adsabs/AstroCLIMB huggingface dataset:
Paper: Chemical Cartography with APOGEE: Mapping Disk Populations with a 2-process Model and Residual Abundances
Authors: David H. Weinberg, Jon A. Holtzman, Jennifer A. Johnson, Christian Hayes, Sten Hasselquist, Matthew Shetrone, Yuan-Sen Ting, 源森 丁, Rachael L. Beaton, Timothy C. Beers, Jonathan C. Bird, Dmitry Bizyaev, Michael R. Blanton, Katia Cunha, José G. Fernández-Trincado, Peter M. Frinchaboy, D. A. García-Hernández, Emily Griffith, James W. Johnson, Henrik Jönsson, Richard R. Lane, Henry W. Leung, J. Ted Mackereth, Steven R. Majewski, Szabolcs Mészáros, Christian Nitschelm, Kaike Pan, Ricardo P. Schiavon, Donald P. Schneider, Mathias Schultheis, Verne Smith, Jennifer S. Sobeck, Keivan G. Stassun, Guy S. Stringfellow, Fiorenzo Vincenzo, John C. Wilson, Gail Zasowski
Figure caption: Top: dispersion of [X/H] values relative to 2-process predictions, in dex. Filled circles show results for the data. Open squares show results from the simulation in which stars lie on the 2-process model except for Gaussian errors. Red crosses show the mean observational error. Elements used in the 2-process fit are denoted in blue on the horizontal axis. Bottom: filled circles, repeated from the top panel, show the total dispersion. Open circles show the intrinsic dispersion estimated by subtracting in quadrature the dispersion of the simulated data set (i.e., the squares in the top panel). Open triangles show an alternative estimate of the intrinsic dispersion obtained by subtracting half of the 16%–84% percentile range (±1σ for a Gaussian distribution), in quadrature, for the simulated data from the same quantity for the observed data.
Paper: Chemical Cartography with APOGEE: Mapping Disk Populations with a 2-process Model and Residual Abundances
Authors: David H. Weinberg, Jon A. Holtzman, Jennifer A. Johnson, Christian Hayes, Sten Hasselquist, Matthew Shetrone, Yuan-Sen Ting, 源森 丁, Rachael L. Beaton, Timothy C. Beers, Jonathan C. Bird, Dmitry Bizyaev, Michael R. Blanton, Katia Cunha, José G. Fernández-Trincado, Peter M. Frinchaboy, D. A. García-Hernández, Emily Griffith, James W. Johnson, Henrik Jönsson, Richard R. Lane, Henry W. Leung, J. Ted Mackereth, Steven R. Majewski, Szabolcs Mészáros, Christian Nitschelm, Kaike Pan, Ricardo P. Schiavon, Donald P. Schneider, Mathias Schultheis, Verne Smith, Jennifer S. Sobeck, Keivan G. Stassun, Guy S. Stringfellow, Fiorenzo Vincenzo, John C. Wilson, Gail Zasowski
Figure caption: Same as Figure 4 but for odd-Z iron-peak elements and the s-process element Ce.
Paper: Chemical Cartography with APOGEE: Mapping Disk Populations with a 2-process Model and Residual Abundances
Authors: David H. Weinberg, Jon A. Holtzman, Jennifer A. Johnson, Christian Hayes, Sten Hasselquist, Matthew Shetrone, Yuan-Sen Ting, 源森 丁, Rachael L. Beaton, Timothy C. Beers, Jonathan C. Bird, Dmitry Bizyaev, Michael R. Blanton, Katia Cunha, José G. Fernández-Trincado, Peter M. Frinchaboy, D. A. García-Hernández, Emily Griffith, James W. Johnson, Henrik Jönsson, Richard R. Lane, Henry W. Leung, J. Ted Mackereth, Steven R. Majewski, Szabolcs Mészáros, Christian Nitschelm, Kaike Pan, Ricardo P. Schiavon, Donald P. Schneider, Mathias Schultheis, Verne Smith, Jennifer S. Sobeck, Keivan G. Stassun, Guy S. Stringfellow, Fiorenzo Vincenzo, John C. Wilson, Gail Zasowski
Figure caption: Distribution of stars in the 2-process parameters A Ia/A cc vs. A cc, in zones of Galactocentric radius (columns) and midplane distance (rows) as labeled. A cc measures the abundance of CCSN elements (e.g., Mg) relative to solar, and A Ia/A cc measures the ratio of SNIa to CCSN enrichment; A Ia = A cc = 1 for solar abundances. Red and blue points show stars in the low-Ia and high-Ia population, respectively. To improve coverage of the inner Galaxy, this plot uses the SN100 sample, which has a S/N threshold of 100 at all [Mg/H] values. Although we use six elements to fit stellar values of A cc and A Ia, they are generally close to the values implied by Mg and Fe, so this plot resembles a plot of [Fe/Mg] vs. [Mg/H] but with transformed variables that are linearly proportional to the inferred CCSN and SNIa content.
