adsabs/AstroCLIMB huggingface dataset:
Paper: Bursty or Heavy? The Surprise of Bright Population III Systems in the Reionization Era
Authors: Alessandra Venditti, Julian B. Muñoz, Volker Bromm, Seiji Fujimoto, Steven L. Finkelstein, John Chisholm
Figure caption: UVLFs resulting from the “BURSTY” and “HEAVY” models from Figure 1 (red/blue, dashed lines), if extrapolated to z = 8 and z = 12.5 (with progressively thinner linestyle). For comparison, we show the observed binned UVLF and fitting functions from R. J. Bouwens et al. (2021, at z = 8) and C. T. Donnan et al. (2024, at z = 12.5), extrapolated toward fainter magnitudes. The bright end of the Pop III UVLF shows a modest increase up to z ≈ 12.5, while a strong decay of the total (Population II-dominated) UVLF is evident from observations. Lensing JWST surveys such as VENUS (S. Fujimoto et al. 2025b) will allow deeper MUV coverage (within the pink, shaded area, computed for z = 10 with Δz = 1).
Paper: Bursty or Heavy? The Surprise of Bright Population III Systems in the Reionization Era
Authors: Alessandra Venditti, Julian B. Muñoz, Volker Bromm, Seiji Fujimoto, Steven L. Finkelstein, John Chisholm
Figure caption: Joint posterior for the stochasticity parameter ﹩{\sigma }_{{\rm{UV}}}^{{\rm{III}}}﹩ and the high-mass cutoff ﹩{M}_{{\rm{up}}}^{{\rm{III}}}﹩, resulting from fitting our Pop III UVLF model against the observed data points from S. Fujimoto et al. (2025a) and T. Morishita et al. (2025) at z ≈ 5.6–6.6, when all model parameters (﹩{\sigma }_{{\rm{UV}}}^{{\rm{III}}}﹩, ﹩{\varepsilon }_{\star ,{\rm{UV}}}^{{\rm{III}}}﹩, ﹩{\beta }_{\star }^{{\rm{III}}}﹩, and ﹩{M}_{{\rm{up}}}^{{\rm{III}}}﹩) are allowed to vary (left) and when we fix ﹩{\beta }_{\star }^{{\rm{III}}}=0﹩ (right); 1σ and 2σ contour lines are shown as black, solid lines in the 2D posterior. Reference values for our “BURSTY” and “HEAVY” models, for the model of H. A. G. Cruz et al. (2025), and for the dustyGadget simulation suite are included as in Figure 2. Low values of both ﹩{\sigma }_{{\rm{UV}}}^{{\rm{III}}}﹩ and ﹩{M}_{{\rm{up}}}^{{\rm{III}}}﹩ simultaneously are strongly disfavored, even more so when ﹩{\beta }_{\star }^{{\rm{III}}}﹩ is free to vary.
Paper: Bursty or Heavy? The Surprise of Bright Population III Systems in the Reionization Era
Authors: Alessandra Venditti, Julian B. Muñoz, Volker Bromm, Seiji Fujimoto, Steven L. Finkelstein, John Chisholm
Figure caption: Same as Figures 1 and 2, but only including the AMORE6 Pop III candidate from T. Morishita et al. (2025) and the z = 6 total UVLF constraints from R. J. Bouwens et al. (2022) in the fit (as detailed in the text); shaded lines refer to the results of corresponding fits without the inclusion of the total UVLF constraints. While the latter allow ﹩{M}_{\mathrm{up}}^{\mathrm{III}}\sim 1{0}^{8}\,{M}_{\odot }﹩ with ﹩{\varepsilon }_{\star ,{\rm{UV}}}^{{\rm{III}}}\sim 1{0}^{-2.4}﹩ (for the “BURSTY” model) and a very large ﹩{\varepsilon }_{\star ,{\rm{UV}}}^{{\rm{III}}}\sim 1{0}^{-1.2}﹩ (for the “HEAVY” model), values of ﹩{M}_{\mathrm{up}}^{\mathrm{III}}\sim 1{0}^{8}/1{0}^{9.5}\,{M}_{\odot }﹩ and ﹩{\varepsilon }_{\star ,{\rm{UV}}}^{{\rm{III}}}\sim 1{0}^{-2.5}/1{0}^{-2.1}﹩, closer to the case including GLIMPSE-16043 (Figures 1 and 2) are found for the “BURSTY”/“HEAVY” models when the total UVLF constraints are included.
