adsabs/AstroCLIMB huggingface dataset:
Paper: ALMA Survey of Orion Planck Galactic Cold Clumps (ALMASOP): Molecular Jets and Episodic Accretion in Protostars
Authors: Somnath Dutta, Chin-Fei Lee, Doug Johnstone, Jeong-Eun Lee, Naomi Hirano, James Di Francesco, Anthony Moraghan, Tie Liu, Dipen Sahu, Sheng-Yuan Liu, Ken'ichi Tatematsu, Paul F. Goldsmith, Chang Won Lee, Shanghuo Li, David Eden, Mika Juvela, Leonardo Bronfman, Shih-Ying Hsu, Kee-Tae Kim, Woojin Kwon, Patricio Sanhueza, Xunchuan Liu, Jesús Alejandro López-Vázquez, Qiuyi Luo, Hee-Weon Yi
Figure caption: G211.47-19.27N. (a) 1.3 mm continuum map at ACA resolution with sensitivity ∼1.15 mJy beam−1. The symbols and contour levels are the same as in Figure 1. (b) The C18O spectra are extracted from high-resolution maps, and V sys = 4.0 km s−1. All symbols are the same as in Figure 3. (c) Integrated CO emission with sensitivity 2.5 K km s−1, with similar symbols to those in Figure 4(a).
Paper: ALMA Survey of Orion Planck Galactic Cold Clumps (ALMASOP): Molecular Jets and Episodic Accretion in Protostars
Authors: Somnath Dutta, Chin-Fei Lee, Doug Johnstone, Jeong-Eun Lee, Naomi Hirano, James Di Francesco, Anthony Moraghan, Tie Liu, Dipen Sahu, Sheng-Yuan Liu, Ken'ichi Tatematsu, Paul F. Goldsmith, Chang Won Lee, Shanghuo Li, David Eden, Mika Juvela, Leonardo Bronfman, Shih-Ying Hsu, Kee-Tae Kim, Woojin Kwon, Patricio Sanhueza, Xunchuan Liu, Jesús Alejandro López-Vázquez, Qiuyi Luo, Hee-Weon Yi
Figure caption: G212.10-19.15S. (a) 1.3 mm continuum map at ACA resolution with sensitivity ∼1.1 mJy beam−1. The symbols and contour levels are the same as in Figure 1. (b) The C18O spectra are extracted from high-resolution maps, and V sys = 4.0 km s−1. All symbols are the same as in Figure 3. (c) Integrated CO emission with sensitivity 1.85 K km s−1, with similar symbols to those in Figure 4(a).
Paper: ALMA Survey of Orion Planck Galactic Cold Clumps (ALMASOP): Molecular Jets and Episodic Accretion in Protostars
Authors: Somnath Dutta, Chin-Fei Lee, Doug Johnstone, Jeong-Eun Lee, Naomi Hirano, James Di Francesco, Anthony Moraghan, Tie Liu, Dipen Sahu, Sheng-Yuan Liu, Ken'ichi Tatematsu, Paul F. Goldsmith, Chang Won Lee, Shanghuo Li, David Eden, Mika Juvela, Leonardo Bronfman, Shih-Ying Hsu, Kee-Tae Kim, Woojin Kwon, Patricio Sanhueza, Xunchuan Liu, Jesús Alejandro López-Vázquez, Qiuyi Luo, Hee-Weon Yi
Figure caption: G211.16-19.33N2. (a) 1.3 mm continuum map at ACA resolution with sensitivity ∼1.1 mJy beam−1. The symbols and contour levels are the same as in Figure 1. (b) The C18O spectra are extracted from high-resolution maps, and V sys = 4.0 km s−1. All symbols are the same as in Figure 3. (c) Integrated CO emission with sensitivity 1.6 K km s−1, with similar symbols to those in Figure 4(a).
