adsabs/AstroCLIMB huggingface dataset:
Paper: Ages of Stars and Planets in the Kepler Field Younger than Four Billion Years
Authors: Luke G. Bouma, Lynne A. Hillenbrand, Andrew W. Howard, Howard Isaacson, Kento Masuda, Elsa K. Palumbo
Figure caption: Comparison of reported literature stellar rotation periods. “Santos” refers to the concatenation of A. R. G. Santos et al. (2019) and A. R. G. Santos et al. (2021). “M14” refers to A. McQuillan et al. (2014). “R23GPS” refers to the gradient of power spectrum (GPS) periods from T. Reinhold et al. (2023). The background is a 2D histogram with a logarithmic color stretch that counts overlapping stars between these studies. The black error bars show the median and ±1σ range of period the differences in 1 day bins. The solid gray “empirical σ P/P” line in the left panel shows the expected ±1σ range that would be spanned if the independent P rot measurements had Gaussian uncertainties drawn following the empirical estimate described in Section 2.1. Note the different vertical scales.
Paper: Ages of Stars and Planets in the Kepler Field Younger than Four Billion Years
Authors: Luke G. Bouma, Lynne A. Hillenbrand, Andrew W. Howard, Howard Isaacson, Kento Masuda, Elsa K. Palumbo
Figure caption: Impact of star formation rate (SFR) and kinematic heating on age distribution. Most Kepler stars are a few hundred parsecs above the Galactic plane (﹩\hat{Z}﹩ points to the north Galactic pole; ﹩\hat{Y}﹩ toward the direction of Galactic rotation). This is comparable to the ≈300 pc mass-weighted scale height. The dotted gray and solid orange lines show synthetic age distributions from TRILEGAL assuming a constant SFR (middle) and a two-step SFR (right), described in the text. A combination of both kinematic heating and a decreasing SFR are needed to qualitatively match the observed paucity of the youngest stars (blue line; as in Figure 6).
Paper: Ages of Stars and Planets in the Kepler Field Younger than Four Billion Years
Authors: Luke G. Bouma, Lynne A. Hillenbrand, Andrew W. Howard, Howard Isaacson, Kento Masuda, Elsa K. Palumbo
Figure caption: Variant of Figure 2, comparing the default rotation periods (left) from A. R. G. Santos et al. (2019, 2021) against the A. McQuillan et al. (2014) rotation periods (right). All stars are required to be amenable to rotation-based age-dating (i.e., none of bit flags 0–10 raised).
Paper: Ages of Stars and Planets in the Kepler Field Younger than Four Billion Years
Authors: Luke G. Bouma, Lynne A. Hillenbrand, Andrew W. Howard, Howard Isaacson, Kento Masuda, Elsa K. Palumbo
Figure caption: Variant of Figure 6, comparing our default adopted age distribution (left) based on the A. R. G. Santos et al. (2019, 2021) rotation periods against the age distribution (middle) based only on rotation periods reported by A. McQuillan et al. (2014).
Paper: Ages of Stars and Planets in the Kepler Field Younger than Four Billion Years
Authors: Luke G. Bouma, Lynne A. Hillenbrand, Andrew W. Howard, Howard Isaacson, Kento Masuda, Elsa K. Palumbo
Figure caption: Rotation-based age vs. effective temperature. The entire Kepler sample is shown on the left. KOI hosts are shown on the right. Each bar shows the ±1σ uncertainty for a star’s age as derived from its rotation period. Notable features are discussed in Appendix D.
Paper: A Photochemical Phosphorus-Hydrogen-Oxygen Network for Hydrogen-dominated Exoplanet Atmospheres
Authors: Elspeth K. H. Lee, Shang-Min Tsai, Julianne I. Moses, John M. C. Plane, Channon Visscher, Stephen J. Klippenstein
Figure caption: UV absorption cross sections for the phosphorus species in the network that undergo photolysis reactions. The photolysis threshold wavelength for each species is indicated by the colored arrows.
Paper: A Photochemical Phosphorus-Hydrogen-Oxygen Network for Hydrogen-dominated Exoplanet Atmospheres
Authors: Elspeth K. H. Lee, Shang-Min Tsai, Julianne I. Moses, John M. C. Plane, Channon Visscher, Stephen J. Klippenstein
Figure caption: VULCAN PHO network results for the benchmark 1D HD 189733b case. The VMR of each species is shown as solid lines and the T–p profile as a black dotted line. The dashed lines denote the chemical equilibrium values. Top left: thermochemistry only at [M/H] = 0. Top right: photochemical model at [M/H] = 0. Bottom left: thermochemistry only at [M/H] = 1. Bottom right: photochemical model at [M/H] = 1.
