adsabs/AstroCLIMB huggingface dataset:
Paper: Black Hole Collisions with Thin Accretion Disks: OJ 287 and Small Mass Ratio Supermassive Black Hole Binary Candidates
Authors: Sean M. Ressler, Luciano Combi, Bart Ripperda, Xinyu Li
Figure caption: The initial conditions for our single black hole, thin-disk simulation. The S. K. Chakrabarti (1985) disk is initially in hydrodynamic equilibrium threaded by a single loop of weak magnetic field such that ﹩{\rm{\max }}(P)/{\rm{\max }}({b}^{2}/2)=100﹩.
Paper: A Metal-free Galaxy at z = 3.19? Evidence of Late Population III Star Formation at Cosmic Noon
Authors: Sijia Cai, Mingyu Li, Zheng Cai, Yunjing Wu, Fujiang Yu, Mark Dickinson, Fengwu Sun, Xiaohui Fan, Ben Wang, Fergus Cullen, Fuyan Bian, Xiaojing Lin, Jiaqi Zou
Figure caption: Multiwavelength images and spectral energy distribution (SED) modeling of CR3. Upper: cutout stamps of CR3 from Subaru/Suprime IA505; Subaru/HSC g, r, and i; and JWST/NIRCam F090W, F115W, F150W, F200W, F277W, F356W, F410M, and F444W. The cutout image size is 4″ for Subaru and 1″ for JWST. Lower: SED modeling of CR3. The best-fit Pop III SED model is shown as a black curve, with model photometry (blue squares) and observed photometry (red circles) overlaid. The 2σ upper limits in the U, B, z, and y bands are indicated by red arrows. The Lyα emission boosts the fluxes in the IA505 and HSC g bands; Hα emission boosts the F277W band; and He I emission enhances the F444W band.
Paper: A Metal-free Galaxy at z = 3.19? Evidence of Late Population III Star Formation at Cosmic Noon
Authors: Sijia Cai, Mingyu Li, Zheng Cai, Yunjing Wu, Fujiang Yu, Mark Dickinson, Fengwu Sun, Xiaohui Fan, Ben Wang, Fergus Cullen, Fuyan Bian, Xiaojing Lin, Jiaqi Zou
Figure caption: Constraints on the gas-phase metallicity of CR3. Left: we apply the R. L. Sanders et al. (2024) strong-line calibration to the measured upper limit on the R3 ratio ([O III] λ5007/Hβ; blue curve). For comparison, metallicity calibration curves from M. Hirschmann et al. (2023) and K. Nakajima et al. (2022) are presented. The dashed–dotted extensions indicate the extrapolated regimes of the calibrations. Our measurement is compared to other known spectroscopically confirmed Pop III candidates or extremely metal-poor galaxies (EMPGs), including the LAP1 stellar complex (orange hexagon, E. Vanzella et al. 2023), the LAP1-B clump (orange hexagon, K. Nakajima et al. 2025), the LAP2-b stellar complex (yellow square, E. Vanzella et al. 2025), the AMORE6-A+B (gray diamond, T. Morishita et al. 2025), the GNHeII J1236+6215 (green circle, C. Mondal et al. 2025), the CANUCS-A370-z8-LAE (purple pentagon, C. J. Willott et al. 2025), the EXCELS-63107 (pink triangle, F. Cullen et al. 2025), and the SAPPHIRES EMPGs (blue diamond, T. Y.-Y. Hsiao et al. 2025). Light gray markers show samples from the MOSDEF (R. L. Sanders et al. 2020), the CEERS (R. L. Sanders et al. 2024), the JADES and the PRIMAL (P. Chakraborty et al. 2025), and the EXCELS (D. Scholte et al. 2025). Right: redshift-metallicity distribution of the sample, highlighting the extremely low metallicity of CR3 compared to other galaxies at similar and higher redshifts. All limits shown represent 1σ upper bounds. The red rectangle indicates the systematic uncertainty associated with the strong-line calibration discussed in Section 4.1.