Paper: Characterizing Nanoflare Energy and Frequency through Field Line Analysis
Authors: Shanwlee Sow Mondal, Lars K. S. Daldorff, James A. Klimchuk, Craig. D. Johnston
Figure caption: The teal curves show various plasma parameters evaluated along a single magnetic field line. The top panel displays the time evolution of the coronal line-integrated shock heating, Qshock, for the field line shown in Figure 20, corresponding to the integration range marked by the white dashed lines in that figure. The middle panel shows the temporal variation of the maximum perpendicular velocity component, v⊥, within the coronal segment of the same field line. Similarly, the bottom panel presents the evolution of the maximum value of the perpendicular component of the curl of current density, (∇ × J)⊥, along the coronal portion of the same field line. In each panel, the red curve indicates the corresponding normalized reconnection jump, labeled to the of the right y-axis.
Paper: Characterizing Nanoflare Energy and Frequency through Field Line Analysis
Authors: Shanwlee Sow Mondal, Lars K. S. Daldorff, James A. Klimchuk, Craig. D. Johnston
Figure caption: An example showing the role of different energy nanoflares in determining the overall temperature evolution.
Paper: Characterizing Nanoflare Energy and Frequency through Field Line Analysis
Authors: Shanwlee Sow Mondal, Lars K. S. Daldorff, James A. Klimchuk, Craig. D. Johnston
Figure caption: Power-law (top) and log-normal (bottom) fits of the nanoflare energy distributions obtained from Methods A, B, and C with δcut = 2 grid cells and twindow = 10 s.
Paper: Characterizing Nanoflare Energy and Frequency through Field Line Analysis
Authors: Shanwlee Sow Mondal, Lars K. S. Daldorff, James A. Klimchuk, Craig. D. Johnston
Figure caption: Temporal evolution of the viscous shock heating rate (Qshock) along a randomly chosen magnetic field line is shown in the top panel. The bottom panel provides a zoomed-in view of the localized heating near the field-line apex. The white dashed vertical lines indicate the approximate coronal extent of the selected field line.
Paper: Characterizing Nanoflare Energy and Frequency through Field Line Analysis
Authors: Shanwlee Sow Mondal, Lars K. S. Daldorff, James A. Klimchuk, Craig. D. Johnston
Figure caption: Snapshot of the coronal z-mid-plane highlighting multiple reconnection sites, characterized by bidirectional flows (vx) and enhanced current density (Jz). The bottom panel presents a zoomed-in view of the reconnection region, outlined by the black rectangular box in the top panel. The color maps are saturated to values shown in the corresponding color bars. Actual peak values are larger.
Paper: Characterizing Nanoflare Energy and Frequency through Field Line Analysis
Authors: Shanwlee Sow Mondal, Lars K. S. Daldorff, James A. Klimchuk, Craig. D. Johnston
Figure caption: Energy partition of nanoflares. The blue, red, and yellow columns each contain nanoflares that constitute one-third of the total energy and are classified as low-, medium-, and high-energy events. The distributions are the same as in Figures 13 and 14.
Paper: Characterizing Nanoflare Energy and Frequency through Field Line Analysis
Authors: Shanwlee Sow Mondal, Lars K. S. Daldorff, James A. Klimchuk, Craig. D. Johnston
Figure caption: Comparison between Methods A, B, and C with δcut = 2 grid cells and twindow = 10 s. (Top panel) 2D histograms of nanoflare energies and durations. (Bottom panel) Nanoflare energy distributions.
