adsabs/AstroCLIMB huggingface dataset:
Paper: Langmuir-wave Excitation in Solar Wind Magnetic Holes
Authors: Jingting Liu, 婧婷 刘, Daniel Verscharen, Jesse Coburn, Georgios Nicolaou, Xiangyu Wu, 翔宇 吴, Wence Jiang, 文策 蒋, Oreste Pezzi, Francesco Pucci, Matteo Zuin, Christopher J. Owen, Hamish Reid
Figure caption: Electron VDFs at three characteristic phases for case 1: (left) before the strahl population enters the MH, (center) at the time of the recorded minimum magnetic field strength with the loss-cone angle indicated by black dashed lines, and (right) after the strahl population exits the MH. The corresponding times in UT (hh:mm:ss) are indicated above each panel. The angles indicate the pitch angle ϕ.
Paper: Langmuir-wave Excitation in Solar Wind Magnetic Holes
Authors: Jingting Liu, 婧婷 刘, Daniel Verscharen, Jesse Coburn, Georgios Nicolaou, Xiangyu Wu, 翔宇 吴, Wence Jiang, 文策 蒋, Oreste Pezzi, Francesco Pucci, Matteo Zuin, Christopher J. Owen, Hamish Reid
Figure caption: Solar Orbiter observations of an MH on 2022 January 2 from 00:20:00 UT to 00:30:00 UT (case 1). The horizontal axis shows the time in UT (hh:mm). (a) Magnetic field strength B in green and electron number density ne in blue. (b) Components of the magnetic field in RTN coordinates, where R is the radial direction, T is the tangential direction, and N completes the right-handed triad. (c) Electron pitch-angle distribution of electrons from 69 eV to 2000 eV. (d) Electron pitch-angle distribution from 1000 eV to 1500 eV. The blue and olive colored dots indicate angles beyond which Equations (9) and (12) are violated for E = Ecrit = 1130 eV. (e) Dynamic spectrum of wave flux vs. time in spectral flux units. (f) Illustration of a possible magnetic field configuration based on a feather plot of our in situ magnetic field measurements. In this panel, time is displayed in hh:mm:ss format.
Paper: Langmuir-wave Excitation in Solar Wind Magnetic Holes
Authors: Jingting Liu, 婧婷 刘, Daniel Verscharen, Jesse Coburn, Georgios Nicolaou, Xiangyu Wu, 翔宇 吴, Wence Jiang, 文策 蒋, Oreste Pezzi, Francesco Pucci, Matteo Zuin, Christopher J. Owen, Hamish Reid
Figure caption: Electron VDFs at three characteristic phases for case 2: (left) before the strahl population enters the MH, (center) at the time of the recorded minimum magnetic field strength with the loss-cone angle indicated by black dashed lines, and (right) after the strahl population exits the MH. The corresponding times in UT (hh:mm:ss) are indicated above each panel. The angles indicate the pitch angle ϕ.
Paper: Langmuir-wave Excitation in Solar Wind Magnetic Holes
Authors: Jingting Liu, 婧婷 刘, Daniel Verscharen, Jesse Coburn, Georgios Nicolaou, Xiangyu Wu, 翔宇 吴, Wence Jiang, 文策 蒋, Oreste Pezzi, Francesco Pucci, Matteo Zuin, Christopher J. Owen, Hamish Reid
Figure caption: Left: LW dispersion relation from Equation (1) for case 1. We overplot the resonance condition ω = k∥v∥,crit for Ecrit = 1130 eV in orange. The purple line shows ω = k∥vthr. Right: triggered snapshot waveform from the RPW-TDS instrument, data captured at 00:24:52.79 UT on 2022 January 2 (case 1). EYSRF and EZSRF represent the electric field components measured along the Y- and Z-axes in the spacecraft reference frame.
