adsabs/AstroCLIMB huggingface dataset:
Paper: Limits on Planetary-mass Primordial Black Holes from the OGLE High-cadence Survey of the Magellanic Clouds
Authors: Przemek Mróz, Andrzej Udalski, Michał K. Szymański, Igor Soszyński, Paweł Pietrukowicz, Szymon Kozłowski, Radosław Poleski, Jan Skowron, Krzysztof Ulaczyk, Mariusz Gromadzki, Krzysztof Rybicki, Patryk Iwanek, Marcin Wrona, Mateusz J. Mróz
Figure caption: Gray dots mark the proper motions of red clump stars in the field LMC503.08. The proper motion of LMC503.08.18967 is marked with a blue circle.
Paper: Limits on Planetary-mass Primordial Black Holes from the OGLE High-cadence Survey of the Magellanic Clouds
Authors: Przemek Mróz, Andrzej Udalski, Michał K. Szymański, Igor Soszyński, Paweł Pietrukowicz, Szymon Kozłowski, Radosław Poleski, Jan Skowron, Krzysztof Ulaczyk, Mariusz Gromadzki, Krzysztof Rybicki, Patryk Iwanek, Marcin Wrona, Mateusz J. Mróz
Figure caption: Event detection efficiency in the field LMC509 as a function of Einstein timescale (upper panel) and normalized source radius (lower panel).
Paper: JWST/MIRI Detection of [Ne V], [Ne VI], and [O IV] Wind Emission in the O9 V Star 10 Lacertae
Authors: David R. Law, Calum Hawcroft, Linda J. Smith, Alexander W. Fullerton, Christopher J. Evans, Karl D. Gordon, Nimisha Kumari, Claus Leitherer
Figure caption: MIRI MRS spectrum of 10 Lac from PID 1524 plotted in Rayleigh–Jeans units. Dashed and dotted–dashed vertical gray lines, respectively, indicate H I and He II photospheric emission features due to non-LTE effects, and dashed red lines indicate highly ionized broad stellar wind [Ne VI], [Ne V], and [O IV] transitions. The extremely broad depression around 10 μm is a known silicate dust absorption feature.
Paper: Observational Signatures of Dust Traffic Jams in Polar-aligning Circumbinary Disks
Authors: Jeremy L. Smallwood, Rebecca Nealon, Hsi-Wei Yen, Christophe Pinte, Cristiano Longarini, Hossam Aly, Min-Kai Lin
Figure caption: Top panel: the density-weighted average of the disk inclination for the gas (black) and dust components, s = 0.7 cm (blue), s = 1.2 cm (red), s = 2.1 cm (green), and s = 3.7 cm (purple). Bottom panel: the azimuthally averaged dust surface density, Σd, as a function disk radius, r, and time in binary orbital periods, P orb. The color bar denotes the dust surface density. The multiple dust rings are labeled by grain size, s. The colored dots indicate the location of the dust traffic jam at the end of the simulation for each dust size: s = 0.7 cm (blue), s = 1.2 cm (red), s = 2.1 cm (green), and s = 3.7 cm (purple).
Paper: Observational Signatures of Dust Traffic Jams in Polar-aligning Circumbinary Disks
Authors: Jeremy L. Smallwood, Rebecca Nealon, Hsi-Wei Yen, Christophe Pinte, Cristiano Longarini, Hossam Aly, Min-Kai Lin
Figure caption: The dust structure of a nearly polar dusty circumbinary disk with multiple dust species. The center image shows the circumbinary disk represented by all dust species. Each dust species is individually rendered and shown in the smaller panels: s = 0.7 cm, s = 1.2 cm, s = 2.1 cm, and s = 3.7 cm. All panels view the disk in the y–z plane at 1000 P orb. The color denotes the dust surface density. The differential precession between the gas and dust during polar alignment produces multiple dust rings with radial locations depending on the grain size.
