adsabs/AstroCLIMB huggingface dataset:
Paper: The First Day of a Type Ia Supernova from a Double-degenerate Binary
Authors: Gabriel Kumar, Logan J. Prust, Lars Bildsten
Figure caption: Ideal momentum transfer efficiency ηideal vs. R/a, based on Equation (A5). For R/a = 0, Equation (A5) reproduces the result for planar ejecta ηideal = 1/2.
Paper: Classifying Metal-poor Stars with Machine Learning Using Nucleosynthesis Calculations
Authors: Nicole Vassh, Yilin Wang, Richard M. Woloshyn, Michelle P. Kuchera, Maude Larivière, Kayle Majic, Benoit Côté
Figure caption: (Top) Abundance patterns for the r-process calculations using the hydrodynamic simulations of Just et al. (pink) and Radice et al. (red). (Middle) Abundance patterns for the s-process calculations from Monash models (light blue) and FRUITY simulations (dark blue). (Bottom) Stellar abundance patterns for all metal-poor stars considered in this work (data from JINAbase) as compared to the solar pattern broken down into its r and s contributions (from C. Sneden et al. 2008).
Paper: Classifying Metal-poor Stars with Machine Learning Using Nucleosynthesis Calculations
Authors: Nicole Vassh, Yilin Wang, Richard M. Woloshyn, Michelle P. Kuchera, Maude Larivière, Kayle Majic, Benoit Côté
Figure caption: Histograms showing the binary classification of the nucleosynthesis data (BC-L model here). Minimal separation for the r and s histograms is shown for training including (a) Er and (b) Pb. Maximal separation is shown for training including (c) Er and (d) Pb. For the results in the bottom panels, the model is trained for 10,000 epochs, and model weights from the epoch with the lowest validation loss are chosen as the final model. How the ML model classifies the stars in each case is also shown. For comparison, the color-coding of each star represents its JINAbase classification, of which the ML model is never informed.
Paper: Classifying Metal-poor Stars with Machine Learning Using Nucleosynthesis Calculations
Authors: Nicole Vassh, Yilin Wang, Richard M. Woloshyn, Michelle P. Kuchera, Maude Larivière, Kayle Majic, Benoit Côté
Figure caption: The two-dimensional latent space values (labeled as dimension 1 and dimension 2) showing the one-class classification of the nucleosynthesis data when the model is trained on either r (top panels) or s ​​​​​​ (bottom panels) data (OCC-L model here). Cases trained on r include Ba, lanthanides (Z = 57–70), and either (a-i) Er or (a-ii) Pb. The cases trained on s also include either (b-i) Er or (b-ii) Pb. The ML model classification for the stars is also shown. For comparison, the color-coding of each star represents its JINAbase classification, of which the ML model is never informed.
Paper: Classifying Metal-poor Stars with Machine Learning Using Nucleosynthesis Calculations
Authors: Nicole Vassh, Yilin Wang, Richard M. Woloshyn, Michelle P. Kuchera, Maude Larivière, Kayle Majic, Benoit Côté
Figure caption: (Left panels) Same as Figure 1 but now with i-process nucleosynthesis calculations (yellow) shown for comparison. (Middle and right panels) Same as Figure 3 but with the i-process calculations and stars currently labeled as “i” run through the OCCs trained on r (top panels) or s (bottom panels).
Paper: Photospheric Radius Expansion Thermonuclear Burst and X-Ray Reflection from the Neutron Star X-Ray Binary 4U 1702-429
Authors: Manoj Mandal, Sachindra Naik, Gaurava Kumar Jaisawal
Figure caption: The light curves of 4U 1702–429 are shown for 4 different energy ranges using NICER observation. The bottom panel represents the evolution of the hardness ratio (HR) during the thermonuclear burst. The shaded region indicates a weak secondary peak in the burst light curve.
Paper: Classifying Metal-poor Stars with Machine Learning Using Nucleosynthesis Calculations
Authors: Nicole Vassh, Yilin Wang, Richard M. Woloshyn, Michelle P. Kuchera, Maude Larivière, Kayle Majic, Benoit Côté
Figure caption: ROC curves using the predicted outputs using the BC-L network trained on nine elements up to Er shown at various epochs, where epoch 118 corresponds to the state of minimum separation.
Paper: Classifying Metal-poor Stars with Machine Learning Using Nucleosynthesis Calculations
Authors: Nicole Vassh, Yilin Wang, Richard M. Woloshyn, Michelle P. Kuchera, Maude Larivière, Kayle Majic, Benoit Côté
Figure caption: Confusion matrix, where TP, FP, FN, and TN are defined based on their true and predicted labels.
