adsabs/AstroCLIMB huggingface dataset:
Paper: Utilizing Maximum Variability to Discern TDE Emission from AGN Flares
Authors: Samaresh Mondal, K. Decker French
Figure caption: Top panel: AGN flare rate (number of flares per unit observation time per galaxy) with flare strength above the MaxVar of TDEs as a function of Δt. The rates were obtained by counting the number of flares that have Var above the MaxVar of TDEs in the simulation of Swift-XRT AGN light curves. Bottom panel: AGN flare rate as a function of time with flare strength above various constant thresholds, which indicates if a transient has a Var of >0.8, >1.0, and >1.2 on a timescale of <30, <200, and <300 days, then it is highly unlikely from an AGN. The red horizontal dashed line indicates the current TDE rate from the optically selected sample. The opposite trend in the two panels is due to the fact that the Var threshold increases with Δt in the top panel, whereas in the bottom panel, the Var thresholds are constant.
Paper: Signatures of Black Hole Seeding on the M•–σ Relation: Predictions from the BRAHMA Simulations
Authors: Jonathan Kho, Aklant Kumar Bhowmick, Paul Torrey, Alex M. Garcia, Niusha Ahvazi, Laura Blecha, Mark Vogelsberger
Figure caption: Redshift evolution of the median BH mass for the four BRAHMA simulations at fixed σ values. All lines have been normalized to the median BH mass at z = 5 to emphasize the different evolutions. Error bars represent 95% confidence intervals about the median mass calculated via bootstrapping of the data. We clearly see here a negative redshift evolution for the more lenient seed models at σ = 101.5 km s−1, very minimal redshift evolution for all seed models at σ = 101.75 km s−1, and a stronger positive redshift evolution for more restrictive seed models at σ = 102 km s−1. At σ = 102 km s−1, for the more restrictive seed models, the increase in median BH mass occurs almost entirely at z < 2.
Paper: Signatures of Black Hole Seeding on the M•–σ Relation: Predictions from the BRAHMA Simulations
Authors: Jonathan Kho, Aklant Kumar Bhowmick, Paul Torrey, Alex M. Garcia, Niusha Ahvazi, Laura Blecha, Mark Vogelsberger
Figure caption: The evolution of the different components that determine the redshift evolution of the M•–σ relation, as identified in Equation (2). Error bars in each panel represent 95% confidence intervals about the derivative being shown, obtained via bootstrapping of the data.
Paper: Signatures of Black Hole Seeding on the M•–σ Relation: Predictions from the BRAHMA Simulations
Authors: Jonathan Kho, Aklant Kumar Bhowmick, Paul Torrey, Alex M. Garcia, Niusha Ahvazi, Laura Blecha, Mark Vogelsberger
Figure caption: Histograms of the full scatter of BHs for the most lenient and most restrictive seed models on the M•–σ relation. Plotted in blue and red is the median trend of the data, with error bars representing the IQR in BH mass. The dotted line shows the observed M•–σ by KH13. While the relation retains a tight correlation for the most lenient model across redshift, the scatter drastically increases with decreasing redshift for the most strict model at intermediate values of σ.
Paper: Signatures of Black Hole Seeding on the M•–σ Relation: Predictions from the BRAHMA Simulations
Authors: Jonathan Kho, Aklant Kumar Bhowmick, Paul Torrey, Alex M. Garcia, Niusha Ahvazi, Laura Blecha, Mark Vogelsberger
Figure caption: BH number density in comoving Mpc−3 for each of the four BRAHMA simulations as a function of redshift. With each incrementally more restrictive seed model, the number density of BHs decreases at all redshifts, and halos start to be seeded at later times. The onset of seeding and the number density of BHs in TNG are greatly reduced due to its extremely restrictive halo mass requirement. Since the more restrictive seed models have much fewer BH seeds, their growth via mergers is significantly reduced.
