adsabs/AstroCLIMB huggingface dataset:
Paper: Discovery of the Optical and Radio Counterpart to the Fast X-Ray Transient EP 240315a
Authors: J. H. Gillanders, L. Rhodes, S. Srivastav, F. Carotenuto, J. Bright, M. E. Huber, H. F. Stevance, S. J. Smartt, K. C. Chambers, T.-W. Chen, R. Fender, A. Andersson, A. J. Cooper, P. G. Jonker, F. J. Cowie, T. de Boer, N. Erasmus, M. D. Fulton, H. Gao, J. Herman, C.-C. Lin, T. Lowe, E. A. Magnier, H.-Y. Miao, P. Minguez, T. Moore, C.-C. Ngeow, M. Nicholl, Y.-C. Pan, G. Pignata, A. Rest, X. Sheng, I. A. Smith, K. W. Smith, J. L. Tonry, R. J. Wainscoat, J. Weston, S. Yang, D. R. Young
Figure caption: Optical photometry of AT 2024eju. All non-detections are represented by downward-pointing triangles (and correspond to 2σ upper limits). Error bars correspond to 1σ values. We present the data in both observer and rest frame and the flux in both magnitude and f  ν  space. The gray band represents the duration of the initial X-ray detection reported by the EP (≈1600 s; see Zhang et al. 2024c). The epoch of spectroscopic observation with Gemini North has also been marked (vertical black line). Inset: a zoom-in of the first ∼1.5 days to emphasize how close our ATLAS c-band detection was to the initial X-ray detection (≲80 observer-frame minutes, ≲800 rest-frame seconds). Note that we do not plot the late-time (T 0 + 18.42 days, observer frame) Gemini non-detections.
Paper: X-Ray View of Little Red Dots: Do They Host Supermassive Black Holes?
Authors: Tonima Tasnim Ananna, অনন্যা তনিমা তাসনিম, Ákos Bogdán, Orsolya E. Kovács, Priyamvada Natarajan, Ryan C. Hickox
Figure caption: Stacked 2–7 keV band Chandra X-ray images of LRD galaxies using different samples. The solid circular region represents a 1.″9 region and the dashed annulus shows a 3″–6″ annulus. The regions shown here are only for illustration purposes, the actual source and background regions used in our analysis were calculated using the local PSF for each observation (Section 3.2 and Appendix A). The stacked samples are as follows. Top left: the 21 individual LRDs in our sample; Top right: nine LRDs from the Greene et al. (2024) sample with broad-line Hα emission and an inferred SMBH mass. We obtain a tentative 2.6σ detection for this subset; Bottom left: 11 massive galaxies with stellar mass ≥2.5 × 109 M ⊙; Bottom right: 10 low-mass galaxies with stellar masses <2.5 × 109 M ⊙.
Paper: X-Ray View of Little Red Dots: Do They Host Supermassive Black Holes?
Authors: Tonima Tasnim Ananna, অনন্যা তনিমা তাসনিম, Ákos Bogdán, Orsolya E. Kovács, Priyamvada Natarajan, Ryan C. Hickox
Figure caption: Merged Chandra ACIS-I image of the lensing cluster, A2744, in the 2–7 keV band. The total exposure time of the merged data is ≈2.07 Ms. We focus on a sample of 23 LRDs (see Table 1) in the redshift range of z = 3–8.5 that were identified by JWST NIRCAM data (Labbe et al. 2023). The location of the galaxies is highlighted with small white circles. The Chandra X-ray data provides data for all galaxies.
Paper: Formation of a Magnetic Cloud from the Merging of Two Successive Coronal Mass Ejections
Authors: Chong Chen, Ying D. Liu, Bei Zhu, Huidong Hu, Rui Wang
Figure caption: Solar wind plasma and magnetic field parameters at Wind associated with the 2022 March 28 CMEs. From top to bottom, the panels show the pitch angle distribution of 265 eV electrons, proton density, bulk speed, proton temperature, and magnetic field strength and components, respectively. The dotted line in the fourth panel denotes the expected proton temperature calculated from the observed speed (Lopez 1987; Richardson & Cane 1995). The shaded region indicates the complex ejecta interval determined by the GS reconstruction. The red vertical dashed line denotes the observed arrival time of the shock. The blue vertical line represents the predicted arrival time of the merged front at the Earth.