Paper: Observational Signatures of Dust Traffic Jams in Polar-aligning Circumbinary Disks
Authors: Jeremy L. Smallwood, Rebecca Nealon, Hsi-Wei Yen, Christophe Pinte, Cristiano Longarini, Hossam Aly, Min-Kai Lin
Figure caption: Top left panel: the azimuthally averaged flux density, I, as a function of distance from the image center from Figure 3 for wavelengths 0.6 cm (dark blue), 1.2 cm (gray), and 2.4 cm (yellow). The fluxes at 1.2 and 2.4 cm are scaled such that their initial flux profile (at t = 0 P orb) is equal to the initial flux profile of 0.6 cm. The vertical dashed lines correspond to the locations of the dust traffic jams at t = 1000 P orb for each grain size, s = 0.7 cm (blue), s = 1.2 cm (red), s = 2.1 cm (green), and s = 3.7 cm (purple) from the bottom panel in Figure 2. Top right panel: the cumulative flux density as a function of distance from the image center from Figure 3 for each wavelength. Bottom panel: a close-up of the azimuthally averaged flux density centered on the outer dust traffic jam, with the beam sizes of ALMA (at 40 GHz), ngVLA (at 27 GHz), and SKA (at 11.9 GHz) overlaid as yellow, green, and red patches, respectively.
Paper: Observational Signatures of Dust Traffic Jams in Polar-aligning Circumbinary Disks
Authors: Jeremy L. Smallwood, Rebecca Nealon, Hsi-Wei Yen, Christophe Pinte, Cristiano Longarini, Hossam Aly, Min-Kai Lin
Figure caption: The dust continuum emission at wavelengths 0.6 cm (top left), 1.2 cm (top right), and 2.4 cm (bottom left). Bottom right panel: the spectral index, α, of the dust continuum emission at wavelengths of 0.6 and 2.4 cm, which reveals differences in the dust structure at different grain sizes. The emission from the two stars are also shown. The estimated beam size for ALMA at ∼40 GHz (yellow) is shown in the bottom left corner of each panel. The smaller subpanel below compares the beam sizes of ngVLA at ∼27 GHz (green) and SKA at ∼11.9 GHz (red) with that of ALMA.
Paper: Observational Signatures of Dust Traffic Jams in Polar-aligning Circumbinary Disks
Authors: Jeremy L. Smallwood, Rebecca Nealon, Hsi-Wei Yen, Christophe Pinte, Cristiano Longarini, Hossam Aly, Min-Kai Lin
Figure caption: The size of St ∼ 1 dust particles as a function of radius r evaluated for different values of the surface density radial profile p, with the disk mass M  d  = 0.01 (top row), and for different values of M  d , with p = 1 (bottom row). Each column represents a different value of x out = r out/r in. The yellow, green, and red shaded regions represent the observational windows of ALMA (0.03 cm; 0.75 cm), ngVLA (0.26 cm; 25 cm), and SKA (2 cm; 3.6 cm), respectively. We highlight the region in the disk where we expect to observe the dust traffic jams (black shaded region) based on the results of our simulations from Figure 2.
Paper: X-Ray Weak Active Galactic Nuclei from Super-Eddington Accretion onto Infant Black Holes
Authors: Piero Madau, Francesco Haardt
Figure caption: Sketch illustrating the super-Eddington corona-funnel model discussed in the main text. Embedded in a funnel-like reflection geometry, the inner hot corona will cool down by Comptonizing a largely isotropic soft radiation field. The resulting X-ray spectra are predicted to be extremely soft, independently of the detailed geometry of the corona.
Paper: Cross-field Diffusion Effects on Particle Transport in a Solar Coronal Flux Rope
Authors: Edin Husidic, Nicolas Wijsen, Luis Linan, Michaela Brchnelova, Rami Vainio, Stefaan Poedts
Figure caption: Visualization of the flux rope CME modeled in COCONUT. The three panels show the evolved flux rope at three different times: at t = 0.48 hr (panel (a)), t = 1.53 hr (panel (b)), and t = 3.06 hr (panel (c)). The sphere of 1 R ⊙ with the mapped radial magnetic field component symbolizes the Sun. The colors of the sphere and flux rope denote the magnetic field’s polarity, where red shades describe positive polarity, blue shades describe negative polarity, and white color stands for zero values. The black lines illustrate a sample of the global magnetic field.
