Data explanations of the stellar population analysis output (based on ppxf software with fsps stellar model; see Section 2.3 for details). The full catalogue of all the stellar population properties and SFH parameters used in this paper can be obtained from the website of MaNGA DynPop (https://manga-dynpop.github.io). The order of galaxies in this catalogue corresponds to their order in the JAM catalogue of Paper I.
| Parameters . | Dimensions . | Units . | Descriptions . |
|---|---|---|---|
| Part 1: General galaxy properties | |||
| plateIFU | (10 296,1) | The plate ID + IFU design ID (e.g. 7443–12 703; unique for each galaxy) | |
| mangaid | (10 296,1) | Unique MaNGA ID (e.g. 1–114 145) | |
| obj_ra | (10 296,1) | degree | Right ascension of the science object in J2000 |
| obj_dec | (10 296,1) | degree | Declination of the science object in J2000 |
| ebvgal | (10 296,1) | E(B − V) value from SDSS dust routine for this IFU | |
| z | (10 296,1) | Redshift of the galaxy | |
| Part 2: Global stellar population properties | |||
| SNR_Re | (10 296,1) | The S/N of the stacked spectrum within the elliptical half-light isophote, which is calculated as the ratio between the median values of flux and noise of the stacked spectra within the wavelength range from |$4730$| to |$4780\ \mathring{\rm A}$| | |
| Mstar_Re | (10 296,1) | |$\lg\ (\mathrm{{\rm M}_{\odot }})$| | Stellar mass enclosed within the elliptical half-light isophote, derived using ppxf with a Salpeter (1955) IMF |
| Lr_int_Re | (10 296,1) | |$\lg\ (\mathrm{L_{\odot }})$| | The intrinsic r-band luminosity within the elliptical half-light isophote, derived from the stacked intrinsic spectrum within the same aperture (see Section 2.3.2 for details) |
| Lr_obs_Re | (10 296,1) | |$\lg\ (\mathrm{L_{\odot }})$| | The observed r-band luminosity within the elliptical half-light isophote, derived from the stacked observed spectrum within the same aperture (see Section 2.3.2 for details) |
| LW_Age_Re | (10 296,1) | |$\lg\ (\mathrm{yr})$| | Global r-band luminosity-weighted age, calculated by performing ppxf fitting on the stacked spectrum within elliptical half-light isophote |
| LW_Metal_Re | (10 296,1) | Global r-band luminosity-weighted [Z/H] | |
| MW_Age_Re | (10 296,1) | |$\lg\ (\mathrm{yr})$| | Global mass-weighted age |
| MW_Metal_Re | (10 296,1) | Global mass-weighted [Z/H] | |
| ML_int_Re | (10 296,1) | |$\lg\ (\mathrm{{\rm M}_{\odot }/L_{\odot }})$| | Averaged intrinsic stellar mass-to-light ratio within the elliptical half-light isophote (calculated as the stellar mass enclosed within the elliptical half-light isophote and the r-band luminosity derived from the intrinsic spectrum within the same aperture; see Section 2.3.2 and Fig. 2 for definition of the intrinsic spectrum) |
| ML_obs_Re | (10 296,1) | |$\lg\ (\mathrm{{\rm M}_{\odot }/L_{\odot }})$| | Averaged observed stellar mass-to-light ratio within the elliptical half-light isophote (calculated as the stellar mass enclosed within the elliptical half-light isophote and the r-band luminosity derived from the observed spectrum within the same aperture) |
| Av_Re | (10 296,1) | Best-fitting dust attenuation at |$\lambda = 5500\ \mathring{\rm A}$| (V band; see Cappellari 2023, section 3.7 for details) | |
| delta_Re | (10 296,1) | Best-fitting UV slope of the spectrum (see Cappellari 2023, section 3.7 for details) | |
| Fred_tot_Re | (10 296,1) | r-band luminosity ratio between the observed spectrum and the intrinsic spectrum | |
| Fred_gal_Re | (10 296,1) | r-band luminosity ratio between the observed spectrum (with the MW dust attenuation corrected) and the intrinsic spectrum | |
| Part 3: Stellar population gradients | |||
| LW_Age_Slope | (10 296,1) | dex/Re | Gradient of r-band luminosity-weighted age within the elliptical half-light isophote (see Section 4 and Fig. 10 for details) |
| LW_Metal_Slope | (10 296,1) | dex/Re | Gradient of r-band luminosity-weighted [Z/H] within the elliptical half-light isophote |
| MW_Age_Slope | (10 296,1) | dex/Re | Gradient of mass-weighted age within the elliptical half-light isophote |
| MW_Metal_Slope | (10 296,1) | dex/Re | Gradient of mass-weighted [Z/H] within the elliptical half-light isophote |
