adsabs/AstroCLIMB huggingface dataset:
Paper: Toward a 2D H I Map of the Local Interstellar Medium
Authors: Allison Youngblood, Kevin France, Tommi Koskinen, James Paul Mason, Seth Redfield, Brian E. Wood, Vincent Bourrier, Leonardo dos Santos, Christopher Johns-Krull, George W. King, Jeffrey L. Linsky, Sarah Peacock
Figure caption: Reconstructions following the methodology of A. Youngblood et al. (2022) are shown for four targets included in this work. The black lines with error bars show the STIS/G140M or E140M data, and the pink lines show the best fit to the data. The blue lines show the reconstructed intrinsic stellar profile, and the blue shading shows the uncertainty. The dotted black lines show the transmission of the ISM, where the top of the axis corresponds to 100% transmission and the bottom to 0% transmission. All curves are shown at the native spectral resolution and binning of the data. The TOI-1231 reconstruction will be presented in more detail in K. Rockcliffe et al. (2025, in preparation).
Paper: Toward a 2D H I Map of the Local Interstellar Medium
Authors: Allison Youngblood, Kevin France, Tommi Koskinen, James Paul Mason, Seth Redfield, Brian E. Wood, Vincent Bourrier, Leonardo dos Santos, Christopher Johns-Krull, George W. King, Jeffrey L. Linsky, Sarah Peacock
Figure caption: Reconstructions following the methodology of B. E. Wood et al. (2005) are shown for six targets included in this work. The light gray lines show the STIS/E140M data, the black dashed lines show the best fit to the data, and the solid black lines show the reconstructed intrinsic stellar profile. Highlighted in red is excess absorption attributed to an astrosphere. These fits will be presented in more detail in C. Johns-Krull et al. (2025, in preparation).
Paper: Toward a 2D H I Map of the Local Interstellar Medium
Authors: Allison Youngblood, Kevin France, Tommi Koskinen, James Paul Mason, Seth Redfield, Brian E. Wood, Vincent Bourrier, Leonardo dos Santos, Christopher Johns-Krull, George W. King, Jeffrey L. Linsky, Sarah Peacock
Figure caption: H I column density maps are shown in Galactic coordinates for six different distance shells from Earth, from <10 pc up to 100 pc. The color shading shows the interpolated log10 N(H I) values based on the stars in that distance shell (marked as black-outlined stars with filled colors matching their measured N(H I) values). The black contours show levels between N(H I) = 17.5–19.0 in 0.1 dex steps; they are printed with the value that they encircle. The star symbols are the observed stars in Table A1; the symbol colors represent the measured N(H I) value.
Paper: Investigating the Effects of Point Source Injection Strategies on KMTNet Real/Bogus Classification
Authors: Dongjin Lee, Gregory S. H. Paek, Seo-Won Chang, Changwan Kim, Mankeun Jeong, Hongjae Moon, Seong-Heon Lee, Jae-Hun Jung, Myungshin Im
Figure caption: Examples of injected sources with R-band AB magnitudes from 16 to 21 in steps of 1 mag. The image is taken from KMTNet-CTIO R-band image. The top figure shows the science image before injection while the bottom figure illustrates injected sources with different magnitudes.
Paper: Investigating the Effects of Point Source Injection Strategies on KMTNet Real/Bogus Classification
Authors: Dongjin Lee, Gregory S. H. Paek, Seo-Won Chang, Changwan Kim, Mankeun Jeong, Hongjae Moon, Seong-Heon Lee, Jae-Hun Jung, Myungshin Im
Figure caption: Histogram of bogus types in the S230518h follow-up data set and the correct (blue) and incorrect (red) classification rates of RB classifiers. For (b)–(e), the threshold value of 0.5 is used. For each training data set, the rates are averaged over 10 classifiers.
