adsabs/AstroCLIMB huggingface dataset:
Paper: Little Red Dots at an Inflection Point: Ubiquitous V-shaped Turnover Consistently Occurs at the Balmer Limit
Authors: David J. Setton, Jenny E. Greene, Anna de Graaff, Yilun Ma, 逸伦 马, Joel Leja, Jorryt Matthee, Rachel Bezanson, Leindert A. Boogaard, Nikko J. Cleri, Harley Katz, Ivo Labbe, Michael V. Maseda, Ian McConachie, Tim B. Miller, Sedona H. Price, Katherine A. Suess, Pieter van Dokkum, Bingjie Wang, 冰洁 王, Andrea Weibel, Katherine E. Whitaker, Christina C. Williams
Figure caption: The results of the broken power-law fits to the red spectra, illustrated by showing the break wavelength versus the difference between the red and blue power-law indices. Sources with kred − kblue > 0 at the 2σ level are colored red, those consistent with kred − kblue > 0 at the 1σ level are colored green, and those consistent with no break are colored blue. Sources which have a well-determined break (λbreak,84 − λbreak,16 < 750 Å) are shown as solid points, and all other sources are shown with transparency. The shaded gray region shows the range of kred − kblue and λbreak that comes from applying this model to PRISM models of dusty poststarburst galaxies (with some scattered light; see Section 4.3). All of the galaxies with a preference for a strong change in slope are fit with a break that occurs near 0.3645 μm, the Balmer break, at a very similar wavelength to the one returned by model fits to simple stellar populations.
Paper: Little Red Dots at an Inflection Point: Ubiquitous V-shaped Turnover Consistently Occurs at the Balmer Limit
Authors: David J. Setton, Jenny E. Greene, Anna de Graaff, Yilun Ma, 逸伦 马, Joel Leja, Jorryt Matthee, Rachel Bezanson, Leindert A. Boogaard, Nikko J. Cleri, Harley Katz, Ivo Labbe, Michael V. Maseda, Ian McConachie, Tim B. Miller, Sedona H. Price, Katherine A. Suess, Pieter van Dokkum, Bingjie Wang, 冰洁 王, Andrea Weibel, Katherine E. Whitaker, Christina C. Williams
Figure caption: PRISM spectra of red, Hα-strong galaxies from the DJA are shown in black, with broken power-law fits to the emission-masked spectra shown in red. The spectra are ordered, from top to bottom, by the 50th percentile constraint on the difference between the red and blue power-law indices, from reddest to bluest. Sources are outlined based on the constraints on kred − kblue, with >0 at the 2σ level shown in red, >0 at the 1σ level shown in green, and ≤0 at at the 1σ level shown in blue. Sources with a gray background have f(0﹩\mathop{.}\limits^{\unicode{x02033}}﹩2/0﹩\mathop{.}\limits^{\unicode{x02033}}﹩1) > 1.8, which we consider to be resolved. The sources which favor a strong change in slope all change slope at an extremely similar wavelength, close to 0.3645 μm (H∞).
Paper: Little Red Dots at an Inflection Point: Ubiquitous V-shaped Turnover Consistently Occurs at the Balmer Limit
Authors: David J. Setton, Jenny E. Greene, Anna de Graaff, Yilun Ma, 逸伦 马, Joel Leja, Jorryt Matthee, Rachel Bezanson, Leindert A. Boogaard, Nikko J. Cleri, Harley Katz, Ivo Labbe, Michael V. Maseda, Ian McConachie, Tim B. Miller, Sedona H. Price, Katherine A. Suess, Pieter van Dokkum, Bingjie Wang, 冰洁 王, Andrea Weibel, Katherine E. Whitaker, Christina C. Williams
Figure caption: A demonstration of our color-EW selection of galaxies with LRD-like rest-frame colors. Left: the spectrum of RUBIES-BLAGN-1 (B. Wang et al. 2025), with synthetic rest-frame “B” and “R” filters (chosen to avoid strong emission lines) labeled as blue and red, respectively. The Balmer limit, H∞, and Hα+[N II] are labeled. Right: B − R versus EW Hα for the entire RUBIES/DJA PRISM sample with mF444W < 26.5. Sources from the RUBIES Cycle 2 program are shown as red, and all other sources from the DJA are shown as black. The top-right box contains extremely red sources with strong Hα emission, capturing sources that were selected photometrically to have a V shape in D. D. Kocevski et al. (2025, orange), and the RUBIES-BLAGN-1 (highlighted as a purple star).
