From e28517c671029ff1f409dd45e9d31c76dc538827 Mon Sep 17 00:00:00 2001 From: Camila Correa <35491033+correac@users.noreply.github.com> Date: Tue, 16 Jan 2024 13:32:32 +0100 Subject: [PATCH] Adding arrow in stellar abundance plots (#272) * Adding arrow in stellar abundance plots to show lower median values not shown in figure * Formatting.. * Updating captions --- colibre/config.yml | 40 +++++++------- colibre/scripts/stellar_abundances.py | 76 ++++++++++++++------------- 2 files changed, 59 insertions(+), 57 deletions(-) diff --git a/colibre/config.yml b/colibre/config.yml index 96023221..dd6e6d21 100644 --- a/colibre/config.yml +++ b/colibre/config.yml @@ -344,7 +344,7 @@ scripts: section: Feedback kick velocities title: Maximal SNII kick velocity - filename: scripts/stellar_abundances.py - caption: '[Fe/H] vs [C/Fe] using Asplund et al. (2009) values for [Fe/H]Sun = 7.5 and [C/H]Sun = 8.43. The median [C/Fe] vs median [Fe/H] is indicated by the solid curve(s). The scatter points show abundances of individual stellar particles. The observational data for MW compiles the data from the GALAH survey (Buder et al. 2021). Contours use a log scale with 0.04 bin size and a minimum star count of 10. All recommended flags are applied to GALAH data to select stars (SN, FE/H and X/Fe quality flags).' + caption: '[Fe/H] vs [C/Fe] using Asplund et al. (2009) values for [Fe/H]Sun = 7.5 and [C/H]Sun = 8.43. The median [C/Fe] vs median [Fe/H] is indicated by the solid curve(s). The scatter points show abundances of individual stellar particles. The observational data for MW compiles the data from the GALAH survey (Buder et al. 2021). Contours use a log scale with 0.04 bin size and a minimum star count of 10. All recommended flags are applied to GALAH data to select stars (SN, FE/H and X/Fe quality flags). The arrows at [Fe/H]=-4 indicate the median value of [C/Fe] of gas with [Fe/H]<-4.' output_file: stellar_abundances_FeH_CFe_GALAH.png section: Stellar Metal Abundances title: '[Fe/H] vs [C/Fe]' @@ -353,7 +353,7 @@ scripts: yvar: C_Fe dataset: GALAH - filename: scripts/stellar_abundances.py - caption: '[Fe/H] vs [C/Fe] using Asplund et al. (2009) values for [Fe/H]Sun = 7.5 and [C/H]Sun = 8.43. The median [C/Fe] vs median [Fe/H] is indicated by the solid curve(s). The scatter points show abundances of individual stellar particles. The observational data for MW compiles the data from the APOGEE survey (Holtzman et al. 2018) and AstroNN added-value catalog (Leung, H.W. & Bovy, Jo 2019b). We create 6 stellar distributions by selecting stars from APOGEE based on galactocentric radial & azimuthal cuts, and combine them in order to derive a joint stellar abundance distribution that gives less weight to stars in the solar vicinity. The resulting contours use a log scale with 0.2 bin size.' + caption: '[Fe/H] vs [C/Fe] using Asplund et al. (2009) values for [Fe/H]Sun = 7.5 and [C/H]Sun = 8.43. The median [C/Fe] vs median [Fe/H] is indicated by the solid curve(s). The scatter points show abundances of individual stellar particles. The observational data for MW compiles the data from the APOGEE survey (Holtzman et al. 2018) and AstroNN added-value catalog (Leung, H.W. & Bovy, Jo 2019b). We create 6 stellar distributions by selecting stars from APOGEE based on galactocentric radial & azimuthal cuts, and combine them in order to derive a joint stellar abundance distribution that gives less weight to stars in the solar vicinity. The resulting contours use a log scale with 0.2 bin size. The arrows at [Fe/H]=-4 indicate the median value of [C/Fe] of gas with [Fe/H]<-4.' output_file: stellar_abundances_FeH_CFe_APOGEE.png section: Stellar Metal Abundances title: '[Fe/H] vs [C/Fe]' @@ -362,7 +362,7 @@ scripts: yvar: C_Fe dataset: APOGEE - filename: scripts/stellar_abundances.py - caption: '[Fe/H] vs [C/O] using Asplund et al. (2009) values for [O/H]Sun = 8.69 and [C/H]Sun = 8.43. The median [C/O] vs median [Fe/H] is indicated by the solid curve(s). The scatter points show abundances of individual stellar particles. The observational data for MW compiles the data from the APOGEE survey (Holtzman et al. 2018) and AstroNN added-value catalog (Leung, H.W. & Bovy, Jo 2019b). We create 6 stellar distributions by selecting stars from APOGEE based on galactocentric radial & azimuthal cuts, and combine them in order to derive a joint stellar abundance distribution that gives less weight to stars in the solar vicinity. The resulting contours use a log scale with 0.2 bin size.' + caption: '[Fe/H] vs [C/O] using Asplund et al. (2009) values for [O/H]Sun = 8.69 and [C/H]Sun = 8.43. The median [C/O] vs median [Fe/H] is indicated by the solid curve(s). The scatter points show abundances of individual stellar particles. The observational data for MW compiles the data from the APOGEE survey (Holtzman et al. 2018) and AstroNN added-value catalog (Leung, H.W. & Bovy, Jo 2019b). We create 6 stellar distributions by selecting stars from APOGEE based on galactocentric radial & azimuthal cuts, and combine them in order to derive a joint stellar abundance distribution that gives less weight to stars in the solar vicinity. The resulting contours use a log scale with 0.2 bin size. The arrows at [Fe/H]=-4 indicate the median value of [C/O] of gas with [Fe/H]<-4.' output_file: stellar_abundances_FeH_CO_APOGEE.png section: Stellar Metal Abundances title: '[Fe/H] vs [C/O]' @@ -371,7 +371,7 @@ scripts: yvar: C_O dataset: APOGEE - filename: scripts/stellar_abundances.py - caption: '[O/H] vs [C/O] using Asplund et al. (2009) values for [O/H]Sun = 8.69 and [C/H]Sun = 8.43. The median [C/O] vs median [O/H] is indicated by the solid curve(s). The scatter points show abundances of individual stellar particles. The observational data for MW compiles the data from the APOGEE survey (Holtzman et al. 2018) and AstroNN added-value catalog (Leung, H.W. & Bovy, Jo 2019b). We create 6 stellar distributions by selecting stars from APOGEE based on galactocentric radial & azimuthal cuts, and combine them in order to derive a joint stellar abundance distribution that gives less weight to stars in the solar vicinity. The resulting contours use a log scale with 0.2 bin size.' + caption: '[O/H] vs [C/O] using Asplund et al. (2009) values for [O/H]Sun = 8.69 and [C/H]Sun = 8.43. The median [C/O] vs median [O/H] is indicated by the solid curve(s). The scatter points show abundances of individual stellar particles. The observational data for MW compiles the data from the APOGEE survey (Holtzman et al. 2018) and AstroNN added-value catalog (Leung, H.W. & Bovy, Jo 2019b). We create 6 stellar distributions by selecting stars from APOGEE based on galactocentric radial & azimuthal cuts, and combine them in order to derive a joint stellar abundance distribution that gives less weight to stars in the solar vicinity. The resulting contours use a log scale with 0.2 bin size. The arrows at [O/H]=-4 indicate the median value of [C/O] of gas with [O/H]<-4.' output_file: stellar_abundances_OH_CO_APOGEE.png section: Stellar Metal Abundances title: '[O/H] vs [C/O]' @@ -380,7 +380,7 @@ scripts: yvar: C_O dataset: APOGEE - filename: scripts/stellar_abundances.py - caption: '[Fe/H] vs [N/Fe] using Asplund et al. (2009) values for [Fe/H]Sun = 7.5 and [N/H]Sun = 7.83. The median [N/Fe] vs median [Fe/H] is indicated by the solid curve(s). The scatter points show abundances of individual stellar particles. The observational data for MW compiles the data from the APOGEE survey (Holtzman et al. 2018) and AstroNN added-value catalog (Leung, H.W. & Bovy, Jo 2019b). We create 6 stellar distributions by selecting stars from APOGEE based on galactocentric radial & azimuthal cuts, and combine them in order to derive a joint stellar abundance distribution that gives less weight to stars in the solar vicinity. The resulting contours use a log scale with 0.2 bin size.' + caption: '[Fe/H] vs [N/Fe] using Asplund et al. (2009) values for [Fe/H]Sun = 7.5 and [N/H]Sun = 7.83. The median [N/Fe] vs median [Fe/H] is indicated by the solid curve(s). The scatter points show abundances of individual stellar particles. The observational data for MW compiles the data from the APOGEE survey (Holtzman et al. 2018) and AstroNN added-value catalog (Leung, H.W. & Bovy, Jo 2019b). We create 6 stellar distributions by selecting stars from APOGEE based on galactocentric radial & azimuthal cuts, and combine them in order to derive a joint stellar abundance distribution that gives less weight to stars in the solar vicinity. The resulting contours use a log scale with 0.2 bin size. The arrows at [Fe/H]=-4 