adsabs/AstroCLIMB huggingface dataset:
Paper: Pinching of ICME Flux Rope: Unprecedented Multipoint Observations of Internal Magnetic Reconnection during Gannon’s Superstorm
Authors: Shibotosh Biswas, Ankush Bhaskar, Anil Raghav, Ajay Kumar, Kalpesh Ghag, Smitha V. Thampi, Vipin K Yadav
Figure caption: Comparison of DSCOVR, ACE, and Wind data during the ICME flux-rope interval. Panels display the IMF magnitude, its components, solar wind velocity components, density, and temperature in a boundary-normal coordinate system (LMN). The gaps in ACE observations are due to the unavailability of observations.
Paper: Pinching of ICME Flux Rope: Unprecedented Multipoint Observations of Internal Magnetic Reconnection during Gannon’s Superstorm
Authors: Shibotosh Biswas, Ankush Bhaskar, Anil Raghav, Ajay Kumar, Kalpesh Ghag, Smitha V. Thampi, Vipin K Yadav
Figure caption: Spacecraft positions in geocentric solar ecliptic (GSE) coordinate system on 2024 May 10 at 22:00 UT.
Paper: The Gravitational-wave Background from Massive Black Holes in the ASTRID Simulation
Authors: Nianyi Chen, Tiziana Di Matteo, Yihao Zhou, Luke Zoltan Kelley, Laura Blecha, Yueying Ni, Simeon Bird, Yanhui Yang, Rupert Croft
Figure caption: Left column: GW production efficiency from past mergers of each local remnant BH as a function of their present-day masses at f = 0.125 yr−1 (4 nHz; top) and at f = 0.625 yr−1 (20 nHz; bottom). We characterize this efficiency as a fraction of an optimal strain (﹩{h}_{s,\mathrm{optimal}}^{2}﹩) expected per local BH (see text for details). The prediction from ASTRID merger trees is shown in green. We also illustrate the effect of merging BHs without a dynamical friction phase (yellow). Middle: cumulative mass growth by merger assuming no dynamical friction time compared to the real ASTRID mergers. We show the relative merger mass growth for local remnant BHs in three mass bins. Right column: BH mass function (top) and GWB (bottom) comparison between the ASTRID merger and a merger tree constructed without a DF phase.
Paper: The Gravitational-wave Background from Massive Black Holes in the ASTRID Simulation
Authors: Nianyi Chen, Tiziana Di Matteo, Yihao Zhou, Luke Zoltan Kelley, Laura Blecha, Yueying Ni, Simeon Bird, Yanhui Yang, Rupert Croft
Figure caption: GW strain distribution of the GWB sources from the ASTRID and TNG300 simulations. Top: the ﹩{h}_{s}^{2}﹩ distribution weighted by the amplitude in the second (f2 ≃ 4 nHz; red) and tenth (f10 ≃ 20 nHz,; blue) frequency bins of the NG15 data. The shaded regions shows the actual strains contributing to the GWB. The dashed curves show potential foreground sources where the total expected occurrence is 1. For reference, we show in vertical lines the strain corresponding to an Mtot = 6.4 × 108 M⊙ and an Mtot = 5.4 × 109 M⊙ equal-mass binary at z = 0.3. Bottom: the ratio between the ASTRID high-frequency (solid blue) and TNG300 low (red shaded) and high (blue shaded) strain distributions to the ASTRID low-frequency distribution.
Paper: Discovery of the Antiglitch in PSR J1835-1106
Authors: Mingyang Wang, Peng Liu, Jianping Yuan, Ang Li, Youli Tuo, Shijun Dang, Weihua Wang, Mingyu Ge, Xia Zhou, Na Wang
Figure caption: The antiglitch of PSR J1835−1106. Gray dashed lines mark the epochs at which the glitches occur, with the event numbers indicated in parentheses above. Panel (a) shows the timing residuals, where filled squares represent data from the Nanshan 26 m telescope and open squares correspond to data from the Parkes 64 m telescope. Panel (b) displays the relative change in spin frequency, defined as the difference between the observed spin frequency and that predicted by the preglitch timing model. Panel (c) presents the temporal evolution of the spin-frequency derivative.