Paper: Little Red Dots at an Inflection Point: Ubiquitous V-shaped Turnover Consistently Occurs at the Balmer Limit
Authors: David J. Setton, Jenny E. Greene, Anna de Graaff, Yilun Ma, 逸伦 马, Joel Leja, Jorryt Matthee, Rachel Bezanson, Leindert A. Boogaard, Nikko J. Cleri, Harley Katz, Ivo Labbe, Michael V. Maseda, Ian McConachie, Tim B. Miller, Sedona H. Price, Katherine A. Suess, Pieter van Dokkum, Bingjie Wang, 冰洁 王, Andrea Weibel, Katherine E. Whitaker, Christina C. Williams
Figure caption: Median stacks of the 2σ (red) and 1σ (green) samples that are unresolved (see Figure 3). Shaded regions denote the error in the median. The sources with well-constrained red changes in slope show a strong preference for an inflection at and around 0.3645 μm, H∞. The stack of sources with less well constrained changes in slope still exhibit a similar shape at H∞. Key emission features are labeled.
Paper: Identification of Large-scale (>100 kpc) Radio Jets in Narrow-line Seyfert 1 Galaxies
Authors: S. Umayal, Vaidehi S. Paliya, D. J. Saikia, C. S. Stalin, S. Muneer, Maheswar Gopinathan
Figure caption: Upper: histogram of the estimated core dominance of the NLSy1s listed in Table 2. Lower: relation between core dominance and black hole mass.
Paper: Identification of Large-scale (>100 kpc) Radio Jets in Narrow-line Seyfert 1 Galaxies
Authors: S. Umayal, Vaidehi S. Paliya, D. J. Saikia, C. S. Stalin, S. Muneer, Maheswar Gopinathan
Figure caption: Power-versus-projected-size (P–D diagram) plot of all the double-lobed NLSy1 sources >100 kpc (listed in Table 2) overlaid onto LOFAR-detected sources published in M. J. Hardcastle et al. (2023).
Paper: Observation and Modeling of Shear Evolution of Post-reconnection Flare Loops
Authors: Drake Osaben, Jiong Qiu, Dana W. Longcope
Figure caption: Top panels: post-reconnection flare loops observed in the EUV 304 Å images by AIA at different times. Bottom panels: (d)–(e) PRFLs identified from the AIA 304 Å images using the OCCULT code, superimposed on a magnetogram of the photospheric radial magnetic field obtained by the Helioseismic Magnetic Imager (HMI) at 21:00 UT. The colors indicate the times when the loops were observed in the AIA 304 Å images minus 15 minutes. (f) Evolution of flare ribbons observed in the AIA 1600 Å passband, with the colors of the contour indicating the time the ribbon pixels are brightened, as denoted in the color bar in the right. The orange curve outlines the PIL of the photospheric radial magnetic field (grayscale). All images in this figure have been rotated to 21:00 UT, and the helioprojective coordinates in the figures reflect this reference time.
Paper: Predicting Stellar Parameters of Massive Stars from Light Curves with Machine Learning
Authors: Rachel C. Zhang, Kaze W. K. Wong, Gonzalo Holgado, Matteo Cantiello
Figure caption: Spectroscopic H–R diagram comparing stellar parameter predictions from the most effective MLP and CNN models, specifically MLP2 (purple squares) and CNN1 (orange stars), against observed spectroscopic measurements of the stellar parameters (gray circles). The diagram plots effective temperature (in units of 103 K) versus spectroscopic luminosity (in units of ﹩{{\mathscr{L}}}_{\odot }﹩). Theoretical stellar evolutionary tracks from MIST (J. Choi et al. 2016) are overlaid, showing the predicted evolutionary pathways for stars with initial masses of 20–50 M⊙. The solid portions of each track indicate the main-sequence phase, while dotted segments represent post-main-sequence phases. The representative error bar in the lower left indicates the mean prediction uncertainty of the CNN1 model relative to observational data.
Paper: Predicting Stellar Parameters of Massive Stars from Light Curves with Machine Learning
Authors: Rachel C. Zhang, Kaze W. K. Wong, Gonzalo Holgado, Matteo Cantiello
Figure caption: Scatter plots in both panels compare actual and predicted values for spectroscopic luminosity (top rows), effective temperature (second rows), and surface gravity for MLP1/CNN1 (bottom row of panel (a)). Panel (a) presents results from MLP1 and CNN1 models, while panel (b) presents results from MLP2 and CNN2 models. The red line in each plot indicates perfect agreement between predicted and actual values, serving as a reference for prediction accuracy.