Paper: Utilizing Maximum Variability to Discern TDE Emission from AGN Flares
Authors: Samaresh Mondal, K. Decker French
Figure caption: The comparison of MaxVar obtained from simulated AGN light curves with eROSITA TDE candidates.
Paper: BASS. LIV. Physical Properties of AGN-hosting Galaxy Mergers from Multiwavelength SED Fitting
Authors: Marco Troncoso, Ezequiel Treister, Alejandra Rojas, Médéric Boquien, Franz Bauer, Michael J. Koss, Roberto J. Assef, Miguel Parra Tello, Ignacio del Moral-Castro, Claudio Ricci, Sophia Dai, Kyuseok Oh, Federica Ricci, Alessandro Peca, C. Megan Urry, Kriti Kamal Gupta, Giacomo Venturi, Matilde Signorini, Richard Mushotzky, David Sanders
Figure caption: Schematic visualization of the custom-made code developed for flux measurements. The first panel shows the stacked image downloaded from the relevant survey (in this case, as an example, we show the source BAT ID 305 in the DES-r band). The second step removes the surrounding sources, replacing their pixels with random values obtained from the background. In the third step, if a foreground star lies along the line of sight, it is removed by extrapolating the galaxy’s brightness profile across the region occupied by the star. If no foreground star is present, this step is skipped. In the fourth panel, we convolve the image to reduce its resolution to match the resolution of the WISE W4 band, which has the lowest. Finally, multiple apertures are applied to determine the optimal one for consistent measurements across all available bands (blue ellipses with “a” and “b” the ellipse axes). A circular annulus is also used to estimate the local background (red circles). The optimal aperture is selected as the smallest that fully encompasses the entire galaxy, guided by the flux–aperture plot. In this example, the chosen aperture is indicated by a red rectangle and the solid red line in the flux–aperture plot.
Paper: BASS. LIV. Physical Properties of AGN-hosting Galaxy Mergers from Multiwavelength SED Fitting
Authors: Marco Troncoso, Ezequiel Treister, Alejandra Rojas, Médéric Boquien, Franz Bauer, Michael J. Koss, Roberto J. Assef, Miguel Parra Tello, Ignacio del Moral-Castro, Claudio Ricci, Sophia Dai, Kyuseok Oh, Federica Ricci, Alessandro Peca, C. Megan Urry, Kriti Kamal Gupta, Giacomo Venturi, Matilde Signorini, Richard Mushotzky, David Sanders
Figure caption: From left to right: N—nonmerging/isolated galaxies; A—pre-stage merger; B—early-stage merger; C—mid-stage merger; D—late-stage merger.
Paper: Spectrotemporal Analysis of X-Ray Reverberation in the Seyfert 1.5 Galaxy 4U 1344–60
Authors: Adam G. Gonzalez, Luigi C. Gallo, Adam Ingram, Yerong Xu, Margaret Z. Buhariwalla
Figure caption: Posterior distributions from the nautilus run on the spectral model in Table 2. Panels along the diagonal display the one-dimensional posterior distribution of each parameter. Panels below the diagonal display the two-dimensional posterior distributions for each parameter pair, with contours representing the two-dimensional 39.3%, 68.3%, 95.5%, and 99.7% levels. Posterior modes are shown as the black points and lines in each panel.
Paper: BASS. LIV. Physical Properties of AGN-hosting Galaxy Mergers from Multiwavelength SED Fitting
Authors: Marco Troncoso, Ezequiel Treister, Alejandra Rojas, Médéric Boquien, Franz Bauer, Michael J. Koss, Roberto J. Assef, Miguel Parra Tello, Ignacio del Moral-Castro, Claudio Ricci, Sophia Dai, Kyuseok Oh, Federica Ricci, Alessandro Peca, C. Megan Urry, Kriti Kamal Gupta, Giacomo Venturi, Matilde Signorini, Richard Mushotzky, David Sanders
Figure caption: Reduced χ2 distribution for the fits performed by CIGALE. The red line represents the theoretical χ2 function for our degrees of freedom, demonstrating that our results are consistent with expectations. Furthermore, 87% of our fits have χ2 < 3 values.