Paper: Classifying Metal-poor Stars with Machine Learning Using Nucleosynthesis Calculations
Authors: Nicole Vassh, Yilin Wang, Richard M. Woloshyn, Michelle P. Kuchera, Maude Larivière, Kayle Majic, Benoit Côté
Figure caption: Training and validation losses as the BC-L network evolves over 10,000 epochs using nine elements (features) up to Er and up to Pb, respectively.
Paper: Classifying Metal-poor Stars with Machine Learning Using Nucleosynthesis Calculations
Authors: Nicole Vassh, Yilin Wang, Richard M. Woloshyn, Michelle P. Kuchera, Maude Larivière, Kayle Majic, Benoit Côté
Figure caption: Schematic of the autoencoder architecture used for OCC.
Paper: Classifying Metal-poor Stars with Machine Learning Using Nucleosynthesis Calculations
Authors: Nicole Vassh, Yilin Wang, Richard M. Woloshyn, Michelle P. Kuchera, Maude Larivière, Kayle Majic, Benoit Côté
Figure caption: Latent space results for MHD supernova r-process cases compared to where r, s training sets and stellar data lie.
Paper: Photospheric Radius Expansion Thermonuclear Burst and X-Ray Reflection from the Neutron Star X-Ray Binary 4U 1702-429
Authors: Manoj Mandal, Sachindra Naik, Gaurava Kumar Jaisawal
Figure caption: Evolution of spectral parameters of 4U 1702–429 obtained with the disk reflection modeling relxillNS approach during the evolution of the thermonuclear burst with NICER. The reported flux values are in units of 10−8 erg cm−2 s−1. The X-axis indicates the time from the rise of the burst.
Paper: Photospheric Radius Expansion Thermonuclear Burst and X-Ray Reflection from the Neutron Star X-Ray Binary 4U 1702-429
Authors: Manoj Mandal, Sachindra Naik, Gaurava Kumar Jaisawal
Figure caption: Evolution of different spectral parameters of 4U 1702–429 obtained from the spectral modeling of the data with the variable persistent emission method (fa method; left panel) and without the fa method (right panel) during the thermonuclear burst detected with NICER. The top panel shows the 0.5 s binned NICER burst light curve in the 0.5–10 keV energy band. The reported flux values are in units of 10−8 erg cm−2 s−1. The expansion of the NS photosphere is observed during the burst.
Paper: Photospheric Radius Expansion Thermonuclear Burst and X-Ray Reflection from the Neutron Star X-Ray Binary 4U 1702-429
Authors: Manoj Mandal, Sachindra Naik, Gaurava Kumar Jaisawal
Figure caption: Best-fit NuSTAR spectrum of 4U 1702–429 with model tbabs × (bbodyrad + relxill). The bottom panel represents the residuals obtained from the spectral fit.
Paper: Photospheric Radius Expansion Thermonuclear Burst and X-Ray Reflection from the Neutron Star X-Ray Binary 4U 1702-429
Authors: Manoj Mandal, Sachindra Naik, Gaurava Kumar Jaisawal
Figure caption: The MCMC chain corner plot is shown for the best-fitting spectra with the model M1 (top panel) and model M2 (bottom panel).
Paper: Photospheric Radius Expansion Thermonuclear Burst and X-Ray Reflection from the Neutron Star X-Ray Binary 4U 1702-429
Authors: Manoj Mandal, Sachindra Naik, Gaurava Kumar Jaisawal
Figure caption: The residuals obtained from the spectral fitting of the persistent emission of 4U 1702–429 using NuSTAR observation. The top and bottom panels show the residuals obtained by fitting the data with tbabs × nthcomp model and tbabs × cutoffpl model, respectively. An iron line ∼6.4 keV and a Compton hump at around 20 keV are visible in both cases.
Paper: Photospheric Radius Expansion Thermonuclear Burst and X-Ray Reflection from the Neutron Star X-Ray Binary 4U 1702-429
Authors: Manoj Mandal, Sachindra Naik, Gaurava Kumar Jaisawal
Figure caption: Evolution of spectral parameters of 4U 1702–429 obtained with the spectral modeling of data with the absorbed blackbody model during three thermonuclear bursts observed with XMM-Newton EPIC-PN. The reported flux values are in units of 10−8 erg cm−2 s−1. The top panel shows the 0.5 s binned EPIC-PN light curve during the burst.
