adsabs/AstroCLIMB huggingface dataset:
Paper: Strong NUV Refractory Absorption and Dissociated Water in the Hubble Transmission Spectrum of the Ultra Hot Jupiter KELT-20 b
Authors: Yayaati Chachan, Joshua Lothringer, Julie Inglis, Hayley Beltz, Heather A. Knutson, Jessica Spake, Bjorn Benneke, Ian Wong, Zafar Rustamkulov, David Sing, Katherine A. Bennett
Figure caption: Compositional constraints for KELT-20 b from this work (solid circle and empty circle correspond to chemical equilibrium retrievals with PETRA and petitRADTRANS, respectively). The C/O = ﹩0.{1}_{-0.1}^{+0.4}﹩ is from L. Finnerty et al. (2025), WASP-178 b (solid square) is from J. D. Lothringer et al. (2025), and WASP-121 b is from S. Pelletier et al. (2025; solid diamond) and P. C. B. Smith et al. (2024; empty diamond). The composition tracks corresponding to accretion in different regions of the disk are based on the models in Y. Chachan et al. (2023). For the sake of comparison, we assume solar composition for the host stars but note that these tracks depend on the stellar elemental ratios and would be different for WASP-121.
Paper: Strong NUV Refractory Absorption and Dissociated Water in the Hubble Transmission Spectrum of the Ultra Hot Jupiter KELT-20 b
Authors: Yayaati Chachan, Joshua Lothringer, Julie Inglis, Hayley Beltz, Heather A. Knutson, Jessica Spake, Bjorn Benneke, Ian Wong, Zafar Rustamkulov, David Sing, Katherine A. Bennett
Figure caption: Comparison of KELT-20 b’s NUV-NIR spectrum with published transit spectra for HAT-P-41 b (H. R. Wakeford et al. 2020), WASP-178 b (J. D. Lothringer et al. 2022, 2025), and WASP-121 b (STIS/E230M; D. K. Sing et al. 2019). The transit spectra are normalized to their equilibrium scale height (assuming a mean molecular weight of 2.3). For KELT-20 b, we assume a mass of 2MJup to calculate the surface gravity for the scale height. While HAT-P-41 b is conspicuously featureless at NUV wavelengths, all three hotter planets show strong NUV absorption, extending over 10 scale heights.
Paper: Strong NUV Refractory Absorption and Dissociated Water in the Hubble Transmission Spectrum of the Ultra Hot Jupiter KELT-20 b
Authors: Yayaati Chachan, Joshua Lothringer, Julie Inglis, Hayley Beltz, Heather A. Knutson, Jessica Spake, Bjorn Benneke, Ian Wong, Zafar Rustamkulov, David Sing, Katherine A. Bennett
Figure caption: The posteriors for the parameters fitted to the elemental abundance ratios from S. Gandhi et al. (2023). The red line shows the median temperature–pressure profile from S. Gandhi et al. (2023). The other colored lines correspond to temperature–pressure profiles from Figure 14, with magenta indicating the nightside from GCMs (solid: 0G, dashed: 5G) and green for the median profile from the chemical equilibrium retrieval with PETRA.
Paper: Strong NUV Refractory Absorption and Dissociated Water in the Hubble Transmission Spectrum of the Ultra Hot Jupiter KELT-20 b
Authors: Yayaati Chachan, Joshua Lothringer, Julie Inglis, Hayley Beltz, Heather A. Knutson, Jessica Spake, Bjorn Benneke, Ian Wong, Zafar Rustamkulov, David Sing, Katherine A. Bennett
Figure caption: The measured elemental abundance ratios (violin plots) from S. Gandhi et al. (2023) and the fitted values from our models (red lines). All ratios are normalized to the solar value. Our model is able to account for all of the observed elemental ratios with the exception of vanadium, which appears to be depleted beyond our model predictions.