Paper: ALMA Survey of Orion Planck Galactic Cold Clumps (ALMASOP): Molecular Jets and Episodic Accretion in Protostars
Authors: Somnath Dutta, Chin-Fei Lee, Doug Johnstone, Jeong-Eun Lee, Naomi Hirano, James Di Francesco, Anthony Moraghan, Tie Liu, Dipen Sahu, Sheng-Yuan Liu, Ken'ichi Tatematsu, Paul F. Goldsmith, Chang Won Lee, Shanghuo Li, David Eden, Mika Juvela, Leonardo Bronfman, Shih-Ying Hsu, Kee-Tae Kim, Woojin Kwon, Patricio Sanhueza, Xunchuan Liu, Jesús Alejandro López-Vázquez, Qiuyi Luo, Hee-Weon Yi
Figure caption: G210.82-19.47S. (a) 1.3 mm continuum map at ACA resolution with sensitivity ∼0.2 mJy beam−1. The symbols and contour levels are the same as in Figure 1. (b) The C18O spectra are extracted from high-resolution maps, and V sys = 6 km s−1. All symbols are the same as in Figure 3. (c) Integrated CO emission with sensitivity 0.8 K km s−1, with similar symbols to those in Figure 4(a).
Paper: JWST Imaging of Edge-on Protoplanetary Disks. I. Fully Vertically Mixed 10 μm Grains in the Outer Regions of a 1000 au Disk
Authors: Gaspard Duchêne, François Ménard, Karl R. Stapelfeldt, Marion Villenave, Schuyler G. Wolff, Marshall D. Perrin, Christophe Pinte, Ryo Tazaki, Deborah L. Padgett
Figure caption: Left: vertical cut across the disk from the optical to the mid-infrared, measured within 0.″25 of the symmetry axis. All curves are normalized to their peak and aligned based on the location of the brighter nebula, except for the 890 μm ALMA profile, which is aligned with the dark lane seen in the scattered light images. Right: Distance between the top and bottom nebulae, normalized to the 0.8 μm value for comparison purposes, as a function of wavelength for Tau 042021 (red stars) and other EODs (black symbols). Data for other systems are from Duchêne et al. (2010); McCabe et al. (2011), Cotera et al. (2001); Watson & Stapelfeldt (2004) for HK Tau B, HV Tau C, and HH 30, respectively.
Paper: JWST Imaging of Edge-on Protoplanetary Disks. I. Fully Vertically Mixed 10 μm Grains in the Outer Regions of a 1000 au Disk
Authors: Gaspard Duchêne, François Ménard, Karl R. Stapelfeldt, Marion Villenave, Schuyler G. Wolff, Marshall D. Perrin, Christophe Pinte, Ryo Tazaki, Deborah L. Padgett
Figure caption: SED of Tau 042021. Closed and open circles represent the adopted and additional photometric data points, respectively (see Appendix A). Red diamonds indicate the fluxes measured in the JWST images presented here. Small gray circles represent the Spitzer/IRS spectrum rebinned to a Δλ/λ  =  10% sampling. The observed scatter observed from the optical to the mid-infrared is most likely due to intrinsic variability and/or changes in disk illumination. The dashed blue and red segments are power-law fits to the UV and/or blue and (sub)millimeter parts of the SED, respectively.
Paper: JWST Imaging of Edge-on Protoplanetary Disks. I. Fully Vertically Mixed 10 μm Grains in the Outer Regions of a 1000 au Disk
Authors: Gaspard Duchêne, François Ménard, Karl R. Stapelfeldt, Marion Villenave, Schuyler G. Wolff, Marshall D. Perrin, Christophe Pinte, Ryo Tazaki, Deborah L. Padgett
Figure caption: HST–JWST 3-color composite image of Tau 042021; the full field of view spans 18″. The 0.8, 2, and 7.7 μm images are rendered (using a logarithmic stretch) in the blue, green, and red channels, respectively. The orange object to the right of the edge-on disk is a background galaxy.
