pith. sign in

arxiv: 2605.29445 · v1 · pith:E46VV5QHnew · submitted 2026-05-28 · 🌌 astro-ph.EP · astro-ph.SR

Optical transmission spectrum of HAT-P-47b: evidence for aerosols and tentative TiO absorption

Wan-Hao Wang , Guo Chen , Fei Yan , Chengzi Jiang , Luigi Mancini , Enric Pall\'e , Felipe Murgas , Hannu Parviainen This is my paper

Pith reviewed 2026-06-29 00:58 UTC · model grok-4.3

classification 🌌 astro-ph.EP astro-ph.SR
keywords exoplanet atmospherestransmission spectroscopyhot JupiterTiO absorptionaerosolsHAT-P-47bBayesian retrievaloptical spectrum
0
0 comments X

The pith

HAT-P-47b's optical transmission spectrum indicates aerosols with 5000 times the scattering of pure H2 and moderate evidence for TiO absorption.

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

The paper measures the optical transmission spectrum of the hot Jupiter HAT-P-47b using data from thirteen TESS transits plus two ground-based transits observed with LBT/MODS and GTC/OSIRIS+. Chromatic light curves are extracted and fed into multiple Bayesian retrievals that test for molecular opacities and aerosol scattering. The joint retrieval finds moderate evidence for TiO at a mass fraction around 10^-7 and an aerosol scattering term much stronger than hydrogen Rayleigh scattering. A sympathetic reader would care because optical wavelengths can reveal metal oxides that shape how a planet absorbs incoming starlight and sets its temperature profile. If the findings hold, they add a data point showing that some hot Jupiters carry both clouds and specific molecular species in their upper atmospheres.

Core claim

The MODS and OSIRIS+ joint free-chemistry retrieval yields moderate evidence (ΔlnZ=3.44) for TiO with a log mass fraction of -6.86+0.64-0.63 dex; the same model indicates an aerosol contribution to the optical scattering opacity approximately 5000× larger than pure H2 Rayleigh scattering. HAT-P-47b appears to host a cloudy atmosphere with evidence for aerosols and tentative evidence for TiO absorption.

What carries the argument

Bayesian spectral retrievals comparing free-chemistry models with and without TiO opacity and an enhanced aerosol scattering term, applied to instrument-specific transmission spectra derived from chromatic transit light curves.

If this is right

  • The planet's optical spectrum is shaped primarily by aerosol scattering rather than molecular features alone.
  • A TiO mass fraction near 10^-7 would contribute to the atmospheric energy balance and thermal structure.
  • The two instruments yield differing strengths of evidence for TiO, with the higher-S/N MODS data dominating the joint result.
  • Future observations are required to confirm or refute the TiO detection and refine the aerosol properties.

Where Pith is reading between the lines

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

  • Similar aerosol levels in other hot Jupiters could systematically suppress molecular features in optical spectra.
  • The moderate Bayesian evidence level means that one or two additional high-quality transits could shift the result from tentative to strong or to absent.
  • Independent constraints on aerosol particle size or composition would test whether the slope attribution is unique.

Load-bearing premise

The wavelength-dependent slope is produced by aerosol scattering rather than residual instrumental systematics or stellar activity.

What would settle it

Additional high-precision optical transit observations that either detect TiO absorption bands at higher significance or reproduce the slope without requiring enhanced aerosol opacity.

Figures

Figures reproduced from arXiv: 2605.29445 by Chengzi Jiang, Enric Pall\'e, Fei Yan, Felipe Murgas, Guo Chen, Hannu Parviainen, Luigi Mancini, Wan-Hao Wang.

