adsabs/AstroCLIMB huggingface dataset:
Paper: Microwave Imaging Spectroscopy Diagnosis of the Slow-rise Precursor of a Major Solar Eruption
Authors: Yuankun Kou, Xin Cheng, Sijie Yu, Yingjie Luo, Bin Chen, Mingde Ding
Figure caption: (a) Composite of the AIA 131 Å (green), 171 Å (red), and 304 Å (blue) images showing the preeruptive hot channel. The white dashed line labels the slit used for creating the height–time plot in Figure 3. (b) The HMI BLOS magnetogram covered with the 131 Å contours (in cyan, at the levels of 70% and 90%, 17:26:32 UT) and 1600 Å contours (in dark red, greater than 20% of the maximum value within the field of view shown in the panel at 17:26:40 UT). Positive (P1 and P2) and negative footpoints (N1 and N2) are labeled in orange. (c) GOES SXR 1–8 Å curve and its derivative curve (5 s smoothed). (d) EOVSA total-power dynamic spectrum during the flare. (e) Microwave flux curves at five frequencies (5 s smoothed), extracted from the above total-power dynamic spectrum. The vertical dashed lines in panels (c)–(e) label the approximate time (around 17:28:30 UT) when the precursor phase transits to the main phase. The vertical dotted lines mark the four time instances as in Figure 4.
Paper: Microwave Imaging Spectroscopy Diagnosis of the Slow-rise Precursor of a Major Solar Eruption
Authors: Yuankun Kou, Xin Cheng, Sijie Yu, Yingjie Luo, Bin Chen, Mingde Ding
Figure caption: (a) AIA 131 Å images showing the evolution of the hot channel. The color is reversed to highlight the hot channel. The solid and dashed white contours show the LOS magnetic field of +500 G and −500 G, respectively. (b) Same as panels (a), but covered by the 1600 Å brightenings (in dark red, greater than 20% of the maximum value) to highlight the footpoints of the hot channel and precursor loops, which are delineated by the dashed lines in different colors. The green (blue) lines are sheared magnetic field lines connecting N1 and P2 (N2 and P1), the red lines are the reconnected precursor/flare loops, and the yellow lines are the reconnected hot channel or the erupting MFR. (c) and (d) DEM-averaged temperature and total EM maps.
Paper: Microwave Imaging Spectroscopy Diagnosis of the Slow-rise Precursor of a Major Solar Eruption
Authors: Yuankun Kou, Xin Cheng, Sijie Yu, Yingjie Luo, Bin Chen, Mingde Ding
Figure caption: (a) Height–time plot of the AIA 131 Å images. Orange points mark the leading front of the rising hot channel. The errors are set as five pixels (2.18 Mm). (b) Speed–time profile calculated from the height–time profile in panel (a). A microwave flux curve at 5.5 GHz is overplotted as a thin blue curve.
Paper: Dynamics of Reconnection Nanojets in Eruptive and Confined Solar Flares
Authors: Annu Bura, Arpit Kumar Shrivastav, Ritesh Patel, Tanmoy Samanta, Sushree S Nayak, Ananya Ghosh, Shanwlee Sow Mondal, Vaibhav Pant, Daniel B. Seaton
Figure caption: Panel (A): NFFF-extrapolated magnetic field lines overlaid on the vertical magnetic field component (Bz) of AR 13465, shown in grayscale, for the confined flare event at 09:00 UT. Panel (B): zoomed-in view of the orange box in panel (A), highlighting the region where nanoflare ejections were observed. Panel (C): NFFF-extrapolated field lines plotted over AR 13842 for the eruptive flare event at 23:36 UT, near the site of the filament eruption. Panel (D): side view of the extrapolated magnetic field configuration shown in panel (C). The orange and green boxes in panels (A) and (C) indicate the regions used for estimating magnetic twist and mean energy density. The x-, y-, and z-directions are indicated at the bottom of panel (A).
