adsabs/AstroCLIMB huggingface dataset:
Paper: Disk in the Circumstellar Envelope of Carbon Mira V Cygni
Authors: Boris S. Safonov, Sergey G. Zheltoukhov, Andrey M. Tatarnikov, Ivan A. Strakhov, Victor I. Shenavrin
Figure caption: Approximation of SED. (a) Red squares represent the observed SED, while the black line shows the optimal model (corresponding to the median value of θ, as discussed in Section 5.2.2). (b) Residuals R. The thick black line represents the optimal model, and the thin colored lines show a subsample of models drawn from the posterior distribution of θ. (c) Residual correlation. The blue line indicates the observed correlation, and the red line represents the model (14) with parameters σ0 = 0.020, σc = 0.71, l = 0.060, as determined in Section 5.2.2.
Paper: Disk in the Circumstellar Envelope of Carbon Mira V Cygni
Authors: Boris S. Safonov, Sergey G. Zheltoukhov, Andrey M. Tatarnikov, Ivan A. Strakhov, Victor I. Shenavrin
Figure caption: Lower part: JHKLM light curves. Upper part: color indices J − K, L − M. Short vertical lines above the horizontal axis indicate the moments of spectral observations.
Paper: Disk in the Circumstellar Envelope of Carbon Mira V Cygni
Authors: Boris S. Safonov, Sergey G. Zheltoukhov, Andrey M. Tatarnikov, Ivan A. Strakhov, Victor I. Shenavrin
Figure caption: (a) Thinning mask in the Fourier space; the brightness is proportional to the logarithm of weight. (b) Covariance matrix for DPV noise. (c) Logarithm of the inverse of the covariance matrix for DPV noise.
Paper: Disk in the Circumstellar Envelope of Carbon Mira V Cygni
Authors: Boris S. Safonov, Sergey G. Zheltoukhov, Andrey M. Tatarnikov, Ivan A. Strakhov, Victor I. Shenavrin
Figure caption: Phase curves of J, M magnitudes and J − K, K − L color indices. Blue lines show approximation by Fourier series containing terms of order of ≤3.
Paper: Disk in the Circumstellar Envelope of Carbon Mira V Cygni
Authors: Boris S. Safonov, Sergey G. Zheltoukhov, Andrey M. Tatarnikov, Ivan A. Strakhov, Victor I. Shenavrin
Figure caption: NIR spectra of V Cyg at maximum and minimum of brightness. The regions of strong telluric absorption bands are shaded in gray. The light gray band at a λ ≈ 1.14 μm marks the region, in which signal recovery is possible.
Paper: Disk in the Circumstellar Envelope of Carbon Mira V Cygni
Authors: Boris S. Safonov, Sergey G. Zheltoukhov, Andrey M. Tatarnikov, Ivan A. Strakhov, Victor I. Shenavrin
Figure caption: SED of V Cyg at the brightness maximum and minimum. The inset shows two flux measurements made with IRAM (A. Castro-Carrizo et al. 2010).
Paper: JWST-TST DREAMS: A Precise Water Abundance for Hot Jupiter WASP-17b from the NIRISS SOSS Transmission Spectrum
Authors: Dana R. Louie, Elijah Mullens, Lili Alderson, Ana Glidden, Nikole K. Lewis, Hannah R. Wakeford, Natasha E. Batalha, Knicole D. Colón, Amélie Gressier, Douglas Long, Michael Radica, Néstor Espinoza, Jayesh Goyal, Ryan J. MacDonald, Erin M. May, Sara Seager, Kevin B. Stevenson, Jeff A. Valenti, Natalie H. Allen, Caleb I. Cañas, Ryan C. Challener, David Grant, Jingcheng Huang, Zifan Lin, Daniel Valentine, Mark Clampin, Marshall Perrin, Laurent Pueyo, Roeland P. van der Marel, C. Matt Mountain
Figure caption: Spectral contribution of POSEIDON model B + H− + SiO2 spectrum (black) displayed in Figure 11. H2 + He continuum opacity (gray) provides a baseline to the spectrum. SiO2 (brown) dominates the opacity at 0.2–0.4 μm via Mie scattering. Na (magenta) has a weak absorption feature at 0.60 μm. K (purple) has an absorption feature at 0.76 μm. H2O (blue) dominates the spectrum in a series of absorption features in the IR. H− (cyan) has a flat continuum opacity extending from 0.4 to 1.5–1.6 μm, giving rise to the flat SOSS order 2 data and the deeper dip in transit depth in SOSS order 1 after 1.5 μm. CO2 (red) has an absorption feature at 4.5 μm that is broadened slightly by CO (orange). SiO2 (brown) has an absorption feature at 8.6 μm that is broadened slightly by H2O. CH4 (yellow) does not contribute to the spectrum.
