adsabs/AstroCLIMB huggingface dataset:
Paper: NEID Reveals That the Young Warm Neptune TOI-2076 b Has a Low Obliquity
Authors: Robert C. Frazier, Gudmundur Stefánsson, Suvrath Mahadevan, Samuel W. Yee, Caleb I. Cañas, Joshua N. Winn, Jacob Luhn, Fei Dai, Lauren Doyle, Heather Cegla, Shubham Kanodia, Paul Robertson, John Wisniewski, Chad F. Bender, Jiayin Dong, Arvind F. Gupta, Samuel Halverson, Suzanne Hawley, Leslie Hebb, Rae Holcomb, Adam Kowalski, Jessica Libby-Roberts, Andrea S. J. Lin, Michael W. McElwain, Joe P. Ninan, Cristobal Petrovich, Arpita Roy, Christian Schwab, Ryan C. Terrien, Jason T. Wright
Figure caption: Sky-projected obliquities (a, c) and 3D obliquities (b, d) for planetary systems as a function of age for single-transiting (a, b), and multi-transiting (c, d) systems. Planets with masses >0.3 M  J  and a/R ⋆ < 10 are classified as hot Jupiters (black points), and as warm Jupiters if a/R ⋆ > 10 (orange points). Planets with masses <0.3 M  J  are classified as sub-Saturns regardless of the value of a/R ⋆. This classification system is adopted from Albrecht et al. (2022). Despite a lack of a mass measurement of TOI-2076 b we classify it as a sub-Saturn due to its radius and distance. The position of TOI-2076 b is highlighted in red. Obliquity measurements for systems excluding TOI-2076 are drawn from Albrecht et al. (2022), Dai et al. (2023), Bourrier et al. (2023), and the TEPCAT database (Southworth 2011) where the error in the sky-projected obliquity was Δλ < 40°, and the fractional error on the age of the system was less than 90%. W107b denotes WASP-107b.
Paper: NEID Reveals That the Young Warm Neptune TOI-2076 b Has a Low Obliquity
Authors: Robert C. Frazier, Gudmundur Stefánsson, Suvrath Mahadevan, Samuel W. Yee, Caleb I. Cañas, Joshua N. Winn, Jacob Luhn, Fei Dai, Lauren Doyle, Heather Cegla, Shubham Kanodia, Paul Robertson, John Wisniewski, Chad F. Bender, Jiayin Dong, Arvind F. Gupta, Samuel Halverson, Suzanne Hawley, Leslie Hebb, Rae Holcomb, Adam Kowalski, Jessica Libby-Roberts, Andrea S. J. Lin, Michael W. McElwain, Joe P. Ninan, Cristobal Petrovich, Arpita Roy, Christian Schwab, Ryan C. Terrien, Jason T. Wright
Figure caption: TESS lightcurves of TOI-2076 from (A) Sector 16, (B) Sector 23, and (C) Sector 50. The top row shows the TESS photometry (blue points) with along with a transit model for TOI-2076 b + GP model (red) to account for stellar activity. The middle panel shows the photometry after subtracting the quasi-periodic GP model, revealing the TOI-2076 b transits. Panel (D) shows the phase-folded TESS photometry phased to the orbital period of TOI-2076 b, with the transit model overlaid.
Paper: NEID Reveals That the Young Warm Neptune TOI-2076 b Has a Low Obliquity
Authors: Robert C. Frazier, Gudmundur Stefánsson, Suvrath Mahadevan, Samuel W. Yee, Caleb I. Cañas, Joshua N. Winn, Jacob Luhn, Fei Dai, Lauren Doyle, Heather Cegla, Shubham Kanodia, Paul Robertson, John Wisniewski, Chad F. Bender, Jiayin Dong, Arvind F. Gupta, Samuel Halverson, Suzanne Hawley, Leslie Hebb, Rae Holcomb, Adam Kowalski, Jessica Libby-Roberts, Andrea S. J. Lin, Michael W. McElwain, Joe P. Ninan, Cristobal Petrovich, Arpita Roy, Christian Schwab, Ryan C. Terrien, Jason T. Wright
Figure caption: Comparing the RM fit to “blue-only” RVs (a) and “red-only” RVs (b). The RV curve for the “blue-only” RV orders spans orders from 3975–6447 Å and the “red-only” orders span orders from 6447–8920 Å. For comparison, the slope of the “white-light” RV model used in the full analysis is overplotted as the gray-dashed line in both panels. The slope in the blue orders is steeper than in the red, suggesting the RV slope is due to stellar activity such as a spot on the surface of the star.
