adsabs/AstroCLIMB huggingface dataset:
Paper: The Circumgalactic Hα Spectrograph (CHαS). I. Design, Engineering, and Early Commissioning
Authors: Nicole Melso, David Schiminovich, Brian Smiley, Hwei Ru Ong, Bárbara Cruvinel Santiago, Meghna Sitaram, Ignacio Cevallos Aleman, Sarah Graber, Marisa Murillo, Marni Rosenthal, Ioana Stelea
Figure caption: The top panels show nonsequential Zemax ray traces showing a section of the CHαS plano-convex microlens array in two orientations: (left) the convex side facing toward the telescope’s focal plane; and (right) the convex side facing away from the telescope’s focal plane. The array can be flipped 180° in the optical path without altering the imaging capability. Orientation 1 reimages the telescope pupil inside the array. Orientation 2 reimages the telescope pupil outside the array, allowing us to access it and add additional masking. The bottom panels show nonsequential ray-trace imaging at the microlens array and at the detector. The bottom left panel shows the geometric pupil of the telescope in the telescope’s focal plane. The plano-convex lenslets reimage the telescope pupil, resulting in the micropupils shown in the bottom middle panel. This reimaging/demagnification adds space between the lenslets, for the spectra to disperse. At the detector (bottom right), the spectra extend vertically and do not overlap for many resolution elements.
Paper: The Circumgalactic Hα Spectrograph (CHαS). I. Design, Engineering, and Early Commissioning
Authors: Nicole Melso, David Schiminovich, Brian Smiley, Hwei Ru Ong, Bárbara Cruvinel Santiago, Meghna Sitaram, Ignacio Cevallos Aleman, Sarah Graber, Marisa Murillo, Marni Rosenthal, Ioana Stelea
Figure caption: The CHαS VPH grating diffraction efficiency (average polarization) as a function of wavelength at a fixed angle of incidence. The solid lines show the RCWA carried out at the Bragg incidence for central wavelengths of 490 nm (blue), 660 nm (green), and 900 nm (red). The same RCWA analysis is conducted for off-axis incidence angles with a Bragg deviation of ±2.°5, creating the angular Bragg envelopes shown by the shaded regions. The dotted lines are the average lossless Kogelnik efficiency predictions, again performed at Bragg incidence for 490 nm (blue), 660 nm (green), and 900 nm (red). The symbols are the manufacturer-measured first-order diffraction efficiencies at three distinct laser wavelengths (488 nm, 650 nm, and 904 nm), taken using a 98 mm aperture and averaged for measurements across the grating. All the data products in this plot were supplied by Wasatch Phonics.
Paper: The Circumgalactic Hα Spectrograph (CHαS). I. Design, Engineering, and Early Commissioning
Authors: Nicole Melso, David Schiminovich, Brian Smiley, Hwei Ru Ong, Bárbara Cruvinel Santiago, Meghna Sitaram, Ignacio Cevallos Aleman, Sarah Graber, Marisa Murillo, Marni Rosenthal, Ioana Stelea
Figure caption: The CHαS optomechanical design, modeled in SolidWorks. The top view is the east side of the spectrograph, and the bottom view is the west side. CHαS is primarily composed of two trusses. The main truss houses the relay, focal plane, and collimator optics. The camera truss houses the custom camera optics. The majority of the mechanical frame is assembled from prefabricated joint connector kits. The main truss is built from the 80–20 T-slot Aluminum Building System, and the camera truss employs the Rock West Composites CARBONNect carbon fiber system. The camera and grating rotate around the labeled pivot axis. The relay optics are mounted on the side of the main truss.
Paper: The Circumgalactic Hα Spectrograph (CHαS). I. Design, Engineering, and Early Commissioning
Authors: Nicole Melso, David Schiminovich, Brian Smiley, Hwei Ru Ong, Bárbara Cruvinel Santiago, Meghna Sitaram, Ignacio Cevallos Aleman, Sarah Graber, Marisa Murillo, Marni Rosenthal, Ioana Stelea
Figure caption: Zemax ray trace of the CHαS design. In this figure, we split the design into three subsets: the relay optics, the entrance optics, and the spectrograph optics. The total sequential optical path through all three is: (relay optics) the telescope focal plane, flat pick-off #1, concave spherical mirror #1, convex spherical mirror, concave spherical mirror #2; (entrance optics) flat pick-off #2, microlens array; and (spectrograph optics) collimator field corrector bundle, collimator primary spherical mirror, collimator asphere, grating, camera asphere, camera flat mirror, camera primary spherical mirror, camera field corrector lens, detector.
