adsabs/AstroCLIMB huggingface dataset:
Paper: Probing the Physical and Chemical Characteristics of an Extremely Early Class 0 Protostar in G204.4-11.3A2-NE
Authors: Hsuan-I (Ethan) Chou, Naomi Hirano, Masayuki Yamaguchi
Figure caption: (a) Moment 1 map of C18O (color) overlaid with the TM1+TM2 continuum map (contour). Contour levels are 5, 10, 20, 40,…×σ (σ = 0.061 mJy beam−1). The moment 1 map was made with C18O emissions below 5σ (σ = 2.5 mJy beam−1) excluded. Magenta-filled ellipse denotes the synthesized beam. (b) Moment 0 maps of the high-velocity C18O emission components overlaid on the SpM continuum image. The integrated velocity ranges of the blueshifted and redshifted components are from −0.3 to +0.6 km s−1 and from +2.2 to +3.0 km s−1, respectively. White dashed line denotes the direction of the velocity gradient, P.A. = 60°. Open and filled ellipses are the beam of the C18O image and the effective resolution of the SpM continuum image, respectively.
Paper: Probing the Physical and Chemical Characteristics of an Extremely Early Class 0 Protostar in G204.4-11.3A2-NE
Authors: Hsuan-I (Ethan) Chou, Naomi Hirano, Masayuki Yamaguchi
Figure caption: High-resolution (TM1) SIO PV diagrams along the redshifted (a) and blueshifted (b) jet axes. Contours are drawn every 2.4 mJy beam−1 (2σ) with the lowest contour level of 3.6 mJy beam−1 (3σ). The locations of the knots are marked in green lines. Annotated cyan arrows (dashed and solid) indicate the observed jet velocities Vobs and velocity dispersions ΔVobs. Dobs and ΔDobs, used for the jet modeling are indicated by cyan horizontal lines. Note that velocity offsets larger than ±40 km s−1 were not covered by the present correlator setting.
Paper: Probing the Physical and Chemical Characteristics of an Extremely Early Class 0 Protostar in G204.4-11.3A2-NE
Authors: Hsuan-I (Ethan) Chou, Naomi Hirano, Masayuki Yamaguchi
Figure caption: (a) DCO+ moment 1 image (color) overlaid on the redshifted CO outflow (contour). Contours are drawn every 5σ (1σ = 15 mJy beam−1 km s−1) with the lowest contour level at 10σ. (b) CO outflow (blue and red) and SiO jet (green) at 0﹩\mathop{.}\limits^{^{\prime\prime} }﹩3 resolution. The location of the r4 knot is indicated.
Paper: Probing the Physical and Chemical Characteristics of an Extremely Early Class 0 Protostar in G204.4-11.3A2-NE
Authors: Hsuan-I (Ethan) Chou, Naomi Hirano, Masayuki Yamaguchi
Figure caption: Channel maps of C18O emission. Velocity offset from vsys = 1.4 km s−1 is given in each panel. Cross indicates the position of the 1.3 mm continuum peak. The blue-filled ellipse in the bottom-left corner denotes the synthesized beam size.
Paper: Probing the Physical and Chemical Characteristics of an Extremely Early Class 0 Protostar in G204.4-11.3A2-NE
Authors: Hsuan-I (Ethan) Chou, Naomi Hirano, Masayuki Yamaguchi
Figure caption: PV diagram of C18O emission along P.A. = 60°, overlaid with contours of the toy model for the specified parameters. Each row corresponds to a different stellar mass (increasing from top to bottom), and each column corresponds to a different centrifugal barrier (increasing from left to right). The contour levels are 0.09, 0.2, 0.4, 0.6, and 0.8 times the maximum value of the model, where the lowest level corresponds to the 3σ level of the emission.
Paper: Probing the Physical and Chemical Characteristics of an Extremely Early Class 0 Protostar in G204.4-11.3A2-NE
Authors: Hsuan-I (Ethan) Chou, Naomi Hirano, Masayuki Yamaguchi
Figure caption: Same as Figure A1 but for DCO+.
Paper: Probing the Physical and Chemical Characteristics of an Extremely Early Class 0 Protostar in G204.4-11.3A2-NE
Authors: Hsuan-I (Ethan) Chou, Naomi Hirano, Masayuki Yamaguchi
Figure caption: Same as Figure A1 but for N2D+.
