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Galaxies of the full TNG100-1 population (centrals and satellites)."},"definitions":{"imf":"chabrier03","massDefinition":"unspecified","population":"all","colourBand":"SDSS g-r (SDSS u,g,r,i,z passbands at airmass 1.3, galaxy at z=0)","colourAperture":"30 pkpc (3D radius from the subhalo centre)","resolutionCut":"10^9 < M* < 10^12 Msun (Fig. 1 caption)","cosmology":{"H0":67.74,"Om":0.3089},"dustTreatment":"attenuated (Model D: resolved dust, uniform-scattering geometry)"},"provenance":{"tier":"digitized-figure","citation":"Nelson et al. 2018, MNRAS 475, 624 (arXiv:1707.03395), Appendix figure: building up the dust model (Models A-D)","doi":"10.1093/mnras/stx3040","url":"https://arxiv.org/abs/1707.03395","retrieved":"2026-10-18","figure":"Appendix fig_dust_model_comparison","panel":"three mass-bin panels, Model D (resolved dust, uniform-scattering geometry)","checksumSha256":"578a6704498c2496c961388da4b11d20cc110a94a54a668eeb9f34a48469d08c","sourceMember":"appendix2.pdf (3 pt stroked curve, legend colour (0.12, 0.47, 0.71))","extractionMethod":"vector path vertices from the figure PDF (PyMuPDF get_drawings), transformed through axes calibrated on labelled tick marks; PDF polyline integrated per 0.01-mag bin","axisCalibrationPixels":"x: labelled ticks -0.2..1.0 of each panel; y: labelled ticks of each panel; every PDF integrates to 1.000 +- 0.001; mass bin identified by the SDSS curve identical to the corresponding Fig. 1 panel","digitizationUncertaintyDex":0.01},"calibration":"prediction","rankable":false,"notes":"Vector-path extraction of a normalised PDF curve (not a count histogram); the curve integrals over the plotted colour range are 1.000, 1.000, 1.001 (bin by bin)."},{"id":"trayford15.eagle-ref100.colour-counts.z0p1.m9p45-10p05","source":"EAGLE","run":"Ref-L0100N1504 (per galaxy counts, 9.45 < log M* <= 10.05)","kind":"simulation","relation":"colour","epoch":{"zRepresentative":0.1,"zNominal":0.1,"zMin":0.1,"zMax":0.1,"mode":"published-epoch","snapshot":null},"axes":{"xDefinition":"log10 stellar mass","xUnit":"log10(Msun)","yDefinition":"rest-frame (g-r) colour (SDSS g and r bands, AB), dust model not stated for this appendix figure","yUnit":"mag (AB)"},"domain":{"xMin":9.75,"xMax":9.75},"representation":{"type":"points","connect":true,"intervalKind":"scatter","points":[{"x":9.75,"y":0.466219,"yLow":0.345728,"yHigh":0.69679,"count":4461}],"distribution":{"xEdges":[9.45,10.05],"yEdges":[-0.061,-0.0171,0.0268,0.0707,0.1146,0.1585,0.2024,0.2463,0.2902,0.3341,0.378,0.422,0.4659,0.5098,0.5537,0.5976,0.6415,0.6854,0.7293,0.7732,0.8171,0.861,0.9049,0.9488,0.9927,1.0366,1.0805,1.1244,1.1683],"counts":[[0,0,1,1,3,22,56,170,327,505,596,546,481,335,246,229,154,290,402,77,17,3,0,0,0,0,0,0]],"weighting":"number","thresholds":[],"summary":{"levels":[0.05,0.16,0.5,0.84,0.95],"minCount":10,"thresholds":[],"n":[4461],"quantiles":[[0.282466],[0.345728],[0.466219],[0.69679],[0.759435]],"fracBelow":[],"between":[null],"bluePeak":[null],"redPeak":[null],"xCentres":[9.75]}}},"scatter":null,"selection":{"population":"all galaxies with M* in the bin, at least 100 star particles","warning":"Counts per colour bin of the galaxies of EAGLE Ref-L0100N1504 with 9.45 < log10(M*/Msun) <= 10.05 at z = 0.1 (rest-frame g-r), read from the step histogram of Trayford et al. 2015 (MNRAS 452, 2879), Appendix Fig. B1 (top panel); no table is published. 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Colour bins are about 0.0438 mag wide."},"definitions":{"imf":"chabrier03","cosmology":{"H0":67.77,"Om":0.307},"massDefinition":"unspecified","population":"all","colourBand":"rest-frame SDSS g-r (ugriz photometric system of the paper, AB magnitudes)","colourAperture":"30 pkpc (3D sphere centred on the subhalo potential minimum)","resolutionCut":"galaxies with at least 100 star particles","dustTreatment":"unspecified (appendix figure on colour convergence; the dust model is not named in the appendix text or caption)"},"provenance":{"tier":"digitized-figure","citation":"Trayford et al. 2015, MNRAS 452, 2879 (arXiv:1504.04374), Appendix Fig. B1 (colour convergence: Ref-100, Ref-25, Recal-25)","doi":"10.1093/mnras/stv1985","url":"https://arxiv.org/abs/1504.04374","retrieved":"2026-10-18","figure":"Fig. B1 (fig:conv), top panel","panel":"Ref-L0100N1504, 9.45 < log M* <= 10.05","checksumSha256":"fba5afe970855ad4c539da53783fa84cfe14575e8cf066ad696217465ed1fbde","sourceMember":"FigB1a.pdf (step-histogram path, solid blue)","extractionMethod":"vector path vertices from the figure PDF (PyMuPDF get_drawings): horizontal segments of the step histogram, transformed through axes calibrated on labelled tick marks","axisCalibrationPixels":"x: labelled ticks 0.0-1.0; y: labelled ticks of the left axis (0-1200) and right axis (0-15); both fits snapped to ticks; counts are integers to within 0.05; left axis = 64 x right axis asserted","digitizationUncertaintyDex":0.01},"calibration":"prediction","rankable":false,"notes":"Vector-path extraction of a count histogram; integer counts."