adsabs/AstroCLIMB huggingface dataset:
Paper: Theoretical Studies on the Evolution of Solar Filaments in Response to New Emerging Flux
Authors: Yuhao Chen, Jialiang Hu, Guanchong Cheng, Jing Ye, Zhixing Mei, Chengcai Shen, Jun Lin
Figure caption: Evolutionary tendencies of the FR as the new flux starts to emerge. The upper and the lower panels are for the NEF with S < 0 and S > 0, respectively. From left to right, four columns display magnetic configuration scenarios when dipole 2 is positioned at different locations: xd = 0, C(xd, yd) < 0, C(xd, yd) = 0, and C(xd, yd) > 0. Here, C(xd, yd) is the channel function defined in Equation (4). The gray dashed curves represent the initial magnetic configuration when the NEF is absent (i.e., at S = 0), while the solid curves represent the configuration after being perturbed by the NEF. The cyan curves are for the magnetic field generated by the NEF. Two black dotted lines below the photosphere are determined by xd = 0 and C(xd, yd) = 0. The red arrows indicate the direction of motion of the FR after the disturbance, and the shading inside the FR represents the distribution of J.
Paper: Theoretical Studies on the Evolution of Solar Filaments in Response to New Emerging Flux
Authors: Yuhao Chen, Jialiang Hu, Guanchong Cheng, Jing Ye, Zhixing Mei, Chengcai Shen, Jun Lin
Figure caption: The FR motion in the early stage and the consequent catastrophes driven by the NEF of varying polarities, strengths, and locations. Upward arrows denote the early ascent of the FR, while downward arrows indicate early descent. The meanings of the triangles and crosses are the same as those in Figure 3. The green region signifies that early FR ascent or descent is able to lead to either the presence or absence of CME, respectively, while the red region is for the cases otherwise. Dotted lines are determined by C(xd, yd) = 0.
Paper: Theoretical Studies on the Evolution of Solar Filaments in Response to New Emerging Flux
Authors: Yuhao Chen, Jialiang Hu, Guanchong Cheng, Jing Ye, Zhixing Mei, Chengcai Shen, Jun Lin
Figure caption: Evolution of the magnetic field (solid curves) and the associated plasma distributions (colorful shadows) after the catastrophe described by Figure 6. The initial magnetic configuration (t = 0 s) corresponds to the critical point in Figure 6 (red dots).
Paper: Theoretical Studies on the Evolution of Solar Filaments in Response to New Emerging Flux
Authors: Yuhao Chen, Jialiang Hu, Guanchong Cheng, Jing Ye, Zhixing Mei, Chengcai Shen, Jun Lin
Figure caption: Counterpart of case 2 in Figure 4 for r00 = 0.05, xd = 7, and yd = 2.5. The NEF occurs as S changes in the negative direction.
Paper: The Small Sizes and High Implied Densities of “Little Red Dots” with Balmer Breaks Could Explain Their Broad Emission Lines without an Active Galactic Nucleus
Authors: Josephine F. W. Baggen, Pieter van Dokkum, Gabriel Brammer, Anna de Graaff, Marijn Franx, Jenny Greene, Ivo Labbé, Joel Leja, Michael V. Maseda, Erica J. Nelson, Hans-Walter Rix, Bingjie Wang, 冰洁 王, Andrea Weibel
Figure caption: The surface density (﹩{{\rm{\Sigma }}}_{\mathrm{eff}}={M}_{* }(\lt {R}_{{\rm{e}}})/\pi {R}_{{\rm{e}}}^{2}﹩) plotted against stellar mass. We show a theoretical limit Σeff ≦ 3 × 105 M⊙ pc−2, determined by M. Y. Grudić et al. (2019), as the dashed black line. For illustration, we show regions in M*–Σeff space for multiple stellar systems estimated from P. F. Hopkins et al. (2010), the class of star clusters (SCs), ultracompact dwarf galaxies (UCDs), and globular clusters (GCs) (green); local elliptical galaxies (gray); and compact z > 2 elliptical galaxies (yellow). We also show (see the text) quiescent galaxies at z ∼ 4–5 (A. C. Carnall et al. 2023; A. de Graaff et al. 2024; D. J. Setton et al. 2024), compact starburst galaxies at z = 0.4–0.8 (A. M. Diamond-Stanic et al. 2021), Cosmic Gems star clusters at z ∼ 10 (A. Adamo et al. 2024), and the MW nuclear star cluster. The surface density measured for the three Balmer break galaxies are shown for the three sets of stellar masses ﹩{M}_{* ,\min }﹩, M*,med, and ﹩{M}_{* ,\max }﹩ in orange, red, and purple, respectively.
