adsabs/AstroCLIMB huggingface dataset:
Paper: Mass and Age Determination of the LAMOST Data with Different Machine-learning Methods
Authors: Qi-Da Li, Hai-Feng Wang, Yang-Ping Luo, Qing Li, Li-Cai Deng, Yuan-Sen Ting
Figure caption: Comparing our predicted age with other works using LAMOST, APOGEE, and Gaia data. On the top left is the age of APOGEE data using a different method (Ting & Rix 2019), the top-right panel is the age of LAMOST data (Ting et al. 2018), the bottom-left panel is the age of Gaia data (Sanders & Das 2018), and the bottom-right panel is Ho et al. (2017). The median value of relative error is shown on the top left and the consistency is acceptable. We have fewer stars around 2 Gyr in the training data set so there are apparently disconnected features.
Paper: Mass and Age Determination of the LAMOST Data with Different Machine-learning Methods
Authors: Qi-Da Li, Hai-Feng Wang, Yang-Ping Luo, Qing Li, Li-Cai Deng, Yuan-Sen Ting
Figure caption: The comparison between the mass and age we predict and the reference values we use during this work, where the number marked on the figure represents the median value of relative error for our method. It consists of the common stars of LAMOST data we predict and APOKASC-2 in this work. The purpose here is method validation and since we use APOKASC-2 to predict our sample, the precision is naturally quite good for the data set since we use the APOKASC-2 data for training.
Paper: Mass and Age Determination of the LAMOST Data with Different Machine-learning Methods
Authors: Qi-Da Li, Hai-Feng Wang, Yang-Ping Luo, Qing Li, Li-Cai Deng, Yuan-Sen Ting
Figure caption: The figure shows the mass comparisons between this work, Yu et al. (2018), and Ho et al. (2017). The median value of relative error is shown on the top left of each panel and the consistency is acceptable.
Paper: Mass and Age Determination of the LAMOST Data with Different Machine-learning Methods
Authors: Qi-Da Li, Hai-Feng Wang, Yang-Ping Luo, Qing Li, Li-Cai Deng, Yuan-Sen Ting
Figure caption: Open-cluster comparisons for our determinations and literature values based on Bragaglia et al. (2006), Geller et al. (2008), Grundahl et al. (2008), Jacobson et al. (2011), Janes et al. (2013), Brewer et al. (2016), Stello et al. (2016), and references therein. The comparison is quite good except for the older last cluster, and the error bars are calculated by the Gaussian dispersion or literature values.
Paper: Mass and Age Determination of the LAMOST Data with Different Machine-learning Methods
Authors: Qi-Da Li, Hai-Feng Wang, Yang-Ping Luo, Qing Li, Li-Cai Deng, Yuan-Sen Ting
Figure caption: The predicted results for some chemical parameters using the first six stellar parameters shown in feature importance in Figure 2. The consistency is quite good and from top left to bottom left these are: [Ba/Fe], [Mg/Fe], [Na/Fe], log g, [Ni/Fe], [Co/Fe], [α/Fe], ΔP, [Ca/Fe], [Si/Fe], [O/Fe], [Cr/Fe], and [Fe/H].
Paper: Mass and Age Determination of the LAMOST Data with Different Machine-learning Methods
Authors: Qi-Da Li, Hai-Feng Wang, Yang-Ping Luo, Qing Li, Li-Cai Deng, Yuan-Sen Ting
Figure caption: The distribution of our predicted ages over every two stellar parameters. From top left to bottom left these are: Δν vs. [Ti/Fe], [C/Fe] vs. [N/Fe], [Mn/Fe] vs. T eff, [Ba/Fe] vs. [Mg/Fe], [Na/Fe] vs. log g, [Ni/Fe] vs. [Co/Fe], [α/Fe] vs. ΔP, [Ca/Fe] vs. [Si/Fe], [O/Fe] vs. [Cr/Fe], and [Fe/H] vs. [α/Fe].
Paper: Mass and Age Determination of the LAMOST Data with Different Machine-learning Methods
Authors: Qi-Da Li, Hai-Feng Wang, Yang-Ping Luo, Qing Li, Li-Cai Deng, Yuan-Sen Ting
Figure caption: The distribution of relative errors of LS-mass and RC-age for our test data set we predict along with T eff (kelvin), log g (dex), and [Fe/H] (dex).
