adsabs/AstroCLIMB huggingface dataset:
Paper: Statistical Evidence for Small-scale Interchange Reconnection at a Coronal Hole Boundary
Authors: Emily I. Mason, Vadim M. Uritsky
Figure caption: (a) SDO AIA 193 Å image of a northern polar CH; note the much more pronounced and smoother appearance of the boundary on the western side, compared to the less-distinct and patchier boundary on the eastern side. (b) SDO composite 171/193/211 Å context image showing the full Sun on 2015 June 4, with a red box showing the neighborhood of the insets. The top inset shows the CH with the three closed structures bounding it, namely two helmet streamer edges and one pseudostreamer edge. The bottom inset shows the 193 Å data paired with a color-coded HMI magnetogram. (c) PFSS model from the Solarsoft tool pfss_viewer, estimating the extrapolated open and closed fields on the same date; the yellow outline is the approximate boundary of the observed CH and the blue circle highlights the anemone-like topology of the pseudostreamer structure on the hole’s northern border.
Paper: Statistical Evidence for Small-scale Interchange Reconnection at a Coronal Hole Boundary
Authors: Emily I. Mason, Vadim M. Uritsky
Figure caption: (a) Perimeter map of the threshold boundary at 22:30 on 2015 June 4, showing P (the full perimeter in pixels) and L (the length of the region along the pseudostreamer boundary). (b) The same map, at 23:30. (c) Correlation dimension map overlaid on the initial cutout; blue denotes straighter boundaries, while yellow corresponds to more irregular boundaries. The inset shown in (d) is outlined in white. (d) An enlargement of the CDM shown in (c); at a greater level of detail it is easier to see the small-scale variations in the boundary.
Paper: Statistical Evidence for Small-scale Interchange Reconnection at a Coronal Hole Boundary
Authors: Emily I. Mason, Vadim M. Uritsky
Figure caption: (a) Binary threshold image of the cutout taken at value ﹩\mathrm{log}({DN})=2﹩. (b) Extracted boundary of the CH overlaid on the cutout in orange.
Paper: Accelerating Early Massive Galaxy Formation with Primordial Black Holes
Authors: Boyuan Liu, Volker Bromm
Figure caption: The PBH parameters required to explain the cumulative stellar mass density at z ∼ 10 measured by JWST (Labbé et al. 2022) with the “Poisson” effect. The PBH models consistent with JWST observations are shown with the solid and dashed curves for ϵ = 1 and 0.1, respectively. In each case, the upper (lower) line corresponds to the data point at the limiting mass M ⋆ ∼ 1010.5 (10). We also show the constraint from the FIRAS cosmic microwave background μ-distortion limit with a non-Gaussianity parameter p = 0.5 (Nakama et al. 2018; long-dashed), and the combined constraint from X-ray binaries (XB, Inoue & Kusenko 2017), dynamical friction (DF, Carr & Sakellariadou 1999), and large-scale structures (LSS, Carr & Silk 2018), compiled by Carr et al. (2021b; dashed–dotted). Three sample models are labeled with triangles (see Table 1), among which the big (small) triangle(s) can(not) explain the JWST results. The darker triangle (M1) satisfies both observational constraints, while the fainter triangles (M2 and M3) only satisfy the XB+DF+LSS constraint.
Paper: Accelerating Early Massive Galaxy Formation with Primordial Black Holes
Authors: Boyuan Liu, Volker Bromm
Figure caption: The cumulative (comoving) stellar mass density in galaxies more massive than M ⋆ at z = 10 (top), 15 (middle), and 20 (bottom). The results for standard ΛCDM and PBH models M1, M2, and M3 (see Table 1 and Figure 2) are shown with the solid, dashed, dashed–dotted, and dotted curves for ϵ = 1 (thin) and 0.1 (thick). The shaded region can only be populated by galaxies in PBH cosmologies. The results inferred from the recent JWST observations at z ∼ 10 (Labbé et al. 2022) are denoted by the data points with error bars. The long-dashed vertical lines mark the lower mass limits of Pop III and II galaxies to be detected by JWST CEERS NIRCam LW imaging (see the main text). We also plot the number count limit M ⋆/V com with the dashed–dotted–dotted line, given the comoving volume V com for a survey like CEERS of ﹩40\ {\mathrm{arcmin}}^{2}﹩ and Δz = 2.