Paper: BASS. LIV. Physical Properties of AGN-hosting Galaxy Mergers from Multiwavelength SED Fitting
Authors: Marco Troncoso, Ezequiel Treister, Alejandra Rojas, Médéric Boquien, Franz Bauer, Michael J. Koss, Roberto J. Assef, Miguel Parra Tello, Ignacio del Moral-Castro, Claudio Ricci, Sophia Dai, Kyuseok Oh, Federica Ricci, Alessandro Peca, C. Megan Urry, Kriti Kamal Gupta, Giacomo Venturi, Matilde Signorini, Richard Mushotzky, David Sanders
Figure caption: Distribution of projected nuclear separation in kpc, for the 64 galaxies involved in merging systems in our sample; 35/64 galaxies are late-stage mergers (D12 < 10 kpc).
Paper: Spectrotemporal Analysis of X-Ray Reverberation in the Seyfert 1.5 Galaxy 4U 1344–60
Authors: Adam G. Gonzalez, Luigi C. Gallo, Adam Ingram, Yerong Xu, Margaret Z. Buhariwalla
Figure caption: Same as Figure 6 but for the radial profile in ξ and ne with the free h and ﹩1/{ \mathcal B }﹩ model in Table 3.
Paper: BASS. LIV. Physical Properties of AGN-hosting Galaxy Mergers from Multiwavelength SED Fitting
Authors: Marco Troncoso, Ezequiel Treister, Alejandra Rojas, Médéric Boquien, Franz Bauer, Michael J. Koss, Roberto J. Assef, Miguel Parra Tello, Ignacio del Moral-Castro, Claudio Ricci, Sophia Dai, Kyuseok Oh, Federica Ricci, Alessandro Peca, C. Megan Urry, Kriti Kamal Gupta, Giacomo Venturi, Matilde Signorini, Richard Mushotzky, David Sanders
Figure caption: SFR as a function of stellar mass. The blue and red contour maps correspond to the inactive population from xCOLD GASS (A. Saintonge et al. 2017) and the active population from M. J. Koss et al. (2021), respectively. The dashed blue line marks the local star-forming MS relation from D. Elbaz et al. (2007), with the background shaded blue region representing a ±0.3 dex width scatter. Additionally, the other background shaded colors highlight different regions of the diagram: salmon for quenched galaxies, green for the green valley, and the upper yellow region for starburst galaxies. The points denote the single AGN iM, while the triangles represent the confirmed dual AGN. Both populations are colored by their projected separation. Moreover, red stars represent galaxies where only one nucleus is visible.
Paper: BASS. LIV. Physical Properties of AGN-hosting Galaxy Mergers from Multiwavelength SED Fitting
Authors: Marco Troncoso, Ezequiel Treister, Alejandra Rojas, Médéric Boquien, Franz Bauer, Michael J. Koss, Roberto J. Assef, Miguel Parra Tello, Ignacio del Moral-Castro, Claudio Ricci, Sophia Dai, Kyuseok Oh, Federica Ricci, Alessandro Peca, C. Megan Urry, Kriti Kamal Gupta, Giacomo Venturi, Matilde Signorini, Richard Mushotzky, David Sanders
Figure caption: Confusion matrix of Spearman correlation values for pairs of physical parameters. Blue squares indicate a negative (anticorrelated) relationship, while red squares indicate a positive (correlated) relationship between the parameters.