Paper: Exploring the Nature of Little Red Dots: Constraints on Active Galactic Nucleus and Stellar Contributions from PRIMER MIRI Imaging
Authors: Gene C. K. Leung, Steven L. Finkelstein, Pablo G. Pérez-González, Alexa M. Morales, Anthony J. Taylor, Guillermo Barro, Dale D. Kocevski, Hollis B. Akins, Adam C. Carnall, Óscar A. Chávez Ortiz, Nikko J. Cleri, Fergus Cullen, Callum T. Donnan, James S. Dunlop, Richard S. Ellis, Norman A. Grogin, Michaela Hirschmann, Anton M. Koekemoer, Vasily Kokorev, Ray A. Lucas, Derek J. McLeod, Casey Papovich, L. Y. Aaron Yung
Figure caption: AGN bolometric luminosity in the AGN-only fit vs. F444W magnitude (left) and photometric redshift (right). The LRDs in our sample are color-coded by their redshift bins. The LRDs detected in F1800W are shown as large orange points. The AGN bolometric luminosities of the LRDs measured by the Hα emission line in J. E. Greene et al. (2024) are shown as gray points. The blue dashed (gray dotted) line shows the best-fit linear relation between the AGN bolometric luminosity and F444W magnitude to the data in this study for the 4.5 < z < 7 redshift bin (the data in J. E. Greene et al. 2024). The downward arrows indicate the direction in which the bolometric luminosity would change if the Eddington ratio is decreased. The derived AGN bolometric luminosity in this study follows a very similar slope to that in J. E. Greene et al. (2024), but is systematically higher by 0.6 dex. The broad-line-detected LRD in our sample, UDS 39469 (A. J. Taylor et al. 2024), is shown with red outlines, whose bolometric luminosity derived from the SED modeling (circle) is 0.7 dex higher than the broad Hα emission line (square), comparable to the difference in the best-fit relation. This could suggest that the AGN contribution to the rest-optical continuum is less than unity.
Paper: Exploring the Nature of Little Red Dots: Constraints on Active Galactic Nucleus and Stellar Contributions from PRIMER MIRI Imaging
Authors: Gene C. K. Leung, Steven L. Finkelstein, Pablo G. Pérez-González, Alexa M. Morales, Anthony J. Taylor, Guillermo Barro, Dale D. Kocevski, Hollis B. Akins, Adam C. Carnall, Óscar A. Chávez Ortiz, Nikko J. Cleri, Fergus Cullen, Callum T. Donnan, James S. Dunlop, Richard S. Ellis, Norman A. Grogin, Michaela Hirschmann, Anton M. Koekemoer, Vasily Kokorev, Ray A. Lucas, Derek J. McLeod, Casey Papovich, L. Y. Aaron Yung
Figure caption: Galaxy properties from the two-component galaxy-only fit. For LRDs where two components are significantly detected, the rest-UV component is shown in blue, and the rest-optical component is shown in orange. The two components of the same LRD are connected by gray dashed lines. LRDs where only one component is required are shown as solid orange points. Left: distribution of AV vs. stellar mass. Right: distribution of age vs. stellar mass. The rest-UV components are substantially less dusty than the rest-optical components, but have similar ages to the latter. This is consistent with the picture that the rest-UV continuum originates from the scattered light of the same stellar population that produces the rest-optical emission.
Paper: Exploring the Nature of Little Red Dots: Constraints on Active Galactic Nucleus and Stellar Contributions from PRIMER MIRI Imaging
Authors: Gene C. K. Leung, Steven L. Finkelstein, Pablo G. Pérez-González, Alexa M. Morales, Anthony J. Taylor, Guillermo Barro, Dale D. Kocevski, Hollis B. Akins, Adam C. Carnall, Óscar A. Chávez Ortiz, Nikko J. Cleri, Fergus Cullen, Callum T. Donnan, James S. Dunlop, Richard S. Ellis, Norman A. Grogin, Michaela Hirschmann, Anton M. Koekemoer, Vasily Kokorev, Ray A. Lucas, Derek J. McLeod, Casey Papovich, L. Y. Aaron Yung
Figure caption: Stellar mass vs. redshift for the LRDs in this study. The stellar masses derived from the galaxy-only fit without MIRI photometry are shown in green, those from the galaxy-only fit with MIRI photometry in red, and those from the hybrid fit (where the rest-optical emission is attributed to an AGN) in violet. We also include the limiting stellar mass expected for baryon conversion efficiencies of 1 and 0.2 as black solid and dashed lines, respectively. The inclusion of MIRI photometry in the galaxy-only fit significantly reduces the stellar mass of LRDs at z ≳ 7, bringing them back to the expected range. Very high baryon conversion efficiencies of >0.3 are still inferred in 10 LRDs when considering the galaxy-only model with MIRI photometry, suggesting that the galaxy-only model could overestimate their stellar mass. With the hybrid model, the stellar mass of all LRDs is within expectations.