Paper: Mass and Age Determination of the LAMOST Data with Different Machine-learning Methods
Authors: Qi-Da Li, Hai-Feng Wang, Yang-Ping Luo, Qing Li, Li-Cai Deng, Yuan-Sen Ting
Figure caption: The relative error of RC-age vs. S/N in this work; the error bars represent the standard deviation in each bin.
Paper: Mass and Age Determination of the LAMOST Data with Different Machine-learning Methods
Authors: Qi-Da Li, Hai-Feng Wang, Yang-Ping Luo, Qing Li, Li-Cai Deng, Yuan-Sen Ting
Figure caption: The relationship between the predicted age and [C/N]. The black line is the median value in each bin with Poisson error.
Paper: The Formation of the Stripped-envelope Type IIb Supernova Progenitors: Rotation, Metallicity, and Overshooting
Authors: Gang Long, Hanfeng Song, Georges Meynet, Andre Maeder, Ruiyu Zhang, Ying Qin, Sylvia Ekströmt, Cyril Georgy, Liuyan Zhao
Figure caption: The evolution of photospheric radii as a function of evolutionary age. (a) For single stars with different initial masses and rotational velocities. (b) For primary stars with different overshoot parameters in a binary system with an initial P orb = 300 days. (c) For primary stars with different initial metallicities in a binary system with an initial P orb = 300 days. (d) For primary stars in a binary system with different initial orbital periods. (e) For primary stars in a binary system with an initial P orb = 300 days but with different initial rotational velocities. (f) The evolution of photospheric radii as a function of stellar mass in binary systems B6, with an initial P orb = 300 days, and B9, with an initial P orb = 1600 days. The dotted lines correspond to the evolution of the corresponding Roche lobe.
Paper: The Formation of the Stripped-envelope Type IIb Supernova Progenitors: Rotation, Metallicity, and Overshooting
Authors: Gang Long, Hanfeng Song, Georges Meynet, Andre Maeder, Ruiyu Zhang, Ying Qin, Sylvia Ekströmt, Cyril Georgy, Liuyan Zhao
Figure caption: The mass of the helium core as a function of evolutionary age. (a) For single stars with different initial masses and rotational velocities. (b) For primary stars with different overshoot parameters in a binary system with an initial P orb = 300 days. (c) For primary stars with different initial metallicities and rotational velocities in a binary system with an initial P orb = 300 days. (d) For primary stars in a binary system with different initial orbital periods. Observations for helium core masses of SNe IIb, which are indicated in shaded regions, are 2–6.0 M ⊙.
Paper: The Formation of the Stripped-envelope Type IIb Supernova Progenitors: Rotation, Metallicity, and Overshooting
Authors: Gang Long, Hanfeng Song, Georges Meynet, Andre Maeder, Ruiyu Zhang, Ying Qin, Sylvia Ekströmt, Cyril Georgy, Liuyan Zhao
Figure caption: (a) Surface mass fraction ratio of nitrogen to carbon as a function of the evolutionary age for single stars with different initial mass and rotational velocities. (b) This ratio as a function of the actual mass for primary stars with different overshoot parameters in a binary system with an initial P orb = 300 days. (c) This ratio as a function of the actual mass for primary stars with different initial metallicities and rotational velocities in a binary system with an initial P orb = 300 days. (d) This ratio as a function of the orbital period for primary stars in a binary system with different initial orbital periods.
Paper: The Formation of the Stripped-envelope Type IIb Supernova Progenitors: Rotation, Metallicity, and Overshooting
Authors: Gang Long, Hanfeng Song, Georges Meynet, Andre Maeder, Ruiyu Zhang, Ying Qin, Sylvia Ekströmt, Cyril Georgy, Liuyan Zhao
Figure caption: The rate of mass transfer via RLOF as a function of evolutionary age. (a) For primary stars with various overshoot parameters in a binary system with an initial P orb = 300 days. (b) For primary stars with various initial metallicities in a binary system with an initial P orb = 300 days. (c) For primary stars in a binary system with various initial orbital periods. (d) For primary stars with various initial rotational velocities in a binary system with an initial P orb = 300 days.
