adsabs/AstroCLIMB huggingface dataset:
Paper: The First Catalog of Candidate White Dwarf–Main-sequence Binaries in Open Star Clusters: A New Window into Common Envelope Evolution
Authors: Steffani M. Grondin, Maria R. Drout, Jason Nordhaus, Philip S. Muirhead, Joshua S. Speagle, 佳士 沈, Ryan Chornock
Figure caption: Properties of the training data used to identify WD+MS binaries. MS cluster members from five OCs (Alessi 10, ASCC 41, NGC 2251, NGC 2632, and NGC 7086) are indicated as gray-filled circles. SDSS WD+MS binaries from A. Rebassa-Mansergas et al. (2010) are marked as filled and open squares, where the sample is split into two classes. Class 1 (dark pink outlined) represents WD+MS binaries that are distinct from the MS cluster members in a  t-SNE  projection, five example color–color spaces, and a Gaia CMD, while Class 2 (light purple) represents a subset of binaries that are more likely to share properties with MS cluster members. To maximize separation between the MS stars and WD+MS binaries and thus minimize potential contamination, we only use Class 1 WD+MS binaries when training our SVM.
Paper: The First Catalog of Candidate White Dwarf–Main-sequence Binaries in Open Star Clusters: A New Window into Common Envelope Evolution
Authors: Steffani M. Grondin, Maria R. Drout, Jason Nordhaus, Philip S. Muirhead, Joshua S. Speagle, 佳士 沈, Ryan Chornock
Figure caption: Our SVM model to identify WD+MS binaries in five different color–color spaces. Our test data is run through the SVM, where each point is colored by its probability of being a WD+MS binary. The training sample containing OC members (gray) and known WD+MS binaries from SDSS (purple; A. Rebassa-Mansergas et al. 2010) is highlighted for reference. Overall, the assigned probabilities for the test data are aligned with the SVM classifier (rainbow gradient), where any outliers can likely be explained by higher-dimensional effects (i.e., here, we use 2D example spaces to visualize the SVM classification; however, the SVM is actually a 10-dimensional hyperplane and uses all input colors to compute probabilities).
Paper: The First Catalog of Candidate White Dwarf–Main-sequence Binaries in Open Star Clusters: A New Window into Common Envelope Evolution
Authors: Steffani M. Grondin, Maria R. Drout, Jason Nordhaus, Philip S. Muirhead, Joshua S. Speagle, 佳士 沈, Ryan Chornock
Figure caption: Reddened MS stars of spectral types B8V to M8V relative to the training samples of OC members from T. Cantat-Gaudin et al. (2020) and SDSS WD+MS binaries in A. Rebassa-Mansergas et al. (2010). The thin line shows the A. J. Pickles (1998) stellar atmosphere models for an extinction of A  V  = 0, while the thick black line depicts an extinction of A  V  = 3. Both lines are colored by the effective temperatures of the stars. It is clear that reddening of MS stars moves them along or away from the known WD+MS sample.
Paper: The First Catalog of Candidate White Dwarf–Main-sequence Binaries in Open Star Clusters: A New Window into Common Envelope Evolution
Authors: Steffani M. Grondin, Maria R. Drout, Jason Nordhaus, Philip S. Muirhead, Joshua S. Speagle, 佳士 沈, Ryan Chornock
Figure caption: LOO-CV results for our training sample. To investigate the performance of our SVM on “new” clusters, we remove one cluster from our training sample and use it as test data with our SVM (each left-out cluster is labeled). Overall, the SVM classifies the cluster members as low-probability WD+MS systems, whereas only a few cluster members are classified as high-probability WD+MS binaries. Specifically, zero sources are classified with probabilities above P > 0.9. Hence, we opt to use this as a metric for defining a high-probability sample of systems in this study. The OC with the highest cluster member contamination is NGC 7086 (dark purple), which is due to its broad colors extending near the known WD+MS binaries (light purple) in color–color spaces.
Paper: The First Catalog of Candidate White Dwarf–Main-sequence Binaries in Open Star Clusters: A New Window into Common Envelope Evolution
Authors: Steffani M. Grondin, Maria R. Drout, Jason Nordhaus, Philip S. Muirhead, Joshua S. Speagle, 佳士 沈, Ryan Chornock
Figure caption: SVM probabilities for subsamples of systems (not) used in our SVM training. As described in Section 3.2.2, we use a sample of likely MS cluster members (gray) and WD+MS binaries from A. Rebassa-Mansergas et al. (2010) to train our SVM. To minimize contamination, we only use “Class 1” binaries (dark pink) in our model, which on average have larger separation from the ZAMS in color–color spaces and a Gaia CMD than the “Class 2” binaries (light pink). Here, we see that while our model is less sensitive to these types of binaries, ∼25% of the “Class 2” systems are still classified with high probability with our SVM. Hence, these types of binaries could be present in our catalog.