Paper: Investigating the Effects of Point Source Injection Strategies on KMTNet Real/Bogus Classification
Authors: Dongjin Lee, Gregory S. H. Paek, Seo-Won Chang, Changwan Kim, Mankeun Jeong, Hongjae Moon, Seong-Heon Lee, Jae-Hun Jung, Myungshin Im
Figure caption: Ten cutouts from four transient events identified by the follow-up survey for GW190814. For each sample, we visualize science (NEW), reference (REF), and subtraction (SUB) cutouts with a size of 51 × 51. The IRAF zscale transform is applied for visualization. The object name is denoted in brown at the top of each science image. The average predicted probabilities over 10 classifiers are marked in red if the values are less than 0.5 and in blue otherwise. R, N, RN and RN† indicates RI, NGI, RI+NGI, and RI+NGI† data sets, respectively.
Paper: Investigating the Effects of Point Source Injection Strategies on KMTNet Real/Bogus Classification
Authors: Dongjin Lee, Gregory S. H. Paek, Seo-Won Chang, Changwan Kim, Mankeun Jeong, Hongjae Moon, Seong-Heon Lee, Jae-Hun Jung, Myungshin Im
Figure caption: Six most prevalent categories of bogus samples in S230518h follow-up data set.
Paper: Investigating the Effects of Point Source Injection Strategies on KMTNet Real/Bogus Classification
Authors: Dongjin Lee, Gregory S. H. Paek, Seo-Won Chang, Changwan Kim, Mankeun Jeong, Hongjae Moon, Seong-Heon Lee, Jae-Hun Jung, Myungshin Im
Figure caption: Histogram of angular distances between injected sources under the NGI method and their associated galaxies in the GLADE+ catalog. Three vertical lines indicate the average seeing, twice the average seeing, and three times average seeing.
Paper: Investigating the Effects of Point Source Injection Strategies on KMTNet Real/Bogus Classification
Authors: Dongjin Lee, Gregory S. H. Paek, Seo-Won Chang, Changwan Kim, Mankeun Jeong, Hongjae Moon, Seong-Heon Lee, Jae-Hun Jung, Myungshin Im
Figure caption: Learning curves. We measure the values of the binary cross-entropy loss function and recall scores for the validation data set (a) and (b) and test data set (c) and (d) over training epochs. The solid lines indicate the average metrics and the shaded region 95% confidence interval over 10 runs.
Paper: Investigating the Effects of Point Source Injection Strategies on KMTNet Real/Bogus Classification
Authors: Dongjin Lee, Gregory S. H. Paek, Seo-Won Chang, Changwan Kim, Mankeun Jeong, Hongjae Moon, Seong-Heon Lee, Jae-Hun Jung, Myungshin Im
Figure caption: Histogram of angular distances between injected sources under the RI method and their nearest stars in the KMTNet catalog. Three vertical lines indicate the average seeing, twice the average seeing, and three times average seeing.
Paper: Investigating the Effects of Point Source Injection Strategies on KMTNet Real/Bogus Classification
Authors: Dongjin Lee, Gregory S. H. Paek, Seo-Won Chang, Changwan Kim, Mankeun Jeong, Hongjae Moon, Seong-Heon Lee, Jae-Hun Jung, Myungshin Im
Figure caption: Examples of variable stars (a) in the S230518h follow-up and injected sources with different distances from galaxies (b)–(f) in the NGI data set. The values at the top of (b)–(f) indicate the angular distances in arcseconds from the galaxies associated with injected point sources.
Paper: Investigating the Effects of Point Source Injection Strategies on KMTNet Real/Bogus Classification
Authors: Dongjin Lee, Gregory S. H. Paek, Seo-Won Chang, Changwan Kim, Mankeun Jeong, Hongjae Moon, Seong-Heon Lee, Jae-Hun Jung, Myungshin Im
Figure caption: ROC curves of trained classifiers. For each data set, ROC curves of 10 classifiers trained with different random configurations are visualized. The average AUC score is shown in the legend.