Paper: The Small Sizes and High Implied Densities of “Little Red Dots” with Balmer Breaks Could Explain Their Broad Emission Lines without an Active Galactic Nucleus
Authors: Josephine F. W. Baggen, Pieter van Dokkum, Gabriel Brammer, Anna de Graaff, Marijn Franx, Jenny Greene, Ivo Labbé, Joel Leja, Michael V. Maseda, Erica J. Nelson, Hans-Walter Rix, Bingjie Wang, 冰洁 王, Andrea Weibel
Figure caption: The size measured in F200W, plotted against the UV magnitude, measured from the spectrum at λrest = 150 nm. We also show size–luminosity derived for local spiral galaxies from R. S. de Jong & C. Lacey (2000) for which we use a magnitude correction MUV–MI = 1.0, and LBGs at z ∼ 8 (T. Shibuya et al. 2015; R. Kawamata et al. 2018; R. J. Bouwens et al. 2022) and z ∼ 9–12 (L. Yang et al. 2022). In addition we show star-forming complexes (Z. Chen et al. 2023) with zphot ∼ 6–8. Finally, we show extremely compact sources, recently detected through lensing with JWST, reported in L. J. Furtak et al. (2024; Re < 35 pc, z = 7.0), M. W. Topping et al. (2024; Re < 22 pc, z = 6.1), and H. Williams et al. (2023; Re = 16 pc, z = 9.5). Finally we show the upper limit of ≲100 pc reported for the brightest LRDs (H. B. Akins et al. 2024; see the text).
Paper: The Small Sizes and High Implied Densities of “Little Red Dots” with Balmer Breaks Could Explain Their Broad Emission Lines without an Active Galactic Nucleus
Authors: Josephine F. W. Baggen, Pieter van Dokkum, Gabriel Brammer, Anna de Graaff, Marijn Franx, Jenny Greene, Ivo Labbé, Joel Leja, Michael V. Maseda, Erica J. Nelson, Hans-Walter Rix, Bingjie Wang, 冰洁 王, Andrea Weibel
Figure caption: The observed velocity dispersion of the broad Hβ lines plotted against the predicted velocity dispersion based on Equation (3) using the measured effective radius and stellar masses (Table 1). We show the three stellar mass models, ﹩{M}_{* ,\min }﹩, M*,med, and ﹩{M}_{* ,\max }﹩ in orange, red, and purple, respectively. We predict high velocity dispersions, up to a few hundred km s−1 for the medium stellar mass scenario and σ ⪆ 1000 km s−1 for the maximum stellar mass scenario, similar to the observed velocities. The black error bar in the lower left corner indicates how each measurement would shift horizontally when using different relations for Equation (3), with C = 5.7 (to the right) and C = 6.1 (to the left). In the no-AGN model, the predicted velocity dispersions are very similar to the observed Hβ line widths. Perhaps, the broad Balmer emission lines in these galaxies could simply be the result of the small sizes and high masses of the galaxies. The right plot shows a schematic view of this scenario.
Paper: The Small Sizes and High Implied Densities of “Little Red Dots” with Balmer Breaks Could Explain Their Broad Emission Lines without an Active Galactic Nucleus
Authors: Josephine F. W. Baggen, Pieter van Dokkum, Gabriel Brammer, Anna de Graaff, Marijn Franx, Jenny Greene, Ivo Labbé, Joel Leja, Michael V. Maseda, Erica J. Nelson, Hans-Walter Rix, Bingjie Wang, 冰洁 王, Andrea Weibel
Figure caption: A possible pathway of the massive compact galaxies at z > 6 in the no-AGN scenario. First, a phase of expansion as a result of mass loss (triggered by feedback; e.g., L. Fan et al. 2008) or interaction of the SMBH with the stars in the central region (e.g., M. C. Begelman et al. 1980; J. G. Hills 1983; T. Ebisuzaki et al. 1991; G. D. Quinlan 1996) is required to lower the densities and velocity dispersions to those of massive compact quiescent galaxies at z = 4–5. After that the galaxies grow mainly in an inside-out fashion, due to minor mergers (e.g., R. Bezanson et al. 2009; T. Naab et al. 2009; P. G. van Dokkum et al. 2010).