Paper: Accelerating Early Massive Galaxy Formation with Primordial Black Holes
Authors: Boyuan Liu, Volker Bromm
Figure caption: The power spectra of the dark matter density field at z = 0 in linear perturbation theory for three PBH models with (m PBH/M ⊙, f PBH) = (3 × 10−5, 0.0003); (dashed), (109, 10−5); (dashed–dotted), and (1010, 10−4); (dotted), compared with the standard ΛCDM power spectrum (solid) as measured by the Planck Collaboration et al. (2020) from the PYTHON package  COLOSSUS   (Diemer 2018).
Paper: Accelerating Early Massive Galaxy Formation with Primordial Black Holes
Authors: Boyuan Liu, Volker Bromm
Figure caption: The PBH parameters (shaded region) required to explain the (comoving) number density n g ∼ 2 × 10−5 Mpc−3 of observed massive (M ⋆ ∼ 1011 M ⊙) galaxies at z ∼ 10 (Boylan-Kolchin 2022; Labbé et al. 2022) with the “seed” effect. The shaded region is defined by simple arguments of number counts, baryon mass budget, and the dominance of the “seed” effect: ﹩{\bar{n}}_{\mathrm{PBH}}\gt {n}_{{\rm{g}}}﹩ (solid), ϵ ≡ M ⋆/[f b M B(m PBH, z)] < 1 (and 0.1, see the dashed and dashed–dotted lines), and f PBH < (1 + z)a eq (dotted, which is the general criterion for the assumption that PBHs evolve in isolation to hold; Carr & Silk 2018).
Paper: Toward a Precision Measurement of Binary Black Holes Formation Channels Using Gravitational Waves and Emission Lines
Authors: Suvodip Mukherjee, Azadeh Moradinezhad Dizgah
Figure caption: The merger rate of GW sources for Madau–Dickinson (MD) and Behroozi models of SFR for two different values of the minimum delay time, ﹩{t}_{d}^{\min }=0.5\,\mathrm{Gyr}﹩ and 2 Gyr. The yellow shaded region denotes the maximum redshift range up to which GW sources can be detected by the LVK detectors. The gray-shaded region is accessible by the stochastic GW background.
Paper: Toward a Precision Measurement of Binary Black Holes Formation Channels Using Gravitational Waves and Emission Lines
Authors: Suvodip Mukherjee, Azadeh Moradinezhad Dizgah
Figure caption: The correlations between GW sources, N GW, and the rms signal of LIM (top panel) and the ELG intensity (bottom panel) as a function of cosmological redshift (shown by the color bar). Different marker styles correspond to the Hα (circles), [O III] (crosses), and [O II] (stars) lines. The large and small markers show the correlations for two different DTDs of ﹩{t}_{d}^{\min }=0.5\,\mathrm{Gyr}﹩ (small markers) and ﹩{t}_{d}^{\min }=2\,\mathrm{Gyr}﹩ (large markers).
Paper: Toward a Precision Measurement of Binary Black Holes Formation Channels Using Gravitational Waves and Emission Lines
Authors: Suvodip Mukherjee, Azadeh Moradinezhad Dizgah
Figure caption: Fisher forecast for measuring the minimum delay time ﹩{t}_{d}^{\min }=0.5\,\mathrm{Gyr}﹩ and power-law index κ of the probability distribution ﹩P({t}_{d})={t}_{d}^{-\kappa }﹩ using LVK data and the emission-line signals from LIM by combining the Hα, [O III], and [O II] lines from SPHEREx (blue and red), and [O II] ELGs from DESI (gray and yellow). The current constraint on the delay time ﹩{t}_{d}^{\min }﹩ is <2.2 Gyr at a 90% credible interval assuming a fixed SFR and κ = 1 obtained from the individual events detected in the first half of the third observation run.
Paper: A Challenge to the Standard Cosmological Model
Authors: Nathan J. Secrest, Sebastian von Hausegger, Mohamed Rameez, Roya Mohayaee, Subir Sarkar
Figure caption: Top: density map of the NVSS-based radio galaxy sample used in this work, in Galactic coordinates, Mollweide projection. The right panel is the smoothed map, using a 1 rad moving average, showing the underlying dipole signal. Bottom: corresponding maps of the WISE-based quasar sample used in this work. The smoothed maps are only for visual purposes and were not used in our analysis.