| ML_int_Slope | (10 296,1) | dex/Re | Gradient of intrinsic r-band stellar mass-to-light ratio within the elliptical half-light isophote |
| ML_obs_Slope | (10 296,1) | dex/Re | Gradient of observed r-band stellar mass-to-light ratio within the elliptical half-light isophote |
| Part 4: Stellar population radial profiles | |||
| LW_Age_Profile | (10 296,8) | |$\lg\ (\mathrm{yr})$| | Radial profile of r-band luminosity-weighted age from 0 to 2Re with the radial step being 0.25Re (i.e. eight radial bins for each galaxy; see Section 4 and Fig. 10 for details) |
| LW_Metal_Profile | (10 296,8) | Radial profile of r-band luminosity-weighted [Z/H] | |
| MW_Age_Profile | (10 296,8) | |$\lg\ (\mathrm{yr})$| | Radial profile of mass-weighted age |
| MW_Metal_Profile | (10 296,8) | Radial profile of mass-weighted [Z/H] | |
| ML_int_Profile | (10 296,8) | |$\lg\ (\mathrm{{\rm M}_{\odot }/L_{\odot }})$| | Radial profile of intrinsic r-band stellar mass-to-light ratio |
| ML_obs_Profile | (10 296,8) | |$\lg\ (\mathrm{{\rm M}_{\odot }/L_{\odot }})$| | Radial profile of observed r-band stellar mass-to-light ratio |
| Part 5: Stellar population maps | |||
| BinID_Map | (10 296, Na, N) | IDs of Voronoi bins that the spaxels are associated with. Spaxels that have the same ID belong to the same Voronoi bin (set as −1 if a spaxel does not belong to any bins) and share the same stellar population properties (i.e. luminosity-/mass-weighted age and metallicity, and stellar mass-to-light ratio) | |
| inRe_Map | (10 296, N, N) | 1 for spaxels within the elliptical half-light isophote and 0 for those outside the elliptical half-light isophote | |
| Mstar_Map | (10 296, N, N) | |$\lg\ (\mathrm{{\rm M}_{\odot }})$| | Stellar mass mapsb, derived using ppxf with a Salpeter (1955) IMF |
| Lr_int_Map | (10 296, N, N) | |$\lg\ (\mathrm{L_{\odot }})$| | The intrinsic SDSS r-band luminosity mapsc |
| Lr_obs_Map | (10 296, N, N) | |$\lg\ (\mathrm{L_{\odot }})$| | The observed SDSS r-band luminosity mapsd |
| LW_Age_Map | (10 296, N, N) | |$\lg\ (\mathrm{yr})$| | Spatially resolved r-band luminosity-weighted age mapse |
| LW_Metal_Map | (10 296, N, N) | Spatially resolved r-band luminosity-weighted [Z/H] maps | |
| MW_Age_Map | (10 296, N, N) | |$\lg\ (\mathrm{yr})$| | Spatially resolved stellar mass-weighted age maps |
| MW_Metal_Map | (10 296, N, N) | Spatially resolved stellar mass-weighted [Z/H] maps | |
| ML_int_Map | (10 296, N, N) | |$\lg\ (\mathrm{{\rm M}_{\odot }/L_{\odot }})$| | Spatially resolved intrinsic r-band stellar mass-to-light ratio maps |
| ML_obs_Map | (10 296, N, N) | |$\lg\ (\mathrm{{\rm M}_{\odot }/L_{\odot }})$| | Spatially resolved observed r-band stellar mass-to-light ratio maps |
| Av_Map | (10 296, N, N) | Maps of best-fitting dust attenuation at |$\lambda = 5500\ \mathring{\rm A}$| (V band; see Cappellari 2023, section 3.7 for details) | |
| delta_Map | (10 296, N, N) | Maps of best-fitting UV slope of the spectrum (see Cappellari 2023, section 3.7 for details) | |
| Fred_tot_Map | (10 296, N, N) | Maps of r-band luminosity ratio between the observed spectrum and the intrinsic spectrum | |
| Fred_gal_Map | (10 296, N, N) | Maps of r-band luminosity ratio between the observed spectrum (with the MW dust attenuation corrected) and the intrinsic spectrum | |
| Part 6: Star-formation history | |||
| T50 | (10 296,1) | Gyr | The lookback time when galaxies reach 50 per cent of their present-day stellar mass |
| T90 | (10 296,1) | Gyr | The lookback time when galaxies reach 90 per cent of their present-day stellar mass |
| SFR_History | (10 296,15) | |$\lg\ (\mathrm{{\rm M}_{\odot }\, yr^{-1}})$| | SFR at different lookback time grids (from 0 to |$14\, \rm Gyr$|, with a linear time step being |$1\rm \, Gyr$|; see Section 5 for details) |
| sSFR_History | (10 296,15) | |$\lg\ (\mathrm{Gyr^{-1}})$| | SSFR at different lookback time grids (from 0 to |$14\, \rm Gyr$|, with a linear time step being |$1\rm \, Gyr$|; see Section 5 for details) |
| Mass_Growth_CDF | (10 296,15) | Cumulative distribution function of stellar mass growth | |
| Parameters . | Dimensions . | Units . | Descriptions . |
|---|---|---|---|
| Part 1: General galaxy properties | |||
| plateIFU | (10 296,1) | The plate ID + IFU design ID (e.g. 7443–12 703; unique for each galaxy) | |