Paper: Langmuir-wave Excitation in Solar Wind Magnetic Holes
Authors: Jingting Liu, 婧婷 刘, Daniel Verscharen, Jesse Coburn, Georgios Nicolaou, Xiangyu Wu, 翔宇 吴, Wence Jiang, 文策 蒋, Oreste Pezzi, Francesco Pucci, Matteo Zuin, Christopher J. Owen, Hamish Reid
Figure caption: Left: LW dispersion relation from Equation (1) for case 2. We overplot the resonance condition ω = k∥v∥,crit for Ecrit = 150 eV in orange. The purple line shows ω = k∥vthr. Right: triggered snapshot waveform from the RPW-TDS instrument, data captured at 08:01:45.84 UT on 2022 January 2 (case 2). EYSRF and EZSRF represent the electric field components measured along the Y- and Z-axes in the spacecraft reference frame.
Paper: JWST’s First View of Tidal Disruption Events: Compact, Accretion-driven Emission Lines and Strong Silicate Emission in an Infrared-selected Sample
Authors: Megan Masterson, Kishalay De, Christos Panagiotou, Erin Kara, Wenbin Lu, Anna-Christina Eilers, Muryel Guolo, Armin Rest, Claudio Ricci, Sjoert van Velzen
Figure caption: JWST MIRI/MRS nuclear spectra, extracted from within 1 FWHM of the PSF. The four sources in our sample are shown in various shades of blue, varying from darkest for the earliest TDE to lightest for the most recent TDE. The wavelengths of key high- and low-IP lines are shown in dark and light green, respectively, where we define the threshold energy between high and low IP at 40 eV. The molecular H2 lines are also labeled on top in red. The locations of key silicate features and PAHs are shown in dark and light purple, respectively. All four sources show strong silicate emission at around 10 and 18 μm, significant emission from the high-IP lines associated with black hole accretion, and some, but relatively weak, PAH features.
Paper: XRISM Spectroscopy of the Stellar-mass Black Hole 4U 1630-472 in Outburst
Authors: Jon M. Miller, Misaki Mizumoto, Megumi Shidatsu, Ralf Ballhausen, Ehud Behar, María Díaz Trigo, Chris Done, Tadayasu Dotani, Javier A. García, Timothy Kallman, Shogo B. Kobayashi, Aya Kubota, Randall Smith, Hiromitsu Takahashi, Makoto Tashiro, Yoshihiro Ueda, Jacco Vink, Shinya Yamada, Shin Watanabe, Ryo Iizuka, Yukikatsu Terada, Chris Baluta, Yoshiaki Kanemaru, Shoji Ogawa, Tessei Yoshida, Katsuhiro Hayashi
Figure caption: Resolve spectra of 4U 1630−472 obtained from the initial “steady” flux phase of the observation and the later “dip” phase. The spectra are dominated by narrow He-like Fe XXV and H-like Fe XXVI absorption lines. In both phases, the best-fit “pion” photoionization model is shown in red; it includes four independent absorption and reemission zones. In each panel, the best fit to the complementary phase is indicated with a dashed blue line. The phases are primarily distinguished by a sharp increase in absorption that cannot be accounted for only through a change in luminosity and corresponding change in ionization. The spectra were binned using the “optimal binning” algorithm and are shown at the same resolution. Please see the text and subsequent figures for additional details.