Paper: A Massive Star Is Born: How Feedback from Stellar Winds, Radiation Pressure, and Collimated Outflows Limits Accretion onto Massive Stars
Authors: Anna L. Rosen
Figure caption: Projections of the density of the wind bubbles along the y–z plane that are moving away from the primary star (v rad > 0) for runs ROFW μ  ϕ  ∞ (top row) and ROFW μ  ϕ  2 (bottom row) for gas with T ≥ 104 K. Each panel is (0.15 pc)2.
Paper: A Massive Star Is Born: How Feedback from Stellar Winds, Radiation Pressure, and Collimated Outflows Limits Accretion onto Massive Stars
Authors: Anna L. Rosen
Figure caption: Stellar feedback momentum (left panel) and energy (right panel) deposition rates as a function of primary stellar mass for stellar winds (solid lines), direct radiation including contributions from both the internal (stellar) and accretion luminosities (dotted–dashed lines), and collimated outflows (dashed lines) for runs ROFW μ  ϕ  ∞ (teal lines) and ROFW μ  ϕ  2 (pink lines), respectively. We show these properties when the star becomes hot enough (T eff ≥ 12.5 kK) to launch isotropic winds following the mass-loss rates formulae from Vink et al. (2001).
Paper: A Massive Star Is Born: How Feedback from Stellar Winds, Radiation Pressure, and Collimated Outflows Limits Accretion onto Massive Stars
Authors: Anna L. Rosen
Figure caption: Entrained wind material (left panels) and wind material volume-filling fraction (right panels) as a function of simulation time (top row) and primary stellar mass (bottom row). The lines show where these quantities contain 5 × 10−3% of wind material. The dark teal and dark pink dashed lines consider all gas for runs ROFW μ  ϕ  ∞ and ROFW μ  ϕ  2, respectively. The light teal and light pink solid lines only consider gas with T ≥ 104 K for runs ROFW μ  ϕ  ∞ and ROFW μ  ϕ  2, respectively.
Paper: A Massive Star Is Born: How Feedback from Stellar Winds, Radiation Pressure, and Collimated Outflows Limits Accretion onto Massive Stars
Authors: Anna L. Rosen
Figure caption: Stellar wind properties as a function of primary stellar mass for runs ROFW μ  ϕ  ∞ (solid teal lines) and ROFW μ  ϕ  2 (dashed pink lines). The top-left panel and bottom-left panel show the wind mass-loss rates and wind velocities following the formulae presented in Section 2.4.3 when the star has T eff ≥ 12.5 kK, following Vink et al. (2001). The top-center and bottom-center panels show the primary star’s effective temperature and radius, respectively. The top-right and bottom-right panels show the total integrated wind kinetic energy as a function of stellar mass and simulation time, respectively.
Paper: A Massive Star Is Born: How Feedback from Stellar Winds, Radiation Pressure, and Collimated Outflows Limits Accretion onto Massive Stars
Authors: Anna L. Rosen
Figure caption: Projections of the density of the entrained wind material along the y–z plane that are moving away from the primary star (v rad > 0) for runs ROFW μ  ϕ  ∞ (top row) and ROFW μ  ϕ  2 (bottom row). Each panel is (0.4 pc)2 .
Paper: A Massive Star Is Born: How Feedback from Stellar Winds, Radiation Pressure, and Collimated Outflows Limits Accretion onto Massive Stars
Authors: Anna L. Rosen
Figure caption: Projections of the density of the entrained outflow material along the y–z plane that are moving away from the primary star (v rad > 0) for runs ROFW μ  ϕ  ∞ (top row) and ROFW μ  ϕ  2 (bottom row). Each panel is (0.4 pc)2.
Paper: A Massive Star Is Born: How Feedback from Stellar Winds, Radiation Pressure, and Collimated Outflows Limits Accretion onto Massive Stars
Authors: Anna L. Rosen
Figure caption: Primary protostar mass as a function of simulation time for runs ROF μ  ϕ  ∞ , ROFW μ  ϕ  ∞ , ROF μ  ϕ  2, ROFW μ  ϕ  2, ROF μ  ϕ  20, and ROFW μ  ϕ  20.