Paper: The Formation of the Stripped-envelope Type IIb Supernova Progenitors: Rotation, Metallicity, and Overshooting
Authors: Gang Long, Hanfeng Song, Georges Meynet, Andre Maeder, Ruiyu Zhang, Ying Qin, Sylvia Ekströmt, Cyril Georgy, Liuyan Zhao
Figure caption: Convective cores as a function of evolutionary age. (a) For single stars with various initial masses and rotational velocities. (b) For primary stars with various overshoot parameters in a binary system with an initial P orb = 300 days. (c) For primary stars with various initial rotational velocities and metallicities in a binary system with an initial P orb = 300 days. (d) For primary stars in a binary system with various initial orbital periods.
Paper: The Formation of the Stripped-envelope Type IIb Supernova Progenitors: Rotation, Metallicity, and Overshooting
Authors: Gang Long, Hanfeng Song, Georges Meynet, Andre Maeder, Ruiyu Zhang, Ying Qin, Sylvia Ekströmt, Cyril Georgy, Liuyan Zhao
Figure caption: The mass of the hydrogen envelope as a function of evolutionary age. (a) For single stars with various initial masses and rotational velocities. (b) For primary stars with various overshoot parameters in the binary system with initial P orb = 300 days. (c) For primary stars with various initial rotational velocities and metallicities in the binary system with initial P orb = 300 days. (d) For primary stars in the binary system with various initial orbital periods. Observations for the hydrogen envelope masses of SNe IIb, indicated in shaded regions, are M H = 0.033–0.5 M ⊙.
Paper: SDSS-IV MaNGA: pyPipe3D Analysis Release for 10,000 Galaxies
Authors: S. F. Sánchez, J. K. Barrera-Ballesteros, E. Lacerda, A. Mejía-Narvaez, A. Camps-Fariña, Gustavo Bruzual, C. Espinosa-Ponce, A. Rodríguez-Puebla, A. R. Calette, H. Ibarra-Medel, V. Avila-Reese, H. Hernandez-Toledo, M. A. Bershady, M. Cano-Diaz, A. M. Munguia-Cordova
Figure caption: Distributions of [O III]/Hβ vs. [N II]/Hα (left panel), [S II]/Hα (central panel), and [O I]/Hα (right panel), corresponding to the central aperture measurements for all the galaxies, color coded by the average EW(Hα) in logarithmic scale in the same aperture (with its histogram, also in logarithmic scale, shown as an inset in the left panel, including the mean value: ∼5 Å). The contours correspond to the density of the points, with the first one encircling 80% of the data, and each consecutive one then encircling 20% fewer points. The stars correspond to the AGNs selected, as described in the text, color coded by EW(Hα) in the case of type-II candidates and by the use of a yellow color in the case of type-I candidates. In each panel, the dashed–dotted lines correspond to the K01 demarcation line, and the dotted line in the left panel corresponds to the Kauffmann et al. (2003a) demarcation line. Those lines are frequently used to separate between SF-like and AGN-like ionization. The diagonal line in the top right quadrant corresponds to the separation between Seyferts and LINERs proposed by Kewley et al. (2001), too.
Paper: SDSS-IV MaNGA: pyPipe3D Analysis Release for 10,000 Galaxies
Authors: S. F. Sánchez, J. K. Barrera-Ballesteros, E. Lacerda, A. Mejía-Narvaez, A. Camps-Fariña, Gustavo Bruzual, C. Espinosa-Ponce, A. Rodríguez-Puebla, A. R. Calette, H. Ibarra-Medel, V. Avila-Reese, H. Hernandez-Toledo, M. A. Bershady, M. Cano-Diaz, A. M. Munguia-Cordova
Figure caption: An example of the information explored in the quality control process for the galaxy/cube manga-7495-12703, extracted from the analysis presented by López-Cobá et al. (2020). Panels (a) and (b) correspond to the same color images, created using broadband and emission-line images, as shown in Figure 3. Panel (c) comprises the spatially resolved WHAN diagnostic diagram, with each spaxel being color coded using the scheme included in panel (b). Classical BPT diagnostic diagrams, showing the spatially resolved distribution of [O III]/Hβ as a function of [N II]/Hα, [S II]/Hα, and [O I]/Hα are shown in panel (d), using a similar color scheme as panel (c). Panels (e) and (f) show the spatial distributions of the [N II]/Hα line ratio, in logarithmic scales, and the Hα velocity dispersion, with panel (g) showing the distribution of those parameters one against the other (color coded using the same scheme as panels (c) and (d)). Panels (h), (i), and (j) show the ionized gas velocity map (derived from Hα), the stellar velocity map, and the residual from subtracting the latter from the former, respectively.