Paper: Toward a Precision Measurement of Binary Black Holes Formation Channels Using Gravitational Waves and Emission Lines
Authors: Suvodip Mukherjee, Azadeh Moradinezhad Dizgah
Figure caption: The values of elements of matrix  K  for BBHs as a function of redshift for different lines and for three different cases of the DTD, as indicated in the label in the following order (emission line, minimum delay time, and power-law index).
Paper: A Challenge to the Standard Cosmological Model
Authors: Nathan J. Secrest, Sebastian von Hausegger, Mohamed Rameez, Roya Mohayaee, Subir Sarkar
Figure caption: Distribution of CMB dipole offsets and kinematic dipole amplitudes of simulated null skies for the NVSS catalog (left) and WISE (right). Contours of equal p-value (scale on right y-axis) translated to equivalent σ are given (where the peak of the distribution corresponds to 0σ), with the found dipoles marked with plus signs and their p-value in the legends.
Paper: A Challenge to the Standard Cosmological Model
Authors: Nathan J. Secrest, Sebastian von Hausegger, Mohamed Rameez, Roya Mohayaee, Subir Sarkar
Figure caption: Top: TGSS before flux calibration correction. Middle: spectral index map. Bottom: TGSS after flux calibration correction.
Paper: A Challenge to the Standard Cosmological Model
Authors: Nathan J. Secrest, Sebastian von Hausegger, Mohamed Rameez, Roya Mohayaee, Subir Sarkar
Figure caption: Top: drop in source density near ecliptic poles in the AllWISE-based AGN catalog used by Singal (2021). Bottom: trend with Galactic latitude. The dashed lines denote the cuts we employ to account for these effects.
Paper: Evidence for Corotation Origin of Super-metal-rich Stars in LAMOST-Gaia: Multiple Ridges with a Similar Slope in the ϕ versus L z Plane
Authors: Yuqin Chen, Gang Zhao, Haopeng Zhang
Figure caption: Median V R in the ϕ vs. L z space for SMR stars. The red lines for ridges (high V R) and blue lines for undulations (low V R) correspond to a slope of −8 km s−1 kpc deg−1 (expected for CR), while the green line corresponds to 0 km s−1 kpc deg−1 (expected for OLR). Note that the red line of L z = −8 ϕ + 1600  km s−1 kpc corresponds to the location of the Hercules moving group as previously reported by Monari et al. (2019a).
Paper: Evidence for Corotation Origin of Super-metal-rich Stars in LAMOST-Gaia: Multiple Ridges with a Similar Slope in the ϕ versus L z Plane
Authors: Yuqin Chen, Gang Zhao, Haopeng Zhang
Figure caption: Distribution of pericenter and apocenter distances for all SMR stars (solid lines) and stars at the solar azimuth of ϕ ∼ 0 (dash lines). The blue lines are for the main (solid) and the second (dot) peaks in the distributions.
Paper: Evidence for Corotation Origin of Super-metal-rich Stars in LAMOST-Gaia: Multiple Ridges with a Similar Slope in the ϕ versus L z Plane
Authors: Yuqin Chen, Gang Zhao, Haopeng Zhang
Figure caption:  R vs. V coded by the median −U for SMR stars. There is also a similar slope found for the six ridges and undulations.
Paper: Ion and Electron Acceleration in Fully Kinetic Plasma Turbulence
Authors: Luca Comisso, Lorenzo Sironi
Figure caption: (a) Kinetic energy evolution for five representative ions (shades of blue) and five representative electrons (shades of red) that end up in the power-law range of the nonthermal tail. (b) PDFs of ∣J  p ∣/J rms experienced by high-energy ions (blue triangles) and high-energy electrons (red circles) at their t inj and by all our tracked particles at t = 1.25 l/v  A  (black diamonds). (c) Distribution of ions (left) and electrons (right) with respect to W tot and W ∥/W tot, at the end of the β 0 = 0.08 simulation (t = 8 l/v  A ). (d) Median of the conditional PDFs at given W tot for ions (left) and electrons (right) at t = 8 l/v  A  from simulations with different β 0.