Paper: Chemical Cartography with APOGEE: Mapping Disk Populations with a 2-process Model and Residual Abundances
Authors: David H. Weinberg, Jon A. Holtzman, Jennifer A. Johnson, Christian Hayes, Sten Hasselquist, Matthew Shetrone, Yuan-Sen Ting, 源森 丁, Rachael L. Beaton, Timothy C. Beers, Jonathan C. Bird, Dmitry Bizyaev, Michael R. Blanton, Katia Cunha, José G. Fernández-Trincado, Peter M. Frinchaboy, D. A. García-Hernández, Emily Griffith, James W. Johnson, Henrik Jönsson, Richard R. Lane, Henry W. Leung, J. Ted Mackereth, Steven R. Majewski, Szabolcs Mészáros, Christian Nitschelm, Kaike Pan, Ricardo P. Schiavon, Donald P. Schneider, Mathias Schultheis, Verne Smith, Jennifer S. Sobeck, Keivan G. Stassun, Guy S. Stringfellow, Fiorenzo Vincenzo, John C. Wilson, Gail Zasowski
Figure caption: Top: correlation of abundance residuals (measured abundance—2-process prediction) with T eff for Ca, Ni, Mn, and Co. Magenta points and lines show the median residuals in 100 K bins of T eff and the linear trends fit to these medians. Middle: correlation of abundance residuals for the element pairs Ca–Ni, Ca–Mn, Co–Ni, and Co–Mn (left to right). Correlation coefficients are listed in each panel. Bottom: same as middle using abundances that have been corrected for the temperature trends as described in the text. In all panels, points have been downsampled by a factor of 10 to reduce crowding, and abundance residuals are shown in dex.
Paper: Chemical Cartography with APOGEE: Mapping Disk Populations with a 2-process Model and Residual Abundances
Authors: David H. Weinberg, Jon A. Holtzman, Jennifer A. Johnson, Christian Hayes, Sten Hasselquist, Matthew Shetrone, Yuan-Sen Ting, 源森 丁, Rachael L. Beaton, Timothy C. Beers, Jonathan C. Bird, Dmitry Bizyaev, Michael R. Blanton, Katia Cunha, José G. Fernández-Trincado, Peter M. Frinchaboy, D. A. García-Hernández, Emily Griffith, James W. Johnson, Henrik Jönsson, Richard R. Lane, Henry W. Leung, J. Ted Mackereth, Steven R. Majewski, Szabolcs Mészáros, Christian Nitschelm, Kaike Pan, Ricardo P. Schiavon, Donald P. Schneider, Mathias Schultheis, Verne Smith, Jennifer S. Sobeck, Keivan G. Stassun, Guy S. Stringfellow, Fiorenzo Vincenzo, John C. Wilson, Gail Zasowski
Figure caption: Examples of 2-process fits to element abundance ratios, for two low-Ia stars (rows one and two) with subsolar [Mg/H] and two high-Ia stars (rows three and four) with near-solar [Mg/H] and [Mg/Fe]. The first and third stars have χ 2 values near the median of the distribution for sample stars, while the second and fourth stars have χ 2 values near the 98th percentile of this distribution. The model has two free parameters for each star and is fit to the six elements listed in blue on the horizontal axis (Mg, O, Si, Ca, Fe, Ni). In each panel, filled points with error bars show the measured value of [X/H] and the ASPCAP error. Open circles show the abundances predicted by the 2-process fit. Solid and dotted lines are present to guide the eye. Colored bars along the bottom of each panel group α elements (blue), light odd-Z elements (green), even-Z iron-peak elements (red), and odd-Z iron-peak elements (magenta).