Paper: EP250108a/SN 2025kg: A Jet-driven Stellar Explosion Interacting with Circumstellar Material
Authors: Gokul P. Srinivasaragavan, Hamid Hamidani, Genevieve Schroeder, Nikhil Sarin, Anna Y. Q. Ho, Anthony L. Piro, S. Bradley Cenko, Shreya Anand, Jesper Sollerman, Daniel A. Perley, Keiichi Maeda, Brendan O'Connor, Hanindyo Kuncarayakti, M. Coleman Miller, Tomás Ahumada, Jada L. Vail, Paul Duffell, Ranadeep Dastidar, Igor Andreoni, Aleksandra Bochenek, Seán. J. Brennan, Jonathan Carney, Ping Chen, James Freeburn, Avishay Gal-Yam, Wynn Jacobson-Galán, Mansi M. Kasliwal, Jiaxuan Li, 嘉轩 李, Maggie L. Li, Niharika Sravan, Daniel E. Warshofsky
Figure caption: Light curve of SN 2025kg in the g, r, and i bands connected with a curve, where all measurements have been corrected for Milky Way extinction and times are in the observer frame. Open circles are photometry points taken from GCNs, while filled circles are photometry taken from our observations. For comparison, we show the B- and V-band light curves of SN 2006aj (M. Modjaz et al. 2006; F. B. Bianco et al. 2014; P. J. Brown et al. 2014), also corrected for Milky Way extinction, transformed to the redshift of SN 2025kg (z = 0.176). We also show the absolute magnitudes on the right axes. SN 2025kg’s light curve displays very similar features to SN 2006aj, though it is more luminous and evolves more slowly.
Paper: Dynamics of Reconnection Nanojets in Eruptive and Confined Solar Flares
Authors: Annu Bura, Arpit Kumar Shrivastav, Ritesh Patel, Tanmoy Samanta, Sushree S Nayak, Ananya Ghosh, Shanwlee Sow Mondal, Vaibhav Pant, Daniel B. Seaton
Figure caption: Examples of nanoflare ejections observed in both confined and eruptive solar flare events. Row (A)—left: outward-directed nanoflare eruption during a confined flare, observed in HRIEUI 174 Å passband at 09:05:56 UT. Middle: persistence map showing the eruption trajectory. Right: distance–time map along the red artificial slit (arrow indicates slit direction); the blue dotted line traces the bright ridge used to estimate the eruption speed. Row (B): inward-directed nanoflare eruption during a confined flare at 09:11:50 UT, with similar analysis as in panels of row (A). Row (C): outward-directed nanoflare eruption during an eruptive flare at 23:44:12 UT. Row (D): inward-directed nanoflare eruption during an eruptive flare at 23:46:00 UT. The black contour marks a 2σ intensity contour used to estimate the length and width of nanoflare ejections.
Paper: Dynamics of Reconnection Nanojets in Eruptive and Confined Solar Flares
Authors: Annu Bura, Arpit Kumar Shrivastav, Ritesh Patel, Tanmoy Samanta, Sushree S Nayak, Ananya Ghosh, Shanwlee Sow Mondal, Vaibhav Pant, Daniel B. Seaton
Figure caption: Panels (A)–(E): histograms showing the distribution of speed, length, width, duration, and kinetic energy for 59 nanoflare ejections observed during the D1 and D2 observation periods from Solar Orbiter/HRI, with the number of nanoflare ejections on the y-axis and the respective parameters on the x-axis. Panel (F) shows the kinetic energy and speed scatterplot for 89 nanoflare ejections, including 59 from our study (depicted as circles with black outlines), 10 from R. Patel & V. Pant (2022) and 20 from A. R. C. Sukarmadji et al. (2022), where we can clearly see the bifurcation of the distribution of kinetic energy of nanoflare ejections with speeds: confined ejections (blue-shaded region) occupy the lower-speed regime, while eruptive ejections (red-shaded region) exhibit higher speeds.