Paper: Characterizing Nanoflare Energy and Frequency through Field Line Analysis
Authors: Shanwlee Sow Mondal, Lars K. S. Daldorff, James A. Klimchuk, Craig. D. Johnston
Figure caption: Table summarizing the global delays and average cooling times in seconds for different energy nanoflares.
Paper: Characterizing Nanoflare Energy and Frequency through Field Line Analysis
Authors: Shanwlee Sow Mondal, Lars K. S. Daldorff, James A. Klimchuk, Craig. D. Johnston
Figure caption: Histograms of the cooling time for low-, medium-, and high-energy nanoflares represented in blue, red, and yellow, respectively.
Paper: Multibaseline NenuFAR Interferometry in Transit Mode: Continuous Low-frequency Spectrum of the Crab Nebula
Authors: Aleksander A. Stanislavsky, Ihor N. Bubnov, Lev A. Stanislavsky, Alexander A. Konovalenko, Philippe Zarka, Alan Loh, Cédric Viou, Rostyslav V. Vashchishyn
Figure caption: The flux density spectrum of the Crab arises from radio emission produced by both the extended shell and the central compact region. The blue curve represents a fit to the current dataset (total flux) and selected archival measurements, while the red curve corresponds to a fit to archival measurements of the compact region (A. L. Bobeiko et al. 1979; V. P. Bovkun et al. 1987). Due to the sparsity and inconsistent error reporting in the original compact component data, we present the averaged spectrum as a smoothed curve. The black curve shows the difference between the two fits and traces the shell component.
Paper: Multibaseline NenuFAR Interferometry in Transit Mode: Continuous Low-frequency Spectrum of the Crab Nebula
Authors: Aleksander A. Stanislavsky, Ihor N. Bubnov, Lev A. Stanislavsky, Alexander A. Konovalenko, Philippe Zarka, Alan Loh, Cédric Viou, Rostyslav V. Vashchishyn
Figure caption: Comparison of flux density measurements from observations with NenuFAR, LOFAR, and URAN–2. The plotted data points labeled URAN–2 (2023) represent our observations at 10.7–25.0 MHz. The NenuFAR (2025) measurements, also obtained by our team, cover the 22–75 MHz range and are shown as red filled circles. The LOFAR (2016) data points correspond to the radio model presented by F. de Gasperin et al. (2020), derived from imaging of the Crab using the LBA system.
Paper: Multibaseline NenuFAR Interferometry in Transit Mode: Continuous Low-frequency Spectrum of the Crab Nebula
Authors: Aleksander A. Stanislavsky, Ihor N. Bubnov, Lev A. Stanislavsky, Alexander A. Konovalenko, Philippe Zarka, Alan Loh, Cédric Viou, Rostyslav V. Vashchishyn
Figure caption: The Crab flux density spectrum from 16.7 to 74.5 MHz with the NenuFAR measurements and using the observational data at 16.7, 20, 25, 26.3, and 38 MHz (blue crosses) obtained by A. L. Bobeiko et al. (1979) and V. P. Bovkun et al. (1987) with the radio telescopes UTR–2 and URAN–1. This radio spectrum corresponds to the entire Crab.
Paper: Multibaseline NenuFAR Interferometry in Transit Mode: Continuous Low-frequency Spectrum of the Crab Nebula
Authors: Aleksander A. Stanislavsky, Ihor N. Bubnov, Lev A. Stanislavsky, Alexander A. Konovalenko, Philippe Zarka, Alan Loh, Cédric Viou, Rostyslav V. Vashchishyn
Figure caption: Distribution of NenuFAR “core” MAs used in the low-frequency observations. Each red dot on the map represents an MA (designated as MA and numbered), consisting of 19 elementary dual-polarization antennas arranged in a hexagonal pattern. The MA configuration is illustrated in the upper-left corner. Each MA has a distinct identifier. Since the figure includes only those MAs involved in the measurements, the antenna numbering appears nonsequential.