indicate the median value of [N/Fe] of gas with [Fe/H]<-4.' output_file: stellar_abundances_FeH_NFe_APOGEE.png section: Stellar Metal Abundances title: '[Fe/H] vs [N/Fe]' @@ -389,7 +389,7 @@ scripts: yvar: N_Fe dataset: APOGEE - filename: scripts/stellar_abundances.py - caption: '[O/H] vs [N/O] using Asplund et al. (2009) values for [O/H]Sun = 8.69 and [N/H]Sun = 7.83. The median [N/O] vs median [O/H] is indicated by the solid curve(s). The scatter points show abundances of individual stellar particles. The observational data for MW compiles the data from the APOGEE survey (Holtzman et al. 2018) and AstroNN added-value catalog (Leung, H.W. & Bovy, Jo 2019b). We create 6 stellar distributions by selecting stars from APOGEE based on galactocentric radial & azimuthal cuts, and combine them in order to derive a joint stellar abundance distribution that gives less weight to stars in the solar vicinity. The resulting contours use a log scale with 0.2 bin size.' + caption: '[O/H] vs [N/O] using Asplund et al. (2009) values for [O/H]Sun = 8.69 and [N/H]Sun = 7.83. The median [N/O] vs median [O/H] is indicated by the solid curve(s). The scatter points show abundances of individual stellar particles. The observational data for MW compiles the data from the APOGEE survey (Holtzman et al. 2018) and AstroNN added-value catalog (Leung, H.W. & Bovy, Jo 2019b). We create 6 stellar distributions by selecting stars from APOGEE based on galactocentric radial & azimuthal cuts, and combine them in order to derive a joint stellar abundance distribution that gives less weight to stars in the solar vicinity. The resulting contours use a log scale with 0.2 bin size. The arrows at [O/H]=-4 indicate the median value of [N/O] of gas with [O/H]<-4.' output_file: stellar_abundances_OH_NO_APOGEE.png section: Stellar Metal Abundances title: '[O/H] vs [N/O]' @@ -398,7 +398,7 @@ scripts: yvar: N_O dataset: APOGEE - filename: scripts/stellar_abundances.py - caption: '[Fe/H] vs [N/O] using Asplund et al. (2009) values for [Fe/H]Sun = 7.5, [N/H]Sun = 7.83 and [O/H]Sun = 8.69. The median [N/O] vs median [Fe/H] is indicated by the solid curve(s). The scatter points show abundances of individual stellar particles. The observational data for MW compiles the data from the APOGEE survey (Holtzman et al. 2018) and AstroNN added-value catalog (Leung, H.W. & Bovy, Jo 2019b). We create 6 stellar distributions by selecting stars from APOGEE based on galactocentric radial & azimuthal cuts, and combine them in order to derive a joint stellar abundance distribution that gives less weight to stars in the solar vicinity. The resulting contours use a log scale with 0.2 bin size.' + caption: '[Fe/H] vs [N/O] using Asplund et al. (2009) values for [Fe/H]Sun = 7.5, [N/H]Sun = 7.83 and [O/H]Sun = 8.69. The median [N/O] vs median [Fe/H] is indicated by the solid curve(s). The scatter points show abundances of individual stellar particles. The observational data for MW compiles the data from the APOGEE survey (Holtzman et al. 2018) and AstroNN added-value catalog (Leung, H.W. & Bovy, Jo 2019b). We create 6 stellar distributions by selecting stars from APOGEE based on galactocentric radial & azimuthal cuts, and combine them in order to derive a joint stellar abundance distribution that gives less weight to stars in the solar vicinity. The resulting contours use a log scale with 0.2 bin size. The arrows at [Fe/H]=-4 indicate the median value of [N/O] of gas with [O/H]<-4.' output_file: stellar_abundances_FeH_NO_APOGEE.png section: Stellar Metal Abundances title: '[Fe/H] vs [N/O]' @@ -407,7 +407,7 @@ scripts: yvar: N_O dataset: APOGEE - filename: scripts/stellar_abundances.py - caption: '[Fe/H] vs [O/Fe] using Asplund et al. (2009) values for [Fe/H]Sun = 7.5 and [O/H]Sun = 8.69. The median [O/Fe] vs median [Fe/H] is indicated by the solid curve(s). The scatter points show abundances of individual stellar particles. The observational data for MW compiles the data from the GALAH survey (Buder et al. 2021). Contours use a log scale with 0.04 bin size and a minimum star count of 10. All recommended flags are applied to GALAH data to select stars (SN, FE/H and X/Fe quality flags).' + caption: '[Fe/H] vs [O/Fe] using Asplund et al. (2009) values for [Fe/H]Sun = 7.5 and [O/H]Sun = 8.69. The median [O/Fe] vs