Paper: JWST-TST DREAMS: A Precise Water Abundance for Hot Jupiter WASP-17b from the NIRISS SOSS Transmission Spectrum
Authors: Dana R. Louie, Elijah Mullens, Lili Alderson, Ana Glidden, Nikole K. Lewis, Hannah R. Wakeford, Natasha E. Batalha, Knicole D. Colón, Amélie Gressier, Douglas Long, Michael Radica, Néstor Espinoza, Jayesh Goyal, Ryan J. MacDonald, Erin M. May, Sara Seager, Kevin B. Stevenson, Jeff A. Valenti, Natalie H. Allen, Caleb I. Cañas, Ryan C. Challener, David Grant, Jingcheng Huang, Zifan Lin, Daniel Valentine, Mark Clampin, Marshall Perrin, Laurent Pueyo, Roeland P. van der Marel, C. Matt Mountain
Figure caption: Comparison of WASP-17b retrieved H2O abundances from L. Alderson et al. (2022, gray posteriors) to those shown in Figures 11 and 12 (posteriors correspond to the same color scheme) and retrievals performed in D. Grant et al. (2023). L. Alderson et al. (2022)'s analysis of HST + Spitzer data found that subsolar (model B), supersolar, and bimodal posterior distributions were all statistically valid, depending upon the model configuration. Retrievals from D. Grant et al. (2023, dark orange and light blue posteriors) included MIRI LRS data and yielded similar results using model B. Adding NIRISS SOSS data, we find tight constraints on a supersolar water abundance from retrievals on HST + SOSS + Spitzer + MIRI, and retrievals on SOSS alone. Clearly, NIRISS SOSS is driving the abundance constraints, since the SOSS-alone retrievals with both POSEIDON and pRT yield similarly constrained abundances.
Paper: JWST-TST DREAMS: A Precise Water Abundance for Hot Jupiter WASP-17b from the NIRISS SOSS Transmission Spectrum
Authors: Dana R. Louie, Elijah Mullens, Lili Alderson, Ana Glidden, Nikole K. Lewis, Hannah R. Wakeford, Natasha E. Batalha, Knicole D. Colón, Amélie Gressier, Douglas Long, Michael Radica, Néstor Espinoza, Jayesh Goyal, Ryan J. MacDonald, Erin M. May, Sara Seager, Kevin B. Stevenson, Jeff A. Valenti, Natalie H. Allen, Caleb I. Cañas, Ryan C. Challener, David Grant, Jingcheng Huang, Zifan Lin, Daniel Valentine, Mark Clampin, Marshall Perrin, Laurent Pueyo, Roeland P. van der Marel, C. Matt Mountain
Figure caption: Atmospheric retrievals with POSEIDON and pRT on SOSS order 1 and 2 data (Ahsoka reduction from this work). Top and middle: median retrieved spectra (solid lines), with 1σ and 2σ confidence intervals (dark and light shaded regions) for POSEIDON (top) and pRT (middle) retrievals. Both retrievals use the chemical inventory of model B (Appendix Table 4), with and without H−. Bottom panels: retrieved posteriors for isothermal atmospheric temperature and gas-phase volume mixing ratios (columns one and two) and cloud properties from POSEIDON (column three) and pRT (column four).
Paper: JWST-TST DREAMS: A Precise Water Abundance for Hot Jupiter WASP-17b from the NIRISS SOSS Transmission Spectrum
Authors: Dana R. Louie, Elijah Mullens, Lili Alderson, Ana Glidden, Nikole K. Lewis, Hannah R. Wakeford, Natasha E. Batalha, Knicole D. Colón, Amélie Gressier, Douglas Long, Michael Radica, Néstor Espinoza, Jayesh Goyal, Ryan J. MacDonald, Erin M. May, Sara Seager, Kevin B. Stevenson, Jeff A. Valenti, Natalie H. Allen, Caleb I. Cañas, Ryan C. Challener, David Grant, Jingcheng Huang, Zifan Lin, Daniel Valentine, Mark Clampin, Marshall Perrin, Laurent Pueyo, Roeland P. van der Marel, C. Matt Mountain
Figure caption: Comparison of nested POSEIDON model B retrievals with and without H− and AlO, zooming in on the 0.2–1.05 μm region. We display median retrieved spectra (solid lines) and 1σ confidence regions (shaded regions). Model B with both H− and AlO (blue) is the best-fit model, but only due to imparting fine structure to fit the STIS slope. Future observations of the 0.2–0.8 μm region will provide more reliable inferences of metal species.