Paper: Multibaseline NenuFAR Interferometry in Transit Mode: Continuous Low-frequency Spectrum of the Crab Nebula
Authors: Aleksander A. Stanislavsky, Ihor N. Bubnov, Lev A. Stanislavsky, Alexander A. Konovalenko, Philippe Zarka, Alan Loh, Cédric Viou, Rostyslav V. Vashchishyn
Figure caption: Image of the Crab at a frequency of 38 MHz (resolution ﹩16\mathop{.}\limits^{^{\prime\prime} }0\times 11\mathop{.}\limits^{^{\prime\prime} }0﹩) from LOFAR LBA (F. de Gasperin et al. 2020).
Paper: Cross-correlating the Patchy Screening and Kinetic Sunyaev–Zel’dovich Effects as a New Probe of Reionization
Authors: Darby Kramer, Alexander van Engelen, Christopher Cain, Niall MacCrann, Hy Trac, Skylar Grayson, Evan Scannapieco, Blake Sherwin
Figure caption: The contribution from each angular scale L to the forecasted signal-to-noise ratios of ﹩{C}_{L}^{\tau \tau }﹩, ﹩{C}_{L}^{KK}﹩, and ﹩{C}_{L}^{K\tau }﹩ for the case of CMB-S4 (neglecting foreground power). The SNRs of all three are dominated by large scales, though ﹩{C}_{L}^{KK}﹩ is highly dominated by the very largest scales, L < 300, due to its sensitivity to velocity fluctuations. In ﹩{C}_{L}^{K\tau }﹩, we do not see this same strong dominance at L < 100 because the constituent fields only have the τ fluctuations in common. This is also reflected in the power spectra in Figure 3.
Paper: Cross-correlating the Patchy Screening and Kinetic Sunyaev–Zel’dovich Effects as a New Probe of Reionization
Authors: Darby Kramer, Alexander van Engelen, Christopher Cain, Niall MacCrann, Hy Trac, Skylar Grayson, Evan Scannapieco, Blake Sherwin
Figure caption: Demonstration of the ansatz in Equation (19), showing that our estimate of the theoretical ﹩{C}_{L}^{K\tau }﹩ (orange) is dominated by the electron density bispectrum (blue), especially on small scales of L > 3000. Even on large scales, the δe bispectrum scaled appropriately by ﹩{v}_{{\rm{rms}}}^{2}﹩ contributes to over half of ﹩{C}_{L}^{K\tau }﹩. This confirms that this cross correlation almost solely probes the non-Gaussianity of electrons during the EoR.
Paper: High-velocity Outflows in [O III] Emitters at 2.5 < z < 9 from JWST NIRSpec Medium-resolution Spectroscopy
Authors: Ryan A. Cooper, Karina I. Caputi, Edoardo Iani, Pierluigi Rinaldi, Guillaume Desprez, Rafael Navarro-Carrera
Figure caption: The normalized distribution of [O III] emitters (gray) and our final outflow candidates (red). The dashed blue line at S/N > 5 is the lower limit at which we first identify outflows within our sample.
Paper: High-velocity Outflows in [O III] Emitters at 2.5 < z < 9 from JWST NIRSpec Medium-resolution Spectroscopy
Authors: Ryan A. Cooper, Karina I. Caputi, Edoardo Iani, Pierluigi Rinaldi, Guillaume Desprez, Rafael Navarro-Carrera
Figure caption: Redshifts from the JADES public data release (D. J. Eisenstein et al. 2023; M. J. Rieke et al. 2023) compared to the fitted redshifts obtained from MSAEXP. Gray dotted lines in the lower panel represent Δz/(1+z) = ±0.025.
Paper: High-velocity Outflows in [O III] Emitters at 2.5 < z < 9 from JWST NIRSpec Medium-resolution Spectroscopy
Authors: Ryan A. Cooper, Karina I. Caputi, Edoardo Iani, Pierluigi Rinaldi, Guillaume Desprez, Rafael Navarro-Carrera
Figure caption: Mass loading factor against stellar mass (upper) and specific SFR (lower) for our outflow candidates. The horizontal line at η = 1 represents the point at which the rate of ionizing gas expelled from the galaxy is equal to the SFR. A horizontal line at η = 5 is also added for reference. Results from Ca24 and Xu25 are shown as orange stars and blue squares, respectively. The starburst regime defined by (K. I. Caputi et al. 2017, 2021) is shaded in blue. Theoretical predictions from the TNG50 (D. Nelson et al. 2019), FIRE (A. L. Muratov et al. 2015), and FIRE-2 (V. Pandya et al. 2021) simulations are shown as shaded regions and purple lines, respectively.
