adsabs/AstroCLIMB huggingface dataset:
Paper: Negative-energy Waves in the Vertical Threads of a Solar Prominence
Authors: Jincheng Wang, Dong Li, Chuan Li, Yijun Hou, Zhike Xue, Zhe Xu, Liheng Yang, Qiaoling Li
Figure caption: Observations of CHASE/HIS Hα spectrum data. (a) Composite map constructed using a set of scanning spectrum data at Hα center at around 04:07 UT. (b) Spectrum image of Hα along the black line in panel (a). (c) Corresponding FWHM map derived from the Hα spectrum. The FWHM is determined to be the width of the profile where the intensity exceeds half of the maximum amplitude. The blue line corresponds to line AB in Figure 2(a), while two yellow asterisks correspond to the two yellow asterisks in Figure 2(d). (d) The profile of the Hα line at the region marked by the white box in panel (c). The Hα line is calculated by the average over the white box, while the error bars represent the corresponding standard deviation. The vertical dotted–dashed line denotes the Hα center. The red dashed line and blue solid/dotted lines represent the fitted lines by single- and double-Gaussian functions, respectively. The red and blue values denote the Doppler velocity derived by single- and double-Gaussian function fitting, respectively.
Paper: Negative-energy Waves in the Vertical Threads of a Solar Prominence
Authors: Jincheng Wang, Dong Li, Chuan Li, Yijun Hou, Zhike Xue, Zhe Xu, Liheng Yang, Qiaoling Li
Figure caption: Evolution of SMa. (a1–a6) Time–distance diagrams along different parallel cuts, spaced at a distance of 0.55 Mm from each other and from higher to lower positions. The FOV is outlined by the dotted box in Figure 3(c1). Yellow plus signs mark the peaks of each transverse swaying motion. The white box in panel (a6) shows the profile of these peaks with respect to time, while the y-axis represents the height of each cut relative to each transverse swaying motion. The start time was at 03:41:39 UT. The yellow line denotes the fitted line with a linear function. (b1–b6) Profiles of each transverse swaying motion. The blue solid lines represent the fitted lines based on the function in Equation (1).
Paper: Negative-energy Waves in the Vertical Threads of a Solar Prominence
Authors: Jincheng Wang, Dong Li, Chuan Li, Yijun Hou, Zhike Xue, Zhe Xu, Liheng Yang, Qiaoling Li
Figure caption: Same as Figure 4, but for SMb. The FOV of panels (a1)–(ab1) is outlined by the dotted box in Figure 3(c2). The start time of the white box in panel (a6) was at 03:46:37 UT.
Paper: A Unifying Model of Mixed Inertial Modes in the Sun
Authors: Rekha Jain, Bradley W. Hindman, Catherine Blume
Figure caption: Eigenfrequencies of inertial modes trapped radially and latitudinally within a millstone-shaped equatorial channel. The dimensionless eigenfrequencies are plotted as a function of the azimuthal order, m. Different colors correspond to different latitudinal orders, λ, as indicated in the legend. The solid and dashed curves are for radial orders n = 0 and 1, respectively. The horizontal gray line corresponds to the zero-frequency geostrophic mode. For reference, we also show the frequencies of equatorial Rossby waves with the gray filled circles, given by ﹩\omega /{\rm{\Omega }}=-2m/{k}_{h}^{2}{R}_{\odot }^{2}﹩. The modes with positive zonal phase speed, ω/m > 0, propagate in the prograde direction, whereas modes with negative phase speed ω/m < 0 are retrograde propagating.
Paper: A Unifying Model of Mixed Inertial Modes in the Sun
Authors: Rekha Jain, Bradley W. Hindman, Catherine Blume
Figure caption: Radial eigenfunctions for an HFR mode (λ = 2) for an azimuthal order m = 2 and for the radial fundamental n = 0. The eigenfunctions are shown as a function of dimensionless radius, r/R ⊙. The real part of the zonal velocity (magenta curve) and radial vorticity (blue) are illustrated, whereas the imaginary part of the horizontal divergence (green curve) is shown. Each eigenfunction is scaled by the mass density ρ 0 and the zonal velocity is further scaled by the horizontal wavenumber k  h  so that it has the same units as the other variables. The radial vorticity and horizontal divergence have similar magnitudes but differing radial structures.
