adsabs/AstroCLIMB huggingface dataset:
Paper: An Atlas of Convection in Main-sequence Stars
Authors: Adam S. Jermyn, Evan H. Anders, Daniel Lecoanet, Matteo Cantiello
Figure caption: The convection optical depth τ CZ (left) and the optical depth to the surface τ outer (right) are shown in terms of ﹩\mathrm{log}{T}_{\mathrm{eff}}﹩/spectral type and ﹩\mathrm{log}L﹩ for stellar models with H I CZs and Milky Way metallicity Z = 0.014. Note that both of these are input parameters and do not depend on a specific theory of convection. Regions with Ra < Racrit are stable to convection and shaded in gray.
Paper: An Atlas of Convection in Main-sequence Stars
Authors: Adam S. Jermyn, Evan H. Anders, Daniel Lecoanet, Matteo Cantiello
Figure caption: The Eddington ratios with the full luminosity ΓEdd (left) and the radiative luminosity (right) are shown in terms of ﹩\mathrm{log}{T}_{\mathrm{eff}}﹩/spectral type and ﹩\mathrm{log}L﹩ for stellar models with H I CZs and Milky Way metallicity Z = 0.014. Note that while ΓEdd is an input parameter and does not depend on a specific theory of convection, ﹩{{\rm{\Gamma }}}_{\mathrm{Edd}}^{\mathrm{rad}}﹩ is an output of such a theory. Regions with Ra < Racrit are stable to convection and shaded in gray.
Paper: An Atlas of Convection in Main-sequence Stars
Authors: Adam S. Jermyn, Evan H. Anders, Daniel Lecoanet, Matteo Cantiello
Figure caption: The density ratio D (left) and Mach number Ma (right) are shown in terms of ﹩\mathrm{log}{T}_{\mathrm{eff}}﹩/spectral type and ﹩\mathrm{log}L﹩ for stellar models with H I CZs and Milky Way metallicity Z = 0.014. Note that while the density ratio is an input parameter and does not depend on a specific theory of convection, the Mach number is an output of such a theory. Regions with Ra < Racrit are stable to convection and shaded in gray.
Paper: An Atlas of Convection in Main-sequence Stars
Authors: Adam S. Jermyn, Evan H. Anders, Daniel Lecoanet, Matteo Cantiello
Figure caption: The Prandtl number Pr (left) and magnetic Prandtl number Pm (right) are shown in terms of ﹩\mathrm{log}{T}_{\mathrm{eff}}﹩/spectral type and ﹩\mathrm{log}L﹩ for stellar models with H I CZs and Milky Way metallicity Z = 0.014. Note that both Pr and Pm are input parameters and so do not depend on a specific theory of convection. Regions with Ra < Racrit are stable to convection and shaded in gray.
Paper: An Atlas of Convection in Main-sequence Stars
Authors: Adam S. Jermyn, Evan H. Anders, Daniel Lecoanet, Matteo Cantiello
Figure caption: The Ekman number Ek is shown in terms of ﹩\mathrm{log}{T}_{\mathrm{eff}}﹩/spectral type and ﹩\mathrm{log}L﹩ for stellar models with H I CZs and Milky Way metallicity Z = 0.014. Note that the Ekman number is an input parameter and does not depend on a specific theory of convection. Regions with Ra < Racrit are stable to convection and shaded in gray.
Paper: An Atlas of Convection in Main-sequence Stars
Authors: Adam S. Jermyn, Evan H. Anders, Daniel Lecoanet, Matteo Cantiello
Figure caption: The radiation pressure ratio β rad is shown in terms of ﹩\mathrm{log}{T}_{\mathrm{eff}}﹩/spectral type and ﹩\mathrm{log}L﹩ for stellar models with H I CZs and Milky Way metallicity Z = 0.014. Note that this ratio is an input parameter and does not depend on a specific theory of convection. Regions with Ra < Racrit are stable to convection and shaded in gray.