| mangaid | (10 296,1) | Unique MaNGA ID (e.g. 1–114 145) | |
| obj_ra | (10 296,1) | degree | Right ascension of the science object in J2000 |
| obj_dec | (10 296,1) | degree | Declination of the science object in J2000 |
| ebvgal | (10 296,1) | E(B − V) value from SDSS dust routine for this IFU | |
| z | (10 296,1) | Redshift of the galaxy | |
| Part 2: Global stellar population properties | |||
| SNR_Re | (10 296,1) | The S/N of the stacked spectrum within the elliptical half-light isophote, which is calculated as the ratio between the median values of flux and noise of the stacked spectra within the wavelength range from |$4730$| to |$4780\ \mathring{\rm A}$| | |
| Mstar_Re | (10 296,1) | |$\lg\ (\mathrm{{\rm M}_{\odot }})$| | Stellar mass enclosed within the elliptical half-light isophote, derived using ppxf with a Salpeter (1955) IMF |
| Lr_int_Re | (10 296,1) | |$\lg\ (\mathrm{L_{\odot }})$| | The intrinsic r-band luminosity within the elliptical half-light isophote, derived from the stacked intrinsic spectrum within the same aperture (see Section 2.3.2 for details) |
| Lr_obs_Re | (10 296,1) | |$\lg\ (\mathrm{L_{\odot }})$| | The observed r-band luminosity within the elliptical half-light isophote, derived from the stacked observed spectrum within the same aperture (see Section 2.3.2 for details) |
| LW_Age_Re | (10 296,1) | |$\lg\ (\mathrm{yr})$| | Global r-band luminosity-weighted age, calculated by performing ppxf fitting on the stacked spectrum within elliptical half-light isophote |
| LW_Metal_Re | (10 296,1) | Global r-band luminosity-weighted [Z/H] | |
| MW_Age_Re | (10 296,1) | |$\lg\ (\mathrm{yr})$| | Global mass-weighted age |
| MW_Metal_Re | (10 296,1) | Global mass-weighted [Z/H] | |
| ML_int_Re | (10 296,1) | |$\lg\ (\mathrm{{\rm M}_{\odot }/L_{\odot }})$| | Averaged intrinsic stellar mass-to-light ratio within the elliptical half-light isophote (calculated as the stellar mass enclosed within the elliptical half-light isophote and the r-band luminosity derived from the intrinsic spectrum within the same aperture; see Section 2.3.2 and Fig. 2 for definition of the intrinsic spectrum) |
| ML_obs_Re | (10 296,1) | |$\lg\ (\mathrm{{\rm M}_{\odot }/L_{\odot }})$| | Averaged observed stellar mass-to-light ratio within the elliptical half-light isophote (calculated as the stellar mass enclosed within the elliptical half-light isophote and the r-band luminosity derived from the observed spectrum within the same aperture) |
| Av_Re | (10 296,1) | Best-fitting dust attenuation at |$\lambda = 5500\ \mathring{\rm A}$| (V band; see Cappellari 2023, section 3.7 for details) | |
| delta_Re | (10 296,1) | Best-fitting UV slope of the spectrum (see Cappellari 2023, section 3.7 for details) | |
| Fred_tot_Re | (10 296,1) | r-band luminosity ratio between the observed spectrum and the intrinsic spectrum | |
| Fred_gal_Re | (10 296,1) | r-band luminosity ratio between the observed spectrum (with the MW dust attenuation corrected) and the intrinsic spectrum | |
| Part 3: Stellar population gradients | |||
| LW_Age_Slope | (10 296,1) | dex/Re | Gradient of r-band luminosity-weighted age within the elliptical half-light isophote (see Section 4 and Fig. 10 for details) |
| LW_Metal_Slope | (10 296,1) | dex/Re | Gradient of r-band luminosity-weighted [Z/H] within the elliptical half-light isophote |
| MW_Age_Slope | (10 296,1) | dex/Re | Gradient of mass-weighted age within the elliptical half-light isophote |
| MW_Metal_Slope | (10 296,1) | dex/Re | Gradient of mass-weighted [Z/H] within the elliptical half-light isophote |
| ML_int_Slope | (10 296,1) | dex/Re | Gradient of intrinsic r-band stellar mass-to-light ratio within the elliptical half-light isophote |
| ML_obs_Slope | (10 296,1) | dex/Re | Gradient of observed r-band stellar mass-to-light ratio within the elliptical half-light isophote |
| Part 4: Stellar population radial profiles | |||
| LW_Age_Profile | (10 296,8) | |$\lg\ (\mathrm{yr})$| | Radial profile of r-band luminosity-weighted age from 0 to 2Re with the radial step being 0.25Re (i.e. eight radial bins for each galaxy; see Section 4 and Fig. 10 for details) |
| LW_Metal_Profile | (10 296,8) | Radial profile of r-band luminosity-weighted [Z/H] | |
| MW_Age_Profile | (10 296,8) | |$\lg\ (\mathrm{yr})$| | Radial profile of mass-weighted age |
