adsabs/AstroCLIMB huggingface dataset:
Paper: A Late-time Radio Search for Highly Off-axis Jets from PTF Broad-lined Ic Supernovae in GRB-like Host Galaxy Environments
Authors: Genevieve Schroeder, Anna Y. Q. Ho, Ranadeep G. Dastidar, Maryam Modjaz, Alessandra Corsi, Paul C. Duffell
Figure caption: Rest-frame light curves for 10 GHz afterglow models at off-axis angles of θobs = 30°, 60°, 90° (lines, orange, pink, purple, respectively) for E = 2 × 1051 erg and n = 0.01 cm−3 generated by the FIREFLY code (R. G. Dastidar & P. C. Duffell 2024). The light curves of PTF10bzf (A. Corsi et al. 2016; this work; triangles) and PTF10tqv (this work; stars) are shown in green. Also shown are the radio nondetections presented in A. Corsi et al. (2023) for a sample of ZTF SNe Ic-bl (gray, triangles represent 3σ upper limits), as well as the radio light curves of several supernova: SN 1998bw (associated with GRB 980425; S. R. Kulkarni et al. 1998; E. Waxman et al. 1998), SN 2006aj (associated with GRB 060218; A. M. Soderberg et al. 2006), SN 2009bb (A. M. Soderberg et al. 2010), SN 2012ap (S. Chakraborti et al. 2015), and SN 2020bvc (A. Y. Q. Ho et al. 2020b). The sampling of PTF10bzf represents a well-spaced observational strategy to constrain the existence of off-axis jets at any θobs. The 5σ depth of a 1 hr 10 GHz VLA observation at our proposed cadence (black horizontal dashed lines), a 3 GHz VLASS observation at ∼1–2 yr (black horizontal dotted line) and a 1.4 GHz observation with the Deep Synoptic Array 2000 (DSA-2000) between ∼0.3 and 14 yr, at the median ZTF BTS Ic-bl redshift of z = 0.04, are presented for reference.
Paper: Fermi-LAT Captures a Late-2024 Gamma-Ray Outburst near Two Newly Identified Gamma-Ray-emitting Galactic Supernova Remnants, without Evidence of Physical Association
Authors: Miltiadis Michailidis, Marianne Lemoine-Goumard, Niccolo Di Lalla, Nicola Omodei, C. C. Cheung, Guillem Marti-Devesa, Denis Bernard
Figure caption: Outburst SEDs and light curves. The top panels present the LAT SEDs in the 100 MeV to 800 GeV energy range. Upper left panel: LAT SEDs using 3 days from August 6, 12:00 to August 9, 12:00 (MET: 744638405 to 744897605), 18 hr from August 7, 12:00 to August 8, 06:00 (MET: 744724805 to 744789605), and 6 hr from August 7, 12:00 to August 7, 18:00 (MET: 744724805 to 744746405) of data sets in green, blue, and orange, respectively. Upper right panel: LAT SED from the location of the outburst using 16.5 yr of data from August 8, 2008, to February 13, 2025 (MET: 239557417 to 761167438). The bottom panels depict the LAT light curves for the 5 days period from August 5, 12:00 to August 10, 12:00 (MET: 744552005 to 744984005) centered at the event peak, >1 GeV (left) and >100 MeV (right), with single-day bins in yellow and 6 hr bins in black.
Paper: A Late-time Radio Search for Highly Off-axis Jets from PTF Broad-lined Ic Supernovae in GRB-like Host Galaxy Environments
Authors: Genevieve Schroeder, Anna Y. Q. Ho, Ranadeep G. Dastidar, Maryam Modjaz, Alessandra Corsi, Paul C. Duffell
Figure caption: The 5–10 GHz light curves and upper limits of our PTF sample (green, with observations presented in this paper filled in), compared to SNe Ic-bl samples from A. Corsi et al. (2016, PTF, light gray) and A. Corsi et al. (2023, ZTF, dark gray). Also shown are off-axis 10 GHz afterglow models generated by the FIREFLY code for three off-axis angles (θobs = 30°, 60°, 90°; orange, pink, purple, respectively) and for two n–E pairs (E = 2 × 1051 erg, n = 10−2 cm−3, solid lines and E = 2 × 1052 erg, n = 10−3 cm−3, dashed lines). Points represent detections and triangles represent upper limits (3σ unless otherwise stated). The detections of PTF10tqv are represented as stars. We also label two SNe Ic-bl, PTF11qcj and PTF11cmh (A. Corsi et al. 2014, 2016; N. T. Palliyaguru et al. 2019, 2021), whose luminous radio emission is thought to arise from circumstellar medium (CSM) interaction, as well as the SNe Ic-bl with the deepest luminosity limits in our sample, PTF10vgv.