Paper: The First Catalog of Candidate White Dwarf–Main-sequence Binaries in Open Star Clusters: A New Window into Common Envelope Evolution
Authors: Steffani M. Grondin, Maria R. Drout, Jason Nordhaus, Philip S. Muirhead, Joshua S. Speagle, 佳士 沈, Ryan Chornock
Figure caption: A normalized confusion matrix of our SVM classifier using our test data. Overall, the SVM performs well, with no false positives and only one false negative identified out of 265 systems when utilizing a prediction probability threshold of P > 0.5.
Paper: Reflected-light Phase Curves with PICASO: A Kepler-7b Case Study
Authors: Colin D. Hamill, Alexandria V. Johnson, Natasha Batalha, Rowan Nag, Peter Gao, Danica Adams, Tiffany Kataria
Figure caption: Reflected-light phase curves of Kepler-7b showing the planet-to-star flux ratio in parts per million (ppm) as a function of phase angle (−168° to 168°) for cloudless (gray solid), and MgSiO3-only (green dashed–dotted), Mg2SiO4-only (orange dashed), and Mg2SiO4, Al2O3, and TiO2 (blue solid) cloudy scenarios. The decreasing opacity of the curves corresponds to increasing values of f sed (0.03, 0.1, 0.3, and 1.0). The secondary eclipse occurs at 0° phase. Each phase curve has 15 unique phase angle computations and is weighed by the Kepler response function.
Paper: Reflected-light Phase Curves with PICASO: A Kepler-7b Case Study
Authors: Colin D. Hamill, Alexandria V. Johnson, Natasha Batalha, Rowan Nag, Peter Gao, Danica Adams, Tiffany Kataria
Figure caption: Albedo spectra at seven unique phase angles ranging from −168° to 168° for the cloudless scenario (left) and the cloudy scenario (right) in which Mg2SiO4, Al2O3, and TiO2 are considered as cloud condensates with f sed = 0.03. Red curves correspond to phases from −168° to 0°, and blue curves correspond to phases from 0° to 168°. A phase of 0° (secondary eclipse) is indicated by the purple curve. Increasing opacity of the curves corresponds to phases closer to 0°. The seven phase angles plotted are 0°, ±72°, ±120°, and ±168°. Phase angles of ±24°, ±48°, ±96°, ±144° are removed for plot clarity. The Kepler response function is plotted in gray.
Paper: Reflected-light Phase Curves with PICASO: A Kepler-7b Case Study
Authors: Colin D. Hamill, Alexandria V. Johnson, Natasha Batalha, Rowan Nag, Peter Gao, Danica Adams, Tiffany Kataria
Figure caption: Same as Figure 9, but with only the f sed = 0.03 models of the three-cloud (blue), Mg2SiO4 (orange), and MgSiO3 (green) scenarios. The output intensities are multiplied by a factor of three in order to better compare the shapes of our reflected phase curves to the observations from B.-O. Demory et al. (2013; gray).
Paper: Reflected-light Phase Curves with PICASO: A Kepler-7b Case Study
Authors: Colin D. Hamill, Alexandria V. Johnson, Natasha Batalha, Rowan Nag, Peter Gao, Danica Adams, Tiffany Kataria
Figure caption: Same as Figure 8, but without the MgSiO3-only scenario and including observational data (Q1–Q14 data from Kepler) of Kepler-7b from B.-O. Demory et al. (2013; gray points; error bars omitted for clarity). The gray line is the three-fixed-band best-fit model from B.-O. Demory et al. (2013).
Paper: Reflected-light Phase Curves with PICASO: A Kepler-7b Case Study
Authors: Colin D. Hamill, Alexandria V. Johnson, Natasha Batalha, Rowan Nag, Peter Gao, Danica Adams, Tiffany Kataria
Figure caption: Top: comparison of the phase curves for the three-cloud scenario that considers Mg2SiO4, Al2O3, and TiO2 as cloud condensates with f sed = 0.03 for three different Chebyshev–Gauss spatial resolutions: 10 × 10 (blue), 20 × 20 (green), and 30 × 30 (orange). Bottom: absolute percent error between each of the models as a function of orbital phase.
