adsabs/AstroCLIMB huggingface dataset:
Paper: Can Supernovae from Runaway Stars Mimic the Signs of Absorbing “Supervirial” Gas?
Authors: Mukesh Singh Bisht, Projjwal Banerjee, Biman B. Nath, Yuri Shchekinov
Figure caption: Temperature (solid lines) and velocity profiles (dashed lines) for different values of β when the reverse shock hits the center of the ejecta in the respective cases. Red, green, magenta, and blue colors show the cases with β = 0, 0.15, 0.3, and 0.5, respectively. The profiles are plotted for the fiducial case with E = 1051 erg, M ej = 10 M ⊙, and n 0 = 0.1 cm−3.
Paper: Can Supernovae from Runaway Stars Mimic the Signs of Absorbing “Supervirial” Gas?
Authors: Mukesh Singh Bisht, Projjwal Banerjee, Biman B. Nath, Yuri Shchekinov
Figure caption: Pressure, mass density, and radius profile as a function of M/M ej at three epochs in the characteristic unit. The solid and dashed line shows the case with core+envelope (β = 0.5) and no core, respectively. The blue color shows the mass density profile (right y-axis). The red and green color shows the pressure and radius profile (left y-axis) respectively. The top panel shows the initial setup at t* = 0.01. The middle panel shows the profiles at t* = 0.34 when the reverse shock is about to hit the core for the core+envelope case. The bottom panel shows the profiles when the reverse shock has hit the center of the ejecta at t* = 3.09 for the core+envelope case. For the no core case, the reverse shock has already hit the center by t* = 3.09, and the secondary shock wave has started traveling outward, as can be seen by the jump in pressure (dashed red line) and density profile (dashed blue line).
Paper: Can Supernovae from Runaway Stars Mimic the Signs of Absorbing “Supervirial” Gas?
Authors: Mukesh Singh Bisht, Projjwal Banerjee, Biman B. Nath, Yuri Shchekinov
Figure caption: Temporal evolution of the position of the reverse shock front in Eulerian coordinate r RS (dashed lines) and Lagrangian coordinate m RS (solid lines) for the different density profiles in characteristic coordinates. The red, green, magenta, and blue lines show the variation for β = 0, 0.15, 0.3, and 0.5, respectively.
Paper: Can Supernovae from Runaway Stars Mimic the Signs of Absorbing “Supervirial” Gas?
Authors: Mukesh Singh Bisht, Projjwal Banerjee, Biman B. Nath, Yuri Shchekinov
Figure caption: Mean molecular weight profile as a function of M/M ej calculated using KEPLER. The black, green, blue, and red lines show the mean molecular weight profile for β = 0, 0.15, 0.30, and 0.50, respectively.
Paper: Can Supernovae from Runaway Stars Mimic the Signs of Absorbing “Supervirial” Gas?
Authors: Mukesh Singh Bisht, Projjwal Banerjee, Biman B. Nath, Yuri Shchekinov
Figure caption: Mass fraction of different elements as a function of M/M ej obtained using KEPLER. The magenta, red, blue, and green lines show oxygen, neon, magnesium, and silicon mass fraction profiles, respectively. The solid, dashed, and dotted lines refer to the case with β = 0.5, 0.3, and 0.15 corresponding to 25, 18, and 11 M ⊙ mass models, respectively.
Paper: A Closer Look at Dwarf Galaxies Exhibiting Mid-infrared Variability: Active Galactic Nuclei Confirmation and Comparison With Nonvariable Dwarf Galaxies
Authors: Archana Aravindan, Gabriela Canalizo, Nathan Secrest, Shobita Satyapal, Thomas Bohn
Figure caption: NIR diagnostic diagrams using AGN and SF limits from A. Calabrò et al. (2023). The targets are marked as J0847 (1), J0928 (2), J1032 (3), J1144 (4), J1205 (5), J1320 (6), J1358 (7), J1428 (8), J1612 (9). For the targets where some of the line fluxes were not available, we plot them as open circles with arrows, indicating upper and lower limits. Dwarf Galaxies with AGN from T. Bohn et al. (2021) and Type 2 AGN from R. Riffel et al. (2006) are plotted in red and green, respectively. The gas-phase metallicity (Z) increases from bottom to top, and the ionization parameter (log (U)) increases from right to left. Four of the targets moved to the composite/AGN region across all four NIR diagnostic diagrams, as compared to their positions in the SF region in the optical diagnostic diagrams.