Paper: Ion and Electron Acceleration in Fully Kinetic Plasma Turbulence
Authors: Luca Comisso, Lorenzo Sironi
Figure caption: (a) PDFs of ﹩\cos \alpha ﹩ for simulations with ﹩{\beta }_{0}\,\in \left\{0.32,0.16,0.08,0.04\right\}﹩. (b) PDFs of ﹩\cos \alpha ﹩ for particles with kinetic energy in different energy intervals for the simulation with β 0 = 0.08. (c) ﹩\langle {\sin }^{2}\alpha \rangle ﹩ as a function of particle kinetic energy (normalized by ε *) for simulations with different β 0. All plots are obtained from data in the time range tv  A /l ∈ [2, 6]. Horizontal dashed black lines indicate the expectation for isotropic particles.
Paper: Ion and Electron Acceleration in Fully Kinetic Plasma Turbulence
Authors: Luca Comisso, Lorenzo Sironi
Figure caption: (a) Volume rendering of the current density ∣ J ∣ at t = 1.25 l/v  A  from the fiducial simulation (β 0 = 0.08). (b) Zoomed-in subdomain with five x–y slices at different z showing the current density J  z , along with selected magnetic field lines illustrating the presence of magnetic flux ropes. (c) One-dimensional k ⊥ energy spectra of magnetic (blue) and velocity (red) fluctuations at t = 1.25 l/v  A . Different spectral slopes are provided for reference.
Paper: Ion and Electron Acceleration in Fully Kinetic Plasma Turbulence
Authors: Luca Comisso, Lorenzo Sironi
Figure caption: Evolution of the particle energy spectra for (a) ions (s  =  i) and (b) electrons (s  =  e) from the fiducial simulation (β 0 = 0.08). Power-law slopes ﹩p=-d\mathrm{log}{f}_{s}/d\mathrm{log}\varepsilon ﹩ for the nonthermal tail at late times are shown for reference. The insets show the late-time ion (top) and electron (bottom) energy spectra for simulations with ﹩{\beta }_{0}\in \left\{0.32,0.16,0.08,0.04\right\}﹩.
Paper: Long-duration Gamma-Ray Burst and Associated Kilonova Emission from Fast-spinning Black Hole–Neutron Star Mergers
Authors: Jin-Ping Zhu, Xiangyu Ivy Wang, Hui Sun, Yuan-Pei Yang, Zhuo Li, Rui-Chong Hu, Ying Qin, Shichao Wu
Figure caption: Left: lGRB/sGRB classification diagram in the T 90–E p domain (Gruber et al. 2014; von Kienlin et al. 2014; Narayana Bhat et al. 2016; von Kienlin et al. 2020). The dashed line and the gray shaded region are the best-fit and 1σ credible boundaries for distinguishing lGRBs from sGRBs, respectively. The redder (bluer) the color of the point, the higher the possibility of the lGRB (sGRB) origin. Right: E p(1 + z) and E  γ,iso correlation diagram with known redshift data (Amati et al. 2002; Zhang et al. 2009; Minaev & Pozanenko 2020). The solid red and blue lines represent the best-fit correlations for lGRBs and sGRBs, respectively. The green, blue, and orange stars (squares) in both panels represent the placement of the MEs (WEs) for GRB 211211A, GRB 060614, and GRB 211227A, respectively.
Paper: Long-duration Gamma-Ray Burst and Associated Kilonova Emission from Fast-spinning Black Hole–Neutron Star Mergers
Authors: Jin-Ping Zhu, Xiangyu Ivy Wang, Hui Sun, Yuan-Pei Yang, Zhuo Li, Rui-Chong Hu, Ying Qin, Shichao Wu
Figure caption: Left: Gamma-ray (blue points from Yang et al. 2022) and X-ray (green points from BAT and XRT) light curves of GRB 211211A. The blue and green lines are the fittings of the EEs using the fallback accretion model. Right: the detections (circles) and upper limits (inverted triangles) of the multiband data for the GRB 211211A afterglow and associated kilonova emissions. The solid lines and shaded areas represent the best fits and 90% credible intervals for the multiband data, while the contributions from the afterglow emissions are marked as the dashed lines.