Paper: A Late-time Radio Search for Highly Off-axis Jets from PTF Broad-lined Ic Supernovae in GRB-like Host Galaxy Environments
Authors: Genevieve Schroeder, Anna Y. Q. Ho, Ranadeep G. Dastidar, Maryam Modjaz, Alessandra Corsi, Paul C. Duffell
Figure caption: Left: Sloan Digital Sky Survey (SDSS) image of the host galaxy of PTF10tqv (SDSS J224654.99+174728.5). Crosshairs represent the optical location of PTF10tqv. Middle: the 10 GHz VLA image of the location of PTF10tqv, obtained on 2020 August 1 (Δt = 3623 days, observer frame). Right: the 3.1 GHz MeerKAT image of the location of PTF10tqv, obtained on 2025 March 1 (Δt = 5296 days, observer frame). For the VLA and MeerKAT images, contours represent the 5σ level of the image and crosses represent the location of the brightest pixel near the location of PTF10tqv. These contours are also overplotted on the SDSS image to demonstrate the location of the radio source. The length scale is the same for all three panels, and stated in the top right of the left panel. The observing frequency is stated in the top left. When available, the beam size is represented as an ellipse in the bottom left, and the observation date is stated on the bottom right of each image.
Paper: A Late-time Radio Search for Highly Off-axis Jets from PTF Broad-lined Ic Supernovae in GRB-like Host Galaxy Environments
Authors: Genevieve Schroeder, Anna Y. Q. Ho, Ranadeep G. Dastidar, Maryam Modjaz, Alessandra Corsi, Paul C. Duffell
Figure caption: The interstellar medium density (n) versus jet energy (E) parameter space for three off-axis observer angles (θobs = 30°, 60°, 90°), from models generated by the FIREFLY code. Lines represent the constraints on the parameter space from each of our 11 nondetections, where the upper right of each line is ruled out and the lower left of each line is still allowed. We similarly display the constraints that can be placed on the n–E parameter space given our suggested observational strategy of future SNe Ic-bl (Section 4, green). Also shown are the beaming-corrected kinetic energy and n values for some on-axis GRBs (A. Panaitescu & P. Kumar 2002; T. Kangas & A. S. Fruchter 2021).
Paper: A Late-time Radio Search for Highly Off-axis Jets from PTF Broad-lined Ic Supernovae in GRB-like Host Galaxy Environments
Authors: Genevieve Schroeder, Anna Y. Q. Ho, Ranadeep G. Dastidar, Maryam Modjaz, Alessandra Corsi, Paul C. Duffell
Figure caption: Host galaxy (left, SDSS g-band or PanSTARRS i-band) and VLA 10 GHz (right) images of PTF09sk, PTF10xem, PTF11lbm (top, middle, bottom, respectively). Crosshairs represent the optical location of each SN. For the VLA images, contours represent the 5σ level of the image. When available, the observatory and observing frequency/band is stated in the top left, the length scale is stated in the top right, the beam size is represented as an ellipse in the bottom left, and the observation date is stated in the bottom right of each image. The radio detection in the PTF10xem VLA image is coincident with the center of its host galaxy, SHOC 084. PTF09sk and PTF11lbm both have <5σ sources near the location of the SN; however association with the SN is not possible with available data (see Section 2.1).
Paper: A Late-time Radio Search for Highly Off-axis Jets from PTF Broad-lined Ic Supernovae in GRB-like Host Galaxy Environments
Authors: Genevieve Schroeder, Anna Y. Q. Ho, Ranadeep G. Dastidar, Maryam Modjaz, Alessandra Corsi, Paul C. Duffell
Figure caption: Left: the 10 GHz (black) and 3.1 GHz (white) radio detections of PTF10tqv. Also shown are off-axis afterglow models consistent within 2σ of the detections, for off-axis angles of θobs = 30°, 60°, 90° (purple, orange, pink, respectively), where solid lines represent 10 GHz models and dashed lines represent 3 GHz models. Right: the circumburst density (n) versus total jet energy (E) space for the off-axis models generated by FIREFLY. Shaded regions represent the space consistent within 2σ of the radio detections of the counterpart to PTF10tqv.