Paper: EP250108a/SN 2025kg: A Jet-driven Stellar Explosion Interacting with Circumstellar Material
Authors: Gokul P. Srinivasaragavan, Hamid Hamidani, Genevieve Schroeder, Nikhil Sarin, Anna Y. Q. Ho, Anthony L. Piro, S. Bradley Cenko, Shreya Anand, Jesper Sollerman, Daniel A. Perley, Keiichi Maeda, Brendan O'Connor, Hanindyo Kuncarayakti, M. Coleman Miller, Tomás Ahumada, Jada L. Vail, Paul Duffell, Ranadeep Dastidar, Igor Andreoni, Aleksandra Bochenek, Seán. J. Brennan, Jonathan Carney, Ping Chen, James Freeburn, Avishay Gal-Yam, Wynn Jacobson-Galán, Mansi M. Kasliwal, Jiaxuan Li, 嘉轩 李, Maggie L. Li, Niharika Sravan, Daniel E. Warshofsky
Figure caption: Bolometric luminosity LC of SN 2025kg, compared to SN 2006aj (M. Modjaz et al. 2006; F. B. Bianco et al. 2014; P. J. Brown et al. 2014), SN 2020bvc (A. Y. Q. Ho et al. 2020), and SN 2018gep (A. Y. Q. Ho et al. 2019; S.-C. Leung et al. 2021; T. A. Pritchard et al. 2021), with times in the rest frame. SN 2025kg’s bolometric luminosity LC has a very similar shape to that of SN 2006aj and SN 2020bvc while being more luminous and evolving on a slightly slower timescale. SN 2018gep does not have a double peak and has a higher initial luminosity, but it has a more rapid decline in luminosity over time.
Paper: Dynamics of Reconnection Nanojets in Eruptive and Confined Solar Flares
Authors: Annu Bura, Arpit Kumar Shrivastav, Ritesh Patel, Tanmoy Samanta, Sushree S Nayak, Ananya Ghosh, Shanwlee Sow Mondal, Vaibhav Pant, Daniel B. Seaton
Figure caption: The blue histogram shows the distribution of kinetic energies of the 59 nanoflare ejections identified in this study. The red dashed line indicates a reference power-law distribution with a slope of −1.79, based on the statistical analysis of EUV flares by M. J. Aschwanden et al. (2000).
Paper: EP250108a/SN 2025kg: A Jet-driven Stellar Explosion Interacting with Circumstellar Material
Authors: Gokul P. Srinivasaragavan, Hamid Hamidani, Genevieve Schroeder, Nikhil Sarin, Anna Y. Q. Ho, Anthony L. Piro, S. Bradley Cenko, Shreya Anand, Jesper Sollerman, Daniel A. Perley, Keiichi Maeda, Brendan O'Connor, Hanindyo Kuncarayakti, M. Coleman Miller, Tomás Ahumada, Jada L. Vail, Paul Duffell, Ranadeep Dastidar, Igor Andreoni, Aleksandra Bochenek, Seán. J. Brennan, Jonathan Carney, Ping Chen, James Freeburn, Avishay Gal-Yam, Wynn Jacobson-Galán, Mansi M. Kasliwal, Jiaxuan Li, 嘉轩 李, Maggie L. Li, Niharika Sravan, Daniel E. Warshofsky
Figure caption: LT images of EP250108a/SN 2025kg. The large left panel shows the wider field of view of EP250108a in the r band 9.3 days after T0. The right panels show the observations taken in the g, r, and i bands, as well as the Pan-STARRS1 templates used for photometry. The host galaxy is faint (r ∼ 23.2; A. Dey et al. 2019), so image subtraction is not necessary until the final epoch. Images have been smoothed for display purposes.