Paper: A Massive Star Is Born: How Feedback from Stellar Winds, Radiation Pressure, and Collimated Outflows Limits Accretion onto Massive Stars
Authors: Anna L. Rosen
Figure caption: Projections of the number density (left column), temperature (center-left column), pressure (center-right column), and velocity magnitude (right column) of the hot gas within the wind bubbles along the y–z plane of the final snapshots for runs ROFW μ  ϕ  ∞ (top row) and ROFW μ  ϕ  2 (bottom row) considering only gas with T ≥ 0.5 keV (T ≥ 5.8 × 106 K). Each panel is (0.15 pc)2.
Paper: A Massive Star Is Born: How Feedback from Stellar Winds, Radiation Pressure, and Collimated Outflows Limits Accretion onto Massive Stars
Authors: Anna L. Rosen
Figure caption: Thin-density-weighted projections of the ratio of the magnetic pressure to thermal gas pressure (P B/P gas) for run ROFW μ  ϕ  2. Each panel is (5000au)2 in area and the projection is taken over a depth of 500 au, with the massive star, denoted by the gray circle, at the center. Each projection is oriented such that the mass-weighted angular momentum axis of the gas within a radius of 500 au from the massive star points out of the page.
Paper: A Massive Star Is Born: How Feedback from Stellar Winds, Radiation Pressure, and Collimated Outflows Limits Accretion onto Massive Stars
Authors: Anna L. Rosen
Figure caption: Density slices for runs ROF μ  ϕ  ∞ (top row) and ROFW μ  ϕ  ∞ (bottom row) as a function of primary stellar mass. The most massive star (denoted by the gray circle) is located at the center of each panel and the slice is oriented such that its angular momentum axis points up, in order to highlight the density structure of the outflows. The primary stellar mass and the simulation time, in units of t ff, are shown in the top-left and bottom-left corners of each panel, respectively. Each panel is (0.4 pc)2.
Paper: Extreme Nature of Four Blue-excess Dust-obscured Galaxies Revealed by Optical Spectroscopy
Authors: Akatoki Noboriguchi, Tohru Nagao, Yoshiki Toba, Kohei Ichikawa, Masaru Kajisawa, Nanako Kato, Toshihiro Kawaguchi, Hideo Matsuhara, Yoshiki Matsuoka, Kyoko Onishi, Masafusa Onoue, Nozomu Tamada, Koki Terao, Yuichi Terashima, Yoshihiro Ueda, Takuji Yamashita
Figure caption: Diagram of SMBH mass vs. bolometric luminosity. The filled-blue stars and gray contour denote the BluDOGs and SDSS quasars, while the filled hexagons with green, orange, purple, cyan, and light green colors denote ERQs (Perrotta et al. 2019), WISSH quasars (Vietri et al. 2018), Hot DOGs (Wu et al. 2018), DOGs (Melbourne et al. 2011, 2012), and a CT DOG (Toba et al. 2020), respectively. The red-dashed lines represent a constant Eddington ratio of λ Edd = 0.01, 0.1, 1.0, and 10.0.
Paper: Extreme Nature of Four Blue-excess Dust-obscured Galaxies Revealed by Optical Spectroscopy
Authors: Akatoki Noboriguchi, Tohru Nagao, Yoshiki Toba, Kohei Ichikawa, Masaru Kajisawa, Nanako Kato, Toshihiro Kawaguchi, Hideo Matsuhara, Yoshiki Matsuoka, Kyoko Onishi, Masafusa Onoue, Nozomu Tamada, Koki Terao, Yuichi Terashima, Yoshihiro Ueda, Takuji Yamashita
Figure caption: REW of the C IV vs. the monochromatic luminosity at 1350 Å. Blue and orange dots represent the four BluDOGs and WISSH quasars (Vietri et al. 2018). The gray 2D histogram represents the number density of the SDSS quasars (Shen et al. 2011). The green line represents the linear fit to the distribution of the SDSS quasars. The red plots show the mean and standard deviation in luminosity bins with 0.5 dex width. The numbers of SDSS quasars in the individual bins are shown at the bottom of the panel.