Paper: The Small Sizes and High Implied Densities of “Little Red Dots” with Balmer Breaks Could Explain Their Broad Emission Lines without an Active Galactic Nucleus
Authors: Josephine F. W. Baggen, Pieter van Dokkum, Gabriel Brammer, Anna de Graaff, Marijn Franx, Jenny Greene, Ivo Labbé, Joel Leja, Michael V. Maseda, Erica J. Nelson, Hans-Walter Rix, Bingjie Wang, 冰洁 王, Andrea Weibel
Figure caption: The median stellar mass profiles for the three sets of stellar masses (see Table 1), ﹩{M}_{* ,\min }﹩, M*,med, and ﹩{M}_{* ,\max }﹩ in orange, red, and purple, respectively. We also show the stellar mass profiles of massive quiescent galaxies at different cosmic times: the mean stellar mass profile of three compact massive quiescent galaxies at z ∼ 4–5 (A. C. Carnall et al. 2023; D. J. Setton et al. 2024; A. de Graaff et al. 2024), z ∼ 2.3 compact elliptical galaxies (R. Bezanson et al. 2009), and massive elliptical galaxies at z = 0 (T. Tal et al. 2009).
Paper: The Small Sizes and High Implied Densities of “Little Red Dots” with Balmer Breaks Could Explain Their Broad Emission Lines without an Active Galactic Nucleus
Authors: Josephine F. W. Baggen, Pieter van Dokkum, Gabriel Brammer, Anna de Graaff, Marijn Franx, Jenny Greene, Ivo Labbé, Joel Leja, Michael V. Maseda, Erica J. Nelson, Hans-Walter Rix, Bingjie Wang, 冰洁 王, Andrea Weibel
Figure caption: The spectra (gray) and best-fit model (dark blue) with maximal stellar mass of three Balmer break galaxies, obtained from B. Wang et al. (2024b). We also show 1″ × 1″ images in four different bands, F115W, F200W, F356W, and F444W. The dotted lines indicate the location of the Balmer break (black), [O III] line (red), and Hβ (blue) line, which are relevant in this work. For information on other emission lines, see B. Wang et al. (2024b).
Paper: The Small Sizes and High Implied Densities of “Little Red Dots” with Balmer Breaks Could Explain Their Broad Emission Lines without an Active Galactic Nucleus
Authors: Josephine F. W. Baggen, Pieter van Dokkum, Gabriel Brammer, Anna de Graaff, Marijn Franx, Jenny Greene, Ivo Labbé, Joel Leja, Michael V. Maseda, Erica J. Nelson, Hans-Walter Rix, Bingjie Wang, 冰洁 王, Andrea Weibel
Figure caption: The top row shows images in the NIRCam F200W band of the three Balmer break galaxies. The second row shows the segmentation maps; the third row shows the best-fitting PSF-convolved GALFIT models. The residuals, obtained by subtracting the best-fitting models from the images, are shown in the fourth row. The fifth row shows RGB images of the galaxies, with F115W as the blue band, F150W as the green band, and F200W as the red band and the final row with F115W, F277W, and F444W. All images are 1″ × 1″.
Paper: The Newly Discovered Nova Super-remnant Surrounding Recurrent Nova T Coronae Borealis: Will it Light Up during the Coming Eruption?
Authors: Michael M. Shara, Kenneth M. Lanzetta, Alexandra Masegian, James T. Garland, Stefan Gromoll, Joanna Mikolajewska, Mikita Misiura, David Valls-Gabaud, Frederick M. Walter, John K. Webb
Figure caption: Difference images of T CrB (position indicated with red ticks) created by directly subtracting each of the four narrowband coadded images from the luminance coadded image, then applying 8 × 8 block-summing as in Figure 2. A hand sketch of the two possible lobes of the nebulosity is drawn over a copy of the [S II] narrowband difference image. All images have the same scaling to allow for direct comparison of the faint emission features. The presence of clear emission in [N II], but none in [O III], demonstrates that the nebulosities are shock-ionized rather than photoionized.
Paper: The Newly Discovered Nova Super-remnant Surrounding Recurrent Nova T Coronae Borealis: Will it Light Up during the Coming Eruption?
Authors: Michael M. Shara, Kenneth M. Lanzetta, Alexandra Masegian, James T. Garland, Stefan Gromoll, Joanna Mikolajewska, Mikita Misiura, David Valls-Gabaud, Frederick M. Walter, John K. Webb
Figure caption: RGB image of T CrB (position indicated with red ticks) and its surrounding emission. Each of the three channels is a block-summed difference image (see Figure 3). Red corresponds to luminance—[S II], green corresponds to luminance—Hα, and blue to luminance—[N II]. The intensity scaling of each channel has been adjusted individually to highlight the emission features. There is a suggestion of a bilobed structure (also noted and sketched in Figure 3). The white arrow points in the direction of the star's Gaia-measured proper motion, with a length corresponding to the angular distance that T CrB has moved in the past 100,000 yr.