Paper: Formation of a Magnetic Cloud from the Merging of Two Successive Coronal Mass Ejections
Authors: Chong Chen, Ying D. Liu, Bei Zhu, Huidong Hu, Rui Wang
Figure caption: Reconstructed cross section of the complex ejecta at Wind. Black contours are the distribution of the vector potential, and the color shading shows the value of the axial magnetic field strength. The location of the maximum axial field is indicated by the white cross. The horizontal dash line marks the trajectory of the Wind spacecraft. The thin black arrows denote the direction and magnitude of the observed magnetic field projected onto the cross section, and the thick colored arrows show the projected RTN directions.
Paper: Latitudinal Asymmetry in the Dayside Atmosphere of WASP-43b
Authors: Ryan C. Challener, Zafar Rustamkulov, Elspeth K. H. Lee, Nikole Lewis, David K. Sing, Stephan M. Birkmann, Nicolas Crouzet, Néstor Espinoza, Elena Manjavacas, Natalia Oliveros-Gomez, Jeff A. Valenti, Jingxuan Yang
Figure caption: Top: a set of 100 of the posterior distribution temperature maps, sliced at the equator and substellar meridian, showing the range of plausible maps. The vertical black lines mark the substellar point. Middle: the white-light light curve (gray), the best-fitting two-dimensional eclipse-mapping model (blue), and the associated brightness-temperature map (inset). The transit has been clipped from the data set, as ThERESA cannot currently adequately model transit events, and the amount of emission mapping information lost is small. The best-fitting model uses third-order spherical harmonics and six mapping components. The region between the vertical black lines on the inset is scanned by the stellar disk during either ingress, egress, or both. Outside these lines, the brightness temperatures are calculated from a cos(latitude)-weighted intensity average, to show that latitudinal information is unconstrained in that region. Bottom: residuals of the best-fitting model.
Paper: Latitudinal Asymmetry in the Dayside Atmosphere of WASP-43b
Authors: Ryan C. Challener, Zafar Rustamkulov, Elspeth K. H. Lee, Nikole Lewis, David K. Sing, Stephan M. Birkmann, Nicolas Crouzet, Néstor Espinoza, Elena Manjavacas, Natalia Oliveros-Gomez, Jeff A. Valenti, Jingxuan Yang
Figure caption: The difference between the white-light best-fitting map model and a uniform-planet model fit to the eclipses, to highlight the eclipse-mapping signal. The purple data points show the data phase-folded and temporally binned by a factor of 4 for visual clarity. The structure in the residuals shows a signal in the data that cannot be fit by a uniform planet model (dashed black line) but is fit well by the mapping model (purple). Vertical black lines denote the beginning and end of ingress and egress. The uniform-planet model was fit to data within ±1 hr of the eclipse midpoint to reduce the impact of the phase-curve variation, which would be fit very poorly by a uniform model. The residuals, which are the difference between the uniform-planet model and the data, show a clear structure that is fit well by the mapping model, and the shape of the residuals agree with the MIRI/LRS map (Hammond et al. 2024). The eclipses are consistent with each other.
Paper: Latitudinal Asymmetry in the Dayside Atmosphere of WASP-43b
Authors: Ryan C. Challener, Zafar Rustamkulov, Elspeth K. H. Lee, Nikole Lewis, David K. Sing, Stephan M. Birkmann, Nicolas Crouzet, Néstor Espinoza, Elena Manjavacas, Natalia Oliveros-Gomez, Jeff A. Valenti, Jingxuan Yang
Figure caption: The six highest-variance (in light-curve space) eigenmaps used to model the white-light light curve. The maps are ordered from top left to bottom right in decreasing light-curve variance. The white-light data are modeled as a linear combination of these maps and, consequentially, the map may only contain these patterns. The map uncertainties are likewise restricted. The flux units are arbitrary, as the eigenmaps are scaled by free-parameter weights in the fitting process. For visual clarity, all eigenmaps have been normalized by their maxima.
Paper: Latitudinal Asymmetry in the Dayside Atmosphere of WASP-43b
Authors: Ryan C. Challener, Zafar Rustamkulov, Elspeth K. H. Lee, Nikole Lewis, David K. Sing, Stephan M. Birkmann, Nicolas Crouzet, Néstor Espinoza, Elena Manjavacas, Natalia Oliveros-Gomez, Jeff A. Valenti, Jingxuan Yang
Figure caption: White-light transit and fit used to determine the system parameters. The residuals show some evidence of correlated noise, particularly during ingress, which could indicate asymmetries in the planetary limbs, although WASP-43 is a K star with some evidence of long-term (>15 days) rotational modulation in the light curve (Hellier et al. 2011), so starspots could also contribute to correlated noise. Detailed modeling of the transit will be explored in follow-up work.