Paper: XRISM Spectroscopy of the Stellar-mass Black Hole 4U 1630-472 in Outburst
Authors: Jon M. Miller, Misaki Mizumoto, Megumi Shidatsu, Ralf Ballhausen, Ehud Behar, María Díaz Trigo, Chris Done, Tadayasu Dotani, Javier A. García, Timothy Kallman, Shogo B. Kobayashi, Aya Kubota, Randall Smith, Hiromitsu Takahashi, Makoto Tashiro, Yoshihiro Ueda, Jacco Vink, Shinya Yamada, Shin Watanabe, Ryo Iizuka, Yukikatsu Terada, Chris Baluta, Yoshiaki Kanemaru, Shoji Ogawa, Tessei Yoshida, Katsuhiro Hayashi
Figure caption: Resolve spectra of 4U 1630−472 in the Fe K band and separated by flux interval. In both phases, the best-fit “pion” photoionization model is shown in red; it includes four independent absorption and reemission zones. In each panel, the best fit to the complementary phase is indicated with a dashed blue line. Line identifications are indicated between the panels, with dashed gray lines indicating the expected rest-frame laboratory energy. The low flux phase includes a zone with strong Fe XXV Heα, -β, and -γ lines (the mid-ξ zone in Table 1). Note that the H-like Fe XXVI complex varies little between the phases (the high-ξ zone in Table 1). The feature at 7.15 keV likely represents Fe XXVI absorption shifted by v = −0.027c (the UFO zone in Table 1); dust absorption and other alternatives are statistically disfavored. The spectra were binned using the “optimal binning” algorithm, but additional binning is adopted above 7 keV in this figure for visual clarity. Please see the text for additional details.
Paper: XRISM Spectroscopy of the Stellar-mass Black Hole 4U 1630-472 in Outburst
Authors: Jon M. Miller, Misaki Mizumoto, Megumi Shidatsu, Ralf Ballhausen, Ehud Behar, María Díaz Trigo, Chris Done, Tadayasu Dotani, Javier A. García, Timothy Kallman, Shogo B. Kobayashi, Aya Kubota, Randall Smith, Hiromitsu Takahashi, Makoto Tashiro, Yoshihiro Ueda, Jacco Vink, Shinya Yamada, Shin Watanabe, Ryo Iizuka, Yukikatsu Terada, Chris Baluta, Yoshiaki Kanemaru, Shoji Ogawa, Tessei Yoshida, Katsuhiro Hayashi
Figure caption: Resolve spectra of 4U 1630−472 in a low-energy band and separated by flux interval. In both flux phases, the best-fit “pion” photoionization model is shown in red; it includes four independent absorption and reemission zones. In each panel, the best fit to the complementary phase is indicated with a dashed blue line. Line identifications are indicated between the panels, with dashed gray lines indicating the expected rest-frame laboratory energy. The spectra were binned using the “optimal binning” algorithm, but additional binning is adopted in this figure for visual clarity. Please see the text for additional details.
Paper: XRISM Spectroscopy of the Stellar-mass Black Hole 4U 1630-472 in Outburst
Authors: Jon M. Miller, Misaki Mizumoto, Megumi Shidatsu, Ralf Ballhausen, Ehud Behar, María Díaz Trigo, Chris Done, Tadayasu Dotani, Javier A. García, Timothy Kallman, Shogo B. Kobayashi, Aya Kubota, Randall Smith, Hiromitsu Takahashi, Makoto Tashiro, Yoshihiro Ueda, Jacco Vink, Shinya Yamada, Shin Watanabe, Ryo Iizuka, Yukikatsu Terada, Chris Baluta, Yoshiaki Kanemaru, Shoji Ogawa, Tessei Yoshida, Katsuhiro Hayashi
Figure caption: The fractional importance of different photoionization zones in our best-fit model, relative to the local continuum flux. The zones correspond to those detailed in Table 1. Small vertical offsets were enforced to improve clarity in crowded regions. The strong variation in the “mid-ξ” absorber is also evident in the prior figure and may signal that an axially asymmetric geometry passed into the line of sight.