Paper: BASS. LIV. Physical Properties of AGN-hosting Galaxy Mergers from Multiwavelength SED Fitting
Authors: Marco Troncoso, Ezequiel Treister, Alejandra Rojas, Médéric Boquien, Franz Bauer, Michael J. Koss, Roberto J. Assef, Miguel Parra Tello, Ignacio del Moral-Castro, Claudio Ricci, Sophia Dai, Kyuseok Oh, Federica Ricci, Alessandro Peca, C. Megan Urry, Kriti Kamal Gupta, Giacomo Venturi, Matilde Signorini, Richard Mushotzky, David Sanders
Figure caption: Projected separation as a function of the merger stage (left panel), along with the cumulative distribution function (CDF) for each stage (right panel). Nonmerging sources (N) are assigned a projected separation of 0. In the left panel, each rectangle represents the interquartile range, spanning from the first quartile (Q1) to the third quartile (Q3), while the whiskers extend to the minimum (Q0) and maximum (Q4) values within the range. The red line within each box indicates the median (Q2) of the distribution.
Paper: BASS. LIV. Physical Properties of AGN-hosting Galaxy Mergers from Multiwavelength SED Fitting
Authors: Marco Troncoso, Ezequiel Treister, Alejandra Rojas, Médéric Boquien, Franz Bauer, Michael J. Koss, Roberto J. Assef, Miguel Parra Tello, Ignacio del Moral-Castro, Claudio Ricci, Sophia Dai, Kyuseok Oh, Federica Ricci, Alessandro Peca, C. Megan Urry, Kriti Kamal Gupta, Giacomo Venturi, Matilde Signorini, Richard Mushotzky, David Sanders
Figure caption: AGN intrinsic luminosity as a function of the SFR. Left panel: red and blue points denote major and minor galaxy mergers, respectively. Right panel: the red line corresponds to the best linear fit for the dual AGN population. Squares represent the mean value of SFR in bins of nine sources. The symbols and colors of the points are the same as in Figure 11. In both panels, the red contours represent the distribution of the sources in the BASS sample.
Paper: BASS. LIV. Physical Properties of AGN-hosting Galaxy Mergers from Multiwavelength SED Fitting
Authors: Marco Troncoso, Ezequiel Treister, Alejandra Rojas, Médéric Boquien, Franz Bauer, Michael J. Koss, Roberto J. Assef, Miguel Parra Tello, Ignacio del Moral-Castro, Claudio Ricci, Sophia Dai, Kyuseok Oh, Federica Ricci, Alessandro Peca, C. Megan Urry, Kriti Kamal Gupta, Giacomo Venturi, Matilde Signorini, Richard Mushotzky, David Sanders
Figure caption: Left panel: SFR as a function of the projected nuclear separation. Right panel: observed total AGN luminosity as a function of nuclear separation. Both figures are colored by the fraction of AGN luminosity in the IR band. Squares represent the mean value of SFR/LAGN in bins of nine sources.
Paper: BASS. LIV. Physical Properties of AGN-hosting Galaxy Mergers from Multiwavelength SED Fitting
Authors: Marco Troncoso, Ezequiel Treister, Alejandra Rojas, Médéric Boquien, Franz Bauer, Michael J. Koss, Roberto J. Assef, Miguel Parra Tello, Ignacio del Moral-Castro, Claudio Ricci, Sophia Dai, Kyuseok Oh, Federica Ricci, Alessandro Peca, C. Megan Urry, Kriti Kamal Gupta, Giacomo Venturi, Matilde Signorini, Richard Mushotzky, David Sanders
Figure caption: Left panel: SFR as a function of the merger stage. Right panel: specific SFR as a function of the merger stage, along with the cumulative distribution function (CDF) for each stage. Symbols are the same as those defined in Figure 10.
Paper: BASS. LIV. Physical Properties of AGN-hosting Galaxy Mergers from Multiwavelength SED Fitting
Authors: Marco Troncoso, Ezequiel Treister, Alejandra Rojas, Médéric Boquien, Franz Bauer, Michael J. Koss, Roberto J. Assef, Miguel Parra Tello, Ignacio del Moral-Castro, Claudio Ricci, Sophia Dai, Kyuseok Oh, Federica Ricci, Alessandro Peca, C. Megan Urry, Kriti Kamal Gupta, Giacomo Venturi, Matilde Signorini, Richard Mushotzky, David Sanders
Figure caption: Confusion matrix of Spearman correlation values for pairs of physical parameters, considering only systems classified as major galaxy mergers. Colors are the same as in Figure 7.