Paper: A Luminous and Hot Infrared through X-Ray Transient at a 5 kpc Offset from a Dwarf Galaxy
Authors: Jean J. Somalwar, Vikram Ravi, Raffaella Margutti, Ryan Chornock, Priyamvada Natarajan, Wenbin Lu, Charlotte Angus, Matthew J. Graham, Erica Hammerstein, Edward Nathan, Matt Nicholl, Kritti Sharma, Robert Stein, Frank Verdi, Yuhan Yao, Eric C. Bellm, Tracy X. Chen, Michael W. Coughlin, David Hale, Mansi M. Kasliwal, Russ R. Laher, Reed Riddle, Jesper Sollerman
Figure caption: Constraints on the origin of the red excess from 24puz. The left panel shows the HST spectral energy distribution of 24puz in black and, for comparison, an epoch of observations of the red excess from AT 2018cow in red. A best-fit hot blackbody is shown in brown. The dashed lines show the hot blackbody with potential red excess emission added on. These are not fits but are meant to guide the eye. In orange, a λ−1 power law was added to represent reprocessing in a shallow medium; in green, a λ−3/2 power law is summed to represent reprocessing in a wind-like medium. In blue, we add a dust blackbody to show that this model peaks redward of the excess. The right panel shows our radio upper limits as black triangles. The gray band shows an extrapolation of a power-law fit to the HST data to radio frequencies. Considering that the HST data is taken at later times than the radio, so we would expect it to have faded with time, the power-law extrapolation overpredicts the radio limits.
Paper: A Luminous and Hot Infrared through X-Ray Transient at a 5 kpc Offset from a Dwarf Galaxy
Authors: Jean J. Somalwar, Vikram Ravi, Raffaella Margutti, Ryan Chornock, Priyamvada Natarajan, Wenbin Lu, Charlotte Angus, Matthew J. Graham, Erica Hammerstein, Edward Nathan, Matt Nicholl, Kritti Sharma, Robert Stein, Frank Verdi, Yuhan Yao, Eric C. Bellm, Tracy X. Chen, Michael W. Coughlin, David Hale, Mansi M. Kasliwal, Russ R. Laher, Reed Riddle, Jesper Sollerman
Figure caption: Constraints on the physical parameters of any synchrotron-emitting region from our radio/millimeter observations. The left panel shows the ambient medium density n at outflow radius R for a spherical, nonrelativistic outflow. The dashed lines mark the boundary between physical parameters excluded and allowed by a model that includes free–free absorption, where the absorbing medium density is assumed to be the same as the emitting region. The gray region is allowed by all models. Each line corresponds to a different observation, and the color scales with the time since discovery. The solid lines do not include free–free emission. Regions to the left of these lines are allowed, while regions to the right are excluded. The LFBOT AT 2018cow is shown in stars for comparison (A. Y. Q. Ho et al. 2019; R. Margutti et al. 2019). The right panel is in the same format as the left, but it shows physical parameters appropriate for a stellar-wind-like circumtransient medium. The x-axis shows velocity v, and the y-axis the mass-loss rate ﹩\dot{M}﹩.
Paper: A Luminous and Hot Infrared through X-Ray Transient at a 5 kpc Offset from a Dwarf Galaxy
Authors: Jean J. Somalwar, Vikram Ravi, Raffaella Margutti, Ryan Chornock, Priyamvada Natarajan, Wenbin Lu, Charlotte Angus, Matthew J. Graham, Erica Hammerstein, Edward Nathan, Matt Nicholl, Kritti Sharma, Robert Stein, Frank Verdi, Yuhan Yao, Eric C. Bellm, Tracy X. Chen, Michael W. Coughlin, David Hale, Mansi M. Kasliwal, Russ R. Laher, Reed Riddle, Jesper Sollerman
Figure caption: Constraints on a shock breakout model for the optical/UV emission from 24puz, assuming that the ejecta mass (Mej) is much larger than the circumtransient medium mass (Mctm), and the circumtransient medium has a power-law density profile with slope s = 1. The optical/UV blackbody luminosity is shown as a function of time in black in both panels. The red points show the luminosity obtained from early g-band-only detections of 24puz, for which we could not fully constrain the luminosity. We assume the temperature is the average of over the first ∼5 days. We show the case of small tbo for illustration. The shock emergence is assumed to occur on the same day in both panels, corresponding to the time at which the luminosity begins to decrease. The blue solid line shows the expected power-law evolution of the lightcurve within the shock breakout model, from Equation (9). The resulting inferred physical parameters (circumtransient medium radius Rctm and mass Mctm) are listed on the bottom, including a range of possible shock velocities inferred from the assumption that Mej ≫ Mctm, and the ejecta mass is reasonably small ≲102 M⊙.