Paper: JWST Imaging of Edge-on Protoplanetary Disks. I. Fully Vertically Mixed 10 μm Grains in the Outer Regions of a 1000 au Disk
Authors: Gaspard Duchêne, François Ménard, Karl R. Stapelfeldt, Marion Villenave, Schuyler G. Wolff, Marshall D. Perrin, Christophe Pinte, Ryo Tazaki, Deborah L. Padgett
Figure caption: Image gallery with the disk oriented horizontally. All images are shown on same angular scale and a log stretch for all panels except at 21 and 890 μm (for which square root and linear stretches are used, respectively). The corresponding beam is shown in the bottom left of each panel. A faint star is detected from 0.8 to 12.8 μm to the SW of the disk. The bright spike indicated by a ⊕ symbol in 0.6 μm image is an uncorrected bad pixel enhanced due to Fourier shifting of the image.
Paper: JWST Imaging of Edge-on Protoplanetary Disks. I. Fully Vertically Mixed 10 μm Grains in the Outer Regions of a 1000 au Disk
Authors: Gaspard Duchêne, François Ménard, Karl R. Stapelfeldt, Marion Villenave, Schuyler G. Wolff, Marshall D. Perrin, Christophe Pinte, Ryo Tazaki, Deborah L. Padgett
Figure caption: MIRI 7.7 μm images of Tau 042021 and a bright star in the same frame (left and right panels, respectively). Both images are shown in the native detector orientation and with a hard log stretch to highlight the X-shaped feature and the low-level structure of the PSF. Notice the smaller field of view of the right panel. To guide the eye, red dashed segments are drawn at 36° on either side of the disk midplane and replicated in the right panel.
Paper: JWST Imaging of Edge-on Protoplanetary Disks. I. Fully Vertically Mixed 10 μm Grains in the Outer Regions of a 1000 au Disk
Authors: Gaspard Duchêne, François Ménard, Karl R. Stapelfeldt, Marion Villenave, Schuyler G. Wolff, Marshall D. Perrin, Christophe Pinte, Ryo Tazaki, Deborah L. Padgett
Figure caption: Spitzer IRS spectrum of Tau 042021 with H2, H, and [Ne II] lines indicated by the solid blue, dotted red, and dashed orange segments, respectively.
Paper: JWST Imaging of Edge-on Protoplanetary Disks. I. Fully Vertically Mixed 10 μm Grains in the Outer Regions of a 1000 au Disk
Authors: Gaspard Duchêne, François Ménard, Karl R. Stapelfeldt, Marion Villenave, Schuyler G. Wolff, Marshall D. Perrin, Christophe Pinte, Ryo Tazaki, Deborah L. Padgett
Figure caption: HST and JWST images of Tau 042021 after application of a 1″ box median filter. The images are rendered with a hard logarithmic stretch to highlight the jet component of the system, leading to saturation in the scattered light disk and X-shaped feature areas.
Paper: JWST Imaging of Edge-on Protoplanetary Disks. I. Fully Vertically Mixed 10 μm Grains in the Outer Regions of a 1000 au Disk
Authors: Gaspard Duchêne, François Ménard, Karl R. Stapelfeldt, Marion Villenave, Schuyler G. Wolff, Marshall D. Perrin, Christophe Pinte, Ryo Tazaki, Deborah L. Padgett
Figure caption: Near- to far-infrared extinction law measured in molecular clouds (colored symbols) as well as function forms for the interstellar extinction from Weingartner & Draine (2001; labeled WD01 in the figure). The Case A and B curves are appropriate for the diffuse ISM and molecular clouds, respectively. Solid circles represent Case B extinction values for standard optical and near-infrared filters. The two sets of blue triangles represent the 1 ≤ A  K  < 2 and A  K  ≥ 2 results from Chapman et al. (2009); the latter corresponds to the lowest value of A 24/A  K . The dotted orange line indicates the opacity law of the pristine dust model that was constructed to match the adopted molecular cloud extinction law (represented by the solid symbols).
Paper: JWST Imaging of Edge-on Protoplanetary Disks. I. Fully Vertically Mixed 10 μm Grains in the Outer Regions of a 1000 au Disk
Authors: Gaspard Duchêne, François Ménard, Karl R. Stapelfeldt, Marion Villenave, Schuyler G. Wolff, Marshall D. Perrin, Christophe Pinte, Ryo Tazaki, Deborah L. Padgett
Figure caption: Extinction law of dust models used in this study. The black and gray symbols represent the extinction law observed in molecular clouds (see Appendix B).
