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A new window in time: a mid-infrared slit spectroscopy mode for precision time-series astronomy with JWST/MIRI

T0 review · 2 major / 5 minor · reviewed 2026-08-15 · deepseek-v4-flash

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Pith's one-line read The first transit observed through the JWST/MIRI LRS slit shows the mode can deliver precision time-series spectra: slit losses below 40 ppm and background 38 times lower than slitless.

desk verdict First MIRI LRS slit time-series observation works, and the background reduction is real, but the headline <40 ppm slit-loss number is a static simulation, not a time-series prediction. read the letter →

arxiv 2608.04110 v1 pith:2GG4UTJK submitted 2026-08-04 astro-ph.EP astro-ph.IM

Achrene Dyrek , Taylor J. Bell , Pierre-Olivier Lagage , Sarah Kendrew , Gareb Fernandez-Rodriguez , Thomas Greene , Giuseppe Morello , Michiel Min
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Mael Voyer Hannu Parviainen
This is my paper · ORCID
classification astro-ph.EPastro-ph.IM
keywords JWSTMIRILRSslitspectroscopytime-seriesobservationsexoplanettransmissionmid-infraredlosseswavelength-correlatednoise
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 reports the first time-series observation taken through the narrow slit of JWST's MIRI low-resolution spectrometer: a 10.2-hour transit of the exoplanet HAT-P-12b. It claims that this slit mode is feasible for precision exoplanet spectroscopy, with pointing-induced slit-loss variations estimated below 40 ppm at $10\,\mu$m and a background about 38 times lower than in the slitless mode. Two independent reductions of the slit transit agree within $1\sigma$, and a joint fit with archival slitless data recovers the same atmospheric feature near $7.5\,\mu$m. The paper also flags a wavelength-correlated noise above about $8\,\mu$m that appears only in the slit dataset and whose physical origin is not yet established. If the mode holds up, it opens slit time-series spectroscopy to faint targets that are background-limited in slitless mode.

What carries the argument

The load-bearing object is the slit itself, a $4.7''\times0.51''$ aperture whose mask carries a filter blocking radiation below $4.5\,\mu$m, so the dispersed spectrum is clean and the background per detector pixel is small. Around this aperture, the feasibility argument runs on three mechanisms: FGS guide-star centroid telemetry converted into pointing dispersions; point-spread-function simulations that propagate a static $3\sigma$ offset into the transmitted flux to bound slit losses; and the residual correlation matrix of the spectroscopic light-curve fits, which exposes the long-wavelength correlated noise. A custom correction for the brighter-fatter detector effect and two independent reduction pipelines are used to show that the extracted spectrum does not depend on one processing chain.

What would settle it

A second slit transit of HAT-P-12b observed with the SUBSLIT subarray, which allows many more groups per integration, would settle the main caveat: if the residual correlation matrix above $8\,\mu$m still shows the same off-diagonal structure, the long-wavelength correlated noise is intrinsic to slit spectroscopy rather than a short-ramp artifact. Comparing the FGS centroid time series with the extracted white-light residuals would independently check whether real slit losses match the simulated 40 ppm level.

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Extended reading notes

Core claim

The central discovery claim is that the MIRI LRS slit, previously reserved for static spectroscopy, is reliable enough to serve as a time-series spectroscopy mode. The paper stakes this on a $\sim$10-hour transit observation of HAT-P-12b: two independent reductions of the slit data agree within $1\sigma$, and a joint fit with the archival slitless spectrum recovers the same atmospheric feature near $7.5\,\mu$m. It further estimates, from measured FGS pointing dispersions ($\sigma_x=1.29\times10^{-3}$ arcsec, $\sigma_y=5.92\times10^{-4}$ arcsec) propagated through point-spread-function simulations, that a conservative $3\sigma$ pointing offset changes the flux through the $4.7''\times0.51''$ slit by 0.004% (40 ppm) at $10\,\mu$m. Because the slit spatially filters background while the prism disperses light, the average background is about 38 times lower than in slitless mode over $5$--$12\,\mu$m. The paper also reports a wavelength-correlated noise above $\sim8\,\mu$m that appears only in the slit dataset and is not yet explained.

Load-bearing premise

The feasibility claim stands on two premises: that the wavelength-correlated noise seen above $\sim8\,\mu$m is a correctable detector effect rather than an intrinsic property of the slit mode, and that the static $3\sigma$ pointing-offset simulation faithfully represents the real jitter-driven slit losses; if either premise is wrong, the precision or the quoted immunity to jitter is lower than claimed.