Paper: Observation and Modeling of Shear Evolution of Post-reconnection Flare Loops
Authors: Drake Osaben, Jiong Qiu, Dana W. Longcope
Figure caption: (a) A sample of field lines traced at various heights for a given α, overlaid on top of an AIA 304 Å image in which the (blue) observed loop is identified. (b): A side view of the same sample of field lines traced with a CEA magnetogram placed at the surface z = 0, saturated at ±300 G. In both panels, the magenta color indicates the observed loop’s center pixel, red curves show the sample of model field lines traced at various heights, and the green curve shows the modeled loop that is the best fit to observation.
Paper: Observation and Modeling of Shear Evolution of Post-reconnection Flare Loops
Authors: Drake Osaben, Jiong Qiu, Dana W. Longcope
Figure caption: (a) Histograms of repeat measurements. The red curve is the histogram of N, read from the left axis, with the green curve showing an exponential fit. The blue curve, read from the right axis, is a cumulative histogram. (b) Histograms of the twist α and its standard deviation δα of the 439 loops that are observed for more than once (N > 1).
Paper: Observation and Modeling of Shear Evolution of Post-reconnection Flare Loops
Authors: Drake Osaben, Jiong Qiu, Dana W. Longcope
Figure caption: (a) An example of several tens of observed loops in both AIA 304 and 171 Å passbands identified with the OCCULT code (red) within a time window of 4 minutes, superimposed on an AIA 304 Å image. The loop in cyan is one of the reference loops within this time window. (b) A zoomed-in view of the consolidation, showing 12 observed loops (blue) that match a model loop (green) of the longest observed loop, or reference loop (cyan), with σ ≤ σthr.
Paper: Observation and Modeling of Shear Evolution of Post-reconnection Flare Loops
Authors: Drake Osaben, Jiong Qiu, Dana W. Longcope
Figure caption: (a) An example demonstrating the error metric between an observed loop (blue) and modeled field line (red). The separation ΔY(X) is shown by vertical black lines. (b) Histogram of the fitting error σ for 2807 loops.
Paper: Observation and Modeling of Shear Evolution of Post-reconnection Flare Loops
Authors: Drake Osaben, Jiong Qiu, Dana W. Longcope
Figure caption: Top (a) and side (b) view of the model field lines of the unique reference loops. Colors indicate their α values illustrated in the color bar.
Paper: Magnetic Flux Cancellation in the Solar Atmosphere through 3D Realistic Numerical Modeling
Authors: Fernando Moreno-Insertis, Viggo H. Hansteen, Daniel Nóbrega-Siverio
Figure caption: Three-dimensional visualization of the general field-line configuration during Phase 1 using a snapshot at t = 113.3 minutes. Panel (a): Closed loops attached to the emerging bipole (purple) and field lines from the preexisting negative polarity that link to the general coronal field in the simulation (red). Panels (b) and (c): six field-line sets illustrating the reconnection process, with different colors for each set, as explained in the text. The vertical plane in panels (a) and (c) subtends an angle of 42 deg to the XZ plane and contains a colormap for ﹩{\mathrm{log}}({{L}_{{\rm{B}}}}^{-1})﹩, with LB in Mm. Panels (d) and (e): details of the upgoing and downgoing reconnected field systems, respectively. The vertical plane contains a colormap of the downflow speed in km s−1. The field lines in panel (e) are colored according to ﹩{\mathrm{log}}T﹩. Panel (f): Three recently reconnected field lines sets with vertices pointing to a common reconnection site in the region above the main photospheric magnetic patches. Colormap and -bar are as in panels (a) and (c).
Paper: Magnetic Flux Cancellation in the Solar Atmosphere through 3D Realistic Numerical Modeling
Authors: Fernando Moreno-Insertis, Viggo H. Hansteen, Daniel Nóbrega-Siverio
Figure caption: Chromospheric line profiles during the cancellation event. Vertical (Bz) magnetic field at z = 150 km (left panel), average profiles of the Ca II 854.2 nm (middle panel), and Mg II k (right panel) lines for the entire computational domain (red curve) and in the small patch centered on the cancellation site (blue curve) indicated by the blue rectangle in the left panel. The line centers of Ca II 854.2 nm and Mg II k are marked with green vertical dashed lines.