Paper: Fermi-LAT Captures a Late-2024 Gamma-Ray Outburst near Two Newly Identified Gamma-Ray-emitting Galactic Supernova Remnants, without Evidence of Physical Association
Authors: Miltiadis Michailidis, Marianne Lemoine-Goumard, Niccolo Di Lalla, Nicola Omodei, C. C. Cheung, Guillem Marti-Devesa, Denis Bernard
Figure caption: The Fermi-LAT SEDs for 3C 434.1 (left panel) and G093.7–00.2 (right panel) spanning the 100 MeV–800 GeV energy range. Systematic contributions are depicted in black in both panels, corresponding to the energy intervals where a statistically significant gamma-ray signal was detected.
Paper: A Data-driven Approach for Star Formation Parameterization Using Symbolic Regression
Authors: Diane M. Salim, 美玲 林, Matthew E. Orr, Blakesley Burkhart, Rachel S. Somerville, Miles Cramner
Figure caption: Points indicating the equation “score” as originally defined by M. Cranmer (2023; top row) and the R2 (bottom row) of all equations found during the 4000 epoch training run for the two experiments when SF is averaged over 〈tSFR〉 = 10 Myr (left) and when averaged over 〈tSFR〉 = 100 Myr (right). In all panels the orange points indicate the models that satisfy the criteria to count as a “top equation,” as highlighted in Section 2. In the bottom panel, the gray dashed–dotted lines are indicative of a perfect R2 value of 1, which occurs when the model and the data are in exact agreement. The dashed pink lines are indicative of the R2 value that the XGBoost model achieves when trained on the same data set, and represents the upper limit to an R2 value that equation-based models can achieve. The shapes of the points showcase the combination of variables that feature in each model. Crosses indicate models that are described by just one constant value, circle points indicate that only Σgas is present in the model, star-shaped points indicate that only Σ* is present in the model, diamond-shaped points indicate that Σgas and Ωdyn are present in the model, triangle points designate models featuring both Σgas and Σ*, and square points specify models constructed via all three of the features Σgas, Σ*, and σgas,z. Note that there exist one and two models in the 〈tSFR〉 = 10 Myr and 〈tSFR〉 = 100 Myr experiments, respectively, that yielded a score of 0, and thus do not appear in the top panel of Figure 5, which features a logarithmic scale.
Paper: A Data-driven Approach for Star Formation Parameterization Using Symbolic Regression
Authors: Diane M. Salim, 美玲 林, Matthew E. Orr, Blakesley Burkhart, Rachel S. Somerville, Miles Cramner
Figure caption: Distribution of points across the KS (logarithmic Σgas–ΣSFR) plane, the logarithmic σgas,z–ΣSFR plane, and the Σ*–ΣSFR planes of the native FIRE data (gray contours) and ΣSFR attained for the respective equations found by PySR (colored contours; green, purple, and blue for Σgas, σgas,z, and Σ*, respectively). For both categories of contours, the outer (lightest colored) to innermost (darkest colored) regions represent where 95%, 80%, 50%, and 20% of the probability mass of the data in this plane lies. The dashed line shows the original K98 relation. The pink line shows how the PySR-found equation would behave on this plane when the features other than Σgas are set to the fiducial values for local spiral galaxies as tabulated in Table 1.
Paper: A Data-driven Approach for Star Formation Parameterization Using Symbolic Regression
Authors: Diane M. Salim, 美玲 林, Matthew E. Orr, Blakesley Burkhart, Rachel S. Somerville, Miles Cramner
Figure caption: Distribution of points across the KS plane of the FIRE data (gray contours) predicted by the respective models labeled in the top-left orange boxes for the 〈tSFR〉 = 10 Myr (left subfigure) and 〈tSFR〉 = 100 Myr (right subfigure) experiments. For all contours (gray and green), the regions represent the 95%, 80%, 50%, and 20% data inclusion region in the plane (from lightest to darkest colored, outside-in). The dashed, dark gray line shows the original K98 relation. The vertical line shows the Σgas cut of Σgas = 10 M⊙ pc−2, points below which we do not consider in this study, and the horizontal line shows the numerical SF floor in the simulations set by ΣSFR,floor = mb/(A · 〈tSFR〉), where mb is the minimum baryonic mass of 7100 M⊙, A is the simulation’s Cartesian projection pixel size of (750 pc)2 in our input maps, and 〈tSFR〉 is the time over which the SF is averaged over, in this case either 10 or 100 Myr.