Figure 1
Figure 1. Figure 1: Example stellar spectra of HAT-P-47 (T; solid line) and [PITH_FULL_IMAGE:figures/full_fig_p003_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: Phase-folded TESS transit light curves of HAT-P-47. Top: [PITH_FULL_IMAGE:figures/full_fig_p004_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: Transit timing residuals of HAT-P-47 relative to a linear [PITH_FULL_IMAGE:figures/full_fig_p005_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: White light curves of HAT-P-47 from LBT/ [PITH_FULL_IMAGE:figures/full_fig_p007_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: Spectroscopic light curves of HAT-P-47 from LBT/ [PITH_FULL_IMAGE:figures/full_fig_p008_5.png] view at source ↗
Figure 6
Figure 6. Figure 6: Individual transmission spectra of HAT-P-47b de [PITH_FULL_IMAGE:figures/full_fig_p009_6.png] view at source ↗
Figure 7
Figure 7. Figure 7: Joint retrieval of the LBT/MODS and GTC/OSIRIS+ transmission spectra of HAT-P-47b assuming equilibrium chemistry (panel a) and free chemistry (panel b). Top sub-panels: observed transmission spectra with the best-fit models, after applying the retrieved vertical offsets and error-scaling factors. The shaded regions indicate the median model and the associated 1σ and 2σ confidence intervals. Bottom sub-pane… view at source ↗
Figure 8
Figure 8. Figure 8: Posterior distributions of the retrieved atmospheric pa [PITH_FULL_IMAGE:figures/full_fig_p012_8.png] view at source ↗
read the original abstract

Transmission spectroscopy enables the characterization of exoplanet atmospheres by probing absorption features in their terminator regions. In the optical, it is particularly sensitive to metal oxides and atomic species that can strongly influence atmospheric energy balance and thermal structure. We aim to investigate the atmospheric properties of the hot Jupiter HAT-P-47b through optical transmission spectroscopy. Thirteen TESS transits were analyzed to refine the planetary ephemeris and system parameters. Two ground-based transits were observed with LBT/MODS and GTC/OSIRIS+. Chromatic transit light curves were modeled to derive instrument-specific transmission spectra and multiple Bayesian spectral retrievals were performed to characterize the atmospheric properties. The MODS transmission spectrum provides moderate Bayesian evidence ($\Delta\ln\mathcal{Z}=2.68$) for TiO absorption, whereas the OSIRIS+ spectrum does not yield statistically significant evidence for any specific opacity source. Both datasets exhibit a wavelength-dependent slope indicative of enhanced aerosol scattering. The MODS and OSIRIS+ joint free-chemistry retrieval, dominated by the higher signal-to-noise MODS data, yields moderate evidence ($\Delta\ln\mathcal{Z}=3.44$) for TiO with a log mass fraction of $-6.86^{+0.64}_{-0.63}$ dex. The same model indicates an aerosol contribution to the optical scattering opacity approximately $5000\times$ larger than pure H$_2$ Rayleigh scattering. HAT-P-47b appears to host a cloudy atmosphere with evidence for aerosols and tentative evidence for TiO absorption. Future high-precision observations will be essential to confirm the presence of TiO and further characterize its atmospheric structure.

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 presents optical transmission spectra of HAT-P-47b from LBT/MODS and GTC/OSIRIS+ observations, combined with 13 TESS transits for ephemeris refinement. Chromatic light curves are modeled to produce instrument-specific transmission spectra, followed by multiple Bayesian retrievals. Both datasets show a negative wavelength-dependent slope; the joint free-chemistry retrieval yields moderate evidence (ΔlnZ=3.44) for TiO at log mass fraction -6.86 dex and an aerosol scattering opacity ~5000× larger than pure H2 Rayleigh, leading to the conclusion of a cloudy atmosphere with aerosols and tentative TiO.