Paper: XRISM Spectroscopy of the Stellar-mass Black Hole 4U 1630-472 in Outburst
Authors: Jon M. Miller, Misaki Mizumoto, Megumi Shidatsu, Ralf Ballhausen, Ehud Behar, María Díaz Trigo, Chris Done, Tadayasu Dotani, Javier A. García, Timothy Kallman, Shogo B. Kobayashi, Aya Kubota, Randall Smith, Hiromitsu Takahashi, Makoto Tashiro, Yoshihiro Ueda, Jacco Vink, Shinya Yamada, Shin Watanabe, Ryo Iizuka, Yukikatsu Terada, Chris Baluta, Yoshiaki Kanemaru, Shoji Ogawa, Tessei Yoshida, Katsuhiro Hayashi
Figure caption: The ratio of the “steady” flux and “dip” intervals to the continuum, without modeling the absorption. In this model-independent representation, the velocity shift in the “high-ξ” zone (dominated by H-like Fe XXVI, a doublet centered at 6.97 keV) is clear. Our best-fit model measures a small but significant blueshift in the “steady flux” phase, v = −130 ± 30 km s−1, and a small but significant redshift in the “dip” phase, v = 220 ± 30 km s−1 (see Table 1). The data are shown with “optimal” binning.
Paper: XRISM Spectroscopy of the Stellar-mass Black Hole 4U 1630-472 in Outburst
Authors: Jon M. Miller, Misaki Mizumoto, Megumi Shidatsu, Ralf Ballhausen, Ehud Behar, María Díaz Trigo, Chris Done, Tadayasu Dotani, Javier A. García, Timothy Kallman, Shogo B. Kobayashi, Aya Kubota, Randall Smith, Hiromitsu Takahashi, Makoto Tashiro, Yoshihiro Ueda, Jacco Vink, Shinya Yamada, Shin Watanabe, Ryo Iizuka, Yukikatsu Terada, Chris Baluta, Yoshiaki Kanemaru, Shoji Ogawa, Tessei Yoshida, Katsuhiro Hayashi
Figure caption: The Resolve image in the detector coordinates. We do not use pixels 5, 23, 29, and 30 due to pseudo-Ls event pollution or pixel 27 due to the possible temperature jump.
Paper: XRISM Spectroscopy of the Stellar-mass Black Hole 4U 1630-472 in Outburst
Authors: Jon M. Miller, Misaki Mizumoto, Megumi Shidatsu, Ralf Ballhausen, Ehud Behar, María Díaz Trigo, Chris Done, Tadayasu Dotani, Javier A. García, Timothy Kallman, Shogo B. Kobayashi, Aya Kubota, Randall Smith, Hiromitsu Takahashi, Makoto Tashiro, Yoshihiro Ueda, Jacco Vink, Shinya Yamada, Shin Watanabe, Ryo Iizuka, Yukikatsu Terada, Chris Baluta, Yoshiaki Kanemaru, Shoji Ogawa, Tessei Yoshida, Katsuhiro Hayashi
Figure caption: The Resolve light curve of 4U 1630−472 in the 2–10 keV band, with 256 s bins. The dashed horizontal red lines in each panel show the mean count rate prior to t = 60,000 s. The solid vertical line in each panel marks the point at which the spectra are divided into “steady” flux and “dip” phases.
Paper: High-resolution Observations of an X6.4 Solar Flare in the Mid-infrared
Authors: Xu Yang, Wenda Cao, Meiqi Wang, Don Jennings, Jiong Qiu, Wen He, Solomon M. Perriyil, Vasyl Yurchyshyn, Lyndsay Fletcher, Paulo J. A. Simões, Murzy Jhabvala, Allen Lunsford, Xingyao Chen, Hugh Hudson
Figure caption: Magnetic field extrapolations and analysis of the UN source. Panels (a1) and (a2) plot magnetic field lines from the CESE-MHD-NLFFF extrapolation over deprojected AIA 94 Å and HMI/Ic images at 22:10 UT. Panels (b1) and (b2) plot STIX/HXR (blue, 28–50 keV) and EOVSA microwave-low-frequency (green, 4–7 GHz) and microwave-high-frequency (orange, 7.4–9.1 GHz) contours over AIA 94 Å and HMI/Ic images at 22:28:12 UT. Panels (c1) and (c2) propose two source distribution speculations for microwave and HXR emissions, with orange solid lines indicating the speculated magnetic loop configurations. Panels (d1) and (d2) modeled brightness temperature Tb at 8.2 μm vs. electron density ne for two slab depths (L = 107, 108 cm), at temperatures ranging from 105 to 107 K. The horizontal black dotted line marks the required 336 K brightness temperature excess (7% brightening).