Paper: A Data-driven Approach for Star Formation Parameterization Using Symbolic Regression
Authors: Diane M. Salim, 美玲 林, Matthew E. Orr, Blakesley Burkhart, Rachel S. Somerville, Miles Cramner
Figure caption: SHAP values for the input features used to train an XGBoost model for when SF is averaged over 〈tSFR〉 = 10 Myr (left) and when averaged over 〈tSFR〉 = 100 Myr (right). Each point in this figure indicates the SHAP value of that corresponding data point, colored by the relative strength of that particular feature, with red indicating high values and blue indicating low values of that feature. A blue to red gradient across the beeswarm diagram for a particular feature indicates a correlation between that input variable and the target variable, whereas a red to blue gradient indicates an anticorrelation. Features are ranked from most predicted influence to least influence on the target variable from top to bottom, respectively.
Paper: A Data-driven Approach for Star Formation Parameterization Using Symbolic Regression
Authors: Diane M. Salim, 美玲 林, Matthew E. Orr, Blakesley Burkhart, Rachel S. Somerville, Miles Cramner
Figure caption: Same as in Figure 7, but showing the results for the 〈tSFR〉 = 100 Myr experiment. Note that only five equations met the criteria to be considered a top equation.
Paper: A Data-driven Approach for Star Formation Parameterization Using Symbolic Regression
Authors: Diane M. Salim, 美玲 林, Matthew E. Orr, Blakesley Burkhart, Rachel S. Somerville, Miles Cramner
Figure caption: Evolution of the total loss values as defined by Equation (6) (top rows) and the quantile loss values as defined by Equation (5) (bottom rows) by training epoch for the 10 Myr averaged SFR target variable experiment (left subfigure) and the 100 Myr averaged SFR target variable experiment (right subfigure). The colored lines indicate the losses as defined by Equation (6) for the training (left columns within subfigures) and test (right columns within subfigures) data samples as a function of the number of training epochs for the top equations as selected by the method described in Section 2. Note that while some equations exhibit the same complexity and therefore are represented by the same line color between the 〈tSFR〉 = 10 Myr SFR and 〈tSFR〉 = 100 Myr SFR experiments, they are indeed representing different equations unique to the experiment of that specific SFR timescale. The gray dotted line shown in the panels of the training loss curves indicates the lowest scoring loss among the analytic models considered in this study. This is the “baseline” loss that the top selected equations must exhibit a lower loss than.
Paper: A Data-driven Approach for Star Formation Parameterization Using Symbolic Regression
Authors: Diane M. Salim, 美玲 林, Matthew E. Orr, Blakesley Burkhart, Rachel S. Somerville, Miles Cramner
Figure caption: Distribution of points across the KS plane of the native FIRE data (gray contours), with the found models at fiducial values for features other than Σgas overlaid, colored by complexity of the models. Style as in Figure 3.
Paper: A Data-driven Approach for Star Formation Parameterization Using Symbolic Regression
Authors: Diane M. Salim, 美玲 林, Matthew E. Orr, Blakesley Burkhart, Rachel S. Somerville, Miles Cramner
Figure caption: The predicted ΣSFR of the top four models found by PySR in comparison to the native ΣSFR of the FIRE-2 test sample, with the color indicating the value of Σgas at that point for the 〈tSFR〉 = 10 Myr (left column) and 100 Myr (right column) experiments. The overlaid contours represent, from the outer to innermost contours, where 90%, 50%, and 20% of the probability mass of the data in this plane lies. The found equation itself is shown in the orange box in the top-left-hand corner of each panel. The one-to-one line is shown as the gray dashed–dotted line. The complexity of the equation and the R2 value of the model is written directly beneath the equation. A model that predicts the data perfectly would exhibit an R2 of 1, and all points would lie on the one-to-one line.