Paper: Investigating the Effects of Point Source Injection Strategies on KMTNet Real/Bogus Classification
Authors: Dongjin Lee, Gregory S. H. Paek, Seo-Won Chang, Changwan Kim, Mankeun Jeong, Hongjae Moon, Seong-Heon Lee, Jae-Hun Jung, Myungshin Im
Figure caption: Learning rate schedule used in the training.
Paper: Investigating the Effects of Point Source Injection Strategies on KMTNet Real/Bogus Classification
Authors: Dongjin Lee, Gregory S. H. Paek, Seo-Won Chang, Changwan Kim, Mankeun Jeong, Hongjae Moon, Seong-Heon Lee, Jae-Hun Jung, Myungshin Im
Figure caption: The number of misclassified bogus (left axes) and real samples (right axes) of a single RB classifier trained on each of the RI (left figure) and RI+NGI† (right figure) data sets over various threshold values.
Paper: The Flocculent Structure of the Inner Milky Way Disk
Authors: Dana S. Balser, W. B. Burton
Figure caption: Integrated brightness temperatures as a function of Galactic longitude for the northern data (left) and southern data (right). Upper: the brightness temperature integrated over all LSR velocities: the positive and negative LSR velocities are shown independently, representing the inner and outer parts of the Galactic disk. The hills and valleys that would be expected if a dominant spiral pattern pertained in the inner Galaxy are absent. The north–south differences are no doubt due to the slightly lopsided nature of the Milky Way, a property not uncommon. Lower: the brightness temperature integrated only over the high-velocity wings, pertaining to gas near the subcentral region. The red curve is a linear fit to the data, yielding ∫TB dV = 6.48 ℓ + 1672 K km s−1 for the northern data and ∫TB dV = –5.19 ℓ + 1524 K km s−1 for the southern data. There are no broad dips that would be expected for the interarm region of a grand design. We comment in the text on the apparently “noisy” nature of the lower plots.
Paper: The Flocculent Structure of the Inner Milky Way Disk
Authors: Dana S. Balser, W. B. Burton
Figure caption: Apparent velocity dispersions as a function of the Galactocentric radius of the subcentral point for the northern data (left) and southern data (right). The red curve is a linear fit to the data, yielding ﹩\sigma =-0.43\,{R}_{\min }+11.67﹩ km s−1 for the northern data and ﹩\sigma =-0.16\,{R}_{\min }+9.71﹩ km s−1 for the southern data. The units of ﹩{R}_{{\rm{\min }}}={R}_{{\rm{o}}}\,{\rm{\sin }}(\ell )﹩ are in kiloparsecs, and we assume Ro = 10 kpc (see text). The measurements show no high σ excursions that would be expected from relatively empty interarm regions.
Paper: The Flocculent Structure of the Inner Milky Way Disk
Authors: Dana S. Balser, W. B. Burton
Figure caption: Representative HI4PI H I spectra for ℓ = 45° (left) and ℓ = 315° (right). The green curve is the Gaussian fit of the high-velocity shoulder and the red curve shows the portion of the H I data that was used to constrain the fit. The shape of the extreme-velocity shoulder is measured by the dispersion, σ, of the Gaussian fit.
Paper: The JDISC Survey: Linking the Physics and Chemistry of Inner and Outer Protoplanetary Disk Zones
Authors: Nicole Arulanantham, Colette Salyk, Klaus Pontoppidan, Andrea Banzatti, Ke Zhang, Karin Öberg, Feng Long, John Carr, Joan Najita, Ilaria Pascucci, María José Colmenares, Chengyan Xie, Jane Huang, Joel Green, Sean M. Andrews, Geoffrey A. Blake, Edwin A. Bergin, Paola Pinilla, Miguel Vioque, Emma Dahl, Eshan Raul, Sebastiaan Krijt
Figure caption: Median emission-line luminosities from C2H2 (left), HCN (middle), and CO2 (right) vs. the median emitting masses measured from the best-fit slab models for each disk, with marker styles indicating the submillimeter dust substructures listed in Table 2. We report statistically significant, positive correlations and linear relationships between the two parameters for all three molecules (see Equation (1)), implying that the emission is optically thin to moderately optically thick (Spearman ρ = 0.97, 0.98, 0.82).