Paper: A Closer Look at Dwarf Galaxies Exhibiting Mid-infrared Variability: Active Galactic Nuclei Confirmation and Comparison With Nonvariable Dwarf Galaxies
Authors: Archana Aravindan, Gabriela Canalizo, Nathan Secrest, Shobita Satyapal, Thomas Bohn
Figure caption: Flowchart summarizing the results characterizing the effectiveness of MIR variability in tracing AGN activity in low-mass galaxies.
Paper: A Closer Look at Dwarf Galaxies Exhibiting Mid-infrared Variability: Active Galactic Nuclei Confirmation and Comparison With Nonvariable Dwarf Galaxies
Authors: Archana Aravindan, Gabriela Canalizo, Nathan Secrest, Shobita Satyapal, Thomas Bohn
Figure caption: Histograms showing the comparison of optical properties of the variable and the nonvariable dwarf galaxies. The dashed lines indicate the average values for the two samples. We do not find a significant difference in several key optical properties, such as extinction, [O III] luminosity, optical colors, and SFRs.
Paper: A Closer Look at Dwarf Galaxies Exhibiting Mid-infrared Variability: Active Galactic Nuclei Confirmation and Comparison With Nonvariable Dwarf Galaxies
Authors: Archana Aravindan, Gabriela Canalizo, Nathan Secrest, Shobita Satyapal, Thomas Bohn
Figure caption: Black hole vs. stellar mass for a sample of galaxies at low redshift. The yellow points are galaxies at a redshift < 0.06 and include dwarf galaxies with broad lines from A. E. Reines & M. Volonteri (2015, RV15). The solid line is the expected linear regression from Equations (4) and (5) in RV15 along with the 0.5 dex error, indicated by the gray-shaded region. The two blue points indicate the calculated BH masses based on the broad Paα for J0928 and J1144, respectively, which fits well with the expected black hole mass for the two galaxies.
Paper: A Closer Look at Dwarf Galaxies Exhibiting Mid-infrared Variability: Active Galactic Nuclei Confirmation and Comparison With Nonvariable Dwarf Galaxies
Authors: Archana Aravindan, Gabriela Canalizo, Nathan Secrest, Shobita Satyapal, Thomas Bohn
Figure caption: The BPT diagram of the variable and nonvariable samples. Galaxies with log [N II]/Hα < −1 (indicative of low metallicity) are in the blue-shaded region. Using log [N II]/Hα as a proxy for metallicity, we find that a larger fraction of variable dwarfs have higher metallicities than nonvariable dwarfs.
Paper: A Closer Look at Dwarf Galaxies Exhibiting Mid-infrared Variability: Active Galactic Nuclei Confirmation and Comparison With Nonvariable Dwarf Galaxies
Authors: Archana Aravindan, Gabriela Canalizo, Nathan Secrest, Shobita Satyapal, Thomas Bohn
Figure caption: The WISE color–color diagram for the variable and nonvariable galaxies, with histograms plotting the distribution of the values in W1 − W2 (right) and W2 − W3 (top). Although both samples have similar W1 − W2 colors, nonvariable galaxies have redder W2 − W3 colors.
Paper: A Closer Look at Dwarf Galaxies Exhibiting Mid-infrared Variability: Active Galactic Nuclei Confirmation and Comparison With Nonvariable Dwarf Galaxies
Authors: Archana Aravindan, Gabriela Canalizo, Nathan Secrest, Shobita Satyapal, Thomas Bohn
Figure caption: Plot of the Hα FWHM vs. the [O III] FWHM for the variable and nonvariable targets. A larger fraction of variable targets have very broad (FWHM > 500 km s−1) Balmer lines than nonvariable targets.
Paper: A Closer Look at Dwarf Galaxies Exhibiting Mid-infrared Variability: Active Galactic Nuclei Confirmation and Comparison With Nonvariable Dwarf Galaxies
Authors: Archana Aravindan, Gabriela Canalizo, Nathan Secrest, Shobita Satyapal, Thomas Bohn
Figure caption: Histograms showing the distribution of the WISE W1 − W2 colors and stellar masses of the target sample of variable dwarf galaxies and the control sample of nonvariable dwarf galaxies.