Paper: Probing the Origin of the Star Formation Excess Discovered by JWST through Gamma-Ray Bursts
Authors: Tatsuya Matsumoto, Yuichi Harikane, Keiichi Maeda, Kunihito Ioka
Figure caption: The evolution of the cosmic SFR density. The black curve shows the SFR density obtained in the “pre-JWST” era. The red triangles denote the lower limit of the SFR density estimated by the spectroscopically confirmed galaxy sample obtained by JWST in Y. Harikane et al. (2024b). The gray open points also show the SFR density obtained by other observations, taken from Y. Harikane et al. (2024b). The SFR density shows an excess beyond z ≳ 10, which we call the “JWST excess” and may be represented by the red solid line. The gray dashed curve shows the SFR density of P. Madau & M. Dickinson (2014), which is frequently used in GRB population studies. The SFR density is estimated by multiplying the conversion factor to the UV luminosity density (on the right axis; see the text).
Paper: Probing the Origin of the Star Formation Excess Discovered by JWST through Gamma-Ray Bursts
Authors: Tatsuya Matsumoto, Yuichi Harikane, Keiichi Maeda, Kunihito Ioka
Figure caption: (Top) Intrinsic (beaming-corrected) GRB formation rate for different scenarios. Red and blue solid curves show the rate of GS22 and the rate extended beyond z > 6 in proportion to the pre-JWST SFR. The latter overlaps with the former below z < 6 and has a constant GRB formation efficiency η GRB. Dashed curves show the same as the solid ones but boosted in proportion to the SFR excess for z > 10. Orange and light-blue triangles represent the GRB rate excess corresponding to the JWST excess (see Figure 2) in this scenario. Dotted curves show the case where the JWST excess is caused by a transition of IMF from Salpeter to top-heavy shape over 10 ≲ z ≲ 11.3. For the models of the SFR excess (red dashed) and IMF transition (red dotted), ΨGRB is artificially suppressed for z ≳ 14. (Bottom) GRB formation efficiency corresponding to models in the top panel, defined by Equation (9) for the pre-JWST SFR, ρ SFR (black curve in Figure 2).
Paper: Probing the Origin of the Star Formation Excess Discovered by JWST through Gamma-Ray Bursts
Authors: Tatsuya Matsumoto, Yuichi Harikane, Keiichi Maeda, Kunihito Ioka
Figure caption: (Top) Prediction for the redshift distribution of GRBs detected by EP. Color and types of curves correspond to the same meaning as in Figure 3. The upper arrow represents a redshift range over which LRDs might be a host galaxy of GRBs; see the discussion in Section 5. (Bottom) The cumulative number of GRBs detected by EP. The upward triangle means an expected lower limit based on the detection of EP240315a.
Paper: Probing the Origin of the Star Formation Excess Discovered by JWST through Gamma-Ray Bursts
Authors: Tatsuya Matsumoto, Yuichi Harikane, Keiichi Maeda, Kunihito Ioka
Figure caption: Origin of the JWST excess implied by the behavior of the GRB event rate for z ≳ 10. If the GRB rate shows an excess at z ≳ 10 proportional to the JWST excess (the red or blue dashed curves in Figure 4), an excess of the SFR is an origin of the JWST excess (Case A). If the GRB rate shows an excess larger than the JWST excess (the red or blue dotted curves), the IMF transition causes the JWST excess (Case B). If there is no excess in the GRB rate (the red or blue solid curves), AGN activity is responsible for the JWST excess (Case C).
Paper: Probing the Origin of the Star Formation Excess Discovered by JWST through Gamma-Ray Bursts
Authors: Tatsuya Matsumoto, Yuichi Harikane, Keiichi Maeda, Kunihito Ioka
Figure caption: Gamma-ray spectra of a GRB with luminosity L = 1052 erg s−1 at different redshifts. The red and blue shaded regions and dashed lines represent the energy bands and sensitivities of EP WXT and Swift BAT, respectively. The black dotted curve shows the spectrum of EP240315a with L ≃ 1.2 × 1053 erg s−1 and z ≃ 4.9 (Y. Liu et al. 2024).
Paper: Probing the Origin of the Star Formation Excess Discovered by JWST through Gamma-Ray Bursts
Authors: Tatsuya Matsumoto, Yuichi Harikane, Keiichi Maeda, Kunihito Ioka
Figure caption: The same as Figures 3 and 4 but for the GRB formation rate and LF of G.-X. Lan et al. (2021; L21, left) and J. T. Palmerio & F. Daigne (2021; PD21, right), respectively.