Paper: Chemical Cartography with APOGEE: Mapping Disk Populations with a 2-process Model and Residual Abundances
Authors: David H. Weinberg, Jon A. Holtzman, Jennifer A. Johnson, Christian Hayes, Sten Hasselquist, Matthew Shetrone, Yuan-Sen Ting, 源森 丁, Rachael L. Beaton, Timothy C. Beers, Jonathan C. Bird, Dmitry Bizyaev, Michael R. Blanton, Katia Cunha, José G. Fernández-Trincado, Peter M. Frinchaboy, D. A. García-Hernández, Emily Griffith, James W. Johnson, Henrik Jönsson, Richard R. Lane, Henry W. Leung, J. Ted Mackereth, Steven R. Majewski, Szabolcs Mészáros, Christian Nitschelm, Kaike Pan, Ricardo P. Schiavon, Donald P. Schneider, Mathias Schultheis, Verne Smith, Jennifer S. Sobeck, Keivan G. Stassun, Guy S. Stringfellow, Fiorenzo Vincenzo, John C. Wilson, Gail Zasowski
Figure caption: Distribution of [X/H] deviations from model predictions, normalized by the reported abundance error. Black histograms show results using the full 2-process fit to six abundances. Blue histograms show deviations from the median sequences. Red curves show a Gaussian for reference. The mean ASPCAP error is listed in each panel. For the median trend deviations, the [Mg/H] deviation is zero by definition, giving a zero-width blue histogram.
Paper: Chemical Cartography with APOGEE: Mapping Disk Populations with a 2-process Model and Residual Abundances
Authors: David H. Weinberg, Jon A. Holtzman, Jennifer A. Johnson, Christian Hayes, Sten Hasselquist, Matthew Shetrone, Yuan-Sen Ting, 源森 丁, Rachael L. Beaton, Timothy C. Beers, Jonathan C. Bird, Dmitry Bizyaev, Michael R. Blanton, Katia Cunha, José G. Fernández-Trincado, Peter M. Frinchaboy, D. A. García-Hernández, Emily Griffith, James W. Johnson, Henrik Jönsson, Richard R. Lane, Henry W. Leung, J. Ted Mackereth, Steven R. Majewski, Szabolcs Mészáros, Christian Nitschelm, Kaike Pan, Ricardo P. Schiavon, Donald P. Schneider, Mathias Schultheis, Verne Smith, Jennifer S. Sobeck, Keivan G. Stassun, Guy S. Stringfellow, Fiorenzo Vincenzo, John C. Wilson, Gail Zasowski
Figure caption: Cumulative distribution of χ 2 values for model fits to the sample of 34,110 stars. Values of χ 2 are computed using all 16 elements shown in Figure 9, omitting flagged values. The black solid curve shows results from applying the full 2-process fit, with points marking the median, 95th-percentile, and 99th-percentile values of the distribution (listed in the lower right). The green dotted curve shows results when A Ia and A cc values are inferred from [Mg/H] and [Fe/Mg] alone. The blue dashed curve shows results when abundances are predicted from the observed median trends (blue and red curves in the left panels of Figures 4–7), independent of the 2-process model. The red dashed curve shows results for a simulated data sample in which all stars lie on the 2-process model and arise only from Gaussian noise with the reported abundance errors.