Paper: A Photochemical Phosphorus-Hydrogen-Oxygen Network for Hydrogen-dominated Exoplanet Atmospheres
Authors: Elspeth K. H. Lee, Shang-Min Tsai, Julianne I. Moses, John M. C. Plane, Channon Visscher, Stephen J. Klippenstein
Figure caption: VULCAN PHO network results for the benchmark GJ 1214b 1D case, with the J. I. Moses et al. (2022) K zz expression. The VMR of each species is shown as solid lines and the T–p profile as a black dotted line. The dashed lines show the chemical equilibrium values for each species. Top left: thermochemistry only at [M/H] = 0. Top right: photochemical model at [M/H] = 0. Middle left: thermochemistry only at [M/H] = 1. Middle right: photochemical model at [M/H] = 1. Bottom left: thermochemistry only at [M/H] = 2. Bottom right: photochemical model at [M/H] = 2.
Paper: A Photochemical Phosphorus-Hydrogen-Oxygen Network for Hydrogen-dominated Exoplanet Atmospheres
Authors: Elspeth K. H. Lee, Shang-Min Tsai, Julianne I. Moses, John M. C. Plane, Channon Visscher, Stephen J. Klippenstein
Figure caption: VULCAN PHO network results for the deep Jupiter (left) and Saturn (right) with the T–p profile from J. I. Moses et al. (2005) extended to 104 bar assuming an adiabat, and assuming a constant K zz = 108 cm2 s−1 (D. Wang et al. 2016). The VMR of each species is shown as solid lines and the T–p profile as a black dotted line. The dashed lines denote the chemical equilibrium abundances. The black arrow denotes the PH3 abundance retrieved by L. N. Fletcher et al. (2009) at lower-pressure regions.
Paper: A Photochemical Phosphorus-Hydrogen-Oxygen Network for Hydrogen-dominated Exoplanet Atmospheres
Authors: Elspeth K. H. Lee, Shang-Min Tsai, Julianne I. Moses, John M. C. Plane, Channon Visscher, Stephen J. Klippenstein
Figure caption: Cross sections of PO, CO2, CO, CH4, H2O, and SO2 at 1000 K and 1 mbar. Features are seen at around 4.1 and 8 μm, which lie in the wavelength range of NIRSpec, NIRCam, and MIRI JWST instruments, commonly used for exoplanet atmosphere characterization. However, these may be obscured by CH4 and SO2.
Paper: A Photochemical Phosphorus-Hydrogen-Oxygen Network for Hydrogen-dominated Exoplanet Atmospheres
Authors: Elspeth K. H. Lee, Shang-Min Tsai, Julianne I. Moses, John M. C. Plane, Channon Visscher, Stephen J. Klippenstein
Figure caption: Input T–p and K zz profiles for the HD 189733b case (left) and GJ 1214b case (right) used in this study.
Paper: A Photochemical Phosphorus-Hydrogen-Oxygen Network for Hydrogen-dominated Exoplanet Atmospheres
Authors: Elspeth K. H. Lee, Shang-Min Tsai, Julianne I. Moses, John M. C. Plane, Channon Visscher, Stephen J. Klippenstein
Figure caption: Updated PHO network (solid lines) compared to the results in D. Wang et al. (2017; dashed lines) for the T eq = 500 K test case from D. Wang et al. (2017).
Paper: A Photochemical Phosphorus-Hydrogen-Oxygen Network for Hydrogen-dominated Exoplanet Atmospheres
Authors: Elspeth K. H. Lee, Shang-Min Tsai, Julianne I. Moses, John M. C. Plane, Channon Visscher, Stephen J. Klippenstein
Figure caption: Molecular geometries of (a) PO, (b) PO2, (c) P2O3, (d) P4O6, (e) PH, (f) PH2, (g) P2H4, (h) P2H2, and (i) P2.
Paper: A Photochemical Phosphorus-Hydrogen-Oxygen Network for Hydrogen-dominated Exoplanet Atmospheres
Authors: Elspeth K. H. Lee, Shang-Min Tsai, Julianne I. Moses, John M. C. Plane, Channon Visscher, Stephen J. Klippenstein
Figure caption: Diagram showing the main chemical pathways present in the PHO scheme between key species.
