adsabs/AstroCLIMB huggingface dataset:
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) near-rest-frame velocities. Maps are shown of the line flux (left column), line velocity (middle column), and FWHM line width (right column) for low-velocity components of the [Ne II] 12.81 μm (first row), [Ne III] 15.56 μm (second row), [Fe II] 17.94 μm (third row), and Brα (fourth row) lines. The green circle roughly outlines the position of the ring in MIRI dust continuum maps, with the same circle overlaid on the GM images shown in Figure 7.
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: Structure of a circumstellar shell after interaction with the remnant at the age of Cas A, as derived from a three-dimensional hydrodynamic simulation (run W15-IIb-sh-HD-1eta-az in S. Orlando et al. 2022). Left panel: three-dimensional volume rendering of the particle density of the shocked shell material (density integrated along the line of sight). Only the upper right quadrant of the numerical domain is shown. The three white square regions mark holes, which are shown enlarged in Figure 10, in comparison with similar structures observed with JWST. Right panel: detail of the structure of the ejecta and their interaction with the shell at the age of Cas A. The semi-opaque irregular isosurfaces correspond to a value of ejecta density, which is at 1% of the peak density; their colors represent the radial velocity in units of 1000 km s−1 on the isosurface (the color coding is defined in the bottom left corner of the panel). The three-dimensional volume rendering in green describes the particle density of the shocked shell material (see color bar on the right of the panel).
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: Left: the locations of dense CSM clumps, often called QSFs, as traced by Hα emission. The figure was adapted from R. A. Fesen (2001) to show a green outline of the location of the GM, which nicely fits in the middle of the formerly identified dense CSM knots. Right: multicolor MIRI image (blue: F1000W, green: F1130W, red: F2550W) with contours indicating the locations of these dense QSFs as identified by B.-C. Koo et al. (2018).
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: A comparison between holes and rings observed with JWST (left panels) and analogous structures predicted by hydrodynamic simulations (right panels; S. Orlando et al. 2022) and identified in the white square regions in Figure 9.
Paper: Composition Variation of the 2023 May 16 Solar Energetic Particle Event Observed by SolO and PSP
Authors: Z. G. Xu, C. M. S Cohen, R. A. Leske, G. D. Muro, A. C. Cummings, D. J. McComas, N. A. Schwadron, E. R. Christian, M. E. Wiedenbeck, R. L. McNutt, D. G. Mitchell, G. M. Mason, A. Kouloumvakos, R. F. Wimmer-Schweingruber, G. C. Ho, J. Rodriguez-Pacheco
Figure caption: The Fe/O ratio and 4He/H ratio measured by PSP and SolO in both sunward and antisunward directions as a function of energy. The dashed lines in two panels indicate the averaged values of the He/H ratio (0.036) over 1–5 MeV nuc−1 and the Fe/O ratio (0.134) over 5–12 MeV nuc−1 for large SEP events (D. V. Reames 1995, 2017).
Paper: Composition Variation of the 2023 May 16 Solar Energetic Particle Event Observed by SolO and PSP
Authors: Z. G. Xu, C. M. S Cohen, R. A. Leske, G. D. Muro, A. C. Cummings, D. J. McComas, N. A. Schwadron, E. R. Christian, M. E. Wiedenbeck, R. L. McNutt, D. G. Mitchell, G. M. Mason, A. Kouloumvakos, R. F. Wimmer-Schweingruber, G. C. Ho, J. Rodriguez-Pacheco
Figure caption: Temporal variation of the Fe/O ratios and He/H ratios measured by PSP and SolO from the sunward and antisunward directions. Ratios calculated at common energies and using the scaled energy are shown; see the text for details. The statistical error bars of Fe/O are significantly below the y-axis scale after May 18 due to their lower counting statistics. To simplify the plot, we use downward arrows to indicate the lower limits of uncertainties.