Paper: SDSS-IV MaNGA: pyPipe3D Analysis Release for 10,000 Galaxies
Authors: S. F. Sánchez, J. K. Barrera-Ballesteros, E. Lacerda, A. Mejía-Narvaez, A. Camps-Fariña, Gustavo Bruzual, C. Espinosa-Ponce, A. Rodríguez-Puebla, A. R. Calette, H. Ibarra-Medel, V. Avila-Reese, H. Hernandez-Toledo, M. A. Bershady, M. Cano-Diaz, A. M. Munguia-Cordova
Figure caption: Distribution of galaxies along the SFR–M ⋆ diagram, color coded by the average EW(Hα) at the effective radius. For the SFR, we adopted the derived value based on the dust-corrected Hα luminosity, and for the stellar mass we adopted the value derived from the stellar analysis performed by pyPipe3D. The contours correspond to the density of the points, with the first one encircling 80% of the data, and each consecutive one encircling 20% fewer points. The stars corresponds to the AGNs selected as described in the text, color coded by the EW(Hα) at the effective radius in the case of type-II candidates and by the use of a yellow color in the case of type-I candidates.
Paper: SDSS-IV MaNGA: pyPipe3D Analysis Release for 10,000 Galaxies
Authors: S. F. Sánchez, J. K. Barrera-Ballesteros, E. Lacerda, A. Mejía-Narvaez, A. Camps-Fariña, Gustavo Bruzual, C. Espinosa-Ponce, A. Rodríguez-Puebla, A. R. Calette, H. Ibarra-Medel, V. Avila-Reese, H. Hernandez-Toledo, M. A. Bershady, M. Cano-Diaz, A. M. Munguia-Cordova
Figure caption: Violin plot of the ﹩{{ \mathcal Z }}_{\star ,L}﹩ (top panel), ﹩{{ \mathcal A }}_{\star ,L}﹩ (middle panel), and stellar masses (bottom panel), segregated by morphology (with cD galaxies excluded; see Section 6.1), for the complete sample (light gray) and the AGN hosts (dark gray). Histograms of the number of galaxies segregated by morphology and mass for both subsamples have been included in the top and right panels, respectively. In both cases, a logarithmic scale was adopted for the histograms, to highlight the bins with low numbers.
Paper: SDSS-IV MaNGA: pyPipe3D Analysis Release for 10,000 Galaxies
Authors: S. F. Sánchez, J. K. Barrera-Ballesteros, E. Lacerda, A. Mejía-Narvaez, A. Camps-Fariña, Gustavo Bruzual, C. Espinosa-Ponce, A. Rodríguez-Puebla, A. R. Calette, H. Ibarra-Medel, V. Avila-Reese, H. Hernandez-Toledo, M. A. Bershady, M. Cano-Diaz, A. M. Munguia-Cordova
Figure caption: Comparison between the oxygen abundances, 12+log(O/H), derived at the effective radius using different calibrators (one for each panel) and listed in the final catalog as a function of the values derived using the Ho (2019) one (adopted as the fiducial one in an arbitrary way). We adopt the same format as described in Figure 19 for the different panels of the figure.
Paper: SDSS-IV MaNGA: pyPipe3D Analysis Release for 10,000 Galaxies
Authors: S. F. Sánchez, J. K. Barrera-Ballesteros, E. Lacerda, A. Mejía-Narvaez, A. Camps-Fariña, Gustavo Bruzual, C. Espinosa-Ponce, A. Rodríguez-Puebla, A. R. Calette, H. Ibarra-Medel, V. Avila-Reese, H. Hernandez-Toledo, M. A. Bershady, M. Cano-Diaz, A. M. Munguia-Cordova
Figure caption: Spatially resolved distribution of the subsample of 5624 well-resolved galaxies in the [OIII/Hβ] vs. [N II]/Hα diagnostic diagram, segregated by mass (rows) and morphology (columns), and color coded by the average EW(Hα) at each location (color distribution). The contours indicate the density of the spaxels, with each consecutive contour encircling 90%, 50%, and 10% of the points. The solid gray circles correspond to the average locations in the diagram of spaxels at different galactocentric distances, with the sizes of the circles being proportional to their distance (ranging from 0.1 to 2.1 Re, in steps of 0.2 Re). In each panel, the solid and short-dashed lines correspond to the Kewley et al. (2001) and Kauffmann et al. (2003a) demarcation lines, which are frequently used to separate between SF- and AGN-like ionization. The long-dashed line corresponds to the separation between Seyferts and LINERs proposed by Kewley et al. (2001).