Paper: A Unifying Model of Mixed Inertial Modes in the Sun
Authors: Rekha Jain, Bradley W. Hindman, Catherine Blume
Figure caption: Arrows indicate the horizontal flow for three distinct modes as a function of longitude and latitude for a depth that is 2 Mm below the photosphere. The underlying color image shows the radial vorticity component with red tones for positive vorticity and blue tones for negative. Each panel illustrates the mode with azimuthal order m = 2 but for different latitudinal orders, as indicated to the right. All flow fields are clearly both vortical and horizontally divergent.
Paper: A Unifying Model of Mixed Inertial Modes in the Sun
Authors: Rekha Jain, Bradley W. Hindman, Catherine Blume
Figure caption: Summary of the family of mixed inertial waves that we explore here and their identification with inertial waves as reported in a selection of previous studies. We argue that many of the waves previously discovered through observations or through theoretical calculations, including the HFR mode, are simply latitudinal overtones within the same family of mixed inertial modes. We have overplotted the observed frequencies of HFR modes (Hanson et al. 2022) with blue pluses and the “mixed modes” of Bekki et al. (2022a) with red asterisks.
Paper: Axial Flux Evolution of Small-scale Magnetic Flux Ropes from 0.06 to 10 au
Authors: Hameedullah Farooki, Jeongwoo Lee, Francesco Pecora, Haimin Wang, Hyomin Kim
Figure caption: (a) Comparison of axial flux for different ranges of distance from the Sun in the form of a (complementary) empirical cumulative distribution function. (b, c) Flux limit as a function of distance from the Sun and as a function of plasma age, estimated as a flux rope’s distance from the Sun divided by its velocity. In panels (b) and (c), each line represents the range of distances used to sample the events. The number of events in each sample is listed below the lines. The 95% confidence level uncertainty estimated with bootstrapping is shown as a shaded region around each line. In panel (b), the distance is virtually constant in the case of Wind, so a single point at 1 au is used instead of a line. The colors of the lines indicate the spacecraft used to detect the events, as labeled in the legend in the lower right corner.
Paper: Discovery of the Longest-period Classical Cepheid in the Milky Way
Authors: I. Soszyński, D. M. Skowron, A. Udalski, P. Pietrukowicz, M. Gromadzki, M. K. Szymański, J. Skowron, P. Mróz, R. Poleski, S. Kozłowski, P. Iwanek, M. Wrona, K. Ulaczyk, K. Rybicki, M. Mróz
Figure caption: Unfolded (left panels) and phase-folded (right panels) I-band light curves of OGLE-GD-CEP-1884 (upper panels) and three example variable stars with periods nearly identical to that of OGLE-GD-CEP-1884: a semiregular variable from the OGLE collection of LPVs in the Galactic bulge (Soszyński et al. 2013), an RV Tauri star from the OGLE collection of type II Cepheids in the bulge (Soszyński et al. 2017), and a spotted variable star from the Galactic bulge (Iwanek et al. 2019). Note the differences between the light curve of a classical Cepheid and those of other types of variable stars.
Paper: Axial Flux Evolution of Small-scale Magnetic Flux Ropes from 0.06 to 10 au
Authors: Hameedullah Farooki, Jeongwoo Lee, Francesco Pecora, Haimin Wang, Hyomin Kim
Figure caption: Area–flux scatter plot. It is in log–log format, so the slope of each proportionality is represented as the y-intercept. Samples of events from different spacecraft and ranges of heliocentric distance are plotted separately. Each line represents direct proportionality, with the slope being the average axial flux density for the sample. The shaded region is partially unresolved because SMFRs of diameter below (600 km s−1)(30 s) (due to the minimum 30 s sliding window) can only be detected when the orientation is sufficiently closely aligned with the velocity in the spacecraft frame of reference (Farooki et al. 2024b).
Paper: Discovery of the Longest-period Classical Cepheid in the Milky Way
Authors: I. Soszyński, D. M. Skowron, A. Udalski, P. Pietrukowicz, M. Gromadzki, M. K. Szymański, J. Skowron, P. Mróz, R. Poleski, S. Kozłowski, P. Iwanek, M. Wrona, K. Ulaczyk, K. Rybicki, M. Mróz
Figure caption: Phase-folded I-band (upper panel) and V-band (middle panel) OGLE light curves of OGLE-GD-CEP-1884 and radial velocity curve of this star from the Gaia Focused Product Release (Gaia Collaboration et al. 2023, lower panel). The orange curves depict template light and radial velocity curves of a classical Cepheid with a period of 78.14 days generated using the code provided by Pejcha & Kochanek (2012).
