adsabs/AstroCLIMB huggingface dataset:
Paper: Formation and Morphology of the First Galaxies in the Cosmic Morning
Authors: Changbom Park, Jaehyun Lee, Juhan Kim, Donghui Jeong, Christophe Pichon, Brad K. Gibson, Owain N. Snaith, Jihye Shin, Yonghwi Kim, Yohan Dubois, C. Gareth Few
Figure caption: Relation between the isophotal axis ratio and Sérsic index of late-type (green circles), early-type (red or magenta circles), abnormal late-type (triangles), and abnormal early-type (crosses) SDSS galaxies in the training set of Park & Choi (2005).
Paper: Formation and Morphology of the First Galaxies in the Cosmic Morning
Authors: Changbom Park, Jaehyun Lee, Juhan Kim, Donghui Jeong, Christophe Pichon, Brad K. Gibson, Owain N. Snaith, Jihye Shin, Yonghwi Kim, Yohan Dubois, C. Gareth Few
Figure caption: Morphological type fractions of galaxies as a function of galaxy stellar mass at z ≈ 2. The blue, black, and red solid lines are for disks, irregulars, and spheroids, respectively.
Paper: Deconfusing Detections in Directly Imaged Multiplanet Systems 
Authors: Leonid Pogorelyuk, Riley Fitzgerald, Sophia Vlahakis, Rhonda Morgan, Kerri Cahoy
Figure caption: Orbit-fitting procedure that guarantees that at an orbit that best fits the image plane data is found within a specified error tolerance. Right: the search is over a 3D parameter space consisting of the semimajor axis, a, and the components of the eccentricity vector, e  x , e  y , in the plane of the orbit (the plane is oriented such that the star is at the origin and y = 0 at t = 0). Center: the rest of the six orbital parameters are implicitly fitted by least-squares fitting a 2D linear transformation, ﹩\tilde{S}﹩, from points in the orbit plane and the image plane (left). The first singular value of the ﹩\tilde{S}﹩ transformation, ﹩\tilde{a}﹩, is should be close to the semimajor axis being tested, a. The transformation used to compute the final fitting error is ﹩S=\tfrac{a}{\tilde{a}}\tilde{S}﹩. To handle some edge cases, we also try fitting a 2D rotation matrix (see Section 2.1.2).
Paper: Deconfusing Detections in Directly Imaged Multiplanet Systems 
Authors: Leonid Pogorelyuk, Riley Fitzgerald, Sophia Vlahakis, Rhonda Morgan, Kerri Cahoy
Figure caption: (a) Rates of spurious orbits (dashed lines): how many orbits fit detections that correspond to different planets within a specified tolerance (a rate above 1 means that there was, on average, more than one spurious orbit per simulated system). The simulated observations were of three planets between 0.5 and 3 au with eccentricities below 0.2. In some cases (solid lines), there are multiple mutually consistent sets of orbits (see the example in Figure 1), i.e., there is confusion. There is more confusion when only three observations over one year (circles) are given as opposed to four (squares). Confusion does not disappear at lower tolerances since many cases of three points in the image plane can be perfectly fit by an orbit. (b) The number of grid points in the exhaustive search (Section 2.1) that guarantees that the best-fitting orbit is found within a given tolerance, ε. It scales as ε −3.
Paper: Inferring the Neutron Star Maximum Mass and Lower Mass Gap in Neutron Star–Black Hole Systems with Spin
Authors: Christine Ye, Maya Fishbach
Figure caption: 90% contours on m 1 and m 2 from the four NSBH events: GW190426 (gray), GW190814 (blue), GW200105 (green), and GW200115 (red). Plot features m 1 and m 2 under three spin priors “U + I” in dotted lines; “ZS” in dashed lines; “ZS + AS” solid (all 90% contours). The spin priors correspond to the models from Section 2.1.1 with β  s  = 0. Three additional GWTC-2 and GWTC-3 events, GW190917_114630, GW191219_163120, and GW200210_092254, are shown in black, using default LVK spin priors.