Paper: Strong NUV Refractory Absorption and Dissociated Water in the Hubble Transmission Spectrum of the Ultra Hot Jupiter KELT-20 b
Authors: Yayaati Chachan, Joshua Lothringer, Julie Inglis, Hayley Beltz, Heather A. Knutson, Jessica Spake, Bjorn Benneke, Ian Wong, Zafar Rustamkulov, David Sing, Katherine A. Bennett
Figure caption: East (left hemisphere) and west (right hemisphere) limbs from the two GCMs presented in this work, plotted in altitude space. The black hash marks correspond to a pressure of roughly 10−4 bars. The 5G model has smaller limb asymmetries than the 0G model and is favored by the data.
Paper: Revealing the Bifurcations of the Milky Way Spiral Arms Based on Hi-GAL and ATLASGAL Clumps
Authors: Deyun Kong, Ye Xu, Dejian Liu, Yiwei Dong, Zehao Lin, Yingjie Li, Chaojie Hao
Figure caption: Left: LSR velocity distribution of Hi-GAL clumps within the longitude range 5° < ℓ < 35°. Panels (a), (b), and (c) show the velocity distribution for three longitude ranges: panel (a) 25° < ℓ < 35° (green), panel (b) 15° < ℓ < 25° (orange), and panel (c) 5° < ℓ < 15° (blue). The regions marked by the purple dashed box, lime solid box, brown dashed box, and dark pink solid box are converted to the XY diagram using the rotation curve and are represented in Figure 3 with the same colors and line styles. Middle: LSR velocity distribution of Hi-GAL clumps within 5° < ℓ < 25° in the left panel evenly divided into four ranges. Black dashed lines in panels (e) and (f) mark reference velocities of 10 and 55 km s−1, respectively. Right: LSR velocity distribution for clumps in 9° < ℓ < 21° in the middle panel evenly divided into four ranges. Black dashed lines in panel (j) mark reference velocities of 20 and 40 km s−1, respectively. The gray dashed lines indicate the multi-Gaussian fitting of the distributions. The peaks are identified as “Per” (Perseus) and “Sag” (Sagittarius).
Paper: Revealing the Bifurcations of the Milky Way Spiral Arms Based on Hi-GAL and ATLASGAL Clumps
Authors: Deyun Kong, Ye Xu, Dejian Liu, Yiwei Dong, Zehao Lin, Yingjie Li, Chaojie Hao
Figure caption: The left and right parts of the figure represent the first and fourth Galactic quadrants, respectively. Panels (a) and (d) show the distribution of Hi-GAL (cyan dots) and ATLASGAL (gray dots) clumps in the ℓ–v diagram. The red solid line indicates the terminal velocity, and the light-red shaded region represents velocity within ±15 km s−1 of the terminal velocity. Panels (b) and (e) present statistical results for the Hi-GAL clumps, while panels (c) and (f) correspond to the statistics of the ATLASGAL clumps. The histogram utilizes 1° longitude bins, and the vertical axis is relative number (defined as the number of sources in each bin divided by the total number of filtered sources in this quadrant). The darker blue dots and lines correspond to the peak and FWHM of Gaussian fitting, respectively. The black dashed lines represent the Gaussian fitting lines for the peaks.
Paper: Revealing the Bifurcations of the Milky Way Spiral Arms Based on Hi-GAL and ATLASGAL Clumps
Authors: Deyun Kong, Ye Xu, Dejian Liu, Yiwei Dong, Zehao Lin, Yingjie Li, Chaojie Hao
Figure caption: Schematic view from the north Galactic pole showing the Xu23 model. The purple dashed region (15° < ℓ < 35°) corresponds to the VLSR > 60 km s−1 range. The lime solid region (15° < ℓ < 35°) corresponds to the 30 km s−1 < VLSR < 65 km s−1 range. The brown dashed region (15° < ℓ < 35°) marks the −10 km s−1 < VLSR < 30 km s−1 range. The dark pink solid region (5° < ℓ < 15°) highlights sources with between −10 and 65 km s−1.