Paper: JWST-TST DREAMS: A Precise Water Abundance for Hot Jupiter WASP-17b from the NIRISS SOSS Transmission Spectrum
Authors: Dana R. Louie, Elijah Mullens, Lili Alderson, Ana Glidden, Nikole K. Lewis, Hannah R. Wakeford, Natasha E. Batalha, Knicole D. Colón, Amélie Gressier, Douglas Long, Michael Radica, Néstor Espinoza, Jayesh Goyal, Ryan J. MacDonald, Erin M. May, Sara Seager, Kevin B. Stevenson, Jeff A. Valenti, Natalie H. Allen, Caleb I. Cañas, Ryan C. Challener, David Grant, Jingcheng Huang, Zifan Lin, Daniel Valentine, Mark Clampin, Marshall Perrin, Laurent Pueyo, Roeland P. van der Marel, C. Matt Mountain
Figure caption: Comparison of nested POSEIDON retrievals with H− opacity and an infinite opacity gray cloud deck. The full data set (top panel) as well as a zoom-in view on the SOSS data (bottom panel) are shown. Though an infinite opacity deck can fit the flat SOSS order 2 data, H− is still preferred by 3.1σ due to a decrease in opacity past 1.5 μm.
Paper: JWST-TST DREAMS: A Precise Water Abundance for Hot Jupiter WASP-17b from the NIRISS SOSS Transmission Spectrum
Authors: Dana R. Louie, Elijah Mullens, Lili Alderson, Ana Glidden, Nikole K. Lewis, Hannah R. Wakeford, Natasha E. Batalha, Knicole D. Colón, Amélie Gressier, Douglas Long, Michael Radica, Néstor Espinoza, Jayesh Goyal, Ryan J. MacDonald, Erin M. May, Sara Seager, Kevin B. Stevenson, Jeff A. Valenti, Natalie H. Allen, Caleb I. Cañas, Ryan C. Challener, David Grant, Jingcheng Huang, Zifan Lin, Daniel Valentine, Mark Clampin, Marshall Perrin, Laurent Pueyo, Roeland P. van der Marel, C. Matt Mountain
Figure caption: POSEIDON retrieval complete corner plot for model B with H−.
Paper: Resolving Pleiades Binary Stars with Gaia and Speckle Interferometric Observations
Authors: Dmitry Chulkov, Ivan Strakhov, Boris Safonov
Figure caption: Left: angular separation and relative proper motion (Equation (1)) for pairs of Gaia DR3 sources with five- or six-parameter astrometric solutions and ρ < 10″. At least one source must have G < 15mag. Cases where both sources meet this criterion are colored blue. Bound binaries are well separated from optical projections. As expected, most of the optical pairs include a faint source. Pairs with Δμ < 10 mas yr−1 are considered bound (green), while the rest are optical (red). Middle: optical pairs (red), bound binary systems (green), and pairs with unknown proper motion depending on angular separation and magnitude of the fainter component. Two-parameter solutions appear only for bright stars at small ρ, where the probability of mere projection is low. Right: magnitude contrast ΔG =∣G2 − G1∣ as a function of angular separation. Pairs with full astrometric solutions (Section 5.1) are shown with green filled circles; empty circles represent two-parameter solutions (Section 5.2). Confirmed optical pairs were excluded. For wide binaries with ρ > 2″, the full solutions are available up to ΔG < 6mag.
