adsabs/AstroCLIMB huggingface dataset:
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: Photocenter analysis of the Hα decretion disk around β CMi. (a) 2D photocenter positions for each spectral channel. The colors indicate the Doppler velocities, and the gray ellipses show the 1σ uncertainties. The green line denotes the derived disk position angle, 126°. (b) Hα spectrum of β CMi (sum of all the 38 ports), showing a double-peaked line profile. The solid and dotted lines indicate the best-fit Keplerian velocity disk models with asymmetric and symmetric power-law intensity distributions. (c) and (d) Photocenter positions for each spectral channel, projected along the disk’s major and minor axes, respectively. The photocenter measurements from two separate observations (circular and triangular markers) show strong agreement, demonstrating the repeatability of the measurement. The photocenter shift along the major axis reveals disk rotation consistent with a Keplerian velocity field. Interestingly, at low velocities, a shift along the minor axis is observed, indicating nearside and farside asymmetry of the disk. (e) Best-fit intensity distribution of the asymmetric Keplerian model. (f) Best-fit velocity distribution of the asymmetric Keplerian model.
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: Image reconstruction of the Hα decretion disk around β CMi. (a) Measured circular 2D Gaussian FWHM, representing the spatial extent of the intensity distribution in each wavelength channel. While there is an apparent FWHM enhancement around the Hα center, it is of marginal statistical significance compared to the 1–2 mas level of systematic fluctuations across the continuum. (b) The half-maximum level of reconstructed images as a function of wavelength (∣v∣ < 180 km s−1), for the two epochs. The colors indicate the velocity and have the same color scale as in panel (a). The photocenter of each image is marked with the circular and triangular symbols. The average images of the continuum level are shown to the lower right, analogous to the “beam size,” the instrumental width. (c) The half-maximum level of the reconstructed images overlaid on best-fit asymmetric Keplerian model images for each wavelength channel from Figures 4(e) and (f). The reconstructed images show consistency with the model, tracing the shift in emission across wavelength—both the rotation seen in Figure 4(f) and the brightness asymmetry in Figure 4(e).
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 PL-IFU concept. (a) A conceptual diagram of using a PL as a compact IFU. The light collected by the telescope is coupled to the multimode end of the PL at the focal plane, which is then converted into multiple single-mode beams encoding the spatial information of the incoming wave front. Using the spectrally dispersed single-mode outputs, both spectral and spatial information can be recovered at high angular resolution within a small FOV (a few λ/D), enabling detailed characterizations of compact astronomical sources. (b) An illustrative diagram of the spatial mode decomposition of a focal-plane field. Using an LP mode basis that describes the spatial modes of circular step-index optical fibers, a PSF with a small shift is primarily described as a linear combination of the fundamental LP01 and first-order LP11 modes, with complex-valued mode amplitudes. The complex mode amplitudes are represented as phasors (white arrows), where the arrow’s length and angle correspond to the magnitude and phase of the coefficient. (c) A PL has unique complex-valued mixing coefficients (transfer matrix) that map the mode amplitudes to complex amplitudes of SMF outputs; for simplicity, we describe the case of a three-port PL here. (d) By imaging the SMF outputs on a detector, one measures the intensities of the SMF outputs, which have spatial information of the input.
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: Spectral-differential spatial signal detection. (a) Hα spectrum of β CMi observed on 2025 February 11, summed over all the 38 traces. (b) Response maps (i.e., Figure 2(e)) of selected velocity channels, for one of the ports. The red solid contours and black dashed contours denote the same contour levels for the measured response maps and the modeled reference response maps. Small shifts are observed between the two contours, as marked with white arrows in the zoom-in images, indicating photocenter shifts. (c) Response maps subtracted by the model reference response maps (difference maps). Deviations from zero indicate that the astronomical scene departs from an unresolved central point source. The positive and negative structures indicate the shift. (d) S/N maps of three ports, which correspond to the difference maps divided by the error maps. The spatial signals are clearly seen in the Hα wavelength range.