median [Fe/H] is indicated by the solid curve(s). The scatter points show abundances of individual stellar particles. The observational data for MW compiles the data from the GALAH survey (Buder et al. 2021). Contours use a log scale with 0.04 bin size and a minimum star count of 10. All recommended flags are applied to GALAH data to select stars (SN, FE/H and X/Fe quality flags). The arrows at [Fe/H]=-4 indicate the median value of [O/Fe] of gas with [Fe/H]<-4.' output_file: stellar_abundances_FeH_OFe_GALAH.png section: Stellar Metal Abundances title: '[Fe/H] vs [O/Fe]' @@ -416,7 +416,7 @@ scripts: yvar: O_Fe dataset: GALAH - filename: scripts/stellar_abundances.py - caption: '[Fe/H] vs [O/Fe] using Asplund et al. (2009) values for [Fe/H]Sun = 7.5 and [O/H]Sun = 8.69. The median [O/Fe] vs median [Fe/H] is indicated by the solid curve(s). The scatter points show abundances of individual stellar particles. The observational data for MW compiles the data from the APOGEE survey (Holtzman et al. 2018) and AstroNN added-value catalog (Leung, H.W. & Bovy, Jo 2019b). We create 6 stellar distributions by selecting stars from APOGEE based on galactocentric radial & azimuthal cuts, and combine them in order to derive a joint stellar abundance distribution that gives less weight to stars in the solar vicinity. The resulting contours use a log scale with 0.2 bin size.' + caption: '[Fe/H] vs [O/Fe] using Asplund et al. (2009) values for [Fe/H]Sun = 7.5 and [O/H]Sun = 8.69. The median [O/Fe] vs median [Fe/H] is indicated by the solid curve(s). The scatter points show abundances of individual stellar particles. The observational data for MW compiles the data from the APOGEE survey (Holtzman et al. 2018) and AstroNN added-value catalog (Leung, H.W. & Bovy, Jo 2019b). We create 6 stellar distributions by selecting stars from APOGEE based on galactocentric radial & azimuthal cuts, and combine them in order to derive a joint stellar abundance distribution that gives less weight to stars in the solar vicinity. The resulting contours use a log scale with 0.2 bin size. The arrows at [Fe/H]=-4 indicate the median value of [O/Fe] of gas with [Fe/H]<-4.' output_file: stellar_abundances_FeH_OFe_APOGEE.png section: Stellar Metal Abundances title: '[Fe/H] vs [O/Fe]' @@ -425,7 +425,7 @@ scripts: yvar: O_Fe dataset: APOGEE - filename: scripts/stellar_abundances.py - caption: '[Fe/H] vs [O/Fe] using Asplund et al. (2009) values for [Fe/H]Sun = 7.5 and [O/H]Sun = 8.69. The median [O/Fe] vs median [Fe/H] is indicated by the solid curve(s). The scatter points show abundances of individual stellar particles. The observational data for MW compiles the works of Mishenina+99, Israelian+98, Cayrel+04, Bai+04, Zhang+05, Koch+08. Most of these works assume Grevesser & Anders (1989) values for solar metallicity, their were corrected to Asplund+09. Additional data includes Fornax (Letarte+07), Carina (Kock+05), Sculptor (Geisler+05) and Sagittarious (Sbordone+07).' + caption: '[Fe/H] vs [O/Fe] using Asplund et al. (2009) values for [Fe/H]Sun = 7.5 and [O/H]Sun = 8.69. The median [O/Fe] vs median [Fe/H] is indicated by the solid curve(s). The scatter points show abundances of individual stellar particles. The observational data for MW compiles the works of Mishenina+99, Israelian+98, Cayrel+04, Bai+04, Zhang+05, Koch+08. Most of these works assume Grevesser & Anders (1989) values for solar metallicity, their were corrected to Asplund+09. Additional data includes Fornax (Letarte+07), Carina (Kock+05), Sculptor (Geisler+05) and Sagittarious (Sbordone+07). The arrows at [Fe/H]=-4 indicate the median value of [O/Fe] of gas with [Fe/H]<-4.' output_file: stellar_abundances_FeH_OFe.png section: Stellar Metal Abundances title: '[Fe/H] vs [O/Fe]' @@ -433,7 +433,7 @@ scripts: xvar: Fe_H yvar: O_Fe - filename: scripts/stellar_abundances.py - caption: '[Fe/H] vs [Ne/Fe] using Asplund et al. (2009) values for [Fe/H]Sun = 7.5 and [Ne/H]Sun = 7.93. The median [Ne/Fe] vs median [Fe/H] is indicated by the solid curve(s). The scatter points show abundances of individual stellar particles.' + caption: '[Fe/H] vs [Ne/Fe] using Asplund et al. (2009) values for [Fe/H]Sun = 7.5 and [Ne/H]Sun = 7.93. The median [Ne/Fe] vs median [Fe/H] is indicated by the solid curve(s). The scatter points show abundances