Paper: Revealing the Bifurcations of the Milky Way Spiral Arms Based on Hi-GAL and ATLASGAL Clumps
Authors: Deyun Kong, Ye Xu, Dejian Liu, Yiwei Dong, Zehao Lin, Yingjie Li, Chaojie Hao
Figure caption: The Hi-GAL clump number histogram, with a longitude range of 9° < ℓ < 18° and a radial velocity of 20 ∼ 40 km s−1. The black dashed lines are at 13﹩\mathop{.}\limits^{\unicode{x000b0}}﹩5 and 15﹩\mathop{.}\limits^{\unicode{x000b0}}﹩5, respectively. The peak position is an indication of the bifurcation point that occurs at 14﹩\mathop{.}\limits^{\unicode{x000b0}}﹩6 ± 0﹩\mathop{.}\limits^{\unicode{x000b0}}﹩3. The gray dashed lines indicate the multi-Gaussian fitting results.
Paper: Revealing the Bifurcations of the Milky Way Spiral Arms Based on Hi-GAL and ATLASGAL Clumps
Authors: Deyun Kong, Ye Xu, Dejian Liu, Yiwei Dong, Zehao Lin, Yingjie Li, Chaojie Hao
Figure caption: Spatial distribution of Hi-GAL (left) and ATLASGAL (right) clumps projected onto the Galactic XY-plane. Sources associated with the Sagittarius (purple), Perseus (black), Centaurus (red), and Norma (vivid blue) arms are highlighted near the bifurcation region. The merged Sagittarius–Perseus arm structure is marked in cobalt blue, while the merged Norma–Centaurus arm is shown in green. Unassociated clumps are indicated by orange dots. Zoomed insets of the bifurcation regions are shown in the top-left and bottom-right corners. In the right panel, the definition of the azimuthal angle β is provided, it is the angle between the source position and the Sun-Galactic center line. The background gray-scale spiral arms are from Xu23 model. Based on the tangent points results of Section 3.1, the 3 kpc arm is incorporated into the Xu23 model and shown as a dark gray shaded region.
Paper: Revealing the Bifurcations of the Milky Way Spiral Arms Based on Hi-GAL and ATLASGAL Clumps
Authors: Deyun Kong, Ye Xu, Dejian Liu, Yiwei Dong, Zehao Lin, Yingjie Li, Chaojie Hao
Figure caption: Left: The radial velocity distributions of Hi-GAL clumps in the region 300° < ℓ < 340°. The peaks are identified as “Nor” (Norma) and “Cen” (Centaurus). The vertical dashed lines indicate characteristic velocity ranges for each arm. Panels (b)–(d) mark velocity boundaries at −70, −55, and −30 km s−1 (black dashed lines, left to right). Panel (e) indicates transition velocities at −60 and −35 km s−1, respectively. Right: The Galactic longitude range is 324° < ℓ < 340°, which divided into four subregions. The black dashed lines in panels (f) and (g) mark velocity boundaries at −70, −55, and −30 km s−1 (left to right). The black dashed lines in panel (h) mark the velocity boundaries at −60 and −40 km s−1. In both left and right, the gray dashed lines show Gaussian fitting of the distributions.
Paper: Revealing the Bifurcations of the Milky Way Spiral Arms Based on Hi-GAL and ATLASGAL Clumps
Authors: Deyun Kong, Ye Xu, Dejian Liu, Yiwei Dong, Zehao Lin, Yingjie Li, Chaojie Hao
Figure caption: The Galactic plane viewed from the north Galactic pole. The background gray-scale spiral arms are from the Xu23 model. The blue dashed circle marks the heliocentric radius of 6 kpc. The orange solid region (300° < ℓ < 332°, and −55 km s−1 < VLSR < −30 km s−1), the dark-red dashed region (308° < ℓ < 332°, and −70 km s−1 < VLSR < −55 km s−1), and the magenta solid region (332° < ℓ < 340°, and −60 km s−1 < VLSR < −35 km s−1) correspond to “Nor” (Norma arm), “Cen” (Centaurus arm), and the merged arm, respectively.