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: PCA of the normalized spectrum. (a) Spectrum of β CMi observed in 2024 September, showing a double-peaked Hα line from the decretion disk and oxygen B-band absorption due to the Earth’s atmosphere. (b) Average normalized spectrum of one of the output ports. Spectral-differential spatial signals are not detected in the average spectrum, due to signal dilution by time-varying WFEs and fixed pattern noise by detector pixel-to-pixel variation. (c) The first four principal components of the time-series normalized spectrum. (d) Zoomed-in cutouts of panel (c) around Hα. The low-frequency component was filtered and the four components were shifted vertically for visualization. Emission-line-scale features are detected in the principal components, implying the presence of spectral-differential spatial signals. (e) The same as panel (d) but for the oxygen B-band. No line-scale features are detected.
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: Average PSF and PSF peak location histograms. (a) Average H-band PSFs of the two observations. For both observations, the low-wind effect affected the PSF quality, splitting the core. (b) Distribution of PSF peak positions. The tip/tilt jitter in 2024 September is nearly circular, whereas in 2025 February it shows an elongated distribution.
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: Mean reflectance spectrum of 3I/ATLAS, coadded from the nights of August 10, 12, 16, and 17 with the 2.4 m MDM telescope (black). For comparison, we show the spectra of 3I/ATLAS reported by D. Z. Seligman et al. (2025; yellow), obtained on July 4 with the 2.2 m University of Hawaii telescope, and the D-type spectral taxonomy from F. E. DeMeo et al. (2009; blue). Squares mark photometric measurements obtained with the 1.3 m MDM telescope. Vertical bands mark the positions of typical cometary emission features: CN at 3870 Å, C3 at 4050 Å, C2(Δν = 1) at 4750 Å, and C2(Δν = 0) at 5150 Å.
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: CN emission feature of 3I/ATLAS detected with the 2.4 m MDM telescope. The vertical green band marks the expected position of CN emission near 3870 Å. Top left: zoom-in on the CN region of the reflectance spectrum. In addition to the comparison spectra shown in Figure 1, we include a Gaussian-smoothed curve to improve visibility (blue). Top right: coadded, continuum-subtracted flux of 3I/ATLAS from this work (gray), compared with the CN emission flux detected in 2I/Borisov by H. W. Lin et al. (2020; brown). A Gaussian smoothing applied to our data is also shown (black). Bottom: continuum-subtracted CN flux measured individually on August 10, 12, 16, and 17.
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: Radial profiles of 3I/ATLAS on three different nights. Left: linear scale. Right: logarithmic scale. A common point-spread function, convolved with the images, is shown for comparison (solid black).
Paper: Prediscovery Activity of New Interstellar Object 3I/ATLAS: Rapid Brightening from 6 to 4 au
Authors: Quanzhi Ye, 泉志 叶, Michael S. P. Kelley, Henry H. Hsieh, Eric C. Bellm, Tracy X. Chen, Richard Dekany, Andrew Drake, Steven L. Groom, George Helou, Shrinivas R. Kulkarni, Thomas A. Prince, Reed Riddle
Figure caption: Best-fit lightcurve of 3I using ZTF photometry from nightly and multinightly stacks from 2024 June 15 to 2025 July 20. Uncertainties of individual data points may be underestimated due to complications associated with crowded field photometry. For multinightly stacks, horizontal bars indicate the time bin sizes. The lightcurve models used are appropriate for a coma or nucleus, described by Equations (1) and (2), respectively. For the 2024 panel, the coma model is fainter than 25.5 mag. We offset the g-band photometry by −0.65 mag using the spectral slope reported by C. Opitom et al. (2025).(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: Prediscovery Activity of New Interstellar Object 3I/ATLAS: Rapid Brightening from 6 to 4 au
Authors: Quanzhi Ye, 泉志 叶, Michael S. P. Kelley, Henry H. Hsieh, Eric C. Bellm, Tracy X. Chen, Richard Dekany, Andrew Drake, Steven L. Groom, George Helou, Shrinivas R. Kulkarni, Thomas A. Prince, Reed Riddle
Figure caption: Plots of (a) nucleus-subtracted V-band absolute magnitudes (assuming a spectral slope of 18%/100 nm; C. Opitom et al. 2025) of 3I’s excess dust inferred from the ZTF data, using the (lower limit) nuclear magnitude of HV > 15.4 mag reported by D. Jewitt et al. (2025), and (b) the dust-to-nucleus flux ratios calculated for each photometry point for 3I as functions of time (bottom axes) and heliocentric distance (top axes). The phases of “plateau” and “uniform brightening,” described in the main text, are marked. Uncertainties of individual data points may be underestimated due to complications associated with crowded field photometry.