Paper: Deconfusing Detections in Directly Imaged Multiplanet Systems 
Authors: Leonid Pogorelyuk, Riley Fitzgerald, Sophia Vlahakis, Rhonda Morgan, Kerri Cahoy
Figure caption: (a) Missed detections (hollow squares and circles) within the 0.5 au IWA result in a large number of spurious orbits (dashed lines) that fit the non-missed detections (full squares and circles). Note that speckles in the IWA might have the same contribution to confusion as the inner planet (red circles) in this case. (b) Estimated probabilities that two planets between 0.5 and 1.5 au and with a 60° inclination will have at least one missed detection out of four. When there are missed detections for both planets, confusion is likely as well. The rates do not show significant dependence on the observation cadence (although planetary phases were not taken into account in our simulations).
Paper: Inferring the Neutron Star Maximum Mass and Lower Mass Gap in Neutron Star–Black Hole Systems with Spin
Authors: Christine Ye, Maya Fishbach
Figure caption: Simulated astrophysical NS mass distributions p(m 2), with M TOV = 2 M ⊙, marked in red. The NS spin distribution follows Equation (1), with β  s  and a max specified in the subcaptions.
Paper: Deconfusing Detections in Directly Imaged Multiplanet Systems 
Authors: Leonid Pogorelyuk, Riley Fitzgerald, Sophia Vlahakis, Rhonda Morgan, Kerri Cahoy
Figure caption: (a) Confusion rates for simulated planets sampled between 0.5 and 6 au with an inclination of 45°, and observed three times within one year with an 0.05 au astrometry error. Confusion increases with the number of planets and the maximum allowed eccentricity, e max. (b) Dependency of the confusion rate on the number of epochs and system inclination (confusion occurs when at least two planets have two or more different orbits that matched all their corresponding data points to within 0.05 au). A total of seven planets is simulated per system with ﹩{e}_{\max }=0.2﹩. Four epochs are sufficient to deconfuse planets except in highly inclined systems.
Paper: Inferring the Neutron Star Maximum Mass and Lower Mass Gap in Neutron Star–Black Hole Systems with Spin
Authors: Christine Ye, Maya Fishbach
Figure caption: Posteriors on NS spin a 2/a Kep from the NSBH events: GW190426, GW190814, GW200105, and GW200115, inferred under different spin priors. “U + I” a 2 samples in dotted black; “ZS” in dashed red; “ZS + AS” in solid blue.
Paper: Inferring the Neutron Star Maximum Mass and Lower Mass Gap in Neutron Star–Black Hole Systems with Spin
Authors: Christine Ye, Maya Fishbach
Figure caption: Sample parameter estimation posterior simulated using the PN approximation; contours show 68% and 95% CI. True values are denoted by the blue crosses.
Paper: Formation and Morphology of the First Galaxies in the Cosmic Morning
Authors: Changbom Park, Jaehyun Lee, Juhan Kim, Donghui Jeong, Christophe Pichon, Brad K. Gibson, Owain N. Snaith, Jihye Shin, Yonghwi Kim, Yohan Dubois, C. Gareth Few
Figure caption: Left: initial dark-matter overdensity peak height ν pk corresponding to the center of mass of the dark matter in the galaxies having a given stellar mass. The solid and dashed lines are for the galaxies with M ⋆ = 2−2.4 × 109 M ⊙ and M ⋆ = 5−6 × 109 M ⊙, respectively. The error bars show the 16th−84th percentile distributions. The open circles mark the median ν pk of spheroids, and the asterisks are for disk-type galaxies. Right: histograms of galaxy number count as a function of ν pk. The cyan, blue, and magenta solid curves correspond to the galaxies with M ⋆ = 2−2.4 × 109 M ⊙ at z = 8, 7, and 6. The magenta dotted and red dashed curves show the distributions of the galaxies with M ⋆ = 5−6 × 109 M ⊙ at z = 6 and 5, respectively.
Paper: Formation and Morphology of the First Galaxies in the Cosmic Morning
Authors: Changbom Park, Jaehyun Lee, Juhan Kim, Donghui Jeong, Christophe Pichon, Brad K. Gibson, Owain N. Snaith, Jihye Shin, Yonghwi Kim, Yohan Dubois, C. Gareth Few
Figure caption: Top: the two-point correlation function for the galaxies with M ⋆ ≥ 2 × 109 M ⊙ at three different redshifts, z = 7 (Magenta), 6 (Green), and 5 (Blue). Bottom: the two-point correlation function at the same three redshifts but with different stellar-mass cuts to sample the same number of the most-massive galaxies, giving the fixed number of galaxies of N gal = 439. For each panel, we also show the linear matter two-point correlation function at the same redshifts as a solid line (z = 5), dotted line (z = 6) and dashed line (z = 7). The stronger evolution of the small-scale nonlinear bias shown for the fixed stellar-mass-limit case (top) has diminished when fixing the total number of galaxies.