Editorial extensions

If this is right

  • Faint planetary hosts with $J\sim13$--$15$ become accessible to MIRI LRS time-series spectroscopy, because the slit's lower background removes a dominant noise source that limits slitless observations of such targets.
  • Future slit TSO programs can drop many position-angle constraints, since the slit prevents nearby sources from being dispersed across the spectrum, which increases scheduling flexibility.
  • The slit's more reproducible illumination history could make detector-settling systematics more repeatable between observations, reducing the diversity of ramp behaviours seen in slitless TSOs.
  • A dedicated SUBSLIT subarray with more groups per integration should mitigate the short-ramp non-linearity and correlated-noise issues, strengthening the mode for Cycle 7 science.

Reading between the lines

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

  • A directly testable extension of the paper's illumination-history hypothesis would be to schedule a slit TSO immediately after a short exposure of the science region; if the long-wavelength correlated noise comes from the detector's prior illumination, it should weaken or disappear.
  • The 40 ppm slit-loss figure is a static estimate, so a time-resolved simulation fed with the full FGS centroid time series could reveal whether slow drifts or high-frequency jitter couple to slit losses differently, a check the paper does not perform.
  • The factor-of-38 background reduction will depend on zodiacal background and roll angle, so comparing slit and slitless backgrounds across multiple epochs and sky positions would test how general the advantage is for the community.
  • For bright targets the background advantage is irrelevant and the slit errors are comparable to slitless, so the strongest case for the mode is its use on fainter targets; a faint-target demonstration would reveal whether the short-ramp and brighter-fatter corrections limit precision in the regime the mode is meant to serve.
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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

2 major / 5 minor

Summary. This manuscript reports the first JWST/MIRI LRS time-series observation through the 4.7 by 0.51 arcsecond slit: a roughly 10 hour transit of HAT-P-12b from Cycle 3 program PID 6219. The data are reduced with two independent pipelines (Eureka! and ExoTEDRF+ExoIris), compared with archival slitless observations of the same target, and used to estimate a 38x background reduction, a slit-loss variation of less than 40 ppm at 10 microns, and a joint spectrum confirming the atmospheric feature near 7.5 microns. The authors conclude that the slit mode is feasible and suitable for precision exoplanet spectroscopy and that it will be offered as a supported mode from Cycle 7 onward.

Significance. If the central claim holds, the paper establishes a new JWST observing mode with a substantially lower background, which is directly relevant to faint-target exoplanet spectroscopy and to scheduling flexibility. Strengths include the use of two independent reduction pipelines, the direct measurement of the background reduction from contemporaneous data, the explicit use of FGS telemetry, and the honest reporting of limitations (first-channel offset, long-wavelength correlated noise). The main quantitative support for 'suitable for precision time series' currently rests on a slit-loss estimate whose uncertainty and time-dependence are not established, so the significance of the paper is high but the supporting evidence for this particular claim is not yet complete.

major comments (2)
  1. [Section 2.5] The <40 ppm slit-loss estimate is not an estimate of time-variable slit loss. It compares a monochromatic 10 micron stpsf PSF at the slit center with a single static offset of (3 sigma_x, 3 sigma_y) and quotes the 0.004% throughput difference. The quantity that matters for a time-series observation is the variation of transmitted flux along the actual pointing trajectory, which is controlled by the local slope of the slit transmission function at the realized, not assumed, centroid position. If the target is systematically offset from the slit center, small jitter can produce a first-order photometric modulation that the centered-versus-3-sigma comparison cannot bound. Please propagate the FGS centroid time series through the stpsf model, quote the wavelength dependence and uncertainty of the slit-loss prediction, and, if possible, check the prediction against the photometric residuals, for example by correlating residuals with FGS x/y positions.
  2. [Section 2.5] The unexplained wavelength-correlated noise above about 8 microns is a limitation the authors correctly identify, but its effect on the central feasibility claim is not quantified. The Gaussian process in the light-curve fits marginalizes over this noise, but that does not establish that the mode delivers precision suitable for science at those wavelengths; it only propagates the increased uncertainty into the retrieved parameters. For a mode-validation paper, please quantify the amplitude and timescale of the correlated noise in physical units, state the resulting degradation of achievable precision at wavelengths above 8 microns, or explicitly restrict the feasibility claim to the wavelengths for which the noise is not present.
minor comments (5)
  1. [Section 2.2] The text says the observation was taken 'as part of PID 6215', while the abstract and introduction identify the program as PID 6219; please correct the program ID.
  2. [Figure 2] The caption describes a transit observation over about 6 hours, while the text reports a 10.22 hour observation with a 2.33 hour transit; please clarify which interval is shown.
  3. [References] References [21] and [26] cite the same paper (Awesome SOSS) with slightly different formatting; please consolidate to a single entry.
  4. [Section 3] The phrase 'nearly saturated imager' is unexplained; please clarify or remove it, since a reader unfamiliar with the MIRI imager context will not know what is meant.
  5. [Figure 3 and Section 2.2.4] The statement that the two reductions are 'consistent within 1 sigma' should explicitly say that this refers to the two independent reductions of the same mode rather than to a comparison between slit and slitless modes, because Section 2.2.4 reports systematic offsets between the modes.