Paper: Prediscovery Activity of New Interstellar Object 3I/ATLAS: Rapid Brightening from 6 to 4 au
Authors: Quanzhi Ye, 泉志 叶, Michael S. P. Kelley, Henry H. Hsieh, Eric C. Bellm, Tracy X. Chen, Richard Dekany, Andrew Drake, Steven L. Groom, George Helou, Shrinivas R. Kulkarni, Thomas A. Prince, Reed Riddle
Figure caption: Multinight ZTF stacks centered at the nominal ephemeris position of 3I of periods from UT 2024 June 15 to UT 2025 May 9. Each stack is smoothed by a 2″ wide Gaussian function for clarity. The 3σ uncertainty ellipses (appearing largely as thin lines due to very small semiminor axes) are plotted in the upper-right corner of each panel. The images are color inverted.
Paper: Prediscovery Activity of New Interstellar Object 3I/ATLAS: Rapid Brightening from 6 to 4 au
Authors: Quanzhi Ye, 泉志 叶, Michael S. P. Kelley, Henry H. Hsieh, Eric C. Bellm, Tracy X. Chen, Richard Dekany, Andrew Drake, Steven L. Groom, George Helou, Shrinivas R. Kulkarni, Thomas A. Prince, Reed Riddle
Figure caption: A selection of nightly ZTF stacks of 3I from its first detection on UT 2025 May 15 to UT 2025 July 20 (the latest stack used in this work). 3I is marked by a filled triangle in each panel. The panels have north up and east to the left. The arrows in the upper left of each panel mark the direction to the Sun (⊙) and velocity vector (+v) of the comet. The images are color inverted.
Paper: How Fast Could Supermassive Black Holes Grow at the Epoch of Reionization?
Authors: Ziyong Wu, Renyue Cen, Romain Teyssier
Figure caption: Left: the gas density and temperature profiles of our zoom-in halo at z = 10 are shown in the top and bottom panels, respectively. While the gas density profiles are broadly consistent across different simulations, which agree well with the analytical form presented in K. Inayoshi et al. (2016), the temperature profiles exhibit significant variation. This contrast highlights that, although gravitational collapse governs the overall gas distribution, the thermal state of the gas is highly sensitive to the feedback prescriptions and physical processes included in each simulation. Right: (a) The BH mass growth curves over time are shown, revealing two distinct phases. Once the BH reaches a mass of 104–105 M⊙ during the super-Eddington accretion phase, AGN feedback self-regulates its growth, causing it to transition to a slower, approximately Eddington-limited rate. We refer to this stage as the self-regulation phase. (b) The evolution of the BH accretion rate (﹩{\dot{M}}_{\mathrm{acc}}﹩) over cosmic time is shown, along with (c) the Eddington ratio λEdd, and ﹩{\lambda }_{\mathrm{Edd}}={\dot{M}}_{\mathrm{acc}}/{\dot{M}}_{\mathrm{Edd}}﹩, which represents the accretion rate relative to the Eddington limit. During the super-Eddington phase, the BH accretion rate ﹩{\dot{M}}_{\mathrm{acc}}﹩ remains close to its maximum ﹩3\times {\dot{M}}_{\mathrm{Edd}}﹩ in the super-Eddington case and ﹩{\dot{M}}_{\mathrm{Edd}}﹩ in the Eddington-limited case. However, upon entering the self-regulation phase, only the simulations without feedback or with SN-only feedback in the super-Eddington case can sustain the maximum accretion rate. In contrast, in simulations with AGN feedback, the accretion rate inevitably declines to the Eddington limit, for the range of the implemented AGN feedback strength or the suite of SN feedback models employed.
Paper: How Fast Could Supermassive Black Holes Grow at the Epoch of Reionization?