Paper: A Study on the Nested Rings CME Structure Observed by the WISPR Imager Onboard Parker Solar Probe
Authors: Shaheda Begum Shaik, Mark G. Linton, Sarah E. Gibson, Phillip Hess, Robin C. Colaninno, Guillermo Stenborg, Carlos R. Braga, Erika Palmerio
Figure caption: Multispacecraft observations of the CME: (a) Orbit plot showing the respective locations of the S/C and Earth on 2021 January 21 at 02:00 UT (as numbered in the inset label). The black arrow points out the reference longitude of the CME, and the black dashed spiral shows a hypothetical heliospheric magnetic field line originating from that position. Radial distances at 0.5 and 1.0 au are delineated with the gray circles concentric on the Sun. The angular information of the plot is given in Stonyhurst longitudes. (b) Image plane plot showing the corresponding image planes of each instrument (red: ST-A/COR2; gray: WISPR-I; blue: SOHO/LASCO C3) as viewed from a perspective looking down on the ecliptic plane (similar to panel (a)), almost antiparallel to the direction of solar north up (marked by blue arrow nearly perpendicular to the page). The plot corresponds to a timestamp at around 02:12 UT on 2021 January 21, when the CME was in the FOVs of WISPR-I and ST-A/COR-2. The diagrams were produced using the Solar-MACH (J. Gieseler et al. 2023) and JHelioviewer (D. Müller et al. 2017) packages.
Paper: A Study on the Nested Rings CME Structure Observed by the WISPR Imager Onboard Parker Solar Probe
Authors: Shaheda Begum Shaik, Mark G. Linton, Sarah E. Gibson, Phillip Hess, Robin C. Colaninno, Guillermo Stenborg, Carlos R. Braga, Erika Palmerio
Figure caption: Cross-sectional representation of the MFR: (a) A cartoon of the internal structure of a magnetic flux rope showing the orientation of the magnetic field at different (concentric) flux surfaces varying from axial at the core to azimuthal at the outermost surface. The two-dimensional view, viewed from an observer on the right looking along the axis of the flux rope, is shown at the bottom of the panel. (b) Running difference with unsharp masking applied to the LW-processed WISPR image at 04:04 UT on 2021 January 21. This processing was applied to retain the contrast of the finer details of the image. (c) The model image generated from the GCS reconstruction with multiple croissant configurations representing each flux surface mimicking the cartoon model in panel (a). (d) Intensity profiles of the horizontal slits taken on the WISPR and model images, in black and green colors, respectively. Each feature denoted by the colored circles in panel (c) corresponds to the peaks in the intensity profiles (marked by the colored vertical lines).
Paper: A Study on the Nested Rings CME Structure Observed by the WISPR Imager Onboard Parker Solar Probe
Authors: Shaheda Begum Shaik, Mark G. Linton, Sarah E. Gibson, Phillip Hess, Robin C. Colaninno, Guillermo Stenborg, Carlos R. Braga, Erika Palmerio
Figure caption: A series of LW-processed WISPR-I detector images show the CME internal structure and its evolution on 2021 January 21 (with times in UT) with the Sun on the left of each image. The curves drawn manually in panels (e) and (h) represent the rings and other features that are observed as the CME propagates. The red curve indicates the inner core ring, the green curves are the two selected, clearly visible rings in the outer layer of the CME front, and the pink curves indicate the herringbone-shaped features at the backside of the core of the CME. The yellow curve within the core ring shows the bright inner base of the ring. Panels (d) and (e) display the WISPR image at the same time with and without the drawings, similarly for panels (g) and (h).
Paper: A Study on the Nested Rings CME Structure Observed by the WISPR Imager Onboard Parker Solar Probe
Authors: Shaheda Begum Shaik, Mark G. Linton, Sarah E. Gibson, Phillip Hess, Robin C. Colaninno, Guillermo Stenborg, Carlos R. Braga, Erika Palmerio
Figure caption: Analysis of longitudes and radial distances for the coherency of the nested rings: (a) and (b) Evolution of image coordinates β obs and γ obs of the tracked features, i.e., the fronts of the three rings (C front, ﹩{O}_{\mathrm{front}}^{{\prime} }﹩, and O front). (c) Inferred radial distances in solar radii as a function of time for each of the rings. (d) Inferred longitudes of each of the ring fronts vs. the radial distance plotted at the initial time of measurement, t 0. The symbols and color of the symbols and lines correspond to the three rings’ fronts, as used in Figure 5(a).