Paper: JWST Imaging of Edge-on Protoplanetary Disks. I. Fully Vertically Mixed 10 μm Grains in the Outer Regions of a 1000 au Disk
Authors: Gaspard Duchêne, François Ménard, Karl R. Stapelfeldt, Marion Villenave, Schuyler G. Wolff, Marshall D. Perrin, Christophe Pinte, Ryo Tazaki, Deborah L. Padgett
Figure caption:  12CO channel map centered at V −V sys = −0.3 km s−1 (contours at 20% and 50% of the peak brightness) and using (u,v) tapering to a 0.″7 circular beam to improve sensitivity in the outer disk, superimposed over the MIRI F770W image, stretched to highlight the direction and extent of the X-shaped feature.
Paper: JWST Imaging of Edge-on Protoplanetary Disks. I. Fully Vertically Mixed 10 μm Grains in the Outer Regions of a 1000 au Disk
Authors: Gaspard Duchêne, François Ménard, Karl R. Stapelfeldt, Marion Villenave, Schuyler G. Wolff, Marshall D. Perrin, Christophe Pinte, Ryo Tazaki, Deborah L. Padgett
Figure caption:  12CO and 13CO position–velocity diagrams (top and bottom, respectively). The dotted, solid, and dashed curves correspond to dynamical masses of 0.25, 0.4, and 0.8 M ⊙, respectively. The lack of low-velocity 12CO emission is due to interferometric filtering of foreground and/or background cloud emission.
Paper: JWST Imaging of Edge-on Protoplanetary Disks. I. Fully Vertically Mixed 10 μm Grains in the Outer Regions of a 1000 au Disk
Authors: Gaspard Duchêne, François Ménard, Karl R. Stapelfeldt, Marion Villenave, Schuyler G. Wolff, Marshall D. Perrin, Christophe Pinte, Ryo Tazaki, Deborah L. Padgett
Figure caption: Left: dark lane thickness as a function of wavelength (left panel) for the models explored here (see Table 3). Right: Observed and model SED for the same models. The dip at 9 μm in the model SEDs is due to a strong albedo feature from the silicates adopted in the DIANA mixture. We stress that the models are constructed solely on the basis of matching the dark lane thickness at 2 μm; all other quantities are merely predicted based on having fit that quantity.
Paper: JWST Imaging of Edge-on Protoplanetary Disks. I. Fully Vertically Mixed 10 μm Grains in the Outer Regions of a 1000 au Disk
Authors: Gaspard Duchêne, François Ménard, Karl R. Stapelfeldt, Marion Villenave, Schuyler G. Wolff, Marshall D. Perrin, Christophe Pinte, Ryo Tazaki, Deborah L. Padgett
Figure caption: MIRI 7.7 μm and NIRCam 4.4 μm images of Tau 042021, with moment zero 12CO contours overplotted in the left panel. Black and green segments indicate the arms of the X-shaped feature and the disk surface orientation as seen in the F770W, respectively, and are reproduced identically in both panels as a visual guide.
Paper: JWST Imaging of Edge-on Protoplanetary Disks. I. Fully Vertically Mixed 10 μm Grains in the Outer Regions of a 1000 au Disk
Authors: Gaspard Duchêne, François Ménard, Karl R. Stapelfeldt, Marion Villenave, Schuyler G. Wolff, Marshall D. Perrin, Christophe Pinte, Ryo Tazaki, Deborah L. Padgett
Figure caption: Moment 0 and 1 maps of the 12CO emission from Tau 042021 (top and bottom, respectively). A 3σ clipping was applied in each data cube prior to computing the moment maps.