Significance. If the central claims hold, the work would contribute a new optical transmission spectrum to the hot-Jupiter sample, illustrating the combined effects of aerosols and possible metal-oxide absorption. The multi-instrument dataset, joint retrieval, and explicit reporting of Bayesian evidence values are positive features that allow direct assessment of the strength of the TiO detection.

major comments (2)
  1. [Abstract and retrieval section] Abstract and retrieval section: the attribution of the entire observed slope to an aerosol scattering term (5000× H2 Rayleigh) is load-bearing for both the aerosol and TiO claims, yet the retrieval description provides no external constraint or test (e.g., simultaneous photometry, activity indicators, or telluric-correction diagnostics) to exclude residual ground-based systematics or stellar activity as the origin of the slope.
  2. [Joint retrieval results] Joint retrieval results: because the joint ΔlnZ=3.44 is dominated by the higher-S/N MODS data, any unmodeled low-level slope in MODS propagates directly into both the aerosol amplitude and the marginal TiO abundance; the manuscript does not report robustness tests that isolate this dependence.
minor comments (1)
  1. [Abstract] The abstract correctly qualifies the TiO result as 'tentative' given ΔlnZ=3.44; this language should be retained consistently in the discussion.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their constructive review and for highlighting key points regarding the robustness of our aerosol scattering and TiO claims. We address each major comment below and indicate where revisions will be made.

read point-by-point responses

  1. Referee: [Abstract and retrieval section] Abstract and retrieval section: the attribution of the entire observed slope to an aerosol scattering term (5000× H2 Rayleigh) is load-bearing for both the aerosol and TiO claims, yet the retrieval description provides no external constraint or test (e.g., simultaneous photometry, activity indicators, or telluric-correction diagnostics) to exclude residual ground-based systematics or stellar activity as the origin of the slope.

    Authors: We agree that external validation would strengthen the interpretation. The slope appears consistently in two independent instruments (LBT/MODS and GTC/OSIRIS+) taken on separate nights with different telescopes and reduction pipelines, which reduces the probability of instrument-specific systematics. The TESS light curves used for ephemeris refinement show no significant out-of-transit variability indicative of strong stellar activity. However, the manuscript does not present dedicated activity indicators extracted from the spectra or simultaneous photometry. We will revise the retrieval section to include an expanded discussion of these limitations and any available telluric diagnostics from the observations. revision: partial

  2. Referee: [Joint retrieval results] Joint retrieval results: because the joint ΔlnZ=3.44 is dominated by the higher-S/N MODS data, any unmodeled low-level slope in MODS propagates directly into both the aerosol amplitude and the marginal TiO abundance; the manuscript does not report robustness tests that isolate this dependence.

    Authors: The manuscript already notes that the joint retrieval is dominated by the higher-S/N MODS dataset. To isolate the dependence, we will add explicit robustness tests in the revised manuscript, including (i) retrievals performed on the MODS spectrum alone, (ii) retrievals on the OSIRIS+ spectrum alone, and (iii) a test in which the MODS slope is artificially flattened to quantify the impact on the TiO Bayesian evidence. These additional results will be reported alongside the existing joint retrieval. revision: yes

Circularity Check

0 steps flagged

No significant circularity detected

full rationale

The paper derives transmission spectra from observed light curves (MODS and OSIRIS+), then performs standard Bayesian retrievals to fit atmospheric parameters including aerosol opacity scale and TiO abundance, reporting ΔlnZ values from model comparison. These steps use external data as input and produce posterior inferences; no equation or claim reduces by construction to a prior fit of the same quantity, no self-citation chain bears the central result, and no ansatz or uniqueness theorem is imported from the authors' prior work. The analysis is self-contained against the provided spectra and TESS ephemeris.

Axiom & Free-Parameter Ledger

2 free parameters · 1 axioms · 0 invented entities

The central claim rests on the retrieval model attributing the entire observed slope to aerosols and on moderate Bayesian evidence thresholds for TiO; these depend on the free-chemistry assumption and the absence of unaccounted systematics.

free parameters (2)
  • TiO log mass fraction = -6.86
    Fitted parameter in the joint free-chemistry retrieval to match the observed spectrum
  • Aerosol scattering opacity multiplier = 5000
    Fitted to reproduce the wavelength-dependent slope
axioms (1)
  • domain assumption Atmosphere is adequately described by a 1D plane-parallel model with free chemistry abundances
    Foundation of the Bayesian spectral retrievals

pith-pipeline@v0.9.1-grok · 5856 in / 1297 out tokens · 56886 ms · 2026-06-29T00:58:43.109926+00:00 · methodology

discussion (0)

Sign in with ORCID, Apple, or X to comment. Anyone can read and Pith papers without signing in.