},{"id":"trayford15.eagle-ref25.colour-counts.z0p1.m9p45-10p05","source":"EAGLE","run":"Ref-L0025N0376 (per galaxy counts, 9.45 < log M* <= 10.05)","kind":"simulation","relation":"colour","epoch":{"zRepresentative":0.1,"zNominal":0.1,"zMin":0.1,"zMax":0.1,"mode":"published-epoch","snapshot":null},"axes":{"xDefinition":"log10 stellar mass","xUnit":"log10(Msun)","yDefinition":"rest-frame (g-r) colour (SDSS g and r bands, AB), dust model not stated for this appendix figure","yUnit":"mag (AB)"},"domain":{"xMin":9.75,"xMax":9.75},"representation":{"type":"points","connect":true,"intervalKind":"scatter","points":[{"x":9.75,"y":0.4659,"yLow":0.341514,"yHigh":0.663325,"count":72}],"distribution":{"xEdges":[9.45,10.05],"yEdges":[-0.061,-0.0171,0.0268,0.0707,0.1146,0.1585,0.2024,0.2463,0.2902,0.3341,0.378,0.422,0.4659,0.5098,0.5537,0.5976,0.6415,0.6854,0.7293,0.7732,0.8171,0.861,0.9049,0.9488,0.9927,1.0366,1.0805,1.1244,1.1683],"counts":[[0,0,0,0,0,0,1,1,8,9,7,10,10,4,5,2,7,4,2,2,0,0,0,0,0,0,0,0]],"weighting":"number","thresholds":[],"summary":{"levels":[0.05,0.16,0.5,0.84,0.95],"minCount":10,"thresholds":[],"n":[72],"quantiles":[[0.29898],[0.341514],[0.4659],[0.663325],[0.73808]],"fracBelow":[],"between":[null],"bluePeak":[null],"redPeak":[null],"xCentres":[9.75]}}},"scatter":null,"selection":{"population":"all galaxies with M* in the bin, at least 100 star particles","warning":"Counts per colour bin of the galaxies of EAGLE Ref-L0025N0376 with 9.45 < log10(M*/Msun) <= 10.05 at z = 0.1 (rest-frame g-r), read from the step histogram of Trayford et al. 2015 (MNRAS 452, 2879), Appendix Fig. B1 (top panel); no table is published. These are galaxy numbers per colour bin (integers, verified): Ref-100 on the left axis, the two 25-Mpc boxes on the right axis (range 1/64 of the left one for the box volume). The sum over the bins is 72 galaxies. The bottom panel of the paper's figure (8.7 < log M* <= 9.3) is not in the arXiv source: FigB1b.pdf duplicates the 9.45-10.05 panel. The paper does not state which dust model the histograms use. Colour bins are about 0.0438 mag wide."},"definitions":{"imf":"chabrier03","cosmology":{"H0":67.77,"Om":0.307},"massDefinition":"unspecified","population":"all","colourBand":"rest-frame SDSS g-r (ugriz photometric system of the paper, AB magnitudes)","colourAperture":"30 pkpc (3D sphere centred on the subhalo potential minimum)","resolutionCut":"galaxies with at least 100 star particles","dustTreatment":"unspecified (appendix figure on colour convergence; the dust model is not named in the appendix text or caption)"},"provenance":{"tier":"digitized-figure","citation":"Trayford et al. 2015, MNRAS 452, 2879 (arXiv:1504.04374), Appendix Fig. B1 (colour convergence: Ref-100, Ref-25, Recal-25)","doi":"10.1093/mnras/stv1985","url":"https://arxiv.org/abs/1504.04374","retrieved":"2026-10-18","figure":"Fig. B1 (fig:conv), top panel","panel":"Ref-L0025N0376, 9.45 < log M* <= 10.05","checksumSha256":"fba5afe970855ad4c539da53783fa84cfe14575e8cf066ad696217465ed1fbde","sourceMember":"FigB1a.pdf (step-histogram path, dashed red)","extractionMethod":"vector path vertices from the figure PDF (PyMuPDF get_drawings): horizontal segments of the step histogram, transformed through axes calibrated on labelled tick marks","axisCalibrationPixels":"x: labelled ticks 0.0-1.0; y: labelled ticks of the left axis (0-1200) and right axis (0-15); both fits snapped to ticks; counts are integers to within 0.05; left axis = 64 x right axis asserted","digitizationUncertaintyDex":0.01},"calibration":"prediction","rankable":false,"notes":"Vector-path extraction of a count histogram; integer counts."},{"id":"trayford15.eagle-recal25.colour-counts.z0p1.m9p45-10p05","source":"EAGLE","run":"Recal-L0025N0752 (per galaxy counts, 9.45 < log M* <= 10.05)","kind":"simulation","relation":"colour","epoch":{"zRepresentative":0.1,"zNominal":0.1,"zMin":0.1,"zMax":0.1,"mode":"published-epoch","snapshot":null},"axes":{"xDefinition":"log10 stellar mass","xUnit":"log10(Msun)","yDefinition":"rest-frame (g-r) colour (SDSS g and r bands, AB), dust model not stated for this appendix figure","yUnit":"mag (AB)"},"domain":{"xMin":9.75,"xMax":9.75},"representation":{"type":"points","connect":true,"intervalKind":"scatter","points":[{"x":9.75,"y":0.387059,"yLow":0.292395,"yHigh":0.51858,"count":85}],"distribution":{"xEdges":[9.45,10.05],"yEdges":[-0.061,-0.0171,0.0268,0.0707,0.1146,0.1585,0.2024,0.2463,0.2902,0.3341,0.378,0.422,0.4659,0.5098,0.5537,0.5976,0.6415,0.6854,0.7293,0.7732,0.8171,0.861,0.9049,0.9488,0.9927,1.0366,1.0805,1.1244,1.1683],"counts":[[0,0,0,0,0,0,4,9,12,14,17,7,8,2,2,2,1,5,0,2,0,0,0,0,0,0,0,0]],"weighting":"number","thresholds":[],"summary":{"levels":[0.05,0.16,0.5,0.84,0.95],"minCount":10,"thresholds":[],"n":[85],"quantiles":[[0.247519],[0.292395],[0.387059],[0.51858],[0.709545]],"fracBelow":[],"between":[null],"bluePeak":[null],"redPeak":[null],"xCentres":[9.75]}}},"scatter":null,"selection":{"population":"all