Paper: A Study on the Nested Rings CME Structure Observed by the WISPR Imager Onboard Parker Solar Probe
Authors: Shaheda Begum Shaik, Mark G. Linton, Sarah E. Gibson, Phillip Hess, Robin C. Colaninno, Guillermo Stenborg, Carlos R. Braga, Erika Palmerio
Figure caption: Image plane analysis of the coherency of the nested rings: (a) Running-difference image produced from the difference of the images at 03:00 UT and 02:44 UT on 2021 January 21. (b) Distance–time profiles and the evolution of the fronts of each ring (C front, ﹩{O}_{\mathrm{front}}^{{\prime} }﹩, and O front) are marked in panel (a) with star, triangle, and circle symbols. The linear fitting of the points is shown by the black line. (c) The aspect ratio (major-axis-length/minor-axis-length) of the rings from the times after which each of the rings becomes completely visible in the image FOV.
Paper: A Study on the Nested Rings CME Structure Observed by the WISPR Imager Onboard Parker Solar Probe
Authors: Shaheda Begum Shaik, Mark G. Linton, Sarah E. Gibson, Phillip Hess, Robin C. Colaninno, Guillermo Stenborg, Carlos R. Braga, Erika Palmerio
Figure caption: Evolution of distinct features of the CME event. (a) Polar representation of a WISPR-I image at 05:56 UT on 2021 January 21, with the location of a radial slit at an angle of 10° from the solar equator (black dashed vertical line) delineated with the yellow vertical line. The green and red symbols point out the features tracked on the outer and core rings, respectively. (b) Distance–time map of the development of the CME in the WISPR-I FOV. The evolution of the features tracked is marked with the same colors as in panel (a). The time period in which the features are clearly traceable is demarcated with the yellow box. (c) Zoomed-in view of the distance–time map for the selected time period in the yellow box of panel (b). The thin dashed green line in panel (c) between O front and O apex marks another ring (﹩{O}_{\mathrm{front}}^{{\prime} }﹩) within the outer shell, whereas the topmost dashed line of O front marks the second outer ring.
Paper: A Study on the Nested Rings CME Structure Observed by the WISPR Imager Onboard Parker Solar Probe
Authors: Shaheda Begum Shaik, Mark G. Linton, Sarah E. Gibson, Phillip Hess, Robin C. Colaninno, Guillermo Stenborg, Carlos R. Braga, Erika Palmerio
Figure caption: GCS reconstruction from background-subtracted ST-A/COR2 (FOV: 2.5–15 R ⊙), LASCO/C3 (FOV: 4–30 R ⊙), and WISPR-I (FOV: 9–70 R ⊙) LW images chosen close to 01:00 UT on 2021 January 21. Note a second CME in the FOVs of COR2 and C2 from the western limb (right) of the Sun (not modeled here). The CME on the eastern limb (left) corresponds to the CME under study and the one observed by WISPR. The flux rope fit of the LASCO C3 coronagraph (panels (b) and (h)) shows its longitudinal extent on the far side of the Sun consistent with the SOHO S/C’s viewing geometry and the CME trajectory as discussed in Figure 1(a). The fitting parameters used for the reconstruction are shown in panel (i).
Paper: A Study on the Nested Rings CME Structure Observed by the WISPR Imager Onboard Parker Solar Probe
Authors: Shaheda Begum Shaik, Mark G. Linton, Sarah E. Gibson, Phillip Hess, Robin C. Colaninno, Guillermo Stenborg, Carlos R. Braga, Erika Palmerio
Figure caption: Comparison of the CME feature as observed by ST-A/COR2 and WISPR-I. (a) ST-A/COR2 snapshot of the event at 00:54:00 UT on 2021 January 21 is processed following a running-difference scheme (i.e., with the preceding frame subtracted). (b) Same ST-A/COR2 snapshot but processed with the LW algorithm. (c) WISPR-I snapshot (processed with the LW algorithm) obtained at a later time, 03:00:21 UT, to match the extent of CME features seen in the ST-A/COR2 image. Both ST-A/COR2 snapshots are mirrored to have the same perspective as the WISPR-I snapshot.