Paper: Extreme Nature of Four Blue-excess Dust-obscured Galaxies Revealed by Optical Spectroscopy
Authors: Akatoki Noboriguchi, Tohru Nagao, Yoshiki Toba, Kohei Ichikawa, Masaru Kajisawa, Nanako Kato, Toshihiro Kawaguchi, Hideo Matsuhara, Yoshiki Matsuoka, Kyoko Onishi, Masafusa Onoue, Nozomu Tamada, Koki Terao, Yuichi Terashima, Yoshihiro Ueda, Takuji Yamashita
Figure caption:  kt 80 vs. α  β  plot for the limited BluDOGs (blue dots), core ERQs without BALs (green dots), and core ERQs with BALs (orange dots). The black solid line and dashed line denote the kt 80 values of a single Gaussian and single Lorentzian, respectively. Note that 41 core ERQs without BALs and seven core ERQs with BALs are fitted with a single Gaussian, and they are plotted at (α  β , kt 80) = (0, ﹩\sqrt{1-\tfrac{2\mathrm{ln}(2)}{\mathrm{ln}(5)}}﹩).
Paper: Extreme Nature of Four Blue-excess Dust-obscured Galaxies Revealed by Optical Spectroscopy
Authors: Akatoki Noboriguchi, Tohru Nagao, Yoshiki Toba, Kohei Ichikawa, Masaru Kajisawa, Nanako Kato, Toshihiro Kawaguchi, Hideo Matsuhara, Yoshiki Matsuoka, Kyoko Onishi, Masafusa Onoue, Nozomu Tamada, Koki Terao, Yuichi Terashima, Yoshihiro Ueda, Takuji Yamashita
Figure caption: REW ratio vs. rest-frame wavelength. REW ratios are defined as REWs of objects over REWs from the composite spectrum of SDSS type 1 quasar measured by Vanden Berk et al. (2001). The red, blue, green, and orange plots show the REW ratios of J0907, J1202, J1207, and J1443, respectively.
Paper: Extreme Nature of Four Blue-excess Dust-obscured Galaxies Revealed by Optical Spectroscopy
Authors: Akatoki Noboriguchi, Tohru Nagao, Yoshiki Toba, Kohei Ichikawa, Masaru Kajisawa, Nanako Kato, Toshihiro Kawaguchi, Hideo Matsuhara, Yoshiki Matsuoka, Kyoko Onishi, Masafusa Onoue, Nozomu Tamada, Koki Terao, Yuichi Terashima, Yoshihiro Ueda, Takuji Yamashita
Figure caption: Cumulative distribution of the α  β  indices for the limited BluDOGs (see the main text; blue line), core ERQs without BALs (green line), and core ERQs with BALs (orange line). The red-dashed line denotes the α  β  index measured for the composite spectrum of SDSS type 1 quasars.
Paper: Extreme Nature of Four Blue-excess Dust-obscured Galaxies Revealed by Optical Spectroscopy
Authors: Akatoki Noboriguchi, Tohru Nagao, Yoshiki Toba, Kohei Ichikawa, Masaru Kajisawa, Nanako Kato, Toshihiro Kawaguchi, Hideo Matsuhara, Yoshiki Matsuoka, Kyoko Onishi, Masafusa Onoue, Nozomu Tamada, Koki Terao, Yuichi Terashima, Yoshihiro Ueda, Takuji Yamashita
Figure caption: Diagram of the redshift vs. the Eddington ratio. The filled-blue stars and hexagons are the same as in Figure 11. The gray 2D histogram represents the number density of SDSS quasars (Shen et al. 2011). The red plots show the mean and standard deviation of λ Edd in redshift bins with a width of Δz = 0.5. The numbers shown at the upper part denote the numbers of SDSS quasars in the redshift bins.
Paper: Extreme Nature of Four Blue-excess Dust-obscured Galaxies Revealed by Optical Spectroscopy
Authors: Akatoki Noboriguchi, Tohru Nagao, Yoshiki Toba, Kohei Ichikawa, Masaru Kajisawa, Nanako Kato, Toshihiro Kawaguchi, Hideo Matsuhara, Yoshiki Matsuoka, Kyoko Onishi, Masafusa Onoue, Nozomu Tamada, Koki Terao, Yuichi Terashima, Yoshihiro Ueda, Takuji Yamashita
Figure caption: Cumulative distribution of the kt 80 indices for the limited BluDOGs (blue line), core ERQs without BALs (green line), and core ERQs with BALs (orange line). The red-dashed line denotes the kt 80 index for the single-Gaussian profile.