Paper: Cross-field Diffusion Effects on Particle Transport in a Solar Coronal Flux Rope
Authors: Edin Husidic, Nicolas Wijsen, Luis Linan, Michaela Brchnelova, Rami Vainio, Stefaan Poedts
Figure caption: Intensity contour plots illustrating particle escape from the flux rope. The 2D plots show the particle intensities at the outer boundary of the domain. The top row contains the results for the Larmor radius-dependent λ ⊥, where α = 10 in panel (a), α = 5 in panel (b), and α = 1 in panel (c). The bottom row contains the results for the model with ﹩{\lambda }_{\perp }=\mathrm{const}﹩, where λ ⊥ = 2.150 × 10−2 R ⊙ in panel (d), λ ⊥ = 1.075 × 10−2 R ⊙ au in panel (e), and 2.150 × 10−3 R ⊙ in panel (f).
Paper: Cross-field Diffusion Effects on Particle Transport in a Solar Coronal Flux Rope
Authors: Edin Husidic, Nicolas Wijsen, Luis Linan, Michaela Brchnelova, Rami Vainio, Stefaan Poedts
Figure caption:                         Contour plots of the Larmor radius–dependent perpendicular MFP λ                      ⊥ (panel (a)) in the case of α = 5 (corresponding to results shown in the middle row of Figure 4) and of the α parameter (panel (b)) based on the case of a constant MFP of 1.075 × 10−2                      R                      ⊙ (corresponding to the middle row of Figure 3). The contours are shown in the two planes perpendicular to the CME.
Paper: Cross-field Diffusion Effects on Particle Transport in a Solar Coronal Flux Rope
Authors: Edin Husidic, Nicolas Wijsen, Luis Linan, Michaela Brchnelova, Rami Vainio, Stefaan Poedts
Figure caption: 3D particle intensity plots illustrating possible sources of numerical diffusion. Panels (a) through (c) are based on a COCONUT snapshot cadence of about 5, 15, and 20 minutes, respectively, with a minimal time step of ﹩{\rm{\Delta }}{t}_{\min }={10}^{-4}﹩ s in PARADISE, while in panel (d) the same COCONUT snapshot cadence is used as in panel (a) but with ﹩{\rm{\Delta }}{t}_{\min }=5\,{\rm{s}}﹩. The same injection samples as in Section 3 have been used for this comparison.
Paper: Cross-field Diffusion Effects on Particle Transport in a Solar Coronal Flux Rope
Authors: Edin Husidic, Nicolas Wijsen, Luis Linan, Michaela Brchnelova, Rami Vainio, Stefaan Poedts
Figure caption: Comparing results of the unstructured COCONUT grid and the interpolated structured grid at t = 1.04 (top row) and 2.01 hr (bottom row). Panels (a) and (c) show 3D plots of the particle intensity contours using the unstructured COCONUT grid, while panels (b) and (d) show the results using the interpolated structured grid.
Paper: Magnetic Field Evolution of the Solar Active Region 13664
Authors: Robert Jarolim, Astrid M. Veronig, Stefan Purkhart, Peijin Zhang, Matthias Rempel
Figure caption: Overview of the temporal evolution of unsigned magnetic flux ∣B  z ∣, magnetic energy E, free magnetic energy E free, and the ratio between the free magnetic energy and magnetic energy (E free/E) of AR 13664 and the observed GOES X-ray flux. Blue lines correspond to the 1 hr running average smoothed quantities, while red lines refer to the first order time derivatives of those quantities. Blue and orange shaded bars indicate M- and X-class flares, respectively. The bars outline the flare start to end times, according to the GOES flare catalog. The black dotted lines indicate the zero level of the time derivatives. The gray dashed line shows the considered −0.5 × 10−6 s−1 threshold to relate the model results to the flaring activity.
Paper: Magnetic Field Evolution of the Solar Active Region 13664
Authors: Robert Jarolim, Astrid M. Veronig, Stefan Purkhart, Peijin Zhang, Matthias Rempel
Figure caption: Example of a supposed separatrix layer and relation to the modeled magnetic field on 2024 May 8 03:00 UT. (a) The observed vertical component of the magnetic field with the outline of the subregion, which is illustrated in panels (b)–(e). The red arrow indicates the supposed separatrix layer in the SDO/AIA EUV observation in the 131 Å filter during a solar flare event (b). We can identify the separatrix layer as a current-free layer in the vertically integrated current density (c). The black and white contours outline the ±1000 G threshold of the magnetic field in panel (a). The squashing factor at a height of 5 Mm outlines different magnetic domains (d). Here, the separatrix layer appears as a clear separation line. From the magnetic field line plot we can further identify the different magnetic domains in the solar atmosphere (e). The color coding refers to the local current density j.