Paper: A Luminous and Hot Infrared through X-Ray Transient at a 5 kpc Offset from a Dwarf Galaxy
Authors: Jean J. Somalwar, Vikram Ravi, Raffaella Margutti, Ryan Chornock, Priyamvada Natarajan, Wenbin Lu, Charlotte Angus, Matthew J. Graham, Erica Hammerstein, Edward Nathan, Matt Nicholl, Kritti Sharma, Robert Stein, Frank Verdi, Yuhan Yao, Eric C. Bellm, Tracy X. Chen, Michael W. Coughlin, David Hale, Mansi M. Kasliwal, Russ R. Laher, Reed Riddle, Jesper Sollerman
Figure caption: Blackbody fits to each epoch of UV/optical imaging of 24puz, as described in Section 4.2. The fits are shown as colored bands, and the data as black scatter points.
Paper: A Luminous and Hot Infrared through X-Ray Transient at a 5 kpc Offset from a Dwarf Galaxy
Authors: Jean J. Somalwar, Vikram Ravi, Raffaella Margutti, Ryan Chornock, Priyamvada Natarajan, Wenbin Lu, Charlotte Angus, Matthew J. Graham, Erica Hammerstein, Edward Nathan, Matt Nicholl, Kritti Sharma, Robert Stein, Frank Verdi, Yuhan Yao, Eric C. Bellm, Tracy X. Chen, Michael W. Coughlin, David Hale, Mansi M. Kasliwal, Russ R. Laher, Reed Riddle, Jesper Sollerman
Figure caption: X-ray lightcurve comparison, adapted from Y. Yao et al. (2022). 24puz is shown in red, and LFBOTs in orange. For completeness, a population of gamma-ray bursts (GRBs) is shown in light blue, as these are common comparison points for X-ray transient emission. The jetted TDE SwJ1644 is shown in blue. 24puz is among the most X-ray luminous LFBOTs. It shows a variability and evolution timescale comparable to both LFBOTs and the jetted TDE.
Paper: A Luminous and Hot Infrared through X-Ray Transient at a 5 kpc Offset from a Dwarf Galaxy
Authors: Jean J. Somalwar, Vikram Ravi, Raffaella Margutti, Ryan Chornock, Priyamvada Natarajan, Wenbin Lu, Charlotte Angus, Matthew J. Graham, Erica Hammerstein, Edward Nathan, Matt Nicholl, Kritti Sharma, Robert Stein, Frank Verdi, Yuhan Yao, Eric C. Bellm, Tracy X. Chen, Michael W. Coughlin, David Hale, Mansi M. Kasliwal, Russ R. Laher, Reed Riddle, Jesper Sollerman
Figure caption: Spectral constraints from the MJD 60558 (37.6 rest-day) XMM-Newton observations, in the same format as Figure 10. We assume no absorption in this fit, based on the results from the higher signal-to-noise MJD 60536 observations. The photon-index from the first epoch is shown in blue. The photon-index has tentatively softened: the probability that the photon-index is consistent with the first epoch is P(Γ ≤ 1.73) = 1%.
Paper: A Luminous and Hot Infrared through X-Ray Transient at a 5 kpc Offset from a Dwarf Galaxy
Authors: Jean J. Somalwar, Vikram Ravi, Raffaella Margutti, Ryan Chornock, Priyamvada Natarajan, Wenbin Lu, Charlotte Angus, Matthew J. Graham, Erica Hammerstein, Edward Nathan, Matt Nicholl, Kritti Sharma, Robert Stein, Frank Verdi, Yuhan Yao, Eric C. Bellm, Tracy X. Chen, Michael W. Coughlin, David Hale, Mansi M. Kasliwal, Russ R. Laher, Reed Riddle, Jesper Sollerman
Figure caption: Summary of results from the MOSFIT TDE modeling. Realizations from the MCMC samples are overlaid on select observations in the left panel. We only include observations in representative bands for clarity, but perform the fit with all data. The constraints on BH (MBH) and disrupted star mass (Ms) are shown in the right panel.