Paper: Revealing the Bifurcations of the Milky Way Spiral Arms Based on Hi-GAL and ATLASGAL Clumps
Authors: Deyun Kong, Ye Xu, Dejian Liu, Yiwei Dong, Zehao Lin, Yingjie Li, Chaojie Hao
Figure caption: Left: The ℓ–b distribution of Hi-GAL clumps. Group 1: Perseus arm sources (dark gray); group 2: Sagittarius arm sources (light gray triangle); group 3: bifurcation point sources (brown). The dark orange diamonds, blue squares, and green points with error bars (±1σ) represent the mean Galactic latitude 1° longitude bins for each population, respectively. The orange line and the sky blue dashed line represent the linear fitting results of the sources on the Perseus arm and the Sagittarius arm, respectively. Right: The histograms of source distributions for the three source populations.
Paper: Revealing the Bifurcations of the Milky Way Spiral Arms Based on Hi-GAL and ATLASGAL Clumps
Authors: Deyun Kong, Ye Xu, Dejian Liu, Yiwei Dong, Zehao Lin, Yingjie Li, Chaojie Hao
Figure caption: The left and right panels show the distribution of Hi-GAL compact sources and ATLASGAL clumps, respectively, as a function of Galactic longitude. The black dashed lines at 331﹩\mathop{.}\limits^{\unicode{x000b0}}﹩2 and 334﹩\mathop{.}\limits^{\unicode{x000b0}}﹩8, from left to right, encompass the distribution peaks. The peak of the Hi-GAL compact source distribution is located at 333﹩\mathop{.}\limits^{\unicode{x000b0}}﹩1 ± 0﹩\mathop{.}\limits^{\unicode{x000b0}}﹩6, while the peak of the ATLASGAL clump distribution is at 333﹩\mathop{.}\limits^{\unicode{x000b0}}﹩0 ± 0﹩\mathop{.}\limits^{\unicode{x000b0}}﹩7. The gray dashed lines indicate the multi-Gaussian fitting results.
Paper: Revealing the Bifurcations of the Milky Way Spiral Arms Based on Hi-GAL and ATLASGAL Clumps
Authors: Deyun Kong, Ye Xu, Dejian Liu, Yiwei Dong, Zehao Lin, Yingjie Li, Chaojie Hao
Figure caption: The distribution of ATLASGAL clumps, with the Galactic latitude segmented and color coded in the same way as in Figure 6.
Paper: Revealing the Bifurcations of the Milky Way Spiral Arms Based on Hi-GAL and ATLASGAL Clumps
Authors: Deyun Kong, Ye Xu, Dejian Liu, Yiwei Dong, Zehao Lin, Yingjie Li, Chaojie Hao
Figure caption: The ℓ–b distributions of Hi-GAL (left) and ATLASGAL (right) clumps. Group 4: Norma arm sources (light gray triangle); group 5: Centaurus arm sources (dark gray); group 6: bifurcation point sources (brown). Orange diamonds, blue squares, and green points with error bars (±1σ) represent the mean Galactic latitude 2° longitude bins for each population, respectively. The blue line and the orange line represent the linear fitting results of the sources on Norma arm and Centaurus arm, respectively.
Paper: Investigating Phosphorus Abundances in a Sample of APOGEE-2 Bulge Globular Clusters
Authors: Beatriz Barbuy, José G. Fernández-Trincado, Morgan S. Camargo, Doug Geisler, Maren Brauner, Sandro Villanova, Dante Minniti, Domingo Anibal García-Hernández, Stefano O. Souza, Heitor Ernandes, Amâncio Friaça, Marco Pignatari
Figure caption: [P/Fe] vs. [Fe/H] for the present results compared with literature data. Dark green open stars: present work; red-filled circles: E. Caffau et al. (2011); red open circles: E. Caffau et al. (2016); blue-filled triangles: I. U. Roederer et al. (2014); filled cyan circles and open black circles: Z. G. Maas et al. (2019); light-gray filled circles: G. Nandakumar et al. (2022); light-gray open four-sided stars: Z. G. Maas et al. (2022); red open stars: B. Barbuy et al. (2025). Different model lines correspond to the outputs of models computed for radii r < 0.5, 0.5 < r < 1, 1 < r  < 2, and 2 < r  < 3 kpc from the Galactic center. Black lines correspond to specific star formation ν = 1 Gyr−1, red lines to ν = 3 Gyr−1.