Paper: Formation and Morphology of the First Galaxies in the Cosmic Morning
Authors: Changbom Park, Jaehyun Lee, Juhan Kim, Donghui Jeong, Christophe Pichon, Brad K. Gibson, Owain N. Snaith, Jihye Shin, Yonghwi Kim, Yohan Dubois, C. Gareth Few
Figure caption: Sérsic index change ﹩{\rm{\Delta }}{n}_{{\rm{S}}\acute{{\rm{e}}}\mathrm{rsic}}﹩ vs. fractional stellar-mass change ΔM ⋆/M star per unit output time step of Δt ≈ 2.5 × 107  yr. Each dot corresponds to a particular time step between z = 4 and the epoch when each galaxy first reaches M ⋆ = 2 × 109 M ⊙. The blue dots indicate galaxies with M ⋆ = 5−6 × 109 M ⊙, and the red dots are for those with M ⋆ > 6 × 109 M ⊙ at z = 6. The cyan and magenta lines show the mean values of ﹩{\rm{\Delta }}{n}_{{\rm{S}}\acute{{\rm{e}}}\mathrm{rsic}}﹩ for blue and red points, respectively. The error bars exhibit the 1σ distribution of the mean curves.
Paper: Formation and Morphology of the First Galaxies in the Cosmic Morning
Authors: Changbom Park, Jaehyun Lee, Juhan Kim, Donghui Jeong, Christophe Pichon, Brad K. Gibson, Owain N. Snaith, Jihye Shin, Yonghwi Kim, Yohan Dubois, C. Gareth Few
Figure caption: A 1.66 cMpc-thick slice of HR5’s initial dark-matter-density field. Gray-scale map: the highest density within the slice along the direction perpendicular to the slice, after being smoothed over 0.35 cMpc with the Gaussian filter. Color lines: contour levels correspond to the overdensity in units of the rms overdensity, ﹩{\nu }_{\mathrm{DM}}\equiv ({\rho }_{\mathrm{DM}}/{\bar{\rho }}_{\mathrm{DM}}-1)/{\sigma }_{\mathrm{DM}}=1.5﹩ (blue), 2.0 (green), 2.5 (orange), 3.0 (magenta), and 3.5 (red). Symbols: the formation sites of the first galaxies, defined as the initial center of mass of dark-matter particles that form the dark-matter halos of galaxies identified at z = 7 (the circle), 6 (triangles), and 5 (crosses). The large-scale structures in the universe emerge at the highest-density regions and grow in time as galaxy-formation sites move from high- to relatively lower-density peaks.
Paper: Formation and Morphology of the First Galaxies in the Cosmic Morning
Authors: Changbom Park, Jaehyun Lee, Juhan Kim, Donghui Jeong, Christophe Pichon, Brad K. Gibson, Owain N. Snaith, Jihye Shin, Yonghwi Kim, Yohan Dubois, C. Gareth Few
Figure caption: Evolution tracks of galaxies in Sérsic index vs. stellar-mass plane. The top panel shows the evolution of two most-massive galaxies at z = 4. The middle and bottom panels exhibit the tracks of the galaxies with M ⋆ ≈ 5 or 2.5 × 1010 M ⊙ randomly chosen at z = 4. All the galaxies are traced after they reach M ⋆ = 2 × 109 M ⊙. The dotted lines mark the periods when galaxy morphology is irregular. Also shown are the time steps when the mass of the most-massive supermassive black hole among the black holes belonging to a galaxy increases more than 50% (filled circles) or 25% (open circles) per 2.5 × 107 yr.
Paper: Formation and Morphology of the First Galaxies in the Cosmic Morning
Authors: Changbom Park, Jaehyun Lee, Juhan Kim, Donghui Jeong, Christophe Pichon, Brad K. Gibson, Owain N. Snaith, Jihye Shin, Yonghwi Kim, Yohan Dubois, C. Gareth Few
Figure caption: Stellar mass (top), Sérsic index (middle), and rotational velocity to velocity dispersion ratio (bottom) of galaxies at redshifts 8, 7, 6, and 5 as a function of the initial dark-matter overdensity peak height ﹩{\nu }_{\mathrm{pk}}=({\rho }_{\mathrm{DM},\mathrm{pk}}-{\bar{\rho }}_{\mathrm{DM}})/{\sigma }_{\mathrm{DM}}﹩ matched to the initial center of mass of the dark matter in galaxies at each epoch.