Paper: An Atlas of Convection in Main-sequence Stars
Authors: Adam S. Jermyn, Evan H. Anders, Daniel Lecoanet, Matteo Cantiello
Figure caption: The aspect ratio A is shown in terms of ﹩\mathrm{log}{T}_{\mathrm{eff}}﹩/spectral type and ﹩\mathrm{log}L﹩ for stellar models with H I CZs and Milky Way metallicity Z = 0.014. Note that the aspect ratio is an input parameter and does not depend on a specific theory of convection. Regions with Ra < Racrit are stable to convection and shaded in gray.
Paper: An Atlas of Convection in Main-sequence Stars
Authors: Adam S. Jermyn, Evan H. Anders, Daniel Lecoanet, Matteo Cantiello
Figure caption: The Eddington ratios with the full luminosity ΓEdd (left) and the radiative luminosity (right) are shown in terms of ﹩\mathrm{log}{T}_{\mathrm{eff}}﹩/spectral type and ﹩\mathrm{log}L﹩ for stellar models with core CZs and Milky Way metallicity Z = 0.014. Note that while ΓEdd is an input parameter and does not depend on a specific theory of convection, ﹩{{\rm{\Gamma }}}_{\mathrm{Edd}}^{\mathrm{rad}}﹩ is an output of such a theory. Regions with Ra < Racrit are stable to convection and shaded in gray.
Paper: An Atlas of Convection in Main-sequence Stars
Authors: Adam S. Jermyn, Evan H. Anders, Daniel Lecoanet, Matteo Cantiello
Figure caption: The convection optical depth τ CZ (left) and the optical depth to the surface τ outer (right) are shown in terms of ﹩\mathrm{log}{T}_{\mathrm{eff}}﹩/spectral type and ﹩\mathrm{log}L﹩ for stellar models with core CZs and Milky Way metallicity Z = 0.014. Note that both of these are input parameters and do not depend on a specific theory of convection. Regions with Ra < Racrit are stable to convection and shaded in gray.
Paper: An Atlas of Convection in Main-sequence Stars
Authors: Adam S. Jermyn, Evan H. Anders, Daniel Lecoanet, Matteo Cantiello
Figure caption: The density ratio D (left) and Mach number Ma (right) are shown in terms of ﹩\mathrm{log}{T}_{\mathrm{eff}}﹩/spectral type and ﹩\mathrm{log}L﹩ for stellar models with core CZs and Milky Way metallicity Z = 0.014. Note that while the density ratio is an input parameter and does not depend on a specific theory of convection, the Mach number is an output of such a theory. Regions with Ra < Racrit are stable to convection and shaded in gray.
Paper: An Atlas of Convection in Main-sequence Stars
Authors: Adam S. Jermyn, Evan H. Anders, Daniel Lecoanet, Matteo Cantiello
Figure caption: The Rossby number Ro (left) and turnover time t conv (right) are shown in terms of ﹩\mathrm{log}{T}_{\mathrm{eff}}﹩/spectral type and ﹩\mathrm{log}L﹩ for stellar models with core CZs and Milky Way metallicity Z = 0.014. Note that both Ro and t conv are outputs of a theory of convection. Regions with Ra < Racrit are stable to convection and shaded in gray.
Paper: An Atlas of Convection in Main-sequence Stars
Authors: Adam S. Jermyn, Evan H. Anders, Daniel Lecoanet, Matteo Cantiello
Figure caption: The Rayleigh number Ra (left) and Reynolds number Re (right) are shown in terms of ﹩\mathrm{log}{T}_{\mathrm{eff}}﹩/spectral type and ﹩\mathrm{log}L﹩ for stellar models with core CZs and Milky Way metallicity Z = 0.014. Note that while the Rayleigh number is an input parameter and does not depend on a specific theory of convection, the Reynolds number is an output of such a theory. Regions with Ra < Racrit are stable to convection and shaded in gray.