| MW_Metal_Profile | (10 296,8) | Radial profile of mass-weighted [Z/H] | |
| ML_int_Profile | (10 296,8) | |$\lg\ (\mathrm{{\rm M}_{\odot }/L_{\odot }})$| | Radial profile of intrinsic r-band stellar mass-to-light ratio |
| ML_obs_Profile | (10 296,8) | |$\lg\ (\mathrm{{\rm M}_{\odot }/L_{\odot }})$| | Radial profile of observed r-band stellar mass-to-light ratio |
| Part 5: Stellar population maps | |||
| BinID_Map | (10 296, Na, N) | IDs of Voronoi bins that the spaxels are associated with. Spaxels that have the same ID belong to the same Voronoi bin (set as −1 if a spaxel does not belong to any bins) and share the same stellar population properties (i.e. luminosity-/mass-weighted age and metallicity, and stellar mass-to-light ratio) | |
| inRe_Map | (10 296, N, N) | 1 for spaxels within the elliptical half-light isophote and 0 for those outside the elliptical half-light isophote | |
| Mstar_Map | (10 296, N, N) | |$\lg\ (\mathrm{{\rm M}_{\odot }})$| | Stellar mass mapsb, derived using ppxf with a Salpeter (1955) IMF |
| Lr_int_Map | (10 296, N, N) | |$\lg\ (\mathrm{L_{\odot }})$| | The intrinsic SDSS r-band luminosity mapsc |
| Lr_obs_Map | (10 296, N, N) | |$\lg\ (\mathrm{L_{\odot }})$| | The observed SDSS r-band luminosity mapsd |
| LW_Age_Map | (10 296, N, N) | |$\lg\ (\mathrm{yr})$| | Spatially resolved r-band luminosity-weighted age mapse |
| LW_Metal_Map | (10 296, N, N) | Spatially resolved r-band luminosity-weighted [Z/H] maps | |
| MW_Age_Map | (10 296, N, N) | |$\lg\ (\mathrm{yr})$| | Spatially resolved stellar mass-weighted age maps |
| MW_Metal_Map | (10 296, N, N) | Spatially resolved stellar mass-weighted [Z/H] maps | |
| ML_int_Map | (10 296, N, N) | |$\lg\ (\mathrm{{\rm M}_{\odot }/L_{\odot }})$| | Spatially resolved intrinsic r-band stellar mass-to-light ratio maps |
| ML_obs_Map | (10 296, N, N) | |$\lg\ (\mathrm{{\rm M}_{\odot }/L_{\odot }})$| | Spatially resolved observed r-band stellar mass-to-light ratio maps |
| Av_Map | (10 296, N, N) | Maps of best-fitting dust attenuation at |$\lambda = 5500\ \mathring{\rm A}$| (V band; see Cappellari 2023, section 3.7 for details) | |
| delta_Map | (10 296, N, N) | Maps of best-fitting UV slope of the spectrum (see Cappellari 2023, section 3.7 for details) | |
| Fred_tot_Map | (10 296, N, N) | Maps of r-band luminosity ratio between the observed spectrum and the intrinsic spectrum | |
| Fred_gal_Map | (10 296, N, N) | Maps of r-band luminosity ratio between the observed spectrum (with the MW dust attenuation corrected) and the intrinsic spectrum | |
| Part 6: Star-formation history | |||
| T50 | (10 296,1) | Gyr | The lookback time when galaxies reach 50 per cent of their present-day stellar mass |
| T90 | (10 296,1) | Gyr | The lookback time when galaxies reach 90 per cent of their present-day stellar mass |
| SFR_History | (10 296,15) | |$\lg\ (\mathrm{{\rm M}_{\odot }\, yr^{-1}})$| | SFR at different lookback time grids (from 0 to |$14\, \rm Gyr$|, with a linear time step being |$1\rm \, Gyr$|; see Section 5 for details) |
| sSFR_History | (10 296,15) | |$\lg\ (\mathrm{Gyr^{-1}})$| | SSFR at different lookback time grids (from 0 to |$14\, \rm Gyr$|, with a linear time step being |$1\rm \, Gyr$|; see Section 5 for details) |
| Mass_Growth_CDF | (10 296,15) | Cumulative distribution function of stellar mass growth | |
Notes.
N is the spaxel number along X- or Y-axis of this map.
For a given Voronoi bin which consists of N spaxels, the stellar mass of each spaxel is the same, given by |$M_{\ast ,\rm spx} = M_{\ast ,\rm bin}/N$|, where |$M_{\ast ,\rm bin}$| is the associated stellar mass of this Voronoi bin.
For a given Voronoi bin which consists of N spaxels, the intrinsic r-band luminosity of each spaxel is the same, given by |$L_{r,\rm spx}^{\rm int} = L_{r,\rm bin}^{\rm int}/N$|, where |$L_{r,\rm bin}^{\rm int}$| is the intrinsic r-band luminosity of this Voronoi bin, derived from the best-fitting intrinsic spectrum of this bin (see Section 2.3.2 for details).
Same as intrinsic luminosity maps, but for observed r-band luminosity.
For a given Voronoi bin, the spaxels in this bin have the same age (and also metallicity, both luminosity- or mass-weighted), fitted from the binned spectrum.