Paper: The Gravitational-wave Background from Massive Black Holes in the ASTRID Simulation
Authors: Nianyi Chen, Tiziana Di Matteo, Yihao Zhou, Luke Zoltan Kelley, Laura Blecha, Yueying Ni, Simeon Bird, Yanhui Yang, Rupert Croft
Figure caption: Distribution of total mass, mass ratio, and redshift of MBHBs weighted by their contribution to the GWB (﹩{h}_{s}^{2}﹩) at f = 0.125 yr−1 and f = 0.625 yr−1. We compare the populations from ASTRID (green) and TNG300 (purple) with the best-fit semianalytical model from NG15-binary (gray dashed). For the 2D distribution, we plot the peak of each distribution with crosses and the 68% contribution contour around the peak. For ASTRID, we also plot the 95% contour in light green.
Paper: The Gravitational-wave Background from Massive Black Holes in the ASTRID Simulation
Authors: Nianyi Chen, Tiziana Di Matteo, Yihao Zhou, Luke Zoltan Kelley, Laura Blecha, Yueying Ni, Simeon Bird, Yanhui Yang, Rupert Croft
Figure caption: Merging timescale of massive mergers (Mtot > 2 × 108 M⊙) in ASTRID. Top: distribution of the merging timescale from galaxy pairing (Δr < 30 kpc) to numerical merger (Δr ∼ 1 kpc for ASTRID; red) and from 5 kpc to numerical merger (blue). Bottom: the MBH merging timescale below 5 kpc plotted against the mass ratio q. For comparison, we also plotted widely adopted analytical galaxy merging (S. Chen et al. 2019) and dynamical friction timescales (J. Binney & S. Tremaine 2008; F. Dosopoulou & F. Antonini 2017).
Paper: Discovery of the Antiglitch in PSR J1835-1106
Authors: Mingyang Wang, Peng Liu, Jianping Yuan, Ang Li, Youli Tuo, Shijun Dang, Weihua Wang, Mingyu Ge, Xia Zhou, Na Wang
Figure caption: Average pulse profiles of PSR J1835−1106 in the ±300 days interval surrounding the antiglitch.
Paper: Coexistence of Longitudinal and Transverse Oscillations in Polar Plumes Observed with Solar Orbiter/Extreme Ultraviolet Imager
Authors: Upasna Baweja, Vaibhav Pant, S. Krishna Prasad, Arpit Kumar Shrivastav, Tom Van Doorsselaere, Nancy Narang, Cis Verbeeck, M. Saleem Khan, David Berghmans
Figure caption: TD maps of the fine-scale substructures in Slits 2, 3, and 4. The slit numbers are mentioned at the top of each TD map. The cyan line depicts the speed of the propagating disturbances.
Paper: High-redshift Merger-induced Bar-like Galaxies in IllustrisTNG
Authors: Ewa L. Łokas
Figure caption: Evolution of different measures of shape (left column) and mass (right column) over time for the four bar-like galaxies. In the left-column panels, the lines show the axis ratios b/a (blue) and c/a (red), the triaxiality parameter T (green), the bar mode A2 (black), and the rotation parameter f (magenta) of the stellar component. In the right-column panels, the lines show the total galaxy mass in dark matter (blue), stars (red), and gas (green). The dark masses are given in units of 1012 M⊙, while the stellar and gas masses are in units of 1011 M⊙. Vertical solid lines in all panels indicate the selected time tsel at or after bar formation. Vertical dashed lines in the upper six panels indicate pericenter passages around a cluster-sized object. The galaxies are identified by their subhalo ID numbers at z = 0 given at the right of each panel.
Paper: High-redshift Merger-induced Bar-like Galaxies in IllustrisTNG
Authors: Ewa L. Łokas
Figure caption: Face-on images of the bar-like galaxies at redshift zsel, as they would be observed in the F444W filter of JWST. The galaxies are identified by their IDs at zsel given at the top of each panel and listed in the sixth column of Table 1.
Paper: High-redshift Merger-induced Bar-like Galaxies in IllustrisTNG
Authors: Ewa L. Łokas
Figure caption: Profiles of bar mode, A2(R),  for the bar-like galaxies at selected times. Measurements were carried out in bins of ΔR = 0.5 kpc.
Paper: High-redshift Merger-induced Bar-like Galaxies in IllustrisTNG
Authors: Ewa L. Łokas
Figure caption: Evolution of the profiles of the bar mode, A2(R), in the four galaxies over time. Measurements were carried out in bins of ΔR = 0.5 kpc. The galaxies are identified by their subhalo ID numbers at z = 0 given at the right of each panel.