Paper: Whole-disk Sampling of Molecular Clouds in M83
Authors: Akihiko Hirota, Jin Koda, Fumi Egusa, Tsuyoshi Sawada, Kazushi Sakamoto, Mark Heyer, Amanda M Lee, Fumiya Maeda, Samuel Boissier, Daniela Calzetti, Bruce G. Elmegreen, Nanase Harada, Luis C. Ho, Masato I. N. Kobayashi, Nario Kuno, Barry F. Madore, Sergio Martín, Jennifer Donovan Meyer, Kazuyuki Muraoka, Yoshimasa Watanabe
Figure caption: Scaling relations of cloud properties. In each plot, the raw data points for the M83 clouds are shown with the gray markers, and the data density is displayed with the black contour lines at 10%, 20%, 40%, and 80% levels of the maximum density, respectively. In the bottom-right corner of the plot, Spearman’s rank correlation coefficient is noted. Orange and cyan contour lines indicate the distribution of T peak > 2 K and <2 K clouds, respectively, at the 20% density level. The green-shaded region indicates the distribution density of the Galactic clouds of S87 at a 20% level. Where appropriate, the resolution limits for σ v of ﹩1/\sqrt{12}﹩ km s−1 and R eff of ∼37 pc (﹩=1.91\times {\theta }_{{\rm{b}}}/\sqrt{8\mathrm{log}2})﹩) and the luminosity limit of ∼6900 K km s−1 pc2, which corresponds to the expected minimum mass of ∼3 × 104 M ⊙ (Section 2.6), are shown with the purple dashed–dotted line in each plot. (a) σ v–R eff relationship. The black dashed line indicates the σ v–R eff relation of S87, which is Equation (9) with C = 0.72 km s−1 pc−1/2. The dotted line is the one with C half of S87's value. The purple open markers indicate the median σ v derived at the binned R eff, and the red open marker running median for T peak > 2 K clouds. (b) M vir–L CO relationship. The dashed line indicates the relation of S87 (M vir ∝ ﹩{L}_{\mathrm{CO}}^{0.81}﹩), and dotted line is α vir = 1. The red line indicates the fit to the M83 clouds with T peak > 2 K (Equation (11)). (c) M cl–R eff relationship. The dotted lines indicate the lines for Σ of 1, 10, 100, and 1000 M ⊙ pc−2, respectively. The dashed line indicates Σ = 200 M ⊙ pc−2, implied from S87's scaling relations. As in (a), the running median for all the samples and >2 K clouds are shown with red and purple markers. (d) ﹩{\sigma }_{{\rm{v}}}/{R}_{\mathrm{eff}}^{1/2}﹩–Σ relationship. The red line indicates the fit to all M83 clouds (Equation (12)). The lines of α vir of 1 and 2 are shown with the dotted and dashed–dotted lines, respectively.
Paper: Whole-disk Sampling of Molecular Clouds in M83
Authors: Akihiko Hirota, Jin Koda, Fumi Egusa, Tsuyoshi Sawada, Kazushi Sakamoto, Mark Heyer, Amanda M Lee, Fumiya Maeda, Samuel Boissier, Daniela Calzetti, Bruce G. Elmegreen, Nanase Harada, Luis C. Ho, Masato I. N. Kobayashi, Nario Kuno, Barry F. Madore, Sergio Martín, Jennifer Donovan Meyer, Kazuyuki Muraoka, Yoshimasa Watanabe
Figure caption: (a) Distribution of cloud mass M cl in M83. In the upper panel, the black histogram shows the overall distribution. The blue solid, green solid, and black dashed histograms indicate the subsamples with M cl > 106 M ⊙, M cl in the range between 105 and 106 M ⊙, and with sizes that failed in the deconvolution (Section 2.3.2). In the same panel, the marker and horizontal line indicate the median and 16th-to-84th percentile range for all clouds (black), clouds with >106 M ⊙ (blue), and clouds with 105–106 M ⊙ (green). In the bottom panel, the mass-weighted histogram is shown. Note that, as the constant CO-to-H2 conversion factor is adopted, it is equivalent to the luminosity-weighted histogram. The marker and horizontal line indicate the median and percentiles as the upper panel. (b)–(g) Same as (a), but for peak temperature T peak, velocity dispersion σ v, effective radius R eff, surface density Σ, and virial parameter α vir, respectively.