Authors: Ziyong Wu, Renyue Cen, Romain Teyssier
Figure caption: (a) The distribution of the transition BH mass ﹩{M}_{{\rm{sink}}}^{t}﹩ determined by the average gas density 〈n〉, and the average gas temperature 〈T〉. The black star represents the typical value obtained from our simulations, while the red region highlights the range where ﹩{M}_{{\rm{sink}}}^{t}﹩ falls between 104 and 105 M⊙. (b) The time evolution of the sound speed near the BH, cs. (c) The squared gas density in spherical shells as a function of radius centered on the BH times radius cubed, n2R3, where the area under the curve is proportional to the cooling rate contribution. (d, e, f) The evolution of stellar mass, total gas mass, hot gas mass, and cold gas mass over time for two regions: the galaxy region (0.1Rvir) and the BH region (0.01Rvir). Panel (d) corresponds to the SN-only case with λEdd < 3; panel (e) to ϵq = 0.15, ϵj = 0.05, and λEdd < 3; and panel (f) to ϵq = 0.15, ϵj = 0.05, and λEdd < 1. Once SMBHs reach masses of 104–105 M⊙, their growth transitions to a self-regulated phase, driven by AGN feedback that expels gas from the surrounding region. This process ultimately regulates accretion, with higher accretion rates leading to stronger feedback.
Paper: The Bigfoot: A Footprint of a Coma Cluster Progenitor at z = 3.98
Authors: Hanwen Sun, Tao Wang, Emanuele Daddi, Qiaoyang Hao, Ke Xu, David Elbaz, Luwenjia Zhou, Houjun Mo, Huiyuan Wang, Longyue Chen, Yangyao Chen, Shuowen Jin, Yipeng Lyu, Nikolaj Sillassen, Kai Wang, Tiancheng Yang
Figure caption: The halo mass of 0217A compared with the constraint from cosmology and the simulated clusters. In the left panel, the orange star shows the halo mass and redshift of 0217A. The red dotted, solid, and dashed lines show the 0.683 (1σ), 0.954 (2σ), and 0.997 (3σ) exclusion curves (I. Harrison & S. Hotchkiss 2013) in the 0.17 deg2 area under the Planck cosmology with σ8 = 0.811 ± 0.006 and Ωm = 0.315 ± 0.007 (Planck Collaboration et al. 2020). The blue lines show the exclusion curves under the cosmology measured by DESI (T. Karim et al. 2025) with σ8 = 0.702 ± 0.030 and Ωm = 0.285 ± 0.010. The green line shows the mass evolution of the most massive progenitor halo in the simulated massive clusters with M0 > 1015M⊙ (Y.-K. Chiang et al. 2013). In the right panel, the blue points show the σ8 measured by the low-redshift probes from BOSS (S.-F. Chen et al. 2022), DES year 3 (T. M. C. Abbott et al. 2022), and the DESI Legacy Imaging Surveys (T. Karim et al. 2025); the orange point shows the σ8 constrained by the local galaxy clusters from the SRG/eROSITA all-sky survey (V. Ghirardini et al. 2024); the arrows show the limits of σ8 under which Bigfoot, J1001, and the combination of them meet the 0.954 (2σ) and 0.997 (3σ) exclusions; and the magenta points show the σ8 measured with CMB (S. Aiola et al. 2020; Planck Collaboration et al. 2020).
Paper: The Bigfoot: A Footprint of a Coma Cluster Progenitor at z = 3.98
Authors: Hanwen Sun, Tao Wang, Emanuele Daddi, Qiaoyang Hao, Ke Xu, David Elbaz, Luwenjia Zhou, Houjun Mo, Huiyuan Wang, Longyue Chen, Yangyao Chen, Shuowen Jin, Yipeng Lyu, Nikolaj Sillassen, Kai Wang, Tiancheng Yang
Figure caption: The total SMF of Bigfoot compared with massive clusters with M0 ∼ 1015M⊙. The left figure shows that Bigfoot has a comparable number of galaxies and occupied volume to simulated progenitors of Coma-type massive galaxy clusters, where the red line shows the total SMF of the nine subgroups of PCL0217 at zspec = 3.97–4.00 subtracted by a predicted contribution from the field SMF. The dashed lines show the total SMF of the progenitors (z = 4.04) of the seven most massive galaxy clusters (M0 ∼ 1015M⊙) from the ELUCID simulation (H. Wang et al. 2014). The right panel compares the total SMF of Bigfoot with the observed mass functions of red galaxies in local clusters from DESI and the Sloan Digital Sky Survey (J. Meng et al. 2023).