of individual stellar particles. The arrows at [Fe/H]=-4 indicate the median value of [Ne/Fe] of gas with [Fe/H]<-4.' output_file: stellar_abundances_FeH_NeFe.png section: Stellar Metal Abundances title: '[Fe/H] vs [Ne/Fe]' @@ -441,7 +441,7 @@ scripts: xvar: Fe_H yvar: Ne_Fe - filename: scripts/stellar_abundances.py - caption: '[Fe/H] vs [Mg/Fe] using Asplund et al. (2009) values for [Fe/H]Sun = 7.5 and [Mg/H]Sun = 7.6. The median [Mg/Fe] vs median [Fe/H] is indicated by the solid curve(s). The scatter points show abundances of individual stellar particles. The observational data for MW compiles the data from the GALAH survey (Buder et al. 2021). Contours use a log scale with 0.04 bin size and a minimum star count of 10. All recommended flags are applied to GALAH data to select stars (SN, FE/H and X/Fe quality flags).' + caption: '[Fe/H] vs [Mg/Fe] using Asplund et al. (2009) values for [Fe/H]Sun = 7.5 and [Mg/H]Sun = 7.6. The median [Mg/Fe] vs median [Fe/H] is indicated by the solid curve(s). The scatter points show abundances of individual stellar particles. The observational data for MW compiles the data from the GALAH survey (Buder et al. 2021). Contours use a log scale with 0.04 bin size and a minimum star count of 10. All recommended flags are applied to GALAH data to select stars (SN, FE/H and X/Fe quality flags). The arrows at [Fe/H]=-4 indicate the median value of [Mg/Fe] of gas with [Fe/H]<-4.' output_file: stellar_abundances_FeH_MgFe_GALAH.png section: Stellar Metal Abundances title: '[Fe/H] vs [Mg/Fe]' @@ -450,7 +450,7 @@ scripts: yvar: Mg_Fe dataset: GALAH - filename: scripts/stellar_abundances.py - caption: '[Fe/H] vs [Mg/Fe] using Asplund et al. (2009) values for [Fe/H]Sun = 7.5 and [Mg/H]Sun = 7.6. The median [Mg/Fe] vs median [Fe/H] is indicated by the solid curve(s). The scatter points show abundances of individual stellar particles. The observational data for MW compiles the data from the APOGEE survey (Holtzman et al. 2018) and AstroNN added-value catalog (Leung, H.W. & Bovy, Jo 2019b). We create 6 stellar distributions by selecting stars from APOGEE based on galactocentric radial & azimuthal cuts, and combine them in order to derive a joint stellar abundance distribution that gives less weight to stars in the solar vicinity. The resulting contours use a log scale with 0.2 bin size.' + caption: '[Fe/H] vs [Mg/Fe] using Asplund et al. (2009) values for [Fe/H]Sun = 7.5 and [Mg/H]Sun = 7.6. The median [Mg/Fe] vs median [Fe/H] is indicated by the solid curve(s). The scatter points show abundances of individual stellar particles. The observational data for MW compiles the data from the APOGEE survey (Holtzman et al. 2018) and AstroNN added-value catalog (Leung, H.W. & Bovy, Jo 2019b). We create 6 stellar distributions by selecting stars from APOGEE based on galactocentric radial & azimuthal cuts, and combine them in order to derive a joint stellar abundance distribution that gives less weight to stars in the solar vicinity. The resulting contours use a log scale with 0.2 bin size. The arrows at [Fe/H]=-4 indicate the median value of [Mg/Fe] of gas with [Fe/H]<-4.' output_file: stellar_abundances_FeH_MgFe_APOGEE.png section: Stellar Metal Abundances title: '[Fe/H] vs [Mg/Fe]' @@ -459,7 +459,7 @@ scripts: yvar: Mg_Fe dataset: APOGEE - filename: scripts/stellar_abundances.py - caption: '[Fe/H] vs [Mg/Fe] using Asplund et al. (2009) values for [Fe/H]Sun = 7.5 and [Mg/H]Sun = 7.6. The median [Mg/Fe] vs median [Fe/H] is indicated by the solid curve(s). The scatter points show abundances of individual stellar particles. The observational data for MW, Carina, Fornax, Sculptor and Sagittarious corresponds to a data compilation presented by Tolstoy, Hill & Tosi (2009) and extracted by Rob Crain. Note solar metallicity of Grevesser & Anders (1989) was corrected to Asplund+09.' + caption: '[Fe/H] vs [Mg/Fe] using Asplund et al. (2009) values for [Fe/H]Sun = 7.5 and [Mg/H]Sun = 7.6. The median [Mg/Fe] vs median [Fe/H] is indicated by the solid curve(s). The scatter points show abundances of individual stellar particles. The observational data for MW, Carina, Fornax, Sculptor and Sagittarious corresponds to a data compilation presented by Tolstoy, Hill & Tosi (2009) and extracted by Rob Crain. Note solar metallicity of Grevesser & Anders (1989) was corrected to Asplund+09. The arrows at [Fe/H]=-4 indicate the median value of [Mg/Fe] of gas with [Fe/H]<-4.' output_file: stellar_abundances_FeH_MgFe.png section: Stellar Metal Abundances title: '[Fe/H] vs [Mg/Fe]' @@ -467,7 +467,7 @@ scripts: xvar: Fe_H yvar: Mg_Fe - filename: scripts/stellar_abundances.py - caption: '[Fe/H] vs [Si/Fe] using Asplund et al. (2009) values for [Fe/H]Sun = 7.5 and [Si/H]Sun = 7.51. The median [Si/Fe] vs median [Fe/H] is indicated by the solid curve(s). The scatter points show abundances of individual stellar particles. The observational data for MW compiles the data from the GALAH survey (Buder et al. 2021). Contours use a log scale with 0.04 bin size and a minimum star count of 10. All recommended flags are applied to GALAH data to select stars (SN, FE/H and X/Fe quality flags).' + caption: '[Fe/H] vs [Si/Fe] using Asplund et al. (2009) values for [Fe/H]Sun = 7.5 and [Si/H]Sun = 7.51. The median [Si/Fe] vs median [Fe/H] is indicated by the solid curve(s). The scatter points show abundances of individual stellar particles. The observational data for MW compiles the data from the GALAH survey (Buder et al. 2021). Contours use a log scale with 0.04 bin size and a minimum star count of 10. All recommended flags are applied to GALAH data to select stars (SN, FE/H and X/Fe quality flags). The arrows at [Fe/H]=-4 indicate the median value of [Si/Fe] of gas with [Fe/H]<-4.' output_file: stellar_abundances_FeH_SiFe_GALAH.png section: Stellar Metal Abundances title: '[Fe/H] vs [Si/Fe]' @@ -476,7 +476,7 @@ scripts: yvar: Si_Fe dataset: GALAH - filename: scripts/stellar_abundances.py - caption: '[Fe/H] vs [Sr/Fe] using Asplund et al. (2009) values for [Fe/H]Sun = 7.5 and [Sr/H]Sun = 2.87. The median [Sr/Fe] vs median [Fe/H] is indicated by the solid curve(s). The scatter points show abundances of individual stellar particles.' + caption: '[Fe/H] vs [Sr/Fe] using Asplund et al. (2009) values for [Fe/H]Sun = 7.5 and [Sr/H]Sun = 2.87. The median [Sr/Fe] vs median [Fe/H] is indicated by the solid curve(s). The scatter points show abundances of individual stellar particles. The arrows at [Fe/H]=-4 indicate the median value of [Sr/Fe] of gas with [Fe/H]<-4.' output_file: stellar_abundances_FeH_SrFe.png section: Stellar Metal Abundances title: '[Fe/H] vs [Sr/Fe]' @@ -484,7 +484,7 @@ scripts: xvar: Fe_H yvar: Sr_Fe - filename: scripts/stellar_abundances.py - caption: '[Fe/H] vs [Ba/Fe] using Asplund et al. (2009) values for [Fe/H]Sun = 7.5 and [Ba/H]Sun = 2.18. The median [Ba/Fe] vs median [Fe/H] is indicated by the solid curve(s). The scatter points show abundances of individual stellar particles. The observational data for MW compiles the data from the GALAH survey (Buder et al. 2021). Contours use a log scale with 0.04 bin size and a minimum star count of 10. All recommended flags are applied to GALAH data to select stars (SN, FE/H and X/Fe quality flags).' + caption: '[Fe/H] vs [Ba/Fe] using Asplund et al. (2009) values for [Fe/H]Sun = 7.5 and [Ba/H]Sun = 2.18. The median [Ba/Fe] vs median [Fe/H] is indicated by the solid curve(s). The scatter points show abundances of individual stellar particles. The observational data for MW compiles the data from the GALAH survey (Buder et al. 2021). Contours use a log scale with 0.04 bin size and a minimum star count of 10. All recommended flags are applied to GALAH data to select stars (SN, FE/H and X/Fe quality flags). The arrows at [Fe/H]=-4 indicate the median value of [Ba/Fe] of gas with [Fe/H]<-4.' output_file: stellar_abundances_FeH_BaFe_GALAH.png section: Stellar Metal Abundances title: '[Fe/H] vs [Ba/Fe]' @@ -493,7 +493,7 @@ scripts: yvar: Ba_Fe dataset: GALAH - filename: scripts/stellar_abundances.py - caption: '[Fe/H] vs [Eu/Fe] using Asplund et al. (2009) values for [Fe/H]Sun = 7.5 and [Eu/H]Sun = 0.52. The median [Eu/Fe] vs median [Fe/H] is indicated by the solid curve(s). The scatter points show abundances of individual stellar particles. The observational data for MW compiles the data from the GALAH survey (Buder et al. 2021). Contours use a log scale with 0.04 bin size and a minimum star count of 10. All recommended flags are applied to GALAH data to select stars (SN, FE/H and X/Fe quality flags).' + caption: '[Fe/H] vs [Eu/Fe] using Asplund et