Paper: JWST Imaging of Edge-on Protoplanetary Disks. I. Fully Vertically Mixed 10 μm Grains in the Outer Regions of a 1000 au Disk
Authors: Gaspard Duchêne, François Ménard, Karl R. Stapelfeldt, Marion Villenave, Schuyler G. Wolff, Marshall D. Perrin, Christophe Pinte, Ryo Tazaki, Deborah L. Padgett
Figure caption: Model and observed images for various dust grain size distribution and disk structure models. Corresponding parameters are summarized in Table 3. All images are shown on a square root stretch except the last column (linear stretch) from 0 to the peak value.
Paper: Librating Kozai–Lidov Cycles with a Precessing Quadrupole Potential Are Analytically Approximately Solved
Authors: Ygal Y. Klein, Boaz Katz
Figure caption: Results for librating KLCs are shown for a case of α = 1° and β = 2.4. Top panels: amplitude of the change in j  z  vs. initial C  K . Middle panels: ﹩{j}_{z}^{\max }﹩ vs. initial C  K . Bottom panels: ﹩{j}_{z}^{\min }﹩ vs. initial C  K . Left column: numerical results. Right column: analytic prediction. The color-coding in all panels is by the nature of the pair ﹩\left(V,E\right)﹩ as defined in Section 3.4: red—Class 1 (no ﹩{V}_{\max }﹩); blue—Class 2 (﹩E\gt {V}_{\max }﹩); magenta—Class 3 (﹩E\lt {V}_{\max }﹩ and ﹩\delta \lt {\delta }_{{V}_{\max }}﹩); cyan—Class 4 (﹩E\lt {V}_{\max }﹩ and ﹩\delta \gt {\delta }_{{V}_{\max }}﹩). The top left panel is identical to the middle left panel of Figure 3.
Paper: Korg: Fitting, Model Atmosphere Interpolation, and Brackett Lines
Authors: Adam J. Wheeler, Andrew R. Casey, Matthew W. Abruzzo
Figure caption: The temperature at selected upper layers in interpolated (using the resampled cubic method) model atmospheres (10−4  ≲  τ 5000  ≲  10−1) in exact (black) and interpolated (dashed red) model atmospheres. The interpolated atmospheres are always interpolated in all five stellar parameters. Each panel shows how the values change as one of the parameters varied and the others stay fixed. The fixed values (T eff  =  3800 K,  ﹩\mathrm{log}\,g\,=\,0.0﹩, solar abundances) are marked with vertical lines. In the last panel, the blue line indicates the number density of CO at the top of the model atmosphere, computed using the uninterpolated atmospheres only. Sharp changes in temperature as a function of stellar parameters driven by molecular formation make model atmosphere interpolation very challenging for cool giants.
Paper: Korg: Fitting, Model Atmosphere Interpolation, and Brackett Lines
Authors: Adam J. Wheeler, Andrew R. Casey, Matthew W. Abruzzo
Figure caption: Estimated error introduced by interpolation as a function of T eff and  ﹩\mathrm{log}\,g﹩ for solar abundances. The color of each point shows the largest flux deviation at any wavelength for spectra synthesized with the APOGEE DR 17 linelist (Abdurro’uf et al. 2022) and convolved to R  =  22, 500 (the approximate APOGEE resolving power). We note, however, that this plot is not sensitive to wavelength range, linelist, or R. For reference, the distribution of stars in APOGEE DR17 is plotted in the background. The colorbar has been truncated for clarity; errors are smaller than 10−6 for some stellar parameters.
Paper: Korg: Fitting, Model Atmosphere Interpolation, and Brackett Lines
Authors: Adam J. Wheeler, Andrew R. Casey, Matthew W. Abruzzo
Figure caption: Differential [Fe/H] abundances of 18 Sco (relative to the Sun) computed by Korg with equivalent widths and stellar parameters from Meléndez et al. (2014). The mean abundance is the same found by Meléndez et al. (2014), and the scatter in line abundances from Korg is nearly half that of Meléndez et al. (2014; 0.0056 dex compared to 0.010 dex).
Paper: Korg: Fitting, Model Atmosphere Interpolation, and Brackett Lines
Authors: Adam J. Wheeler, Andrew R. Casey, Matthew W. Abruzzo
Figure caption: Estimated error introduced by interpolation using the method tailored for cool dwarfs, described in text. Changes which improved interpolation for cool dwarfs make it worse for cool giants. (Compare the main sequence and red-giant branch to those in Figure 3).