Paper: The Newly Discovered Nova Super-remnant Surrounding Recurrent Nova T Coronae Borealis: Will it Light Up during the Coming Eruption?
Authors: Michael M. Shara, Kenneth M. Lanzetta, Alexandra Masegian, James T. Garland, Stefan Gromoll, Joanna Mikolajewska, Mikita Misiura, David Valls-Gabaud, Frederick M. Walter, John K. Webb
Figure caption: “Star-cleaned” versions of the luminance—[S II], luminance—Hα, and luminance—[N II] images, created with STARNET2. The scaling of each image matches the scaling of the channels in the RGB image (Figures 4 and 5). The images have been smoothed with a 2D Gaussian kernel to emphasize the nebulosity. Note that the (noisy) [N II] image has the lowest reach (and highest background) of the three narrowband images shown. The position of T CrB is indicated with red ticks.
Paper: The Newly Discovered Nova Super-remnant Surrounding Recurrent Nova T Coronae Borealis: Will it Light Up during the Coming Eruption?
Authors: Michael M. Shara, Kenneth M. Lanzetta, Alexandra Masegian, James T. Garland, Stefan Gromoll, Joanna Mikolajewska, Mikita Misiura, David Valls-Gabaud, Frederick M. Walter, John K. Webb
Figure caption: Same as Figure 1, but each image has been 8 × 8 block-summed (see text). Faint, nebulous structures are seen to surround T CrB in Hα, [N II], and [S II] in all directions.
Paper: The Newly Discovered Nova Super-remnant Surrounding Recurrent Nova T Coronae Borealis: Will it Light Up during the Coming Eruption?
Authors: Michael M. Shara, Kenneth M. Lanzetta, Alexandra Masegian, James T. Garland, Stefan Gromoll, Joanna Mikolajewska, Mikita Misiura, David Valls-Gabaud, Frederick M. Walter, John K. Webb
Figure caption: Same as Figure 4 but after the “star-cleaning” algorithm STARNET2 is applied. The bilobed structure is again seen, with a maximum diameter of ~2 deg in the NW to SE direction. The location of T CrB is indicated with red ticks.
Paper: The Newly Discovered Nova Super-remnant Surrounding Recurrent Nova T Coronae Borealis: Will it Light Up during the Coming Eruption?
Authors: Michael M. Shara, Kenneth M. Lanzetta, Alexandra Masegian, James T. Garland, Stefan Gromoll, Joanna Mikolajewska, Mikita Misiura, David Valls-Gabaud, Frederick M. Walter, John K. Webb
Figure caption: Coadded images of T CrB (position indicated with red ticks) in the luminance broadband and four narrowband ([O III], Hα, [N II], and [S II]) filters. Each image has a different contrast scaling corresponding to the parameters assigned by the “zscale” function in SAO DS9.
Paper: Potential for Life to Exist and be Detected on Earth-like Planets Orbiting White Dwarfs
Authors: Caldon T. Whyte, L. H. Quiroga-Nuñez, Manasvi Lingam, Paola Pinilla
Figure caption: (Top panel) The orbital radius (a [au]) at which the flux of photosynthetically active photons and UV radiation reaches their critical flux of 1.2 × 1016 m−2 s−1 and 5.44 × 1016 m−2 s−1, respectively (M. Lingam & A. Loeb 2021, Chapter 4). Boundaries for the critical PAR and UV fluxes are the dashed–dotted and dotted lines, respectively. Orbital distances below these curves may receive the appropriate flux to support photosynthetic life or abiogenesis. (Middle panel) The peak wavelength (λpeak [nm]) of a white dwarf’s spectral radiation flux as a function of its age (Gyr); cooling of the white dwarf leads to a shift toward longer wavelengths. The green dashed line is the maximum wavelength used for photosynthesis on Earth (750 nm). (Bottom panel) JWST in-transit integration time needed to achieve a S/N of 5 using transmission spectroscopy to observe biosignatures present in an Earth-like atmosphere, calculated using Equation (19).