Paper: Evolution of the Postmerger Remnants from the Coalescence of Oxygen–Neon and Carbon–Oxygen White Dwarf Pairs
Authors: Chengyuan Wu, Heran Xiong, Jie Lin, Yunlang Guo, Xiaofeng Wang, Zhanwen Han, Bo Wang
Figure caption: Example of the evolution of two merger remnants (a 1.1 M ⊙ ONe WD merges with a 0.8 M ⊙ CO WD, M tot = 1.90 M ⊙; a 1.1 M ⊙ ONe WD merges with a 0.85 M ⊙ CO WD, M tot = 1.95 M ⊙). Panel (a): HRD. Panel (b): central density–temperature evolution. Panels (c) and (d): elemental abundance distributions of 1.90 and 1.95 M ⊙ merger remnants at the final stage of their evolution just prior to the explosions. In panels (a) and (b), diamonds represent the position of Ne ignition, whereas circles and triangles represent every 1000 and 100 yr after merger, respectively. Squares in panel (b) represent the position of the final evolutionary stage, near which the corresponding evolutionary times are labeled. Black dotted lines in panel (b) represent the carbon- and oxygen-burning lines, whereas brown and magenta dotted lines represent the starting lines of the electron-capture reactions of 24Mg and 20Ne. Note that the diamond on the blue line of panel (b) is out of range.
Paper: Evolution of the Postmerger Remnants from the Coalescence of Oxygen–Neon and Carbon–Oxygen White Dwarf Pairs
Authors: Chengyuan Wu, Heran Xiong, Jie Lin, Yunlang Guo, Xiaofeng Wang, Zhanwen Han, Bo Wang
Figure caption: Initial profiles and evolutionary tracks of 1.90 and 1.95 M ⊙ merger remnants with different envelope entropies. Panels (a) and (b): initial T–M r profiles. The red (blue) solid line represents our fiducial model, whereas the magenta (cyan) double dotted–dashed and gold (navy) dotted lines represent remnants with lower (﹩\mathrm{ln}({s}_{\mathrm{env}}/\mathrm{erg}\,{{\rm{g}}}^{-1}\,{{\rm{K}}}^{-1})=8.7﹩) and higher (﹩\mathrm{ln}({s}_{\mathrm{env}}/\mathrm{erg}\,{{\rm{g}}}^{-1}\,{{\rm{K}}}^{-1})=9.1﹩) envelope entropies, respectively. Panels (c) and (d): evolutionary tracks of merger remnants in the ﹩\mathrm{log}{T}_{{\rm{c}}}-\mathrm{log}{\rho }_{{\rm{c}}}﹩ diagram.
Paper: Evolution of the Postmerger Remnants from the Coalescence of Oxygen–Neon and Carbon–Oxygen White Dwarf Pairs
Authors: Chengyuan Wu, Heran Xiong, Jie Lin, Yunlang Guo, Xiaofeng Wang, Zhanwen Han, Bo Wang
Figure caption: Evolutionary tracks of different remnants (﹩{M}_{\mathrm{ONe}}^{{\rm{i}}}=1.10{M}_{\odot }﹩) in the HRD and central temperature–density profile. Black dotted lines in panel (b) represent the carbon- and oxygen-burning conditions, whereas brown and magenta dotted lines represent the starting lines of the electron-capture reactions of 24Mg and 20Ne. The gray vertical line in panel (b) represents the critical density, below which the explosion of the core will lead to the formation of an ONeFe WD and above which will lead to the formation of an NS.
Paper: Evolution of the Postmerger Remnants from the Coalescence of Oxygen–Neon and Carbon–Oxygen White Dwarf Pairs
Authors: Chengyuan Wu, Heran Xiong, Jie Lin, Yunlang Guo, Xiaofeng Wang, Zhanwen Han, Bo Wang
Figure caption: Evolution of 1.90 and 1.95 M ⊙ ONe+CO WD merger remnants under different wind mass-loss prescriptions. Panel (a): HRD. The representatives of each line are labeled. Squares on each line represent the positions on the HRD of the corresponding models when supernova explosions occur. Panel (b): evolution of mass-loss rate.