Paper: EP250108a/SN 2025kg: A Jet-driven Stellar Explosion Interacting with Circumstellar Material
Authors: Gokul P. Srinivasaragavan, Hamid Hamidani, Genevieve Schroeder, Nikhil Sarin, Anna Y. Q. Ho, Anthony L. Piro, S. Bradley Cenko, Shreya Anand, Jesper Sollerman, Daniel A. Perley, Keiichi Maeda, Brendan O'Connor, Hanindyo Kuncarayakti, M. Coleman Miller, Tomás Ahumada, Jada L. Vail, Paul Duffell, Ranadeep Dastidar, Igor Andreoni, Aleksandra Bochenek, Seán. J. Brennan, Jonathan Carney, Ping Chen, James Freeburn, Avishay Gal-Yam, Wynn Jacobson-Galán, Mansi M. Kasliwal, Jiaxuan Li, 嘉轩 李, Maggie L. Li, Niharika Sravan, Daniel E. Warshofsky
Figure caption: Optical spectra of SN 2025kg. The phases are relative to the time of the accompanying X-ray transient EP250108a’s detection. The spectra start dominated by a blue underlying continuum, though broad features already are beginning to develop in the first epoch. The spectra redden with time and strongly resemble an SN Ic-BL.
Paper: Evidence for Evolutionary Pathway-dependent Black Hole Scaling Relations
Authors: Jonathan H. Cohn, Emmanuel Durodola, Quinn O. Casey, Erini Lambrides, Ryan C. Hickox
Figure caption: The MBH–M⋆ relationship at high-z and z ∼ 0. AGN at 4 ≲ z ≲ 7 are colored by their redshift as per the scale bar on the right. QSOs from M. Yue et al. (2024) are plotted as squares, AGN from R. Maiolino et al. (2024a) are plotted as Xs, and LRDs from E. Durodola et al. (2025) are plotted as dots. GN-z11, as measured in R. Maiolino et al. (2024b), is shown as a black star. The stellar-dynamical MBH measured in a ∼2 lensed quiescent galaxy is plotted as a black diamond outlined in yellow (A. B. Newman et al. 2025). Dynamical MBH measurements in red nugget relic galaxies—local galaxies representative of common quiescent galaxies at z ∼ 2—are plotted as black diamonds outlined in cyan and magenta for molecular gas-dynamical (J. H. Cohn et al. 2021, 2023, 2024) and stellar-dynamical measurements (J. L. Walsh et al. 2015, 2016, 2017), respectively. The A. E. Reines & M. Volonteri (2015) z ∼ 0  MBH–M⋆ relations for AGN (blue dashed line) and bulges (blue dotted line) are shown alongside the F. Pacucci et al. (2023) 4 < z < 7  MBH–M⋆ AGN relation (black solid line). Shaded regions represent the intrinsic scatter of the relations. The M. Yue et al. (2024) and R. Maiolino et al. (2024a) samples follow the F. Pacucci et al. (2023) relation more closely than the z ∼ 0 relations, while the E. Durodola et al. (2025) LRDs are scattered across all three relations. Remarkably, the red nugget relics and the z ∼ 2 quiescent galaxy are aligned with both the high-z F. Pacucci et al. (2023) relation and the z ∼ 0  A. E. Reines & M. Volonteri (2015) relation for bulges.
Paper: Evidence for Evolutionary Pathway-dependent Black Hole Scaling Relations
Authors: Jonathan H. Cohn, Emmanuel Durodola, Quinn O. Casey, Erini Lambrides, Ryan C. Hickox
Figure caption: Schematic showing how different evolutionary pathways may determine the locations of galaxies in the MBH–M⋆ (left) and MBH–σ⋆ (right) parameter spaces. On MBH–M⋆: red nugget relics and compact z ∼ 2 quiescent galaxies exist on the z ∼ 0 relation for bulges, reflecting that MBH growth may correspond with the assembly of galaxy centers. However, total stellar mass includes stars assembled beyond the cores, indicating different assembly histories may lead to different positions on the MBH–M⋆ diagram. AGN systems at high-z are accreting material, rapidly growing their BHs and forming new stars in a regime where much of the galaxy mass likely remains in gas reservoirs. Typical red nuggets assemble their cores by z ∼ 2, then grow into local ETGs through dry mergers that increase total stellar mass without feeding the core or BH. AGN in the nearby Universe have undergone a different growth history, assembling large total stellar masses without completing their core or BH growth. Included in the panel for guidance are the z ∼ 0 relations from A. E. Reines & M. Volonteri (2015). On MBH–σ⋆: both MBH and σ⋆ reflect the central gravitational potential of the galaxy, explaining why this relation may change less with redshift or diverging evolutionary histories. Shown in this panel is the R. P. Saglia et al. (2016) MBH–σ⋆ relation.