Paper: Potential for Life to Exist and be Detected on Earth-like Planets Orbiting White Dwarfs
Authors: Caldon T. Whyte, L. H. Quiroga-Nuñez, Manasvi Lingam, Paola Pinilla
Figure caption: Shaded blue region shows a simplified habitable zone (HZ) explained in Section 2.3. This is compared against the standard approach of determining the HZ limits based on the stellar flux (described in Section 2.3): inner limits of the HZ are the moist greenhouse (black dashed–dotted), runaway greenhouse (black dashed), and recent Venus (black solid) thresholds, whereas outer limits are the maximum greenhouse (magenta dashed) and early Mars (magenta solid) thresholds. Solid orange line marks the orbital radius at which the interval spent in the temporally changing habitable zone is maximized.
Paper: Potential for Life to Exist and be Detected on Earth-like Planets Orbiting White Dwarfs
Authors: Caldon T. Whyte, L. H. Quiroga-Nuñez, Manasvi Lingam, Paola Pinilla
Figure caption: Habitable zone for a white dwarf (blue region) at ages of 2, 6, and 10 Gyr compared to the habitable zone of the red dwarf TRAPPIST-1 (orange region). The inset shows the size comparison of a typical 0.6M⊙ white dwarf (cyan region) to that of TRAPPIST-1 (pink region). The optimistic habitable zone for TRAPPIST-1 is calculated from the recent Venus and early Mars limits from R. K. Kopparapu et al. (2013) using the luminosity and effective temperature from V. Van Grootel et al. (2018). The magenta region specifies where overlap of the two habitable zones occurs. The dashed black line shows the orbital radius at which an Earth-like planet around a 0.6M⊙ white dwarf stays in the habitable zone for the maximum amount of time (i.e., maximum habitable lifetime), and the dashed red line shows the Roche limit (i.e., tidal disruption limit) for such a system.
Paper: Large Eruptive and Confined Flares in Relation to the Solar Active Region Evolution
Authors: Fuyu Li, Changhui Rao, Huaning Wang, Xinhua Zhao, Nanbin Xiang, Linhua Deng, Haitang Li, Yu Liu
Figure caption: Flare outbreak situation in developing and decaying phases. The eruptive (red circles) and confined flare (blue circles) numbers for every ARs and the cumulative counts are exhibited in the four top panels. The conditions for flare indexes are shown in the four left panels. In decaying phases, the stored counts of eruptive flare quantities and indexes are significantly over those of confined flares.
Paper: Large Eruptive and Confined Flares in Relation to the Solar Active Region Evolution
Authors: Fuyu Li, Changhui Rao, Huaning Wang, Xinhua Zhao, Nanbin Xiang, Linhua Deng, Haitang Li, Yu Liu
Figure caption: Relationship between flare eruption and sunspot group area in logarithmic coordinates. The three panels in the top row show the relation of the sunspot group area to the numbers of total flare, confined flares, and eruptive flares. Similar graphics for flare indexes are in the bottom line.
Paper: Large Eruptive and Confined Flares in Relation to the Solar Active Region Evolution
Authors: Fuyu Li, Changhui Rao, Huaning Wang, Xinhua Zhao, Nanbin Xiang, Linhua Deng, Haitang Li, Yu Liu
Figure caption: Yearly eruptive rate of flares in the AR developing phase and decaying phase computed from flare quantities (left panel) and flare indexes (right panel). The eruptive rate is obviously higher in decaying phase than in the developing phase.
Paper: CEERS Key Paper. IX. Identifying Galaxy Mergers in CEERS NIRCam Images Using Random Forests and Convolutional Neural Networks
Authors: Caitlin Rose, Jeyhan S. Kartaltepe, Gregory F. Snyder, Marc Huertas-Company, L. Y. Aaron Yung, Pablo Arrabal Haro, Micaela B. Bagley, Laura Bisigello, Antonello Calabrò, Nikko J. Cleri, Mark Dickinson, Henry C. Ferguson, Steven L. Finkelstein, Adriano Fontana, Andrea Grazian, Norman A. Grogin, Benne W. Holwerda, Kartheik G. Iyer, Lisa J. Kewley, Allison Kirkpatrick, Dale D. Kocevski, Anton M. Koekemoer, Jennifer M. Lotz, Ray A. Lucas, Lorenzo Napolitano, Casey Papovich, Laura Pentericci, Pablo G. Pérez-González, Nor Pirzkal, Swara Ravindranath, Rachel S. Somerville, Amber N. Straughn, Jonathan R. Trump, Stephen M. Wilkins, Guang Yang
Figure caption: Stellar mass vs. redshift for objects from the mock CEERS sample at 3 < z < 5 (gray) and from the observed CEERS sample with 3 < z < 5 (blue). Above and to the right are the distributions of redshift and stellar mass, respectively. These samples do include the S/N and flag cuts discussed in Sections 3.3 and 4.1.