Circularity Check

0 steps flagged · score 0.0 of 10

No significant circularity: the slit-mode validation is an empirical, externally benchmarked demonstration, with no derived quantity defined in terms of its own target.

full rationale

The paper's central claim is that a single JWST/MIRI LRS slit transit observation of HAT-P-12b is feasible for precision time-series work. That claim is validated by comparing the new slit spectrum against archival slitless observations of the same target and by checking that two reduction routes agree within 1 sigma. Neither comparison defines the claimed result in terms of the inputs: the slit spectrum is a new measurement, the archival slitless data are re-reduced in this paper rather than merely cited, and the 7.5 micron feature is jointly fitted from both datasets. The slit-loss estimate in Section 2.3 is not circular either: the pointing dispersions sigma_x and sigma_y are measured FGS centroids, the PSF is generated with the external stpsf/WebbPSF tool, and the 40 ppm number is the throughput difference between a centered and a 3-sigma-offset static PSF. That is a simplified estimate and carries methodological risk, but it is not a fitted parameter renamed as a prediction. The same applies to the 38x background reduction, which is a direct comparison of measured background levels in the two configurations. Some citations are to work with overlapping authorship (notably PID 1281 and references 4-5), but the cited results are used as observational benchmarks and are re-analyzed here, so they are not load-bearing in a circular sense. The paper also self-identifies the main limitation, wavelength-correlated noise above about 8 microns, without using it to support the feasibility claim. Overall, no derivation chain reduces to its own inputs, and no prediction is defined in terms of its fitting target.

Assumptions & free parameters 4 free parameters · 4 assumptions · 0 invented entities

The paper introduces no new physical entities. Its central validation depends on standard observatory assumptions (pointing telemetry, PSF simulation, detector calibration corrections) and on several fitted nuisance parameters in the lightcurve systematics model. The 40 ppm slit-loss number is the most model-dependent quantitative claim.

free parameters (4)
  • per-lightcurve systematics coefficients = not tabulated
    Each binned lightcurve is fit with a linear trend, exponential ramp, and PSF position/width decorrelation terms, with a white-noise multiplier; transit depths depend on these nuisance fits.
  • Gaussian process hyperparameters (Matern-3/2 amplitude, timescale) = timescale approximately 1 minute
    Fitted per lightcurve to absorb residual red noise; the kernel choice is a modeling assumption, not derived from first principles.
  • orbital parameters P, a/R*, i, t0 = see Table 1
    Fitted jointly with normal priors from ref 11 and then fixed for spectroscopic fits; they carry prior information from ground-based ephemerides.
  • pointing offset multiplier for slit-loss simulation = 3 sigma
    Chosen as a conservative upper limit on pointing excursions; the 40 ppm figure is conditional on this choice and on a monochromatic 10 micrometer PSF simulation.
assumptions (4)
  • domain assumption FGS guide-star centroid variations represent the pointing of the MIRI science aperture over the full observation.
    Used in Section 2.3 to convert measured centroid dispersions into expected slit-loss variations; there is no independent check on the science-aperture pointing.
  • domain assumption The stpsf/WebbPSF model predicts the MIRI LRS slit PSF and throughput accurately enough to estimate slit losses.
    The 40 ppm prediction comes from these simulations; no absolute slit throughput measurement is reported for the TSO configuration.
  • domain assumption The custom BFE deconvolution correction removes the brighter-fatter effect without introducing wavelength-dependent bias.
    Invoked in Section 2.2.1; the reported offset in the first spectral channel suggests residual nonlinearity or BFE effects remain.
  • domain assumption A Matern-3/2 Gaussian process adequately models the time-correlated noise so that transit depths are unbiased.
    Used in Section 2.2.2; the paper reports residual correlations and notes the origin of the noise is unknown, so this assumption is not verified.