Paper: Composition Variation of the 2023 May 16 Solar Energetic Particle Event Observed by SolO and PSP
Authors: Z. G. Xu, C. M. S Cohen, R. A. Leske, G. D. Muro, A. C. Cummings, D. J. McComas, N. A. Schwadron, E. R. Christian, M. E. Wiedenbeck, R. L. McNutt, D. G. Mitchell, G. M. Mason, A. Kouloumvakos, R. F. Wimmer-Schweingruber, G. C. Ho, J. Rodriguez-Pacheco
Figure caption: Two top panels: 4He observation on PSP/LET and PSP/HET. Two bottom panels: the radio observation on PSP/FIELD.
Paper: Rates and Beaming Angles of Gamma-Ray Bursts Associated with Compact Binary Coalescences
Authors: Shasvath J. Kapadia, Dimple, Dhruv Jain, Kuntal Misra, K. G. Arun, Resmi Lekshmi
Figure caption: Left panel: the posteriors on the rate of GRB-bright BNS mergers, ﹩p({R}_{\mathrm{GRB}}| {{ \mathcal N }}_{\mathrm{BNS}})﹩, estimated using Fermi data and Swift data. These are both broadly consistent with the GW BNS rate posterior p(R GW∣d GW). The 90% rate estimates are quoted on the top-left corner of the panel. The larger error bar on the Fermi rate estimates can be attributed to the larger uncertainty in the fraction of events in the BNS cluster that have a BNS provenance, as compared to the Swift rate estimates. Right panel: same as the left panel but for NSBHs. The Fermi and Swift rate estimates are broadly consistent with each other but are markedly smaller than the GW NSBH rate posterior, as expected.
Paper: Direct Measurements of Synchrotron-emitting Electrons at Near-Sun Shocks
Authors: I. C. Jebaraj, O. V. Agapitov, M. Gedalin, L. Vuorinen, M. Miceli, C. M. S. Cohen, A. Voshchepynets, A. Kouloumvakos, N. Dresing, A. Marmyleva, V. Krasnoselskikh, M. Balikhin, J. G. Mitchell, A. W. Labrador, N. Wijsen, E. Palmerio, L. Colomban, J. Pomoell, E. K. J. Kilpua, M. Pulupa, F. S. Mozer, N. E. Raouafi, D. J. McComas, S. D. Bale, R. Vainio
Figure caption: The brightness temperatures (T B) of the synchrotron emission for S1 and S2 are shown in panels (A) and (B). The inverse Compton scattering limit is explicitly stated in both panels and also represented by the blue dotted–dashed in panel (B).
Paper: Rates and Beaming Angles of Gamma-Ray Bursts Associated with Compact Binary Coalescences
Authors: Shasvath J. Kapadia, Dimple, Dhruv Jain, Kuntal Misra, K. G. Arun, Resmi Lekshmi
Figure caption: Left panel: constraints on the distribution of beaming fractions for GRBs with a BNS provenance, assuming that all BNSs produce GRBs. The constraints from Fermi are less stringent than those from Swift. The reason is the same as what was described in Figure 2 to explain the broader rate posteriors for Fermi as compared to Swift. Right panel: distributions of beaming fractions in the left panel converted to distributions of beaming angles θ  j  (in °). These span θ  j  ∈ [0.°8, 33.°5] across both Fermi and Swift estimates.
Paper: Rates and Beaming Angles of Gamma-Ray Bursts Associated with Compact Binary Coalescences
Authors: Shasvath J. Kapadia, Dimple, Dhruv Jain, Kuntal Misra, K. G. Arun, Resmi Lekshmi
Figure caption: Two-dimensional embeddings obtained using PCA-UMAP for Swift/BAT and Fermi/GBM catalogs. The red squares show the locations of KN-associated lGRBs. The blue squares show the locations of KN-associated sGRBs. GRB 170817A is highlighted in the red label, suggesting the origin of neighboring GRBs to be BNS mergers. Therefore, we assume clusters highlighted in orange to be a BNS cluster and those in cyan to be an NSBH cluster. The SN-associated GRBs are represented by the magenta color circles. Notice that some of these clusters contain known false positives. (See Dimple et al. 2023, 2024 for details.)