Paper: A Luminous and Hot Infrared through X-Ray Transient at a 5 kpc Offset from a Dwarf Galaxy
Authors: Jean J. Somalwar, Vikram Ravi, Raffaella Margutti, Ryan Chornock, Priyamvada Natarajan, Wenbin Lu, Charlotte Angus, Matthew J. Graham, Erica Hammerstein, Edward Nathan, Matt Nicholl, Kritti Sharma, Robert Stein, Frank Verdi, Yuhan Yao, Eric C. Bellm, Tracy X. Chen, Michael W. Coughlin, David Hale, Mansi M. Kasliwal, Russ R. Laher, Reed Riddle, Jesper Sollerman
Figure caption: Corner plot showing the full MOSFIT parameter set.
Paper: Kinematically Complex Circumgalactic Gas Around a Low-mass Galaxy: Filamentary Inflow and Counterrotation in J0910b
Authors: Zeren Lin, D. Christopher Martin, Mateusz Matuszewski, James D. Neill, Drew M. Miles, Vincent Picouet, Nikolaus Z. Prusinski, Keri Hoadley, Rosalie McGurk
Figure caption: Top row: surface brightness maps of Hα and [O III] λ5007 with an overlay of a pseudo-slit tracing Filament 1. The red dashed rectangle marks the spatial region corresponding to Filament 1, beginning 10″ from the galaxy center. Bottom row: velocity along the slit, with x-marked weighted-median velocities. The red dashed horizontal line marks the 10″ location, corresponding to the starting point of Filament 1. As the slit extends farther from the galaxy center, the velocity width narrows, and the median velocity beyond 10″ approaches zero. The Hα velocity is 13.1 ± 2.5 km s−1 and [O III] is −27.2 ± 6.0 km s−1, consistent with a quiet inflow. The slight difference between the redshifted Hα and blueshifted [O III] velocities may be due to the differing spectral resolutions of KCWI-red and KCWI-blue, as well as variations in line shapes. As shown in Figure 13, [O III] is also slightly blueshifted at the galaxy center due to line profile asymmetry. We verified that Hβ does not show this issue and behaves similarly to Hα. The Hα velocities are therefore considered more reliable, as the line appears more symmetric and likely traces a single kinematic component.
Paper: Kinematically Complex Circumgalactic Gas Around a Low-mass Galaxy: Filamentary Inflow and Counterrotation in J0910b
Authors: Zeren Lin, D. Christopher Martin, Mateusz Matuszewski, James D. Neill, Drew M. Miles, Vincent Picouet, Nikolaus Z. Prusinski, Keri Hoadley, Rosalie McGurk
Figure caption: Observed emission-line ratios compared to predictions from the radiative shock and precursor models of M. G. Allen et al. (2008). The left panel shows [O III] λ5007/Hα vs. [O II] λλ3727, 3729/Hα, while the right panel shows [N II] λ6583/Hα vs. [S II] λλ6716, 6731/Hα. Observed values are shown with 15% flux uncertainties as explained in Section 5.2.3. Velocity annotations denote selected shock speeds. The shaded region in the right panel indicates the upper limit on [N II] λ6583/Hα set by the KCWI-red detection threshold. The shock model predictions shown here assume solar abundances, a preshock hydrogen density of nH = 1 cm−3, and a magnetic parameter of ﹩B/\sqrt{n}=3.23\,\mu {\rm{G}}{\,{\rm{cm}}}^{3/2}﹩. None of the model families can simultaneously reproduce all three observed ratios, disfavoring fast shocks as the dominant ionization source.
Paper: Kinematically Complex Circumgalactic Gas Around a Low-mass Galaxy: Filamentary Inflow and Counterrotation in J0910b
Authors: Zeren Lin, D. Christopher Martin, Mateusz Matuszewski, James D. Neill, Drew M. Miles, Vincent Picouet, Nikolaus Z. Prusinski, Keri Hoadley, Rosalie McGurk
Figure caption: Comparison of the Hα emission and the adjacent continuum region. Left: adaptive smoothing applied to the Hα emission line (7188–7192 Å). Right: continuum near the Hα region (7198–7202 Å). The black contour marks the 95% light threshold of the stellar continuum, which we adopt as the ISM–CGM boundary, and is overlaid on both panels for clarity. A circle representing a 2″ radius PSF is shown to illustrate the hypothetical worst-case scenario for seeing conditions.