Paper: The Complete CEERS Early Universe Galaxy Sample: A Surprisingly Slow Evolution of the Space Density of Bright Galaxies at z ∼ 8.5–14.5
Authors: Steven L. Finkelstein, Gene C. K. Leung, Micaela B. Bagley, Mark Dickinson, Henry C. Ferguson, Casey Papovich, Hollis B. Akins, Pablo Arrabal Haro, Romeel Davé, Avishai Dekel, Jeyhan S. Kartaltepe, Dale D. Kocevski, Anton M. Koekemoer, Nor Pirzkal, Rachel S. Somerville, L. Y. Aaron Yung, Ricardo O. Amorín, Bren E. Backhaus, Peter Behroozi, Laura Bisigello, Volker Bromm, Caitlin M. Casey, Óscar A. Chávez Ortiz, Yingjie Cheng, Katherine Chworowsky, Nikko J. Cleri, M. C. Cooper, Kelcey Davis, Alexander de la Vega, David Elbaz, Maximilien Franco, Adriano Fontana, Seiji Fujimoto, Mauro Giavalisco, Norman A. Grogin, Benne W. Holwerda, Marc Huertas-Company, Michaela Hirschmann, Kartheik G. Iyer, Shardha Jogee, Intae Jung, Rebecca L. Larson, Ray A. Lucas, Bahram Mobasher, Alexa M. Morales, Caroline V. Morley, Sagnick Mukherjee, Pablo G. Pérez-González, Swara Ravindranath, Giulia Rodighiero, Melanie J. Rowland, Sandro Tacchella, Anthony J. Taylor, Jonathan R. Trump, Stephen M. Wilkins
Figure caption: The top panel shows the redshift distribution of our sample (scattered vertically for clarity), while the main panel shows the cumulative surface density of galaxies per unit surface area at redshift greater than z for m < 28.5. The dotted line shows the raw counts from our CEERS z > 8.5 galaxy sample, while the shaded region shows the 68% confidence interval on the completeness-corrected surface density (including only sources with completeness estimates >20%), inclusive of photometric, photometric redshift, and Poisson uncertainties. The vertical error bars show the estimated cosmic variance uncertainty. The colored lines show predictions from a range of prelaunch simulations (including hydrodynamic, analytic, semianalytic, and semiempirical models), all also for m < 28.5. The observed surface density of galaxies lies above most predictions at z > 10, and above all except the Behroozi & Silk (2015) and FLARES models at z > 11. This confirms early results based on smaller samples that the observed abundance of z ≳ 10 galaxies significantly exceeds most prelaunch physically motivated expectations.
Paper: The Complete CEERS Early Universe Galaxy Sample: A Surprisingly Slow Evolution of the Space Density of Bright Galaxies at z ∼ 8.5–14.5
Authors: Steven L. Finkelstein, Gene C. K. Leung, Micaela B. Bagley, Mark Dickinson, Henry C. Ferguson, Casey Papovich, Hollis B. Akins, Pablo Arrabal Haro, Romeel Davé, Avishai Dekel, Jeyhan S. Kartaltepe, Dale D. Kocevski, Anton M. Koekemoer, Nor Pirzkal, Rachel S. Somerville, L. Y. Aaron Yung, Ricardo O. Amorín, Bren E. Backhaus, Peter Behroozi, Laura Bisigello, Volker Bromm, Caitlin M. Casey, Óscar A. Chávez Ortiz, Yingjie Cheng, Katherine Chworowsky, Nikko J. Cleri, M. C. Cooper, Kelcey Davis, Alexander de la Vega, David Elbaz, Maximilien Franco, Adriano Fontana, Seiji Fujimoto, Mauro Giavalisco, Norman A. Grogin, Benne W. Holwerda, Marc Huertas-Company, Michaela Hirschmann, Kartheik G. Iyer, Shardha Jogee, Intae Jung, Rebecca L. Larson, Ray A. Lucas, Bahram Mobasher, Alexa M. Morales, Caroline V. Morley, Sagnick Mukherjee, Pablo G. Pérez-González, Swara Ravindranath, Giulia Rodighiero, Melanie J. Rowland, Sandro Tacchella, Anthony J. Taylor, Jonathan R. Trump, Stephen M. Wilkins
Figure caption: The left panel shows the effective volume for our z ∼ 11 (9.7 < z ≤ 13) galaxy sample. The purple dashed line shows the maximum volume one would obtain with a 100% completeness over an ideal (though unrealistic) top-hat selection function. The colored curves show our calculated effective volumes as a function of source half-light radii. The circles show the volumes we use, calculated by weighting the volumes by the sizes of galaxies in a given magnitude bin. The size distribution of our z ∼ 11 galaxy sample is given in the bottom right panel, while the completeness as a function of size at fixed input UV absolute magnitude is shown in the top right panel. The completeness is very sensitive to the size, particularly at fainter magnitudes.