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Cite this review

Pith. "Pith review of A new window in time: a mid-infrared slit spectroscopy mode for precision time-series astronomy with JWST/MIRI." pith.science (2026). https://pith.science/paper/2GG4UTJK

@misc{pith2026260804110,
  author       = {Pith},
  title        = {Pith review of: A new window in time: a mid-infrared slit spectroscopy mode for precision time-series astronomy with JWST/MIRI},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/2GG4UTJK}},
  note         = {Machine review of arXiv:2608.04110}
}
read the original abstract

The Mid-Infrared Instrument (MIRI) on board the James Webb Space Telescope (JWST) provides Low Resolution Spectroscopy (LRS) over 5-12 um at a resolving power of R ~ 100. To date, all MIRI LRS time-series observations (TSOs) have been carried out in slitless mode, since long-duration pointing stability within the narrow 4.7'' x 0.51'' slit could not previously be guaranteed, leading to the possibility of degraded TSOs due to jitter. Commissioning activities established the telescope jitter to be less than 1 milliarcsecond (mas), four times less than the initial requirement. It was, therefore, worth assessing the suitability of the MIRI LRS slit as a TSO mode for precision time-domain science; this is the aim of the Cycle 3 program (PID 6219, PI: A. Dyrek). We observed a transit of the exoplanet HAT-P-12b over ~10 hours and compared the results to archival slitless observations of the same target (PID 1281, PI: P.-O. Lagage). Two independent data reductions of the transit spectra of both slit and slitless configurations are consistent within 1 sigma, validating the feasibility of the new mode. A joint fit of the slit and slitless observations confirms the presence of a spectral feature near 7.5 um. Using measured JWST pointing variations, we estimated slit-loss variations to be smaller than 40 ppm at 10 um. The drawback of the slitless mode is a higher background. Compellingly, the slit background is ~ 38 times lower on average than in slitless mode, improving sensitivity for faint targets (Jmag ~ 13-15). We also identified time-correlated noise unique to the slit dataset at long wavelengths, which requires further investigation. This new capability of TSOs in slit mode, which will be supported in Cycle 7 (in 2028), opens a new avenue for precision time-series astronomy for faint targets with JWST/MIRI.

Figures

Figures reproduced from arXiv: 2608.04110 by the authors.

Figure 1
Figure 1. MIRI detector showing the regions used for slitless and slit spectroscopy. The slitless spectral region reads out [PITH_FULL_IMAGE:figures/full_fig_p002_1.png] view at source ↗
Figure 2
Figure 2. Transit observation of the exoplanet HAT-P-12b over [PITH_FULL_IMAGE:figures/full_fig_p003_2.png] view at source ↗
Figure 3
Figure 3. Two independent data reductions of the first transit spectrum acquired in the slit mode of MIRI/LRS, showing [PITH_FULL_IMAGE:figures/full_fig_p006_3.png] view at source ↗
Figures from the paper (5 more)
Figure 4
Figure 4. Figure 4: Comparison of the transmission spectra of HAT-P-12b retrieved from the MIRI LRS slit (blue) and archival [PITH_FULL_IMAGE:figures/full_fig_p006_4.png]
Figure 5
Figure 5. Figure 5: Time series of the Fine Guidance Sensor (FGS) guide-star centroid positions during the [PITH_FULL_IMAGE:figures/full_fig_p007_5.png]
Figure 6
Figure 6. Figure 6: Simulated MIRI LRS point spread function at 10 [PITH_FULL_IMAGE:figures/full_fig_p008_6.png]
Figure 7
Figure 7. Figure 7: Median background values of all integrations for both slit and slitless datasets along the dispersion axis (5– [PITH_FULL_IMAGE:figures/full_fig_p009_7.png]
Figure 8
Figure 8. Figure 8: Correlation matrices of the residuals from the spectroscopic light-curve fit. [PITH_FULL_IMAGE:figures/full_fig_p009_8.png]