Paper: Kinematically Complex Circumgalactic Gas Around a Low-mass Galaxy: Filamentary Inflow and Counterrotation in J0910b
Authors: Zeren Lin, D. Christopher Martin, Mateusz Matuszewski, James D. Neill, Drew M. Miles, Vincent Picouet, Nikolaus Z. Prusinski, Keri Hoadley, Rosalie McGurk
Figure caption: Penalized PiXel-Fitting (pPXF) results of J0910b. Top: the observed galaxy spectrum and the best-fit model, similar to Figure 1. For clarity, only the stellar continuum fitting results are displayed, though gas components are fitted simultaneously. The two dominant simple stellar population components correspond to ages of 0.4 and 7.1 Gyr. Bottom: observed vs. fitted photometry from GALEX FUV to WISE W2 bands, corrected for Galactic extinction. The gray shaded region denotes the wavelength range covered by KCWI-blue and KCWI-red data.
Paper: Kinematically Complex Circumgalactic Gas Around a Low-mass Galaxy: Filamentary Inflow and Counterrotation in J0910b
Authors: Zeren Lin, D. Christopher Martin, Mateusz Matuszewski, James D. Neill, Drew M. Miles, Vincent Picouet, Nikolaus Z. Prusinski, Keri Hoadley, Rosalie McGurk
Figure caption: Same as Figure 17, but for Filament 2 (∼30 kpc). The posteriors indicate low density, low metallicity, and a modest UV field, broadly consistent with Filament 1. Slightly higher density and metallicity may reflect localized enrichment, geometric variations, or different physical conditions in the inflow.
Paper: Kinematically Complex Circumgalactic Gas Around a Low-mass Galaxy: Filamentary Inflow and Counterrotation in J0910b
Authors: Zeren Lin, D. Christopher Martin, Mateusz Matuszewski, James D. Neill, Drew M. Miles, Vincent Picouet, Nikolaus Z. Prusinski, Keri Hoadley, Rosalie McGurk
Figure caption: Same as Figure 17, but for Filament 1 (∼30 kpc). The posteriors indicate lower density and metallicity than in the counterrotating CGM, along with a modest UV field. The elevated column density suggests a long path length through the filament, consistent with its extended morphology.
Paper: Kinematically Complex Circumgalactic Gas Around a Low-mass Galaxy: Filamentary Inflow and Counterrotation in J0910b
Authors: Zeren Lin, D. Christopher Martin, Mateusz Matuszewski, James D. Neill, Drew M. Miles, Vincent Picouet, Nikolaus Z. Prusinski, Keri Hoadley, Rosalie McGurk
Figure caption: Posterior distributions for hydrogen density, UV boost factor, gas-phase metallicity, and hydrogen column density at Point A (9 kpc) based on MCMC sampling of the CLOUDY grid. Contours show 1σ, 2σ, and 3σ confidence levels.
Paper: Kinematically Complex Circumgalactic Gas Around a Low-mass Galaxy: Filamentary Inflow and Counterrotation in J0910b
Authors: Zeren Lin, D. Christopher Martin, Mateusz Matuszewski, James D. Neill, Drew M. Miles, Vincent Picouet, Nikolaus Z. Prusinski, Keri Hoadley, Rosalie McGurk
Figure caption: Schematic illustration of the inferred gas flow structure in J0910b. Filaments 1 and 2 supply cold gas into the halo, where it becomes part of the counterrotating CGM. The dashed oval marks the ISM–CGM interface, which coincides with both the shell-like structure seen in the velocity dispersion maps and the radial transition where counterrotation emerges.
Paper: Kinematically Complex Circumgalactic Gas Around a Low-mass Galaxy: Filamentary Inflow and Counterrotation in J0910b
Authors: Zeren Lin, D. Christopher Martin, Mateusz Matuszewski, James D. Neill, Drew M. Miles, Vincent Picouet, Nikolaus Z. Prusinski, Keri Hoadley, Rosalie McGurk
Figure caption: Same as Figure 17, but for Point B (16 kpc). The posteriors suggest a lower gas density and UV field strength, but higher metallicity compared to Point A.