Paper: Evidence for Evolutionary Pathway-dependent Black Hole Scaling Relations
Authors: Jonathan H. Cohn, Emmanuel Durodola, Quinn O. Casey, Erini Lambrides, Ryan C. Hickox
Figure caption: High-redshift AGN and z ∼ 2-representative galaxies on the MBH–σ⋆ relation. Symbols are the same as in Figure 2. R. Maiolino et al. (2024a) is the only high-z sample with estimated stellar velocity dispersions. The z ∼ 0  MBH–σ⋆ relation (dashed–dotted green line; R. P. Saglia et al. 2016) is also shown, with the shaded region showing its intrinsic scatter. Although the AGN and red nugget relic galaxy populations overlap with the z ∼ 0 relation, every galaxy is offset above the median of the relation except for the lensed z ∼ 2 system from A. B. Newman et al. (2025).
Paper: Evidence for Evolutionary Pathway-dependent Black Hole Scaling Relations
Authors: Jonathan H. Cohn, Emmanuel Durodola, Quinn O. Casey, Erini Lambrides, Ryan C. Hickox
Figure caption: Schematic showing the history of red nuggets, red nugget relics, and massive ETGs. Massive quiescent galaxies at z ∼ 2, known as red nuggets, typically grow via minor mergers that add stellar mass to their outskirts, becoming the cores of local massive ETGs (e.g., P. G. van Dokkum et al. 2010). In rare cases, some red nuggets fail to undergo any significant merging activity, resulting in a well-preserved relic at z ∼ 0 (e.g., A. Yıldırım et al. 2017).
Paper: Cooling Regimes of Nonthermal Electrons: The Slow, the Fast, and the Very Fast
Authors: Sk. Minhajur Rahaman, Jonathan Granot, Paz Beniamini
Figure caption: Effect of synchrotron self-absorption on prompt-phase optical emission in GRBs. The following parameters are fixed: isotropic observed luminosity Liso = 1052 erg s−1, radius scaling factor f  = 2, variability timescale tvz = 0.1 s, jet magnetization σ = 0.1, electron power-law index p = 2.5, and minimal comoving LF γm = 2 × 104. The conversion efficiency of jet power into nonthermal electrons is ﹩\bar{\epsilon }={\epsilon }_{{\rm{e}}}{\epsilon }_{{\rm{th}}}=0.3﹩, and ϵrad is estimated according to the cooling regime (see Table 1). In all panels, vertical lines indicate transition LFs: Γτ (white dashed, Equation (8)), Γc1 (green dotted–dashed, Equation (9)), and Γcm (purple dashed, Equation (10)), separating (shaded) regions of subphotospheric (gray), VFC (red), FC (green), and SC (purple). In all panels, the vertical dashed orange line indicates the critical LF Γswitch where the cooling break equals the self-absorption frequency. In both bottom panels, the different shading of orange indicates the PLSs where the optical emission (hνopt = 2 eV) lies (notation following J. Granot & R. Sari 2002). The lighter gray shaded region (in the Thomson-thick regime) and white space (in the Thomson-thin regime) below the cyclotron photon energy denote that there is no emission below it. Left: the top left panel shows (in comoving frame) the minimal electron LF γm (horizontal dotted–dashed cyan), cooling LF γc ( solid red), LF of particles contributing to self-absorption γsa ( dashed blue), and modified cooling LF ﹩{\bar{\gamma }}_{{\rm{c}}}﹩ (dotted black; see Equation (7) and Table 2) as a function of the bulk LF. Middle left panel: the prompt optical (2 eV) luminosity ﹩{(\nu {L}_{\nu })}_{{\rm{2eV}}}﹩ (solid orange). The horizontal dotted–dashed orange line shows ﹩{(\nu {L}_{\nu })}_{{\rm{\max }}}={L}_{{\rm{iso}}}/{ \mathcal W }﹩, with ﹩{ \mathcal W }=7﹩ (see Appendix E; mean of W(p = 2.5) = 6 for FC/VFC and G(p = 2.5) = 8 for