Paper: Axial Flux Evolution of Small-scale Magnetic Flux Ropes from 0.06 to 10 au
Authors: Hameedullah Farooki, Jeongwoo Lee, Francesco Pecora, Haimin Wang, Hyomin Kim
Figure caption: Histogram of τ  c  at different ranges of heliocentric distance. Binned in log space. The y-axis is in linear space (values not shown to save space).
Paper: Axial Flux Evolution of Small-scale Magnetic Flux Ropes from 0.06 to 10 au
Authors: Hameedullah Farooki, Jeongwoo Lee, Francesco Pecora, Haimin Wang, Hyomin Kim
Figure caption: Map of events detected in the inner heliosphere in heliocentric inertial polar coordinates. Each event is plotted as a circle such that the area of the marker is proportional to the axial flux of the SMFR (not its cross-sectional area, which naturally increases as a function of distance owing to the expansion of the solar wind).
Paper: Axial Flux Evolution of Small-scale Magnetic Flux Ropes from 0.06 to 10 au
Authors: Hameedullah Farooki, Jeongwoo Lee, Francesco Pecora, Haimin Wang, Hyomin Kim
Figure caption: Three examples of SMFR events detected by our algorithm from PSP, SolO, and Voyager 1 data. The top panels display the GS reconstruction of each event. The bottom panels show the raw measurements transformed into the flux rope coordinate system.
Paper: Cold Dark Matter and Self-interacting Dark Matter Interpretations of the Strong Gravitational Lensing Object JWST-ER1
Authors: Demao Kong, Daneng Yang, Hai-Bo Yu
Figure caption: JWST-ER1g: the projected halo mass profile of the contracted CDM halo (solid black), the initial NFW halo (dashed black), and the SIDM halos with σ/m = 0.1 cm2 g−1 (solid magenta) and 0.3 cm2 g−1 (solid orange). The corresponding SIDM halos without including the influence of baryons are shown for comparison (dotted). The measured value is ﹩{5.4}_{-1.5}^{+3.7}\times {10}^{11}\,{M}_{\odot }﹩ within the Einstein radius 6.6 kpc (red diamond) after subtracting the baryon mass from the total enclosed mass (van Dokkum et al. 2024).
Paper: Cold Dark Matter and Self-interacting Dark Matter Interpretations of the Strong Gravitational Lensing Object JWST-ER1
Authors: Demao Kong, Daneng Yang, Hai-Bo Yu
Figure caption: Left panel: the projected halo mass profile of the simulated SIDM halo at t = 0 Gyr (solid green), 3.4 Gyr (dashed green), and 11.3 Gyr (dashed–dotted green) for JWST-ER1g. Right panel: the surface density profile of the simulated SIDM halo at t = 0 Gyr (solid green) and 11.3 Gyr (dashed-dotted green) for J1636+4707. For both simulated halos, σ/m = 0.1 cm2 g−1. Other curves are the same as those in Figures 2 and 3.
Paper: Discovery of the Longest-period Classical Cepheid in the Milky Way
Authors: I. Soszyński, D. M. Skowron, A. Udalski, P. Pietrukowicz, M. Gromadzki, M. K. Szymański, J. Skowron, P. Mróz, R. Poleski, S. Kozłowski, P. Iwanek, M. Wrona, K. Ulaczyk, K. Rybicki, M. Mróz
Figure caption: Face-on view of the Milky Way traced by 2388 classical Cepheids with distances measured using mid-IR period–luminosity relations (Skowron et al. 2019a, 2019b). The colors of the points indicate the ages of the Cepheids (as shown by the scale on the right side) derived from the period–age relation by Anderson et al. (2016). OGLE-GD-CEP-1884 is marked by the star symbol, the Sun is indicated by the white circle, and the Galactic center is shown by the black cross.