Paper: The JDISC Survey: Linking the Physics and Chemistry of Inner and Outer Protoplanetary Disk Zones
Authors: Nicole Arulanantham, Colette Salyk, Klaus Pontoppidan, Andrea Banzatti, Ke Zhang, Karin Öberg, Feng Long, John Carr, Joan Najita, Ilaria Pascucci, María José Colmenares, Chengyan Xie, Jane Huang, Joel Green, Sean M. Andrews, Geoffrey A. Blake, Edwin A. Bergin, Paola Pinilla, Miguel Vioque, Emma Dahl, Eshan Raul, Sebastiaan Krijt
Figure caption: Left panel: ratios of C2H2 to CO2 integrated emission-line luminosities vs. submillimeter dust disk sizes from Table 2. Red markers denote lower limits for disks where CO2 was not detected (VZ Cha, TW Cha, Sz 129, MWC 480) and upper limits for disks where C2H2 was not detected (AS 205S, MY Lup, Elias 27), and red X symbols denote disks where neither molecule was detected (RY Lup). Right panel: ratios of HCN integrated emission-line luminosities and cold 23.85 μm H2O emission from A. Banzatti et al. (2025) vs. submillimeter dust disk size. Black markers are used to identify submillimeter substructures, as listed in Table 2.
Paper: The JDISC Survey: Linking the Physics and Chemistry of Inner and Outer Protoplanetary Disk Zones
Authors: Nicole Arulanantham, Colette Salyk, Klaus Pontoppidan, Andrea Banzatti, Ke Zhang, Karin Öberg, Feng Long, John Carr, Joan Najita, Ilaria Pascucci, María José Colmenares, Chengyan Xie, Jane Huang, Joel Green, Sean M. Andrews, Geoffrey A. Blake, Edwin A. Bergin, Paola Pinilla, Miguel Vioque, Emma Dahl, Eshan Raul, Sebastiaan Krijt
Figure caption: Subset of JDISCS Cycle 1 targets with retrieved C2H2 slab temperatures of ∼1000 K, required to reproduce broader “pedestal”-like emission than observed in the other disks from our sample (magenta; full models from Figure 4 are filled in gray). Optically thick C2H2 components with ﹩{\mathrm{log}}\,N=22﹩ cm−2 are overplotted for comparison (cyan; B. Tabone et al. 2023; A. M. Arabhavi et al. 2024), and OH emission lines that were not included in our fits are marked with purple, dashed lines. While the optically thick gas models can reproduce the excess emission near the bandheads, they overpredict the emission from the P and R branch transitions and are therefore not consistent with the overall shapes of the pedestals.
Paper: The JDISC Survey: Linking the Physics and Chemistry of Inner and Outer Protoplanetary Disk Zones
Authors: Nicole Arulanantham, Colette Salyk, Klaus Pontoppidan, Andrea Banzatti, Ke Zhang, Karin Öberg, Feng Long, John Carr, Joan Najita, Ilaria Pascucci, María José Colmenares, Chengyan Xie, Jane Huang, Joel Green, Sean M. Andrews, Geoffrey A. Blake, Edwin A. Bergin, Paola Pinilla, Miguel Vioque, Emma Dahl, Eshan Raul, Sebastiaan Krijt
Figure caption: Optical depths vs. column densities for the combinations of C2H2 (magenta), HCN (green), and CO2 (brown) slab model parameters that best reproduce the spectrum of AS 205N; markers with stars correspond to the column densities used in Figure 7, and the black, dashed line shows τ = 1. In general, the C2H2 and HCN slab models are optically thin to larger column densities than the CO2. We note that the 13CO2 Q branch near 15.4 μm is not detected in this target (see, e.g., S. L. Grant et al. 2023; C. Xie et al. 2023; C. Salyk et al. 2025), or the 13C12CH2 Q branch seen in DoAr 33 and GO Tau (B. Tabone et al. 2023; A. M. Arabhavi et al. 2024; M. J. Colmenares et al. 2024; J. Kanwar et al. 2024a).