Reference graph

Works this paper leans on

103 extracted references · 4 canonical work pages · 3 internal anchors

  1. [1]

    2025, MNRAS, 540, 2535

    Ahrer, E.-M., Gandhi, S., Alderson, L., et al. 2025, MNRAS, 540, 2535

    2025

  2. [2]

    R., MacDonald, R

    Alderson, L., Wakeford, H. R., MacDonald, R. J., et al. 2022, MNRAS, 512, 4185

    2022

  3. [3]

    W., & O’Neil, M

    Ambikasaran, S., Foreman-Mackey, D., Greengard, L., Hogg, D. W., & O’Neil, M. 2015, IEEE Transactions on Pattern Analysis and Machine Intelligence, 38, 252

    2015

  4. [4]

    HAT-P-47b AND HAT-P-48b: Two Low Density Sub-Saturn-Mass Transiting Planets on the Edge of the Period--Mass Desert

    Bakos, G. Á., Hartman, J. D., Torres, G., et al. 2016, arXiv e-prints, arXiv:1606.04556

    work page internal anchor Pith review Pith/arXiv arXiv 2016

  5. [5]

    J., Crouzet, N., Cubillos, P

    Bell, T. J., Crouzet, N., Cubillos, P. E., et al. 2024, Nature Astronomy, 8, 879

    2024

  6. [6]

    2002, A&A, 390, 779 Article number, page 13 A&A proofs:manuscript no

    Borysow, A. 2002, A&A, 390, 779 Article number, page 13 A&A proofs:manuscript no. manuscripts_clean

    2002

  7. [7]

    & Frommhold, L

    Borysow, A. & Frommhold, L. 1989, ApJ, 341, 549

    1989

  8. [8]

    1989, ApJ, 336, 495

    Borysow, A., Frommhold, L., & Moraldi, M. 1989, ApJ, 336, 495

    1989

  9. [9]

    G., & Fu, Y

    Borysow, A., Jorgensen, U. G., & Fu, Y . 2001, J. Quant. Spectr. Rad. Transf., 68, 235

    2001

  10. [10]

    1988, ApJ, 326, 509

    Borysow, J., Frommhold, L., & Birnbaum, G. 1988, ApJ, 326, 509

    1988

  11. [11]

    The TESS All-Sky Rotation Survey: Periods for 1,046,317 Stars Within 500 pc

    Boyle, A. W., Bouma, L. G., & Mann, A. W. 2026, arXiv e-prints, arXiv:2603.05586

    work page internal anchor Pith review Pith/arXiv arXiv 2026

  12. [12]

    2014, A&A, 564, A125

    Buchner, J., Georgakakis, A., Nandra, K., et al. 2014, A&A, 564, A125

    2014

  13. [13]

    A., Tenenbaum, P., Twicken, J

    Caldwell, D. A., Tenenbaum, P., Twicken, J. D., et al. 2020, Research Notes of the American Astronomical Society, 4, 201

    2020

  14. [14]

    G., et al

    Cepa, J., Aguiar, M., Escalera, V . G., et al. 2000, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, V ol. 4008, Optical and IR Telescope Instrumentation and Detectors, ed. M. Iye & A. F. Moorwood, 623–631

    2000

  15. [15]

    A., Lothringer, J., & Blake, G

    Chachan, Y ., Knutson, H. A., Lothringer, J., & Blake, G. A. 2023, ApJ, 943, 112

    2023

  16. [16]

    Chan, Y . M. & Dalgarno, A. 1965, Proceedings of the Physical Society, 85, 227

    1965

  17. [17]