Paper: Formation and Morphology of the First Galaxies in the Cosmic Morning
Authors: Changbom Park, Jaehyun Lee, Juhan Kim, Donghui Jeong, Christophe Pichon, Brad K. Gibson, Owain N. Snaith, Jihye Shin, Yonghwi Kim, Yohan Dubois, C. Gareth Few
Figure caption: Fractions of disk (blue), spheroid (red), and irregular (black) morphological types, at redshifts 5 (solid), 6 (dashed), and 7 (dotted) as a function of galaxy stellar mass.
Paper: Formation and Morphology of the First Galaxies in the Cosmic Morning
Authors: Changbom Park, Jaehyun Lee, Juhan Kim, Donghui Jeong, Christophe Pichon, Brad K. Gibson, Owain N. Snaith, Jihye Shin, Yonghwi Kim, Yohan Dubois, C. Gareth Few
Figure caption: Distributions of stars and gas of three galaxies identified at z = 6. The first and second rows show edge-on and face-on views of stellar particle distributions, respectively, the third row shows stellar-mass-density distribution colored according to their ages (bluer is younger), and the bottom panels show gas-density distribution. Gas density increases from red to blue. The scale bar is in units of proper kpc. M ⋆, A, and ﹩{n}_{{\rm{S}}\acute{{\rm{e}}}\mathrm{rsic}}﹩ are stellar mass, asymmetry parameter, and Sérsic index, respectively.
Paper: Formation and Morphology of the First Galaxies in the Cosmic Morning
Authors: Changbom Park, Jaehyun Lee, Juhan Kim, Donghui Jeong, Christophe Pichon, Brad K. Gibson, Owain N. Snaith, Jihye Shin, Yonghwi Kim, Yohan Dubois, C. Gareth Few
Figure caption: Gas density (top) and stellar particle distribution of a small group at z = 6. The group of galaxies is connected to each other via a gaseous filament. The central galaxy has a stellar mass of M ⋆ = 1.76 × 1010 M ⊙, and its gas shows spiral arms. Small objects in the neighbor have a stellar mass smaller than 109 M ⊙.
Paper: Locations and Morphologies of Jellyfish Galaxies in A2744 and A370
Authors: Callum Bellhouse, Bianca Poggianti, Alessia Moretti, Benedetta Vulcani, Ariel Werle, Marco Gullieuszik, Mario Radovich, Yara Jaffé, Jacopo Fritz, Alessandro Ignesti, Cecilia Bacchini, Neven Tomičić, Johan Richard, Geneviève Soucail
Figure caption: Morphological parameters for galaxies within A2744 and A370 combined. Galaxies are colored accordingly as described in the color–magnitude diagrams, Figure 1. RPS galaxies are marked with solid black stars if they have Hα tails longer than 20 kpc according to Moretti et al. (2022) and open black stars otherwise. PSB galaxies are marked with open black squares. A2744_01 (black star in a hollow square) and A2744_07 (hollow star in a hollow square) are thus marked as both RPS and PSB as explained in Section 2.4. Upper left: plot of the concentration and asymmetry parameters, derived as described in the text. The median and the standard deviation of concentration and asymmetry within each category are shown as error bars marked with the relevant color or symbol. Upper right: plot of the Gini and M 20 parameters, derived as described in the text. The median and the standard deviation of Gini and M 20 within each category are shown as error bars marked with the relevant color or symbol. Lower left: plot of the outer and full centroid variance parameters, derived as described in the text. The median and the standard deviation of the centroid variance within each category are shown as error bars marked with the relevant color or symbol.
