@v0.9.0 · 5579 in / 1183 out tokens · 61155 ms · 2026-05-10T19:36:02.813293+00:00 · methodology

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