Paper: A Metal-free Galaxy at z = 3.19? Evidence of Late Population III Star Formation at Cosmic Noon
Authors: Sijia Cai, Mingyu Li, Zheng Cai, Yunjing Wu, Fujiang Yu, Mark Dickinson, Fengwu Sun, Xiaohui Fan, Ben Wang, Fergus Cullen, Fuyan Bian, Xiaojing Lin, Jiaqi Zou
Figure caption: JWST and VLT observation of CR3. Upper left: pseudocolor composite image constructed from JWST/NIRCam images, using blue (F115W, F150W), green (F200W, F277W), and red (F356W, F444W) channels. The orientation of the MSA shutters is indicated by the white region. Upper right: JWST/NIRSpec prism 2D and 1D spectra. The red dashed lines indicate the optimal extraction aperture on the 2D spectrum. In the 1D panel, the black solid line shows the flux, while the red dotted line shows the associated error. The Hα and He I λ10830 emission features are highlighted with blue shaded regions. Lower: 1D VLT/MUSE spectrum extracted from a circular aperture, rebinned and Hanning-smoothed. The black solid line shows the flux, and the red dotted line indicates the error. The Subaru/HSC r-band continuum level is overplotted as a gray dashed line. The Lyα emission line is highlighted with a blue shaded region. Strong sky emission lines are marked with light gray shaded areas. Hydrogen and helium emission lines are labeled in blue, while metal lines are labeled in red.
Paper: A Metal-free Galaxy at z = 3.19? Evidence of Late Population III Star Formation at Cosmic Noon
Authors: Sijia Cai, Mingyu Li, Zheng Cai, Yunjing Wu, Fujiang Yu, Mark Dickinson, Fengwu Sun, Xiaohui Fan, Ben Wang, Fergus Cullen, Fuyan Bian, Xiaojing Lin, Jiaqi Zou
Figure caption: Large-scale environment of CR3. The background shows the galaxy overdensity field at z = 3.2 ± 0.1 based on COSMOS2025 LePhare photometric redshifts, with red (blue) indicating overdense (underdense) regions. Masked regions are shown in white.
Paper: Induction Heating in Super-Earths: A Thermochemical Perspective
Authors: Yihang Peng, Kristina Kislyakova, Donghao Zheng, Zhongtian Zhang, Jie Deng
Figure caption: Color maps and contour plots of three metrics of induction heating efficiency as a function of potential temperature and mantle Fe contents (XFe) in GJ 486b ((a)–(c)), HD 3167b ((d)–(f)), and GJ 357b ((g)–(i)). ((a), (d), and (g)) Total induction heating power inside the planet; ((b), (e), and (h)) Maximum depth-dependent energy release per unit mass; ((c), (f), and (i)) Depth of the partially molten mantle layer that has an energy release exceeding the critical value of 10−11 W kg−1. The white dashed lines mark the equilibrium temperature of HD 3167b (1759 K; K. Kislyakova & L. Noack 2020).
Paper: Induction Heating in Super-Earths: A Thermochemical Perspective
Authors: Yihang Peng, Kristina Kislyakova, Donghao Zheng, Zhongtian Zhang, Jie Deng
Figure caption: ((a) and (b)) Energy release due to induction heating as a function of depth in HD 3167b (a) and GJ 486b (b) with the presence of mantle partial melting with different potential temperatures. ((c) and (d)) The depth of the partial melt that can be sustained by induction heating in HD 3167b (c) and GJ 486b (d). ((e) and (f)) The surface heat flux produced by induction heating as a function of potential temperature in HD 3167b (e) and GJ 486b (f). The energy release due to tidal heating in Io (V. Lainey et al. 2009) is shown for comparison in (f). The gray curves labeled 1E-10 adopt a high critical threshold of 10−10 W kg−1 for mantle partial melting. All other calculations use a threshold value of 10−11 W kg−1. The pink and gray curves in panel (f) almost overlap. The mantle iron content is set to be an Earth-like value of 11 mol%.