Data explanations of the stellar population analysis output (based on ppxf software with fsps stellar model; see Section 2.3 for details). The full catalogue of all the stellar population properties and SFH parameters used in this paper can be obtained from the website of MaNGA DynPop (https://manga-dynpop.github.io). The order of galaxies in this catalogue corresponds to their order in the JAM catalogue of Paper I.
| Parameters . | Dimensions . | Units . | Descriptions . |
|---|---|---|---|
| Part 1: General galaxy properties | |||
| plateIFU | (10 296,1) | The plate ID + IFU design ID (e.g. 7443–12 703; unique for each galaxy) | |
| mangaid | (10 296,1) | Unique MaNGA ID (e.g. 1–114 145) | |
| obj_ra | (10 296,1) | degree | Right ascension of the science object in J2000 |
| obj_dec | (10 296,1) | degree | Declination of the science object in J2000 |
| ebvgal | (10 296,1) | E(B − V) value from SDSS dust routine for this IFU | |
| z | (10 296,1) | Redshift of the galaxy | |
| Part 2: Global stellar population properties | |||
| SNR_Re | (10 296,1) | The S/N of the stacked spectrum within the elliptical half-light isophote, which is calculated as the ratio between the median values of flux and noise of the stacked spectra within the wavelength range from |$4730$| to |$4780\ \mathring{\rm A}$| | |
| Mstar_Re | (10 296,1) | |$\lg\ (\mathrm{{\rm M}_{\odot }})$| | Stellar mass enclosed within the elliptical half-light isophote, derived using ppxf with a Salpeter (1955) IMF |
| Lr_int_Re | (10 296,1) | |$\lg\ (\mathrm{L_{\odot }})$| | The intrinsic r-band luminosity within the elliptical half-light isophote, derived from the stacked intrinsic spectrum within the same aperture (see Section 2.3.2 for details) |
| Lr_obs_Re | (10 296,1) | |$\lg\ (\mathrm{L_{\odot }})$| | The observed r-band luminosity within the elliptical half-light isophote, derived from the stacked observed spectrum within the same aperture (see Section 2.3.2 for details) |
| LW_Age_Re | (10 296,1) | |$\lg\ (\mathrm{yr})$| | Global r-band luminosity-weighted age, calculated by performing ppxf fitting on the stacked spectrum within elliptical half-light isophote |
| LW_Metal_Re | (10 296,1) | Global r-band luminosity-weighted [Z/H] | |
| MW_Age_Re | (10 296,1) | |$\lg\ (\mathrm{yr})$| | Global mass-weighted age |
| MW_Metal_Re | (10 296,1) | Global mass-weighted [Z/H] | |
| ML_int_Re | (10 296,1) | |$\lg\ (\mathrm{{\rm M}_{\odot }/L_{\odot }})$| | Averaged intrinsic stellar mass-to-light ratio within the elliptical half-light isophote (calculated as the stellar mass enclosed within the elliptical half-light isophote and the r-band luminosity derived from the intrinsic spectrum within the same aperture; see Section 2.3.2 and Fig. 2 for definition of the intrinsic spectrum) |
| ML_obs_Re | (10 296,1) | |$\lg\ (\mathrm{{\rm M}_{\odot }/L_{\odot }})$| | Averaged observed stellar mass-to-light ratio within the elliptical half-light isophote (calculated as the stellar mass enclosed within the elliptical half-light isophote and the r-band luminosity derived from the observed spectrum within the same aperture) |
| Av_Re | (10 296,1) | Best-fitting dust attenuation at |$\lambda = 5500\ \mathring{\rm A}$| (V band; see Cappellari 2023, section 3.7 for details) | |
| delta_Re | (10 296,1) | Best-fitting UV slope of the spectrum (see Cappellari 2023, section 3.7 for details) | |
| Fred_tot_Re | (10 296,1) | r-band luminosity ratio between the observed spectrum and the intrinsic spectrum | |
| Fred_gal_Re | (10 296,1) | r-band luminosity ratio between the observed spectrum (with the MW dust attenuation corrected) and the intrinsic spectrum | |
| Part 3: Stellar population gradients | |||
| LW_Age_Slope | (10 296,1) | dex/Re | Gradient of r-band luminosity-weighted age within the elliptical half-light isophote (see Section 4 and Fig. 10 for details) |
| LW_Metal_Slope | (10 296,1) | dex/Re | Gradient of r-band luminosity-weighted [Z/H] within the elliptical half-light isophote |
| MW_Age_Slope | (10 296,1) | dex/Re | Gradient of mass-weighted age within the elliptical half-light isophote |
| MW_Metal_Slope | (10 296,1) | dex/Re | Gradient of mass-weighted [Z/H] within the elliptical half-light isophote |