Paper: Locations and Morphologies of Jellyfish Galaxies in A2744 and A370
Authors: Callum Bellhouse, Bianca Poggianti, Alessia Moretti, Benedetta Vulcani, Ariel Werle, Marco Gullieuszik, Mario Radovich, Yara Jaffé, Jacopo Fritz, Alessandro Ignesti, Cecilia Bacchini, Neven Tomičić, Johan Richard, Geneviève Soucail
Figure caption: DS tests for A2744 (left) and A370 (right), showing a bubble plot in the upper panel and a histogram of the delta distribution in the lower panel. Galaxies are shown as circles, highlighted red if they lie on the red sequence described in Section 2.3, or blue otherwise. Black stars indicate the ram-pressure stripped sample and black squares indicate the PSB sample. A2744_01 is highlighted as a black star in a light gray square, while A2744_07 is highlighted as a black square in a light gray star, for the reasons explained in Section 2.4. All points on the figure are filled if their velocity deviation surpasses the substructure threshold described in the text (black dashed line in lower panel), or unfilled otherwise. The cluster centers used in this analysis are marked with + symbols. The histograms below each plot show the distribution of delta values from the DS test for blue and red galaxies, colored accordingly, with the total combining both colors shown in gray. Black dashed vertical lines indicate the threshold for substructure as described in the text. For A2744, we mark on the bubble plot the regions of interest defined in Owers et al. (2011): the light green circle marks the CTD, the blue circle marks the SMRC, and the gray X marks the location of the X-ray surface-brightness peak.
Paper: Locations and Morphologies of Jellyfish Galaxies in A2744 and A370
Authors: Callum Bellhouse, Bianca Poggianti, Alessia Moretti, Benedetta Vulcani, Ariel Werle, Marco Gullieuszik, Mario Radovich, Yara Jaffé, Jacopo Fritz, Alessandro Ignesti, Cecilia Bacchini, Neven Tomičić, Johan Richard, Geneviève Soucail
Figure caption: Histogram of coincident ICM X-ray fluxes at the locations of all PSB galaxies (gray shaded) all RPS galaxies (black hashed) and all remaining blue cluster galaxies (blue) for A2744 (top) and A370 (bottom). The median values for the ICM X-ray flux for each sample are plotted as dashed vertical lines with the same colors. The location of A2744_01 is highlighted with a black star in a hollow box, while the location of A2744_07 is highlighted as a black box in a hollow star, for the reasons explained in Section 2.4.
Paper: Locations and Morphologies of Jellyfish Galaxies in A2744 and A370
Authors: Callum Bellhouse, Bianca Poggianti, Alessia Moretti, Benedetta Vulcani, Ariel Werle, Marco Gullieuszik, Mario Radovich, Yara Jaffé, Jacopo Fritz, Alessandro Ignesti, Cecilia Bacchini, Neven Tomičić, Johan Richard, Geneviève Soucail
Figure caption: Histogram of coincident ICM X-ray fluxes at the locations of all PSB galaxies (gray shaded) all RPS galaxies (black hashed) and all remaining blue cluster galaxies (blue) for A2744 and A370 combined. The lines and symbols are as described in Figure 6.
Paper: Locations and Morphologies of Jellyfish Galaxies in A2744 and A370
Authors: Callum Bellhouse, Bianca Poggianti, Alessia Moretti, Benedetta Vulcani, Ariel Werle, Marco Gullieuszik, Mario Radovich, Yara Jaffé, Jacopo Fritz, Alessandro Ignesti, Cecilia Bacchini, Neven Tomičić, Johan Richard, Geneviève Soucail
Figure caption: X-ray and lensing maps of A370 with F606W + Hα maps of RPS galaxies and PSBs overlaid. The magenta image and contours show the smoothed X-ray map from Chandra. The CATS v4 lensing mass map is shown in cyan. Whitelight images of RPS and PSB galaxies are shown in white, with MUSE Hα maps shown in yellow. PSB galaxies are marked with red diamonds. The cluster center used in the analysis is marked with a white X. The peak in the X-ray emission is marked with a magenta circle.
Paper: Locations and Morphologies of Jellyfish Galaxies in A2744 and A370
Authors: Callum Bellhouse, Bianca Poggianti, Alessia Moretti, Benedetta Vulcani, Ariel Werle, Marco Gullieuszik, Mario Radovich, Yara Jaffé, Jacopo Fritz, Alessandro Ignesti, Cecilia Bacchini, Neven Tomičić, Johan Richard, Geneviève Soucail
Figure caption: X-ray and lensing maps of A2744 with F606W + Hα maps of RPS galaxies and PSBs overlaid. The magenta image and contours show the smoothed X-ray map from Chandra. The CATS v4 lensing mass map is shown in cyan. F606W images of RPS and PSB galaxies are shown in white, with MUSE Hα maps shown in yellow. PSB galaxies are marked with red diamonds. The cluster center used in the analysis is marked with a white X. The peak in the X-ray emission is marked with a magenta circle.