Paper: Induction Heating in Super-Earths: A Thermochemical Perspective
Authors: Yihang Peng, Kristina Kislyakova, Donghao Zheng, Zhongtian Zhang, Jie Deng
Figure caption: Energy release per unit mass due to induction heating as a function of depth inside GJ 486b, considering different potential temperatures (a) and Fe fraction (XFe) in mantle silicates (b). The critical value of energy release that can keep the mantle rock molten (10−11 W kg−1) and its plausible range (K. G. Kislyakova et al. 2018; E. W. Guenther & K. G. Kislyakova 2020) are shown as dashed lines and shaded regions, respectively.
Paper: Induction Heating in Super-Earths: A Thermochemical Perspective
Authors: Yihang Peng, Kristina Kislyakova, Donghao Zheng, Zhongtian Zhang, Jie Deng
Figure caption: Mantle conductivity profiles for a 4 M⊕ super-Earth with an Earth-like core mass fraction (0.32). (a) Conductivity profiles with various potential temperatures. (b) Conductivity profiles with various Fe fractions (XFe) in mantle silicates.
Paper: On-sky Demonstration of Subdiffraction-limited Astronomical Measurement Using a Photonic Lantern
Authors: Yoo Jung Kim, Michael P. Fitzgerald, Sébastien Vievard, Jonathan Lin, Yinzi Xin, Miles Lucas, Olivier Guyon, Julien Lozi, Vincent Deo, Elsa Huby, Sylvestre Lacour, Manon Lallement, Rodrigo Amezcua-Correa, Sergio Leon-Saval, Barnaby Norris, Mathias Nowak, Steph Sallum, Jehanne Sarrazin, Adam Taras, Stephanos Yerolatsitis, Nemanja Jovanovic
Figure caption: Simulated response maps and their derivatives for standard and mode-selective three-port PLs. (a) Example response maps (﹩{M}_{0i}^{{\prime} }﹩) of mode-selective (left) and standard (right) three-port PLs. A random unitary matrix is used to simulate standard PL responses. The maps are normalized such that ﹩{\sum }_{i=1}^{3}{M}_{0i}^{{\prime} }=1﹩. (b) Gradients of ﹩{M}_{0i}^{{\prime} }﹩ along x. While the mode-selective PL exhibits zeros at the center, the standard PL has substantial gradients. (c) Second-order derivatives of ﹩{M}_{0i}^{{\prime} }﹩ along x. A large second-order derivative and zero intensity at (0, 0) for the LP11a port of the mode-selective PL suggests nonzero Fisher information at the small separation limit (Equation (G10)).
Paper: Dual-band Ion-scale Waves in the Solar Wind: Statistical Properties and Comparison with Single-band Ion-scale Waves
Authors: Sung Jun Noh, Dae-Young Lee, Xiangrong Fu, Fan Guo, Misa M. Cowee, Lan K. Jian, Ilya Kuzichev, Jungjoon Seough, John T. Steinberg, Ruth M. Skoug, Daniel B. Reisenfeld, Jia Huang, Kyung-Eun Choi, Xiaocan Li, Jaye L. Verniero
Figure caption: Statistical properties of the background magnetic field. The same colors are used for each category as Figure 2, and the entire PSP observation is included in black. Panels show (a)–(b) magnetic field intensity, (c)–(d) angle between the magnetic field and the radial direction, and (e)–(f) magnetic compressibility. The left column presents the radial distribution of each parameter, while the right column shows histograms compiled only between 0.15 and 0.3 au, where DBIW occurrence peaks. The histograms are normalized by maximum values. The error bars represent 16th and 84th quantiles. Numbers in panels (b), (d), and (f) give median values between 0.15 and 0.3 au for each category.