Paper: Kinematically Complex Circumgalactic Gas Around a Low-mass Galaxy: Filamentary Inflow and Counterrotation in J0910b
Authors: Zeren Lin, D. Christopher Martin, Mateusz Matuszewski, James D. Neill, Drew M. Miles, Vincent Picouet, Nikolaus Z. Prusinski, Keri Hoadley, Rosalie McGurk
Figure caption: LSF variations for different illumination patterns and spectrographs. Top row: simulated light distributions for uniform illumination (left), asymmetric illumination with light concentrated on the left (middle), and asymmetric illumination with light concentrated on the right (right), overlaid on a schematic representation of three slicers. These illustrate how light interacts with the slicers under different spatial distributions. Middle row: LSF profiles for KCWI-blue for the central slicer under uniform and asymmetric illumination, showing how the spectrograph’s resolution interacts with varying illumination patterns. Bottom row: LSF profiles for KCWI-red for the central slicer under the same illumination patterns, highlighting differences due to the higher spectral resolution of the spectrograph. Uniform LSFs are observed for diffuse CGM-like regions, while asymmetric illumination introduces significant variations in the LSF, impacting velocity measurements. The choice of spectrograph LSF σ and slicer width values are based on arc lamp calibration images, ensuring consistency with instrument characteristics.
Paper: Kinematically Complex Circumgalactic Gas Around a Low-mass Galaxy: Filamentary Inflow and Counterrotation in J0910b
Authors: Zeren Lin, D. Christopher Martin, Mateusz Matuszewski, James D. Neill, Drew M. Miles, Vincent Picouet, Nikolaus Z. Prusinski, Keri Hoadley, Rosalie McGurk
Figure caption: Covariance calibration before adaptive smoothing. Instead of employing exact error propagation with the covariance matrix, we calibrate the effective variance change caused by the nondiagonal elements. This calibration depends on the kernel sizes (for box2d kernels of size n, Nkernel = n2) and can be described by a logarithmic function ﹩{\sigma }_{{\rm{meas}}}={\sigma }_{{\rm{nocov}}}(1+\alpha {\mathrm{log}}({N}_{{\rm{kernel}}}))﹩, where σmeas represents the measured standard deviation, and σnocov indicates the standard deviation assuming no correlation between the pixels (B. Husemann et al. 2013). The calibration approaches an asymptotic value after a threshold of Nkernel,th ∼ 40, reflecting the finite correlation length introduced during the coaddition step.
Paper: Kinematically Complex Circumgalactic Gas Around a Low-mass Galaxy: Filamentary Inflow and Counterrotation in J0910b
Authors: Zeren Lin, D. Christopher Martin, Mateusz Matuszewski, James D. Neill, Drew M. Miles, Vincent Picouet, Nikolaus Z. Prusinski, Keri Hoadley, Rosalie McGurk
Figure caption: Statistical properties of the adaptive smoothing residual. Left: the autocorrelation function ξ(r) is displayed before (top) and after (bottom) adaptive smoothing. Each wavelength layer is plotted, with the black solid line representing the median, and the shaded gray region indicating the 25th to 75th percentiles of the distribution. The correlation scale is approximately r < 5, consistent with the findings in Figure D1. Notably, except for the outlying curves that represent the detected signal, ξ(r) shows no significant changes before and after the adaptive smoothing process. Right: histogram of the SNR for the adaptive smoothing residual. The distribution exhibits slight deviations from a normal distribution, likely resulting from a combination of the removal of bins with SNR > 2.5 due to adaptive smoothing and error propagation, as we normalize the variance immediately following coaddition, as discussed in Section 3.1.
Paper: Kinematically Complex Circumgalactic Gas Around a Low-mass Galaxy: Filamentary Inflow and Counterrotation in J0910b
Authors: Zeren Lin, D. Christopher Martin, Mateusz Matuszewski, James D. Neill, Drew M. Miles, Vincent Picouet, Nikolaus Z. Prusinski, Keri Hoadley, Rosalie McGurk
Figure caption: Radial profiles of the [O III] λ5007 and Hα emission with an interval of 5″ (left) and 1″ (right) with and without adaptive smoothing. The profiles show the [O III] λ5007 (blue) and Hα (red) emissions. Scattered points represent the unsmoothed data before adaptive smoothing and after continuum subtraction, with error bars indicating the 25th to 75th percentiles. The 5″ interval profiles exhibit smaller noise levels for the unsmoothed data, while the 1″ interval profiles are provided for comparison with Figure 9. Solid lines represent the profiles after adaptive smoothing, with shaded regions reflecting the 25th to 75th percentiles. Other lines are not included due to insufficient detection in the unsmoothed data. Notably, the profiles for [O III] λ5007 and Hα remain largely unchanged after adaptive smoothing, even with the finer 1″ radial grids.