Paper: The JDISC Survey: Linking the Physics and Chemistry of Inner and Outer Protoplanetary Disk Zones
Authors: Nicole Arulanantham, Colette Salyk, Klaus Pontoppidan, Andrea Banzatti, Ke Zhang, Karin Öberg, Feng Long, John Carr, Joan Najita, Ilaria Pascucci, María José Colmenares, Chengyan Xie, Jane Huang, Joel Green, Sean M. Andrews, Geoffrey A. Blake, Edwin A. Bergin, Paola Pinilla, Miguel Vioque, Emma Dahl, Eshan Raul, Sebastiaan Krijt
Figure caption: Retrieved temperatures from C2H2 (left), HCN (middle), and CO2 (right) vs. the median emitting masses measured from the best-fit slab models for each disk, with marker styles indicating the submillimeter dust substructures listed in Table 2. No significant correlations are observed for C2H2 or HCN (Spearman ρ = −0.1, −0.04; p = 0.6, 0.8), but we report a significant negative correlation between CO2 temperature and emitting mass (Spearman ρ = −0.55; p = 0.02).
Paper: The JDISC Survey: Linking the Physics and Chemistry of Inner and Outer Protoplanetary Disk Zones
Authors: Nicole Arulanantham, Colette Salyk, Klaus Pontoppidan, Andrea Banzatti, Ke Zhang, Karin Öberg, Feng Long, John Carr, Joan Najita, Ilaria Pascucci, María José Colmenares, Chengyan Xie, Jane Huang, Joel Green, Sean M. Andrews, Geoffrey A. Blake, Edwin A. Bergin, Paola Pinilla, Miguel Vioque, Emma Dahl, Eshan Raul, Sebastiaan Krijt
Figure caption: Left panel: C2H2 emission-line luminosities vs. [Ne II] emission-line fluxes. Right panel: C2H2 slab temperatures vs. [Ne III] to [Ne II] flux ratios. In both panels, marker colors represent mass accretion rates (see also, M. J. Colmenares et al. 2024). Upper limits are omitted from the plot and correlation coefficient calculation (see Table 9), due to the large uncertainty in the water removal at 15.555 μm.
Paper: The JDISC Survey: Linking the Physics and Chemistry of Inner and Outer Protoplanetary Disk Zones
Authors: Nicole Arulanantham, Colette Salyk, Klaus Pontoppidan, Andrea Banzatti, Ke Zhang, Karin Öberg, Feng Long, John Carr, Joan Najita, Ilaria Pascucci, María José Colmenares, Chengyan Xie, Jane Huang, Joel Green, Sean M. Andrews, Geoffrey A. Blake, Edwin A. Bergin, Paola Pinilla, Miguel Vioque, Emma Dahl, Eshan Raul, Sebastiaan Krijt
Figure caption: Correlations between best-fit parameters retrieved from single-temperature slab model fits to H2O emission lines between 12 and 17.5 μm. Although statistically significant, the correlation between emission-line luminosities and emitting masses (left) is significantly weaker (Spearman ρ = 0.66; p = 10−4) than what is observed for C2H2, HCN, and CO2 (see Figure 8). The single slab temperatures are not correlated with either the emission-line luminosities (middle; Spearman ρ = 0.35; p = 0.064) or emitting masses (right; Spearman ρ = −0.24; p = 0.21).