Paper: High-resolution Observations of an X6.4 Solar Flare in the Mid-infrared
Authors: Xu Yang, Wenda Cao, Meiqi Wang, Don Jennings, Jiong Qiu, Wen He, Solomon M. Perriyil, Vasyl Yurchyshyn, Lyndsay Fletcher, Paulo J. A. Simões, Murzy Jhabvala, Allen Lunsford, Xingyao Chen, Hugh Hudson
Figure caption: Evolution of the UN. Panels (a1)–(a7) present AIA 94 Å reversed grayscale images showing hot flare loop emission moving toward flare ribbon R3 (cyan contours). Magenta contours mark emission from the UN source (3% enhanced intensity relative to quiet-Sun area) from the MIRI 8.2 μm channel. Two streams (S1 and S2) are resolved in panel (a6). Panel (b) presents AIA 1600 Å image at the same time as in panel (a3). Panel (c) presents a time-distance map along Pa-Pb from AIA 94 Å channel. The black dashed lines in panel (c) indicate 22:27:35 and 22:30:47 UT, respectively.
Paper: High-resolution Observations of an X6.4 Solar Flare in the Mid-infrared
Authors: Xu Yang, Wenda Cao, Meiqi Wang, Don Jennings, Jiong Qiu, Wen He, Solomon M. Perriyil, Vasyl Yurchyshyn, Lyndsay Fletcher, Paulo J. A. Simões, Murzy Jhabvala, Allen Lunsford, Xingyao Chen, Hugh Hudson
Figure caption: Flare light-curves (LCs) in multiple wavelengths. Panel (a) plots the high-energy HXR (red: 32–50 keV; cyan: 50–76 keV) and high-frequency microwave (magenta: 12.3 GHz) Panels (b)–(f) plot LCs of AIA 94 Å (green), 1600 Å (orange), HMI/Ic (red), and MIRI/8.2 μm (blue) integrated over the selected areas. The baseline intensity for each wavelength is defined as the average during 22:22:00–22:23:00 UT. AIA 94 and 1600 Å LCs are normalized to their base intensity levels. HMI/Ic and MIRI/8.2 μm LCs are presented as percentage deviations from their baseline levels. The shaded regions in panels (b)–(f) mark a weather-impacted period (22:29:06–22:30:01 UT) of relatively low data quality.
Paper: A Plasma Torus around a Young Low-mass Star
Authors: Luke G. Bouma, Moira M. Jardine
Figure caption: Photometric evolution of TIC 141146667 around the Keck/HIRES observation (green bar). (a) TESS simple aperture photometry. Data gaps were caused by stray light from Earth (BTJD 3356–3358.5) and the Moon (BTJD 3359.5–3360.5). Raw 2-minute data are in gray; black time-averages to 10-minute sampling. (b–c) Folded TESS light curve before and after spectroscopy. Black now phase-averages to 100 points per 3.93 hr cycle. During BTJD 3352–3356, a state switch occurred near BTJD 3353, and the dip at ϕ  ≈ 0.8 became less pronounced. While the dip spanning ϕ = 0.6–1.1 was present both before and after the HIRES sequence, its photometric shape evolved during the data gap. The orange bar denotes times of spectroscopic transits for the inner two Hα clumps observed with HIRES (see Figure 3).