Paper: Discovery of a Filamentary Synchrotron Structure Connected to the Coherent Magnetic Field in the Outer Galaxy
Authors: J. L. West, J. L. Campbell, P. Bhaura, R. Kothes, S. Safi-Harb, J. M. Stil, A. R. Taylor, T. Foster, B. M. Gaensler, S. J. George, S. J. Gibson, R. Ricci
Figure caption: Top panel: Best-fit bow shock model (gray line), with the origin (pulsar position) fixed at the location of the X-ray source, 1RXS J053300.7+260827 (shown with a red cross). The black lines are a series of points defined by a data contour with a level of 0.01 K. The fitted value of R 0 = 321″ and the fitted rotation of the model is 5° counterclockwise. The blue cross shows the position of 1RXS J053239.0+261747. The model is shown overlaid on the DRAO polarized intensity image. Middle panel: Same as the top panel, but for the origin (pulsar position) fixed at the location of the X-ray source, 1RXS J053239.0+261747 (shown with a red cross). The fitted value of R 0 = 310″ and the fitted rotation of the model is 5° counterclockwise. Bottom panel: Same as the top panel, but without fixing the pulsar position. The best-fit position (shown with a red cross) has R.A. = 5:32:54.5, decl. = +26:18:55, with R 0 = 313″ and the fitted rotation of 7° counterclockwise.
Paper: Discovery of a Filamentary Synchrotron Structure Connected to the Coherent Magnetic Field in the Outer Galaxy
Authors: J. L. West, J. L. Campbell, P. Bhaura, R. Kothes, S. Safi-Harb, J. M. Stil, A. R. Taylor, T. Foster, B. M. Gaensler, S. J. George, S. J. Gibson, R. Ricci
Figure caption: Top left: Map of the peak polarized intensity,  F (ϕ peak), from GALFACTS. Top right: Map of peak Faraday depth, ϕ peak. Bottom left: WHAM Hα map toward the region around G182.5–4.0. Bottom right: LIC drapery lines showing the plane-of-sky magnetic field orientation (χ src + 90°). All panels have black contours that show the Hα emission at levels of 7, 9, and 13 Rayleighs (R). The white contours (blue in the bottom-right panel) are from the DRAO Stokes I data with a level of 0.015 K, showing the position and orientation of the G182.5–4.0 filaments.
Paper: Discovery of a Filamentary Synchrotron Structure Connected to the Coherent Magnetic Field in the Outer Galaxy
Authors: J. L. West, J. L. Campbell, P. Bhaura, R. Kothes, S. Safi-Harb, J. M. Stil, A. R. Taylor, T. Foster, B. M. Gaensler, S. J. George, S. J. Gibson, R. Ricci
Figure caption: Top: Profile across both the northern and southern filaments of G182.5–4.0. The peak brightness has been normalized to 1. The shading shows the 1σ uncertainty on the average. Bottom: Profile across both the northern and southern filaments of G182.5–4.0 shown in comparison to the profile of the eastern limb of SN1006. Here the northern filament profile has been flipped such that the center of the shell is at a distance of 0 pc. The peak brightness has been normalized to 1. As in the top panel, the shading (upper and lower dashed lines in the case of SN1006) shows the 1σ uncertainty on the average.
Paper: Discovery of a Filamentary Synchrotron Structure Connected to the Coherent Magnetic Field in the Outer Galaxy
Authors: J. L. West, J. L. Campbell, P. Bhaura, R. Kothes, S. Safi-Harb, J. M. Stil, A. R. Taylor, T. Foster, B. M. Gaensler, S. J. George, S. J. Gibson, R. Ricci
Figure caption: Swift spacecraft images of 1RXS J053239.0+261747 (top) and 1RXS J053300.7+260827 (bottom) including X-ray XRT image (left) and UV UVOT images (right). The white circle in all panels indicates the J2000 catalog coordinates for the stars HD 244599 (top) and G98-9 (bottom). The dotted circles in the bottom panel are drawn centered on the sources seen in the Swift UVOT image. The white dotted circle in the bottom panel is the presumed current location of the high-proper-motion star G98-9. There is a second, unidentified UV component in the bottom-right panel (magenta circle) that is offset by ∼10″ from the X-ray peak.
Paper: Discovery of a Filamentary Synchrotron Structure Connected to the Coherent Magnetic Field in the Outer Galaxy
Authors: J. L. West, J. L. Campbell, P. Bhaura, R. Kothes, S. Safi-Harb, J. M. Stil, A. R. Taylor, T. Foster, B. M. Gaensler, S. J. George, S. J. Gibson, R. Ricci
Figure caption: The distribution of RHT orientation angles of H I structures, measured from Galactic north through east, for velocities from 28.21 to –43.51 km s−1. Each curve is an integration over all of the pixels enclosed in a region from 180.°75 < l < 184.°00 and −3.°33 > b > −4.°50, and for a particular velocity channel. The black curve shows the result from the Stokes I image. The thicker cyan curve is for an H I velocity channel at –8.8880 km s−1, which shows the greatest agreement with Stokes I.