Paper: Magnetic Field Evolution of the Solar Active Region 13664
Authors: Robert Jarolim, Astrid M. Veronig, Stefan Purkhart, Peijin Zhang, Matthias Rempel
Figure caption: Major solar flares during 2024 May 7–11 and their magnetic energy distribution. The left column shows for each event the AIA 94 Å EUV map time integrated over the flare duration. The middle column shows the corresponding vertically integrated maps of free magnetic energy E free, which outline the primary regions where energy can be released. The right column shows the vertically integrated change in magnetic energy, indicating where energy is decreased (blue) or increased (red) over the event duration. The red contours in the integrated EUV maps indicate the 1012 erg cm−2 level of energy depletion (ΔE −). For the X-class events we note a relation between the observed EUV emission and regions of magnetic energy change, both in terms of energy depletion (extended blue regions) and energy increase (red regions).
Paper: Magnetic Field Evolution of the Solar Active Region 13664
Authors: Robert Jarolim, Astrid M. Veronig, Stefan Purkhart, Peijin Zhang, Matthias Rempel
Figure caption: Comparison of the temporal evolution of the modeled vertically integrated current density (left) and the observed SDO/AIA 131 Å filtergrams (right) for the X3.9 flare and filament eruption on 2024 May 10 ((a)–(f)). (g) Difference map between first and last current density map. The blue arrows indicate the reconfiguration of the magnetic flux rope, visible in the current density map. The black arrow highlights the current-free layer, which undergoes substantial reconfiguration during the flare and associated filament eruption.
Paper: Magnetic Field Evolution of the Solar Active Region 13664
Authors: Robert Jarolim, Astrid M. Veronig, Stefan Purkhart, Peijin Zhang, Matthias Rempel
Figure caption: Metrics for divergence freeness (top) and force freeness (bottom) over the evolution of the AR. The dashed line indicates the start of major flux emergence (see Figure 1). The decrease of θ  J can be related to the increase in magnetic currents.
Paper: Magnetic Field Evolution of the Solar Active Region 13664
Authors: Robert Jarolim, Astrid M. Veronig, Stefan Purkhart, Peijin Zhang, Matthias Rempel
Figure caption: Uncertainty maps prior to the X3.9 and X5.8 flares. We show the vertically integrated current density of the five ensemble runs and the corresponding standard deviation at the top. The bottom plots show the reference magnetogram and the corresponding uncertainty maps. The stronger projection effects on 2024 May 11 01:00 lead to a substantial increase in uncertainty toward the west limb.
Paper: X-Ray Weak Active Galactic Nuclei from Super-Eddington Accretion onto Infant Black Holes
Authors: Piero Madau, Francesco Haardt
Figure caption: Equilibrium electron temperature (θ = kTe/mec2) of the hot coronal phase (lower curves) and the resulting photon index Γ of the X-ray Comptonized component (upper curves). The corona has an assumed electron scattering opacity of τ = 0.5, comparable to the value inferred in Seyfert galaxies. Two values, fc = 1/2 and fc = 1/3, have been assumed for the fraction of the locally generated radiation power that is dissipated in the corona. The parameter m on the horizontal axis measures the strength of the incoming external radiation field in units of the net flux. In our two supercritical thick disk models, we estimate m ≃ 3 (Model A) and m ≃ 2 (Model B) at the bottom of the funnel.
Paper: X-Ray Weak Active Galactic Nuclei from Super-Eddington Accretion onto Infant Black Holes
Authors: Piero Madau, Francesco Haardt
Figure caption: Meridional cross sections (over one quadrant) for the supercritical thick disks described by Models A (magenta line) and B (green line). As rin decreases, rout increases as does the ratio L/LEdd, while the efficiency of mass to energy conversion drops. Smaller values of rin imply steeper and deeper funnels, where pressure gradients are balanced by centrifugal forces rather than by gravity and luminosities exceed the Eddington limit. The square symbols mark the location on the surface inside which 90% of the disk luminosity Lrad is actually emitted. The inset shows the Keplerian specific angular momentum distribution for the adopted pseudo-Newtonian potential (black line) and the angular momentum distributions corresponding to our supercritical disks (Models A and B).