Paper: CEERS Key Paper. IX. Identifying Galaxy Mergers in CEERS NIRCam Images Using Random Forests and Convolutional Neural Networks
Authors: Caitlin Rose, Jeyhan S. Kartaltepe, Gregory F. Snyder, Marc Huertas-Company, L. Y. Aaron Yung, Pablo Arrabal Haro, Micaela B. Bagley, Laura Bisigello, Antonello Calabrò, Nikko J. Cleri, Mark Dickinson, Henry C. Ferguson, Steven L. Finkelstein, Adriano Fontana, Andrea Grazian, Norman A. Grogin, Benne W. Holwerda, Kartheik G. Iyer, Lisa J. Kewley, Allison Kirkpatrick, Dale D. Kocevski, Anton M. Koekemoer, Jennifer M. Lotz, Ray A. Lucas, Lorenzo Napolitano, Casey Papovich, Laura Pentericci, Pablo G. Pérez-González, Nor Pirzkal, Swara Ravindranath, Rachel S. Somerville, Amber N. Straughn, Jonathan R. Trump, Stephen M. Wilkins, Guang Yang
Figure caption: Example of a normalized, stretched, and augmented 3 < z < 3.5 galaxy merger. For this redshift bin, normalization was based on the F115W filter. After normalizing and stretching, the extended structures of this merger are more distinct from the background.
Paper: CEERS Key Paper. IX. Identifying Galaxy Mergers in CEERS NIRCam Images Using Random Forests and Convolutional Neural Networks
Authors: Caitlin Rose, Jeyhan S. Kartaltepe, Gregory F. Snyder, Marc Huertas-Company, L. Y. Aaron Yung, Pablo Arrabal Haro, Micaela B. Bagley, Laura Bisigello, Antonello Calabrò, Nikko J. Cleri, Mark Dickinson, Henry C. Ferguson, Steven L. Finkelstein, Adriano Fontana, Andrea Grazian, Norman A. Grogin, Benne W. Holwerda, Kartheik G. Iyer, Lisa J. Kewley, Allison Kirkpatrick, Dale D. Kocevski, Anton M. Koekemoer, Jennifer M. Lotz, Ray A. Lucas, Lorenzo Napolitano, Casey Papovich, Laura Pentericci, Pablo G. Pérez-González, Nor Pirzkal, Swara Ravindranath, Rachel S. Somerville, Amber N. Straughn, Jonathan R. Trump, Stephen M. Wilkins, Guang Yang
Figure caption: Examples of CEERS galaxies (F150W+F200W+F356W stamps) for each visually classified interaction class at 3.5 < z < 4, 3.5 < z < 4, and 4 < z < 5.
Paper: CEERS Key Paper. IX. Identifying Galaxy Mergers in CEERS NIRCam Images Using Random Forests and Convolutional Neural Networks
Authors: Caitlin Rose, Jeyhan S. Kartaltepe, Gregory F. Snyder, Marc Huertas-Company, L. Y. Aaron Yung, Pablo Arrabal Haro, Micaela B. Bagley, Laura Bisigello, Antonello Calabrò, Nikko J. Cleri, Mark Dickinson, Henry C. Ferguson, Steven L. Finkelstein, Adriano Fontana, Andrea Grazian, Norman A. Grogin, Benne W. Holwerda, Kartheik G. Iyer, Lisa J. Kewley, Allison Kirkpatrick, Dale D. Kocevski, Anton M. Koekemoer, Jennifer M. Lotz, Ray A. Lucas, Lorenzo Napolitano, Casey Papovich, Laura Pentericci, Pablo G. Pérez-González, Nor Pirzkal, Swara Ravindranath, Rachel S. Somerville, Amber N. Straughn, Jonathan R. Trump, Stephen M. Wilkins, Guang Yang
Figure caption: Merger rate based on visual classifications (left panel), random forest classifications (middle panel), and neural network classifications (right panel) as compared to the theoretical Illustris merger rate (black line) derived from V. Rodriguez-Gomez et al. (2015) and the major merger rate (gray line: power-law + exponential model; gray stars: binned JWST data) of Q. Duan et al. (2024) derived from the close pair method. The green shaded regions and the observed galaxy error bars indicate the binomial 95% confidence interval.