Paper: Imaging and Radio Signatures of Shock–Plasmoid Interaction
Authors: Pankaj Kumar, Judith T. Karpen, P. K. Manoharan, N. Gopalswamy
Figure caption: Kinematics of the blob, CME/shock, and associated radio signatures. (a) and (b) Time–distance intensity plot along the slits PQ (shown in Figure 3(d)) and RS (shown in Figure 2(a1)) using LASCO C2 and STEREO-A COR-2 images. The vertical green line marks the onset of the interaction between the CME-driven shock and the slowly moving blob at ≈19:24 UT. LE indicates the leading edge of the CME. The blue dashed curve represents the second-order polynomial fit to the blob, while the red dashed curve shows the linear fit to the CME shock. (c) and (d) Dynamic radio spectra from Wind/WAVES (0.02–13.85 MHz) and STEREO-A/WAVES (0.2–16 MHz). The vertical white line marks the onset of the interaction between the CME-driven shock and the slowly moving blob. (e) SEP electron flux (26–512 keV) observed by Wind/3DP at 1 au. (f) and (g) RSTN radio flux density profiles (sfu) at 245 and 410 MHz from the RSTN Sagamore Hill Radio Observatory. The vertical white line marks the onset of the interaction between the CME-driven shock and the slowly moving blob.
Paper: Imaging and Radio Signatures of Shock–Plasmoid Interaction
Authors: Pankaj Kumar, Judith T. Karpen, P. K. Manoharan, N. Gopalswamy
Figure caption: Eruption and associated fast EUV (shock) wave. (a) AIA 211 Å image showing the active region with a nested null-point topology. N1 and N2 mark the approximate positions of the inner and outer nulls, respectively. (b) AIA 131 Å image capturing the eruption of the hot flux rope (FR). (c) and (d) AIA 211 Å running-difference images displaying the fast EUV wave (marked by S) ahead of the leading edge (LE) of the flux rope. The red box in (c) indicates the size of the top-row panels. (e) Magnetic connectivity map for Earth and STEREO-A on 2014 March 29, at 17:50 UT. The arrow indicates the direction of the eruption. (f) Dynamic radio spectrum in the 25–180 MHz range from the RSTN Sagamore Hill Radio Observatory. The right Y-axis shows the GOES soft X-ray flux profile in the 1–8 Å channel.
Paper: Imaging and Radio Signatures of Shock–Plasmoid Interaction
Authors: Pankaj Kumar, Judith T. Karpen, P. K. Manoharan, N. Gopalswamy
Figure caption: Radio bursts during the CME/shock–blob interaction. (a) and (b) Zoomed view of radio bursts detected during the interaction and the merging of the blob into the CME. (c) and (d) Radio flux density (sfu) profiles at 245/410 MHz (metric/decimetric frequencies) from the RSTN Sagamore Hill Radio Observatory.
Paper: Imaging and Radio Signatures of Shock–Plasmoid Interaction
Authors: Pankaj Kumar, Judith T. Karpen, P. K. Manoharan, N. Gopalswamy
Figure caption: CME/shock–blob interaction in LASCO C2. A sequence of LASCO C2 coronagraph running-difference images leading up to the interaction at 19:24–19:36 UT between the CME shock and the slowly moving blob (indicated by arrows). The slit PQ marked in panel (d) is used to generate the time–distance intensity plot shown in Figure 4.
Paper: Imaging and Radio Signatures of Shock–Plasmoid Interaction
Authors: Pankaj Kumar, Judith T. Karpen, P. K. Manoharan, N. Gopalswamy
Figure caption: Coalescence of the blob into the CME. STEREO-A COR2 coronagraph intensity (top row) and running-difference (bottom row) images showing the interaction between the shock and the blob, and subsequent merging of the blob (marked by arrows) into the CME. The slit RS marked in panel (a1) is used to generate the time–distance intensity plot shown in Figure 4.
Paper: Imaging and Radio Signatures of Shock–Plasmoid Interaction
Authors: Pankaj Kumar, Judith T. Karpen, P. K. Manoharan, N. Gopalswamy
Figure caption: Blob origin. (a) AIA 211 Å image overlaid by Helioseismic and Magnetic Imager (HMI) magnetogram contours showing the active region with a nested null-point topology. (b)–(f) AIA 211 Å running-difference images demonstrating the expansion of the loop system on the right side (cyan dashed curve above the nested null N1 and arrow in panel (c)) of the pseudostreamer and associated reconnection between cyan and yellow structures. The arrow in panel (d) indicates the downflow, while the arrows in the bottom panels ((e) and (f)) reveal the upward-moving structure connected to the blob observed in STEREO COR-1.