Paper: Magnetic Flux Cancellation in the Solar Atmosphere through 3D Realistic Numerical Modeling
Authors: Fernando Moreno-Insertis, Viggo H. Hansteen, Daniel Nóbrega-Siverio
Figure caption: The twisted flux rope below the post-reconnection loops. Panel (a): early stage (t = 108.3 minutes), with braided flux strands (like the yellow and red ones) below the post-reconnection loops (in green) at heights 500–700 km above the photosphere. The vertical map is for ﹩{\mathrm{log}}({L}_{{\rm{B}}}{[\,\rm{Mm}\,]}^{-1})﹩. Panel (b): intermediate stage (t = 113.3 minutes), with a twisted flux rope (in yellow) below the post-reconnection loops (in green); the vertical map is the downflow speed, in km s−1. Panel (c): final stage, at t = 115.0 minutes. Panel (d): view of the general emerged field at t = 113.3 minutes (orange), next to field lines similar to those of panel (b) (in yellow in both panels).
Paper: Magnetic Flux Cancellation in the Solar Atmosphere through 3D Realistic Numerical Modeling
Authors: Fernando Moreno-Insertis, Viggo H. Hansteen, Daniel Nóbrega-Siverio
Figure caption: Statistics on the current sheet at t = 113.3 minutes. Top: Isosurface ﹩{\mathrm{log}}({L}_{{\rm{B}}}{[\,\rm{Mm}\,]}^{-1})=1.4﹩ in the region above the colliding polarities. The vertical map is the same as in Figure 7, panels (a) or (c); the horizontal background is the magnetogram at z = 0. Center: Top view of the region selected for calculation of average quantities in the current sheet. The base of the cuboid where the high-﹩{{L}_{{\rm{B}}}}^{-1}﹩-test was carried out is delineated as a red dashed rectangle; the (x, y) locations of the pixels fulfilling the criterion are marked in green, all of them restricted to the height range (1, 3.5) Mm. Bottom: Colormap of LB[Mm]−1 on a vertical cut at y = 10.3 Mm with, superimposed, the points on the map with ﹩{{L}_{{\rm{B}}}}^{-1}\gt 1{0}^{1.5}﹩ Mm−1. The position of the vertical cut at y = 10.3 Mm has been marked in the middle panel with a white dashed line.
Paper: Magnetic Flux Cancellation in the Solar Atmosphere through 3D Realistic Numerical Modeling
Authors: Fernando Moreno-Insertis, Viggo H. Hansteen, Daniel Nóbrega-Siverio
Figure caption: View at t = 116.0 minutes of the twisted magnetic flux rope arising at the front of the expanding emerging domain (yellow). Three recently reconnected, V-shaped field-line sets are also shown colored in red, purple, and orange. The colormaps on the vertical planes are for ﹩{\mathrm{log}}({L}_{{\rm{B}}}{[\,\rm{Mm}\,]}^{-1})﹩.
Paper: Magnetic Flux Cancellation in the Solar Atmosphere through 3D Realistic Numerical Modeling
Authors: Fernando Moreno-Insertis, Viggo H. Hansteen, Daniel Nóbrega-Siverio
Figure caption: Selected field lines at t = 117.0 minutes, illustrating the reconnection process in the photospheric cancellation phase. Upper panel: field lines for three magnetic systems. Red: just-reconnected V-shaped upward-running field lines. Light blue: just-reconnected closed loops. Yellow: closed post-reconnection loops filling the space below the reconnection point down to the photosphere. Vertical plane: colormap of ﹩{\mathrm{log}}({L}_{{\rm{B}}}{[\,\rm{Mm}\,]}^{-1})﹩. Lower panel: colormap for the downflow speed (in km s−1) on a plane that cuts across the post-reconnection domain, together with simple post-reconnection loops.
Paper: Magnetic Flux Cancellation in the Solar Atmosphere through 3D Realistic Numerical Modeling
Authors: Fernando Moreno-Insertis, Viggo H. Hansteen, Daniel Nóbrega-Siverio
Figure caption: The region of supercritical downflow originating in the reconnection site. The three panels show a collection of closed reconnected loops; the colormap is for (a) the module of the velocity in km s−1(top), (b) the magnetosonic Mach number (center), and (c) the logarithm of the plasma β (bottom).