al. (2009) values for [Fe/H]Sun = 7.5 and [Eu/H]Sun = 0.52. The median [Eu/Fe] vs median [Fe/H] is indicated by the solid curve(s). The scatter points show abundances of individual stellar particles. The observational data for MW compiles the data from the GALAH survey (Buder et al. 2021). Contours use a log scale with 0.04 bin size and a minimum star count of 10. All recommended flags are applied to GALAH data to select stars (SN, FE/H and X/Fe quality flags). The arrows at [Fe/H]=-4 indicate the median value of [Eu/Fe] of gas with [Fe/H]<-4.' output_file: stellar_abundances_FeH_EuFe_GALAH.png section: Stellar Metal Abundances title: '[Fe/H] vs [Eu/Fe]' @@ -502,7 +502,7 @@ scripts: yvar: Eu_Fe dataset: GALAH - filename: scripts/stellar_abundances.py - caption: '[O/H] vs [O/Fe] using Asplund et al. (2009) values for [Fe/H]Sun = 7.5 and [O/H]Sun = 8.69. The median [O/Fe] vs median [O/H] is indicated by the solid curve(s). The scatter points show abundances of individual stellar particles. The observational data for MW compiles the data from the APOGEE survey (Holtzman et al. 2018) and AstroNN added-value catalog (Leung, H.W. & Bovy, Jo 2019b). We create 6 stellar distributions by selecting stars from APOGEE based on galactocentric radial & azimuthal cuts, and combine them in order to derive a joint stellar abundance distribution that gives less weight to stars in the solar vicinity. The resulting contours use a log scale with 0.2 bin size.' + caption: '[O/H] vs [O/Fe] using Asplund et al. (2009) values for [Fe/H]Sun = 7.5 and [O/H]Sun = 8.69. The median [O/Fe] vs median [O/H] is indicated by the solid curve(s). The scatter points show abundances of individual stellar particles. The observational data for MW compiles the data from the APOGEE survey (Holtzman et al. 2018) and AstroNN added-value catalog (Leung, H.W. & Bovy, Jo 2019b). We create 6 stellar distributions by selecting stars from APOGEE based on galactocentric radial & azimuthal cuts, and combine them in order to derive a joint stellar abundance distribution that gives less weight to stars in the solar vicinity. The resulting contours use a log scale with 0.2 bin size. The arrows at [O/H]=-4 indicate the median value of [O/Fe] of gas with [O/H]<-4.' output_file: stellar_abundances_OH_OFe_APOGEE.png section: Stellar Metal Abundances title: '[O/H] vs [O/Fe]' @@ -511,7 +511,7 @@ scripts: yvar: O_Fe dataset: APOGEE - filename: scripts/stellar_abundances.py - caption: '[O/H] vs [Mg/Fe] using Asplund et al. (2009) values for [O/H]Sun = 8.69 and [Mg/H]Sun = 7.6. The median [Mg/Fe] vs median [O/H] is indicated by the solid curve(s). The scatter points show abundances of individual stellar particles. The observational data for MW compiles the data from the APOGEE survey (Holtzman et al. 2018) and AstroNN added-value catalog (Leung, H.W. & Bovy, Jo 2019b). We create 6 stellar distributions by selecting stars from APOGEE based on galactocentric radial & azimuthal cuts, and combine them in order to derive a joint stellar abundance distribution that gives less weight to stars in the solar vicinity. The resulting contours use a log scale with 0.2 bin size.' + caption: '[O/H] vs [Mg/Fe] using Asplund et al. (2009) values for [O/H]Sun = 8.69 and [Mg/H]Sun = 7.6. The median [Mg/Fe] vs median [O/H] is indicated by the solid curve(s). The scatter points show abundances of individual stellar particles. The observational data for MW compiles the data from the APOGEE survey (Holtzman et al. 2018) and AstroNN added-value catalog (Leung, H.W. & Bovy, Jo 2019b). We create 6 stellar distributions by selecting stars from APOGEE based on galactocentric radial & azimuthal cuts, and combine them in order to derive a joint stellar abundance distribution that gives less weight to stars in the solar vicinity. The resulting contours use a log scale with 0.2 bin size. The arrows at [O/H]=-4 indicate the median value of [Mg/Fe] of gas with [O/H]<-4.' output_file: stellar_abundances_OH_MgFe_APOGEE.png section: Stellar Metal Abundances title: '[O/H] vs [Mg/Fe]' diff --git a/colibre/scripts/stellar_abundances.py b/colibre/scripts/stellar_abundances.py index 425e6d4a..a5f28a92 100644 --- a/colibre/scripts/stellar_abundances.py +++ b/colibre/scripts/stellar_abundances.py @@ -129,82 +129,69 @@ def read_data(data, xvar, yvar): if