Paper: SDSS-IV MaNGA: pyPipe3D Analysis Release for 10,000 Galaxies
Authors: S. F. Sánchez, J. K. Barrera-Ballesteros, E. Lacerda, A. Mejía-Narvaez, A. Camps-Fariña, Gustavo Bruzual, C. Espinosa-Ponce, A. Rodríguez-Puebla, A. R. Calette, H. Ibarra-Medel, V. Avila-Reese, H. Hernandez-Toledo, M. A. Bershady, M. Cano-Diaz, A. M. Munguia-Cordova
Figure caption: Σ⋆ as derived from the weights included in the SFH extension, using the mass-to-light ratio of each SSP and the flux intensity in each tessella (spatial bin) for the different age ranges, indicated in the bottom left insets, corresponding to the channels in the bottom right legends. The first panel shows the actual Σ⋆, corresponding to integration along all lookback times. The subsequent panels show the cumulative Σ⋆,t  at the lookback time t, corresponding to the lower age of the considered range, without considering the redshift of the target. The age (﹩{{ \mathcal A }}_{\star }﹩) of the stellar population and the lookback time of the universe in which it was formed (τ lbt,⋆) are related via the lookback time corresponding to the redshift at which the stellar population was observed (τ lbt,z ): τ lbt,⋆ = τ lbt,z +﹩{{ \mathcal A }}_{\star }﹩. For simplicity, in this plot, we consider τ lbt,z  ∼ 0.
Paper: SDSS-IV MaNGA: pyPipe3D Analysis Release for 10,000 Galaxies
Authors: S. F. Sánchez, J. K. Barrera-Ballesteros, E. Lacerda, A. Mejía-Narvaez, A. Camps-Fariña, Gustavo Bruzual, C. Espinosa-Ponce, A. Rodríguez-Puebla, A. R. Calette, H. Ibarra-Medel, V. Avila-Reese, H. Hernandez-Toledo, M. A. Bershady, M. Cano-Diaz, A. M. Munguia-Cordova
Figure caption: Example of the content of the ELINES extension in the Pipe3D file, corresponding to the MaNGA data cube (galaxy) manga-7495-12704. Each panel shows a color image of the content of a channel from this data cube. The first panel corresponds to the velocity, in km s−1, and the second panel corresponds to EW(Hα), in angstroms. The remaining panels represent the distributions of the flux intensities for the different analyzed emission lines (lower left legend), in units of 10−16 erg s−1 Å− cm−2.
Paper: SDSS-IV MaNGA: pyPipe3D Analysis Release for 10,000 Galaxies
Authors: S. F. Sánchez, J. K. Barrera-Ballesteros, E. Lacerda, A. Mejía-Narvaez, A. Camps-Fariña, Gustavo Bruzual, C. Espinosa-Ponce, A. Rodríguez-Puebla, A. R. Calette, H. Ibarra-Medel, V. Avila-Reese, H. Hernandez-Toledo, M. A. Bershady, M. Cano-Diaz, A. M. Munguia-Cordova
Figure caption: Example of the content of the INDICES extension in the Pipe3D file, corresponding to the MaNGA data cube (galaxy) manga-7495-12704. Each panel shows a color image of the content of the channel in the data cube. The actual content is indicated in the lower left of each panel, the channel in the lower right, and the units of the represented quantity are given in the upper right legend. For the flux and flux error, the units are 10−16 erg s−1 Å− cm−2.
Paper: SDSS-IV MaNGA: pyPipe3D Analysis Release for 10,000 Galaxies
Authors: S. F. Sánchez, J. K. Barrera-Ballesteros, E. Lacerda, A. Mejía-Narvaez, A. Camps-Fariña, Gustavo Bruzual, C. Espinosa-Ponce, A. Rodríguez-Puebla, A. R. Calette, H. Ibarra-Medel, V. Avila-Reese, H. Hernandez-Toledo, M. A. Bershady, M. Cano-Diaz, A. M. Munguia-Cordova
Figure caption: Comparison between the stellar masses derived from the stellar population decomposition performed as part of the pyPipe3D analysis (M ⋆) and the stellar masses derived by ourselves using only photometric information (M ⋆,phot; left panel) and the stellar masses included in the NSA catalog (M ⋆,NSA; right panel), both of which are included in our catalog. Offsets of 0.28 dex and 0.15 dex have been applied to M ⋆,phot and M ⋆,NSA, to correct for the different IMF adopted (Chabrier 2003, in both cases) and the different cosmology for the NSA values. We adopt the same format of Figure 19.