Paper: Korg: Fitting, Model Atmosphere Interpolation, and Brackett Lines
Authors: Adam J. Wheeler, Andrew R. Casey, Matthew W. Abruzzo
Figure caption: The line-to-line scatter in the abundance of each element measured using equivalent widths from Meléndez et al. (2014). Comparison between  Korg  reanalysis and original abundances. Computing abundances with  Korg  results in significantly smaller scatter for most elements.
Paper: Using AI for Wave-front Estimation with the Rubin Observatory Active Optics System
Authors: John Franklin Crenshaw, Andrew J. Connolly, Joshua E. Meyers, J. Bryce Kalmbach, Guillem Megias Homar, Tiago Ribeiro, Krzysztof Suberlak, Sandrine Thomas, Te-Wei Tsai
Figure caption: Distribution of errors for each Zernike coefficient α  i . The stars denote the median error.
Paper: Deconvolution of JWST/MIRI Images: Applications to an Active Galactic Nucleus Model and GATOS Observations of NGC 5728
Authors: M. T. Leist, C. Packham, D. J. V. Rosario, D. A. Hope, A. Alonso-Herrero, E. K. S. Hicks, S. Hönig, L. Zhang, R. Davies, T. Díaz-Santos, O. González-Martín, E. Bellocchi, P. G. Boorman, F. Combes, I. García-Bernete, S. García-Burillo, B. García-Lorenzo, H. Haidar, K. Ichikawa, M. Imanishi, S. M. Jefferies, Á. Labiano, N. A. Levenson, R. Nikutta, M. Pereira-Santaella, C. Ramos Almeida, C. Ricci, D. Rigopoulou, W. Schaefer, M. Stalevski, M. J. Ward, L. Fuller, T. Izumi, D. Rouan, T. Shimizu
Figure caption: Five color JWST/MIRIM (left) and Kraken deconvolved images (right). Each image is ∼20″ × 20″, oriented N–E, and log scaled. Note the ∼2.″5 SE to NW extended nuclear emission visible in the deconvolved image. Evidence of the Airy ring remnant (∼1″ NW of the nucleus) and the F560W crosshair are also clearly visible in the deconvolved image.
Paper: Deconvolution of JWST/MIRI Images: Applications to an Active Galactic Nucleus Model and GATOS Observations of NGC 5728
Authors: M. T. Leist, C. Packham, D. J. V. Rosario, D. A. Hope, A. Alonso-Herrero, E. K. S. Hicks, S. Hönig, L. Zhang, R. Davies, T. Díaz-Santos, O. González-Martín, E. Bellocchi, P. G. Boorman, F. Combes, I. García-Bernete, S. García-Burillo, B. García-Lorenzo, H. Haidar, K. Ichikawa, M. Imanishi, S. M. Jefferies, Á. Labiano, N. A. Levenson, R. Nikutta, M. Pereira-Santaella, C. Ramos Almeida, C. Ricci, D. Rigopoulou, W. Schaefer, M. Stalevski, M. J. Ward, L. Fuller, T. Izumi, D. Rouan, T. Shimizu
Figure caption: Left: FWHM of the nuclear source of NGC 5728 as a function of observed central wavelength. The dotted line shows the JWST/MIRIM PSF FWHM at the center of the respective filter, and the length of the dotted line represents the filter width. Right: comparative log-scaled aperture flux measurements of the central 4.″1 between the JWST/MIRIM and Kraken deconvolved images.