Paper: A Data-driven Approach for Star Formation Parameterization Using Symbolic Regression
Authors: Diane M. Salim, 美玲 林, Matthew E. Orr, Blakesley Burkhart, Rachel S. Somerville, Miles Cramner
Figure caption: SHAP values for the four input features used to create the synthetic FG13 data set and train an XGBoost model. Each point in this figure indicates the SHAP value of that corresponding data point, colored by the relative strength of that particular feature, with red indicating high values and blue indicating low values of that feature. Features are ranked from most predicted influence to least influence on the target variable from top to bottom, respectively.
Paper: Unveiling Central Ortho-H2D+ Depletion at Sub-kau Scales in Prestellar Core G205.46-14.56 M3: The First Interferometric Evidence and Implications for Deuterium Chemistry
Authors: Sheng-Jun Lin, Sheng-Yaun Liu, Dipen Sahu, Laurent Pagani, Tien-Hao Hsieh, Naomi Hirano, Shih-Ping Lai, Tie Liu, Shih-Ying Hsu, Shanghuo Li, Kee-Tae Kim
Figure caption: Multiscale view of the prestellar core G205.46−14.56 M3 in dust continuum and integrated molecular line emission. (a) Spitzer IRAC 8 μm image of the three JCMT dense cores G205.46−14.56 M1, M2, and M3 (S. Dutta et al. 2020). JCMT SCUBA-2 850 μm continuum contours overlaid at 10%–90% (20% steps) of the peak of the faintest prestellar core, G205 M3 (500 mJy beam−1), with additional contours at 1000 and 2000 mJy beam−1. Colored symbols mark protostars compiled by B. Reipurth et al. (2023): five cyan circles denote the Class 0/I multiple system SSV 63 hosted by M2, one red square marks the Class 0 source HOPS 317 embedded in M1, and the green triangle indicates the Class II source IRS 1. A cyan dashed box outlines the region enlarged in panels (b) and (c), and a magenta box encloses panels (d)–(f); these same borders are repeated around the zoom-in panels to guide the eye. (b) ALMA Band 7 820 μm continuum. (c) ALMA Band 7 ortho-H2D+ (110–111) map integrated over vLSR = 9.5–10.8 km s−1. (d) ALMA Band 6 N2D+ (3–2) map integrated over vLSR = 9.1–11.6 km s−1, where the Total-Power (TP) data are included to recover extended emission. (e) ALMA Band 3 N2H+ (1–0) isolated hyperfine component integrated over vLSR = 9.0–11.1 km s−1 and combined with TRAO single-dish data. (f) ALMA Band 7 N2H+ (4–3) map integrated over vLSR = 9.6–10.9 km s−1. ALMA emission contour levels are labeled in each panel; the 3σ contour is drawn in white to maximize contrast against the color scale, whereas higher levels are black for molecular lines. These 1σ levels are 0.5 mJy beam−1 in panel (b), and 4.5, 12, 1.6, and 5 mJy beam−1 km s−1 in panels (c)–(f), respectively. Contours from panel (b) are overlaid on all other panels for reference. Crosses denote the substructures B1 and B2 (D. Sahu et al. 2021), asterisks mark positions adopted for the non-LTE radiative-transfer analysis (Section 4.3). Beam sizes and scale bars are indicated in each panel. We note that the ALMA color images are primary-beam corrected, whereas contours are drawn from uncorrected images with uniform noise.
Paper: Unveiling Central Ortho-H2D+ Depletion at Sub-kau Scales in Prestellar Core G205.46-14.56 M3: The First Interferometric Evidence and Implications for Deuterium Chemistry
Authors: Sheng-Jun Lin, Sheng-Yaun Liu, Dipen Sahu, Laurent Pagani, Tien-Hao Hsieh, Naomi Hirano, Shih-Ping Lai, Tie Liu, Shih-Ying Hsu, Shanghuo Li, Kee-Tae Kim
Figure caption: Spherical physical model of G205.46−14.56 M3 B1 based on spectra extracted along the southwest cut in the non-LTE radiative transfer analysis. The finer model grid (light gray vertical lines) resolves the x(o-H2D+) profile with a step size of 0﹩\mathop{.}\limits^{^{\prime\prime} }﹩79, while the coarser model grid (dark gray vertical lines) resolves the x(N2D+) and x(N2H+) profiles with a step size of 2﹩\mathop{.}\limits^{^{\prime\prime} }﹩38. (a) Plummer-like ﹩{n}_{{{\rm{H}}}_{2}}﹩ profile is adopted from D. Sahu et al. (2023), with error bars reflecting a factor-of-2 variation due to typical dust opacity uncertainties. (b) Tk profile is assumed to be 10 K, except for r < 1﹩\mathop{.}\limits^{^{\prime\prime} }﹩91, where 8 K is inferred from multitransition N2H+ observations. The Tex profiles derived from non-LTE modeling are shown for each spectral line. (c) Volumetric abundance profiles, including (d) N2H+ deuteration, are fitted to the extracted spectra (Figure 4) with 1σ error bars shown. Chemodynamical model results at a core age of 0.42 Ma for the ﹩{n}_{{{\rm{H}}}_{2}}﹩, Tk, x(o-H2D+), and several deuteration profiles are overlaid for comparison.