Paper: Dual-band Ion-scale Waves in the Solar Wind: Statistical Properties and Comparison with Single-band Ion-scale Waves
Authors: Sung Jun Noh, Dae-Young Lee, Xiangrong Fu, Fan Guo, Misa M. Cowee, Lan K. Jian, Ilya Kuzichev, Jungjoon Seough, John T. Steinberg, Ruth M. Skoug, Daniel B. Reisenfeld, Jia Huang, Kyung-Eun Choi, Xiaocan Li, Jaye L. Verniero
Figure caption: Spatial distribution of all SBIWs (blue), L-mode (gold), R-mode (green), and DBIWs (red). Occurrence rates are shown as functions of (a) radial distribution and (b) HG latitude. The occurrence rates are calculated as the ratio of the total event duration to the spacecraft’s dwell time in each spatial bin. The values shown in (a) and (b) are further normalized to their respective maximum occurrence rates. Panels (c) and (d) show events on the PSP trajectory as a function of time in terms of radial distance and distance from the solar equator, respectively. Vertical dashed lines mark the times of perihelia. Panel (e) shows event distributions projected onto the meridional plane. In panels (c) to (e), the same color scheme for the different event hours is used as in panels (a) and (b). Only DBIWs are presented in stars, and L- and R-modes are presented in dot. Note that L- and R-modes reassemble SBIWs.
Paper: Dual-band Ion-scale Waves in the Solar Wind: Statistical Properties and Comparison with Single-band Ion-scale Waves
Authors: Sung Jun Noh, Dae-Young Lee, Xiangrong Fu, Fan Guo, Misa M. Cowee, Lan K. Jian, Ilya Kuzichev, Jungjoon Seough, John T. Steinberg, Ruth M. Skoug, Daniel B. Reisenfeld, Jia Huang, Kyung-Eun Choi, Xiaocan Li, Jaye L. Verniero
Figure caption: Statistical analysis of inertial-range spectral index (﹩\gamma ﹩). (a)–(b) Parallel components, (c)–(d) perpendicular components, and (e)–(f) the ratio between the two components, ﹩{\gamma }_{\perp }/{\gamma }_{\parallel }﹩. Reference lines for ﹩\gamma =3/2﹩ and ﹩5/3﹩ (gray dashed lines) are included in panels (a)–(d).
Paper: Limits on Stellar Flybys in the Solar Birth Cluster
Authors: Amir Siraj, Christopher F. Chyba, Scott Tremaine
Figure caption: Fraction of flyby histories that are compatible with the observed inclination distribution of cold classicals as a function of number of flybys with impact parameter <104 au. The initial condition for the inclination distribution is a Rayleigh distribution with a mode of 1﹩\mathop{.}\limits^{\unicode{x000b0}}﹩7. The resulting upper limit on χ, if we adopt a KS test threshold of p1 = 0.05 and require at least p2 = 0.05 of all simulations to exceed this threshold in order to remain compatible, is ≲6 × 104 Myr pc−3. The fraction starts near 1 because the KS test is relative to an assumed distribution of inclinations that matches the initial distribution.
Paper: Dual-band Ion-scale Waves in the Solar Wind: Statistical Properties and Comparison with Single-band Ion-scale Waves
Authors: Sung Jun Noh, Dae-Young Lee, Xiangrong Fu, Fan Guo, Misa M. Cowee, Lan K. Jian, Ilya Kuzichev, Jungjoon Seough, John T. Steinberg, Ruth M. Skoug, Daniel B. Reisenfeld, Jia Huang, Kyung-Eun Choi, Xiaocan Li, Jaye L. Verniero
Figure caption: Statistical analysis of the inertial-range spectral intensity (A), presented in the same format as Figure 4.