Paper: Direct Measurements of Synchrotron-emitting Electrons at Near-Sun Shocks
Authors: I. C. Jebaraj, O. V. Agapitov, M. Gedalin, L. Vuorinen, M. Miceli, C. M. S. Cohen, A. Voshchepynets, A. Kouloumvakos, N. Dresing, A. Marmyleva, V. Krasnoselskikh, M. Balikhin, J. G. Mitchell, A. W. Labrador, N. Wijsen, E. Palmerio, L. Colomban, J. Pomoell, E. K. J. Kilpua, M. Pulupa, F. S. Mozer, N. E. Raouafi, D. J. McComas, S. D. Bale, R. Vainio
Figure caption: The potential waveforms recorded by TDS on 2023 March 13, 07:04:17.301. (a) and (b) Two components of the electric field. (c) The magnetic field. (d) The potential recorded on antenna 1 (black) and 2 (red). Panels (e)–(h): waveforms recorded by FIELDS/TDS on 2022 September 5, 17:27:13.222.
Paper: Composition Variation of the 2023 May 16 Solar Energetic Particle Event Observed by SolO and PSP
Authors: Z. G. Xu, C. M. S Cohen, R. A. Leske, G. D. Muro, A. C. Cummings, D. J. McComas, N. A. Schwadron, E. R. Christian, M. E. Wiedenbeck, R. L. McNutt, D. G. Mitchell, G. M. Mason, A. Kouloumvakos, R. F. Wimmer-Schweingruber, G. C. Ho, J. Rodriguez-Pacheco
Figure caption: (A) The constellation of different spacecraft at the start of the SEP event, created by Solar Mach (J. Gieseler et al. 2023). The black arrow indicates the approximate longitudinal location of the flare. (B) The in situ observations of energetic particles from SolO/EPD SIS, EPT, and HET. From top to bottom, the panels are the dynamic spectra of protons, helium, oxygen, and iron. The bottom panel displays the magnetic field magnitude and its components. (C) The running difference image of the CME observed by SOHO/Lasco C2 at 18:00 on 2023 May 16. (D) The in situ PSP/IS⊙IS LET-A observations presented in the same format as panel (B). Note that the top axis of (B) and (D) indicates the radial distance of SolO and PSP from the Sun.
Paper: Composition Variation of the 2023 May 16 Solar Energetic Particle Event Observed by SolO and PSP
Authors: Z. G. Xu, C. M. S Cohen, R. A. Leske, G. D. Muro, A. C. Cummings, D. J. McComas, N. A. Schwadron, E. R. Christian, M. E. Wiedenbeck, R. L. McNutt, D. G. Mitchell, G. M. Mason, A. Kouloumvakos, R. F. Wimmer-Schweingruber, G. C. Ho, J. Rodriguez-Pacheco
Figure caption: The fluence spectra of H (purple), 4He (green), O (orange), and Fe (blue) integrated between 2023-05-16T17:00:00 and 2023-05-21T00:00:00. Spectra from SolO are shown as triangles, PSP/EPI-Lo as empty circles, and PSP/EPI-Hi as filled circles. The two panels in the left half present the spectra measured by the sunward telescopes, and the right half represents the spectra measured by the antisunward telescopes. The solid lines represent the best-fitted Band function (D. Band et al. 1993).
Paper: She’s Got Her Mother’s Hair: Unveiling the Origin of Black Hole Magnetic Fields through Stellar to Collapsar Simulations
Authors: Ore Gottlieb, Mathieu Renzo, Brian D. Metzger, Jared A. Goldberg, Matteo Cantiello
Figure caption: From top to bottom, as a function of the local freefall timescale: specific angular momentum profile (gray band brackets j ISCO(a BH = 0) and j ISCO(a BH = 1)); mass density (red) and enclosed mass (orange; right vertical axis); estimate of the accretion rate (magenta) and local infall velocity profile (cyan; right vertical axis); B-field components predicted by the TSD; Alfvén, TSD, and freefall local timescales (purple, yellow, and dashed gray, respectively); and estimated cumulative magnetic flux Φ, where the red band is the required flux to power a GRB jet (see text).