Paper: High-velocity Outflows in [O III] Emitters at 2.5 < z < 9 from JWST NIRSpec Medium-resolution Spectroscopy
Authors: Ryan A. Cooper, Karina I. Caputi, Edoardo Iani, Pierluigi Rinaldi, Guillaume Desprez, Rafael Navarro-Carrera
Figure caption: Gaussian fits of all outflow candidates in our sample including those produced by rotating clumps. Left: 1″ RGB postage stamp of the outflow candidate. These stamps are created following the same method as described in Figure 7. Center: The [O III]5007 line fitted with a single narrow Gaussian (blue). Right: The same emission line fitted with an additional broad component (red). Residuals for both fits are seen in the lower panels in blue and red, respectively.
Paper: High-velocity Outflows in [O III] Emitters at 2.5 < z < 9 from JWST NIRSpec Medium-resolution Spectroscopy
Authors: Ryan A. Cooper, Karina I. Caputi, Edoardo Iani, Pierluigi Rinaldi, Guillaume Desprez, Rafael Navarro-Carrera
Figure caption: Continuation of Figure 17.
Paper: High-velocity Outflows in [O III] Emitters at 2.5 < z < 9 from JWST NIRSpec Medium-resolution Spectroscopy
Authors: Ryan A. Cooper, Karina I. Caputi, Edoardo Iani, Pierluigi Rinaldi, Guillaume Desprez, Rafael Navarro-Carrera
Figure caption: Median stacked spectrum of all objects in our sample with S/N < 10. Both [O III]5007 and [O III]4959 are m2odeled and show evidence of a blueshifted component.
Paper: High-velocity Outflows in [O III] Emitters at 2.5 < z < 9 from JWST NIRSpec Medium-resolution Spectroscopy
Authors: Ryan A. Cooper, Karina I. Caputi, Edoardo Iani, Pierluigi Rinaldi, Guillaume Desprez, Rafael Navarro-Carrera
Figure caption: The ratio of outflow velocity and escape velocity against galaxy physical parameters. The escape velocity is calculated through an empirical relationship between UV magnitude and dark matter halo mass.
Paper: High-velocity Outflows in [O III] Emitters at 2.5 < z < 9 from JWST NIRSpec Medium-resolution Spectroscopy
Authors: Ryan A. Cooper, Karina I. Caputi, Edoardo Iani, Pierluigi Rinaldi, Guillaume Desprez, Rafael Navarro-Carrera
Figure caption: Example spectra of two outflow candidates extended to cover the full [O III]+Hβ complex. The footprint of the MSA slit for each object is included on the RGB cutout.
Paper: High-velocity Outflows in [O III] Emitters at 2.5 < z < 9 from JWST NIRSpec Medium-resolution Spectroscopy
Authors: Ryan A. Cooper, Karina I. Caputi, Edoardo Iani, Pierluigi Rinaldi, Guillaume Desprez, Rafael Navarro-Carrera
Figure caption: [O III]5007 line fluxes from the JADES public data release (D. J. Eisenstein et al. 2023; M. J. Rieke et al. 2023) compared to our line fluxes extracted with MSAEXP.
Paper: The Balmer Break and Optical Continuum of Little Red Dots from Super-Eddington Accretion
Authors: Hanpu Liu, 翰溥 刘, Yan-Fei Jiang, 燕飞 姜, Eliot Quataert, Jenny E. Greene, Yilun Ma, 逸伦 马
Figure caption: Continuum spectra from spherical models compared to four LRD spectra showing strong Balmer breaks. The names of the observed objects are annotated. The model and observed spectra of UNCOVER-45924 and RUBIES-UDS-154183 are shifted up by 10 for visual clarity. The parameters for the four model curves are (L, ρref) = (7.4 × 1044, 2.0 × 10−12), (1.8 × 1044, 2.1 × 10−12), (4.4 × 1044, 5.5 × 10−12), and (7.4 × 1043, 1.6 × 10−12) (in CGS units) respectively, from top to bottom.