Paper: Chemical Cartography with APOGEE: Mapping Disk Populations with a 2-process Model and Residual Abundances
Authors: David H. Weinberg, Jon A. Holtzman, Jennifer A. Johnson, Christian Hayes, Sten Hasselquist, Matthew Shetrone, Yuan-Sen Ting, 源森 丁, Rachael L. Beaton, Timothy C. Beers, Jonathan C. Bird, Dmitry Bizyaev, Michael R. Blanton, Katia Cunha, José G. Fernández-Trincado, Peter M. Frinchaboy, D. A. García-Hernández, Emily Griffith, James W. Johnson, Henrik Jönsson, Richard R. Lane, Henry W. Leung, J. Ted Mackereth, Steven R. Majewski, Szabolcs Mészáros, Christian Nitschelm, Kaike Pan, Ricardo P. Schiavon, Donald P. Schneider, Mathias Schultheis, Verne Smith, Jennifer S. Sobeck, Keivan G. Stassun, Guy S. Stringfellow, Fiorenzo Vincenzo, John C. Wilson, Gail Zasowski
Figure caption: Same as Figure 4 but showing the light odd-Z elements Na, Al, and K and the element combination C+N.
Paper: Chemical Cartography with APOGEE: Mapping Disk Populations with a 2-process Model and Residual Abundances
Authors: David H. Weinberg, Jon A. Holtzman, Jennifer A. Johnson, Christian Hayes, Sten Hasselquist, Matthew Shetrone, Yuan-Sen Ting, 源森 丁, Rachael L. Beaton, Timothy C. Beers, Jonathan C. Bird, Dmitry Bizyaev, Michael R. Blanton, Katia Cunha, José G. Fernández-Trincado, Peter M. Frinchaboy, D. A. García-Hernández, Emily Griffith, James W. Johnson, Henrik Jönsson, Richard R. Lane, Henry W. Leung, J. Ted Mackereth, Steven R. Majewski, Szabolcs Mészáros, Christian Nitschelm, Kaike Pan, Ricardo P. Schiavon, Donald P. Schneider, Mathias Schultheis, Verne Smith, Jennifer S. Sobeck, Keivan G. Stassun, Guy S. Stringfellow, Fiorenzo Vincenzo, John C. Wilson, Gail Zasowski
Figure caption: Same as Figure 4 but for even-Z iron-peak elements.
Paper: Chemical Cartography with APOGEE: Mapping Disk Populations with a 2-process Model and Residual Abundances
Authors: David H. Weinberg, Jon A. Holtzman, Jennifer A. Johnson, Christian Hayes, Sten Hasselquist, Matthew Shetrone, Yuan-Sen Ting, 源森 丁, Rachael L. Beaton, Timothy C. Beers, Jonathan C. Bird, Dmitry Bizyaev, Michael R. Blanton, Katia Cunha, José G. Fernández-Trincado, Peter M. Frinchaboy, D. A. García-Hernández, Emily Griffith, James W. Johnson, Henrik Jönsson, Richard R. Lane, Henry W. Leung, J. Ted Mackereth, Steven R. Majewski, Szabolcs Mészáros, Christian Nitschelm, Kaike Pan, Ricardo P. Schiavon, Donald P. Schneider, Mathias Schultheis, Verne Smith, Jennifer S. Sobeck, Keivan G. Stassun, Guy S. Stringfellow, Fiorenzo Vincenzo, John C. Wilson, Gail Zasowski
Figure caption: Left: [Mg/Fe] vs. [Mg/H] for sample stars in the low-Ia (red) and high-Ia (blue) populations. Points are randomly downsampled by a factor of 4 to reduce crowding. Connected large points show the median [Mg/Fe] in bins of [Mg/H]. An offset of 0.053 dex has been applied to the APOGEE Fe abundances (decreasing [Mg/Fe] by 0.053) so that the median high-Ia sequence passes through [Mg/Fe] = 0 at [Mg/H] = 0. The dotted horizontal line shows the ratio ﹩{\left[\mathrm{Mg}/\mathrm{Fe}\right]}_{\mathrm{pl}}=0.30﹩ that is assumed to correspond to pure CCSN enrichment in our 2-process modeling. Right: the fraction of iron inferred (via the 2-process model) to arise from CCSN at points along the median low-Ia (red) and high-Ia (blue) sequences (Equation (6)). The dashed curve shows A cc = 10[Mg/H].