Paper: BASS. LIV. Physical Properties of AGN-hosting Galaxy Mergers from Multiwavelength SED Fitting
Authors: Marco Troncoso, Ezequiel Treister, Alejandra Rojas, Médéric Boquien, Franz Bauer, Michael J. Koss, Roberto J. Assef, Miguel Parra Tello, Ignacio del Moral-Castro, Claudio Ricci, Sophia Dai, Kyuseok Oh, Federica Ricci, Alessandro Peca, C. Megan Urry, Kriti Kamal Gupta, Giacomo Venturi, Matilde Signorini, Richard Mushotzky, David Sanders
Figure caption: SFR as a function of the fraction of the AGN luminosity in the IR band. Squares represent the mean value of SFR in bins of nine sources. The symbols and colors of the points are the same as in Figure 11.
Paper: The JWST Early Release Science Program for Direct Observations of Exoplanetary Systems. VI. Evidence for Radially Evolving Icy Grains in the HD 141569A Disk via NIRCam Coronagraphic Imaging
Authors: Maxwell A. Millar-Blanchaer, Élodie Choquet, Kellen Lawson, Sebastián Marino, Jens Kammerer, Aarynn L. Carter, Isabel Rebollido, Jarron M. Leisenring, Minjae Kim, Paul Kalas, Karl R Stapelfeldt, Sasha Hinkley, Mark Booth, Carol A. Grady, Elisabeth C. Matthews, Beth A. Biller, Andrew Skemer, Julien H. Girard, Schuyler G. Wolff, Kimberly Ward-Duong, Michael R. Meyer, Anthony Boccaletti, Eric Pantin, Brenda C. Matthews, Stanimir Metchev, Marshall D. Perrin, Christine H. Chen, Katie Crotts, Olivier Absil, William O. Balmer, Per Calissendorff, Gabriele Cugno, Thayne Currie, Camilla Danielski, Kielan K. W. Hoch, Markus Janson, Elena Manjavacas, Pierre-Olivier Lagage, Ben J. Sutlieff, Shrishmoy Ray, Bin B. Ren, Emily Rickman, Genaro Suárez, Christopher A. Theissen, Taichi Uyama, Andreas Quirrenbach, Jason J. Wang, Niall Whiteford, Mark C. Wyatt, Alice Zurlo
Figure caption: Left panel: the normalized surface brightness as a function of deprojected stellocentric distance for the data and the models. The vertical gray dashed lines show the locations of the A, B, and C rings identified by M. Konishi et al. (2016), and the vertical red dashed line shows the radial separation at which the coronagraph throughput reaches 50%. Right panel: the scattering efficiency ratio between the F300M and F360M images as a function of deprojected stellocentric distance. The vertical dashed lines represent the same values as in the left plot. The MCMC samples in both plots, which are fit to the noisy data, closely follow the data (orange) and demonstrate that the increasing trend seen in the data as a function of radial distance is detected with high significance.
Paper: The JWST Early Release Science Program for Direct Observations of Exoplanetary Systems. VI. Evidence for Radially Evolving Icy Grains in the HD 141569A Disk via NIRCam Coronagraphic Imaging
Authors: Maxwell A. Millar-Blanchaer, Élodie Choquet, Kellen Lawson, Sebastián Marino, Jens Kammerer, Aarynn L. Carter, Isabel Rebollido, Jarron M. Leisenring, Minjae Kim, Paul Kalas, Karl R Stapelfeldt, Sasha Hinkley, Mark Booth, Carol A. Grady, Elisabeth C. Matthews, Beth A. Biller, Andrew Skemer, Julien H. Girard, Schuyler G. Wolff, Kimberly Ward-Duong, Michael R. Meyer, Anthony Boccaletti, Eric Pantin, Brenda C. Matthews, Stanimir Metchev, Marshall D. Perrin, Christine H. Chen, Katie Crotts, Olivier Absil, William O. Balmer, Per Calissendorff, Gabriele Cugno, Thayne Currie, Camilla Danielski, Kielan K. W. Hoch, Markus Janson, Elena Manjavacas, Pierre-Olivier Lagage, Ben J. Sutlieff, Shrishmoy Ray, Bin B. Ren, Emily Rickman, Genaro Suárez, Christopher A. Theissen, Taichi Uyama, Andreas Quirrenbach, Jason J. Wang, Niall Whiteford, Mark C. Wyatt, Alice Zurlo
Figure caption: Expected surface brightness ratio between F300M and F360M as a function of the minimum grain size and the water ice fraction in grains (by mass). The top panel presents a case of compact grains (0% porosity), while the bottom panel presents a porous case (50% porosity). The white and black contours represent a brightness ratio of 0.4 and 0.8 as found at 100 and 400 au, respectively. The orange dashed line represents the expected minimum grain size as a function of the ice fraction.