Paper: The Bigfoot: A Footprint of a Coma Cluster Progenitor at z = 3.98
Authors: Hanwen Sun, Tao Wang, Emanuele Daddi, Qiaoyang Hao, Ke Xu, David Elbaz, Luwenjia Zhou, Houjun Mo, Huiyuan Wang, Longyue Chen, Yangyao Chen, Shuowen Jin, Yipeng Lyu, Nikolaj Sillassen, Kai Wang, Tiancheng Yang
Figure caption: Stellar mass functions with massive galaxy excess in Bigfoot. In the first 11 panels, the blue lines show the SMFs of SFGs in each subgroup of Bigfoot, while the green dashed lines show the SMF of field galaxies at 3.5 < z < 4.5 (T. Wang et al. 2025), which is based on the same catalog as this work and has been renormalized to match the SMFs of Bigfoot. All of the four massive subgroups show a top-heavy SMF of SFGs compared with the renormalized field SMF and the less massive subgroups, suggesting the accelerated formation of massive galaxies in massive overdensities. The last panel shows the total SMF of massive subgroups with ﹩{\mathrm{log}}({M}_{{\rm{h}}}/{M}_{\odot })\gt 12.5﹩; the blue line and the red line show the distribution of SFGs and QGs, respectively. The orange line shows the total SMF, which is the sum of blue line and red line. The QGs, including both passive galaxies and poststarburst galaxies, are classified using an updated UVJ criterion (S. E. Cutler et al. 2024). Due to the limited number of QGs in each subgroup, we can only plot the total SMF of QGs instead of the SMF of QGs in each subgroup.
Paper: The Bigfoot: A Footprint of a Coma Cluster Progenitor at z = 3.98
Authors: Hanwen Sun, Tao Wang, Emanuele Daddi, Qiaoyang Hao, Ke Xu, David Elbaz, Luwenjia Zhou, Houjun Mo, Huiyuan Wang, Longyue Chen, Yangyao Chen, Shuowen Jin, Yipeng Lyu, Nikolaj Sillassen, Kai Wang, Tiancheng Yang
Figure caption: The stellar mass and number density profile of 0217A: the left panel shows the projected stellar mass density profile, while the right panel shows the projected number density profile. The surface overdensities of 0217A are shown as the red lines, which have been subtracted by the field level (estimated as the density of field galaxies at 3.73 < z < 4.23 in PRIMER-COSMOS). For comparison, the orange dashed–dotted lines show the density profile of cluster J1001 at z = 2.51 (H. Sun et al. 2024), the purple dashed lines show the result of the GCLASS clusters at z ∼ 1 (R. F. J. van der Burg et al. 2014), and the blue dotted lines show the results of local clusters at z ∼ 0.15 (R. F. J. van der Burg et al. 2015). All of these archival results have been corrected to the density down to M* = 108.5M⊙ using their total SMF.
Paper: How Fast Could Supermassive Black Holes Grow at the Epoch of Reionization?
Authors: Ziyong Wu, Renyue Cen, Romain Teyssier
Figure caption: The dark matter projected density (bottom), gas projected density (top left), and gas temperature plot (top right) at z = 10. All the length units in the figure are in physical units. The zoom-in region contains two halos with 2 × 109 M⊙ < Mhalo < 5 × 109 M⊙ at z ∼ 10.
Paper: The Bigfoot: A Footprint of a Coma Cluster Progenitor at z = 3.98
Authors: Hanwen Sun, Tao Wang, Emanuele Daddi, Qiaoyang Hao, Ke Xu, David Elbaz, Luwenjia Zhou, Houjun Mo, Huiyuan Wang, Longyue Chen, Yangyao Chen, Shuowen Jin, Yipeng Lyu, Nikolaj Sillassen, Kai Wang, Tiancheng Yang
Figure caption: The RGB composite color image of the most massive protocluster core (0217A). The red, green, and blue channels correspond to the JWST/NIRCam F444W, F277W, and F150W filters, respectively. Member galaxies are overlaid as open circles: massive SFGs (M* > 1010M⊙) in yellow, low-mass SFGs (M* < 109M⊙) in cyan, and quiescent galaxies (QGs, including both passive galaxies and poststarburst galaxies) in red.