Paper: Chemical Cartography with APOGEE: Mapping Disk Populations with a 2-process Model and Residual Abundances
Authors: David H. Weinberg, Jon A. Holtzman, Jennifer A. Johnson, Christian Hayes, Sten Hasselquist, Matthew Shetrone, Yuan-Sen Ting, 源森 丁, Rachael L. Beaton, Timothy C. Beers, Jonathan C. Bird, Dmitry Bizyaev, Michael R. Blanton, Katia Cunha, José G. Fernández-Trincado, Peter M. Frinchaboy, D. A. García-Hernández, Emily Griffith, James W. Johnson, Henrik Jönsson, Richard R. Lane, Henry W. Leung, J. Ted Mackereth, Steven R. Majewski, Szabolcs Mészáros, Christian Nitschelm, Kaike Pan, Ricardo P. Schiavon, Donald P. Schneider, Mathias Schultheis, Verne Smith, Jennifer S. Sobeck, Keivan G. Stassun, Guy S. Stringfellow, Fiorenzo Vincenzo, John C. Wilson, Gail Zasowski
Figure caption: Left: [X/Mg] vs. [Mg/H] for the α elements of sample stars, color-coded as low-Ia (red) or high-Ia (blue). Stars are randomly downsampled by a factor of 4 to reduce crowding. Connected large points show the median values in bins of [Mg/H], which the 2-process model fits exactly by construction. Right: solar-scaled values of the CCSN and SNIa process vector components for each element, ﹩{q}_{\mathrm{cc}}^{X}﹩ (circles) and ﹩{q}_{\mathrm{Ia}}^{X}﹩ (triangles), inferred by fitting the observed median sequences. Red and blue curves show the CCSN fractions ﹩{f}_{\mathrm{cc}}^{X}﹩, which depend on the values of ﹩{q}_{\mathrm{cc}}^{X}﹩ and ﹩{q}_{\mathrm{Ia}}^{X}﹩ and on the amplitude ratio A Ia/A cc at the corresponding point on the median sequence (Equation (7)). Our abundances include zero-point calibrations (Table 1) that force the high-Ia sequence to pass through [X/Mg] = 0 at [Mg/H] = 0. For solar abundances, ﹩{f}_{\mathrm{cc}}^{X}={q}_{\mathrm{cc}}^{X}﹩, so blue curves in the right panels always pass through the open circle at [Mg/H] = 0.
Paper: Chemical Cartography with APOGEE: Mapping Disk Populations with a 2-process Model and Residual Abundances
Authors: David H. Weinberg, Jon A. Holtzman, Jennifer A. Johnson, Christian Hayes, Sten Hasselquist, Matthew Shetrone, Yuan-Sen Ting, 源森 丁, Rachael L. Beaton, Timothy C. Beers, Jonathan C. Bird, Dmitry Bizyaev, Michael R. Blanton, Katia Cunha, José G. Fernández-Trincado, Peter M. Frinchaboy, D. A. García-Hernández, Emily Griffith, James W. Johnson, Henrik Jönsson, Richard R. Lane, Henry W. Leung, J. Ted Mackereth, Steven R. Majewski, Szabolcs Mészáros, Christian Nitschelm, Kaike Pan, Ricardo P. Schiavon, Donald P. Schneider, Mathias Schultheis, Verne Smith, Jennifer S. Sobeck, Keivan G. Stassun, Guy S. Stringfellow, Fiorenzo Vincenzo, John C. Wilson, Gail Zasowski
Figure caption: Illustration of the 2-process model for the 16 elements considered in our analysis (one of which is the element combination C+N). In the top panel, open circles and filled triangles show the 2-process vectors ﹩{q}_{\mathrm{cc}}^{X}﹩ and ﹩{q}_{\mathrm{Ia}}^{X}﹩ at [Mg/H] = 0 inferred from the APOGEE data in Section 4. For a star with A cc = A Ia = 1, the predicted abundances are the sum of these two vectors, which in this case yields exactly solar values (blue points) by construction. Red points show the predicted abundances for a low-Ia star with A cc = 1, A Ia = 0.2. The lower panel shows analogous results at [Mg/H] = −0.5, with predicted abundances multiplied by a factor of 3 in this panel to aid visual comparison with the top panel. In each panel, colored horizontal lines group elements with similar physical properties. The four combinations of (A cc, A Ia) in this Figure are the same cases illustrated in Figure 2.