Paper: Evolution of the Postmerger Remnants from the Coalescence of Oxygen–Neon and Carbon–Oxygen White Dwarf Pairs
Authors: Chengyuan Wu, Heran Xiong, Jie Lin, Yunlang Guo, Xiaofeng Wang, Zhanwen Han, Bo Wang
Figure caption: Main properties of the merger remnants (﹩{T}_{\max }﹩ in panel (a), core mass in panel (b), envelope mass in panel (c), and disk mass in panel (d)) with different initial ONe and CO WD masses. Red, green, and blue filled circles in each panel represent the parameters of the merger remnants with initial ONe WD masses equal to 1.10, 1.15, and 1.20 M ⊙ in our models, whereas gray diamonds in each panel represent the corresponding parameters resulting from Dan et al. (2014).
Paper: Evolution of the Postmerger Remnants from the Coalescence of Oxygen–Neon and Carbon–Oxygen White Dwarf Pairs
Authors: Chengyuan Wu, Heran Xiong, Jie Lin, Yunlang Guo, Xiaofeng Wang, Zhanwen Han, Bo Wang
Figure caption: Temperature–mass coordinate profile of the merger remnants just after the energy injection processes. Panel (a): temperature profiles of three merger remnants of different total masses and the same ONe WD mass. Panel (b): temperature profiles of three merger remnants of equal ONe WD mass and different total masses. Different lines in panel (a) and (b) represent the corresponding structures of double WD mergers with various mass ratios.
Paper: Molecular Gas Properties in Young Stellar Clusters with a Suppressed Star Cluster Wind
Authors: Sergiy Silich, Jean Turner, Jonathan Mackey, Sergio Martínez-González
Figure caption: The model-predicted D1 cloud structure. The stellar mass distribution derived from the Gaussian fit to the radio and IR integrated intensity maps is shown by the dotted line in panel (a). The solid and dashed lines in this panel display the molecular gas distributions obtained for two different η ⋆ factor values: η ⋆ = 1 (solid line) and η ⋆ = 5 (dashed line). The model-predicted velocity dispersions are shown on panel (b), where the solid and dashed lines correspond to the same models as in panel (a).
Paper: Molecular Gas Properties in Young Stellar Clusters with a Suppressed Star Cluster Wind
Authors: Sergiy Silich, Jean Turner, Jonathan Mackey, Sergio Martínez-González
Figure caption: The gas velocity gradient calculated upon the assumption that η ⋆ = 5.
Paper: Probing the Milky Way Stellar and Brown Dwarf Initial Mass Function with Modern Microlensing Observations
Authors: Gilles Chabrier, Romain Lenoble
Figure caption: Comparison of the various IMFs ﹩\xi (\mathrm{log}m)={dn}/d\mathrm{log}(m)﹩ given in Table 2: C05 (solid red), C03 (long-dashed red), K01 (long-dashed blue), A16 thin disk (short-dashed magenta), A16 thick disk (long-dashed magenta), A16 bulge (dashed–dotted green). (Note that the values of the slopes of the A16 IMFs were extended for m < 0.08 M ⊙ by their value for the thick disk, α = 0.5, to ensure a decreasing IMF in the BD domain.) The black dotted and dotted–dashed lines correspond to the functional form given in Equation (34) of Chabrier et al. (2014a), which ensures the continuity of the derivative. The dotted line reproduces the C05 IMF for parameters (m 0 = 2.0 M ⊙, m  c  = 0.182 M ⊙, σ = 0.58, A  h  = 0.35), while the dotted–dashed line corresponds to the IMF derived for the OGLE-IV central fields (cf Section 5.2.2) with (m 0 = 0.8 M ⊙, m  c  = 0.06 M ⊙, σ = 0.607, A  h  = 0.09), both with α = 1.35. The IMFs are normalized such that ﹩{\int }_{0.01{M}_{\odot }}^{100{M}_{\odot }}\xi (m){\rm{d}}m﹩ = 1. All of the IMFs are normalized at 1 M ⊙ for comparison.