Paper: The JDISC Survey: Linking the Physics and Chemistry of Inner and Outer Protoplanetary Disk Zones
Authors: Nicole Arulanantham, Colette Salyk, Klaus Pontoppidan, Andrea Banzatti, Ke Zhang, Karin Öberg, Feng Long, John Carr, Joan Najita, Ilaria Pascucci, María José Colmenares, Chengyan Xie, Jane Huang, Joel Green, Sean M. Andrews, Geoffrey A. Blake, Edwin A. Bergin, Paola Pinilla, Miguel Vioque, Emma Dahl, Eshan Raul, Sebastiaan Krijt
Figure caption: Water emission lines between 16.6 and 17.6 μm and [Ar II] emission lines for JDISCS spectra that are dominated by atomic features, with the best-fit H2O slab models overlaid (cyan). We place upper limits of ﹩{\mathrm{log}}\,{L}_{{\rm{emit}}}\lt -5.3,-4.3\,{L}_{\odot }﹩ for HD 142666 and HD 143006, respectively. The OH-rich spectrum of GM Aur will be presented in a forthcoming paper (C. E. Romero-Mirza et al. 2025, in preparation).
Paper: The JDISC Survey: Linking the Physics and Chemistry of Inner and Outer Protoplanetary Disk Zones
Authors: Nicole Arulanantham, Colette Salyk, Klaus Pontoppidan, Andrea Banzatti, Ke Zhang, Karin Öberg, Feng Long, John Carr, Joan Najita, Ilaria Pascucci, María José Colmenares, Chengyan Xie, Jane Huang, Joel Green, Sean M. Andrews, Geoffrey A. Blake, Edwin A. Bergin, Paola Pinilla, Miguel Vioque, Emma Dahl, Eshan Raul, Sebastiaan Krijt
Figure caption: Emission-line luminosities measured from the best-fit slab models vs. the infrared spectral indices measured between 13 and 26 μm (top) and the literature mass accretion rates (bottom). Both trends are consistent with the Spitzer results reported in A. Banzatti et al. (2020).
Paper: Metal-polluted White Dwarfs with 21 μm IR Excesses from JWST/MIRI: Planets or Dust?
Authors: John H. Debes, Sabrina Poulsen, Ashley Messier, Susan E. Mullally, Katherine Thibault, Loïc Albert, Misty Cracraft, Érika Le Bourdais, Patrick Dufour, Tom Barclay, J. J. Hermes, Mukremin Kilic, David Lafrenière, Fergal Mullally, William Reach, Elisa Quintana
Figure caption: Top panel: SED of WD 1202−232 and comparison to its predicted photospheric emission. The black line represents the model photosphere for the WD, the red asterisks are the predicted model fluxes in a given filter, and the black squares are archival photometry for the WD (See Table 1). The blue squares represent the observed JWST fluxes in F560W, F770W, F1500W, and F2100W. Bottom panel: residual photometry relative to the model photosphere, weighted by the photometric uncertainties. The black squares are archival photometry, while the blue squares represent the JWST photometry.
Paper: Metal-polluted White Dwarfs with 21 μm IR Excesses from JWST/MIRI: Planets or Dust?
Authors: John H. Debes, Sabrina Poulsen, Ashley Messier, Susan E. Mullally, Katherine Thibault, Loïc Albert, Misty Cracraft, Érika Le Bourdais, Patrick Dufour, Tom Barclay, J. J. Hermes, Mukremin Kilic, David Lafrenière, Fergal Mullally, William Reach, Elisa Quintana
Figure caption: Same as Figure 5, but for WD 2149+021. Note the significant 5.1σ excess at 21 μm.
Paper: Metal-polluted White Dwarfs with 21 μm IR Excesses from JWST/MIRI: Planets or Dust?
Authors: John H. Debes, Sabrina Poulsen, Ashley Messier, Susan E. Mullally, Katherine Thibault, Loïc Albert, Misty Cracraft, Érika Le Bourdais, Patrick Dufour, Tom Barclay, J. J. Hermes, Mukremin Kilic, David Lafrenière, Fergal Mullally, William Reach, Elisa Quintana
Figure caption: Same as Figure 5, but for WD 2105–820. Note the significant 5.6σ excess at 21 μm. Additionally, there is a tentative excess at 2.0σ at 15 μm.