    2021, ApJ, 913, L16

    Chen, G., Pallé, E., Parviainen, H., Murgas, F., & Yan, F. 2021, ApJ, 913, L16

    2021

  18. [18]

    2024, A&A, 682, A136

    Claudi, R., Bruno, G., Fossati, L., et al. 2024, A&A, 682, A136

    2024

  19. [19]

    2021, A&A, 651, A33

    Cont, D., Yan, F., Reiners, A., et al. 2021, A&A, 651, A33

    2021

  20. [20]

    & Williams, D

    Dalgarno, A. & Williams, D. A. 1962, ApJ, 136, 690

    1962

  21. [21]

    2024, Nature, 625, 51

    Dyrek, A., Min, M., Decin, L., et al. 2024, Nature, 625, 51

    2024

  22. [22]

    Eastman, J., Siverd, R., & Gaudi, B. S. 2010, PASP, 122, 935

    2010

  23. [23]

    & Changeat, Q

    Edwards, B. & Changeat, Q. 2024, ApJ, 962, L30

    2024

  24. [24]

    & Jordán, A

    Espinoza, N. & Jordán, A. 2015, MNRAS, 450, 1879

    2015

  25. [25]

    V ., Jordán, A., et al

    Espinoza, N., Rackham, B. V ., Jordán, A., et al. 2019, MNRAS, 482, 2065

    2019

  26. [26]

    M., Sing, D

    Evans, T. M., Sing, D. K., Goyal, J. M., et al. 2018, AJ, 156, 283

    2018

  27. [27]

    2017, AJ, 154, 220

    Foreman-Mackey, D., Agol, E., Ambikasaran, S., & Angus, R. 2017, AJ, 154, 220

    2017

  28. [28]

    W., Lang, D., & Goodman, J

    Foreman-Mackey, D., Hogg, D. W., Lang, D., & Goodman, J. 2013, PASP, 125, 306

    2013

  29. [29]

    J., Lodders, K., Marley, M

    Fortney, J. J., Lodders, K., Marley, M. S., & Freedman, R. S. 2008, ApJ, 678, 1419

    2008

  30. [30]

    J., Radica, M., et al

    Fournier-Tondreau, M., MacDonald, R. J., Radica, M., et al. 2024, MNRAS, 528, 3354

    2024

  31. [31]

    2023, AJ, 165, 242

    Gandhi, S., Kesseli, A., Zhang, Y ., et al. 2023, AJ, 165, 242

    2023

  32. [32]

    R., Moran, S

    Gao, P., Wakeford, H. R., Moran, S. E., & Parmentier, V . 2021, Journal of Geo- physical Research (Planets), 126, e06655

    2021

  33. [33]

    P., Aigrain, S., Barstow, J

    Gibson, N. P., Aigrain, S., Barstow, J. K., et al. 2013, MNRAS, 428, 3680

    2013

  34. [34]

    P., Aigrain, S., Roberts, S., et al

    Gibson, N. P., Aigrain, S., Roberts, S., et al. 2012, MNRAS, 419, 2683

    2012

  35. [35]

    K., Wakeford, H

    Grant, D., Lewis, N. K., Wakeford, H. R., et al. 2023, ApJ, 956, L32

    2023

  36. [36]

    2010, A&A, 520, A27

    Guillot, T. 2010, A&A, 520, A27

    2010

  37. [37]

    J., de Kok, R

    Hoeijmakers, H. J., de Kok, R. J., Snellen, I. A. G., et al. 2015, A&A, 575, A20

    2015

  38. [38]

    J., Kitzmann, D., Morris, B

    Hoeijmakers, H. J., Kitzmann, D., Morris, B. M., et al. 2024, A&A, 685, A139

    2024

  39. [39]

    J., Seidel, J

    Hoeijmakers, H. J., Seidel, J. V ., Pino, L., et al. 2020, A&A, 641, A123

    2020

  40. [40]