| ML_int_Slope | (10 296,1) | dex/Re | Gradient of intrinsic r-band stellar mass-to-light ratio within the elliptical half-light isophote |
| ML_obs_Slope | (10 296,1) | dex/Re | Gradient of observed r-band stellar mass-to-light ratio within the elliptical half-light isophote |
| Part 4: Stellar population radial profiles | |||
| LW_Age_Profile | (10 296,8) | |$\lg\ (\mathrm{yr})$| | Radial profile of r-band luminosity-weighted age from 0 to 2Re with the radial step being 0.25Re (i.e. eight radial bins for each galaxy; see Section 4 and Fig. 10 for details) |
| LW_Metal_Profile | (10 296,8) | Radial profile of r-band luminosity-weighted [Z/H] | |
| MW_Age_Profile | (10 296,8) | |$\lg\ (\mathrm{yr})$| | Radial profile of mass-weighted age |
| MW_Metal_Profile | (10 296,8) | Radial profile of mass-weighted [Z/H] | |
| ML_int_Profile | (10 296,8) | |$\lg\ (\mathrm{{\rm M}_{\odot }/L_{\odot }})$| | Radial profile of intrinsic r-band stellar mass-to-light ratio |
| ML_obs_Profile | (10 296,8) | |$\lg\ (\mathrm{{\rm M}_{\odot }/L_{\odot }})$| | Radial profile of observed r-band stellar mass-to-light ratio |
| Part 5: Stellar population maps | |||
| BinID_Map | (10 296, Na, N) | IDs of Voronoi bins that the spaxels are associated with. Spaxels that have the same ID belong to the same Voronoi bin (set as −1 if a spaxel does not belong to any bins) and share the same stellar population properties (i.e. luminosity-/mass-weighted age and metallicity, and stellar mass-to-light ratio) | |
| inRe_Map | (10 296, N, N) | 1 for spaxels within the elliptical half-light isophote and 0 for those outside the elliptical half-light isophote | |
| Mstar_Map | (10 296, N, N) | |$\lg\ (\mathrm{{\rm M}_{\odot }})$| | Stellar mass mapsb, derived using ppxf with a Salpeter (1955) IMF |
| Lr_int_Map | (10 296, N, N) | |$\lg\ (\mathrm{L_{\odot }})$| | The intrinsic SDSS r-band luminosity mapsc |
| Lr_obs_Map | (10 296, N, N) | |$\lg\ (\mathrm{L_{\odot }})$| | The observed SDSS r-band luminosity mapsd |
| LW_Age_Map | (10 296, N, N) | |$\lg\ (\mathrm{yr})$| | Spatially resolved r-band luminosity-weighted age mapse |
| LW_Metal_Map | (10 296, N, N) | Spatially resolved r-band luminosity-weighted [Z/H] maps | |
| MW_Age_Map | (10 296, N, N) | |$\lg\ (\mathrm{yr})$| | Spatially resolved stellar mass-weighted age maps |
| MW_Metal_Map | (10 296, N, N) | Spatially resolved stellar mass-weighted [Z/H] maps | |
| ML_int_Map | (10 296, N, N) | |$\lg\ (\mathrm{{\rm M}_{\odot }/L_{\odot }})$| | Spatially resolved intrinsic r-band stellar mass-to-light ratio maps |
| ML_obs_Map | (10 296, N, N) | |$\lg\ (\mathrm{{\rm M}_{\odot }/L_{\odot }})$| | Spatially resolved observed r-band stellar mass-to-light ratio maps |
| Av_Map | (10 296, N, N) | Maps of best-fitting dust attenuation at |$\lambda = 5500\ \mathring{\rm A}$| (V band; see Cappellari 2023, section 3.7 for details) | |
| delta_Map | (10 296, N, N) | Maps of best-fitting UV slope of the spectrum (see Cappellari 2023, section 3.7 for details) | |
| Fred_tot_Map | (10 296, N, N) | Maps of r-band luminosity ratio between the observed spectrum and the intrinsic spectrum | |
| Fred_gal_Map | (10 296, N, N) | Maps of r-band luminosity ratio between the observed spectrum (with the MW dust attenuation corrected) and the intrinsic spectrum | |
| Part 6: Star-formation history | |||
| T50 | (10 296,1) | Gyr | The lookback time when galaxies reach 50 per cent of their present-day stellar mass |
| T90 | (10 296,1) | Gyr | The lookback time when galaxies reach 90 per cent of their present-day stellar mass |
| SFR_History | (10 296,15) | |$\lg\ (\mathrm{{\rm M}_{\odot }\, yr^{-1}})$| | SFR at different lookback time grids (from 0 to |$14\, \rm Gyr$|, with a linear time step being |$1\rm \, Gyr$|; see Section 5 for details) |
| sSFR_History | (10 296,15) | |$\lg\ (\mathrm{Gyr^{-1}})$| | SSFR at different lookback time grids (from 0 to |$14\, \rm Gyr$|, with a linear time step being |$1\rm \, Gyr$|; see Section 5 for details) |
| Mass_Growth_CDF | (10 296,15) | Cumulative distribution function of stellar mass growth | |
| Parameters . | Dimensions . | Units . | Descriptions . |
|---|---|---|---|
| Part 1: General galaxy properties | |||
| plateIFU | (10 296,1) | The plate ID + IFU design ID (e.g. 7443–12 703; unique for each galaxy) | |
| mangaid | (10 296,1) | Unique MaNGA ID (e.g. 1–114 145) | |