Paper: Unveiling Central Ortho-H2D+ Depletion at Sub-kau Scales in Prestellar Core G205.46-14.56 M3: The First Interferometric Evidence and Implications for Deuterium Chemistry
Authors: Sheng-Jun Lin, Sheng-Yaun Liu, Dipen Sahu, Laurent Pagani, Tien-Hao Hsieh, Naomi Hirano, Shih-Ping Lai, Tie Liu, Shih-Ying Hsu, Shanghuo Li, Kee-Tae Kim
Figure caption: G205.46−14.56 M3 kinematics traced by ortho-H2D+. (a) Centroid velocity map, using data with ≥3σ detection on the integrated-intensity map (with the 3σ and 7σ contours overlaid; see Figure 1(b)). (b) Velocity dispersion map, only using data with ≥5σ detection at the spectral peaks. (c) Averaged spectra for B1 (blue) and B2 (red), extracted from the regions enclosed by the corresponding dashed circles in panel (a), with fitted Gaussian profiles and annotated parameters. The centroid velocity of B1 serves as the velocity reference in panel (a). The normalized o-H2D+ (110–111) HFS pattern is also shown in black beneath the B1 spectrum. (d) KDE distribution of velocity dispersions with a rug plot. The fitted bimodal model and its parameters are annotated, with the two dispersion peaks overlaid on panel (b) as contours. Vertical lines show the expected velocity dispersion including channel broadening for pure thermal cases and ﹩{ \mathcal M }=1﹩ cases assuming 5 K and/or 8 K (see Appendix C).
Paper: Unveiling Central Ortho-H2D+ Depletion at Sub-kau Scales in Prestellar Core G205.46-14.56 M3: The First Interferometric Evidence and Implications for Deuterium Chemistry
Authors: Sheng-Jun Lin, Sheng-Yaun Liu, Dipen Sahu, Laurent Pagani, Tien-Hao Hsieh, Naomi Hirano, Shih-Ping Lai, Tie Liu, Shih-Ying Hsu, Shanghuo Li, Kee-Tae Kim
Figure caption: Ortho-H2D+ column density analysis assuming LTE with Tex = 8 K. Calculations are limited to regions with ortho-H2D+ (110–111) integrated intensities of S/N > 3. (a) Spectral peak map overlaid with contour levels at 4σ, 6σ, and 8σ, where 1σ = 0.17 K. These ﹩{T}_{{\rm{b}}}﹩ contour levels correspond to optical depths, ﹩{\tau }_{\nu }﹩, of the order of 0.4, 0.7, and 1.0. (b) o-H2D+ column density map, N(o-H2D+), overlaid with contour levels at 5σ, 8σ, 11σ, and 14σ, where σ = 1.7 × 1012 cm-2. (c) Molecular hydrogen column density map, N(H2), derived from dust continuum emission assuming Tdust = 8 K. Contour levels are at 3σ, 7σ, and 11σ, corresponding to 8.5 × 1022, 2.0 × 1023, and 3.1 × 1023 cm−2, with σ = 2.8 × 1022 cm−2. (d) Column abundance map, X(o-H2D+) = N(o-H2D+)/N(H2), masked at the cyan N(H2) 3σ contour, with logarithmically spaced X(o-H2D+) contour levels annotated on the panel. Crosses mark the substructures B1 and B2, and cyan asterisks/circles indicate positions used for non-LTE radiative transfer modeling (Section 4.3). Beam sizes and spatial scales are shown in the bottom left and top right corners, respectively.