Paper: Whole-disk Sampling of Molecular Clouds in M83
Authors: Akihiko Hirota, Jin Koda, Fumi Egusa, Tsuyoshi Sawada, Kazushi Sakamoto, Mark Heyer, Amanda M Lee, Fumiya Maeda, Samuel Boissier, Daniela Calzetti, Bruce G. Elmegreen, Nanase Harada, Luis C. Ho, Masato I. N. Kobayashi, Nario Kuno, Barry F. Madore, Sergio Martín, Jennifer Donovan Meyer, Kazuyuki Muraoka, Yoshimasa Watanabe
Figure caption: (a) rms noise map of the 12CO (1–0) used here. The white lines indicate the rms map with the contour levels of 0.9σ and 1σ, where 1σ is the global median of the rms noise of 6.5 mJy beam−1 (∼0.17 K), and the black line indicates the level of 1.1σ. (b) Integrated intensity map of 12CO (1–) data used here. The cyan lines indicate the galactocentric radii of 25″ (∼0.55 kpc), 100″ (∼2.2 kpc), 140″ (∼3.1 kpc), 210″ (∼4.6 kpc), and 280″ (∼6.1 kpc), respectively.
Paper: Whole-disk Sampling of Molecular Clouds in M83
Authors: Akihiko Hirota, Jin Koda, Fumi Egusa, Tsuyoshi Sawada, Kazushi Sakamoto, Mark Heyer, Amanda M Lee, Fumiya Maeda, Samuel Boissier, Daniela Calzetti, Bruce G. Elmegreen, Nanase Harada, Luis C. Ho, Masato I. N. Kobayashi, Nario Kuno, Barry F. Madore, Sergio Martín, Jennifer Donovan Meyer, Kazuyuki Muraoka, Yoshimasa Watanabe
Figure caption: Distribution of the identified clouds overlaid on the CO map. Clouds with masses over 106 M ⊙, between 105 M ⊙ and 106 M ⊙, and below 105 M ⊙ are indicated with red-filled, blue open, and green open markers, respectively.
Paper: Whole-disk Sampling of Molecular Clouds in M83
Authors: Akihiko Hirota, Jin Koda, Fumi Egusa, Tsuyoshi Sawada, Kazushi Sakamoto, Mark Heyer, Amanda M Lee, Fumiya Maeda, Samuel Boissier, Daniela Calzetti, Bruce G. Elmegreen, Nanase Harada, Luis C. Ho, Masato I. N. Kobayashi, Nario Kuno, Barry F. Madore, Sergio Martín, Jennifer Donovan Meyer, Kazuyuki Muraoka, Yoshimasa Watanabe
Figure caption: (a)–(c) Ratio of the extrapolated to unextrapolated values for L CO, R eff, and σ v, respectively, are shown as a function of the cloud mass. The red markers and error bars indicate the median and 16th-to-84th percentile ranges of each quantity at the binning masses. (d)–(f) Same as (a)–(c), but for fractional uncertainty for each quantity in (a)–(c) as a function of the cloud mass.
Paper: Whole-disk Sampling of Molecular Clouds in M83
Authors: Akihiko Hirota, Jin Koda, Fumi Egusa, Tsuyoshi Sawada, Kazushi Sakamoto, Mark Heyer, Amanda M Lee, Fumiya Maeda, Samuel Boissier, Daniela Calzetti, Bruce G. Elmegreen, Nanase Harada, Luis C. Ho, Masato I. N. Kobayashi, Nario Kuno, Barry F. Madore, Sergio Martín, Jennifer Donovan Meyer, Kazuyuki Muraoka, Yoshimasa Watanabe
Figure caption: Same as Figure 5, but clouds are classified with a T peak threshold of 2 K. Clouds with T peak > 2 K and <2 K are indicated with orange and blue markers, respectively.
Paper: Strong Nongravitational Accelerations and the Potential for Misidentification of Near-Earth Objects
Authors: Aster G. Taylor, Darryl Z. Seligman, Matthew J. Holman, Peter Vereš, Davide Farnocchia, Nikole Lewis, Marco Micheli, Jason T. Wright
Figure caption: The U parameter (Equation (6)) over a range of (a, e) values and the V parameter (Equation (10)) over a range of (i, ω) values (we set Ω = 0). Contours are shown for both functions. For the U parameter, the contours trace the phase-space trajectories of these objects, which is not the case for the V parameter. In the top panel, the arrows indicate the direction of motion for positive A 2. The contours shown in the bottom panel are not equivalent to the phase-space trajectories.