Paper: Deconvolution of JWST/MIRI Images: Applications to an Active Galactic Nucleus Model and GATOS Observations of NGC 5728
Authors: M. T. Leist, C. Packham, D. J. V. Rosario, D. A. Hope, A. Alonso-Herrero, E. K. S. Hicks, S. Hönig, L. Zhang, R. Davies, T. Díaz-Santos, O. González-Martín, E. Bellocchi, P. G. Boorman, F. Combes, I. García-Bernete, S. García-Burillo, B. García-Lorenzo, H. Haidar, K. Ichikawa, M. Imanishi, S. M. Jefferies, Á. Labiano, N. A. Levenson, R. Nikutta, M. Pereira-Santaella, C. Ramos Almeida, C. Ricci, D. Rigopoulou, W. Schaefer, M. Stalevski, M. J. Ward, L. Fuller, T. Izumi, D. Rouan, T. Shimizu
Figure caption: Kraken deconvolution imaging results for D AGN (top row), D  V3 (middle row), and D  V4 (bottom row). Each image is displayed log scaled, scaled to the F2100W for each row, and shows the central 150 × 150 MIRIM pixels. The number of iterations for each column of images is displayed as an inset in the D AGN images.
Paper: Deconvolution of JWST/MIRI Images: Applications to an Active Galactic Nucleus Model and GATOS Observations of NGC 5728
Authors: M. T. Leist, C. Packham, D. J. V. Rosario, D. A. Hope, A. Alonso-Herrero, E. K. S. Hicks, S. Hönig, L. Zhang, R. Davies, T. Díaz-Santos, O. González-Martín, E. Bellocchi, P. G. Boorman, F. Combes, I. García-Bernete, S. García-Burillo, B. García-Lorenzo, H. Haidar, K. Ichikawa, M. Imanishi, S. M. Jefferies, Á. Labiano, N. A. Levenson, R. Nikutta, M. Pereira-Santaella, C. Ramos Almeida, C. Ricci, D. Rigopoulou, W. Schaefer, M. Stalevski, M. J. Ward, L. Fuller, T. Izumi, D. Rouan, T. Shimizu
Figure caption: Same as Figure 6 for the Kraken deconvolved images of NGC 5728, except the FWHM is expressed in arcseconds. Aperture flux measurements were normalized to the JWST/MIRIM image in the same wave band.
Paper: Deconvolution of JWST/MIRI Images: Applications to an Active Galactic Nucleus Model and GATOS Observations of NGC 5728
Authors: M. T. Leist, C. Packham, D. J. V. Rosario, D. A. Hope, A. Alonso-Herrero, E. K. S. Hicks, S. Hönig, L. Zhang, R. Davies, T. Díaz-Santos, O. González-Martín, E. Bellocchi, P. G. Boorman, F. Combes, I. García-Bernete, S. García-Burillo, B. García-Lorenzo, H. Haidar, K. Ichikawa, M. Imanishi, S. M. Jefferies, Á. Labiano, N. A. Levenson, R. Nikutta, M. Pereira-Santaella, C. Ramos Almeida, C. Ricci, D. Rigopoulou, W. Schaefer, M. Stalevski, M. J. Ward, L. Fuller, T. Izumi, D. Rouan, T. Shimizu
Figure caption: Same as Figure B1 but showing MS V2 (top row), K  V2 (middle row), and RL V2 (bottom row).
Paper: Deconvolution of JWST/MIRI Images: Applications to an Active Galactic Nucleus Model and GATOS Observations of NGC 5728
Authors: M. T. Leist, C. Packham, D. J. V. Rosario, D. A. Hope, A. Alonso-Herrero, E. K. S. Hicks, S. Hönig, L. Zhang, R. Davies, T. Díaz-Santos, O. González-Martín, E. Bellocchi, P. G. Boorman, F. Combes, I. García-Bernete, S. García-Burillo, B. García-Lorenzo, H. Haidar, K. Ichikawa, M. Imanishi, S. M. Jefferies, Á. Labiano, N. A. Levenson, R. Nikutta, M. Pereira-Santaella, C. Ramos Almeida, C. Ricci, D. Rigopoulou, W. Schaefer, M. Stalevski, M. J. Ward, L. Fuller, T. Izumi, D. Rouan, T. Shimizu
Figure caption: Image grid comparison between MS V1 (top row), K  V1 (middle row), and RL V1 (bottom row). Each image is displayed log scaled, scaled to the K  V1 F2100W filter, and shows the central 150 × 150 MIRIM pixels.