Paper: An Atlas of Convection in Main-sequence Stars
Authors: Adam S. Jermyn, Evan H. Anders, Daniel Lecoanet, Matteo Cantiello
Figure caption: The stiffnesses of the inner (left) and outer (right) convective boundaries are shown in terms of ﹩\mathrm{log}{T}_{\mathrm{eff}}﹩ and ﹩\mathrm{log}L﹩ for stellar models with FeCZs and Milky Way metallicity Z = 0.014. Note that the stiffness is an output of a theory of convection. Regions with Ra < Racrit are stable to convection and shaded in gray.
Paper: An Atlas of Convection in Main-sequence Stars
Authors: Adam S. Jermyn, Evan H. Anders, Daniel Lecoanet, Matteo Cantiello
Figure caption: The Prandtl number Pr (left) and magnetic Prandtl number Pm (right) are shown in terms of ﹩\mathrm{log}{T}_{\mathrm{eff}}﹩/spectral type and ﹩\mathrm{log}L﹩ for stellar models with core CZs and Milky Way metallicity Z = 0.014. Note that both Pr and Pm are input parameters and so do not depend on a specific theory of convection. Regions with Ra < Racrit are stable to convection and shaded in gray.
Paper: An Atlas of Convection in Main-sequence Stars
Authors: Adam S. Jermyn, Evan H. Anders, Daniel Lecoanet, Matteo Cantiello
Figure caption: The radiation pressure ratio β rad is shown in terms of ﹩\mathrm{log}{T}_{\mathrm{eff}}﹩/spectral type and ﹩\mathrm{log}L﹩ for stellar models with core CZs and Milky Way metallicity Z = 0.014. Note that this ratio is an input parameter and does not depend on a specific theory of convection. Regions with Ra < Racrit are stable to convection and shaded in gray.
Paper: An Atlas of Convection in Main-sequence Stars
Authors: Adam S. Jermyn, Evan H. Anders, Daniel Lecoanet, Matteo Cantiello
Figure caption: The Ekman number Ek is shown in terms of ﹩\mathrm{log}{T}_{\mathrm{eff}}﹩/spectral type and ﹩\mathrm{log}L﹩ for stellar models with core CZs and Milky Way metallicity Z = 0.014. Note that the Ekman number is an input parameter and does not depend on a specific theory of convection. Regions with Ra < Racrit are stable to convection and shaded in gray.
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: Evolutionary tracks of the stars on a HR diagram. (a) For single stars with different initial masses and rotational velocities. (b) For primary stars with different overshooting 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 the theoretical B1 and B13 models. The observational regions of two component stars for the SN 1993J progenitor are marked in the HR diagram. Observations for various types of SNe IIb are indicated in different shaded regions (Gilkis & Arcavi 2022). Five Type IIb SNe are marked in the HR diagram and their observations are from Sravan et al. (2020).
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: Carbon mass fraction as a function of the mass coordinate at the moment of core carbon depletion. (a) For primary stars with different overshoot parameters in a binary system with an initial P orb = 300 days. (b) For primary stars with different initial metallicities in a binary system with an initial P orb = 300 days. (c) For primary stars in a binary system with different initial orbital periods. (d) For primary stars with different initial orbital periods and for single stars with different initial masses and rotational velocities.
Paper: The California Legacy Survey. III. On the Shoulders of (Some) Giants: The Relationship between Inner Small Planets and Outer Massive Planets
Authors: Lee J. Rosenthal, Heather A. Knutson, Yayaati Chachan, Fei Dai, Andrew W. Howard, Benjamin J. Fulton, Ashley Chontos, Justin R. Crepp, Paul A. Dalba, Gregory W. Henry, Stephen R. Kane, Erik A. Petigura, Lauren M. Weiss, Jason T. Wright
Figure caption: The results of three Monte Carlo experiments detailed in Section 5.5. We estimate how planet multiplicity biases our estimates of the probability that a star hosts at least one small planet, or P(1+). The black vertical line is the true value of P(1+) for all three experiments. The legend shows the multiplicity distribution and resulting average number of planets per host 〈N  P 〉 for all three experiments. In the one-per-host case, the Poisson model accurately recovers P(1+), while cases with higher 〈N  P 〉 increasingly overestimate the true value.