Paper: Locations and Morphologies of Jellyfish Galaxies in A2744 and A370
Authors: Callum Bellhouse, Bianca Poggianti, Alessia Moretti, Benedetta Vulcani, Ariel Werle, Marco Gullieuszik, Mario Radovich, Yara Jaffé, Jacopo Fritz, Alessandro Ignesti, Cecilia Bacchini, Neven Tomičić, Johan Richard, Geneviève Soucail
Figure caption: Grid of sample galaxies in the dimensionally reduced space yielded by the PCA described in Section 5. At each location on the grid, an example galaxy is shown in order to visualize the different morphologies that occupy different regions of the reduced morphology space. RPS and PSB galaxies are marked with yellow and red borders, respectively. If multiple types occupy a bin, priority is given to showing RPS galaxies, then PSB galaxies, then undisturbed cluster galaxies. The yellow dashed line indicates the PC1 > 4.3 threshold described in the text, above which the majority of RPS galaxies are found.
Paper: Locations and Morphologies of Jellyfish Galaxies in A2744 and A370
Authors: Callum Bellhouse, Bianca Poggianti, Alessia Moretti, Benedetta Vulcani, Ariel Werle, Marco Gullieuszik, Mario Radovich, Yara Jaffé, Jacopo Fritz, Alessandro Ignesti, Cecilia Bacchini, Neven Tomičić, Johan Richard, Geneviève Soucail
Figure caption: Scatter plots of the three components resulting from the PCA described in the text, for all cluster members in A2744 and A370 combined. Data points are colored or indicated by symbols as described in Figure 8. The median and the standard deviation of the two components within each category are shown as error bars marked with the relevant color or symbol. The vertical dashed line indicates the PC1 > 4.3 threshold suggested here to select potential ram-pressure-stripped galaxies.
Paper: Locations and Morphologies of Jellyfish Galaxies in A2744 and A370
Authors: Callum Bellhouse, Bianca Poggianti, Alessia Moretti, Benedetta Vulcani, Ariel Werle, Marco Gullieuszik, Mario Radovich, Yara Jaffé, Jacopo Fritz, Alessandro Ignesti, Cecilia Bacchini, Neven Tomičić, Johan Richard, Geneviève Soucail
Figure caption: Example of centroid variance measurement on the RPS galaxy A370_08. The F606W image of the galaxy is shown overlaid with the flux isocontours and their corresponding centroids as x markers.
Paper: Li Distribution, Kinematics, and Detailed Abundance Analysis among Very Metal-poor Stars in the Galactic Halo from the HESP-GOMPA Survey
Authors: Avrajit Bandyopadhyay, Thirupathi Sivarani, Timothy C. Beers, A. Susmitha, Prasanta K. Nayak, Jeewan C. Pandey
Figure caption: The determination of stellar parameters. The Hα feature is shown in the top panel and the wavelength range shown here for the fitting is 6556–6570 Å, while the Mg triplet region is shown in the bottom panel for the wavelength range 5170–5186 Å. In the top panel, the red line indicates the best fit to the wings, while black-filled dots indicate the observed spectrum. A wavelength range of 10 Å on either side of the core is used for fitting the line wing profile. The black and blue lines indicate deviations from the adopted temperature by 150 K. In the bottom panel, the red line denotes the best fit, while the black and blue lines show the deviation from the adopted logg by 0.50 dex.
Paper: Li Distribution, Kinematics, and Detailed Abundance Analysis among Very Metal-poor Stars in the Galactic Halo from the HESP-GOMPA Survey
Authors: Avrajit Bandyopadhyay, Thirupathi Sivarani, Timothy C. Beers, A. Susmitha, Prasanta K. Nayak, Jeewan C. Pandey
Figure caption: The synthesis of the Li line. The red line shows the best-fit synthetic spectrum, while black-filled circles indicate the observed spectra. The black and blue lines show the synthetic spectra for deviations in the Li abundance of 0.50 dex from the best fit.