Paper: Probing the Milky Way Stellar and Brown Dwarf Initial Mass Function with Modern Microlensing Observations
Authors: Gilles Chabrier, Romain Lenoble
Figure caption: Comparison of the t E histograms obtained with our fiducial Galactic model, for three IMFs (C05, C03, K01), and for β = −1.0 and −1.2 for the density of source stars (Equation (A25)), with the results of OGLE-IV all-fields observations. The efficiency of each corresponding field has been applied. The lower dashed line shows the contribution from BDs. The bin size is the same as in Mróz et al. (2019), namely, 25 bins equally spaced between ﹩\mathrm{log}{t}_{{\rm{E}}}=0.1﹩ and 2.5.
Paper: Probing the Milky Way Stellar and Brown Dwarf Initial Mass Function with Modern Microlensing Observations
Authors: Gilles Chabrier, Romain Lenoble
Figure caption: Same as Figure 2 for the OGLE-IV central fields (Mróz et al. 2017) as obtained with the same IMFs as in Figure 2 and the one portrayed in Figure 5 in Appendix B, similar to the ones derived in Chabrier et al. (2014a; see text).
Paper: Probing the Milky Way Stellar and Brown Dwarf Initial Mass Function with Modern Microlensing Observations
Authors: Gilles Chabrier, Romain Lenoble
Figure caption: Comparison of τ, Γ, and 〈t E〉 obtained with our fiducial model with the MOA II and OGLE-IV experiments for all stars as a function of latitude b for three values of the parameter β in Equation (A25). The data are averaged for ∣l∣ < 3° and binned by Δb = 0.°6. The efficiency of each corresponding OGLE-IV field has been applied, which explains the “spikes” at some latitudes.
Paper: Molecular Gas Properties in Young Stellar Clusters with a Suppressed Star Cluster Wind
Authors: Sergiy Silich, Jean Turner, Jonathan Mackey, Sergio Martínez-González
Figure caption: The model-predicted gas temperature distribution. The solid, dashed, and dotted lines present the model-predicted temperature distribution in the cases when the CR ionization rate is equal to that in our Galaxy, 10, and 100 times larger, respectively. The temperatures were calculated upon the assumption that η ⋆ = 5.
Paper: Probing the Milky Way Stellar and Brown Dwarf Initial Mass Function with Modern Microlensing Observations
Authors: Gilles Chabrier, Romain Lenoble
Figure caption: Influence of various parameters of the model upon the t E histogram distribution (bins = 1 day). Top left: bar angle; top right: bulge model; bottom left: disk model; top right: velocity dispersion.
Paper: Probing the Milky Way Stellar and Brown Dwarf Initial Mass Function with Modern Microlensing Observations
Authors: Gilles Chabrier, Romain Lenoble
Figure caption: Averaged optical depth (left column) and event rate (right column) distributions in the Galactic plane as a function of longitude (top row) and latitude (bottom row). The data are from Mróz et al. (2020). Solid lines show the results from the present calculations with the fiducial Galactic model.
Paper: Probing the Milky Way Stellar and Brown Dwarf Initial Mass Function with Modern Microlensing Observations
Authors: Gilles Chabrier, Romain Lenoble
Figure caption: Optical depth, τ, and event rate, Γ, with the model based on δ Scuti stars (Deka et al. 2022) with a C05 IMF. Calculations with β = −1.0 in Equation (A25) yield similar results.
Paper: Probing the Milky Way Stellar and Brown Dwarf Initial Mass Function with Modern Microlensing Observations
Authors: Gilles Chabrier, Romain Lenoble
Figure caption: Comparison of the normalized number of events, without taking into account the experimental efficiency, as a function of v ⊥ and D  S  x(1 − x) for the four IMFs examined in Section 5.2.2.
Paper: Evolution of the Postmerger Remnants from the Coalescence of Oxygen–Neon and Carbon–Oxygen White Dwarf Pairs
Authors: Chengyuan Wu, Heran Xiong, Jie Lin, Yunlang Guo, Xiaofeng Wang, Zhanwen Han, Bo Wang
Figure caption: Evolution of ONe+CO and CO+CO WD models when considering rotation (Ωc = 0.5 rad s−1, Ωe = 0.5 Ωcrit) and Bloecker’s wind mass-loss prescription (η B = 0.05). Panel (a): HRD. Cyan and navy lines represent the evolution of ONe+CO WD merger remnants with total masses equal to 1.60 and 1.80 M ⊙, respectively. In comparison, the evolution of double CO WD mergers with the same total masses (a mass ratio equal to 0.9) are shown as orange and red lines, respectively. Panel (b): evolution of wind mass-loss rate for the corresponding models. The brown point with an error bar in panel (a) represents the position of J005311 on the HRD, whereas the brown shaded area in panel (b) represents the estimated wind mass-loss rate of J005311. The thick solid portion of each line in panels (a) and (b) represents the position of each model when it evolves to the same temperature as J005311. Panels (c) and (d): elemental abundance distributions of ONe+CO and CO+CO WD models at the moment when they evolve to the position close to J005311 on the HRD, respectively.