galaxies with M* in the bin, at least 100 star particles","warning":"Counts per colour bin of the galaxies of EAGLE Recal-L0025N0752 with 9.45 < log10(M*/Msun) <= 10.05 at z = 0.1 (rest-frame g-r), read from the step histogram of Trayford et al. 2015 (MNRAS 452, 2879), Appendix Fig. B1 (top panel); no table is published. These are galaxy numbers per colour bin (integers, verified): Ref-100 on the left axis, the two 25-Mpc boxes on the right axis (range 1/64 of the left one for the box volume). The sum over the bins is 85 galaxies. The bottom panel of the paper's figure (8.7 < log M* <= 9.3) is not in the arXiv source: FigB1b.pdf duplicates the 9.45-10.05 panel. The paper does not state which dust model the histograms use. Colour bins are about 0.0438 mag wide."},"definitions":{"imf":"chabrier03","cosmology":{"H0":67.77,"Om":0.307},"massDefinition":"unspecified","population":"all","colourBand":"rest-frame SDSS g-r (ugriz photometric system of the paper, AB magnitudes)","colourAperture":"30 pkpc (3D sphere centred on the subhalo potential minimum)","resolutionCut":"galaxies with at least 100 star particles","dustTreatment":"unspecified (appendix figure on colour convergence; the dust model is not named in the appendix text or caption)"},"provenance":{"tier":"digitized-figure","citation":"Trayford et al. 2015, MNRAS 452, 2879 (arXiv:1504.04374), Appendix Fig. B1 (colour convergence: Ref-100, Ref-25, Recal-25)","doi":"10.1093/mnras/stv1985","url":"https://arxiv.org/abs/1504.04374","retrieved":"2026-10-18","figure":"Fig. B1 (fig:conv), top panel","panel":"Recal-L0025N0752, 9.45 < log M* <= 10.05","checksumSha256":"fba5afe970855ad4c539da53783fa84cfe14575e8cf066ad696217465ed1fbde","sourceMember":"FigB1a.pdf (step-histogram path, solid red)","extractionMethod":"vector path vertices from the figure PDF (PyMuPDF get_drawings): horizontal segments of the step histogram, transformed through axes calibrated on labelled tick marks","axisCalibrationPixels":"x: labelled ticks 0.0-1.0; y: labelled ticks of the left axis (0-1200) and right axis (0-15); both fits snapped to ticks; counts are integers to within 0.05; left axis = 64 x right axis asserted","digitizationUncertaintyDex":0.01},"calibration":"prediction","rankable":false,"notes":"Vector-path extraction of a count histogram; integer counts."},{"id":"dave19.simba.ssfr-hist.m100n1024.z0p1","source":"SIMBA","run":"m100n1024 (per galaxy, normalised sSFR histogram in three mass bins)","kind":"simulation","relation":"ssfr","epoch":{"zRepresentative":0.1,"zNominal":0.1,"zMin":0.1,"zMax":0.1,"mode":"published-epoch","snapshot":null},"axes":{"xDefinition":"log10 stellar mass (bins 1e9-1e10, 1e10-1e11, >1e11; the last bin is open: 12.0 is a nominal upper edge)","xUnit":"log10(Msun)","yDefinition":"log10 specific SFR (instantaneous SFR of the gas elements / stellar mass); the lowest bin holds all galaxies with sSFR < 10^-2.5 Gyr^-1 (axis in Gyr^-1, converted by subtracting 9 dex)","yUnit":"log10(yr^-1)"},"domain":{"xMin":9.5,"xMax":11.5},"representation":{"type":"points","connect":true,"intervalKind":"scatter","points":[{"x":9.5,"y":-9.779149,"yLow":-10.786037,"yHigh":-9.348161,"count":99996},{"x":10.5,"y":-11.004378,"yLow":-11.477163,"yHigh":-10.102135,"count":99997},{"x":11.5,"y":-11.466273,"yLow":-11.557207,"yHigh":-10.850878,"count":99996}],"distribution":{"xEdges":[9,10,11,12],"yEdges":[-11.6,-11.4,-11.2,-11,-10.8,-10.6,-10.4,-10.2,-10,-9.8,-9.6,-9.4,-9.2,-9,-8.8,-8.6],"counts":[[11750,851,1294,1907,2827,4393,6301,7561,11580,14714,16996,14748,4734,340,0],[26050,11414,12815,10084,8053,7493,4902,6512,5182,3851,2661,770,210,0,0],[74776,2702,4504,2702,3603,2702,4504,2702,1801,0,0,0,0,0,0]],"weighting":"pseudo-counts: fraction of the galaxies of the mass bin per 0.2-dex sSFR bin (the figure's 'fraction', sums to 1) x 100000; relative within a mass bin only, not galaxy numbers","thresholds":[-11,-10.5],"summary":{"levels":[0.05,0.16,0.5,0.84,0.95],"minCount":10,"thresholds":[-11,-10.5],"n":[99996,99997,99996],"quantiles":[[-11.514897,-11.561613,-11.586627],[-10.786037,-11.477163,-11.557207],[-9.779149,-11.004378,-11.466273],[-9.348161,-10.102135,-10.850878],[-9.196865,-9.670571,-10.22206]],"fracBelow":[[0.138956,0.502805,0.819853],[0.208263,0.721647,0.896416]],"between":[0.069308,0.218842,0.076563],"bluePeak":[-9.5,-10.1,-10.3],"redPeak":[-11.5,-11.5,-11.5],"xCentres":[9.5,10.5,11.5]}}},"scatter":null,"selection":{"population":"all SIMBA m100n1024 galaxies in the stellar-mass bin at z=0.1 (centrals and satellites)","warning":"Fractions of galaxies per sSFR bin read from the vector lines (through the bin centres) of Dave et al. 2019 (MNRAS 486, 2827), Fig. mainseqhist (solid lines, SIMBA z=0.1); no table is published. The caption says 'All galaxies with sSFR<10^-2.5 Gyr^-1 are placed in the lowest bin': the lowest bin (centre log sSFR = -2.5 Gyr^-1 = -11.5 yr^-1) is therefore an underflow bin and its nominal edges are not physical limits. The stellar-mass bins are 1e9-1e10, 1e10-1e11 and >1e11 Msun; the upper edge of the last bin is not stated and 12.0 is a nominal value. The dotted GSWLC-D2 observed histograms are not stored. The figure plots fractions, not counts; no galaxy numbers are given. The SFR-M* scatter plots of the same paper (mainseq_z0.jpg, mainseq_z2.jpg) are JPEG rasters and cannot be used."