Paper: Do Strong Bars Exhibit Strong Noncircular Motions?
Authors: Taehyun Kim, Dimitri A. Gadotti, Yun Hee Lee, Carlos López-Cobá, Woong-Tae Kim, Minjin Kim, Myeong-gu Park
Figure caption: (a) The radial profiles of V cir, V rad, and ﹩{V}_{\tan }﹩ for ESO 476–016, obtained by fitting the velocity fields with the bisymmetric model (K. Spekkens & J. A. Sellwood 2007). (b) The radial profiles of ellipticity (e), Q  b , and A 2. The vertical dotted line denotes the bar radius (R bar) estimated from the maximum of the bar ellipticity, and the vertical dashed–dotted line stands for R max where the noncircular motions (V rad and ﹩{V}_{\tan }﹩) become zero for more than two consecutive points. (c) Deprojected image of ESO 476–016, overlaid with R bar in a dashed ellipse. The green “+” points denote positions where Q  b  is estimated, and the bronze “+” points denote positions where A 2 is estimated. (d) The azimuthal profile of Q  T  at the radius where the radial profile of Q  T  reaches its maximum in (c). The local maxima of the azimuthal profile of Q  T  are denoted by green asterisks. The dotted line at Q  T  = 0.05 marks the threshold for counting the number of peaks associated with the bar. Q  b  is the average of the four local maxima.
Paper: Do Strong Bars Exhibit Strong Noncircular Motions?
Authors: Taehyun Kim, Dimitri A. Gadotti, Yun Hee Lee, Carlos López-Cobá, Woong-Tae Kim, Minjin Kim, Myeong-gu Park
Figure caption: Comparisons of bar strength (bar ellipticity, Q  b  and A 2) and the degree of noncircular motions. We present the maximum and the mean ratio of the noncircular velocity over circular velocity, Max(f NC) and Mean(f NC), respectively, which are indicators of the degree of noncircular motions. ﹩{R}_{\min }﹩ is the larger one between 2″ (the innermost annulus of the bisymmetric fit) and 0.2R bar, to avoid nuclear structures. ﹩{R}_{\max }﹩ is set to the radius where both V rad and ﹩{V}_{\tan }﹩ become zero for more than two consecutive annuli, which may go beyond the bar radius. The blue squares denote galaxies with a B/P bulge. Galaxies are plotted in light gray (one square and one circle) if the alignment between the bar and the major axis of the galaxy is within 10°, since in these cases the determination of f NC is compromised (see the text). The Spearman correlation coefficients are shown in each panel. The Spearman correlation coefficients in black represent samples whose bars are not aligned with the major axis of the galaxy, whereas those in gray include all galaxies. Note that the range of A 2 is different from that of ﹩{e}_{\max }﹩ and Q  b .
Paper: Do Strong Bars Exhibit Strong Noncircular Motions?
Authors: Taehyun Kim, Dimitri A. Gadotti, Yun Hee Lee, Carlos López-Cobá, Woong-Tae Kim, Minjin Kim, Myeong-gu Park
Figure caption: Profiles of the boxiness parameter, B4, for two example galaxies having (a) a disky bulge and (b) a B/P bulge. If B4 is positive, the isophote at that radius is disky. Conversely, if B4 is negative, the isophote is boxy. The blue points are from the DESI r-band images and the orange points are from the Spitzer 3.6 μm image. The vertical dashed lines represents the bar radius (R bar) from the maximum ellipticity. The vertical blue dotted line indicates the size of the B/P bulge (R BP), measured from the minimum of B4 inside the bar radius. B4 profiles are measured on projected images to prevent artificial elongation of bulges due to the deprojection process. B4 profiles for the other samples are presented in the Appendix.
Paper: A Study on the Nested Rings CME Structure Observed by the WISPR Imager Onboard Parker Solar Probe
Authors: Shaheda Begum Shaik, Mark G. Linton, Sarah E. Gibson, Phillip Hess, Robin C. Colaninno, Guillermo Stenborg, Carlos R. Braga, Erika Palmerio
Figure caption: Projectional representation of an MFR: the complex, three-dimensional structure of an MFR as it erupts and propagates from the Sun can be visualized through the projections, where each twist within the flux rope in three dimensions can be seen as translated into a two-dimensional representation. The inset box to the right illustrates this projected two-dimensional view.