Paper: Evolution of the Postmerger Remnants from the Coalescence of Oxygen–Neon and Carbon–Oxygen White Dwarf Pairs
Authors: Chengyuan Wu, Heran Xiong, Jie Lin, Yunlang Guo, Xiaofeng Wang, Zhanwen Han, Bo Wang
Figure caption: Evolutionary tracks when considering the rotational effect. Panel (a): initial rotation profile of 1.90 and 1.95 M ⊙ merger remnants. Solid, double dotted–dashed, and dotted lines represent the angular velocity, critical angular velocity, and ratio of angular and critical angular velocity of 1.90 and 1.95 M ⊙ merger remnants with different initial rotational velocities, respectively. Panel (b): evolution of the core (solid lines) and envelope (dotted lines) angular velocity of four models under different angular momentum transport prescriptions. The region inside the rectangle represents the most visible portion of the angular momentum transfer process. Panel (c): evolutionary tracks of four models compared with nonrotational models on the HRD. Similar to panel (b), the region inside the rectangle represents the most visible portion of the angular momentum transfer process.
Paper: Evolution of the Postmerger Remnants from the Coalescence of Oxygen–Neon and Carbon–Oxygen White Dwarf Pairs
Authors: Chengyuan Wu, Heran Xiong, Jie Lin, Yunlang Guo, Xiaofeng Wang, Zhanwen Han, Bo Wang
Figure caption: Evolutionary tracks of 1.60 M ⊙ ONe+CO and ONe+HeCO WD merger remnants on the HRD. Black plus signs on the red curve represent every 5000 yr during evolution, whereas blue circles on the blue curve represent every 1000 yr during evolution. The black square represents the final position on the HRD for each evolutionary track.
Paper: Evolution of the Postmerger Remnants from the Coalescence of Oxygen–Neon and Carbon–Oxygen White Dwarf Pairs
Authors: Chengyuan Wu, Heran Xiong, Jie Lin, Yunlang Guo, Xiaofeng Wang, Zhanwen Han, Bo Wang
Figure caption: Evolutionary tracks of 1.90 and 1.95 M ⊙ merger remnants in a ﹩\mathrm{log}{T}_{{\rm{c}}}\mbox{--}\mathrm{log}{\rho }_{{\rm{c}}}﹩ diagram. Solid and dashed lines represent the corresponding tracks with and without considering Urca-process cooling during evolution, respectively.
Paper: Inferring More from Less: Prospector as a Photometric Redshift Engine in the Era of JWST
Authors: Bingjie Wang, 冰洁 王, Joel Leja, Rachel Bezanson, Benjamin D. Johnson, Gourav Khullar, Ivo Labbé, Sedona H. Price, John R. Weaver, Katherine E. Whitaker
Figure caption: Here we show the technical details of the implementation of our priors from observations of galaxy evolution. (a) Number densities of galaxies, n, assuming different evolutions of the mass complete limit, M  c , are plotted as functions of redshift. Shown in black is n based on a constant M  c , while shown in dark orange is based on a constant mass-to-light ratio. The inserted panel shows M  c  as a function of z. (b) A schematic diagram demonstrating our δ formalism, which introduces mass dependence to the SFH prior. The cosmic SFRD (Behroozi et al. 2019), which we take to be the expectation value, is plotted as a function of the age of the universe in gray. At an observed redshift, z obs, the expected SFR values of a galaxy are shifted back/forward in time depending on its mass. The constructed SFH prior favors rising SFHs in the early universe, and falling SFHs in the late universe. (c) Specific SFRs of two galaxies of masses 108 M ⊙ and 1010.5 M ⊙, observed at z = 1, are plotted as functions of lookback time in blue and red, respectively. The x-axis is the time between the onset of star formation (birth of the galaxy) and z = 1. The shades indicate the 16–84th and the 2.5–97.5th percentiles of the prior distribution.