Paper: The Balmer Break and Optical Continuum of Little Red Dots from Super-Eddington Accretion
Authors: Hanpu Liu, 翰溥 刘, Yan-Fei Jiang, 燕飞 姜, Eliot Quataert, Jenny E. Greene, Yilun Ma, 逸伦 马
Figure caption: Balmer break strength and optical color of the sphere models (color-coded proportional to ρrefL−1/2; points with high transparency represent spectra extincted by a Small Magellanic Cloud–averaged dust law with AV = 1) compared to observations (blue points with error bars). As qualitatively indicated by the light shade in the background, the spherical model can explain the region below the model data points (due to filling by the UV component), consistent with the distribution of known LRDs.
Paper: A Semianalytic Framework of Population III and Subsequent Galaxy Formation on Cosmological N-body Simulations
Authors: Tomoaki Ishiyama, Shingo Hirano
Figure caption: Difference between the self-consistent (first and third rows) and the uniform models (second and fourth rows) on the fiducial Phi-4096 simulation (L = 16h−1 Mpc) with zero streaming velocity. Supermassive Pop III stars (more massive than 104.5 M⊙) are shown as crosses. From left to right, each row shows the spatial distribution of the total mass density of Pop III, Pop II stars, and Lyman–Werner flux. See also Figure 6.
Paper: The Balmer Break and Optical Continuum of Little Red Dots from Super-Eddington Accretion
Authors: Hanpu Liu, 翰溥 刘, Yan-Fei Jiang, 燕飞 姜, Eliot Quataert, Jenny E. Greene, Yilun Ma, 逸伦 马
Figure caption: Temperature (left) from gray simulations of the sphere model with L = LEdd(106 M⊙). The effective opacity and optical depth at 5000 Å (middle and right) are calculated using the temperature profiles. Dark colors indicate high ρref and hence a high accretion rate. The three crosses on each curve mark the locations where Teff (5000 Å) = 1/4, 1/2, and 1 to indicate the photosphere location and its scale height.
Paper: The Balmer Break and Optical Continuum of Little Red Dots from Super-Eddington Accretion
Authors: Hanpu Liu, 翰溥 刘, Yan-Fei Jiang, 燕飞 姜, Eliot Quataert, Jenny E. Greene, Yilun Ma, 逸伦 马
Figure caption: Continuum spectra from sphere models at a total luminosity L = LEdd(106 M⊙) = 1.47 × 1044 erg s−1. Model spectra are color-coded by the reference density, ρref, a proxy for the Eddington ratio (Equation (11)) and the photosphere density (ρref ∼ ρph if Teff ∼ 5000 K). A collection of observed LRD spectra are shown in the background for comparison.
Paper: The Balmer Break and Optical Continuum of Little Red Dots from Super-Eddington Accretion
Authors: Hanpu Liu, 翰溥 刘, Yan-Fei Jiang, 燕飞 姜, Eliot Quataert, Jenny E. Greene, Yilun Ma, 逸伦 马
Figure caption: Comparison of model disk vertical profiles for the case MBH = 107 M⊙, λEdd = 1. The vertical axis is scaled linearly below 10−12 g cm−3 and logarithmically above. Solid curves denote the full solution described in Appendix A.1. Dashed curves denote the approximation described in the Appendix and applied in the main text. The full model shows density inversion at radii r ≥ 103.2 Rg, which is avoided in the approximate model.
Paper: The Balmer Break and Optical Continuum of Little Red Dots from Super-Eddington Accretion
Authors: Hanpu Liu, 翰溥 刘, Yan-Fei Jiang, 燕飞 姜, Eliot Quataert, Jenny E. Greene, Yilun Ma, 逸伦 马
Figure caption: Disk vertical temperature profile from the gray simulations. The disk has MBH = 107 M⊙ and λEdd = 102. Each curve represents an individual simulation of an annulus.