| obj_ra | (10 296,1) | degree | Right ascension of the science object in J2000 |
| obj_dec | (10 296,1) | degree | Declination of the science object in J2000 |
| ebvgal | (10 296,1) | E(B − V) value from SDSS dust routine for this IFU | |
| z | (10 296,1) | Redshift of the galaxy | |
| Part 2: Global stellar population properties | |||
| SNR_Re | (10 296,1) | The S/N of the stacked spectrum within the elliptical half-light isophote, which is calculated as the ratio between the median values of flux and noise of the stacked spectra within the wavelength range from |$4730$| to |$4780\ \mathring{\rm A}$| | |
| Mstar_Re | (10 296,1) | |$\lg\ (\mathrm{{\rm M}_{\odot }})$| | Stellar mass enclosed within the elliptical half-light isophote, derived using ppxf with a Salpeter (1955) IMF |
| Lr_int_Re | (10 296,1) | |$\lg\ (\mathrm{L_{\odot }})$| | The intrinsic r-band luminosity within the elliptical half-light isophote, derived from the stacked intrinsic spectrum within the same aperture (see Section 2.3.2 for details) |
| Lr_obs_Re | (10 296,1) | |$\lg\ (\mathrm{L_{\odot }})$| | The observed r-band luminosity within the elliptical half-light isophote, derived from the stacked observed spectrum within the same aperture (see Section 2.3.2 for details) |
| LW_Age_Re | (10 296,1) | |$\lg\ (\mathrm{yr})$| | Global r-band luminosity-weighted age, calculated by performing ppxf fitting on the stacked spectrum within elliptical half-light isophote |
| LW_Metal_Re | (10 296,1) | Global r-band luminosity-weighted [Z/H] | |
| MW_Age_Re | (10 296,1) | |$\lg\ (\mathrm{yr})$| | Global mass-weighted age |
| MW_Metal_Re | (10 296,1) | Global mass-weighted [Z/H] | |
| ML_int_Re | (10 296,1) | |$\lg\ (\mathrm{{\rm M}_{\odot }/L_{\odot }})$| | Averaged intrinsic stellar mass-to-light ratio within the elliptical half-light isophote (calculated as the stellar mass enclosed within the elliptical half-light isophote and the r-band luminosity derived from the intrinsic spectrum within the same aperture; see Section 2.3.2 and Fig. 2 for definition of the intrinsic spectrum) |
| ML_obs_Re | (10 296,1) | |$\lg\ (\mathrm{{\rm M}_{\odot }/L_{\odot }})$| | Averaged observed stellar mass-to-light ratio within the elliptical half-light isophote (calculated as the stellar mass enclosed within the elliptical half-light isophote and the r-band luminosity derived from the observed spectrum within the same aperture) |
| Av_Re | (10 296,1) | Best-fitting dust attenuation at |$\lambda = 5500\ \mathring{\rm A}$| (V band; see Cappellari 2023, section 3.7 for details) | |
| delta_Re | (10 296,1) | Best-fitting UV slope of the spectrum (see Cappellari 2023, section 3.7 for details) | |
| Fred_tot_Re | (10 296,1) | r-band luminosity ratio between the observed spectrum and the intrinsic spectrum | |
| Fred_gal_Re | (10 296,1) | r-band luminosity ratio between the observed spectrum (with the MW dust attenuation corrected) and the intrinsic spectrum | |
| Part 3: Stellar population gradients | |||
| LW_Age_Slope | (10 296,1) | dex/Re | Gradient of r-band luminosity-weighted age within the elliptical half-light isophote (see Section 4 and Fig. 10 for details) |
| LW_Metal_Slope | (10 296,1) | dex/Re | Gradient of r-band luminosity-weighted [Z/H] within the elliptical half-light isophote |
| MW_Age_Slope | (10 296,1) | dex/Re | Gradient of mass-weighted age within the elliptical half-light isophote |
| MW_Metal_Slope | (10 296,1) | dex/Re | Gradient of mass-weighted [Z/H] within the elliptical half-light isophote |
| ML_int_Slope | (10 296,1) | dex/Re | Gradient of intrinsic r-band stellar mass-to-light ratio within the elliptical half-light isophote |
| ML_obs_Slope | (10 296,1) | dex/Re | Gradient of observed r-band stellar mass-to-light ratio within the elliptical half-light isophote |
| Part 4: Stellar population radial profiles | |||
| LW_Age_Profile | (10 296,8) | |$\lg\ (\mathrm{yr})$| | Radial profile of r-band luminosity-weighted age from 0 to 2Re with the radial step being 0.25Re (i.e. eight radial bins for each galaxy; see Section 4 and Fig. 10 for details) |
| LW_Metal_Profile | (10 296,8) | Radial profile of r-band luminosity-weighted [Z/H] | |
| MW_Age_Profile | (10 296,8) | |$\lg\ (\mathrm{yr})$| | Radial profile of mass-weighted age |