Paper: Constraining Ongoing Volcanic Outgassing Rates and Interior Compositions of Extrasolar Planets with Mass Measurements of Plasma Tori
Authors: V. Abby Boehm, Darryl Z. Seligman, Nikole K. Lewis
Figure caption: B* and ﹩{\dot{M}}_{{\rm{wind}}}﹩ priors and the resultant RA posterior for GJ 367 A (R* = 0.458 R⊕, v∞ ≃ 616 km s−1; E. Goffo et al. 2023). Left: lognormal prior for B*. As an M dwarf star with P* = 51.3 days, the most probable value of the magnetic field strength for GJ 367 A is ﹩{B}_{* }=20{0}_{-100}^{+200}﹩ G (L. T. Lehmann et al. 2024). Middle: lognormal prior for ﹩\mathrm{log}({\dot{M}}_{\mathrm{wind}}[{M}_{\odot }\,{\mathrm{yr}}^{-1}])﹩. The measured X-ray flux of GJ 367 A (K. Poppenhaeger et al. 2024) and likely B* ≃ 200 G suggest a most likely stellar wind mass-loss rate of ﹩\mathrm{log}({\dot{M}}_{\mathrm{wind}}[{M}_{\odot }\,{\mathrm{yr}}^{-1}])\,=-14\pm 0.3﹩ and disfavors loss rates greater than 10−13 M⊙ yr−1 (S. Bloot et al. 2025). Right: the resultant posterior distribution of the Alfvén radius. The expected Alfvén radius in stellar radii is ﹩16.{7}_{-5.3}^{+8.6}﹩, equivalent to an orbit distance of about 0.035 au.
Paper: Responses of a Coronal Hole to a Fast Flare-driven Coronal Wave
Authors: Xiaofan Zhang, Huadong Chen, Guiping Zhou, Li Feng, Yang Su, Jinhan Guo, Leping Li, Wei Lin, Suli Ma, Yuandeng Shen, Ruisheng Zheng, Suo Liu, Xianyong Bai, Yuanyong Deng, Jingxiu Wang
Figure caption: Time profiles of essential parameters were analyzed to understand the dynamics within the CH. In panels (a1)–(a3), the evolution of EM (black curves) and the electron number density (ne, blue curves) with 1σ uncertainties are depicted. Panels (b1)–(b3) display the DEM-weighted mean temperature (T, gray curves) with 1σ uncertainties, the adiabatic temperature (black dashed curves) and radiative loss rates Λ(T) (blue curves). Moving to panels ((c1)–(c3)), thermal energy per unit area (Et, black curves), radiative loss flux (Fr, blue curves), and heat conduction flux (Fc, green curves) with 1σ uncertainties are illustrated. These profiles are generated for three distinct regions: the CH area (panels (a1)–(c1)), the northern boundary of the CH (panels (a2)–(c2)), and the primary part of the CH excluding the northern boundary (panels (a3)-(c3)). In the top two rows, three vertical dashed lines in each panel signify the onset, peak, and minimum decay points for the varying EM and T. The x-axis represents time, while the y-axes display the values of the respective parameters.
Paper: Responses of a Coronal Hole to a Fast Flare-driven Coronal Wave
Authors: Xiaofan Zhang, Huadong Chen, Guiping Zhou, Li Feng, Yang Su, Jinhan Guo, Leping Li, Wei Lin, Suli Ma, Yuandeng Shen, Ruisheng Zheng, Suo Liu, Xianyong Bai, Yuanyong Deng, Jingxiu Wang
Figure caption: Multiwavelength observations revealing the flare-associated coronal wave and its sweeping region. Panel (a) displays an HMI image at 20:58 UT on December 31, showcasing AR13536 in N05E75, a nearby PIL indicated by a white dashed line, and the examined CH with predominantly positive polarity outlined by yellow contours. In panel (b), an image at 1216 Å from the LST illustrates the flare progression observed in Lyα. Panel (c) presents a subset of panel (b) enclosed in a white box, superimposed with HXR contours representing energy ranges of 15–20 and 30–50 keV, respectively. Within the Chase/HIS observations depicted in panel (d), a long filament (indicated by a black dashed line) runs along the PIL. Panel (e) exhibits an EUV image at 193 Å from AIA, revealing the flare activity in AR13536 and outlining the CH with yellow contours. The wave potentially accumulates at the CH boundary during its propagation, as evidenced by the difference image between 21:54 and 21:24 UT in 211 Å . Panel (g) showcases the X5 flaring process captured through the GOES SXR flux. The contours in panels ((a), (d), and (e)) represent positive (red/white) and negative flux densities (cyan/black) at ±15 G, respectively.