Paper: The Complete CEERS Early Universe Galaxy Sample: A Surprisingly Slow Evolution of the Space Density of Bright Galaxies at z ∼ 8.5–14.5
Authors: Steven L. Finkelstein, Gene C. K. Leung, Micaela B. Bagley, Mark Dickinson, Henry C. Ferguson, Casey Papovich, Hollis B. Akins, Pablo Arrabal Haro, Romeel Davé, Avishai Dekel, Jeyhan S. Kartaltepe, Dale D. Kocevski, Anton M. Koekemoer, Nor Pirzkal, Rachel S. Somerville, L. Y. Aaron Yung, Ricardo O. Amorín, Bren E. Backhaus, Peter Behroozi, Laura Bisigello, Volker Bromm, Caitlin M. Casey, Óscar A. Chávez Ortiz, Yingjie Cheng, Katherine Chworowsky, Nikko J. Cleri, M. C. Cooper, Kelcey Davis, Alexander de la Vega, David Elbaz, Maximilien Franco, Adriano Fontana, Seiji Fujimoto, Mauro Giavalisco, Norman A. Grogin, Benne W. Holwerda, Marc Huertas-Company, Michaela Hirschmann, Kartheik G. Iyer, Shardha Jogee, Intae Jung, Rebecca L. Larson, Ray A. Lucas, Bahram Mobasher, Alexa M. Morales, Caroline V. Morley, Sagnick Mukherjee, Pablo G. Pérez-González, Swara Ravindranath, Giulia Rodighiero, Melanie J. Rowland, Sandro Tacchella, Anthony J. Taylor, Jonathan R. Trump, Stephen M. Wilkins
Figure caption: A comparison of the photometric redshifts to the measured spectroscopic redshifts for the 17 galaxies in our initial sample with spectroscopic confirmation. With the exception of the (not shown) z ∼ 16 candidate at z spec = 4.9 (Arrabal Haro et al. 2023b), the agreement is generally good. After removal of three sources (in red) with spectroscopic redshifts below our cut of z > 8.5, we find a median (mean) z phot − z spec = 0.1 (0.3), with 8/13 sources having ∣z phot − z spec∣ < 0.2. As noted by Arrabal Haro et al. (2023a) and Fujimoto et al. (2023a), there does appear to be a mild systematic offset toward higher photometric redshifts. We also note that there are four sources with z phot > 10 observed with NIRSpec that showed no detectable signatures, which is consistent with z > 10, where all strong lines are shifted out of the NIRSpec range.