Paper: Discovery of a Filamentary Synchrotron Structure Connected to the Coherent Magnetic Field in the Outer Galaxy
Authors: J. L. West, J. L. Campbell, P. Bhaura, R. Kothes, S. Safi-Harb, J. M. Stil, A. R. Taylor, T. Foster, B. M. Gaensler, S. J. George, S. J. Gibson, R. Ricci
Figure caption: Hα filaments detected in the IGAPS data with contours from Stokes I. The DRAO Stokes I image is shown at upper left with white rectangles indicating the regions shown in the Hα mosaics. In all panels, yellow shows bright emission and dark blue shows faint.
Paper: Discovery of a Filamentary Synchrotron Structure Connected to the Coherent Magnetic Field in the Outer Galaxy
Authors: J. L. West, J. L. Campbell, P. Bhaura, R. Kothes, S. Safi-Harb, J. M. Stil, A. R. Taylor, T. Foster, B. M. Gaensler, S. J. George, S. J. Gibson, R. Ricci
Figure caption: H I velocity maps showing a range of velocities from 15.02 to –28.67 km s−1. Each subplot has been averaged over six velocity channels, showing a total range of 4.95 km s−1. Each map is shown with the same linear brightness scaling from –0.12 (dark blue) to 0.12 K (yellow). The white contours show the position of the Stokes I emission of G182.5–4.0.
Paper: Discovery of a Filamentary Synchrotron Structure Connected to the Coherent Magnetic Field in the Outer Galaxy
Authors: J. L. West, J. L. Campbell, P. Bhaura, R. Kothes, S. Safi-Harb, J. M. Stil, A. R. Taylor, T. Foster, B. M. Gaensler, S. J. George, S. J. Gibson, R. Ricci
Figure caption: Plot of the orientation angle vs. distance for stars in the catalog of Meng & Sun (2021). The horizontal lines represent the orientation of the two parts of G182.5–4.0 with uncertainty (dotted lines). The black points show the mean and standard deviation of the orientation angles using 200 pc bins.
Paper: Properties of Type Iax Supernova 2019muj in the Late Phase: Existence, Nature, and Origin of the Iron-rich Dense Core
Authors: Keiichi Maeda, Miho Kawabata
Figure caption: An expanded view on the spectral region between 4500 and 5600  Å on day 131, as compared to the optical-depth distribution of the reference model (left) and that of the 56Ni-rich inner core having a total mass of 0.033 M ⊙ and the 56Ni mass of 0.02 M ⊙ (right). The optical depth is shown in a linear and absolute scale (Fe II shown by blue; Fe I by red; total including other species by green), while the observed spectrum is shown with different normalizations in the two panels. Strong lines in the observed spectrum are marked by the gray-shaded areas.
Paper: Properties of Type Iax Supernova 2019muj in the Late Phase: Existence, Nature, and Origin of the Iron-rich Dense Core
Authors: Keiichi Maeda, Miho Kawabata
Figure caption: The density distributions assumed in the TARDIS spectral synthesis calculations; the reference model (black), the 56Ni-rich inner core (red), and the C+O-rich inner core (blue). The dashed lines are for day 131 and the solid lines are for day 480, assuming the homologous expansion. The squares mark the positions of the photosphere on day 131 (open) and day 480 (filled) overplotted on the 56Ni-rich model. Also plotted here for comparison are the outermost homologous component in the wind model of Shen & Schwab (2017) scaled to days 131 and 480 (gray; see Section 5 for details).
Paper: Properties of Type Iax Supernova 2019muj in the Late Phase: Existence, Nature, and Origin of the Iron-rich Dense Core
Authors: Keiichi Maeda, Miho Kawabata
Figure caption: The same as Figure 10, but for the 56Ni-rich inner core having a total mass of 0.033 M ⊙ and the 56Ni mass of 0.02 M ⊙, without C nor O (upper panels). The same but for the C+O-rich inner core having a total mass of 0.33 M ⊙ is shown in the lower panels, where the 56Ni mass is 0.02 M ⊙ (therefore, this model is rich in C and O).