Paper: Exploring the Nature of Little Red Dots: Constraints on Active Galactic Nucleus and Stellar Contributions from PRIMER MIRI Imaging
Authors: Gene C. K. Leung, Steven L. Finkelstein, Pablo G. Pérez-González, Alexa M. Morales, Anthony J. Taylor, Guillermo Barro, Dale D. Kocevski, Hollis B. Akins, Adam C. Carnall, Óscar A. Chávez Ortiz, Nikko J. Cleri, Fergus Cullen, Callum T. Donnan, James S. Dunlop, Richard S. Ellis, Norman A. Grogin, Michaela Hirschmann, Anton M. Koekemoer, Vasily Kokorev, Ray A. Lucas, Derek J. McLeod, Casey Papovich, L. Y. Aaron Yung
Figure caption: Left: the F444W magnitude vs. photometric redshift in D. D. Kocevski et al. (2024) for the LRD sample in this paper. The six LRDs with a significant detection in F1800W at S/N > 5 are shown as orange points. The horizontal error bars show the 68% confidence intervals of the photometric redshift. The LRDs detected in F1800W are generally bright, with F444W magnitude of <25 AB mag. Right: the F277W − F444W vs. F444W − F1800W color–color diagram. The LRDs are red in F277W − F444W by selection. The LRDs detected in F1800W span a wide range of F444W − F1800W colors. For the rest of the sample, the 5σ upper limit on the F444W − F1800W color is shown.
Paper: Exploring the Nature of Little Red Dots: Constraints on Active Galactic Nucleus and Stellar Contributions from PRIMER MIRI Imaging
Authors: Gene C. K. Leung, Steven L. Finkelstein, Pablo G. Pérez-González, Alexa M. Morales, Anthony J. Taylor, Guillermo Barro, Dale D. Kocevski, Hollis B. Akins, Adam C. Carnall, Óscar A. Chávez Ortiz, Nikko J. Cleri, Fergus Cullen, Callum T. Donnan, James S. Dunlop, Richard S. Ellis, Norman A. Grogin, Michaela Hirschmann, Anton M. Koekemoer, Vasily Kokorev, Ray A. Lucas, Derek J. McLeod, Casey Papovich, L. Y. Aaron Yung
Figure caption: AGN properties derived from the AGN-only SED fits. Left: the hot dust fraction vs. the F444W magnitude. Middle: AV vs. F444W magnitude. Right: hot dust fraction vs. AV. The hot dust fraction is low (≲0.2) in the majority of the LRDs, with the exception of UDS 9235. Our results also show a high AV of ≳2, consistent with a dust-obscured AGN producing the rest-optical continuum. There is no correlation between fHD and AV, suggesting that the dust responsible for the reddening of the AGN does not reside in a hot dust torus.
Paper: Exploring the Nature of Little Red Dots: Constraints on Active Galactic Nucleus and Stellar Contributions from PRIMER MIRI Imaging
Authors: Gene C. K. Leung, Steven L. Finkelstein, Pablo G. Pérez-González, Alexa M. Morales, Anthony J. Taylor, Guillermo Barro, Dale D. Kocevski, Hollis B. Akins, Adam C. Carnall, Óscar A. Chávez Ortiz, Nikko J. Cleri, Fergus Cullen, Callum T. Donnan, James S. Dunlop, Richard S. Ellis, Norman A. Grogin, Michaela Hirschmann, Anton M. Koekemoer, Vasily Kokorev, Ray A. Lucas, Derek J. McLeod, Casey Papovich, L. Y. Aaron Yung
Figure caption: Visualization of the components in our AGN-only SED model based on the quasar templates in M. J. Temple et al. (2021). The red solid lines show the accretion disk emission subject to a varying degree of dust reddening. The violet dashed lines show the emission from the hot dust at 1240 K with variable hot dust fractions (fHD). The green dotted lines show the scattered light represented by a fraction of the unobscured accretion disk emission.