Paper: Long-duration Gamma-Ray Burst and Associated Kilonova Emission from Fast-spinning Black Hole–Neutron Star Mergers
Authors: Jin-Ping Zhu, Xiangyu Ivy Wang, Hui Sun, Yuan-Pei Yang, Zhuo Li, Rui-Chong Hu, Ying Qin, Shichao Wu
Figure caption: Burst Alert Telescope (BAT) and Swift X-Ray Telescope (XRT) light curves of GRB211211A (green), GRB060614 (blue), and GRB211227A (orange). The BAT luminosity is calculated at 10 keV. Their MEs and EEs are marked with the triangles and circles, respectively. The dashed lines represent the X-ray light curves that track the ∝ t −5/3 mass fallback accretion.
Paper: Long-duration Gamma-Ray Burst and Associated Kilonova Emission from Fast-spinning Black Hole–Neutron Star Mergers
Authors: Jin-Ping Zhu, Xiangyu Ivy Wang, Hui Sun, Yuan-Pei Yang, Zhuo Li, Rui-Chong Hu, Ying Qin, Shichao Wu
Figure caption: Similar to Figure 2, but for GRB 061006 (green), GRB 061210 (dark blue), and GRB 071227 (purple).
Paper: Long-duration Gamma-Ray Burst and Associated Kilonova Emission from Fast-spinning Black Hole–Neutron Star Mergers
Authors: Jin-Ping Zhu, Xiangyu Ivy Wang, Hui Sun, Yuan-Pei Yang, Zhuo Li, Rui-Chong Hu, Ying Qin, Shichao Wu
Figure caption: The posteriors of the fitting parameters. The medians and 1σ credible intervals are labeled.
Paper: A Mathematical Treatment of the Offset Microlensing Degeneracy
Authors: Keming Zhang, 可名 张, B. Scott Gaudi
Figure caption: Top: fractional magnification difference between (s A = 1, q = 10−4) and (s B = 1.04, q = 10−4), with the color scale shown to the right in log10. Black contours illustrate the locus of equal magnification. The x- and y-axes are in units of θ E. Middle: a zoom-in of the dashed-line boxed region in the top panel. The location of the lens-axis null expected from ξ null,0 is marked with the gold star in the center. Source trajectories with α = 30°, 60° are shown in green and blue dashed lines. Bottom: differences to single-lens light curves for null-crossing trajectories. Dashed lines correspond to s  A  = 1, whereas solid lines are for s  B  = 1.04. Trajectory orientation is marked in the subpanel upper right corners with the same color coding as the middle panel. The α = 30° case is seen to have different caustic entry–exit times but similar caustic-crossing durations.
Paper: Supernova-driven Turbulent Metal Mixing in High-redshift Galactic Disks: Metallicity Fluctuations in the Interstellar Medium and its Imprints on Metal-poor Stars in the Milky Way
Authors: Anne Noer Kolborg, Davide Martizzi, Enrico Ramirez-Ruiz, Hugo Pfister, Charli Sakari, Risa H. Wechsler, Melinda Soares-Furtado
Figure caption: Abundances of selected α-elements of the metal-poor halo stars from Roederer et al. (2014), which we use as our comparison sample. From top left, to bottom right, the panels show the measured abundances of: Mg, Si, Ca, and Ti relative to Fe as function of [Fe/H]. Error bars indicate the total uncertainty as reported by Roederer et al. (2014). The solid, dark purple lines indicate the mean in 0.5 dex wide bins in [Fe/H], and the dashed lines are the 1σ spread in the same bins. The insets in each panel show the abundances of the same elements relative to H. The solid fuchsia lines indicate the best orthogonal distance regression (ODR) fit to the abundances.
Paper: Supernova-driven Turbulent Metal Mixing in High-redshift Galactic Disks: Metallicity Fluctuations in the Interstellar Medium and its Imprints on Metal-poor Stars in the Milky Way
Authors: Anne Noer Kolborg, Davide Martizzi, Enrico Ramirez-Ruiz, Hugo Pfister, Charli Sakari, Risa H. Wechsler, Melinda Soares-Furtado
Figure caption: Same as the bottom row panels in Figure 2 but for the three MW progenitor models with varying ϵ *. The slices are taken at the same mean metallicity as those in Figure 2. Because the total gas mass is the same in the three models the time to reach the same level of enrichment depends solely on ϵ *. The effects of rapid enrichment for the high ϵ * model are clearly evident in the right panel.