Paper: She’s Got Her Mother’s Hair: Unveiling the Origin of Black Hole Magnetic Fields through Stellar to Collapsar Simulations
Authors: Ore Gottlieb, Mathieu Renzo, Brian D. Metzger, Jared A. Goldberg, Matteo Cantiello
Figure caption: Mapping of the PNS poloidal magnetic field strength (left axis), flux (right axis), and (assumed temporally constant) mass accretion rate onto the PNS (horizontal axis) to the natal BH spin (color map), PNS spin-down energy released prior to BH formation (yellow contours; in logarithmic units), and logarithmic BZ jet power (black contours), assuming initial P 0 = 1ms. The BH cannot inherit the PNS field if the Alfvén radius fails to satisfy R A ≲ R NS (the excluded area is in gray). The dotted vertical (dashed horizontal) black lines delineate the estimated range of mass accretion rates (PNS dipole field) at the time of collapse from PNS simulations by M. Á. Aloy & M. Obergaulinger (2021, vertical lines; R. Raynaud et al. 2020, horizontal lines). The moderate spin leads to jets with a characteristic GRB power. The MAD state with η  ϕ  ≈ 1 is located deep in the gray zone, where the BH does not acquire the PNS field. The natal BH spin distribution does not change significantly for P 0 = 10 ms.
Paper: She’s Got Her Mother’s Hair: Unveiling the Origin of Black Hole Magnetic Fields through Stellar to Collapsar Simulations
Authors: Ore Gottlieb, Mathieu Renzo, Brian D. Metzger, Jared A. Goldberg, Matteo Cantiello
Figure caption: Not-to-scale illustration of the proposed model. Top: a rotating massive star (light blue) collapses, forming a rapidly rotating PNS (white) surrounded by an accretion disk (dark blue) due to the excess angular momentum of the innermost layers of the stellar core (Section 2). The magnetic field present in the progenitor star due to the TSD is too weak and/or small-scale (randomly oriented cyan loops) to contribute a substantial magnetic flux onto the compact object (Section 2.1). A convective dynamo within the rapidly spinning PNS efficiently generates a strong, ordered magnetic field (pink lines). Bottom: the PNS collapses into a moderately spinning BH (black). The accretion disk surrounding the PNS at the time of collapse quickly spreads inward viscously to the BH’s ISCO, anchoring the PNS’s magnetic field lines to the BH faster than the “balding” process. This enables the BH to form with strong magnetic fields already threading through it (Section 3). The strongly magnetized and moderately spinning BH then launches a pair of BZ jets (yellow) that break through the outer layers of the collapsing star and power GRB emission (Section 4).
Paper: She’s Got Her Mother’s Hair: Unveiling the Origin of Black Hole Magnetic Fields through Stellar to Collapsar Simulations
Authors: Ore Gottlieb, Mathieu Renzo, Brian D. Metzger, Jared A. Goldberg, Matteo Cantiello
Figure caption: Vertical slices of the logarithmic mass density in the simulated models, as measured at t = T  s . The black contours outline the magnetic field lines, where solid and dashed lines delineate positive and negative magnetic polarity, respectively. BHs with higher spins and magnetic fluxes retain the remnant poloidal field of the PNS to maintain steady jet launching. When the BH spin and the initial flux on the BH are low or an accretion disk is absent (model a9ΦhI), the BH cannot sustain a large-scale field. As a result, magnetic loops of opposite polarity are accreted onto the BH, causing the BH magnetic flux to reconnect and reduce the flux on the BH, resulting in the depletion of jets. Full 2D and 3D movies showcasing the evolution of the magnetic field on the BH in the simulations are available at doi:10.5281/zenodo.13901023 and http://www.oregottlieb.com/BH_field.html. There are 10 movies in the Zenodo repository corresponding to the different models outlined in Table 1.
Paper: She’s Got Her Mother’s Hair: Unveiling the Origin of Black Hole Magnetic Fields through Stellar to Collapsar Simulations
Authors: Ore Gottlieb, Mathieu Renzo, Brian D. Metzger, Jared A. Goldberg, Matteo Cantiello
Figure caption: Resolution test for 40 M ⊙, Z = 0.001 initially rotating at the 0.6ω crit model, which experiences rotationally induced chemically homogeneous evolution. The left panels show, from top to bottom, the specific angular momentum, density, temperature, and velocity profile as a function of radius at the onset of core collapse. The right panel shows the Hertzsprung–Russell diagram, where each dot marks 105 yr of evolution. The label indicates the number of mesh points at the onset of core collapse. The higher-resolution model was recomputed post–oxygen core depletion only.