Paper: Cold Dark Matter and Self-interacting Dark Matter Interpretations of the Strong Gravitational Lensing Object JWST-ER1
Authors: Demao Kong, Daneng Yang, Hai-Bo Yu
Figure caption: Left panel: the projected mass profile of the contracted CDM halo (solid black), the initial NFW halo (dashed black), and the SIDM halos with σ/m = 0.1 cm2 g−1 (solid magenta) and 0.3 cm2 g−1 (solid orange) for JWST-ER1g based on the measurement in Mercier et al. (2023; blue diamond). Right panel: the projected mass profile of the contracted CDM halo (solid black) and the initial NFW halo (dashed black), where the halo parameters are chosen such that the NFW halo without adiabatic contraction could explain the measurement in Mercier et al. (2023; blue diamond).
Paper: Cold Dark Matter and Self-interacting Dark Matter Interpretations of the Strong Gravitational Lensing Object JWST-ER1
Authors: Demao Kong, Daneng Yang, Hai-Bo Yu
Figure caption: J1636+4707: the surface density profile of the SIDM halo with σ/m = 0.1 cm2 g−1 (solid magenta), the stars (cyan), and the NFW-like halo (gray) from observations (1σ band) (Shajib et al. 2021). For comparison, the CDM halo with adiabatic contraction (solid black) and the SIDM halo without baryons (dotted magenta) are shown.
Paper: Cold Dark Matter and Self-interacting Dark Matter Interpretations of the Strong Gravitational Lensing Object JWST-ER1
Authors: Demao Kong, Daneng Yang, Hai-Bo Yu
Figure caption: The posterior distribution of the cross section σ/m, halo mass M 200, and concentration c 200 for JWST-ER1g with the measurement from van Dokkum et al. (2024), where the contours denote 1σ and 2σ confidence regions.
Paper: Cold Dark Matter and Self-interacting Dark Matter Interpretations of the Strong Gravitational Lensing Object JWST-ER1
Authors: Demao Kong, Daneng Yang, Hai-Bo Yu
Figure caption: The projected halo mass profiles for six different sets of the model parameters for JWST-ER1g: M 200, c 200, and M  b . The line style is the same as in Figure 2.
Paper: Cold Dark Matter and Self-interacting Dark Matter Interpretations of the Strong Gravitational Lensing Object JWST-ER1
Authors: Demao Kong, Daneng Yang, Hai-Bo Yu
Figure caption: The projected mass profile of the Hernquist profile used for modeling the stellar distribution of JWST-ERg, compared to the Sérsic profile from van Dokkum et al. (2024).
Paper: Vortex Fiber Nulling for Exoplanet Observations: First Direct Detection of M Dwarf Companions around HIP 21543, HIP 94666, and HIP 50319
Authors: Daniel Echeverri, Jerry W. Xuan, John D. Monnier, Jacques-Robert Delorme, Jason J. Wang, Nemanja Jovanovic, Katelyn Horstman, Garreth Ruane, Bertrand Mennesson, Eugene Serabyn, Dimitri Mawet, J. Kent Wallace, Sofia Hillman, Ashley Baker, Randall Bartos, Benjamin Calvin, Sylvain Cetre, Greg Doppmann, Luke Finnerty, Michael P. Fitzgerald, Chih-Chun Hsu, Joshua Liberman, Ronald López, Maxwell Millar-Blanchaer, Evan Morris, Jacklyn Pezzato, Jean-Baptiste Ruffio, Ben Sappey, Tobias Schofield, Andrew J. Skemer, Ji Wang, Yinzi Xin, Narsireddy Anugu, Sorabh Chhabra, Noura Ibrahim, Stefan Kraus, Gail H. Schaefer, Cyprien Lanthermann
Figure caption: Top row: CCF between the best-fit model and the measured spectra for (a) HIP 21543, (b) HIP 94666, and (c) HIP 50319. The CCF S/N is included in the top left of the plots. The periodic oscillations in the CCF for HIP 50319 are due to residual fringing that was not fully removed in the fits, limiting us to a tentative detection on this target. Lower two rows: CHARA detection maps for HIP 21543 and HIP 50319. HIP 94666 is omitted as it was not detected by CHARA. The axes mark the distance in milliarcseconds from the primary, with north up and east left. The white crosshairs denote the detected companion. Four maps are shown for HIP 21543, two for MIRC-X ((d) and (f)) and two for MYSTIC ((e) and (g)), across both nights. HIP 50319 has two maps ((h) and (i)), both from MYSTIC, one for each night. The upper left text in the CHARA maps denotes the observing night, beam combiner, and band for each plot.