Paper: Imaging and Radio Signatures of Shock–Plasmoid Interaction
Authors: Pankaj Kumar, Judith T. Karpen, P. K. Manoharan, N. Gopalswamy
Figure caption: CME–blob interaction. STEREO-A COR-2 coronagraph intensity (rows 1 and 3) and running-difference (rows 2 and 4) images showing a slowly moving blob (marked by arrows) and its interaction with a CME and its shock.
Paper: Imaging and Radio Signatures of Shock–Plasmoid Interaction
Authors: Pankaj Kumar, Judith T. Karpen, P. K. Manoharan, N. Gopalswamy
Figure caption: (a)–(c) STEREO-A COR1 images showing the blob (marked by white arrows) and CME originating from the nested null-point topology. (d) The height–time evolution of the blob as observed in AIA, COR1, and COR2 images.
Paper: Born Dry or Born Wet? A Palette of Water Growth Histories in TRAPPIST-1 Analogs and Compact Planetary Systems
Authors: Howard Chen, Matthew S. Clement, Le “Chris” Wang, Jesse T. Gu
Figure caption: Schematic of our modeling framework, illustrating the connection between N-body accretion outcomes and volatile growth simulations. Each panel highlights the primary physical processes represented at each stage of the model. Terrestrial planet formation begins with planetesimals and planetary embryos assumed to emerge from an initial gas plus dust disk. Their subsequent growth is explicitly simulated using an N-body accretion model that incorporates processes such as collision fragmentation. The outputs from each collision event and accretion phase then serve as inputs to a self-consistent volatile growth model, which evolves key volatile species such as H2O, C, and N, based on cosmochemically informed initial compositions. Major processes contributing to volatile delivery and loss include impact erosion and mantle degassing. Roman numerals denote model subcomponents: mantle (i), atmosphere (ii), core (iii), impactors (iv), and stellar EUV activity (v). Components (i)–(iii) constitute the three primary reservoirs of the growing protoplanet. The schematic layout is conceptually inspired by J. T. Gu et al. (2024).
Paper: Born Dry or Born Wet? A Palette of Water Growth Histories in TRAPPIST-1 Analogs and Compact Planetary Systems
Authors: Howard Chen, Matthew S. Clement, Le “Chris” Wang, Jesse T. Gu
Figure caption: Histogram for the occurrence of final planets across two distinct populations of TRAPPIST-1 analogs binned over their surface water mass fractions (in units of Earth ocean mass). Colors denote whether the initial materials are assumed to have formed in a system with the inclusion of a luminous PMS phase (gold) or without (gray). Color shading separates planets capable of sustaining at least a shallow global ocean (10% of Earth’s surface water mass) and those that are considered to be “dry.” Across most planets, simulations without a PMS phase yield wetter outcomes, particularly for inner planets, highlighting the strong role of early stellar luminosity in depleting primordial planetesimal and embryo volatiles.
Paper: Born Dry or Born Wet? A Palette of Water Growth Histories in TRAPPIST-1 Analogs and Compact Planetary Systems
Authors: Howard Chen, Matthew S. Clement, Le “Chris” Wang, Jesse T. Gu
Figure caption: Snapshots of VGS-calculated surface water mass (in units of Earth’s ocean mass) for TRAPPIST-1 analogs, shown as a function of total planet mass (M⊕) and final orbital distance (au). Panel (a) depicts planets at the halfway point of accretion (i.e., when the protoplanet reaches half its final mass), while panels (b) shows the final planet properties. Measured properties of the TRAPPIST-1 planets are indicated by black circles (E. Agol et al. 2021). At mid-assembly, most inner planets are water-poor due to early impact-driven loss and higher irradiation. By the end of accretion, increased volatile delivery events from more water-rich materials and reduced erosion allow many planets, particularly beyond ~0.03 AU,to accumulate and preserve large water reservoirs, leading to the strong radial gradient in water content.