Paper: SDSS-IV MaNGA: pyPipe3D Analysis Release for 10,000 Galaxies
Authors: S. F. Sánchez, J. K. Barrera-Ballesteros, E. Lacerda, A. Mejía-Narvaez, A. Camps-Fariña, Gustavo Bruzual, C. Espinosa-Ponce, A. Rodríguez-Puebla, A. R. Calette, H. Ibarra-Medel, V. Avila-Reese, H. Hernandez-Toledo, M. A. Bershady, M. Cano-Diaz, A. M. Munguia-Cordova
Figure caption: Comparison between the oxygen abundances, 12+log(O/H), derived at the effective radius using four different calibrators (one for each panel) and listed in the final catalog as a function of the values derived using the Ho (2019) one (adopted as the fiducial one in an arbitrary way). We adopt the same format as described in Figure 19 for the different panels of the figure.
Paper: SDSS-IV MaNGA: pyPipe3D Analysis Release for 10,000 Galaxies
Authors: S. F. Sánchez, J. K. Barrera-Ballesteros, E. Lacerda, A. Mejía-Narvaez, A. Camps-Fariña, Gustavo Bruzual, C. Espinosa-Ponce, A. Rodríguez-Puebla, A. R. Calette, H. Ibarra-Medel, V. Avila-Reese, H. Hernandez-Toledo, M. A. Bershady, M. Cano-Diaz, A. M. Munguia-Cordova
Figure caption: Top left panel: distribution of the Hδ vs. D4000 spectral index, measured at the effective radius for the full sample of galaxies (with contours encircling 95%, 65%, and 40% of the objects, successively). The locations of the different morphological types (E, S0, Sa/b, and Sc/d) are color coded in the shaded areas. Histograms of the parameters segregated by morphological type are presented at the top and right of each panel. Top right panel: distribution of ﹩{{ \mathcal A }}_{\star ,L}﹩ vs. D4000. Bottom left panel: distribution of ﹩{{ \mathcal A }}_{\star ,L}﹩ vs. Hδ. Bottom right panel: distribution of ﹩{{ \mathcal Z }}_{\star ,L}﹩ vs. Mgb.
Paper: SDSS-IV MaNGA: pyPipe3D Analysis Release for 10,000 Galaxies
Authors: S. F. Sánchez, J. K. Barrera-Ballesteros, E. Lacerda, A. Mejía-Narvaez, A. Camps-Fariña, Gustavo Bruzual, C. Espinosa-Ponce, A. Rodríguez-Puebla, A. R. Calette, H. Ibarra-Medel, V. Avila-Reese, H. Hernandez-Toledo, M. A. Bershady, M. Cano-Diaz, A. M. Munguia-Cordova
Figure caption: Example of the content of the FLUX_ELINES extension in the Pipe3D file, corresponding to the MaNGA data cube (galaxy) manga-7495-12704. Each panel shows a color image of the content of a channel from this data cube. For each panel, the actual content is indicated in the lower left, the channel number in the lower right, and the units of the represented quantity in the upper right legend. For the flux and flux error, the units are 10−16 erg s−1 Å−1 cm−2.
Paper: SDSS-IV MaNGA: pyPipe3D Analysis Release for 10,000 Galaxies
Authors: S. F. Sánchez, J. K. Barrera-Ballesteros, E. Lacerda, A. Mejía-Narvaez, A. Camps-Fariña, Gustavo Bruzual, C. Espinosa-Ponce, A. Rodríguez-Puebla, A. R. Calette, H. Ibarra-Medel, V. Avila-Reese, H. Hernandez-Toledo, M. A. Bershady, M. Cano-Diaz, A. M. Munguia-Cordova
Figure caption: Comparison between the three values for N/O relative abundance measured at the effective radius included in the final catalog. We adopt the same format as described in Figure 19. Details of the compared quantities are given in Section 5.3.