Paper: Inferring More from Less: Prospector as a Photometric Redshift Engine in the Era of JWST
Authors: Bingjie Wang, 冰洁 王, Joel Leja, Rachel Bezanson, Benjamin D. Johnson, Gourav Khullar, Ivo Labbé, Sedona H. Price, John R. Weaver, Katherine E. Whitaker
Figure caption: The three panels illustrate the difference between the proposed priors on mass, number density, and SFH of this Letter, and uniform priors (black dashed lines). (a) Mass function at z = 1 (Leja et al. 2020) is shown in red. (b) Observable galaxy number density (i.e., M  c  cut applied), as a function of redshift is plotted in red. Also shown in gray is the number density directly calculated from the mock catalog, which differs from our P(z) due to the different assumptions built in; in particular, mass functions at z ≳ 5. Nevertheless, we are able to improve the parameter inference by assuming a reasonable approximation of the mass functions used in the mock catalog. (c) Four SFHs from our prior are shown as colored lines. The x-axis is lookback time, t L, normalized by the age of the universe, t univ, at the respective z, and the y-axis is also normalized so that all SFRs can be shown on the same scale.
Paper: Inferring More from Less: Prospector as a Photometric Redshift Engine in the Era of JWST
Authors: Bingjie Wang, 冰洁 王, Joel Leja, Rachel Bezanson, Benjamin D. Johnson, Gourav Khullar, Ivo Labbé, Sedona H. Price, John R. Weaver, Katherine E. Whitaker
Figure caption: We compare the photo-z accuracy between Prospector-β and EAzY using both simulated and observed data. (Upper panel) On the left, we show true z vs. posterior median z med from a mock catalog. Red contours show results from Prospector-β, while blue contours show these from EAzY. On the right, we show residuals as histograms. We also include results based on uniform priors, plotted as gray histograms. NMAD, outlier fraction, and MBE are reported in the same colors as the corresponding histogram. (Lower panel) Same as the upper panel, but for redshifts inferred from a spec-z sample with newly acquired data from a JWST DD program. In both cases, we find that Prospector-β performs at least as accurately as EAzY.
Paper: Inferring More from Less: Prospector as a Photometric Redshift Engine in the Era of JWST
Authors: Bingjie Wang, 冰洁 王, Joel Leja, Rachel Bezanson, Benjamin D. Johnson, Gourav Khullar, Ivo Labbé, Sedona H. Price, John R. Weaver, Katherine E. Whitaker
Figure caption: Here we demonstrate the performance of Prospector-β in recovering physical parameters, and contrast it with the fiducial Prospector-α model that assumes uniform priors. Residuals in mass, mass-weighted age, and SFR(0–100Myr) are shown as histograms. Results based on uniform priors are shown in gray, while those based on Prospector-β are shown in red. NMAD, outlier fraction, and MBE are reported in the same colors as the corresponding histogram. To avoid counting the error in redshift twice, we only include residuals for the subset where (z med − z true)/(1 + z true) ≤ 0.1. We find that Prospector-β results in less bias consistently in mass, age, and SFR as compared to uniform prior cases.
Paper: Inferring More from Less: Prospector as a Photometric Redshift Engine in the Era of JWST
Authors: Bingjie Wang, 冰洁 王, Joel Leja, Rachel Bezanson, Benjamin D. Johnson, Gourav Khullar, Ivo Labbé, Sedona H. Price, John R. Weaver, Katherine E. Whitaker
Figure caption: (a) Posteriors of a sample fit illustrating the degeneracy. The red contours show results assuming the Prospector-β priors, while the gray contours show those assuming uniform priors. Truths are overplotted on the corner plot in yellow. (b) The 2D histogram shows the average redshift offset when assuming uniform priors. Overplotted are contours showing the density of points. The fact that the contour lines are right along the line of the age–mass–redshift degeneracy suggests that uniform priors get the correct redshifts by exploiting this degeneracy.
Paper: Inferring More from Less: Prospector as a Photometric Redshift Engine in the Era of JWST
Authors: Bingjie Wang, 冰洁 王, Joel Leja, Rachel Bezanson, Benjamin D. Johnson, Gourav Khullar, Ivo Labbé, Sedona H. Price, John R. Weaver, Katherine E. Whitaker
Figure caption: Magnitudes in F444W are plotted as a function of redshifts for the the mock galaxies that we test our model on.