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Works this paper leans on

27 extracted references · 19 canonical work pages

  1. [1]

    The Mid-Infrared Instrument for the James Webb Space Telescope: IV. The Low Resolution Spectrometer,

    Kendrew, S., Scheithauer, S., Bouchet, P., Amiaux, J., Azzolini, R., Bouwman, J., Chen, C., Dubreuil, D., Fischer, S., Glasse, A., Greene, T., Lagage, P.-O., Lahuis, F., Ronayette, S., Wright, D., and Wright, G. S., “The Mid-Infrared Instrument for the James Webb Space Telescope: IV. The Low Resolution Spectrometer,” Publications of the Astronomical Socie...

    arXiv 2015

  2. [2]

    Spectroscopic time series performance of the Mid-Infrared Instrument on the JWST

    Bouwman, J., Kendrew, S., Greene, T. P., Bell, T. J., Lagage, P.-O., Schreiber, J., Dicken, D., Sloan, G. C., Espinoza, N., Scheithauer, S., Coulais, A., Fox, O. D., Gastaud, R., Glauser, A. M., Jones, O. C., Labiano, A., Lahuis, F., Morrison, J. E., Murray, K., Mueller, M., Nayak, O., Wright, G. S., Glasse, A., and Rieke, G., “Spectroscopic time series p...

    work page Pith review arXiv 2023

  3. [3]

    The Science Performance of JWST as Characterized in Commissioning,

    Rigby, J., Perrin, M., McElwain, M., Kimble, R., Friedman, S., Lallo, M., Doyon, R., Feinberg, L., Ferruit, P., Glasse, A., Rieke, M., Rieke, G., Wright, G., Willott, C., Colon, K., Milam, S., Neff, S., Stark, C., Valenti, J., Abell, J., Abney, F., Abul-Huda, Y., Scott Acton, D., Adams, E., Adler, D., Aguilar, J., Ahmed, N., Albert, L., Alberts, S., Aldri...

    work page 2023

  4. [4]

    Detection of CO$ 2$, CO, and H$ 2$O in the atmosphere of the warm sub-Saturn HAT-P-12b,

    Crouzet, N., Edwards, B., Konings, T., Bouwman, J., Min, M., Lagage, P.-O., Waters, L. B. F. M., Pye, J. P., Heinke, L., Guedel, M., Henning, T., Vandenbussche, B., Absil, O., Argyriou, I., Barrado, D., Boccaletti, A., Cossou, C., Coulais, A., Decin, L., Gastaud, R., Glasse, A., Glauser, A. M., Lahuis, F., Olofsson, G., Patapis, P., Rouan, D., Royer, P., ...

    arXiv 2025

  5. [5]

    Information content of JWST transmission spectroscopy of the exoplanet HAT-P-12b from the optical to the mid-infrared,

    Heinke, L., Min, M., Bouwman, J., Crouzet, N., Konings, T., Decin, L., Waters, L. B. F. M., Lagage, P.-O., Henning, T., Palmer, P. I., Edwards, B., Pye, J. P., G¨ udel, M., Absil, O., Barrado, D., Cossou, C., Glasse, A., Glauser, A. M., ¨Ostlin, G., Whiteford, N., and Ray, T. P., “Information content of JWST transmission spectroscopy of the exoplanet HAT-...

    arXiv 2026

  6. [6]

    Eureka!: An End-to-End Pipeline for JWST Time-Series Observations,

    Bell, T. J., Ahrer, E.-M., Brande, J., Carter, A. L., Feinstein, A. D., Caloca, G. G., Mansfield, M., Zieba, S., Piaulet, C., Benneke, B., Filippazzo, J., May, E. M., Roy, P.-A., Kreidberg, L., and Stevenson, K. B., “Eureka!: An End-to-End Pipeline for JWST Time-Series Observations,”Journal of Open Source Software7, 4503 (Nov. 2022). arXiv:2207.03585 [astro-ph]

    arXiv 2022

  7. [7]

    The Brighter-Fatter Effect in the JWST MIRI Si:As IBC detectors I. Observations, impact on science, and modelling,

    Argyriou, I., Lage, C., Rieke, G. H., Gasman, D., Bouwman, J., Morrison, J., Libralato, M., Dicken, D., Brandl, B. R., ´Alvarez M´ arquez, J., Labiano, A., Regan, M., and Ressler, M. E., “The Brighter-Fatter Effect in the JWST MIRI Si:As IBC detectors I. Observations, impact on science, and modelling,” (Mar. 2023). arXiv:2303.13517 [astro-ph]

    arXiv 2023

  8. [8]