Paper: Chemical Cartography with APOGEE: Mapping Disk Populations with a 2-process Model and Residual Abundances
Authors: David H. Weinberg, Jon A. Holtzman, Jennifer A. Johnson, Christian Hayes, Sten Hasselquist, Matthew Shetrone, Yuan-Sen Ting, 源森 丁, Rachael L. Beaton, Timothy C. Beers, Jonathan C. Bird, Dmitry Bizyaev, Michael R. Blanton, Katia Cunha, José G. Fernández-Trincado, Peter M. Frinchaboy, D. A. García-Hernández, Emily Griffith, James W. Johnson, Henrik Jönsson, Richard R. Lane, Henry W. Leung, J. Ted Mackereth, Steven R. Majewski, Szabolcs Mészáros, Christian Nitschelm, Kaike Pan, Ricardo P. Schiavon, Donald P. Schneider, Mathias Schultheis, Verne Smith, Jennifer S. Sobeck, Keivan G. Stassun, Guy S. Stringfellow, Fiorenzo Vincenzo, John C. Wilson, Gail Zasowski
Figure caption: Illustration of the 2-process model for the simple case of two abundances, (Mg/H) and (Fe/H); both linear ratios scaled to solar values. The (Mg,Fe) components of the 2-process vectors are  q  cc = (1, 0.5) and  q  Ia = (0, 0.5), respectively. Large points show the abundances of stars with (A cc, A Ia) = (1.0, 1.0) (filled blue circle), (0.33, 0.33) (open blue circle), (1.0, 0.2) (filled red square), (0.33, 0.02) (open red square). The inset marks the position of these four stars in the [Mg/Fe]-[Fe/H] plane, with red and blue curves showing the observed median sequences of low-Ia and high-Ia stars from Figure 1. The dotted blue line marks the locus of [Mg/Fe] = 0.
Paper: NuSTAR Observations of 52 Compton-thick Active Galactic Nuclei Selected by the Swift/Burst Alert Telescope All-sky Hard X-Ray Survey
Authors: Atsushi Tanimoto, Yoshihiro Ueda, Hirokazu Odaka, Satoshi Yamada, Claudio Ricci
Figure caption: (a) Correlation between the logarithmic Eddington ratio (﹩\mathrm{log}{R}_{\mathrm{Edd}}﹩) and the Compton-thick torus covering factor (C 24). (b) Correlation between ﹩\mathrm{log}{R}_{\mathrm{Edd}}﹩ and mean C 24 in the four ﹩\mathrm{log}{R}_{\mathrm{Edd}}﹩ bins. The blue lines represent the radiation-regulated AGN unification model (Ricci et al. 2017b). Note that we apply the standard error as the error of C 24.
Paper: NuSTAR Observations of 52 Compton-thick Active Galactic Nuclei Selected by the Swift/Burst Alert Telescope All-sky Hard X-Ray Survey
Authors: Atsushi Tanimoto, Yoshihiro Ueda, Hirokazu Odaka, Satoshi Yamada, Claudio Ricci
Figure caption: (a) Correlation between the logarithmic Eddington ratio (﹩\mathrm{log}{R}_{\mathrm{Edd}}﹩) and the Compton-thin torus covering factor (C 22). (b) Correlation between ﹩\mathrm{log}{R}_{\mathrm{Edd}}﹩ and mean C 22 in the four ﹩\mathrm{log}{R}_{\mathrm{Edd}}﹩ bins. The blue lines represent the radiation-regulated AGN unification model (Ricci et al. 2017b). Note that we apply the standard error as the error of C 22.
Paper: NuSTAR Observations of 52 Compton-thick Active Galactic Nuclei Selected by the Swift/Burst Alert Telescope All-sky Hard X-Ray Survey
Authors: Atsushi Tanimoto, Yoshihiro Ueda, Hirokazu Odaka, Satoshi Yamada, Claudio Ricci
Figure caption: (a) Correlation between the logarithmic hydrogen column density along the line of sight (﹩\mathrm{log}{N}_{{\rm{H}}}^{\mathrm{LOS}}/{\mathrm{cm}}^{-2}﹩) obtained from the XClumpy model and those inferred from the Borus02 model of previous works. (b) Correlation between the photon index (Γ) obtained from the XClumpy model and those inferred from the Borus02 model of previous works.