Paper: Dual-band Ion-scale Waves in the Solar Wind: Statistical Properties and Comparison with Single-band Ion-scale Waves
Authors: Sung Jun Noh, Dae-Young Lee, Xiangrong Fu, Fan Guo, Misa M. Cowee, Lan K. Jian, Ilya Kuzichev, Jungjoon Seough, John T. Steinberg, Ruth M. Skoug, Daniel B. Reisenfeld, Jia Huang, Kyung-Eun Choi, Xiaocan Li, Jaye L. Verniero
Figure caption: Example of a DBIW event observed on 2019 August 26. (a) Ellipticity (L-mode in blue and R-mode in red), (b) WNA, (c) identified waves, satisfying ellipticity, WNA, and DOP criteria, shown in red, (d) perpendicular component of the power spectral density, and (e) vector magnetic field in the RTN coordinate system. The black and gray horizontal lines in panels (a)–(d) indicate the local proton gyrofrequency (fcH+). This figure is adapted from Figure A1 in S. J. Noh et al. (2025).
Paper: Limits on Stellar Flybys in the Solar Birth Cluster
Authors: Amir Siraj, Christopher F. Chyba, Scott Tremaine
Figure caption: Example of inclination, perihelion, and semimajor axis evolution for each of the nine TNOs (median values in bold, individual clones in the background) in an individual simulation. Clones are only plotted and taken into the median calculation if they instantaneously pass the mask described in the text.
Paper: Limits on Stellar Flybys in the Solar Birth Cluster
Authors: Amir Siraj, Christopher F. Chyba, Scott Tremaine
Figure caption: Fraction of flyby histories that are compatible with the observed inclination distribution of distant sednoids (initial inclinations are set to zero) as a function of number of flybys with impact parameter <104 au. The resulting upper limit on χ, if we adopt a KS test threshold of p1 = 0.05 and require at least p2 = 0.05 of all simulations to exceed this threshold in order to remain compatible, is ≲5 × 103 Myr pc−3. The fraction starts near zero because the initial inclinations are set at zero.
Paper: Onset of CN Emission in 3I/ATLAS: Evidence for Strong Carbon-chain Depletion
Authors: Luis E. Salazar Manzano, Hsing Wen Lin, 省文 林, Aster G. Taylor, Darryl Z. Seligman, Fred C. Adams, David W. Gerdes, Thomas Ruch, Tessa T. Frincke, Kevin J. Napier
Figure caption: Comparison of carbon-chain to CN ratio and gas-to-dust ratio constraints for interstellar and solar system comets. Left: logarithmic C2/CN ratio as a function of heliocentric distance. The white and black circle with a downward-pointing arrow marks our upper limit for 3I/ATLAS, while the orange squares indicate, in order of decreasing distance, the measurements for 2I/Borisov reported by H. W. Lin et al. (2020), M. T. Bannister et al. (2020), and K. Aravind et al. (2021). Points show measurements of solar system comets from the D. J. Osip et al. (2010) database, with red points corresponding to Jupiter-family (JF) comets, green points to Halley-type (HT) comets, and blue points to long-period comets (LPC). The horizontal dotted line separates typical from carbon-chain-depleted comets. Middle: logarithmic C3/CN ratio versus heliocentric distance. Right: logarithmic gas-to-dust ratio versus heliocentric distance. Formatting in the middle and right panels follows the left panel, with only the K. Aravind et al. (2021) measurement for 2I/Borisov shown. The white and black circle in the right panel represents our measured value for 3I/ATLAS (not an upper limit).
Paper: Onset of CN Emission in 3I/ATLAS: Evidence for Strong Carbon-chain Depletion
Authors: Luis E. Salazar Manzano, Hsing Wen Lin, 省文 林, Aster G. Taylor, Darryl Z. Seligman, Fred C. Adams, David W. Gerdes, Thomas Ruch, Tessa T. Frincke, Kevin J. Napier
Figure caption: Measured brightness and expected brightness evolution of 3I/ATLAS. The expected curve shows the estimated development of the comet’s brightness based on previous observations, fitted to data from the Comet Observations Database and the Minor Planet Center.