    JWST Calibration Pipeline,

    Bushouse, H., Eisenhamer, J., Dencheva, N., Davies, J., Greenfield, P., Morrison, J., Hodge, P., Simon, B., Grumm, D., Droettboom, M., Slavich, E., Sosey, M., Pauly, T., Miller, T., Jedrzejewski, R., Hack, W., Davis, D., Crawford, S., Law, D., Gordon, K., Regan, M., Cara, M., MacDonald, K., Bradley, L., Shanahan, C., Jamieson, W., Teodoro, M., Williams, T...

    work page 2025

Show all 27 references
  1. [9]

    Exploring the Brighter- fatter Effect with the Hyper Suprime-Cam,

    Coulton, W. R., Armstrong, R., Smith, K. M., Lupton, R. H., and Spergel, D. N., “Exploring the Brighter- fatter Effect with the Hyper Suprime-Cam,”The Astronomical Journal155, 258 (June 2018)

    2018

  2. [10]

    An optimal extraction algorithm for ccd spectroscopy.,

    Horne, K., “An optimal extraction algorithm for ccd spectroscopy.,”Publications of the Astronomical Society of the Pacific98, 609–617 (June 1986)

    1986

  3. [11]

    ExoClock Project. III. 450 New Exoplanet Ephemerides from Ground and Space Observations,

    Kokori, A., Tsiaras, A., Edwards, B., Jones, A., Pantelidou, G., Tinetti, G., Bewersdorff, L., Iliadou, A., Jongen, Y., Lekkas, G., Nastasi, A., Poultourtzidis, E., Sidiropoulos, C., Walter, F., W¨ unsche, A., Abraham, R., Agnihotri, V. K., Albanesi, R., Arce-Mansego, E., Arno...

    2023

  4. [12]

    batman: BAsic Transit Model cAlculatioN in Python,

    Kreidberg, L., “batman: BAsic Transit Model cAlculatioN in Python,”Publications of the Astronomical Society of the Pacific127, 1161–1165 (Nov. 2015). arXiv:1507.08285 [astro-ph]

    2015 arXiv

  5. [13]

    Fast and Scalable Gaussian Process Modeling with Applications to Astronomical Time Series,

    Foreman-Mackey, D., Agol, E., Ambikasaran, S., and Angus, R., “Fast and Scalable Gaussian Process Modeling with Applications to Astronomical Time Series,”The Astronomical Journal154, 220 (Dec. 2017)

    2017

  6. [14]

    Scalable Backpropagation for Gaussian Processes using Celerite,

    Foreman-Mackey, D., “Scalable Backpropagation for Gaussian Processes using Celerite,”Research Notes of the American Astronomical Society2, 31 (Feb. 2018)

    2018

  7. [15]

    dynesty: A Dynamic Nested Sampling Package for Estimating Bayesian Posteriors and Evi- dences,

    Speagle, J. S., “dynesty: A Dynamic Nested Sampling Package for Estimating Bayesian Posteriors and Evi- dences,”Monthly Notices of the Royal Astronomical Society493, 3132–3158 (Apr. 2020). arXiv:1904.02180 [astro-ph, stat]

    2020 arXiv

  8. [16]

    The stagger-grid: A grid of 3d stellar atmosphere models-iv. limb darkening coefficients,

    Magic, Z., Chiavassa, A., Collet, R., and Asplund, M., “The stagger-grid: A grid of 3d stellar atmosphere models-iv. limb darkening coefficients,”Astronomy & Astrophysics573, A90 (2015)

    2015

  9. [17]

    Exotic-ld: thirty seconds to stellar limb-darkening coefficients,

    Grant, D. and Wakeford, H. R., “Exotic-ld: thirty seconds to stellar limb-darkening coefficients,”Journal of Open Source Software9(100), 6816 (2024)

    2024

  10. [18]

    The Revised TESS Input Catalog and Candidate Target List,

    Stassun, K. G., Oelkers, R. J., Paegert, M., Torres, G., Pepper, J., De Lee, N., Collins, K., Latham, D. W., Muirhead, P. S., Chittidi, J., Rojas-Ayala, B., Fleming, S. W., Rose, M. E., Tenenbaum, P., Ting, E. B., Kane, S. R., Barclay, T., Bean, J. L., Brassuer, C. E., Charbon...