Paper: Born Dry or Born Wet? A Palette of Water Growth Histories in TRAPPIST-1 Analogs and Compact Planetary Systems
Authors: Howard Chen, Matthew S. Clement, Le “Chris” Wang, Jesse T. Gu
Figure caption: Histogram of simulated TRAPPIST-1 analogs, binned by final atmospheric water content (in Earth ocean masses, M⊕,ocn). Blue bars denote water-rich worlds capable of sustaining at least a shallow global ocean (>10% of Earth’s surface water), while red bars represent water-poor worlds (>10%). Each panel corresponds to a specific TRAPPIST-1 planet, with the center panel showing the combined distribution for all seven. Across the ensemble, inner planets (e.g., b–c) are predominantly dry, whereas mid-to-outer planets (e.g., e–h) are skewed toward water-rich outcomes, reflecting the strong radial dependence of volatile retention identified in our simulations.
Paper: RIOJA. JWST and ALMA Unveil the Inhomogeneous and Complex Interstellar Medium Structure in a Star-forming Galaxy at z = 6.81
Authors: Mitsutaka Usui, Ken Mawatari, Javier Álvarez-Márquez, Takuya Hashimoto, Yuma Sugahara, Rui Marques-Chaves, Akio K. Inoue, Luis Colina, Santiago Arribas, Carmen Blanco-Prieto, Yurina Nakazato, Naoki Yoshida, Tom J. L. C. Bakx, Daniel Ceverino, Luca Costantin, Alejandro Crespo Gómez, Masato Hagimoto, Hiroshi Matsuo, Wataru Osone, Yi W. Ren, Yoshinobu Fudamoto, Takeshi Hashigaya, Miguel Pereira-Santaella, Yoichi Tamura
Figure caption: Left: diagnostic diagram of the [O III] line ratios overlaid with Te–ne model grids generated using PyNeb (V. Luridiana et al. 2015). The red star indicates the observed [O III] line ratios of COS-2987 (Table 1). The gray star shows the ratios dust-corrected on a pixel-by-pixel basis using the AV map shown in the right panel (Section 5.1). The black filled symbols represent high-z star-forming galaxies (J. Witstok et al. 2022; M. Stiavelli et al. 2023; S. Fujimoto et al. 2024; A. Harshan et al. 2024; Y. Harikane et al. 2025b), where the optical [O III] data are obtained from NIRSpec/IFS for COS-2987, COS-3018, SXDF-NB1006-2, J0217-0208, and J1211-0118 and from NIRSpec/MOS for the remaining galaxies. The open symbols represent local dwarf galaxies (Y. Chen et al. 2023, 2024; N. Kumari et al. 2024). The [O III] line ratios of COS-2987 lie outside the model grids, indicating that they cannot be reproduced by a homogeneous ionized gas with a single set of electron temperature and density. Right: AV map derived from the Hα/Hβ ratio, constructed within the 3σ regions of both the Hα and Hβ integrated intensity maps after the Voronoi binning (M. Cappellari & Y. Copin 2003; M. Cappellari 2009). The gray and cyan contours indicate the [O III] 5008 and [O III] 4364 integrated intensity maps, respectively, at the 2σ and 3σ levels.
Paper: RIOJA. JWST and ALMA Unveil the Inhomogeneous and Complex Interstellar Medium Structure in a Star-forming Galaxy at z = 6.81
Authors: Mitsutaka Usui, Ken Mawatari, Javier Álvarez-Márquez, Takuya Hashimoto, Yuma Sugahara, Rui Marques-Chaves, Akio K. Inoue, Luis Colina, Santiago Arribas, Carmen Blanco-Prieto, Yurina Nakazato, Naoki Yoshida, Tom J. L. C. Bakx, Daniel Ceverino, Luca Costantin, Alejandro Crespo Gómez, Masato Hagimoto, Hiroshi Matsuo, Wataru Osone, Yi W. Ren, Yoshinobu Fudamoto, Takeshi Hashigaya, Miguel Pereira-Santaella, Yoichi Tamura
Figure caption: Top left: the same as the left panel of Figure 3 but shown with linear scales on both axes. The two squares correspond to the two gas components: the dark red square indicates component 1, with (Te, ne) = (26,000 K, 500 cm−3), and the orange square indicates component 2, with (Te, ne) = (8000 K, 50 cm−3). The observed line ratios of COS-2987 (red star) can be explained by an ISM composed of these two components, mixed at an appropriate volume ratio and represented by the line connecting the two squares. Top right: [O III] 88/5008 and [O III] 4364/5008 luminosity ratios as a function of volume ratio V1/V2 in our two-component model. The black curves show the predicted ratios from the model. The horizontal solid lines and shaded regions indicate the observed ratios and their 1σ uncertainties, respectively. The observed values are reproduced when V1: V2 ∼ 1: 300 (vertical dashed lines). Bottom: schematic illustration of our proposed two-component gas scenario. Hot and dense H II regions around young massive stars or clusters (component 1) are surrounded by relatively cool and diffuse H II regions (component 2). From the perspective of pressure balance, the component 1 gas is expected to be expanding. The [O III] 4364 and [O III] 88 emissions arise primarily from the component 1 and 2 regions, respectively, while both components contribute to the [O III] 5008 emission.