Paper: Do Strong Bars Exhibit Strong Noncircular Motions?
Authors: Taehyun Kim, Dimitri A. Gadotti, Yun Hee Lee, Carlos López-Cobá, Woong-Tae Kim, Minjin Kim, Myeong-gu Park
Figure caption: The same as Figure 5, but now showing bar strengths and the maximum and the mean of the stellar radial velocity (V rad) over circular velocity (V cir).
Paper: Do Strong Bars Exhibit Strong Noncircular Motions?
Authors: Taehyun Kim, Dimitri A. Gadotti, Yun Hee Lee, Carlos López-Cobá, Woong-Tae Kim, Minjin Kim, Myeong-gu Park
Figure caption: ESO 476–016. (a) Optical r-band image constructed from the MUSE datacube. (b) Stellar velocity map (V st). (c) Bisymmetric model (V bis). (d) Residual velocity (﹩{V}_{\mathrm{res}}={V}_{\mathrm{st}}-{V}_{\mathrm{bis}}﹩). (b), (c), and (d) are taken from C. López-Cobá et al. (2022) and reconstructed.
Paper: Do Strong Bars Exhibit Strong Noncircular Motions?
Authors: Taehyun Kim, Dimitri A. Gadotti, Yun Hee Lee, Carlos López-Cobá, Woong-Tae Kim, Minjin Kim, Myeong-gu Park
Figure caption: Isophotes of galaxies in the bar region from the DESI and Pan-STARRS r-band images for UGC 03634. The white line at the bottom left spans 1 kpc for each galaxy. Images are not corrected for deprojection, as this may distort the shape of the bulge.
Paper: Do Strong Bars Exhibit Strong Noncircular Motions?
Authors: Taehyun Kim, Dimitri A. Gadotti, Yun Hee Lee, Carlos López-Cobá, Woong-Tae Kim, Minjin Kim, Myeong-gu Park
Figure caption: Radial profiles of (a) ﹩{V}_{\mathrm{cir}},{V}_{\mathrm{rad}},{V}_{\tan }﹩, and f NC from fitting the stellar velocity fields with the bisymmetric model (K. Spekkens & J. A. Sellwood 2007). The vertical dashed–dotted line stands for R max, where V rad and ﹩{V}_{\tan }﹩ (noncircular motions) become zero for more than two consecutive data points. (b) Ellipticity (e), Q  b , and A 2. The purple vertical dotted line represents the bar radius. All quantities are obtained from deprojected images. (c) Radial profiles of B4, the boxiness parameter obtained from projected images. The vertical dashed line denotes the size of the B/P (R BP) in the case where the galaxy exhibits B/P structure.
Paper: Do Strong Bars Exhibit Strong Noncircular Motions?
Authors: Taehyun Kim, Dimitri A. Gadotti, Yun Hee Lee, Carlos López-Cobá, Woong-Tae Kim, Minjin Kim, Myeong-gu Park
Figure caption: Continued.
Paper: Combined JWST–MUSE Integral Field Spectroscopy of the Most Luminous Quasar in the Local Universe, PDS 456
Authors: Jerome Seebeck, Sylvain Veilleux, Weizhe Liu, David S. N. Rupke, Andrey Vayner, Dominika Wylezalek, Nadia L. Zakamska, Caroline Bertemes
Figure caption: 1D spectrum of PDS 456 extracted from the MIRI data cube showing the sensitivity drop at longer wavelengths and its correction. We show the uncorrected spectrum extracted with a conical aperture (purple), the simulated WISE measurements from the JWST spectrum (purple points), the correction factor derived from the JWST correction (gray), the JWST spectrum corrected with this factor (brown), the simulated WISE measurements from the corrected JWST spectrum (brown points), and the WISE measurements (colored points). The left axis displays the flux density in units of Jy for the spectrum and the right axis displays the scale of the correction factor.
Paper: Combined JWST–MUSE Integral Field Spectroscopy of the Most Luminous Quasar in the Local Universe, PDS 456
Authors: Jerome Seebeck, Sylvain Veilleux, Weizhe Liu, David S. N. Rupke, Andrey Vayner, Dominika Wylezalek, Nadia L. Zakamska, Caroline Bertemes
Figure caption: Footprints of the MIRI channels (green) and NIRSpec data (red) plotted over that of the MUSE data, which has been cut down to 14″ × 16″.