Paper: Resolving Pleiades Binary Stars with Gaia and Speckle Interferometric Observations
Authors: Dmitry Chulkov, Ivan Strakhov, Boris Safonov
Figure caption: Color–color diagram for Pleiades sample stars. As discussed in D. Chulkov (2024), single stars and close unresolved systems belong to the main sequence, while pairs with ρ ≳ 0﹩\mathop{.}\limits^{\unicode{x02033}}﹩1 appear as outliers due to blending. (Left) Violet inverted triangle: another Gaia DR3 source with G < 19mag within 2″ is present; black square: source with ipd_frac_multi_peak  ≥ 4%; orange cross: bright star (G = 5.75mag) at ρ = 8﹩\mathop{.}\limits^{\unicode{x02033}}﹩8 causes blending; cyan circle: Alcyone; green triangle: speckle-resolved binary with ipd_frac_multi_peak  ≤ 1%. (Right) The value of ipd_frac_multi_peak is color coded. Sources with another Gaia DR3 source with G < 19mag within 2″ are marked with a square. All outlying stars either have another Gaia source in close vicinity or ipd_frac_multi_peak excess.
Paper: Resolving Pleiades Binary Stars with Gaia and Speckle Interferometric Observations
Authors: Dmitry Chulkov, Ivan Strakhov, Boris Safonov
Figure caption: Mass ratio and separation of the resolved binaries in the Pleiades. Blue is used for binaries with primary magnitude G1 < 12mag, and red for 12mag < G1 < 15mag. In the middle panel, only q > 0.5 systems are considered. For the right panel, ρ > 0﹩\mathop{.}\limits^{\unicode{x02033}}﹩​​​​​​2 pairs are selected to eliminate incompleteness. While it is tempting to see hints of bimodality in q distribution, we beware of overinterpretation, as the sample size is small, and the accuracy of speckle measurements is limited.
Paper: Resolving Pleiades Binary Stars with Gaia and Speckle Interferometric Observations
Authors: Dmitry Chulkov, Ivan Strakhov, Boris Safonov
Figure caption: Angular separation and magnitude difference ΔG = ∣G2 − G1∣ for neighboring Gaia DR3 sources. Some pairs are optical. Left: 2° Pleiades field (cluster membership not required), at least one source has G < 15mag. Pairs with G < 12mag stars are marked with a red dot. Right: all-sky sample of G < 9mag sources, where G < 6.5mag stars are marked by red dots.
Paper: Resolving Pleiades Binary Stars with Gaia and Speckle Interferometric Observations
Authors: Dmitry Chulkov, Ivan Strakhov, Boris Safonov
Figure caption: System response functions for speckle observations filters, the input of atmospheric airmass at the zenith is taken into account. Solid green: 550 nm mid band, 50 nm half-width, designated ﹩\hat{y}﹩. Solid orange: Johnson-Cousins Rc, solid black Johnson-Cousins Ic. Solid red: 880 nm mid band, 70 nm half-width, designated ﹩\hat{z}﹩. Since the 550 and 880 nm filters are not included in the library used by PARSEC isochrones, Strömgren y (dotted green) and UKIRT Infrared Deep Sky Survey Z (dotted red) passbands are used as their substitutes.
Paper: Resolving Pleiades Binary Stars with Gaia and Speckle Interferometric Observations
Authors: Dmitry Chulkov, Ivan Strakhov, Boris Safonov
Figure caption: PARSEC (version 2.0; A. Bressan et al. 2012; C. T. Nguyen et al. 2022) isochrone with rotation Ω/Ωc = 0.3 (inclination 60∘) for 100 Myr age and [Fe/H] = 0.05, plotted against sample Pleiades stars. A distance of 135 pc (5.65mag modulus) with an extinction of AV = 0.15mag is applied. The mass of a single star is shown along the right axis.
Paper: Resolving Pleiades Binary Stars with Gaia and Speckle Interferometric Observations
Authors: Dmitry Chulkov, Ivan Strakhov, Boris Safonov
Figure caption: The images of the speckle autocorrelation function for the discovered systems (Section 7.1). Circles indicate the recovered position angle; north is up, east is left. Images of all resolved systems and contrast curves are available at Zenodo (doi:10.5281/zenodo.14252721).
Paper: Resolving Pleiades Binary Stars with Gaia and Speckle Interferometric Observations
Authors: Dmitry Chulkov, Ivan Strakhov, Boris Safonov
Figure caption: The Pleiades (Messier 45, Melotte 22 (C. Messier 1781; P. J. Melotte 1915)). A red circle encompasses the surveyed area with a radius of 2°. Photo by Dmitry Trushin.