    2019

  11. [19]

    Insufficient evidence for DMS and DMDS in the atmosphere of K2-18 b: From a joint analysis of JWST NIRISS, NIRSpec, and MIRI observations,

    Luque, R., Piaulet-Ghorayeb, C., Radica, M., Xue, Q., Zhang, M., Bean, J. L., Samra, D., and Steinrueck, M. E., “Insufficient evidence for DMS and DMDS in the atmosphere of K2-18 b: From a joint analysis of JWST NIRISS, NIRSpec, and MIRI observations,”Astronomy & Astrophysics7...

    2025

  12. [20]

    exoTEDRF: An EXOplanet Transit and Eclipse Data Reduction Framework,

    Radica, M., “exoTEDRF: An EXOplanet Transit and Eclipse Data Reduction Framework,”The Journal of Open Source Software9, 6898 (Aug. 2024). ADS Bibcode: 2024JOSS....9.6898R

    2024

  13. [21]

    Awesome SOSS: transmission spectroscopy of WASP-96b with NIRISS/SOSS,

    Radica, M., Welbanks, L., Espinoza, N., Taylor, J., Coulombe, L.-P., Feinstein, A. D., Goyal, J., Scarsdale, N., Albert, L., Baghel, P., Bean, J. L., Blecic, J., Lafreni` ere, D., MacDonald, R. J., Zamyatina, M., Allart1, R., Artigau, ´E., Batalha, N. E., Cook, N. J., Cowan, N...

    2023

  14. [22]

    Early Release Science of the exoplanet WASP-39b with JWST NIRISS,

    Feinstein, A. D., Radica, M., Welbanks, L., Murray, C. A., Ohno, K., Coulombe, L.-P., Espinoza, N., Bean, J. L., Teske, J. K., Benneke, B., Line, M. R., Rustamkulov, Z., Saba, A., Tsiaras, A., Barstow, J. K., Fortney, J. J., Gao, P., Knutson, H. A., MacDonald, R. J., Mikal-Eva...

    2023

  15. [23]

    ExoIris: Fast Exoplanet Transmission Spectroscopy in Python,

    Parviainen, H., “ExoIris: Fast Exoplanet Transmission Spectroscopy in Python,”The Astrophysical Jour- nal171, 237 (Apr. 2026)

    2026

  16. [24]

    Updated point spread function simulations for JWST with WebbPSF,

    Perrin, M. D., Sivaramakrishnan, A., Lajoie, C.-P., Elliott, E., Pueyo, L., Ravindranath, S., and Albert, L., “Updated point spread function simulations for JWST with WebbPSF,” 91433X (Aug. 2014)

    2014

  17. [25]

    Exoplanet Spectroscopy with JWST NIRISS: Diagnostics and Case Studies,

    Holmberg, M. and Madhusudhan, N., “Exoplanet Spectroscopy with JWST NIRISS: Diagnostics and Case Studies,”Monthly Notices of the Royal Astronomical Society524, 377–402 (July 2023). arXiv:2306.04676 [astro-ph.EP]

    2023 arXiv

  18. [26]

    Awesome SOSS: transmission spectroscopy of WASP-96b with NIRISS/SOSS,

    Radica, M., Welbanks, L., Espinoza, N., Taylor, J., Coulombe, L.-P., Feinstein, A. D., Goyal, J., Scarsdale, N., Albert, L., Baghel, P., Bean, J. L., Blecic, J., Lafreni` ere, D., MacDonald, R. J., Zamyatina, M., Allart1, R., Artigau, E., Batalha, N. E., Cook, N. J., Cowan, N....

    2023

  19. [27]

    MIRI-LRS Spectrum of a Cold Exoplanet around a White Dwarf: Water, Ammonia, and Methane Measurements,

    Voyer, M., Changeat, Q., Lagage, P.-O., Tremblin, P., Waters, R., G¨ udel, M., Henning, T., Absil, O., Barrado, D., Boccaletti, A., Bouwman, J., Coulais, A., Decin, L., Glauser, A. M., Pye, J., Glasse, A., Gastaud, R., Kendrew, S., Patapis, P., Rouan, D., van Dishoeck, E. F., ...

    2025

Pith tools

Reviewed August 15, 2026 · model on record in the stance chip above.