Paper: She’s Got Her Mother’s Hair: Unveiling the Origin of Black Hole Magnetic Fields through Stellar to Collapsar Simulations
Authors: Ore Gottlieb, Mathieu Renzo, Brian D. Metzger, Jared A. Goldberg, Matteo Cantiello
Figure caption: Time evolution of physical quantities on the horizon. The magnetic field strength on the north pole (a) and integrated flux (b) illustrate that the BH retains high magnetization/flux when the initial magnetic field is strong or the BH spin is moderate or high. (c): the flux on the northern hemisphere indicates that in models in which magnetic flux reconnects away, negative polarity loops thread the horizon (dashed lines). The dimensionless flux (d), electromagnetic launching efficiency (e), and jet luminosity (f) of models with an initially strong magnetic field or moderate/high BH spin produce jets. Otherwise, if the BH spin and initial field are too low, or there is no disk to confine the jet, no outflows are observed.
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: Multicolor JWST/NIRCam and MIRI image of Cas A adapted from D. Milisavljevic et al. (2024) with the locations of the four MIRI MRS pointings overlaid as black squares. The green rectangular region marks the position of the GM, which is shown enlarged in Figure 2, whereas the magenta rectangles outline several regions of interest of which we provide a multiwavelength view in Figure 4. The explosion center is highlighted with a blue star. Beyond the coverage of the JWST images, we use a 2023 epoch HST image to fill in the emission in the background. The legend outlines the representation for each color in this multicolor image. The prominent green emission observed from the GM originates mostly from the MIRI/F1280W filter with contributions from MIRI/F1130W. The GM emission is not to be confused with the reverse-shocked Ne-rich ejecta visible in light green (representative of the bright Ne line in the F1280W filter). The reverse-shocked Ar-rich ejecta are instead mostly colored pink and white thanks to the Ar line contributions to the F770W filter and the dust continuum emission with a characteristic 21 μm peak significantly contributing to the F2100W and F2550W images. The forward-shocked CSM dust in the north, east, and west is colored red and orange owing to the circumstellar dust emission peaking in the F2100W and F2550W filters.
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 zoomed in on a few specific regions of interest (see the boxes in Figure 1 for their specific locations). The first column shows RGB images (blue: NIRCam/F444W; green: MIRI/F1000W; red: MIRI/F1800W) of each position, with the subsequent columns presenting the HST/F625W, NIRCam/F162M, NIRCam/F444W, MIRI/F1000W, and MIRI/F2550W images. The HST/F625W and NIRCam/F162M images have the contours of previously identified dense circumstellar clumps (QSFs) in deep [Fe II]+[Si I] (B.-C. Koo et al. 2018) imaging overlaid in green.
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: Line profiles for the brightest lines observed with NIRSpec and MIRI/MRS for the specific ring in the GM located in position P2 with the velocity on the x-axis, calculated relative to the rest-frame wavelength in vacuum for each of the transitions (see Table 1) and the line flux density (in units of MJy sr−1) on the y-axis. The spectra were grouped depending on whether the emission originates from quasi-stationary (v near 0 km s−1) CSM (yellow box), high-velocity ejecta material (red box), or interstellar material (blue box). In case of the neon lines, there is a contribution from quasi-stationary CSM near the rest-frame velocity and high-velocity ejecta material near 5000 km s−1. The vertical dotted lines indicate different velocity components with blueshifts of −4900, −2350, −1750, −1250, and −550 km s−1 (in blue); a rest-frame velocity of 0 km s−1 (in green); and redshifts of +950, +1550, +4000, +4400, and +4950 km s−1 (in red) in the top three panels in the right column. The other panels have vertical lines overlaid to highlight velocity components with a rest-frame velocity of 0 km s−1 (in green) and a redshift of +4950 km s−1 (in red).