Paper: The JWST Early Release Science Program for Direct Observations of Exoplanetary Systems. VI. Evidence for Radially Evolving Icy Grains in the HD 141569A Disk via NIRCam Coronagraphic Imaging
Authors: Maxwell A. Millar-Blanchaer, Élodie Choquet, Kellen Lawson, Sebastián Marino, Jens Kammerer, Aarynn L. Carter, Isabel Rebollido, Jarron M. Leisenring, Minjae Kim, Paul Kalas, Karl R Stapelfeldt, Sasha Hinkley, Mark Booth, Carol A. Grady, Elisabeth C. Matthews, Beth A. Biller, Andrew Skemer, Julien H. Girard, Schuyler G. Wolff, Kimberly Ward-Duong, Michael R. Meyer, Anthony Boccaletti, Eric Pantin, Brenda C. Matthews, Stanimir Metchev, Marshall D. Perrin, Christine H. Chen, Katie Crotts, Olivier Absil, William O. Balmer, Per Calissendorff, Gabriele Cugno, Thayne Currie, Camilla Danielski, Kielan K. W. Hoch, Markus Janson, Elena Manjavacas, Pierre-Olivier Lagage, Ben J. Sutlieff, Shrishmoy Ray, Bin B. Ren, Emily Rickman, Genaro Suárez, Christopher A. Theissen, Taichi Uyama, Andreas Quirrenbach, Jason J. Wang, Niall Whiteford, Mark C. Wyatt, Alice Zurlo
Figure caption: Left column: roll-combined images of the F300M and F360M data after PSF subtraction. Center column: roll-combined images of the models convolved with the NIRCam off-axis PSF. Right column: the data minus the model.
Paper: The JWST Early Release Science Program for Direct Observations of Exoplanetary Systems. VI. Evidence for Radially Evolving Icy Grains in the HD 141569A Disk via NIRCam Coronagraphic Imaging
Authors: Maxwell A. Millar-Blanchaer, Élodie Choquet, Kellen Lawson, Sebastián Marino, Jens Kammerer, Aarynn L. Carter, Isabel Rebollido, Jarron M. Leisenring, Minjae Kim, Paul Kalas, Karl R Stapelfeldt, Sasha Hinkley, Mark Booth, Carol A. Grady, Elisabeth C. Matthews, Beth A. Biller, Andrew Skemer, Julien H. Girard, Schuyler G. Wolff, Kimberly Ward-Duong, Michael R. Meyer, Anthony Boccaletti, Eric Pantin, Brenda C. Matthews, Stanimir Metchev, Marshall D. Perrin, Christine H. Chen, Katie Crotts, Olivier Absil, William O. Balmer, Per Calissendorff, Gabriele Cugno, Thayne Currie, Camilla Danielski, Kielan K. W. Hoch, Markus Janson, Elena Manjavacas, Pierre-Olivier Lagage, Ben J. Sutlieff, Shrishmoy Ray, Bin B. Ren, Emily Rickman, Genaro Suárez, Christopher A. Theissen, Taichi Uyama, Andreas Quirrenbach, Jason J. Wang, Niall Whiteford, Mark C. Wyatt, Alice Zurlo
Figure caption: Comparison of disk structures between archival HST/STIS optical coronagraphic data (left panel) and the JWST/NIRCAM F300M observations (right panel). A key difference in the morphologies is that the JWST data do not show a well-defined deep gap between the A and B ring components. North is up, and east is left.