Paper: Testing the Origin of Hot Jupiters with Atmospheric Surveys
Authors: Lina D'Aoust, Ben Coull-Neveu, Eve J. Lee, Nicolas B. Cowan
Figure caption: Number of targets required to distinguish the water abundance of hot (<10 days) vs. warm (>10 days) Jupiters at 3σ (left column) and 2σ (right column) significance levels as a function of added noise, representing additional scatter in planet metallicity. We focus on the case of pebble accretion with perfect dust trap as the difference in water abundance between hot and warm Jupiters is smaller compared to the case with no dust trap. At a given level of extra noise, we run 100 iterations, reporting the median as the solid line and the 16th and 84th percentiles as the edges of the shaded regions.
Paper: High-energy Gamma Rays and Neutrinos from the Sun, Jupiter, and Earth
Authors: Pablo de la Torre, Miguel Gutiérrez, Manuel Masip, Alejandro Oliver
Figure caption: Minimum energy of a CR proton able to reach the surface of Jupiter for different values of ρ and α and for two relative orientations of the magnetic north pole. On the right is the observation angle θobs; the position of the north pole in the disk goes from ρ = 0 for θobs = 0 to ρ = 1 for θobs = π/2 and back to ρ = 0 for θobs = π, always with α = 0.
Paper: High-energy Gamma Rays and Neutrinos from the Sun, Jupiter, and Earth
Authors: Pablo de la Torre, Miguel Gutiérrez, Manuel Masip, Alejandro Oliver
Figure caption: Gamma-ray flux from the solar disk (data at E ≤ 200 GeV from Fermi-LAT, T. Linden et al. 2018, and at 1 TeV from HAWC, A. Albert et al. 2023) and our average gamma, neutron, and neutrino fluxes from the Sun.
Paper: High-energy Gamma Rays and Neutrinos from the Sun, Jupiter, and Earth
Authors: Pablo de la Torre, Miguel Gutiérrez, Manuel Masip, Alejandro Oliver
Figure caption: Matter density encountered by a particle approaching vertically the Earth, Jupiter, and the Sun after crossing a distance d (initial point at a depth of 1 g cm−2 and final point at 1000 g cm−2).
Paper: High-energy Gamma Rays and Neutrinos from the Sun, Jupiter, and Earth
Authors: Pablo de la Torre, Miguel Gutiérrez, Manuel Masip, Alejandro Oliver
Figure caption: Schematic CR trajectories in the vicinity of the Sun. As the energy grows trajectories that were supposed to reach the Earth cross a larger depth of solar matter, increasing the probability that CRs are absorbed and define a shadow.
Paper: High-energy Gamma Rays and Neutrinos from the Sun, Jupiter, and Earth
Authors: Pablo de la Torre, Miguel Gutiérrez, Manuel Masip, Alejandro Oliver
Figure caption: Trajectories of a 2 TeV proton reaching a point on the surface of Jupiter with the same zenith (θz = 60°) and different azimuths (in units of RJ, with the center of the planet at (0, 0, 0) and the north pole at (0, 0, 1)). The trajectory from the west (in dashes) is shadowed by Jupiter.
Paper: High-energy Gamma Rays and Neutrinos from the Sun, Jupiter, and Earth
Authors: Pablo de la Torre, Miguel Gutiérrez, Manuel Masip, Alejandro Oliver
Figure caption: Density profile of the each astrophysical object (r is the normalized radius) and fraction of neutrinos not absorbed through a trajectory with ρ = 0.5 (see Figure 6).
Paper: High-energy Gamma Rays and Neutrinos from the Sun, Jupiter, and Earth
Authors: Pablo de la Torre, Miguel Gutiérrez, Manuel Masip, Alejandro Oliver
Figure caption: Absorbed proton and He fluxes during a solar maximum (thick) and a solar minimum (thin). On the right are typical CR trajectories at different energies.