Paper: Exploring the Nature of Little Red Dots: Constraints on Active Galactic Nucleus and Stellar Contributions from PRIMER MIRI Imaging
Authors: Gene C. K. Leung, Steven L. Finkelstein, Pablo G. Pérez-González, Alexa M. Morales, Anthony J. Taylor, Guillermo Barro, Dale D. Kocevski, Hollis B. Akins, Adam C. Carnall, Óscar A. Chávez Ortiz, Nikko J. Cleri, Fergus Cullen, Callum T. Donnan, James S. Dunlop, Richard S. Ellis, Norman A. Grogin, Michaela Hirschmann, Anton M. Koekemoer, Vasily Kokorev, Ray A. Lucas, Derek J. McLeod, Casey Papovich, L. Y. Aaron Yung
Figure caption: Effective radius in the F444W filter vs. stellar mass. The red symbols show the stellar mass estimates from the galaxy-only fit, while the violet symbols show those from the hybrid fit. Upper limits using the HWHM of the F444W filter are shown with triangles for the 92 LRDs that are not significantly resolved. The three resolved LRDs are highlighted by black outlines. Values for a collection of z = 5–7 galaxies in CEERS from W. Sun et al. (2024) are shown as gray points. The best-fit size–mass relations for elliptical galaxies at z = 0.25 (A. van der Wel et al. 2014) and typical star-forming galaxies at z = 6–9 (N. Allen et al. 2025) and their 1σ scatter are shown as orange and blue lines and shaded regions, respectively. We also show lines of constant predicted velocity dispersion from J. F. W. Baggen et al. (2024) as green dotted lines. The stellar mass estimates from the galaxy-only model result in size–mass relations deviating from the z = 6–9 best fit by >1σ–2σ, implying high stellar mass densities of ∼105 M⊙ pc−2. These high densities are also 1–2 dex higher than those of local ellipticals, suggesting a drastic evolution in stellar mass distribution is required to produce present-day galaxies. The hybrid fit results in lower stellar masses that are largely in agreement with the best-fit relation at z = 6–9 within its intrinsic scatter. Stellar mass densities inferred from the galaxy-only model are capable of producing velocity dispersions of at least a few hundred kilometers per second, similar to broad emission lines in LRDs.
Paper: Exploring the Nature of Little Red Dots: Constraints on Active Galactic Nucleus and Stellar Contributions from PRIMER MIRI Imaging
Authors: Gene C. K. Leung, Steven L. Finkelstein, Pablo G. Pérez-González, Alexa M. Morales, Anthony J. Taylor, Guillermo Barro, Dale D. Kocevski, Hollis B. Akins, Adam C. Carnall, Óscar A. Chávez Ortiz, Nikko J. Cleri, Fergus Cullen, Callum T. Donnan, James S. Dunlop, Richard S. Ellis, Norman A. Grogin, Michaela Hirschmann, Anton M. Koekemoer, Vasily Kokorev, Ray A. Lucas, Derek J. McLeod, Casey Papovich, L. Y. Aaron Yung
Figure caption: Black hole mass vs. stellar mass. The LRDs in this study assuming the hybrid (minimal M*) model are shown as blue circles, while those detected in F1800W are shown as orange circles. We also show the sample median for the minimal M* values as a light blue square, as well as that for the maximal M* values from the galaxy-only fit as a dark blue square. Literature values for high-redshift AGNs observed by JWST from D. D. Kocevski et al. (2023), R. Maiolino et al. (2023), Y. Harikane et al. (2023), and M. Yue et al. (2024b) are shown as gray points. For context, we also plot the best-fit MBH–M* relation and its scatter at high redshift in F. Pacucci et al. (2023) as a red line and shaded region, and those in the local Universe in A. E. Reines & M. Volonteri (2015) as a green line and shaded region. The MBH/M* ratios inferred from the hybrid model are higher than the high-redshift relation by ∼1 dex, while the galaxy-only model produces ratios at the lower end of the high-redshift relation. If the AGN contribution to the rest-optical continuum is less than unity, the stellar mass of the hybrid model can be underestimated, leading to an apparent elevation in MBH/M* in the LRDs. Therefore, the rest-optical continuum of the LRDs is likely contributed by both AGN and galaxy emission. Alternatively, super-Eddington accretion could lower MBH by ∼1 dex, alleviating the tension in the MBH/M* relation.