Paper: Investigating Phosphorus Abundances in a Sample of APOGEE-2 Bulge Globular Clusters
Authors: Beatriz Barbuy, José G. Fernández-Trincado, Morgan S. Camargo, Doug Geisler, Maren Brauner, Sandro Villanova, Dante Minniti, Domingo Anibal García-Hernández, Stefano O. Souza, Heitor Ernandes, Amâncio Friaça, Marco Pignatari
Figure caption: P I lines and CO lines in star Ton 1: 2M17343616–3903344 for stellar parameters from Abdurro’uf et al. (2022) and ASPCAP parameters, with Teff = 3890 K and 3982 K, respectively. CO line intensity changes more dramatically in the temperature range.
Paper: Investigating Phosphorus Abundances in a Sample of APOGEE-2 Bulge Globular Clusters
Authors: Beatriz Barbuy, José G. Fernández-Trincado, Morgan S. Camargo, Doug Geisler, Maren Brauner, Sandro Villanova, Dante Minniti, Domingo Anibal García-Hernández, Stefano O. Souza, Heitor Ernandes, Amâncio Friaça, Marco Pignatari
Figure caption: [P/Fe] vs. [N/O] (upper panel) and [Al/Fe] vs. [N/O] (lower panel) for Ton 1 (green squares) and NGC 6316 (red squares).
Paper: Investigating Phosphorus Abundances in a Sample of APOGEE-2 Bulge Globular Clusters
Authors: Beatriz Barbuy, José G. Fernández-Trincado, Morgan S. Camargo, Doug Geisler, Maren Brauner, Sandro Villanova, Dante Minniti, Domingo Anibal García-Hernández, Stefano O. Souza, Heitor Ernandes, Amâncio Friaça, Marco Pignatari
Figure caption: P I 16482.932 Å line in four stars in Ton 1 (rows 1 and 2) and NGC 6316 (rows 3 and 4), fitted with synthetic spectra computed with [P/Fe] = 0.0 (green), 1.0 (blue, and final values (red) if different from 0.0 or 1.0. Synthetic spectra computed with molecular lines only are shown as dotted lines.
Paper: Investigating Phosphorus Abundances in a Sample of APOGEE-2 Bulge Globular Clusters
Authors: Beatriz Barbuy, José G. Fernández-Trincado, Morgan S. Camargo, Doug Geisler, Maren Brauner, Sandro Villanova, Dante Minniti, Domingo Anibal García-Hernández, Stefano O. Souza, Heitor Ernandes, Amâncio Friaça, Marco Pignatari
Figure caption: [P/Fe] vs. Teff and [P/Fe] vs. log g, for stellar parameters from references cited in the text, and ASPCAP parameters.
Paper: JWST/MIRI Imaging of the Warm Dust Component of the ϵ Eridani Debris Disk
Authors: Schuyler G. Wolff, András Gáspár, George Rieke, Jarron M. Leisenring, Antranik A. Sefilian, Marie Ygouf, Jorge Llop-Sayson
Figure caption: The background on blank sky at 25.5 μm, near δ Eri (Background 1) and ϵ Eri (Background 2), scaled linearly between 820 and 1000 MJy sr−1. The latent patterns imprinted on the detector, following the observation of δ Eri, are apparent in background 2 (and in the difference image, shown in the bottom panel, scaled between −8 and 8 MJy sr−1). The background imaged at ϵ Eri is on average 0.84 MJy sr−1 brighter than the one at δ Eri.