SC/VSC). Bottom left panel: the critical photon energies hνm (dotted–dashed cyan), hνc (solid red), hνsa (dashed blue), and hνB (dotted black); the horizontal orange line marks the optical band (hνopt = 2 eV). Right: the top right panel shows the combined dissipation and nonthermal electron acceleration efficiency, ﹩\bar{\epsilon }={\epsilon }_{{\rm{e}}}{\epsilon }_{{\rm{th}}}﹩ (solid red), and the radiative efficiency ϵrad (dotted–dashed purple). Middle right panel: the isotropic jet luminosity Lj,iso for our assumed Liso (dotted–dashed blue). Bottom right panel: the spectral index α2eV (in dotted blue) in the optical band (at hνopt = 2 eV).
Paper: Cooling Regimes of Nonthermal Electrons: The Slow, the Fast, and the Very Fast
Authors: Sk. Minhajur Rahaman, Jonathan Granot, Paz Beniamini
Figure caption: Schematic log–log plots of the particle energy distribution (top panel) and the emitted spectrum (bottom panel) after one dynamical timescale. Injected electrons follow a power-law distribution with index p, bounded by minimum and maximum LFs, γm and γM, respectively. The photon spectrum excludes self-absorption, and Table 1 in Appendix B summarizes the scaling relations. Red, orange, cyan, and purple lines represent the VFC, FC, SC, and VSC regimes, respectively. Top panel: the number density of nonthermal electrons as a function of LF (log–log scale). The vertical black line marks γe = 1. The red and purple dotted–dashed lines indicate γm and γM, while the red arrow shows the fraction of electrons contributing to emission in the VFC regime. The orange and cyan dotted–dashed lines mark the cooling LF γc for the FC and SC regimes, and the black dotted line traces the cooling LF in the FC regime. Bottom panel: the flux density as a function of frequency. The vertical black line marks the cyclotron frequency, νB, and the shaded region represents an emission-free zone. The dotted black line indicates the (unphysical) VFC cooling frequency. The orange, red, cyan, and purple lines marking the FC cooling frequency, minimal frequency, SC cooling frequency, and maximum synchrotron frequency, respectively.
Paper: Cooling Regimes of Nonthermal Electrons: The Slow, the Fast, and the Very Fast
Authors: Sk. Minhajur Rahaman, Jonathan Granot, Paz Beniamini
Figure caption: Comparison of the radiative efficiency, ϵrad, between the exact analytical expression and the power-law approximation (as summarized in Table 1). In both panels, we adopt (γm, γM) = (102,  105). The color scheme denotes different cooling regimes: red for VFC, orange for FC, cyan for SC, and purple for VSC. Left panel: radiative efficiency is shown as a function of the power-law index p on a semilogarithmic scale. Dashed lines represent the exact analytical solution, and solid lines correspond to the power-law approximation. Each curve represents a different value of the generalized cooling Lorentz factor ﹩{\bar{\gamma }}_{{\rm{c}}}﹩, highlighting transitions across cooling regimes. The lower subplot provides a linear-scale zoom-in of the exact analytical solution FC and VFC regimes for clarity (for these regimes, the power-law approximation is ϵrad = 1). Right panel: radiative efficiency is plotted against ﹩{\bar{\gamma }}_{{\rm{c}}}﹩ on a log–log scale. Thinner lines indicate the analytical solution, and thicker lines represent the power-law approximation for different values of p. Colors distinguish p values: dark and light green for p = 1.5, purple and blue for p = 2.5, and black and gray for p = 3.5.