xvar == "O_H": O_H = np.log10(oxygen / hydrogen) - O_H_Sun - O_H[oxygen == 0] = -4 # set lower limit - O_H[O_H < -4] = -4 # set lower limit + O_H[oxygen == 0] = -10 # set lower limit xval = O_H elif xvar == "Fe_H": Fe_H = np.log10(iron / hydrogen) - Fe_H_Sun - Fe_H[iron == 0] = -4 # set lower limit - Fe_H[Fe_H < -4] = -4 # set lower limit + Fe_H[iron == 0] = -10 # set lower limit xval = Fe_H else: raise AttributeError(f"Unknown x variable: {xvar}!") if yvar == "C_Fe": C_Fe = np.log10(carbon / iron) - C_Fe_Sun - C_Fe[iron == 0] = -2 # set lower limit - C_Fe[carbon == 0] = -2 # set lower limit - C_Fe[C_Fe < -2] = -2 # set lower limit + C_Fe[iron == 0] = -10 # set lower limit + C_Fe[carbon == 0] = -10 # set lower limit yval = C_Fe elif yvar == "N_Fe": N_Fe = np.log10(nitrogen / iron) - N_Fe_Sun - N_Fe[iron == 0] = -2 # set lower limit - N_Fe[nitrogen == 0] = -2 # set lower limit - N_Fe[N_Fe < -2] = -2 # set lower limit + N_Fe[iron == 0] = -10 # set lower limit + N_Fe[nitrogen == 0] = -10 # set lower limit yval = N_Fe elif yvar == "N_O": N_O = np.log10(nitrogen / oxygen) - N_O_Sun - N_O[oxygen == 0] = -2 # set lower limit - N_O[nitrogen == 0] = -2 # set lower limit - N_O[N_O < -2] = -2 # set lower limit + N_O[oxygen == 0] = -10 # set lower limit + N_O[nitrogen == 0] = -10 # set lower limit yval = N_O elif yvar == "C_O": C_O = np.log10(carbon / oxygen) - C_O_Sun - C_O[oxygen == 0] = -2 # set lower limit - C_O[carbon == 0] = -2 # set lower limit - C_O[C_O < -2] = -2 # set lower limit + C_O[oxygen == 0] = -10 # set lower limit + C_O[carbon == 0] = -10 # set lower limit yval = C_O elif yvar == "O_Fe": O_Fe = np.log10(oxygen / iron) - O_Fe_Sun - O_Fe[iron == 0] = -2 # set lower limit - O_Fe[oxygen == 0] = -2 # set lower limit - O_Fe[O_Fe < -2] = -2 # set lower limit + O_Fe[iron == 0] = -10 # set lower limit + O_Fe[oxygen == 0] = -10 # set lower limit yval = O_Fe elif yvar == "Mg_Fe": Mg_Fe = np.log10(magnesium / iron) - Mg_Fe_Sun - Mg_Fe[iron == 0] = -2 # set lower limit - Mg_Fe[magnesium == 0] = -2 # set lower limit - Mg_Fe[Mg_Fe < -2] = -2 # set lower limit + Mg_Fe[iron == 0] = -10 # set lower limit + Mg_Fe[magnesium == 0] = -10 # set lower limit yval = Mg_Fe elif yvar == "Si_Fe": Si_Fe = np.log10(silicon / iron) - Si_Fe_Sun - Si_Fe[iron == 0] = -2 # set lower limit - Si_Fe[silicon == 0] = -2 # set lower limit - Si_Fe[Si_Fe < -2] = -2 # set lower limit + Si_Fe[iron == 0] = -10 # set lower limit + Si_Fe[silicon == 0] = -10 # set lower limit yval = Si_Fe elif yvar == "Ne_Fe": Ne_Fe = np.log10(neon / iron) - Ne_Fe_Sun - Ne_Fe[iron == 0] = -2 # set lower limit - Ne_Fe[neon == 0] = -2 # set lower limit - Ne_Fe[Ne_Fe < -2] = -2 # set lower limit + Ne_Fe[iron == 0] = -10 # set lower limit + Ne_Fe[neon == 0] = -10 # set lower limit yval = Ne_Fe elif yvar == "Eu_Fe": Eu_Fe = np.log10(europium / iron) - Eu_Fe_Sun - Eu_Fe[iron == 0] = -2 # set lower limit - Eu_Fe[europium == 0] = -2 # set lower limit - Eu_Fe[Eu_Fe < -2] = -2 # set lower limit + Eu_Fe[iron == 0] = -10 # set lower limit + Eu_Fe[europium == 0] = -10 # set lower limit yval = Eu_Fe elif yvar == "Ba_Fe": Ba_Fe = np.log10(barium / iron) - Ba_Fe_Sun - Ba_Fe[iron == 0] = -2 # set lower limit - Ba_Fe[barium == 0] = -2 # set lower limit - Ba_Fe[Ba_Fe < -2] = -2 # set lower limit + Ba_Fe[iron == 0] = -10 # set lower limit + Ba_Fe[barium == 0] = -10 # set lower limit yval = Ba_Fe elif yvar == "Sr_Fe": Sr_Fe = np.log10(strontium / iron) - Sr_Fe_Sun - Sr_Fe[iron == 0] = -2 # set lower limit - Sr_Fe[strontium == 0] = -2 # set lower limit - Sr_Fe[Sr_Fe < -2] = -2 # set lower limit + Sr_Fe[iron == 0] = -10 # set lower limit + Sr_Fe[strontium == 0] = -10 # set lower limit yval = Sr_Fe elif yvar == "Fe_SNIa_fraction": Fe_snia_fraction = unyt_array(np.zeros_like(iron), "dimensionless") @@ -285,6 +272,21 @@ def read_data(data, xvar, yvar): ) simulation_labels.append(f"{name} ($z={redshift:.1f}$)") + # Let's add lower symbol indicating the median for [Fe/H]<-4: + if yvar != "Fe_SNIa_fraction": + mask = xval < -4 + ym = np.median(yval[mask]) + ax.arrow( + -3.6, + ym, + -0.2, + 0, + head_width=0.05, + head_length=0.1, + color=colour, + zorder=1000, + ) + path_to_obs_data = f"{arguments.config.config_directory}/{arguments.config.observational_data_directory}" if dataset == "APOGEE": if xvar == "Fe_H":