Paper: JWST/MIRI Imaging of the Warm Dust Component of the ϵ Eridani Debris Disk
Authors: Schuyler G. Wolff, András Gáspár, George Rieke, Jarron M. Leisenring, Antranik A. Sefilian, Marie Ygouf, Jorge Llop-Sayson
Figure caption: Results of the ellipse fitting to the 60.5 MJy sr−1 contour of the F2550W image of ϵ Eri. The MCMC results are well constrained for all parameters except the argument of periastron (ω), as expected. The upper-right corner shows the derived (x, y) coordinates for the contour value (blue) alongside a sample of 250 models drawn from the chain. The 16%, 50%, and 84% quantiles are shown with dashed lines and listed in Table 2.
Paper: JWST/MIRI Imaging of the Warm Dust Component of the ϵ Eridani Debris Disk
Authors: Schuyler G. Wolff, András Gáspár, George Rieke, Jarron M. Leisenring, Antranik A. Sefilian, Marie Ygouf, Jorge Llop-Sayson
Figure caption: The final data products of our JWST/MIRI ϵ Eri observations at the four wavelengths of the observations. Images are oriented north up and east to the left, with a displayed FOV of 28﹩\mathop{.}\limits^{\unicode{x02033}}﹩16 × 28﹩\mathop{.}\limits^{\unicode{x02033}}﹩16 to highlight the bright, inner disk regions. The outer planetesimal belt (observed by ALMA at ∼70 au) is not detected and is outside the FOV of these images.
Paper: JWST/MIRI Imaging of the Warm Dust Component of the ϵ Eridani Debris Disk
Authors: Schuyler G. Wolff, András Gáspár, George Rieke, Jarron M. Leisenring, Antranik A. Sefilian, Marie Ygouf, Jorge Llop-Sayson
Figure caption: False-color combination image, using all four MIRI imaging wavelength bands. For scale, we display the spatial extent of the giant planets in the solar system, highlighting that we are spatially resolving a relatively extended disk component in the ϵ Eri system.
Paper: JWST/MIRI Imaging of the Warm Dust Component of the ϵ Eridani Debris Disk
Authors: Schuyler G. Wolff, András Gáspár, George Rieke, Jarron M. Leisenring, Antranik A. Sefilian, Marie Ygouf, Jorge Llop-Sayson
Figure caption: Snapshots from the DiskDyn ϵ Eri simulation at 25.5 μm (top to bottom), with the dynamic effects of ϵ Eri b and that of SW drag and PR drag included. Images are shown for both relative planet–disk inclinations modeled (ι = 0° and 10°), as well as convolved with the F2550W PSF and at MIRI pixel scale resolution (0﹩\mathop{.}\limits^{^{\prime\prime} }﹩11). The first four columns have a FOV of 56″, while the last two are zoomed in to 13﹩\mathop{.}\limits^{^{\prime\prime} }﹩75. The position of ϵ Eri b is shown in the zoomed-in panels with blue circles.
Paper: JWST/MIRI Imaging of the Warm Dust Component of the ϵ Eridani Debris Disk
Authors: Schuyler G. Wolff, András Gáspár, George Rieke, Jarron M. Leisenring, Antranik A. Sefilian, Marie Ygouf, Jorge Llop-Sayson
Figure caption: Left panel: the β values for radiation and stellar wind (SW) calculated for the ϵ Eri system (see system variables described in the text). Middle panel: the ratio of the SW and PR drag forces in the system (note the increase in SW drag forces, due to the increase in aberration angle; see text). Right panel: the total drag timescale in the ϵ Eri system as a function of particle radius from the outer Kuiper Belt–analog ring located at 64 au, due to the combined effects of SW and PR drag.