Paper: The Balmer Break and Optical Continuum of Little Red Dots from Super-Eddington Accretion
Authors: Hanpu Liu, 翰溥 刘, Yan-Fei Jiang, 燕飞 姜, Eliot Quataert, Jenny E. Greene, Yilun Ma, 逸伦 马
Figure caption: Same as Figure 7 but for the models with L = LEdd(107 M⊙).
Paper: Early Coformation of the Milky Way’s Thin and Thick Disks at Redshift z > 2
Authors: Lais Borbolato, Silvia Rossi, Hélio D. Perottoni, Guilherme Limberg, João A. S. Amarante, Anna B. A. Queiroz, Cristina Chiappini, Friedrich Anders, Rafael M. Santucci, Fabrícia O. Barbosa, João V. Nogueira-Santos
Figure caption: Distribution of APOGEE and LAMOST data in the top and bottom rows, respectively. The panels from the first to the fourth column show the [Mg/Fe]–[Fe/H] space separated into different age intervals. The first column shows the density contours of data with ages older than 11 Gyr. These contours were used to divide the chemical thick disk (red region, high-α) and chemical thin disk (green region, low-α) populations, the exact division being represented by the pink dashed line. For the APOGEE panel, the separation line represents [Mg/Fe] = 0.18 for the interval −1.0  <  [Fe/H] < −0.6, [Mg/Fe] = −0.15 × [Fe/H] +0.09 between −0.6  <  [Fe/H]  <  0.1 and [Mg/Fe] = 0.08 for [Fe/H] > 0.1. For the LAMOST panels, the curve is represented by [Mg/Fe] = 0.18 for the interval −1.0 < [Fe/H]  < −0.6, [Mg/Fe] = −0.20 × [Fe/H] +0.06 between −0.6 < [Fe/H] < 0.1 and [Mg/Fe] = 0.04 for [Fe/H] > 0.1. From the second to the fourth column, the data presented correspond to our final selection of thin (green dots) and thick disk (red dots) stars separated into three age ranges: older than 11 Gyr, before the GSE accretion, between 9 Gyr and 11 Gyr, merger period with the GSE, and between 4 Gyr and 9 Gyr, postmerger. The number of stars in each sample is also shown in the panels. Finally, the rightmost panel shows the projection of the thin and thick disk samples into the Toomre diagram (﹩\sqrt{{V}_{R}^{2}+{V}_{Z}^{2}}\,\rm{vs.}\,{V}_{\phi }﹩ cylindrical frame), where the innermost curve represents ∥v − vcirc∥ = 100 km s−1 and the outermost curve is ∥v − vcirc∥ = 220 km s−1.
Paper: Early Coformation of the Milky Way’s Thin and Thick Disks at Redshift z > 2
Authors: Lais Borbolato, Silvia Rossi, Hélio D. Perottoni, Guilherme Limberg, João A. S. Amarante, Anna B. A. Queiroz, Cristina Chiappini, Friedrich Anders, Rafael M. Santucci, Fabrícia O. Barbosa, João V. Nogueira-Santos
Figure caption: Spatial distribution of the YGC–XGC (top panels) and ZGC–XGC (bottom panels) planes of the final APOGEE DR17 and LAMOST MRS DR7 samples in the first and second columns, respectively. The yellow star indicates the position of the Sun ([X, Y, Z]GC =  [−8.2, 0.0, 0.0] kpc). In the top panels, the dashed lines indicate the Galactocentric circumference for the radius of the Sun, and in the bottom panels, the dashed line indicates the Galactic plane (ZGC = 0 kpc). The top panel of the rightmost column shows the age distribution of the entire sample, considering the quality cuts. The bottom row of the same column shows the uncertainty in age (σAGE) of samples, and the vertical black dashed line represents σAGE = 1 Gyr.