Paper: Variable Ionized Disk Winds in MAXI J1803−298 Revealed by NICER
Authors: Zuobin Zhang, Cosimo Bambi, Honghui Liu, Jiachen Jiang, Fangzheng Shi, Yuexin Zhang, Andrew J. Young, John A. Tomsick, Benjamin M. Coughenour, Menglei Zhou
Figure caption: Sketch of the wind evolution across the HID of MAXI J1803−298 (based on D. Mata Sánchez et al. 2022 and this work). We use stars to mark the spectroscopic epochs of optical observations, with solid stars for the observation showing optical wind features and hollow stars for the observations without optical wind features. We use circles to mark the 10 epochs analyzed in this work. The darkness of the filling color represents the intensity of the X-ray disk winds (using the column density as proxy). The stronger the X-ray wind, the darker the filling color. The blurred green and red line indicate the (approximate) location of the wind detections at optical and X-ray band, respectively. The darkness of the color of the red line shows the strength of X-ray disk winds. A transition from optical wind to X-ray wind is clearly shown.
Paper: Variable Ionized Disk Winds in MAXI J1803−298 Revealed by NICER
Authors: Zuobin Zhang, Cosimo Bambi, Honghui Liu, Jiachen Jiang, Fangzheng Shi, Yuexin Zhang, Andrew J. Young, John A. Tomsick, Benjamin M. Coughenour, Menglei Zhou
Figure caption: NICER light curve with a time bin size of 30 s derived in the 0.5–10 keV (top panel), 0.5–4 keV (middle top panel), 4–10 keV bands (middle panel), and hardness derived between the 4–10 and 0.5–4 keV bands (middle bottom panel). The corresponding dynamical power density is shown in the bottom panel.
Paper: Variable Ionized Disk Winds in MAXI J1803−298 Revealed by NICER
Authors: Zuobin Zhang, Cosimo Bambi, Honghui Liu, Jiachen Jiang, Fangzheng Shi, Yuexin Zhang, Andrew J. Young, John A. Tomsick, Benjamin M. Coughenour, Menglei Zhou
Figure caption: PDS of Epoch 1 (red), Epoch 2 (green), and Epoch 3 (blue), scaled with frequency to illustrate the potential QPOs rather than the low-frequency red noise. We artificially multiply the power by a different factor for plotting clarity.
Paper: A Two-zone Accretion Disk in the Changing-look Active Galactic Nucleus 1ES 1927+654: Physical Implications for Tidal Disruption Events and Super-Eddington Accretion
Authors: Ruancun Li, Luis C. Ho, Claudio Ricci, Benny Trakhtenbrot
Figure caption: The blackbody temperature (T bb) as a function of photosphere size (R ph; Equation (24)) of the inner overheated disk from this work (green points) and from the NICER X-ray observations (gray points) of M. Masterson et al. (2022). The green solid line gives the linear fit for the points with ﹩{R}_{\mathrm{tr}}\gtrsim {R}_{\mathrm{br}}﹩, ﹩\mathrm{log}{T}_{\mathrm{bb}}=-0.60\mathrm{log}({R}_{\mathrm{ph}}/{R}_{g})+6.85﹩, with the 1σ uncertainty shown as the shaded region. The vertical lines mark the inner disk radius (R in; dashed) and the break radius (R br; dotted) in Equation (28). The three blue shaded curves depict the temperature–size relation of the slim accretion disk solution of M. A. Abramowicz et al. (1988) for ﹩\dot{m}=10﹩, 1, and 0.1.
Paper: A Two-zone Accretion Disk in the Changing-look Active Galactic Nucleus 1ES 1927+654: Physical Implications for Tidal Disruption Events and Super-Eddington Accretion
Authors: Ruancun Li, Luis C. Ho, Claudio Ricci, Benny Trakhtenbrot
Figure caption: Characteristic radius of the accretion flow as a function of time since the optical outburst. Red points give the inner truncation radius (R tr) of the outer thin disk, which was derived directly from broadband SED fitting (R. Li et al. 2024). Green points show the photosphere size (﹩{R}_{\mathrm{ph}}^{\mathrm{SED}}﹩) calculated through Equation (24), with T bb and L bb derived from broadband SED fitting (R. Li et al. 2024). The gray points correspond to the photosphere size (﹩{R}_{\mathrm{ph}}^{{\rm{X}}-\mathrm{ray}}﹩) obtained from X-ray observations alone (M. Masterson et al. 2022). The stars and the horizontal dashed lines mark the preoutburst values of R tr (red) and ﹩{R}_{\mathrm{ph}}^{\mathrm{SED}}﹩ (green) calculated from the 2011 observation (R. Li et al. 2024). The black dotted line shows the inner disk radius (R in = 1.45 R  g ) adopted in this paper.