Paper: Return of the Clocked Burster: Exceptionally Short Recurrence Time in GS 1826−238
Authors: Tomoshi Takeda, Toru Tamagawa, Teruaki Enoto, Wataru Iwakiri, Akira Dohi, Tatehiro Mihara, Hiromitsu Takahashi, Chin-Ping Hu, Amira Aoyama, Naoyuki Ota, Satoko Iwata, Takuya Takahashi, Kaede Yamasaki, Takayuki Kita, Soma Tsuchiya, Yosuke Nakano, Mayu Ichibakase, Nobuya Nishimura
Figure caption: (a) Variations of (a-1) burst recurrence time, (a-2) burst fluence, (a-3) α-value, and (a-4) blackbody normalization Kbb as a function of the bolometric persistent flux in the 0.1–1000 keV range. The dotted curve in panel (a-1) represents an empirical fit to the data from D. K. Galloway et al. (2017) (open black circles), assuming ﹩{t}_{{\rm{rec}}}\propto {F}_{{\rm{per}}}^{-1.05}﹩ (D. K. Galloway et al. 2004). Panels (a-2) and (a-4) include linear fits to the same subset of data. The blue triangles represent the data from the 2003 April epoch reported by T. W. J. Thompson et al. (2008), while the red squares show the results from the 2025 June epoch. In both cases, open and filled markers correspond to spectral fits without and with an additional disk blackbody component below 2 keV, respectively (see Section 3.3 for details). For the three previous epochs, Kbb values are the mean and standard deviation over 20–50 s after each burst onset, based on Figure 3(c). For the 2025 June epoch, Kbb is derived from a spectral fit over the same interval. (b) Fboltrec plotted against Kbb during the burst tail. The black dotted line represents the best-fit linear model (Fboltrec = aKbb) to all data points excluding the 2025 June epoch results with an additional soft component, yielding a = 0.388 ± 0.009 ﹩{({R}_{{\rm{km}}}/{D}_{10})}^{-2}﹩erg cm−2 and χ2/degrees of freedom = 5.01/3.
Paper: Return of the Clocked Burster: Exceptionally Short Recurrence Time in GS 1826−238
Authors: Tomoshi Takeda, Toru Tamagawa, Teruaki Enoto, Wataru Iwakiri, Akira Dohi, Tatehiro Mihara, Hiromitsu Takahashi, Chin-Ping Hu, Amira Aoyama, Naoyuki Ota, Satoko Iwata, Takuya Takahashi, Kaede Yamasaki, Takayuki Kita, Soma Tsuchiya, Yosuke Nakano, Mayu Ichibakase, Nobuya Nishimura
Figure caption: (a) NinjaSat light curves of GS 1826−238 in 2–10 keV, 10–20 keV, and their hardness ratio with a bin size of 1.5 hr. The time intervals between 50 s before and 300 s after the burst onset are excluded to show the persistent flux, while these burst onsets are indicated by black vertical lines in each panel. (b) MAXI/GSC light curve in the 2–20 keV energy range with 1 day bins, downloaded from the MAXI on-demand archive (T. Mihara et al. 2024). (c) Same as (b), but zoomed in on the latter part. This period is highlighted in panel (b) by the shaded teal region, while the shaded gray region corresponds to the NinjaSat observation interval. (d) Color–color diagram observed during the NinjaSat observation campaign with a bin size of 6.0 hr. The IDs of the observed bursts are indicated at corresponding data points.