    X., Vanderburg, A., Pál, A., et al

    Huang, C. X., Vanderburg, A., Pál, A., et al. 2020, Research Notes of the Amer- ican Astronomical Society, 4, 206

    2020

  41. [41]

    2003, ApJ, 594, 1011

    Hubeny, I., Burrows, A., & Sudarsky, D. 2003, ApJ, 594, 1011

    2003

  42. [42]

    M., Sing, D

    Huitson, C. M., Sing, D. K., Pont, F., et al. 2013, MNRAS, 434, 3252

    2013

  43. [43]

    2013, A&A, 553, A6

    Husser, T.-O., Wende-von Berg, S., Dreizler, S., et al. 2013, A&A, 553, A6

    2013

  44. [44]

    E., Lewis, N

    Inglis, J., Batalha, N. E., Lewis, N. K., et al. 2024, ApJ, 973, L41

    2024

  45. [45]

    M., Twicken, J

    Jenkins, J. M., Twicken, J. D., McCauliff, S., et al. 2016, in Society of Photo- Optical Instrumentation Engineers (SPIE) Conference Series, V ol. 9913, Soft- ware and Cyberinfrastructure for Astronomy IV , ed. G. Chiozzi & J. C. Guz- man, 99133E

    2016

  46. [46]

    2024, A&A, 682, A73

    Jiang, C., Chen, G., Murgas, F., et al. 2024, A&A, 682, A73

    2024

  47. [47]

    2022, A&A, 664, A50

    Jiang, C., Chen, G., Pallé, E., et al. 2022, A&A, 664, A50

    2022

  48. [48]

    The Effect of Atmospheric Chemistry on the Optical Geometric Albedos of Hot Jupiters

    Jones, K. D., Morris, B. M., & Heng, K. 2026, arXiv e-prints, arXiv:2603.02409

    work page internal anchor Pith review Pith/arXiv arXiv 2026

  49. [49]

    & Ikoma, M

    Kawashima, Y . & Ikoma, M. 2019, ApJ, 877, 109

    2019

  50. [50]

    Kipping, D. M. 2010, MNRAS, 408, 1758

    2010

  51. [51]

    A., Howard, A

    Knutson, H. A., Howard, A. W., & Isaacson, H. 2010, ApJ, 720, 1569

    2010

  52. [52]

    2015, PASP, 127, 1161 Lecavelier Des Etangs, A., Pont, F., Vidal-Madjar, A., & Sing, D

    Kreidberg, L. 2015, PASP, 127, 1161 Lecavelier Des Etangs, A., Pont, F., Vidal-Madjar, A., & Sing, D. 2008, A&A, 481, L83

    2015

  53. [53]

    & Mollière, P

    Lei, E. & Mollière, P. 2025, The Journal of Open Source Software, 10, 7712 Lightkurve Collaboration, Cardoso, J. V . d. M., Hedges, C., et al. 2018, Lightkurve: Kepler and TESS time series analysis in Python, Astrophysics Source Code Library, record ascl:1812.013

    2025

  54. [54]

    2003, ApJ, 591, 1220

    Lodders, K. 2003, ApJ, 591, 1220

    2003

  55. [55]

    D., Barman, T., & Koskinen, T

    Lothringer, J. D., Barman, T., & Koskinen, T. 2018, ApJ, 866, 27

    2018

  56. [56]

    R., Mullens, E., Alderson, L., et al

    Louie, D. R., Mullens, E., Alderson, L., et al. 2025, AJ, 169, 86

    2025

  57. [57]

    MacDonald, R. J. & Madhusudhan, N. 2017, MNRAS, 469, 1979

    2017

  58. [58]

    2012, ApJ, 758, 36

    Madhusudhan, N. 2012, ApJ, 758, 36

    2012

  59. [59]

    P., Nugroho, S

    Maguire, C., Gibson, N. P., Nugroho, S. K., et al. 2023, MNRAS, 519, 1030

    2023

  60. [60]

    2016, A&A, 589, A75

    Mazeh, T., Holczer, T., & Faigler, S. 2016, A&A, 589, A75

    2016

  61. [61]