Paper: The Complete CEERS Early Universe Galaxy Sample: A Surprisingly Slow Evolution of the Space Density of Bright Galaxies at z ∼ 8.5–14.5
Authors: Steven L. Finkelstein, Gene C. K. Leung, Micaela B. Bagley, Mark Dickinson, Henry C. Ferguson, Casey Papovich, Hollis B. Akins, Pablo Arrabal Haro, Romeel Davé, Avishai Dekel, Jeyhan S. Kartaltepe, Dale D. Kocevski, Anton M. Koekemoer, Nor Pirzkal, Rachel S. Somerville, L. Y. Aaron Yung, Ricardo O. Amorín, Bren E. Backhaus, Peter Behroozi, Laura Bisigello, Volker Bromm, Caitlin M. Casey, Óscar A. Chávez Ortiz, Yingjie Cheng, Katherine Chworowsky, Nikko J. Cleri, M. C. Cooper, Kelcey Davis, Alexander de la Vega, David Elbaz, Maximilien Franco, Adriano Fontana, Seiji Fujimoto, Mauro Giavalisco, Norman A. Grogin, Benne W. Holwerda, Marc Huertas-Company, Michaela Hirschmann, Kartheik G. Iyer, Shardha Jogee, Intae Jung, Rebecca L. Larson, Ray A. Lucas, Bahram Mobasher, Alexa M. Morales, Caroline V. Morley, Sagnick Mukherjee, Pablo G. Pérez-González, Swara Ravindranath, Giulia Rodighiero, Melanie J. Rowland, Sandro Tacchella, Anthony J. Taylor, Jonathan R. Trump, Stephen M. Wilkins
Figure caption: The F200W half-light radius (measured from SExtractor) vs. F200W apparent magnitude. The gray bar shows the half-light radius from stars in the image (with the width showing the 68% spread in the values). The data points are color-coded by the difference in χ 2 between the best-fitting (sub)stellar model and the best-fitting EAZY galaxy model. Most objects are clearly resolved and thus extragalactic in origin. Only one object is formally compact with a stellar χ 2 comparable to the best-fitting EAZY model, though even for this object we conclude that it is likely extragalactic owing to its noncompact appearance in the imaging and the very large (∼4 kpc) implied distance were it stellar. We conclude that stellar contamination is not significant in our sample.
Paper: The Complete CEERS Early Universe Galaxy Sample: A Surprisingly Slow Evolution of the Space Density of Bright Galaxies at z ∼ 8.5–14.5
Authors: Steven L. Finkelstein, Gene C. K. Leung, Micaela B. Bagley, Mark Dickinson, Henry C. Ferguson, Casey Papovich, Hollis B. Akins, Pablo Arrabal Haro, Romeel Davé, Avishai Dekel, Jeyhan S. Kartaltepe, Dale D. Kocevski, Anton M. Koekemoer, Nor Pirzkal, Rachel S. Somerville, L. Y. Aaron Yung, Ricardo O. Amorín, Bren E. Backhaus, Peter Behroozi, Laura Bisigello, Volker Bromm, Caitlin M. Casey, Óscar A. Chávez Ortiz, Yingjie Cheng, Katherine Chworowsky, Nikko J. Cleri, M. C. Cooper, Kelcey Davis, Alexander de la Vega, David Elbaz, Maximilien Franco, Adriano Fontana, Seiji Fujimoto, Mauro Giavalisco, Norman A. Grogin, Benne W. Holwerda, Marc Huertas-Company, Michaela Hirschmann, Kartheik G. Iyer, Shardha Jogee, Intae Jung, Rebecca L. Larson, Ray A. Lucas, Bahram Mobasher, Alexa M. Morales, Caroline V. Morley, Sagnick Mukherjee, Pablo G. Pérez-González, Swara Ravindranath, Giulia Rodighiero, Melanie J. Rowland, Sandro Tacchella, Anthony J. Taylor, Jonathan R. Trump, Stephen M. Wilkins
Figure caption: Summary figures of the three objects in our sample with z best > 13. The top row shows 1″ cutout images in the F814W, F115W, F150W, F200W, F277W, F356W, and F444W filters (the F410M and remaining HST bands are not shown for brevity). The cyan circle in the first panel shows a 0.″2-diameter circle (the size used to measure detection significance). The bottom left panel shows the SED, with blue (green) points representing photometry from NIRCam (HST). Upper limits shown are 1σ. The bottom right panel shows the photometric redshift distribution in blue (with the corresponding best-fit model in blue in the bottom left panel). The light-red curves show the photometric redshift results when constrained to z < 7.