Paper: A Two-zone Accretion Disk in the Changing-look Active Galactic Nucleus 1ES 1927+654: Physical Implications for Tidal Disruption Events and Super-Eddington Accretion
Authors: Ruancun Li, Luis C. Ho, Claudio Ricci, Benny Trakhtenbrot
Figure caption: The variation with truncation radius (R tr) of (a) the normalized effective temperature (﹩{T}_{\mathrm{eff}}\,{\dot{m}}^{-1/4}﹩) and (b) corona bolometric correction (L bol/L cor). The color of the circles represents the time since the outburst (2017 December 23), from the beginning (green) to the end (red), where the orange one denotes t ≈ 650 days. The red star shows the value in May 2011, before the outburst. The red dashed line shows the power-law fit of Equation (26) and its 1σ uncertainty (shaded region), while the corresponding broken power-law fit of Equation (27) is depicted as the blue solid line and shaded region. The vertical black dotted line marks the break radius (R br).
Paper: A Two-zone Accretion Disk in the Changing-look Active Galactic Nucleus 1ES 1927+654: Physical Implications for Tidal Disruption Events and Super-Eddington Accretion
Authors: Ruancun Li, Luis C. Ho, Claudio Ricci, Benny Trakhtenbrot
Figure caption: The normalized disk equatorial temperature (﹩{{T}_{c}}^{{\prime} }﹩; Equation (34)) as a function of normalized disk mass surface density (﹩{{\rm{\Sigma }}}^{{\prime} }﹩; Equation (35)). The color of the circles represents the time since the outburst (2017 December 23), from the beginning (green) to the end (red), where the orange one denotes t ≈ 650 days. The red star shows the value in 2011 May, before the outburst. The dashed line shows ﹩{T}_{c}^{{\prime} }\propto {{\rm{\Sigma }}}^{{\prime} 1/4}﹩, which is expected from an advection-dominated slim disk, while the dotted line represents ﹩{T}_{c}^{{\prime} }\propto {{\rm{\Sigma }}}^{{\prime} 0}﹩ as expected from a radiation-pressure-dominated thin disk. The two arrows indicate the direction of movement of 1ES 1927+654 along the slim disk and thin disk branches of the S-curve before and after t = 650 days, respectively.
Paper: A Two-zone Accretion Disk in the Changing-look Active Galactic Nucleus 1ES 1927+654: Physical Implications for Tidal Disruption Events and Super-Eddington Accretion
Authors: Ruancun Li, Luis C. Ho, Claudio Ricci, Benny Trakhtenbrot
Figure caption: The variation with R tr of the disk midplane temperature (T  c ; blue points) and effective temperature (T eff; red points) at R tr. The corresponding linear fits and 1σ uncertainty are ﹩\mathrm{log}({T}_{c}/{\rm{K}})=(-0.37\pm 0.02)\mathrm{log}({R}_{\mathrm{tr}}/{R}_{g})+(6.38\pm 0.02)﹩ (blue line) and ﹩\mathrm{log}{T}_{\mathrm{eff}}=(-0.47\pm 0.04)\mathrm{log}({R}_{\mathrm{tr}}/{R}_{g})+(6.11\pm 0.04)﹩ (red line). The vertical black dashed line marks the inner disk radius (R in).
Paper: A Two-zone Accretion Disk in the Changing-look Active Galactic Nucleus 1ES 1927+654: Physical Implications for Tidal Disruption Events and Super-Eddington Accretion
Authors: Ruancun Li, Luis C. Ho, Claudio Ricci, Benny Trakhtenbrot
Figure caption: Flux reduction factor (χ ≡ F out/σ T 4) as a function of radius of the inner disk overheated because of photon trapping (Section 3.2) and electron scattering (Section 3.3), as deduced for the 2018 May 17 observations of 1ES 1927+654. Solid lines assume the ﹩\bar{\rho }﹩ and T profile for a radiatively cooled accretion flow (thin disk), while dotted lines pertain to an optically thick ADAF (slim disk). Different colors represent different inclination angles of the disk.