Paper: Supernova-driven Turbulent Metal Mixing in High-redshift Galactic Disks: Metallicity Fluctuations in the Interstellar Medium and its Imprints on Metal-poor Stars in the Milky Way
Authors: Anne Noer Kolborg, Davide Martizzi, Enrico Ramirez-Ruiz, Hugo Pfister, Charli Sakari, Risa H. Wechsler, Melinda Soares-Furtado
Figure caption: Comparison of the turbulent velocity dispersion, σ  v , in the three models using the same galaxy potential with varying rates of SNe per unit volume. Time is normalized by the relaxation time, t  r  in all cases. Both the base and low ϵ * models reach a steady state, and the velocity dispersion stays relatively constant. The high ϵ * case, however, does not reach dynamical stability, similarly to what was observed for the satellite model in Section 3.1.
Paper: Supernova-driven Turbulent Metal Mixing in High-redshift Galactic Disks: Metallicity Fluctuations in the Interstellar Medium and its Imprints on Metal-poor Stars in the Milky Way
Authors: Anne Noer Kolborg, Davide Martizzi, Enrico Ramirez-Ruiz, Hugo Pfister, Charli Sakari, Risa H. Wechsler, Melinda Soares-Furtado
Figure caption: [Mg/Fe] vs. [Fe/H] abundance measurements of non-CEMP stars in the MW halo from Jinabase (Abohalima & Frebel 2018). The colored crosses the intrinsic dispersion of measurements for a selection of stars. Black dashed–dotted lines indicate the 1σ spread of these stars in the same [Fe/H] bins as used in Figure A1. The purple dashed lines are the same as in the [Mg/Fe] panel in Figure A1 and have been added to aid comparison.
Paper: Supernova-driven Turbulent Metal Mixing in High-redshift Galactic Disks: Metallicity Fluctuations in the Interstellar Medium and its Imprints on Metal-poor Stars in the Milky Way
Authors: Anne Noer Kolborg, Davide Martizzi, Enrico Ramirez-Ruiz, Hugo Pfister, Charli Sakari, Risa H. Wechsler, Melinda Soares-Furtado
Figure caption: Yield abundances of SNe as a function of the progenitor mass and metallicity according to Kobayashi et al. (2006). The horizontal lines show the IMF-weighted average yields at the same metallicities. Also shown is the mean abundance of the (Roederer et al. 2014) sample (solid black line) as well as the abundance of the most and least enriched stars in that sample (black dashed lines). The gray box indicates the yields used in this work [Mg/Fe] = 0.72 and [Mg/Fe] = −1.39 (lower yield not visible in this panel).
Paper: Supernova-driven Turbulent Metal Mixing in High-redshift Galactic Disks: Metallicity Fluctuations in the Interstellar Medium and its Imprints on Metal-poor Stars in the Milky Way
Authors: Anne Noer Kolborg, Davide Martizzi, Enrico Ramirez-Ruiz, Hugo Pfister, Charli Sakari, Risa H. Wechsler, Melinda Soares-Furtado
Figure caption: Mass ratio of Mg to H as a function of the same for Fe to H for the 224 stars from (Roederer et al. 2014). The solid line is the best linear fit to the data and is used to determine the mass of Fe per SNe for the chemically identical SNe models used in this project.
Paper: Supernova-driven Turbulent Metal Mixing in High-redshift Galactic Disks: Metallicity Fluctuations in the Interstellar Medium and its Imprints on Metal-poor Stars in the Milky Way
Authors: Anne Noer Kolborg, Davide Martizzi, Enrico Ramirez-Ruiz, Hugo Pfister, Charli Sakari, Risa H. Wechsler, Melinda Soares-Furtado
Figure caption: Same as Figure 2 but showing the [Mg/Fe] abundance in place of the [Fe/H] abundance from the simulations with intrinsic SN yield variations described in Section 2.1 and empirically derived in Appendix A.
Paper: Supernova-driven Turbulent Metal Mixing in High-redshift Galactic Disks: Metallicity Fluctuations in the Interstellar Medium and its Imprints on Metal-poor Stars in the Milky Way
Authors: Anne Noer Kolborg, Davide Martizzi, Enrico Ramirez-Ruiz, Hugo Pfister, Charli Sakari, Risa H. Wechsler, Melinda Soares-Furtado
Figure caption: Comparison of the 1D distribution of [Fe/H] in the three models at mean [Fe/H] = −2.25. Also shown are the 1σ spread of observations of [Fe/H] at the same corresponding mean [Fe/H] metallicity (dashed lines).