Paper: Quantifying the Effect of Short-timescale Stellar Activity Upon Transit Detection in M Dwarfs
Authors: Dana Clarice Yaptangco, Sarah Ballard, Jason Dittmann, Mariangel Albornoz
Figure caption: Our stellar sample, selected from A. A. Medina et al. (2020), E. R. Newton et al. (2017), M. Coréts Contreras (2016), and F. J. Alonso-Floriano et al. (2015) for extant TESS photometry of stars of similar size and magnitude. Our sample comprises of 16 active and 14 inactive stars between 0.18 R⊙ and 0.23 R⊙ with apparent TESS magnitudes between 10.0 and 11.5. We show histograms of these distributions above and to the side of the plot. This sample of stars are similar enough in physical properties to serve as a useful benchmark sample for this study.
Paper: Quantifying the Effect of Short-timescale Stellar Activity Upon Transit Detection in M Dwarfs
Authors: Dana Clarice Yaptangco, Sarah Ballard, Jason Dittmann, Mariangel Albornoz
Figure caption: Detectability sensitivity map of exoplanets around active and inactive stars. These maps represent the average detectability, where “detection” constitutes a FAP < 0.001, and a recovery of the true period within 1%. Detectability ranges from 0% to 100%. Overplotted is the confidence interval for the 50% contour. Top: transiting planet detectability for our active star population. We find that planet recovery decreases significantly below Earth-radii planets at periods longer than 1.6 days. Middle: same as the top panel but for our inactive stellar sample. We find broadly increased recovery of injected planet signals, reaching down to sub-Earth radii and periods as large as 6.0 days. We find that imperfect correction of photometric modulation can significantly degrade the ability to detect transiting planet signals. Bottom: Gaussian distributions for the SNR associated with the 50% detection contour. The 50% detection contour corresponds to an SNR of 7 for inactive stars, and an effective SNR of 14 is required for active stars.
Paper: Quantifying the Effect of Short-timescale Stellar Activity Upon Transit Detection in M Dwarfs
Authors: Dana Clarice Yaptangco, Sarah Ballard, Jason Dittmann, Mariangel Albornoz
Figure caption: Planets are randomly injected at different points on the sensitivity maps from Figure 3 then assigned a value of “detected” or “not detected” based on the corresponding probabilities of detection at that point. Red planets are not detected around active nor inactive stars. Yellow planets are only detected around inactive stars. Green planets are only detected around active stars. Finally, blue planets are detected around both. The orbital periods and radii of TRAPPIST-1b, c, and d (M. Gillon et al. 2016) are overplotted as star symbols. We find that some TRAPPIST-1 planets are not detectable under a TESS-like survey and therefore existing TESS objects of interest may in fact be a TRAPPIST-1 like system that remains unexplored or not fully understood. As TRAPPIST-1 is itself an active star, this further degrades the probability of detecting a similar system blindly in TESS data.
Paper: Quantifying the Effect of Short-timescale Stellar Activity Upon Transit Detection in M Dwarfs
Authors: Dana Clarice Yaptangco, Sarah Ballard, Jason Dittmann, Mariangel Albornoz
Figure caption: TESS lightcurves of all thirty stars in our sample. Panel (a) to left shows the active sample and panel (b) to the right shows the inactive sample. The left side of each panel shows the original nondetrended SPOC (J. M. Jenkins et al. 2016) photometry in black. We have overplotted the Gaussian process stellar rotation model in yellow, and identified flare events in red. The right side of each panel displays the treated lightcurve, normalized by the rotation model and with flares (and points within 3 hr of flare data points) excised.
Paper: Quantifying the Effect of Short-timescale Stellar Activity Upon Transit Detection in M Dwarfs
Authors: Dana Clarice Yaptangco, Sarah Ballard, Jason Dittmann, Mariangel Albornoz
Figure caption: Sensitivity map for TIC 11893637, using the methodology described in Section 2. We show a comparison to K. Ment & D. Charbonneau (2023) to show consistency in completeness across methodologies. Axes drawn from K. Ment & D. Charbonneau (2023).