Paper: Metal-polluted White Dwarfs with 21 μm IR Excesses from JWST/MIRI: Planets or Dust?
Authors: John H. Debes, Sabrina Poulsen, Ashley Messier, Susan E. Mullally, Katherine Thibault, Loïc Albert, Misty Cracraft, Érika Le Bourdais, Patrick Dufour, Tom Barclay, J. J. Hermes, Mukremin Kilic, David Lafrenière, Fergal Mullally, William Reach, Elisa Quintana
Figure caption: The four MIRI images of WD 1202−232. Each field represents 22″ × 22″, with the WD at the center.
Paper: Metal-polluted White Dwarfs with 21 μm IR Excesses from JWST/MIRI: Planets or Dust?
Authors: John H. Debes, Sabrina Poulsen, Ashley Messier, Susan E. Mullally, Katherine Thibault, Loïc Albert, Misty Cracraft, Érika Le Bourdais, Patrick Dufour, Tom Barclay, J. J. Hermes, Mukremin Kilic, David Lafrenière, Fergal Mullally, William Reach, Elisa Quintana
Figure caption: Same as Figure 1, but for WD 2149+021.
Paper: Metal-polluted White Dwarfs with 21 μm IR Excesses from JWST/MIRI: Planets or Dust?
Authors: John H. Debes, Sabrina Poulsen, Ashley Messier, Susan E. Mullally, Katherine Thibault, Loïc Albert, Misty Cracraft, Érika Le Bourdais, Patrick Dufour, Tom Barclay, J. J. Hermes, Mukremin Kilic, David Lafrenière, Fergal Mullally, William Reach, Elisa Quintana
Figure caption: Same as Figure 1, but for WD 1620−391.
Paper: Metal-polluted White Dwarfs with 21 μm IR Excesses from JWST/MIRI: Planets or Dust?
Authors: John H. Debes, Sabrina Poulsen, Ashley Messier, Susan E. Mullally, Katherine Thibault, Loïc Albert, Misty Cracraft, Érika Le Bourdais, Patrick Dufour, Tom Barclay, J. J. Hermes, Mukremin Kilic, David Lafrenière, Fergal Mullally, William Reach, Elisa Quintana
Figure caption: Same as Figure 5, but for WD 1620−391.
Paper: Metal-polluted White Dwarfs with 21 μm IR Excesses from JWST/MIRI: Planets or Dust?
Authors: John H. Debes, Sabrina Poulsen, Ashley Messier, Susan E. Mullally, Katherine Thibault, Loïc Albert, Misty Cracraft, Érika Le Bourdais, Patrick Dufour, Tom Barclay, J. J. Hermes, Mukremin Kilic, David Lafrenière, Fergal Mullally, William Reach, Elisa Quintana
Figure caption: Same as Figure 1, but for WD 2105–820.
Paper: The JDISC Survey: Linking the Physics and Chemistry of Inner and Outer Protoplanetary Disk Zones
Authors: Nicole Arulanantham, Colette Salyk, Klaus Pontoppidan, Andrea Banzatti, Ke Zhang, Karin Öberg, Feng Long, John Carr, Joan Najita, Ilaria Pascucci, María José Colmenares, Chengyan Xie, Jane Huang, Joel Green, Sean M. Andrews, Geoffrey A. Blake, Edwin A. Bergin, Paola Pinilla, Miguel Vioque, Emma Dahl, Eshan Raul, Sebastiaan Krijt
Figure caption: MIRI spectra of select targets from the JDISCS sample, representing broad categories of sources, namely: intermediate-mass, transition disk (with a large dust cavity), solar-mass with weak water emission, solar-mass with strong water emission, and a low-mass star. Emission lines from prominent atomic and molecular gas, and solid state features, are highlighted with labels.