},"definitions":{"imf":"chabrier03","cosmology":{"H0":68,"Om":0.3},"massDefinition":"unspecified","population":"all","sfrTimescaleMyr":"instantaneous","sfrStatistic":"per-galaxy","sfrIndicator":"instantaneous SFRs from the gas elements"},"provenance":{"tier":"digitized-figure","citation":"Dave et al. 2019, MNRAS 486, 2827 (arXiv:1901.10203), sSFR histograms in three stellar-mass bins at z=0.1 (SIMBA, solid lines)","doi":"10.1093/mnras/stz937","url":"https://arxiv.org/abs/1901.10203","retrieved":"2026-10-18","figure":"mainseqhist (histogram of sSFR in three bins of stellar mass)","panel":"SIMBA z=0.1 solid lines","checksumSha256":"9ee4dd849016da695b5affb9863aa63be4d39071e54ef4f8ab37fa3a4656f593","sourceMember":"mainseqhist_z0.pdf (2 pt solid lines blue, green, red)","extractionMethod":"vector path vertices from the figure PDF (PyMuPDF get_drawings), transformed through axes calibrated on labelled tick marks","axisCalibrationPixels":"x: labelled ticks -3.0..0.5 (the minus signs are missing from the text layer; the six negative labels share the same offset to their ticks, asserted); y: labelled ticks 0.0-0.7; each curve sums to 0.9999","digitizationUncertaintyDex":0.01,"definitionFills":["dave20-simba-imf"]},"calibration":"prediction","rankable":false,"notes":"Vector-path extraction. 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The paper's own relation (Fig. 11) is a raster image and is not in the dataset. 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The kinks at the refinement redshifts z = 1.5 and 4 are numerical (the paper says so)."},"definitions":{"imf":"kroupa01","cosmology":{"H0":67.4,"Om":0.315},"densityFrame":"comoving","sfrIndicator":"stellar mass formed per 50 Myr from particle birth times","sfrIntegrationLimit":"all stellar particles in the simulation volume (bound, unbound and outside halos)","dustCorrection":"none","population":"all stars formed in the box"},"provenance":{"tier":"digitized-figure","citation":"Lee et al. 2026 (The DARWIN Project; arXiv:2610.25786, submitted to ApJ), Fig. 5 (star formation rate density)","doi":"10.48550/arXiv.2610.25786","url":"https://arxiv.org/abs/2610.25786","retrieved":"2026-10-23","figure":"Fig. 5 (star formation rate density)","panel":"DARWIN-1 curve (red)","checksumSha256":"61d509dc85b80ef379790c95e949d87ddcd390bb5083e66264c9bceb7567cd24","sourceMember":"figures/rho_sfr.pdf","extractionMethod":"vector path vertices from the figure PDF (PyMuPDF get_drawings), transformed through axes calibrated on labelled tick marks","axisCalibrationPixels":"x: 1+z on a log axis (labelled ticks read as 1 and 10, minor ticks at log10 2 to 9); y: log axis (labelled ticks read as 0.10 and 0.01); the labels are outlined paths, so their values were read from the rendered figure and checked against the four dotted refinement lines (z = 0.25, 1.5, 4, 9)","digitizationUncertaintyDex":0.01,"sourceTexSha256":"81efa70c506f72278f7afba3b7baffd1961d6b8522063d31f073b9c70db90c11"},"calibration":"prediction","rankable":false,"notes":"Vector-path extraction; exact to PDF coordinate precision. The paper prints no SFRD values; the axes are checked against the printed refinement redshifts and the printed peak epoch."},{"id":"lee26.darwin1.gsmf.z5","source":"DARWIN","run":"DARWIN-1 (65.5 cMpc box)","kind":"simulation","relation":"gsmf","epoch":{"zRepresentative":5,"zNominal":5,"zMin":5,"zMax":5,"mode":"published-epoch","snapshot":null},"axes":{"xDefinition":"log10 total stellar mass","xUnit":"log10(Msun)","yDefinition":"log10 number density per dex of stellar mass (comoving)","yUnit":"log10(cMpc^-3 dex^-1)"},"domain":{"xMin":9.167,"xMax":10.167},"representation":{"type":"points","intervalKind":"uncertainty","connect":true,"points":[{"x":9.167,"y":-3.1333,"yHigh":-3.0843,"yLow":-3.1891},{"x":9.5,"y":-3.63,"yHigh":-3.5456,"yLow":-3.7341},{"x":9.834,"y":-4.0183,"yHigh":-3.8932,"yLow":-4.194},{"x":10.167,"y":-4.6712,"yHigh":-4.439,"yLow":-5.2049}]},"scatter":null,"selection":{"population":"all galaxies of the box","warning":"Galaxy stellar mass function of the DARWIN-1 box at z = 5 (the panel label; the galaxy counts of the public catalogue snapshots at z = 5.015, 3.002, 1.002 and 0.2517 reproduce the bins of the four panels, see the records darwin1.catalogue.gsmf.