Paper: The Baryonic Tully–Fisher Relation. II. Stellar Mass Models
Authors: Francis Duey, James Schombert, Stacy McGaugh, Federico Lelli
Figure caption: The luminosity and stellar mass TF relations for the SPARC WISE sample. Blue symbols indicate galaxies with Hubble flow distances, and red symbols are galaxies with redshift-independent distances (typical Cepheids or tip of the red giant branch estimates). The luminosity TF is key as a distance indicator. High-mass cluster spirals from E. Kourkchi et al. (2020) and R. Bell et al. (2023) are shown. The bottom panel displays the same data converted into stellar mass using the ϒ values deduced as discussed in Section 2. For comparison, the stellar mass TF from A. Ristea et al. (2024) is shown. The range of fits for stellar vs. gas rotation curves is shown as the magenta band.
Paper: The Baryonic Tully–Fisher Relation. II. Stellar Mass Models
Authors: Francis Duey, James Schombert, Stacy McGaugh, Federico Lelli
Figure caption: The WISE W1 surface brightness profiles (blue symbols) are compared to Spitzer IRAC 3.6 μm (red symbols) and SDSS i (black lines) profiles for six SPARC galaxies of varying mass, morphological type, and scale length. The W1 and 3.6 μm profiles are in excellent agreement with a small W1 − [3.6] color offset. All the same stellar luminosity features detected in 3.6 μm are seen in the W1 profiles. The SDSS i profiles are offset by an i − [3.6] = 2.5 color for comparison. The correspondence between the far-IR and near-IR is also excellent, providing additional confidence in the use of optical imaging to follow profiles to smaller radii where WISE imaging lacks resolution.
Paper: The Baryonic Tully–Fisher Relation. II. Stellar Mass Models
Authors: Francis Duey, James Schombert, Stacy McGaugh, Federico Lelli
Figure caption: The comparison of three SPARC galaxy mass density profiles using WISE W1 surface brightness profiles vs. Spitzer IRAC 3.6 μm profiles.
Paper: Water in Protoplanetary Disks with JWST-MIRI: Spectral Excitation Atlas and Radial Distribution from Temperature Diagnostic Diagrams and Doppler Mapping
Authors: Andrea Banzatti, Colette Salyk, Klaus M. Pontoppidan, John S. Carr, Ke Zhang, Nicole Arulanantham, Sebastiaan Krijt, Karin I. Öberg, L. Ilsedore Cleeves, Joan R. Najita, Ilaria Pascucci, Geoffrey A. Blake, Carlos E. Romero-Mirza, Edwin A. Bergin, Lucas A. Cieza, Paola Pinilla, Feng Long, Patrick Mallaney, Chengyan Xie, Abygail R. Waggoner, Till Kaeufer
Figure caption: Definition of water diagnostic diagrams using the lines selected in Table 1. In case of nondetections, 2σ limits are marked with arrows. Some targets mentioned in the text are labeled for easier visualization. The distribution of the sample in these plots is shown in reference to multiple series of slab models that are fully explained in Appendix D and Figure 25. Left: the 6000 K line luminosity reflects the emitting area of a hot component (H model), while the vertical spread in the 1500 K line luminosity reflects a range of emitting areas for colder water (W and C models). Middle: the 3340 K line ratio is sensitive to the column density of the warm component, as shown with a dashed line (lower column, W models) and solid line (higher column, W(TK) models), demonstrating that it is typically optically thick in this sample (line ratio ​​​​​​≈1). Right: the 3600/6000 K and 1500/3600 K line ratios reflect a range of emitting areas for the warm and cold components, respectively, as shown by the red arrows. The temperature distribution in terms of radial gradients is discussed in Section 6.1, Figure 22.
Paper: Water in Protoplanetary Disks with JWST-MIRI: Spectral Excitation Atlas and Radial Distribution from Temperature Diagnostic Diagrams and Doppler Mapping
Authors: Andrea Banzatti, Colette Salyk, Klaus M. Pontoppidan, John S. Carr, Ke Zhang, Nicole Arulanantham, Sebastiaan Krijt, Karin I. Öberg, L. Ilsedore Cleeves, Joan R. Najita, Ilaria Pascucci, Geoffrey A. Blake, Carlos E. Romero-Mirza, Edwin A. Bergin, Lucas A. Cieza, Paola Pinilla, Feng Long, Patrick Mallaney, Chengyan Xie, Abygail R. Waggoner, Till Kaeufer
Figure caption: Atlas of water emission in MIRI-MRS spectra (continued from Figure 3): the long MIRI wavelengths. A colder component of water emission (∼190 K) is prominent in two low-energy (Eu ∼ 1500 K) lines near 23.85 μm (Section 4).