Paper: Vortex Fiber Nulling for Exoplanet Observations: First Direct Detection of M Dwarf Companions around HIP 21543, HIP 94666, and HIP 50319
Authors: Daniel Echeverri, Jerry W. Xuan, John D. Monnier, Jacques-Robert Delorme, Jason J. Wang, Nemanja Jovanovic, Katelyn Horstman, Garreth Ruane, Bertrand Mennesson, Eugene Serabyn, Dimitri Mawet, J. Kent Wallace, Sofia Hillman, Ashley Baker, Randall Bartos, Benjamin Calvin, Sylvain Cetre, Greg Doppmann, Luke Finnerty, Michael P. Fitzgerald, Chih-Chun Hsu, Joshua Liberman, Ronald López, Maxwell Millar-Blanchaer, Evan Morris, Jacklyn Pezzato, Jean-Baptiste Ruffio, Ben Sappey, Tobias Schofield, Andrew J. Skemer, Ji Wang, Yinzi Xin, Narsireddy Anugu, Sorabh Chhabra, Noura Ibrahim, Stefan Kraus, Gail H. Schaefer, Cyprien Lanthermann
Figure caption: Spectrum at R ∼ 35,000 from VFN observations of HIP 21543. Only KPIC echelle order 6, the one used for the forward model fits, is shown. The raw spectrum has been median-filtered to remove the continuum and is shown as the solid gold line, while the best-fit full model is in dashed green. Various components of the best-fit model are also shown: primary star spectrum (blue), companion spectrum (red), and residuals (gray dots). The companion spectrum is about 5 times fainter than that of the primary after partial nulling of the latter by VFN. The true flux ratio for the system is 70 ± 11, as measured by CHARA and shown in Table 3.
Paper: Tidal Disruption Encores
Authors: Taeho Ryu, Rosalba Perna, Matteo Cantiello
Figure caption: Differential rates of all sBH TDEs of 1 M ⊙ stars by 10 M ⊙ BHs (left) and integrated rates (right). In the right panel, the gray solid line depicts the total rate for sBH TDEs, and the black dashed line depicts the rate for sBH TDEs producing the debris that could potentially fall into the SMBH and creating flares. Their rates are almost identical because most of sBH TDEs happen close to the SMBH where the spilled debris is tightly bound to the SMBH. Note that the fallback rates of the spilled debris are super-Eddington in almost all sBH TDEs. In addition, the rate of events with the debris falling at a super-Eddington fallback rate on highly eccentric orbits (e ≳ 0.9) is depicted with the blue dotted line. The SMBH-“TDE”-like rates are indicated using the orange horizontal strip.
Paper: Tidal Disruption Encores
Authors: Taeho Ryu, Rosalba Perna, Matteo Cantiello
Figure caption: The energy distribution dM/dE of debris, originally unbound from the sBH, in the frame of the 106 M ⊙ SMBH. E grav is the local gravitational potential, G M •/R. The colors show how much the debris was unbound from the sBH originally: most unbound (yellow) to least unbound (blue).
Paper: Tidal Disruption Encores
Authors: Taeho Ryu, Rosalba Perna, Matteo Cantiello
Figure caption: Several distances that determine the lower limit in the integration for the event rate: 10r g (black solid), tidal radius r t (red dashed), the minimum distance at which there is at least one star R(N ⋆ = 1) (blue dashed), and the minimum distance at which there is at least one sBH R(N • = 1) (orange solid). The maximum of those distances is used as the integration lower limit for the total rate calculation.
Paper: Tidal Disruption Encores
Authors: Taeho Ryu, Rosalba Perna, Matteo Cantiello
Figure caption: Eccentricity e (left) and pericenter distance r p (right) of the “spilled” debris unbound from the sBH but bound to the 106 M ⊙ SMBH. Those quantities are measured for the debris’s orbit relative to the SMBH. In both panels, the hatched regions indicate highly eccentric debris (e > 0.9). The region with a white background indicates debris unbound from the SMBH. The binding energy of the spilled debris relative to the SMBH is determined by its kinetic energy at the point it escapes the RL around the sBH at a given location. The debris moving in the opposite direction to the sBH (θ ≃ 180°) tend to have less kinetic energy and smaller angular momentum, resulting in a more bound and more eccentric orbit around the SMBH. As the distance of the sBH TDEs from the SMBH gets smaller, the kinetic energy of the sBH is more dominant with respect to the debris’s kinetic energy, leading to the spilled debris’s orbit becoming more similar to that of the sBH.