Paper: X-Ray Weak Active Galactic Nuclei from Super-Eddington Accretion onto Infant Black Holes
Authors: Piero Madau, Francesco Haardt
Figure caption: The funnel regions of supercritical disks around black holes. The two configurations (Models A and B) have funnel opening half-angles of ﹩{\rm{\Theta }}=\mathrm{arccot}{(h/r)}_{\max }=35^\circ ﹩ and 44°, respectively. The dot on each funnel indicates the point where h/r reaches a maximum, and the percentage next to it denotes the fraction of total disk luminosity emitted interior to that point.
Paper: The Green Monster Hiding in Front of Cas A: JWST Reveals a Dense and Dusty Circumstellar Structure Pockmarked by Ejecta Interactions
Authors: Ilse De Looze, Dan Milisavljevic, Tea Temim, Danielle Dickinson, Robert Fesen, Richard G. Arendt, Jeremy Chastenet, Salvatore Orlando, Jacco Vink, Michael J. Barlow, Florian Kirchschlager, Felix D. Priestley, John C. Raymond, Jeonghee Rho, Nina S. Sartorio, Tassilo Scheffler, Franziska Schmidt, William P. Blair, Ori Fox, Christopher Fryer, Hans-Thomas Janka, Bon-Chul Koo, J. Martin Laming, Mikako Matsuura, Dan Patnaude, Mónica Relaño, Armin Rest, Judy Schmidt, Nathan Smith, Niharika Sravan
Figure caption: Multiwavelength view of the GM ring in position P2 (see Figure 1) showing the NIRCam F162M (PSF FWHM: 0.″055), F356W (PSF FWHM: 0.″116), and F444W (PSF FWHM: 0.″145) images (top row); NIRCam+MIRI RGB image (F444W, F1000W, and F1800W with PSF FWHMs of 0.″145, 0.″328, and 0.″591, respectively) and MRS line flux maps for the [Ne II] 12.81 μm (PSF FWHM: ∼0.″529) and [Ne III] 15.56 μm (PSF FWHM: ∼0.″619) lines (middle row); and MRS [Fe II] 17.94 μm (PSF FWHM: ∼0.″698) and NIRSpec Brα 4.05 μm (PSF FWHM: ∼0.″15) line flux maps for the near v rad = 0 km s−1 velocity component and a multicolor RGB image comparing the dust with the line emission (bottom row). The images are at their native resolution; the FWHM of the PSF has been indicated in parentheses here for guidance. Each of the cutouts has the same 5″ × 5″ field of view. The green or black circle with a radius of 0.″8 overlaid on the continuum and line emission maps serves to guide the eye when comparing dust continuum, synchrotron, and line emission in this region.
Paper: The Green Monster Hiding in Front of Cas A: JWST Reveals a Dense and Dusty Circumstellar Structure Pockmarked by Ejecta Interactions
Authors: Ilse De Looze, Dan Milisavljevic, Tea Temim, Danielle Dickinson, Robert Fesen, Richard G. Arendt, Jeremy Chastenet, Salvatore Orlando, Jacco Vink, Michael J. Barlow, Florian Kirchschlager, Felix D. Priestley, John C. Raymond, Jeonghee Rho, Nina S. Sartorio, Tassilo Scheffler, Franziska Schmidt, William P. Blair, Ori Fox, Christopher Fryer, Hans-Thomas Janka, Bon-Chul Koo, J. Martin Laming, Mikako Matsuura, Dan Patnaude, Mónica Relaño, Armin Rest, Judy Schmidt, Nathan Smith, Niharika Sravan
Figure caption: Spectral mapping of the GM ring region in position P2 (see Figure 1) for the high-velocity (v = 5000 km s−1) ejecta component (top row) and the stationary ISM component (bottom row). For the high-velocity ejecta component, maps are shown of the line flux (left column), line velocity (middle column), and FWHM line width (right column) for the [O IV] 25.89 μm (first row), [Ne II] 12.81 μm (second row), and [Ne III] 15.56 μm (third row) lines. The line flux, line velocity, and line width maps of the H2 (0, 0) 17.03 μm line of interstellar origin are shown in the bottom panels. The green circle roughly outlines the position of the ring in MIRI dust continuum maps (see Figure 7) and is overlaid on the line maps to guide the eye.