* counted from them), read from the markers and error-bar caps of the black curve of Lee et al. 2026 (the drawn curve is a smooth line through the 4 bins; it is not extracted). Bins are 0.315 dex wide; error bars are Poisson counting errors, and where the lower bar runs off the axis (one or few galaxies) the lower limit is absent. The paper does not state how the galaxy stellar mass of the GSMF is defined; for the stellar mass-halo mass relation it defines it as the total stellar mass bound to the galaxy as found by PGalF, and it says the massive end depends on the definition. The Schechter fits of McLeod+21, Davidzon+17 and Ilbert+13 are not extracted."},"definitions":{"imf":"kroupa01","cosmology":{"H0":67.4,"Om":0.315},"massDefinition":"unspecified","densityFrame":"comoving","population":"all galaxies (PGalF)"},"provenance":{"tier":"digitized-figure","citation":"Lee et al. 2026 (The DARWIN Project; arXiv:2610.25786, submitted to ApJ), Fig. 7 (galaxy stellar mass functions)","doi":"10.48550/arXiv.2610.25786","url":"https://arxiv.org/abs/2610.25786","retrieved":"2026-10-23","figure":"Fig. 7 (galaxy stellar mass functions)","panel":"DARWIN-1 binned GSMF at z = 5 (black curve with Poisson error bars)","checksumSha256":"b8e9e32bba3b8481c123c3257cfc9f608a8ba80d439ad8ccfb9e3cdeac1780d2","sourceMember":"figures/gsmf.pdf","extractionMethod":"vector path vertices from the figure PDF (PyMuPDF get_drawings), transformed through axes calibrated on labelled tick marks","axisCalibrationPixels":"x: log axis (labelled ticks read as 10^9 to 10^12, equally spaced); y: log axis per panel (labelled ticks read as 10^-1 to 10^-5, minor ticks at log10 2 to 9); labels are outlined paths read from the rendered figure; checked against the printed box size (every bin's Poisson error bar must match the count implied by its value)","digitizationUncertaintyDex":0.01,"sourceTexSha256":"81efa70c506f72278f7afba3b7baffd1961d6b8522063d31f073b9c70db90c11"},"calibration":"prediction","rankable":false,"notes":"Vector-path extraction; exact to PDF coordinate precision, so uncertainty is the plotted line, not marker tracing."},{"id":"lee26.darwin1.gsmf.z3","source":"DARWIN","run":"DARWIN-1 (65.5 cMpc box)","kind":"simulation","relation":"gsmf","epoch":{"zRepresentative":3,"zNominal":3,"zMin":3,"zMax":3,"mode":"published-epoch","snapshot":null},"axes":{"xDefinition":"log10 total stellar mass","xUnit":"log10(Msun)","yDefinition":"log10 number density per dex of stellar mass (comoving)","yUnit":"log10(cMpc^-3 dex^-1)"},"domain":{"xMin":9.167,"xMax":11.5},"representation":{"type":"points","intervalKind":"uncertainty","connect":true,"points":[{"x":9.167,"y":-2.1405,"yHigh":-2.1239,"yLow":-2.157},{"x":9.5,"y":-2.4562,"yHigh":-2.4329,"yLow":-2.4812},{"x":9.834,"y":-2.8075,"yHigh":-2.7737,"yLow":-2.8453},{"x":10.167,"y":-3.153,"yHigh":-3.1024,"yLow":-3.2102},{"x":10.5,"y":-3.7418,"yHigh":-3.6474,"yLow":-3.8623},{"x":10.833,"y":-4.2731,"yHigh":-4.1126,"yLow":-4.5309},{"x":11.5,"y":-4.9728,"yHigh":-4.6712}]},"scatter":null,"selection":{"population":"all galaxies of the box","warning":"Galaxy stellar mass function of the DARWIN-1 box at z = 3 (the panel label; the galaxy counts of the public catalogue snapshots at z = 5.015, 3.002, 1.002 and 0.2517 reproduce the bins of the four panels, see the records darwin1.catalogue.gsmf.* counted from them), read from the markers and error-bar caps of the black curve of Lee et al. 2026 (the drawn curve is a smooth line through the 7 bins; it is not extracted). Bins are 0.315 dex wide; error bars are Poisson counting errors, and where the lower bar runs off the axis (one or few galaxies) the lower limit is absent. The paper does not state how the galaxy stellar mass of the GSMF is defined; for the stellar mass-halo mass relation it defines it as the total stellar mass bound to the galaxy as found by PGalF, and it says the massive end depends on the definition. The Schechter fits of McLeod+21, Davidzon+17 and Ilbert+13 are not extracted."},"definitions":{"imf":"kroupa01","cosmology":{"H0":67.4,"Om":0.315},"massDefinition":"unspecified","densityFrame":"comoving","population":"all galaxies (PGalF)"},"provenance":{"tier":"digitized-figure","citation":"Lee et al. 2026 (The DARWIN Project; arXiv:2610.25786, submitted to ApJ), Fig. 7 (galaxy stellar mass functions)","doi":"10.48550/arXiv.2610.25786","url":"https://arxiv.org/abs/2610.25786","retrieved":"2026-10-23","figure":"Fig. 7 (galaxy stellar mass functions)","panel":"DARWIN-1 binned GSMF at z = 3 (black curve with Poisson error bars)","checksumSha256":"b8e9e32bba3b8481c123c3257cfc9f608a8ba80d439ad8ccfb9e3cdeac1780d2","sourceMember":"figures/gsmf.pdf","extractionMethod":"vector path vertices from the figure PDF (PyMuPDF get_drawings), transformed through axes calibrated on labelled tick marks","axisCalibrationPixels":"x: log axis (labelled ticks read as 10^9 to 10^12, equally spaced); y: log axis per panel (labelled ticks read as 10^-1 to 10^-5, minor ticks at log10 2 to 9); labels are outlined paths read from the rendered figure; checked against the printed box size (every bin's Poisson error bar must match the count implied by its value)","digitizationUncertaintyDex":0.01,"sourceTexSha256":"81efa70c506f72278f7afba3b7baffd1961d6b8522063d31f073b9c70db90c11"},"calibration":"prediction","rankable":false,"notes":"Vector-path extraction; exact to PDF coordinate precision, so uncertainty is the plotted line, not marker tracing."