Paper: A Two-zone Accretion Disk in the Changing-look Active Galactic Nucleus 1ES 1927+654: Physical Implications for Tidal Disruption Events and Super-Eddington Accretion
Authors: Ruancun Li, Luis C. Ho, Claudio Ricci, Benny Trakhtenbrot
Figure caption: The dependence of the truncation radius (R tr) on the dimensionless mass accretion rate (﹩\dot{m}﹩). The horizontal dotted line marks the break radius defined in Equation (28). The green solid line shows a linear fit for all the points, while the blue solid line only fits the points with ﹩{R}_{\mathrm{tr}}\gt {R}_{\mathrm{br}};﹩ the shaded regions denote the 1σ uncertainties of the fits.
Paper: A Two-zone Accretion Disk in the Changing-look Active Galactic Nucleus 1ES 1927+654: Physical Implications for Tidal Disruption Events and Super-Eddington Accretion
Authors: Ruancun Li, Luis C. Ho, Claudio Ricci, Benny Trakhtenbrot
Figure caption: The free–free emission capability (﹩{\dot{w}}_{\mathrm{ff}}﹩) vs. the viscous heating rate density (﹩{\dot{w}}^{+}﹩) at ﹩R={R}_{\mathrm{tr}}﹩, color-coded by the time since the outburst (2017 December 23), from the beginning (green) to the end (red), where the orange one denotes t ≈ 650 days. The red star shows the value in 2011 May, before the outburst. The black dashed line denotes ﹩{\dot{w}}_{\mathrm{ff}}=0.1{\dot{w}}^{+}﹩, while the dotted line gives ﹩{\dot{w}}_{\mathrm{ff}}={\dot{w}}^{+}﹩.
Paper: A Two-zone Accretion Disk in the Changing-look Active Galactic Nucleus 1ES 1927+654: Physical Implications for Tidal Disruption Events and Super-Eddington Accretion
Authors: Ruancun Li, Luis C. Ho, Claudio Ricci, Benny Trakhtenbrot
Figure caption: The normalized disk mass surface density (﹩{{\rm{\Sigma }}}^{{\prime} }﹩; Equation (35)) as a function of the corona optical depth (τ). The color of the circles represents the time since the outburst (2017 December 23), from the beginning (green) to the end (red), where the orange one denotes t ≈ 650 days. The red star shows the value in 2011 May, before the outburst. The solid line gives the linear fit ﹩\mathrm{log}{{\rm{\Sigma }}}^{{\prime} }=(0.37\pm 0.08)\mathrm{log}\tau +(4.01\pm 0.13)﹩, with the gray shaded region representing the 1σ uncertainty of the fit.
Paper: SMILES: A Prototype JWST Multiband Mid-infrared Survey
Authors: G. H. Rieke, Stacey Alberts, Irene Shivaei, Jianwei Lyu, Christopher N. A. Willmer, Pablo Pérez-González, Christina C. Williams
Figure caption: Identification of embedded AGNs with SMILES data: the top and third frames show purely star-forming galaxies at redshifts of ∼1 and 2. The second frame is a powerful obscured AGN at z ∼ 1, and the bottom frame is a mixed AGN/star-forming galaxy at z ∼ 2, from J. Lyu et al. (2024). All of the filter profiles are shown along the bottom of the frames, and the wavelengths have been shifted to the rest frame; in addition to SMILES data, the shorter wavelength measurements are from CANDELS (N. A. Grogin et al. 2011), JADES (M. J. Rieke et al. 2023), and JEMS (C. C. Williams et al. 2023). A model has been fitted to the photometry using Prospector: the green lines are for the stellar component, both the direct photospheric output and the infrared excess; the blue line is a template AGN SED. The measurements are shown as open circles with error bars, and the blue squares are the result of synthetic photometry on the model. For these sources, there are solid detections out through 25.5 μm, except for JADES 200174 where there is a significant error bar on that point. Very light lines show a range of SEDs for the AGN and star-forming templates.
Paper: SMILES: A Prototype JWST Multiband Mid-infrared Survey
Authors: G. H. Rieke, Stacey Alberts, Irene Shivaei, Jianwei Lyu, Christopher N. A. Willmer, Pablo Pérez-González, Christina C. Williams
Figure caption: A summary of the characteristics of mid-infrared surveys operating over the range 8 < λ < 30 μm. The detection limits and beam areas are plotted in reverse order so that better is always to the upper right. The bands in a survey are color coded, from dark blue for 8–9.5 μm to red for 24.5–27 μm. This figure illustrates the nearly unique status of SMILES in terms of sensitivity, angular resolution, and number of bands between 8 and 26 μm (the CEERS MIRI survey (G. Yang et al. 2023) includes all the bands shown but one and covers ∼20% as large a field). To avoid clutter, the MSX/SPIRIT III survey has been left out of the figure; the sensitivity values are similar to those from IRAS, and the beam area falls modestly to the left (larger values) compared with the other 1996–2011 surveys.