Paper: Return of the Clocked Burster: Exceptionally Short Recurrence Time in GS 1826−238
Authors: Tomoshi Takeda, Toru Tamagawa, Teruaki Enoto, Wataru Iwakiri, Akira Dohi, Tatehiro Mihara, Hiromitsu Takahashi, Chin-Ping Hu, Amira Aoyama, Naoyuki Ota, Satoko Iwata, Takuya Takahashi, Kaede Yamasaki, Takayuki Kita, Soma Tsuchiya, Yosuke Nakano, Mayu Ichibakase, Nobuya Nishimura
Figure caption: Evolution of the blackbody components during the type I X-ray burst from time-resolved spectroscopy, including data from the previous three clocked bursting epochs (D. K. Galloway et al. 2017; https://burst.sci.monash.edu/reference). (a) bolometric (0.1–200 keV) unabsorbed flux in units of 10−8 erg cm−2 s−1; (b) blackbody temperature, kTbb (keV); (c) blackbody normalization, Kbb ﹩{({R}_{{\rm{km}}}/{D}_{10})}^{2}﹩, where Rkm represents the source radius in kilometers and D10 indicates the distance to the source in units of 10 kpc; (d) reduced C-statistic value for the fit.
Paper: Return of the Clocked Burster: Exceptionally Short Recurrence Time in GS 1826−238
Authors: Tomoshi Takeda, Toru Tamagawa, Teruaki Enoto, Wataru Iwakiri, Akira Dohi, Tatehiro Mihara, Hiromitsu Takahashi, Chin-Ping Hu, Amira Aoyama, Naoyuki Ota, Satoko Iwata, Takuya Takahashi, Kaede Yamasaki, Takayuki Kita, Soma Tsuchiya, Yosuke Nakano, Mayu Ichibakase, Nobuya Nishimura
Figure caption: Average energy spectra of the persistent emission (blue circles) and burst emission (pink crosses) in the hard state (IDs 1–14 except 10), along with their respective best-fit models (top), and the corresponding data-to-model ratios (bottom). The burst spectrum was extracted using the interval 10–20 s after burst onset and rebinned to maintain a minimum significance of 5σ per bin for display purposes.
Paper: On-sky Demonstration of Subdiffraction-limited Astronomical Measurement Using a Photonic Lantern
Authors: Yoo Jung Kim, Michael P. Fitzgerald, Sébastien Vievard, Jonathan Lin, Yinzi Xin, Miles Lucas, Olivier Guyon, Julien Lozi, Vincent Deo, Elsa Huby, Sylvestre Lacour, Manon Lallement, Rodrigo Amezcua-Correa, Sergio Leon-Saval, Barnaby Norris, Mathias Nowak, Steph Sallum, Jehanne Sarrazin, Adam Taras, Stephanos Yerolatsitis, Nemanja Jovanovic
Figure caption: The observation setup and data processing procedure. (a) A simplified diagram of the observation setup. After two-stage AO correction of the light collected by the Subaru Telescope, the visible light is directed to the FIRST-PL module recording spectrally dispersed outputs of the 19-port PL, and the infrared light is sent to a high-speed detector at the focal plane with an H-band filter in. (b) Example H-band PSF and corresponding PL spectrum. The PSF peak location (x*, y*) is measured from each H-band focal-plane frame and is associated with the corresponding PL spectrum frame. (c) Frame-sorting procedure. The PL spectrum data are binned by the PSF peak locations, with a resolution of 15 × 15 spanning 48.6 mas. (d) Reconstructed PL response maps. Each port’s response map exhibits a unique response, with gradual variation across wavelengths. The model responses are constructed by masking the Hα wavelength range (where spatial signals are expected) and fitting the measured response maps with polynomial functions, then interpolating the coefficients in the masked wavelength range. Spectral-differential spatial signals are identified as deviations of the response maps from the model. (e) Model reference response maps, which correspond to the response maps of a point-like source. (f) Image reconstruction is achieved by solving for the intensity distribution that, when convolved with the reference response maps, best describes the measured response maps. The first and second moments can be estimated by modeling the image as a point source and a 2D Gaussian, respectively. Without any simplifying models, nonparametric image reconstruction can be achieved.