Paper: Cooling Regimes of Nonthermal Electrons: The Slow, the Fast, and the Very Fast
Authors: Sk. Minhajur Rahaman, Jonathan Granot, Paz Beniamini
Figure caption: Synchrotron cooling of a charged particle with an initial LF γi in a homogeneous comoving magnetic field ﹩{B}^{{\prime} }﹩. The figure depicts the evolution of the particle’s kinetic energy, normalized by its rest-mass energy mec2, i.e., γ − 1, as a function of comoving time ﹩{t}^{{\prime} }﹩, normalized by the characteristic comoving timescale ﹩{t}_{{\rm{c1}}}^{{\prime} }﹩. The dotted blue, dotted–dashed green, and solid red lines correspond to initial LFs γi of 103, 102, and ﹩\sqrt{2}﹩, respectively. The vertical dotted blue and green lines indicate the cooling timescales ﹩{t}_{{\rm{c}}}^{{\prime} }﹩ at which the electron cools to half of its initial LF. The shaded cyan region marks the phase where electron cooling transitions from the power-law decay regime into the exponential regime, characterized by the timescale ﹩{t}_{{\rm{c1}}}^{{\prime} }/2﹩.
Paper: Cooling Regimes of Nonthermal Electrons: The Slow, the Fast, and the Very Fast
Authors: Sk. Minhajur Rahaman, Jonathan Granot, Paz Beniamini
Figure caption: Annihilation cross section of electron–positron pairs (see Equation (12)), shown in red, as a function of the proper speed of the recombining pairs. Dashed and dotted segments show the asymptotic behavior at the low- and high-proper-speed regimes, respectively. The VFC regime is indicated by the shaded gray region.
Paper: The Importance of Dust Distribution in Ionizing-photon Escape: NIRCam and MIRI Imaging of a Lyman Continuum-emitting Galaxy at z ∼ 3.8
Authors: Zhiyuan Ji, Stacey Alberts, Yongda Zhu, Eros Vanzella, Mauro Giavalisco, Kevin Hainline, William M. Baker, Andrew J. Bunker, Jakob M. Helton, Jianwei Lyu, Pierluigi Rinaldi, Brant Robertson, Charlotte Simmonds, Sandro Tacchella, Christina C. Williams, Christopher N. A. Willmer, Joris Witstok
Figure caption: Comparison of the spatial distribution of the rest-frame ∼3 μm dust emission (MIRI/F1500W, the same color scale as shown in Figure 3) with the LyC, FUV, and Hα emission of Ion1. From top to bottom, the left panel shows the smoothed HST/F410M (LyC, the contours levels are the same as those shown in Figure 1), HST/F435W (LyC+FUV, the contour levels correspond to 2σ, 3σ, and 4σ surface brightness levels, with the 1σ level being ≈25.5 magAB/arcsec2), and the observed Hα map of Ion1. The Hα map was derived using NIRCam/F356W and F335M imaging, reaching a 1σ sensitivity of line flux per pixel at 1.9 × 10−20 erg s−1 cm−2 (see Section 4.2 for details). The contour levels in the Hα map correspond to line flux per pixel values of 5.0 × 10−20, 1.0 × 10−19, 5.0 × 10−19, and 1.0 × 10−18 erg s−1 cm−2. On the right, the contours from the corresponding images shown on the left are overlaid onto the F1500W image of Ion1, with the centroid of the stellar light marked by a white “+.”