Paper: The California Legacy Survey. III. On the Shoulders of (Some) Giants: The Relationship between Inner Small Planets and Outer Massive Planets
Authors: Lee J. Rosenthal, Heather A. Knutson, Yayaati Chachan, Fei Dai, Andrew W. Howard, Benjamin J. Fulton, Ashley Chontos, Justin R. Crepp, Paul A. Dalba, Gregory W. Henry, Stephen R. Kane, Erik A. Petigura, Lauren M. Weiss, Jason T. Wright
Figure caption: Left: cumulative metallicity distributions for hosts of lonely small planets and hosts of both inner small and outer giant planets. Solid and dashed steps show distributions of median metallicity measurements, while transparent steps show metallicities drawn many times from Gaussian distributions, with means and standard deviations taken from measurement means and uncertainties. Right: a distribution of P-values from many Kolmogorov–Smirnov tests, performed on 5 × 105 drawn sets of metallicities for the two stellar host groups; 97% of the draws produce P < 0.05, and 73% of the draws produce P < 0.01. This implies that the underlying metallicity distributions of these two groups are distinct.
Paper: The California Legacy Survey. III. On the Shoulders of (Some) Giants: The Relationship between Inner Small Planets and Outer Massive Planets
Authors: Lee J. Rosenthal, Heather A. Knutson, Yayaati Chachan, Fei Dai, Andrew W. Howard, Benjamin J. Fulton, Ashley Chontos, Justin R. Crepp, Paul A. Dalba, Gregory W. Henry, Stephen R. Kane, Erik A. Petigura, Lauren M. Weiss, Jason T. Wright
Figure caption: Mass functions for all planets and outer companions within 0.23–10 au produced by marginalizing the occurrence grids in Figure 6 along their orbital separation axes. Steps and dots show maximum a posteriori values; vertical bars show 15.9%–84.1% confidence intervals.
Paper: The California Legacy Survey. III. On the Shoulders of (Some) Giants: The Relationship between Inner Small Planets and Outer Massive Planets
Authors: Lee J. Rosenthal, Heather A. Knutson, Yayaati Chachan, Fei Dai, Andrew W. Howard, Benjamin J. Fulton, Ashley Chontos, Justin R. Crepp, Paul A. Dalba, Gregory W. Henry, Stephen R. Kane, Erik A. Petigura, Lauren M. Weiss, Jason T. Wright
Figure caption: A comparison between outer giant companions and the rest of the CLS giant sample in semimajor axis and orbital eccentricity space. Circle size is proportional to log(M sin i). Companions to inner small planets are less eccentric than the parent sample, and less massive.
Paper: The California Legacy Survey. III. On the Shoulders of (Some) Giants: The Relationship between Inner Small Planets and Outer Massive Planets
Authors: Lee J. Rosenthal, Heather A. Knutson, Yayaati Chachan, Fei Dai, Andrew W. Howard, Benjamin J. Fulton, Ashley Chontos, Justin R. Crepp, Paul A. Dalba, Gregory W. Henry, Stephen R. Kane, Erik A. Petigura, Lauren M. Weiss, Jason T. Wright
Figure caption: Observed eccentricity distributions for all giant planets and outer giant companions. This plot shows histograms of the maximum a posteriori eccentricities of our sample.