Paper: Tidal Disruption Encores
Authors: Taeho Ryu, Rosalba Perna, Matteo Cantiello
Figure caption: Schematic diagram for a double-flare event in a 2D configuration. While an sBH (small yellow circle) is orbiting around an SMBH (large yellow circle), it tidally destroys a star (red circle) (left). The angle of the incoming star’s orbit at disruption relative to the line connecting the sBH and SMBH is θ. The debris bound to the sBH returns and creates the first flare (middle). The debris, originally unbound from the sBH, spills out of its RL. If the kinetic energy of the spilled debris is not sufficiently high, it remains bound to the SMBH and falls into it, creating the second flare (right). The diagram is not to scale.
Paper: Tidal Disruption Encores
Authors: Taeho Ryu, Rosalba Perna, Matteo Cantiello
Figure caption: The returning rate of the spilled debris, originally unbound from the sBH following an sBH TDE at distance R, to the SMBH for a range of values of θ. ﹩{\dot{M}}_{\mathrm{Edd}}={L}_{\mathrm{Edd}}/{c}^{2}﹩, where L Edd is the Eddington luminosity. The lines are color-coded based on the mass-weighted average eccentricity. Unlike ordinary TDEs, the fallback rates can have a variety of shapes, depending on θ, R, and M •, including the t −5/3 power-law decay.
Paper: An X-Ray Census of Active Galactic Nuclei in the Virgo and Fornax Clusters of Galaxies with SRG/eROSITA
Authors: Meicun Hou, Zhensong Hu, Zhiyuan Li
Figure caption: The sky distribution of member galaxies in Virgo (left) and Fornax (right). Member galaxies in the Extended Virgo Cluster Catalog and Fornax Cluster Catalog are indicated by blue symbols. The nuclear X-ray sources detected by eRASS1 are marked by red symbols color-coded by the 0.2–2.3 keV luminosity. ETGs and LTGs are represented by circles and triangles. The size of each symbol is scaled with stellar mass (approximated by B  T  mag for the Fornax galaxies).
Paper: An X-Ray Census of Active Galactic Nuclei in the Virgo and Fornax Clusters of Galaxies with SRG/eROSITA
Authors: Meicun Hou, Zhensong Hu, Zhiyuan Li
Figure caption: X-ray flux and luminosity distributions of all the eRASS1 point sources in the Virgo (left) and Fornax (right) footprint. Soft-band and hard-band sources are shown in blue and orange histograms. The peak of the distributions indicates the detection completeness limit.
Paper: A JWST Survey of the Supernova Remnant Cassiopeia A
Authors: Dan Milisavljevic, Tea Temim, Ilse De Looze, Danielle Dickinson, J. Martin Laming, Robert Fesen, John C. Raymond, Richard G. Arendt, Jacco Vink, Bettina Posselt, George G. Pavlov, Ori D. Fox, Ethan Pinarski, Bhagya Subrayan, Judy Schmidt, William P. Blair, Armin Rest, Daniel Patnaude, Bon-Chul Koo, Jeonghee Rho, Salvatore Orlando, Hans-Thomas Janka, Moira Andrews, Michael J. Barlow, Adam Burrows, Roger Chevalier, Geoffrey Clayton, Claes Fransson, Christopher Fryer, Haley L. Gomez, Florian Kirchschlager, Jae-Joon Lee, Mikako Matsuura, Maria Niculescu-Duvaz, Justin D. R. Pierel, Paul P. Plucinsky, Felix D. Priestley, Aravind P. Ravi, Nina S. Sartorio, Franziska Schmidt, Melissa Shahbandeh, Patrick Slane, Nathan Smith, Niharika Sravan, Kathryn Weil, Roger Wesson, J. Craig Wheeler
Figure caption: Important features of Cas A identified in our survey and discussed in this paper. The composite image in the center panel combines NIRCam and MIRI filters as indicated. Large boxes outlined with dashed white lines show areas of interest enlarged in the surrounding panels that use the same filters and color scheme, with the exception of panels (1b) and (6), which only use NIRCam filters. Small boxes outlined with solid white lines show the positions of the four regions of MIRI/MRS IFU spectroscopy.