},{"id":"lee26.darwin1.gsmf.z1","source":"DARWIN","run":"DARWIN-1 (65.5 cMpc box)","kind":"simulation","relation":"gsmf","epoch":{"zRepresentative":1,"zNominal":1,"zMin":1,"zMax":1,"mode":"published-epoch","snapshot":null},"axes":{"xDefinition":"log10 total stellar mass","xUnit":"log10(Msun)","yDefinition":"log10 number density per dex of stellar mass (comoving)","yUnit":"log10(cMpc^-3 dex^-1)"},"domain":{"xMin":9.167,"xMax":12.167},"representation":{"type":"points","intervalKind":"uncertainty","connect":true,"points":[{"x":9.167,"y":-1.5908,"yHigh":-1.5818,"yLow":-1.5999},{"x":9.5,"y":-1.8086,"yHigh":-1.7982,"yLow":-1.8208},{"x":9.834,"y":-2.0884,"yHigh":-2.0734,"yLow":-2.1043},{"x":10.167,"y":-2.3379,"yHigh":-2.3176,"yLow":-2.3591},{"x":10.5,"y":-2.7097,"yHigh":-2.6787,"yLow":-2.7435},{"x":10.833,"y":-2.923,"yHigh":-2.8838,"yLow":-2.9659},{"x":11.167,"y":-3.2817,"yHigh":-3.2245,"yLow":-3.3489},{"x":11.5,"y":-3.7681,"yHigh":-3.6715,"yLow":-3.8932},{"x":11.834,"y":-4.9726,"yHigh":-4.6712},{"x":12.167,"y":-4.9726,"yHigh":-4.6712}]},"scatter":null,"selection":{"population":"all galaxies of the box","warning":"Galaxy stellar mass function of the DARWIN-1 box at z = 1 (the panel label; the galaxy counts of the public catalogue snapshots at z = 5.015, 3.002, 1.002 and 0.2517 reproduce the bins of the four panels, see the records darwin1.catalogue.gsmf.* counted from them), read from the markers and error-bar caps of the black curve of Lee et al. 2026 (the drawn curve is a smooth line through the 10 bins; it is not extracted). Bins are 0.315 dex wide; error bars are Poisson counting errors, and where the lower bar runs off the axis (one or few galaxies) the lower limit is absent. The paper does not state how the galaxy stellar mass of the GSMF is defined; for the stellar mass-halo mass relation it defines it as the total stellar mass bound to the galaxy as found by PGalF, and it says the massive end depends on the definition. The Schechter fits of McLeod+21, Davidzon+17 and Ilbert+13 are not extracted."},"definitions":{"imf":"kroupa01","cosmology":{"H0":67.4,"Om":0.315},"massDefinition":"unspecified","densityFrame":"comoving","population":"all galaxies (PGalF)"},"provenance":{"tier":"digitized-figure","citation":"Lee et al. 2026 (The DARWIN Project; arXiv:2610.25786, submitted to ApJ), Fig. 7 (galaxy stellar mass functions)","doi":"10.48550/arXiv.2610.25786","url":"https://arxiv.org/abs/2610.25786","retrieved":"2026-10-23","figure":"Fig. 7 (galaxy stellar mass functions)","panel":"DARWIN-1 binned GSMF at z = 1 (black curve with Poisson error bars)","checksumSha256":"b8e9e32bba3b8481c123c3257cfc9f608a8ba80d439ad8ccfb9e3cdeac1780d2","sourceMember":"figures/gsmf.pdf","extractionMethod":"vector path vertices from the figure PDF (PyMuPDF get_drawings), transformed through axes calibrated on labelled tick marks","axisCalibrationPixels":"x: log axis (labelled ticks read as 10^9 to 10^12, equally spaced); y: log axis per panel (labelled ticks read as 10^-1 to 10^-5, minor ticks at log10 2 to 9); labels are outlined paths read from the rendered figure; checked against the printed box size (every bin's Poisson error bar must match the count implied by its value)","digitizationUncertaintyDex":0.01,"sourceTexSha256":"81efa70c506f72278f7afba3b7baffd1961d6b8522063d31f073b9c70db90c11"},"calibration":"prediction","rankable":false,"notes":"Vector-path extraction; exact to PDF coordinate precision, so uncertainty is the plotted line, not marker tracing."},{"id":"lee26.darwin1.gsmf.z0.25","source":"DARWIN","run":"DARWIN-1 (65.5 cMpc box)","kind":"simulation","relation":"gsmf","epoch":{"zRepresentative":0.25,"zNominal":0.25,"zMin":0.25,"zMax":0.25,"mode":"published-epoch","snapshot":null},"axes":{"xDefinition":"log10 total stellar mass","xUnit":"log10(Msun)","yDefinition":"log10 number density per dex of stellar mass (comoving)","yUnit":"log10(cMpc^-3 dex^-1)"},"domain":{"xMin":9.167,"xMax":12.167},"representation":{"type":"points","intervalKind":"uncertainty","connect":true,"points":[{"x":9.167,"y":-1.5342,"yHigh":-1.5261,"yLow":-1.5426},{"x":9.5,"y":-1.7055,"yHigh":-1.6957,"yLow":-1.716},{"x":9.834,"y":-1.9459,"yHigh":-1.9324,"yLow":-1.9595},{"x":10.167,"y":-2.2196,"yHigh":-2.2015,"yLow":-2.2385},{"x":10.5,"y":-2.5158,"yHigh":-2.491,"yLow":-2.5423},{"x":10.833,"y":-2.7517,"yHigh":-2.7194,"yLow":-2.7873},{"x":11.167,"y":-3.0232,"yHigh":-2.9795,"yLow":-3.0715},{"x":11.5,"y":-3.3812,"yHigh":-3.3165,"yLow":-3.4567},{"x":11.834,"y":-3.9724,"yHigh":-3.8532,"yLow":-4.1374},{"x":12.167,"y":-4.9726,"yHigh":-4.6712}]},"scatter":null,"selection":{"population":"all galaxies of the box","warning":"Galaxy stellar mass function of the DARWIN-1 box at z = 0.25 (the panel label; the galaxy counts of the public catalogue snapshots at z = 5.015, 3.002, 1.002 and 0.2517 reproduce the bins of the four panels, see the records darwin1.catalogue.gsmf.