Paper: Osaka Feedback Model. II. Modeling Supernova Feedback Based on High-resolution Simulations
Authors: Yuri Oku, Kengo Tomida, Kentaro Nagamine, Ikkoh Shimizu, Renyue Cen
Figure caption: Evolution of momentum p normalized by p sf,m vs. time normalized by t sf,m. Red and blue points depict the runs with ﹩{\rm{\Delta }}{t}_{\mathrm{SN}}\lt 0.1{t}_{\mathrm{PDS}}﹩ and ﹩{\rm{\Delta }}{t}_{\mathrm{SN}}\gt 0.1{t}_{\mathrm{PDS}}﹩, respectively. Different symbols connected by lines correspond to runs at different SN intervals: ﹩{\rm{\Delta }}{t}_{\mathrm{SN}}=0.01\,\mathrm{Myr}﹩ (circle), ﹩{\rm{\Delta }}{t}_{\mathrm{SN}}=0.1\,\mathrm{Myr}﹩ (triangle), ﹩{\rm{\Delta }}{t}_{\mathrm{SN}}=1\,\mathrm{Myr}﹩ (diamond). The black dotted lines indicate the ﹩(p/{p}_{\mathrm{sf},{\rm{m}}})\propto {\left(t/{t}_{\mathrm{sf},{\rm{m}}}\right)}^{7/5}﹩ and (p/p sf,m) ∝ (t/t sf,m) power law, respectively. The thick gray, yellow, and cyan dotted lines indicate the fitting functions of Equations (28a), (28b), and (28c), respectively.
Paper: Osaka Feedback Model. II. Modeling Supernova Feedback Based on High-resolution Simulations
Authors: Yuri Oku, Kengo Tomida, Kentaro Nagamine, Ikkoh Shimizu, Renyue Cen
Figure caption: Evolution of R hot normalized by R sf,m vs. time normalized by t sf,m. Red and blue points depict the runs with ﹩{\rm{\Delta }}{t}_{\mathrm{SN}}\lt 0.1{t}_{\mathrm{PDS}}﹩ and ﹩{\rm{\Delta }}{t}_{\mathrm{SN}}\gt 0.1{t}_{\mathrm{PDS}}﹩, respectively. Different symbols connected by lines correspond to runs at different SN intervals: ﹩{\rm{\Delta }}{t}_{\mathrm{SN}}=0.01\,\mathrm{Myr}﹩ (circle), ﹩{\rm{\Delta }}{t}_{\mathrm{SN}}=0.1\,\mathrm{Myr}﹩ (triangle), ﹩{\rm{\Delta }}{t}_{\mathrm{SN}}=1\,\mathrm{Myr}﹩ (diamond). The thick black dotted line shows the power law of Equation (25).
Paper: Osaka Feedback Model. II. Modeling Supernova Feedback Based on High-resolution Simulations
Authors: Yuri Oku, Kengo Tomida, Kentaro Nagamine, Ikkoh Shimizu, Renyue Cen
Figure caption: Schematic description of the spherical superbubble feedback model developed in this paper. The left-hand side shows the particle distribution of gas and star particles when the supernova explosions begin, whereas the right-hand side shows the superbubble shell formation, and how we split the shell using Voronoi tessellation based on the gas particle distribution inside the bubble.
Paper: Osaka Feedback Model. II. Modeling Supernova Feedback Based on High-resolution Simulations
Authors: Yuri Oku, Kengo Tomida, Kentaro Nagamine, Ikkoh Shimizu, Renyue Cen
Figure caption: Time evolution of mass (top row), energy (middle row), and momentum (bottom row) of the superbubble for SN injection time intervals of ﹩{\rm{\Delta }}{t}_{\mathrm{SN}}﹩ = 0.01 Myr. For each component, we also show four different metallicities as indicated in the legend. Left column: n H = 0.1 cm−3. Middle column: n H = 1 cm−3. Right column: n H = 10 cm−3. In the top panels for mass, the solid lines are for the hot gas inside the superbubble while dotted lines are for the shell. In the middle panels for energy, the solid lines are for kinetic energy while the dotted lines are for the thermal energy of superbubble gas including the shell. In the left column, the lines for the four metallicities overlap because of low density and long shell-formation time, which prolongs the adiabatic phase with little metal-cooling. In the right column, the effect of intermittent SN injection is visible.
Paper: Osaka Feedback Model. II. Modeling Supernova Feedback Based on High-resolution Simulations
Authors: Yuri Oku, Kengo Tomida, Kentaro Nagamine, Ikkoh Shimizu, Renyue Cen
Figure caption: Same as Figure 5, but for SN injection time interval Δt SN = 0.1 Myr. Note that the time range in the abscissa is different from that in Figure 5.