| MW_Metal_Profile | (10 296,8) | Radial profile of mass-weighted [Z/H] | |
| ML_int_Profile | (10 296,8) | |$\lg\ (\mathrm{{\rm M}_{\odot }/L_{\odot }})$| | Radial profile of intrinsic r-band stellar mass-to-light ratio |
| ML_obs_Profile | (10 296,8) | |$\lg\ (\mathrm{{\rm M}_{\odot }/L_{\odot }})$| | Radial profile of observed r-band stellar mass-to-light ratio |
| Part 5: Stellar population maps | |||
| BinID_Map | (10 296, Na, N) | IDs of Voronoi bins that the spaxels are associated with. Spaxels that have the same ID belong to the same Voronoi bin (set as −1 if a spaxel does not belong to any bins) and share the same stellar population properties (i.e. luminosity-/mass-weighted age and metallicity, and stellar mass-to-light ratio) | |
| inRe_Map | (10 296, N, N) | 1 for spaxels within the elliptical half-light isophote and 0 for those outside the elliptical half-light isophote | |
| Mstar_Map | (10 296, N, N) | |$\lg\ (\mathrm{{\rm M}_{\odot }})$| | Stellar mass mapsb, derived using ppxf with a Salpeter (1955) IMF |
| Lr_int_Map | (10 296, N, N) | |$\lg\ (\mathrm{L_{\odot }})$| | The intrinsic SDSS r-band luminosity mapsc |
| Lr_obs_Map | (10 296, N, N) | |$\lg\ (\mathrm{L_{\odot }})$| | The observed SDSS r-band luminosity mapsd |
| LW_Age_Map | (10 296, N, N) | |$\lg\ (\mathrm{yr})$| | Spatially resolved r-band luminosity-weighted age mapse |
| LW_Metal_Map | (10 296, N, N) | Spatially resolved r-band luminosity-weighted [Z/H] maps | |
| MW_Age_Map | (10 296, N, N) | |$\lg\ (\mathrm{yr})$| | Spatially resolved stellar mass-weighted age maps |
| MW_Metal_Map | (10 296, N, N) | Spatially resolved stellar mass-weighted [Z/H] maps | |
| ML_int_Map | (10 296, N, N) | |$\lg\ (\mathrm{{\rm M}_{\odot }/L_{\odot }})$| | Spatially resolved intrinsic r-band stellar mass-to-light ratio maps |
| ML_obs_Map | (10 296, N, N) | |$\lg\ (\mathrm{{\rm M}_{\odot }/L_{\odot }})$| | Spatially resolved observed r-band stellar mass-to-light ratio maps |
| Av_Map | (10 296, N, N) | Maps of best-fitting dust attenuation at |$\lambda = 5500\ \mathring{\rm A}$| (V band; see Cappellari 2023, section 3.7 for details) | |
| delta_Map | (10 296, N, N) | Maps of best-fitting UV slope of the spectrum (see Cappellari 2023, section 3.7 for details) | |
| Fred_tot_Map | (10 296, N, N) | Maps of r-band luminosity ratio between the observed spectrum and the intrinsic spectrum | |
| Fred_gal_Map | (10 296, N, N) | Maps of r-band luminosity ratio between the observed spectrum (with the MW dust attenuation corrected) and the intrinsic spectrum | |
| Part 6: Star-formation history | |||
| T50 | (10 296,1) | Gyr | The lookback time when galaxies reach 50 per cent of their present-day stellar mass |
| T90 | (10 296,1) | Gyr | The lookback time when galaxies reach 90 per cent of their present-day stellar mass |
| SFR_History | (10 296,15) | |$\lg\ (\mathrm{{\rm M}_{\odot }\, yr^{-1}})$| | SFR at different lookback time grids (from 0 to |$14\, \rm Gyr$|, with a linear time step being |$1\rm \, Gyr$|; see Section 5 for details) |
| sSFR_History | (10 296,15) | |$\lg\ (\mathrm{Gyr^{-1}})$| | SSFR at different lookback time grids (from 0 to |$14\, \rm Gyr$|, with a linear time step being |$1\rm \, Gyr$|; see Section 5 for details) |
| Mass_Growth_CDF | (10 296,15) | Cumulative distribution function of stellar mass growth | |
Notes.
N is the spaxel number along X- or Y-axis of this map.
For a given Voronoi bin which consists of N spaxels, the stellar mass of each spaxel is the same, given by |$M_{\ast ,\rm spx} = M_{\ast ,\rm bin}/N$|, where |$M_{\ast ,\rm bin}$| is the associated stellar mass of this Voronoi bin.
For a given Voronoi bin which consists of N spaxels, the intrinsic r-band luminosity of each spaxel is the same, given by |$L_{r,\rm spx}^{\rm int} = L_{r,\rm bin}^{\rm int}/N$|, where |$L_{r,\rm bin}^{\rm int}$| is the intrinsic r-band luminosity of this Voronoi bin, derived from the best-fitting intrinsic spectrum of this bin (see Section 2.3.2 for details).
Same as intrinsic luminosity maps, but for observed r-band luminosity.
For a given Voronoi bin, the spaxels in this bin have the same age (and also metallicity, both luminosity- or mass-weighted), fitted from the binned spectrum.
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