    2014, ApJS, 211, 24

    McQuillan, A., Mazeh, T., & Aigrain, S. 2014, ApJS, 211, 24

    2014

  62. [62]

    R., Gibson, N

    Merritt, S. R., Gibson, N. P., Nugroho, S. K., et al. 2020, A&A, 636, A117 Mollière, P., van Boekel, R., Bouwman, J., et al. 2017, A&A, 600, A10 Mollière, P., Wardenier, J. P., van Boekel, R., et al. 2019, A&A, 627, A67

    2020

  63. [63]

    2016, ApJ, 832, 41

    Mordasini, C., van Boekel, R., Mollière, P., Henning, T., & Benneke, B. 2016, ApJ, 832, 41

    2016

  64. [64]

    2020, ApJ, 896, L22

    Mousis, O., Deleuil, M., Aguichine, A., et al. 2020, ApJ, 896, L22

    2020

  65. [65]

    K., & MacDonald, R

    Mullens, E., Lewis, N. K., & MacDonald, R. J. 2024, ApJ, 977, 105

    2024

  66. [66]

    K., Kawahara, H., Masuda, K., et al

    Nugroho, S. K., Kawahara, H., Masuda, K., et al. 2017, AJ, 154, 221

    2017

  67. [67]

    & Kawashima, Y

    Ohno, K. & Kawashima, Y . 2020, ApJ, 895, L47

    2020

  68. [68]

    2023, MNRAS, 521, 5860

    Ouyang, Q., Wang, W., Zhai, M., et al. 2023, MNRAS, 521, 5860

    2023

  69. [69]

    R., Bean, J

    Parmentier, V ., Line, M. R., Bean, J. L., et al. 2018, A&A, 617, A110

    2018

  70. [70]

    P., & Lian, Y

    Parmentier, V ., Showman, A. P., & Lian, Y . 2013, A&A, 558, A91

    2013

  71. [71]

    2023, Nature, 619, 491

    Pelletier, S., Benneke, B., Ali-Dib, M., et al. 2023, Nature, 619, 491

    2023

  72. [72]

    2026, arXiv e-prints, arXiv:2602.02845

    Pelletier, S., Kitzmann, D., Vaulato, V ., et al. 2026, arXiv e-prints, arXiv:2602.02845

    work page arXiv 2026

  73. [73]

    & Madhusudhan, N

    Pinhas, A. & Madhusudhan, N. 2017, MNRAS, 471, 4355

    2017

  74. [74]

    2018, A&A, 612, A53

    Pino, L., Ehrenreich, D., Wyttenbach, A., et al. 2018, A&A, 612, A53

    2018

  75. [75]

    2019, rwpogge/modsCCDRed: v2.0.1

    Pogge, R. 2019, rwpogge/modsCCDRed: v2.0.1

    2019

  76. [76]

    W., Atwood, B., Brewer, D

    Pogge, R. W., Atwood, B., Brewer, D. F., et al. 2010, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, V ol. 7735, Ground- based and Airborne Instrumentation for Astronomy III, ed. I. S. McLean, S. K. Ramsay, & H. Takami, 77350A

    2010

  77. [77]

    K., Gibson, N

    Pont, F., Sing, D. K., Gibson, N. P., et al. 2013, MNRAS, 432, 2917

    2013

  78. [78]

    J., Kitzmann, D., et al

    Prinoth, B., Hoeijmakers, H. J., Kitzmann, D., et al. 2022, Nature Astronomy, 6, 449

    2022

  79. [79]

    J., Pelletier, S., et al

    Prinoth, B., Hoeijmakers, H. J., Pelletier, S., et al. 2023, A&A, 678, A182

    2023

  80. [80]

    V ., Hoeijmakers, H

    Prinoth, B., Seidel, J. V ., Hoeijmakers, H. J., et al. 2025, A&A, 694, A284

    2025

Showing first 80 references.