* counted from them), read from the markers and error-bar caps of the black curve of Lee et al. 2026 (the drawn curve is a smooth line through the 10 bins; it is not extracted). Bins are 0.315 dex wide; error bars are Poisson counting errors, and where the lower bar runs off the axis (one or few galaxies) the lower limit is absent. The paper does not state how the galaxy stellar mass of the GSMF is defined; for the stellar mass-halo mass relation it defines it as the total stellar mass bound to the galaxy as found by PGalF, and it says the massive end depends on the definition. The Schechter fits of McLeod+21, Davidzon+17 and Ilbert+13 are not extracted."},"definitions":{"imf":"kroupa01","cosmology":{"H0":67.4,"Om":0.315},"massDefinition":"unspecified","densityFrame":"comoving","population":"all galaxies (PGalF)"},"provenance":{"tier":"digitized-figure","citation":"Lee et al. 2026 (The DARWIN Project; arXiv:2610.25786, submitted to ApJ), Fig. 7 (galaxy stellar mass functions)","doi":"10.48550/arXiv.2610.25786","url":"https://arxiv.org/abs/2610.25786","retrieved":"2026-10-23","figure":"Fig. 7 (galaxy stellar mass functions)","panel":"DARWIN-1 binned GSMF at z = 0.25 (black curve with Poisson error bars)","checksumSha256":"b8e9e32bba3b8481c123c3257cfc9f608a8ba80d439ad8ccfb9e3cdeac1780d2","sourceMember":"figures/gsmf.pdf","extractionMethod":"vector path vertices from the figure PDF (PyMuPDF get_drawings), transformed through axes calibrated on labelled tick marks","axisCalibrationPixels":"x: log axis (labelled ticks read as 10^9 to 10^12, equally spaced); y: log axis per panel (labelled ticks read as 10^-1 to 10^-5, minor ticks at log10 2 to 9); labels are outlined paths read from the rendered figure; checked against the printed box size (every bin's Poisson error bar must match the count implied by its value)","digitizationUncertaintyDex":0.01,"sourceTexSha256":"81efa70c506f72278f7afba3b7baffd1961d6b8522063d31f073b9c70db90c11"},"calibration":"prediction","rankable":false,"notes":"Vector-path extraction; exact to PDF coordinate precision, so uncertainty is the plotted line, not marker tracing."},{"id":"lee26.darwin1.size.z4.5","source":"DARWIN","run":"DARWIN-1 (65.5 cMpc box)","kind":"simulation","relation":"size","epoch":{"zRepresentative":4.5,"zNominal":4.5,"zMin":4.5,"zMax":4.5,"mode":"published-epoch","snapshot":null},"axes":{"xDefinition":"log10 total stellar mass","xUnit":"log10(Msun)","yDefinition":"log10 projected stellar half-mass radius R_1/2 (2D, galaxies projected on the XY plane of the box)","yUnit":"log10(kpc)"},"domain":{"xMin":7.1,"xMax":9.9},"representation":{"type":"points","intervalKind":"scatter","connect":true,"points":[{"x":7.1,"y":0.0656,"yLow":-0.1007,"yHigh":0.2803},{"x":7.3,"y":0.1247,"yLow":-0.0476,"yHigh":0.3493},{"x":7.5,"y":0.1843,"yLow":0.0043,"yHigh":0.4132},{"x":7.7,"y":0.2259,"yLow":0.0399,"yHigh":0.4329},{"x":7.9,"y":0.2499,"yLow":0.0737,"yHigh":0.4457},{"x":8.1,"y":0.2889,"yLow":0.1543,"yHigh":0.4646},{"x":8.3,"y":0.3536,"yLow":0.2224,"yHigh":0.4963},{"x":8.5,"y":0.3952,"yLow":0.2777,"yHigh":0.5276},{"x":8.7,"y":0.447,"yLow":0.3326,"yHigh":0.5833},{"x":8.9,"y":0.4804,"yLow":0.3506,"yHigh":0.606},{"x":9.1,"y":0.4783,"yLow":0.3909,"yHigh":0.6129},{"x":9.3,"y":0.5134,"yLow":0.4239,"yHigh":0.6523},{"x":9.5,"y":0.5636,"yLow":0.4586,"yHigh":0.6759},{"x":9.7,"y":0.5554,"yLow":0.4809,"yHigh":0.678},{"x":9.9,"y":0.5284,"yLow":0.4252,"yHigh":0.7042}]},"scatter":null,"selection":{"population":"all galaxies of the box","warning":"Projected stellar half-mass radius against total stellar mass for DARWIN-1 galaxies at z = 4.5: the median (solid grey) with the 16th and 84th percentiles (dashed grey), read from the vector paths of Lee et al. 2026; the three curves share their mass grid. Galaxies are projected on the XY plane of the box. The DARWIN-1 resolution limit is 500 pc (log R = -0.3, dotted line); sizes below a few resolution elements are not reliable (the paper says the low-mass sizes are probably resolution-limited and larger than observed). The observed relations drawn in the figure are not extracted; the observed radii are luminosity-weighted, the simulated ones mass-weighted. The text quotes an offset of roughly 0.3 dex above the observed relation of Miller+25; the extracted median lies 0.44 dex above that line averaged over their overlap."