Paper: Exploring the Nature of Little Red Dots: Constraints on Active Galactic Nucleus and Stellar Contributions from PRIMER MIRI Imaging
Authors: Gene C. K. Leung, Steven L. Finkelstein, Pablo G. Pérez-González, Alexa M. Morales, Anthony J. Taylor, Guillermo Barro, Dale D. Kocevski, Hollis B. Akins, Adam C. Carnall, Óscar A. Chávez Ortiz, Nikko J. Cleri, Fergus Cullen, Callum T. Donnan, James S. Dunlop, Richard S. Ellis, Norman A. Grogin, Michaela Hirschmann, Anton M. Koekemoer, Vasily Kokorev, Ray A. Lucas, Derek J. McLeod, Casey Papovich, L. Y. Aaron Yung
Figure caption: The mass of the central black hole assuming Eddington accretion vs. F444W magnitude. We also show the results from spectroscopic observations of LRDs in J. E. Greene et al. (2024) and broad-line AGNs in J. Matthee et al. (2024). The best-fit linear relation between MBH and F444W magnitude to the 4.5 < z < 7 LRDs in this study is shown as a blue dashed line, and spectroscopic results as a gray dotted line. The upward arrow indicates the direction in which MBH would change if the Eddington ratio is decreased, while the downward arrow indicates the direction if the AGN contribution to the rest-optical is decreased. Our results are in agreement with those of spectroscopic studies. The MBH for UDS 39469 derived from SED modeling and the broad Hα emission line are also in close agreement. Given that our AGN bolometric luminosity is likely overestimated in the AGN-only model, the actual Eddington ratios are possibly several times lower than unity.
Paper: On the Singularity Structure of Alfvénic Turbulence
Authors: N. H. Bian, Gang Li
Figure caption: P(Δz⊥, l⊥) deriving from the log-Poisson cascade model of R. Grauer et al. (1994) and H. Politano & A. Pouquet (1995). The PDFs are shifted vertically as the scale l⊥ is decreased from the integral scale L⊥ to L⊥/50.
Paper: On the Singularity Structure of Alfvénic Turbulence
Authors: N. H. Bian, Gang Li
Figure caption: The scaling exponent ζ⊥(n) for the five models given in Table 1. The K41+GS (1/3) and the IK+B (1/4) models are self-similar without intermittency. Difference of ζ⊥(n) between different multifractal models is noticeable already for n = 4.
Paper: On the Singularity Structure of Alfvénic Turbulence
Authors: N. H. Bian, Gang Li
Figure caption: The singularity spectrum C⊥(h⊥) resulting from the three multifractal models given in Table 1. Singularities with h⊥ ≤ h⊥c = 1/3 are responsible for inertial dissipation of the electromagnetic energy in the collisionless plasma.
Paper: Exploring the Nature of Little Red Dots: Constraints on Active Galactic Nucleus and Stellar Contributions from PRIMER MIRI Imaging
Authors: Gene C. K. Leung, Steven L. Finkelstein, Pablo G. Pérez-González, Alexa M. Morales, Anthony J. Taylor, Guillermo Barro, Dale D. Kocevski, Hollis B. Akins, Adam C. Carnall, Óscar A. Chávez Ortiz, Nikko J. Cleri, Fergus Cullen, Callum T. Donnan, James S. Dunlop, Richard S. Ellis, Norman A. Grogin, Michaela Hirschmann, Anton M. Koekemoer, Vasily Kokorev, Ray A. Lucas, Derek J. McLeod, Casey Papovich, L. Y. Aaron Yung
Figure caption: Same as Figure 6, but replacing the F444W magnitude with νLν at 5100 Å.
Paper: Exploring the Nature of Little Red Dots: Constraints on Active Galactic Nucleus and Stellar Contributions from PRIMER MIRI Imaging
Authors: Gene C. K. Leung, Steven L. Finkelstein, Pablo G. Pérez-González, Alexa M. Morales, Anthony J. Taylor, Guillermo Barro, Dale D. Kocevski, Hollis B. Akins, Adam C. Carnall, Óscar A. Chávez Ortiz, Nikko J. Cleri, Fergus Cullen, Callum T. Donnan, James S. Dunlop, Richard S. Ellis, Norman A. Grogin, Michaela Hirschmann, Anton M. Koekemoer, Vasily Kokorev, Ray A. Lucas, Derek J. McLeod, Casey Papovich, L. Y. Aaron Yung
Figure caption: Same as Figure 9, but replacing the F444W magnitude with νLν at 5100 Å.