Paper: Comprehensive JWST+ALMA Study on the Extended Lyα Emitters, Himiko, and CR7 at z ∼ 7: Blue Major Merger Systems in Stark Contrast to Submillimeter Galaxies
Authors: Tomokazu Kiyota, Masami Ouchi, Yi Xu, Yurina Nakazato, Kenta Soga, Hidenobu Yajima, Seiji Fujimoto, Yuichi Harikane, Kimihiko Nakajima, Yoshiaki Ono, Dongsheng Sun, Haruka Kusakabe, Daniel Ceverino, Bunyo Hatsukade, Daisuke Iono, Kotaro Kohno, Kouichiro Nakanishi
Figure caption: Left: [N II] BPT diagram. Himiko and CR7 are plotted as red diamonds and magenta squares, respectively. Labels indicate clump names. Blue plots show JADES stacked results at z ≳ 6 (A. J. Cameron et al. 2023). Two demarcation curves between AGNs and star-forming galaxies are also shown as solid (L. J. Kewley et al. 2001) and dashed (G. Kauffmann et al. 2003) lines. The gray regions show the SDSS galaxy distributions (SDSS DR16; R. Ahumada et al. 2020). Middle: O32-R23 diagram. The gray-open circles show the JWST samples at z = 4–10 (K. Nakajima et al. 2023). Others are the same as the left panel. Right: gas-phase metallicities as a function of stellar mass. The solid, dashed, and dotted–dashed lines show the mass–metallicity relation based on the JWST samples at z > 4 presented in K. Nakajima et al. (2023), M. Curti et al. (2024), and K. E. Heintz et al. (2023), respectively. The gray shade represents the uncertainty of the K. E. Heintz et al. (2023) relation. The solid black curve shows the relationship in the local Universe (B. H. Andrews & P. Martini 2013). Others are the same as the two panels.
Paper: Comprehensive JWST+ALMA Study on the Extended Lyα Emitters, Himiko, and CR7 at z ∼ 7: Blue Major Merger Systems in Stark Contrast to Submillimeter Galaxies
Authors: Tomokazu Kiyota, Masami Ouchi, Yi Xu, Yurina Nakazato, Kenta Soga, Hidenobu Yajima, Seiji Fujimoto, Yuichi Harikane, Kimihiko Nakajima, Yoshiaki Ono, Dongsheng Sun, Haruka Kusakabe, Daniel Ceverino, Bunyo Hatsukade, Daisuke Iono, Kotaro Kohno, Kouichiro Nakanishi
Figure caption: Best-fit SFHs of Himiko (top) and CR7 (bottom) inferred from the SED fitting with NIRCam photometry. The orange, blue, and green lines show the best-fit SFHs of clumps A, B, and C, respectively. The shaded regions show the corresponding 1σ uncertainties.
Paper: Comprehensive JWST+ALMA Study on the Extended Lyα Emitters, Himiko, and CR7 at z ∼ 7: Blue Major Merger Systems in Stark Contrast to Submillimeter Galaxies
Authors: Tomokazu Kiyota, Masami Ouchi, Yi Xu, Yurina Nakazato, Kenta Soga, Hidenobu Yajima, Seiji Fujimoto, Yuichi Harikane, Kimihiko Nakajima, Yoshiaki Ono, Dongsheng Sun, Haruka Kusakabe, Daniel Ceverino, Bunyo Hatsukade, Daisuke Iono, Kotaro Kohno, Kouichiro Nakanishi
Figure caption: [O III]λ5007 moment maps of Himiko (top) and CR7 (bottom) obtained by NIRSpec-IFU G395H. Moment 0, 1, and 2 maps are shown from left to right. A fiducial velocity corresponds to the redshift of Himiko-C or CR7-B. We only use the spaxels of S/N > 5. Velocity dispersions are corrected for instrumental broadening. No dust-extinction correction is applied. Black contours show arbitrary [O III]λ5007 flux levels. The upper left gray circle shows the PSF FWHM around the [O III]λ5007 emission-line wavelength.
Paper: Comprehensive JWST+ALMA Study on the Extended Lyα Emitters, Himiko, and CR7 at z ∼ 7: Blue Major Merger Systems in Stark Contrast to Submillimeter Galaxies
Authors: Tomokazu Kiyota, Masami Ouchi, Yi Xu, Yurina Nakazato, Kenta Soga, Hidenobu Yajima, Seiji Fujimoto, Yuichi Harikane, Kimihiko Nakajima, Yoshiaki Ono, Dongsheng Sun, Haruka Kusakabe, Daniel Ceverino, Bunyo Hatsukade, Daisuke Iono, Kotaro Kohno, Kouichiro Nakanishi
Figure caption: Hα emission lines of Himiko (top) and CR7 (bottom), observed with NIRSpec-IFU G395H. Clumps A to C are displayed from left to right. The black histograms represent the spectra, with gray shading indicating 1σ uncertainties. The red lines show the total Gaussian fit, while the gray lines represent individual Gaussian components. For Himiko-B, the broad (FWHM∼1000 km s−1) Hα component is highlighted with the red shading (see Section 4.4).