Paper: Strong Nongravitational Accelerations and the Potential for Misidentification of Near-Earth Objects
Authors: Aster G. Taylor, Darryl Z. Seligman, Matthew J. Holman, Peter Vereš, Davide Farnocchia, Nikole Lewis, Marco Micheli, Jason T. Wright
Figure caption: Similar to Figure 2, but with radial A 1 acceleration instead of transverse A 2 acceleration. The contour is at 1 × 103 arcsec.
Paper: Strong Nongravitational Accelerations and the Potential for Misidentification of Near-Earth Objects
Authors: Aster G. Taylor, Darryl Z. Seligman, Matthew J. Holman, Peter Vereš, Davide Farnocchia, Nikole Lewis, Marco Micheli, Jason T. Wright
Figure caption: Similar to Figure 2, but with out-of-plane A 3 acceleration and an apparition difference of 1 yr.
Paper: Strong Nongravitational Accelerations and the Potential for Misidentification of Near-Earth Objects
Authors: Aster G. Taylor, Darryl Z. Seligman, Matthew J. Holman, Peter Vereš, Davide Farnocchia, Nikole Lewis, Marco Micheli, Jason T. Wright
Figure caption: Histograms of the nearest-neighbor distance in orbital angular momentum (top), orbital elements (middle), and the constants of motion given by Equations (6) and (10) (bottom).
Paper: Strong Nongravitational Accelerations and the Potential for Misidentification of Near-Earth Objects
Authors: Aster G. Taylor, Darryl Z. Seligman, Matthew J. Holman, Peter Vereš, Davide Farnocchia, Nikole Lewis, Marco Micheli, Jason T. Wright
Figure caption: Similar to Figure 2, but with out-of-plane A 3 acceleration instead of transverse A 2 acceleration.
Paper: Strong Nongravitational Accelerations and the Potential for Misidentification of Near-Earth Objects
Authors: Aster G. Taylor, Darryl Z. Seligman, Matthew J. Holman, Peter Vereš, Davide Farnocchia, Nikole Lewis, Marco Micheli, Jason T. Wright
Figure caption: Similar to Figure 2, but with radial A 1 acceleration and an apparition difference of 1 yr.
Paper: Strong Nongravitational Accelerations and the Potential for Misidentification of Near-Earth Objects
Authors: Aster G. Taylor, Darryl Z. Seligman, Matthew J. Holman, Peter Vereš, Davide Farnocchia, Nikole Lewis, Marco Micheli, Jason T. Wright
Figure caption: Similar to Figure 2, but for an apparition difference of 1 yr. The contour is at 1 × 103 arcsec.
Paper: An Elemental Abundance Diagnostic for Coordinated Solar Orbiter/SPICE and Hinode/EIS Observations
Authors: David H. Brooks, Harry P. Warren, Deborah Baker, Sarah A. Matthews, Stephanie L. Yardley
Figure caption: Plasma composition analysis for the predicted footpoints of the magnetic field connected to Solar Orbiter. Left to right: EIS Fe VIII 185.213 Å intensity map, SPICE observed Ne VIII 770.428 Å intensity map, and EIS simulated and SPICE observed Ne VIII 770.428 Å intensities for the blue and red boxed regions in the left and middle panels. The red and blue boxes encompass regions where the magnetic field connected to Solar Orbiter is predicted to be located. The pale blue and pink dots show the actual predictions for the footpoints of the magnetic field connected to the spacecraft (see text). The blue line in the right-hand panel indicates photospheric abundance ratios, and the red line shows coronal abundance ratios.
Paper: An Elemental Abundance Diagnostic for Coordinated Solar Orbiter/SPICE and Hinode/EIS Observations
Authors: David H. Brooks, Harry P. Warren, Deborah Baker, Sarah A. Matthews, Stephanie L. Yardley
Figure caption: SWA/HIS measurements of the Fe/O intensity ratio in situ in the solar wind for the period 2023 March 30 to April 3. The corresponding FIP bias values (Fe/O normalized to the photospheric ratio) are shown on the right axis. The horizontal dashed line indicates the photospheric ratio. The light-blue shaded area shows when EIS and SPICE were observing. The red shaded area indicates when solar wind from the AR 13262 arrives at Solar Orbiter.