Paper: The JWST Early Release Science Program for Direct Observations of Exoplanetary Systems. VI. Evidence for Radially Evolving Icy Grains in the HD 141569A Disk via NIRCam Coronagraphic Imaging
Authors: Maxwell A. Millar-Blanchaer, Élodie Choquet, Kellen Lawson, Sebastián Marino, Jens Kammerer, Aarynn L. Carter, Isabel Rebollido, Jarron M. Leisenring, Minjae Kim, Paul Kalas, Karl R Stapelfeldt, Sasha Hinkley, Mark Booth, Carol A. Grady, Elisabeth C. Matthews, Beth A. Biller, Andrew Skemer, Julien H. Girard, Schuyler G. Wolff, Kimberly Ward-Duong, Michael R. Meyer, Anthony Boccaletti, Eric Pantin, Brenda C. Matthews, Stanimir Metchev, Marshall D. Perrin, Christine H. Chen, Katie Crotts, Olivier Absil, William O. Balmer, Per Calissendorff, Gabriele Cugno, Thayne Currie, Camilla Danielski, Kielan K. W. Hoch, Markus Janson, Elena Manjavacas, Pierre-Olivier Lagage, Ben J. Sutlieff, Shrishmoy Ray, Bin B. Ren, Emily Rickman, Genaro Suárez, Christopher A. Theissen, Taichi Uyama, Andreas Quirrenbach, Jason J. Wang, Niall Whiteford, Mark C. Wyatt, Alice Zurlo
Figure caption: Top row: the F300M data from one roll angle after sequentially subtracting the different ring models. The images are shown at four different display levels to show the disk components from the bright inner dust component to the fainter outer ring. Bottom row: the individual ring components of our convolved model. All images are shown at the orientation of the raw data.
Paper: The JWST Early Release Science Program for Direct Observations of Exoplanetary Systems. VI. Evidence for Radially Evolving Icy Grains in the HD 141569A Disk via NIRCam Coronagraphic Imaging
Authors: Maxwell A. Millar-Blanchaer, Élodie Choquet, Kellen Lawson, Sebastián Marino, Jens Kammerer, Aarynn L. Carter, Isabel Rebollido, Jarron M. Leisenring, Minjae Kim, Paul Kalas, Karl R Stapelfeldt, Sasha Hinkley, Mark Booth, Carol A. Grady, Elisabeth C. Matthews, Beth A. Biller, Andrew Skemer, Julien H. Girard, Schuyler G. Wolff, Kimberly Ward-Duong, Michael R. Meyer, Anthony Boccaletti, Eric Pantin, Brenda C. Matthews, Stanimir Metchev, Marshall D. Perrin, Christine H. Chen, Katie Crotts, Olivier Absil, William O. Balmer, Per Calissendorff, Gabriele Cugno, Thayne Currie, Camilla Danielski, Kielan K. W. Hoch, Markus Janson, Elena Manjavacas, Pierre-Olivier Lagage, Ben J. Sutlieff, Shrishmoy Ray, Bin B. Ren, Emily Rickman, Genaro Suárez, Christopher A. Theissen, Taichi Uyama, Andreas Quirrenbach, Jason J. Wang, Niall Whiteford, Mark C. Wyatt, Alice Zurlo
Figure caption: The median-collapsed calibrated data (left panel), the M-star model (center panel), and the model-subtracted data (right panel) for the first roll of the F300M data. All three panels are shown with the same logarithmic color stretch. The color stretch highlights the extent of the M-star PSF wings, which can be seen to extend to a ∼10″ radius.