Paper: SMILES: A Prototype JWST Multiband Mid-infrared Survey
Authors: G. H. Rieke, Stacey Alberts, Irene Shivaei, Jianwei Lyu, Christopher N. A. Willmer, Pablo Pérez-González, Christina C. Williams
Figure caption: Measurement of PAH band strengths with the SMILES photometry, for galaxies from z = 0.72 (bottom) to 1.92 (top), from I. Shivaei et al. (2024; all measurements are shifted to the rest frame). The shorter wavelength bands that extensively trace the output of the stars in the galaxies are from the CANDELS (N. A. Grogin et al. 2011), JADES (M. J. Rieke et al. 2023), and JEMS (C. C. Williams et al. 2023) programs. The MIRI filter bands are shown along the bottom of each frame with the corresponding fluxes as dots against a template-derived PAH spectrum. The detections extend through 25.5  μm.
Paper: SMILES: A Prototype JWST Multiband Mid-infrared Survey
Authors: G. H. Rieke, Stacey Alberts, Irene Shivaei, Jianwei Lyu, Christopher N. A. Willmer, Pablo Pérez-González, Christina C. Williams
Figure caption: SMILES footprint (red) relative to other HUDF surveys: JADES NIRCam deep (solid green line) and medium (dashed green line), FRESCO NIRCam/grism coverage (solid blue line), HST ACS GOODS-S coverage (thick gray line), and Chandra X-ray coverage (light-blue shaded region) and JVLA radio observations at 3 GHz (dark green lines) and 6 GHz (dark orange lines), respectively.
Paper: A Comprehensive Study of Open Cluster Chemical Homogeneity Using APOGEE and Milky Way Mapper Abundances
Authors: Amaya Sinha, Gail Zasowski, Peter Frinchaboy, Katia Cunha, Diogo Souto, Jamie Tayar, Keivan Stassun
Figure caption: A violin plot comparing the difference in element intrinsic scatter between open clusters and matched samples of field stars as shown in Section 5.1. Here the elements that belong to the α, CNO, and iron-peak families are shaded in gray as we expect them to be similar due to our selection criteria. Within these elements P and V have larger limits due to them being weak-lined elements from the BAWLAS catalog. While broadly we find that the field-star samples have more scatter than their OC counterparts, we do not find any conclusive difference in any element between the two samples.
Paper: A Comprehensive Study of Open Cluster Chemical Homogeneity Using APOGEE and Milky Way Mapper Abundances
Authors: Amaya Sinha, Gail Zasowski, Peter Frinchaboy, Katia Cunha, Diogo Souto, Jamie Tayar, Keivan Stassun
Figure caption: The 99.7% upper limits using abundances from IPL-3 ASPCAP in M67, NGC 6791, and NGC 6819. The median 99.7 percentile upper limit for each cluster is shown as a magenta horizontal line. We compare our findings to upper limits and measurements from previous literature. The upper limits are broadly in agreement with other studies for well-measured elements in APOGEE and Milky Way Mapper.
Paper: A Comprehensive Study of Open Cluster Chemical Homogeneity Using APOGEE and Milky Way Mapper Abundances
Authors: Amaya Sinha, Gail Zasowski, Peter Frinchaboy, Katia Cunha, Diogo Souto, Jamie Tayar, Keivan Stassun
Figure caption: Outside red: the initial likelihood surface over which we initially test to determine a best guess for σ [X/Fe]. Within red: using the findings from the initial run, we more finely sample the likelihood surface in order to measure the final intrinsic scatter and uncertainty.
Paper: A Comprehensive Study of Open Cluster Chemical Homogeneity Using APOGEE and Milky Way Mapper Abundances
Authors: Amaya Sinha, Gail Zasowski, Peter Frinchaboy, Katia Cunha, Diogo Souto, Jamie Tayar, Keivan Stassun
Figure caption: Uncalibrated surface gravity vs. [Mg/Fe] for M67. The [Mg/Fe] values from DR17 are shown in black, and have a clear linear relationship with log(g). The adjusted abundances used in the calculation of intrinsic scatter are shown in red.