Paper: The Complete CEERS Early Universe Galaxy Sample: A Surprisingly Slow Evolution of the Space Density of Bright Galaxies at z ∼ 8.5–14.5
Authors: Steven L. Finkelstein, Gene C. K. Leung, Micaela B. Bagley, Mark Dickinson, Henry C. Ferguson, Casey Papovich, Hollis B. Akins, Pablo Arrabal Haro, Romeel Davé, Avishai Dekel, Jeyhan S. Kartaltepe, Dale D. Kocevski, Anton M. Koekemoer, Nor Pirzkal, Rachel S. Somerville, L. Y. Aaron Yung, Ricardo O. Amorín, Bren E. Backhaus, Peter Behroozi, Laura Bisigello, Volker Bromm, Caitlin M. Casey, Óscar A. Chávez Ortiz, Yingjie Cheng, Katherine Chworowsky, Nikko J. Cleri, M. C. Cooper, Kelcey Davis, Alexander de la Vega, David Elbaz, Maximilien Franco, Adriano Fontana, Seiji Fujimoto, Mauro Giavalisco, Norman A. Grogin, Benne W. Holwerda, Marc Huertas-Company, Michaela Hirschmann, Kartheik G. Iyer, Shardha Jogee, Intae Jung, Rebecca L. Larson, Ray A. Lucas, Bahram Mobasher, Alexa M. Morales, Caroline V. Morley, Sagnick Mukherjee, Pablo G. Pérez-González, Swara Ravindranath, Giulia Rodighiero, Melanie J. Rowland, Sandro Tacchella, Anthony J. Taylor, Jonathan R. Trump, Stephen M. Wilkins
Figure caption: The symbols show our sample of 88 z > 8.5 galaxy candidates in a plane of F277W magnitude versus redshift, with the different colors representing the different redshift samples. Squares denote objects with spectroscopic confirmation, while the circles are plotted at the photometric redshifts. Triangles denote objects with spectroscopic observations but no confirmation. The small star denotes Maisie’s Galaxy (Finkelstein et al. 2022b), one of the first JWST very high redshift galaxy discoveries, while the small circle denotes CEERS-1019, a confirmed z = 8.7 galaxy that appears to have broad Hβ emission, indicative of an active supermassive black hole (Larson et al. 2023a). The background shading shows the completeness (inclusive of both photometric and sample selection completeness) of our sample (for sources with half-light radii of 3.3 pixels), as described in Section 4.1; the black line shows the 20% completeness contour.
Paper: The Complete CEERS Early Universe Galaxy Sample: A Surprisingly Slow Evolution of the Space Density of Bright Galaxies at z ∼ 8.5–14.5
Authors: Steven L. Finkelstein, Gene C. K. Leung, Micaela B. Bagley, Mark Dickinson, Henry C. Ferguson, Casey Papovich, Hollis B. Akins, Pablo Arrabal Haro, Romeel Davé, Avishai Dekel, Jeyhan S. Kartaltepe, Dale D. Kocevski, Anton M. Koekemoer, Nor Pirzkal, Rachel S. Somerville, L. Y. Aaron Yung, Ricardo O. Amorín, Bren E. Backhaus, Peter Behroozi, Laura Bisigello, Volker Bromm, Caitlin M. Casey, Óscar A. Chávez Ortiz, Yingjie Cheng, Katherine Chworowsky, Nikko J. Cleri, M. C. Cooper, Kelcey Davis, Alexander de la Vega, David Elbaz, Maximilien Franco, Adriano Fontana, Seiji Fujimoto, Mauro Giavalisco, Norman A. Grogin, Benne W. Holwerda, Marc Huertas-Company, Michaela Hirschmann, Kartheik G. Iyer, Shardha Jogee, Intae Jung, Rebecca L. Larson, Ray A. Lucas, Bahram Mobasher, Alexa M. Morales, Caroline V. Morley, Sagnick Mukherjee, Pablo G. Pérez-González, Swara Ravindranath, Giulia Rodighiero, Melanie J. Rowland, Sandro Tacchella, Anthony J. Taylor, Jonathan R. Trump, Stephen M. Wilkins
Figure caption: A comparison of the observed z ∼ 11 UV luminosity function from CEERS and NGDEEP (symbols are the same as in the top panel of Figure 9) to model predictions. Prelaunch predictions from FLARES, DELPHI, UniverseMachine, THESAN, and BlueTides are shown as thin gray lines, while the colored lines show more recent predictions from Ferrara et al. (2023; green), Dekel et al. (2023; the blue shaded region shows a range of maximum SFE from 0.2 to 1), Shen et al. (2023; yellow; the dashed line includes a strong stochastic star formation component), Yung et al. (2024a; red; the dashed line indicates a top-heavy IMF UV luminosity enhancement of 3×), and Jones et al. (2024; purple). The thick gray line shows the empirical DPL luminosity function from Finkelstein & Bagley (2022) extrapolated to z = 11. These predictions show that a variety of potential physical solutions can predict a z ∼ 11 luminosity function in agreement with observations.