Paper: RIOJA. JWST and ALMA Unveil the Inhomogeneous and Complex Interstellar Medium Structure in a Star-forming Galaxy at z = 6.81
Authors: Mitsutaka Usui, Ken Mawatari, Javier Álvarez-Márquez, Takuya Hashimoto, Yuma Sugahara, Rui Marques-Chaves, Akio K. Inoue, Luis Colina, Santiago Arribas, Carmen Blanco-Prieto, Yurina Nakazato, Naoki Yoshida, Tom J. L. C. Bakx, Daniel Ceverino, Luca Costantin, Alejandro Crespo Gómez, Masato Hagimoto, Hiroshi Matsuo, Wataru Osone, Yi W. Ren, Yoshinobu Fudamoto, Takeshi Hashigaya, Miguel Pereira-Santaella, Yoichi Tamura
Figure caption: Left: integrated intensity map of the NIRSpec [O III] 5008 emission. The red contours show the ±2nσ significance levels (n = 1, 2, 3, … ), where σ = 1.16 × 10−20 erg s−1 cm−2 pixel−1. Positive and negative contours are shown by the solid and dashed lines, respectively. The orange circle at the bottom left indicates the FWHM of ﹩0\mathop{.}\limits^{^{\prime\prime} }21﹩ at the observed wavelength of Hα (5.125 μm). Right: one-dimensional spectra of [O III] 4364, [O III] 5008, and [O III] 88, where the horizontal axis is the velocity relative to the best-fit redshift to the [O III] 5008 line. In each panel, the red solid histogram and gray shade indicate the observed flux density and 1σ uncertainty, respectively. The gray shade is not visible for [O III] 5008, due to its negligible 1σ uncertainty.
Paper: RIOJA. JWST and ALMA Unveil the Inhomogeneous and Complex Interstellar Medium Structure in a Star-forming Galaxy at z = 6.81
Authors: Mitsutaka Usui, Ken Mawatari, Javier Álvarez-Márquez, Takuya Hashimoto, Yuma Sugahara, Rui Marques-Chaves, Akio K. Inoue, Luis Colina, Santiago Arribas, Carmen Blanco-Prieto, Yurina Nakazato, Naoki Yoshida, Tom J. L. C. Bakx, Daniel Ceverino, Luca Costantin, Alejandro Crespo Gómez, Masato Hagimoto, Hiroshi Matsuo, Wataru Osone, Yi W. Ren, Yoshinobu Fudamoto, Takeshi Hashigaya, Miguel Pereira-Santaella, Yoichi Tamura
Figure caption: Left: integrated intensity map of the NIRSpec [O III] 5008 emission, after convolution to match the ALMA beam size (﹩0\mathop{.}\limits^{^{\prime\prime} }80\times 0\mathop{.}\limits^{^{\prime\prime} }61﹩). The red contours show the ±2nσ significance levels (n = 1, 2, 3, … ), where σ = 1.16 × 10−20 erg s−1 cm−2 pixel−1. The orange circle at the bottom left indicates the FWHM of ﹩0\mathop{.}\limits^{^{\prime\prime} }21﹩ at the observed wavelength of Hα (5.125 μm). Right: integrated intensity map of the ALMA [O III] 88 emission. The white contours show the ±(2, 4, 6)σ significance levels, where σ = 82.6 mJy beam−1 km s−1. Positive and negative contours are shown by the white solid and dashed lines, respectively. The white ellipse at the bottom left represents the synthesized beam size of ﹩0\mathop{.}\limits^{^{\prime\prime} }80\times 0\mathop{.}\limits^{^{\prime\prime} }61﹩.