Paper: JWST/MIRI Imaging of the Warm Dust Component of the ϵ Eridani Debris Disk
Authors: Schuyler G. Wolff, András Gáspár, George Rieke, Jarron M. Leisenring, Antranik A. Sefilian, Marie Ygouf, Jorge Llop-Sayson
Figure caption: Derived disk photometry from the four MIRI imager observations are compared to the photosphere-corrected Spitzer/IRS spectrum (K. Y. L. Su et al. 2017) and flux estimates available in the literature corrected to only include inner disk flux as described in S. G. Wolff et al. (2023). Values agree to within 1σ. The red diamond is derived from HOSTS survey nulling interferometry (S. Ertel et al. 2020), corrected approximately for the interferometer response. It is insensitive to any emission outside about 1″.
Paper: JWST/MIRI Imaging of the Warm Dust Component of the ϵ Eridani Debris Disk
Authors: Schuyler G. Wolff, András Gáspár, George Rieke, Jarron M. Leisenring, Antranik A. Sefilian, Marie Ygouf, Jorge Llop-Sayson
Figure caption: The SED of the DiskDyn models over the 10 Myr evolution of our models. We plot broadband photometry values from S. G. Wolff et al. (2023), with the inner disk flux values included (see Tables 2 and 4 in their paper).
Paper: JWST/MIRI Imaging of the Warm Dust Component of the ϵ Eridani Debris Disk
Authors: Schuyler G. Wolff, András Gáspár, George Rieke, Jarron M. Leisenring, Antranik A. Sefilian, Marie Ygouf, Jorge Llop-Sayson
Figure caption: The evolution of the radial distance of the particles as a function of particle size, simulated using DiskDyn.
Paper: JWST/MIRI Imaging of the Warm Dust Component of the ϵ Eridani Debris Disk
Authors: Schuyler G. Wolff, András Gáspár, George Rieke, Jarron M. Leisenring, Antranik A. Sefilian, Marie Ygouf, Jorge Llop-Sayson
Figure caption: Radiative transfer modeling results for the extended disk emission and PSF residual spokes resulting from unresolved warm dust emission. The MCFOST model for the best-fit parameters (center) given in Table 3 is compared with the MIRI 18 μm observations (left). Observation – model residuals are shown on the right. Despite some core residuals resulting from an imperfect reference PSF, the model does an excellent job of fitting both the extended disk emission and the residual spokes.
Paper: JWST/MIRI Imaging of the Warm Dust Component of the ϵ Eridani Debris Disk
Authors: Schuyler G. Wolff, András Gáspár, George Rieke, Jarron M. Leisenring, Antranik A. Sefilian, Marie Ygouf, Jorge Llop-Sayson
Figure caption: The radial profile for the MIRI 25.5 μm observations are compared to the MIPS and SOFIA radial profiles. The outer extent of the disk is consistent. While the MIRI profile shows a brighter peak closer into the central star and is fainter in the outer regions of the disk, this can be explained by PSF convolution. The dotted line shows the MIRI profile smoothed by a 1D Gaussian filter consistent with the MIPS 24 μm PSF FWHM.
Paper: JWST/MIRI Imaging of the Warm Dust Component of the ϵ Eridani Debris Disk
Authors: Schuyler G. Wolff, András Gáspár, George Rieke, Jarron M. Leisenring, Antranik A. Sefilian, Marie Ygouf, Jorge Llop-Sayson
Figure caption: Radial profiles of the deprojected images of ϵ Eri for the four wavelengths. The vertical shaded regions represent the location of the region potentially cleared by the planet candidate ϵ Eri b (gray), and the planetesimal belt observed with ALMA (red). While a small enhancement of the disk surface brightness is possibly discernible at the location of the cold outer belt at 15 μm, this is not seen at longer wavelengths.
Paper: JWST/MIRI Imaging of the Warm Dust Component of the ϵ Eridani Debris Disk
Authors: Schuyler G. Wolff, András Gáspár, George Rieke, Jarron M. Leisenring, Antranik A. Sefilian, Marie Ygouf, Jorge Llop-Sayson
Figure caption: Posterior distributions from the MCMC fit to the 18 μm image using a two-disk-component MCFOST radiative transfer model. The 16%, 50%, and 84% quantiles are shown with dashed lines and listed in Table 3.