Paper: An Elemental Abundance Diagnostic for Coordinated Solar Orbiter/SPICE and Hinode/EIS Observations
Authors: David H. Brooks, Harry P. Warren, Deborah Baker, Sarah A. Matthews, Stephanie L. Yardley
Figure caption: Plasma composition analysis from the combined EIS and SPICE observations. The histogram shows the FIP bias measurements for the coaligned FOV shown in Figure 7.
Paper: JWST Resolves Collision-induced Absorption Features in White Dwarfs
Authors: Simon Blouin, Mukremin Kilic, Loïc Albert, Bianca Azartash-Namin, Patrick Dufour
Figure caption: Best-fit models for LHS 1126. The solid blue line displays the best-fit solution to the JWST data for a grid of models using the M. Abel et al. (2012) opacities for H2–He CIA, while the dashed orange line is for a grid of models using the U. G. Jørgensen et al. (2000) H2–He CIA. Also shown as a dotted dark blue line is the best-fit solution to the combined HST and JWST SED assuming a pure-helium-atmosphere.
Paper: JWST Resolves Collision-induced Absorption Features in White Dwarfs
Authors: Simon Blouin, Mukremin Kilic, Loïc Albert, Bianca Azartash-Namin, Patrick Dufour
Figure caption: H2–He CIA spectra at different temperatures from M. Abel et al. (2012). Each absorption spectrum is normalized at its maximum (without this normalization, the higher-temperature spectra would sit above the lower-temperature spectra). Note that the CIA-forming region of the atmosphere is typically much cooler than T eff due to the high opacity at these wavelengths (Figure 13). This results in the emergent flux originating predominantly from the cooler, upper atmospheric layers.
Paper: JWST Resolves Collision-induced Absorption Features in White Dwarfs
Authors: Simon Blouin, Mukremin Kilic, Loïc Albert, Bianca Azartash-Namin, Patrick Dufour
Figure caption: Model spectra for a helium-atmosphere white dwarf with the same parameters as the best-fit pure-helium solution shown in Figure 8. The solid line is the model obtained using the default He–He–He CIA of P. M. Kowalski (2014), as in the model shown as a dotted dark blue line in Figure 8. The dotted and dashed lines illustrate the effect of decreasing or increasing this absorption source. The JWST data are shown for comparison. This supports the idea that an enhanced He–He–He CIA could explain LHS 1126's SED.
Paper: JWST Resolves Collision-induced Absorption Features in White Dwarfs
Authors: Simon Blouin, Mukremin Kilic, Loïc Albert, Bianca Azartash-Namin, Patrick Dufour
Figure caption: Model spectra for a star with the same parameters as those obtained by A. K. Elms et al. (2022) for WD J1922+0233. The solid line shows a model without metal pollution, while the dashed line corresponds to the case with metals (﹩\mathrm{log}\,\mathrm{Na}/\mathrm{He}=-12.6﹩ and chondritic metal-to-metal abundance ratios for the other elements).
Paper: JWST Resolves Collision-induced Absorption Features in White Dwarfs
Authors: Simon Blouin, Mukremin Kilic, Loïc Albert, Bianca Azartash-Namin, Patrick Dufour
Figure caption: JWST MIRI spectra of the three IR-faint white dwarfs in our sample, focused on the 3.5–14 μm region. The spectra are normalized at 3.5 μm and vertically offset for clarity. Thin lines show the original spectra, while thick lines represent smoothed versions using a Savitzky–Golay filter. No clear silicate emission features are detected in the 8–12 μm range. For WD J1922+0233 and LHS 3250, the spectra are cut off at 12 μm due to poor S/Ns at longer wavelengths.
Paper: JWST Resolves Collision-induced Absorption Features in White Dwarfs
Authors: Simon Blouin, Mukremin Kilic, Loïc Albert, Bianca Azartash-Namin, Patrick Dufour
Figure caption: Smoothed SED (red curve) used to calculate the total wavelength-integrated flux of LHS 1126. The HST and JWST data points used to build the smoothed SED are shown as blue and gray symbols. Archival optical and infrared photometry is also shown with black error bars.
Paper: JWST Resolves Collision-induced Absorption Features in White Dwarfs
Authors: Simon Blouin, Mukremin Kilic, Loïc Albert, Bianca Azartash-Namin, Patrick Dufour
Figure caption: Best-fit models to the JWST spectrum of LHS 3250. The solid blue line displays the best fit for a grid of models using the M. Abel et al. (2012) opacities for H2–He CIA, while the dashed orange line is for a grid of models using the U. G. Jørgensen et al. (2000) H2–He CIA.