Paper: NuSTAR Observations of 52 Compton-thick Active Galactic Nuclei Selected by the Swift/Burst Alert Telescope All-sky Hard X-Ray Survey
Authors: Atsushi Tanimoto, Yoshihiro Ueda, Hirokazu Odaka, Satoshi Yamada, Claudio Ricci
Figure caption: (a) Correlation between the logarithmic hydrogen column density along the line of sight (﹩\mathrm{log}{N}_{{\rm{H}}}^{\mathrm{LOS}}/{\mathrm{cm}}^{-2}﹩) obtained from the XClumpy model and those inferred from the Torus model (Ricci et al. 2015). (b) Correlation between the ﹩\mathrm{log}{N}_{{\rm{H}}}^{\mathrm{LOS}}/{\mathrm{cm}}^{-2}﹩ obtained from the XClumpy model and those inferred from the Borus02 model.
Paper: Best Practices for Data Publication in the Astronomical Literature
Authors: Tracy X. Chen, Marion Schmitz, Joseph M. Mazzarella, Xiuqin Wu, Julian C. van Eyken, Alberto Accomazzi, Rachel L. Akeson, Mark Allen, Rachael Beaton, G. Bruce Berriman, Andrew W. Boyle, Marianne Brouty, Ben H. P. Chan, Jessie L. Christiansen, David R. Ciardi, David Cook, Raffaele D'Abrusco, Rick Ebert, Cren Frayer, Benjamin J. Fulton, Christopher Gelino, George Helou, Calen B. Henderson, Justin Howell, Joyce Kim, Gilles Landais, Tak Lo, Cécile Loup, Barry Madore, Giacomo Monari, August Muench, Anaïs Oberto, Pierre Ocvirk, Joshua E. G. Peek, Emmanuelle Perret, Olga Pevunova, Solange V. Ramirez, Luisa Rebull, Ohad Shemmer, Alan Smale, Raymond Tam, Scott Terek, Doug Van Orsow, Patricia Vannier, Shin-Ywan Wang
Figure caption: Example of a clearly labeled, accessible plot. We revised Figure 28 from Cook et al. (2019) with the help of the original lead author, adding the previously missed units for the axis labels and explanation of what each line is representing in the caption.
Paper: Chemical Cartography with APOGEE: Mapping Disk Populations with a 2-process Model and Residual Abundances
Authors: David H. Weinberg, Jon A. Holtzman, Jennifer A. Johnson, Christian Hayes, Sten Hasselquist, Matthew Shetrone, Yuan-Sen Ting, 源森 丁, Rachael L. Beaton, Timothy C. Beers, Jonathan C. Bird, Dmitry Bizyaev, Michael R. Blanton, Katia Cunha, José G. Fernández-Trincado, Peter M. Frinchaboy, D. A. García-Hernández, Emily Griffith, James W. Johnson, Henrik Jönsson, Richard R. Lane, Henry W. Leung, J. Ted Mackereth, Steven R. Majewski, Szabolcs Mészáros, Christian Nitschelm, Kaike Pan, Ricardo P. Schiavon, Donald P. Schneider, Mathias Schultheis, Verne Smith, Jennifer S. Sobeck, Keivan G. Stassun, Guy S. Stringfellow, Fiorenzo Vincenzo, John C. Wilson, Gail Zasowski
Figure caption: Distributions of stars in the 2%-tails of the D 3 distribution (left column) or D 4 distribution (right column), with the same color-coding as in Figure 24. Black dots show a 25% random sampling of the full distribution. Top panels show the 2-process plane A Ia/A cc vs. A Ia. Middle and bottom rows plot A Ia/A cc vs. AstroNN values of stellar age and orbital eccentricity, respectively. Stars with extreme values of D 3 and D 4 are found throughout these distributions. Low-D 3 stars tend to have younger ages than the full population. The population of high-eccentricity stars with A Ia/A cc > 0.2 tends to have low values of D 3 and D 4; these “accreted halo” stars also have values of [Mg/H] (and thus A cc) near the minimum of our sample.