Paper: Responses of a Coronal Hole to a Fast Flare-driven Coronal Wave
Authors: Xiaofan Zhang, Huadong Chen, Guiping Zhou, Li Feng, Yang Su, Jinhan Guo, Leping Li, Wei Lin, Suli Ma, Yuandeng Shen, Ruisheng Zheng, Suo Liu, Xianyong Bai, Yuanyong Deng, Jingxiu Wang
Figure caption: Two types of coronal waves illustrated in the time–distance maps along the slice “S1–S2” as depicted in Figure 2(d). The slice crosses the boundary of the CH twice, marked as “b1” and “b2.” These two modes of coronal waves propagated over the CH, with velocities of 948 and 466 km s−1 based on linear fitting. The positions of the CH boundary are indicated by two yellow horizontal dashed lines.
Paper: A Disintegrating Rocky World Shrouded in Dust and Gas: Mid-infrared Observations of K2-22 b Using JWST
Authors: Nick Tusay, Jason T. Wright, Thomas G. Beatty, Steve Desch, Knicole Colón, Tushar Mittal, Hugh P. Osborn, Beatriz Campos Estrada, James E. Owen, Jessica Libby-Roberts, Arvind F. Gupta, Brad Foley, Erik Meier Valdés, Daniel J. Stevens, Ashley Herbst
Figure caption: Results from JWST Cycle 2 GO Program 3315.Top: lightcurve of the second half of the phase curve, collected on 2024 April 28, showing a clear transit at the predicted ephemeris. The unbinned time series data (at a cadence of 72 s) is plotted in gray in the background. The blue points are binned to a time resolution of 8 minutes. The average 46 minute duration drawn from R. Sanchis-Ojeda et al. (2015) is shown as vertical dashed gray lines for reference. Since the transit duration incorporating the cloud of material is not precisely known and potentially variable with wavelength, the baseline flux was calculated from data outside the baseline boundaries set at 1.5× the average 46 minute duration, centered at the ephemeris and shown as vertical dashed green lines. The red line is a second-order polynomial model fit to the data during transit and set to zero elsewhere. The residuals of the lightcurve model are shown in the bottom panel.Middle: JWST MIRI spectrum showing a clear detection of a transit from 4.4 to 8 μm except at 4.8 μm. A flat spectrum is disfavored (reduced ﹩{\chi }_{\nu }^{2}=3.56﹩). The unbinned JWST data for each channel are plotted in gray in the background. The binned JWST spectrum in the foreground has a constant spectral resolution of R = 17. The horizontal red dashed line shows the overall transit depth from the MIRI lightcurve in the top panel. The dotted curves show the spectral models of plausible gas species from the DACE database (S. L. Grimm et al. 2021). The dashed curves show representative combinations of iron, magnesium, and silicate species predicted by E. H. Bodman et al. (2018) and B. Campos Estrada et al. (2024). The solid purple line shows a total opacity model representing a combination of these minerals and gases with features that plausibly correspond to features in the data. CHEOPS photometry is also shown over its 0.33–1.1 μm bandpass. The measured CHEOPS transit depth is consistent with the overall transit depth from the MIRI lightcurve.Bottom insets: the lightcurve and transit models in two channels that illustrate an unexpected spectral feature with the most significance at ∼5 μm. The unexpected feature at 5.1 μm, consistent with nitric oxide (NO) gas is clearly detected, in contrast to a clear nondetection at 4.8 μm (see Figure 4).