Paper: Osaka Feedback Model. II. Modeling Supernova Feedback Based on High-resolution Simulations
Authors: Yuri Oku, Kengo Tomida, Kentaro Nagamine, Ikkoh Shimizu, Renyue Cen
Figure caption: Same as Figure 5, but for SN injection time interval Δt SN = 1 Myr. Note that the time range in the abscissa is different from that in Figure 5.
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 a set of stellar properties derived using Pipe3D for the ∼4500 galaxies in MaNGA DR15 and using pyPipe3D for the same galaxies in MaNGA DR17. We show only the galaxies/cubes reported in both analyses with good quality. Each panel shows a density distribution in the DR15 vs. DR17 parameter diagram as a set of filled contours, with each consecutive contour encircling 99%, 95%, and 65% of the points (i.e., 3σ, 2σ, and 1σ), respectively. The dashed line shows the one-to-one relation. The upper left inset shows the density distribution of the difference between the DR15 and DR17 values for the corresponding parameter. The mean value of this difference (Δ) and its standard deviation are shown in the lower right legends of each panel. From left to right, and from top to bottom, we show this comparison for: stellar mass (M ⋆), average mass-to-light ratio (ϒ⋆), SFR derived from the analysis of the stellar population (SFRssp), LW age at the effective radius (﹩{{ \mathcal A }}_{\star ,L}﹩), LW metallicity at the effective radius (﹩{{ \mathcal Z }}_{\star ,L}﹩), average stellar dust extinction (A ⋆,V ), stellar velocity dispersion in the central aperture (σ ⋆,cen), stellar velocity at the effective radius (﹩{v}_{\star ,1\mathrm{Re}}﹩), and apparent angular momentum (﹩{\lambda }_{\star ,1\mathrm{Re}}﹩). For details of the derivations of these quantities, see Section 5.3.
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 a set of ionized gas properties derived using Pipe3D for the ∼4500 galaxies in MaNGA DR15 and using pyPipe3D for the same galaxies in MaNGA DR17. We show only the galaxies/cubes reported in both analyses with good quality, using the same format adopted in Figure 19. From left to right, and from top to bottom, we compare: Hα flux (F Hα,cen), equivalent width of Hα (EWHα,cen), Hα-to-Hβ line ratio, [O III]-to-Hα line ratio, [N II]-to-Hα line ratio, and [S II]-to-Hα line ratio, all of them at the central aperture; and the average dust extinction across the optical extension of the galaxy derived from the Hα-to-Hβ ratio, the integrated SFR derived from the Hα luminosity, and the molecular gas integrated mass derived from the dust-to-gas ratio. For details of the derivations of these quantities, see Section 5.3.
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 set of stellar indices common to both our analysis and the MaNGA-DAP DR for the full DR17 sample. We adopt the same format as in Figure 19. From left to right, we compare the values derived at the effective radius for the Fe5270, Fe5335, and Mgb metallic indices (top panels), and the Hδ, Hβ, and D4000 age-sensitive indices (bottom panels). For Hδ, we adopt our Hd_Re_fit parameter and the HDeltaA parameter in the dapall file. For D4000, we scale our estimate by the factor proposed by Gorgas et al. (1999; Section 6.3), and for the DAP we adopt the average between D4000 and Dn4000. Details of the compared quantities are given in Section 5.3 and in the MaNGA DAP presentation article (Westfall et al. 2019).
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 (σ ⋆; left panel) and Hα (σ Hα ; central panel) velocity dispersions derived using pyPipe3D and the values derived by the MaNGA DAP within 1 Re for the full DR17 sample. The right panel shows the distribution of σ ⋆ as a function of M ⋆, derived from our analysis of the RGs—those with ∣ EW(Hα)∣ < 3 Å at the effective radius. We adopt the same format as in Figure 19. In the right panel, with the dotted–dashed line, we include the FJ relation (Faber & Jackson 1976), as published by Aquino-Ortíz et al. (2018), for comparison purposes.