},"definitions":{"imf":"kroupa01","cosmology":{"H0":67.4,"Om":0.315},"massDefinition":"total-galaxy-finder","population":"all galaxies (PGalF)","sizeDefinition":"stellar-half-mass-projected"},"provenance":{"tier":"digitized-figure","citation":"Lee et al. 2026 (The DARWIN Project; arXiv:2610.25786, submitted to ApJ), Fig. 8 (mass-size relation)","doi":"10.48550/arXiv.2610.25786","url":"https://arxiv.org/abs/2610.25786","retrieved":"2026-10-23","figure":"Fig. 8 (mass-size relation)","panel":"DARWIN-1 median (solid grey) and 16th-84th percentiles (dashed), z = 4.5","checksumSha256":"25f907212423e40a8883dceb0dc16e02e4af9e7fcd5cd692179211980a27207e","sourceMember":"figures/mgal_size.pdf","extractionMethod":"vector path vertices from the figure PDF (PyMuPDF get_drawings), transformed through axes calibrated on labelled tick 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Checks: Phi_obs recomputed from the printed numbers, volumes and bin widths to 0.005 dex; the paper's Schechter fit (log phi* = -2.55, log L* = 41.79, alpha = -1.6 fixed) reproduces the points to rms 1.83 times the printed error (largest 2.8); the infinite integral of that fit, log rho_L = 39.59, equals the 39.58 printed in the table."},{"id":"khostovan15.hizels.elf.hbeta-oiii.z1.42","source":"Khostovan et al. 2015 (HiZELS)","run":"H-beta+[OIII] luminosity function, binned (Phi_final: completeness and filter-profile corrected; not corrected for dust or AGN)","kind":"observation","relation":"elf","epoch":{"zRepresentative":1.42,"zNominal":1.42,"zMin":1.41,"zMax":1.43,"mode":"observational-bin","snapshot":null},"axes":{"xDefinition":"log10 luminosity of the H-beta+[OIII] emission of narrow-band selected emitters, not corrected for dust or AGN contribution","xUnit":"log10(erg s^-1)","yDefinition":"log10 comoving number density of emitters per dex of luminosity (the paper's Phi_final: corrected for completeness and for the filter profile)","yUnit":"log10(Mpc^-3 dex^-1)"},"domain":{"xMin":41.95,"xMax":42.85},"representation":{"type":"points","intervalKind":"uncertainty","connect":true,"points":[{"x":41.95,"y":-2.49,"yLow":-2.52,"yHigh":-2.46},{"x":42.25,"y":-3.14,"yLow":-3.21,"yHigh":-3.07},{"x":42.55,"y":-3.89,"yLow":-4.08,"yHigh":-3.7},{"x":42.85,"y":-4.64,"yLow":-5.12,"yHigh":-4.16}]},"scatter":null,"selection":{"population":"narrow-band selected emitters (colour-colour, photometric and spectroscopic redshift selection), COSMOS and UDS fields","warning":"Luminosities are not corrected for dust extinction or for AGN contribution (the paper states so). 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Checks: Phi_obs recomputed from the printed numbers, volumes and bin widths to 0.005 dex; the paper's Schechter fit (log phi* = -2.61, log L* = 42.06, alpha = -1.6 fixed) reproduces the points to rms 1.19 times the printed error (largest 1.6); the infinite integral of that fit, log rho_L = 39.80, equals the 39.8 printed in the table."},{"id":"khostovan15.hizels.elf.hbeta-oiii.z2.23","source":"Khostovan et al. 2015 (HiZELS)","run":"H-beta+[OIII] luminosity function, binned (Phi_final: completeness and filter-profile corrected; not corrected for dust or AGN)","kind":"observation","relation":"elf","epoch":{"zRepresentative":2.23,"zNominal":2.23,"zMin":2.21,"zMax":2.25,"mode":"observational-bin","snapshot":null},"axes":{"xDefinition":"log10 luminosity of the H-beta+[OIII] emission of narrow-band selected emitters, not corrected for dust or AGN contribution","xUnit":"log10(erg s^-1)","yDefinition":"log10 comoving number density of emitters per dex of luminosity (the paper's Phi_final: corrected for completeness and for the filter profile)","yUnit":"log10(Mpc^-3 dex^-1)"},"domain":{"xMin":42.6,"xMax":43.05},"representation":{"type":"points","intervalKind":"uncertainty","connect":true,"points":[{"x":42.6,"y":-3.08,"yLow":-3.14,"yHigh":-3.02},{"x":42.75,"y":-3.14,"yLow":-3.21,"yHigh":-3.07},{"x":42.9,"y":-3.65,"yLow":-3.78,"yHigh":-3.52},{"x":43.05,"y":-4.26,"yLow":-4.55,"yHigh":-3.97}]},"scatter":null,"selection":{"population":"narrow-band selected emitters (colour-colour, photometric and spectroscopic redshift selection), COSMOS and UDS fields","warning":"Luminosities are not corrected for dust extinction or for AGN contribution (the paper states so). 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Checks: Phi_obs recomputed from the printed numbers, volumes and bin widths to 0.004 dex; the paper's Schechter fit (log phi* = -3.03, log L* = 42.66, alpha = -1.6 fixed) reproduces the points to rms 1.18 times the printed error (largest 1.7); the infinite integral of that fit, log rho_L = 39.98, equals the 39.98 printed in the table."},{"id":"khostovan15.hizels.elf.hbeta-oiii.z3.24","source":"Khostovan et al. 2015 (HiZELS)","run":"H-beta+[OIII] luminosity function, binned (Phi_final: completeness and filter-profile corrected; not corrected for dust or AGN)","kind":"observation","relation":"elf","epoch":{"zRepresentative":3.24,"zNominal":3.24,"zMin":3.22,"zMax":3.26,"mode":"observational-bin","snapshot":null},"axes":{"xDefinition":"log10 luminosity of the H-beta+[OIII] emission of narrow-band selected emitters, not corrected for dust or AGN contribution","xUnit":"log10(erg s^-1)","yDefinition":"log10 comoving number density of emitters per dex of luminosity (the paper's Phi_final: corrected for completeness and for the filter profile)","yUnit":"log10(Mpc^-3 dex^-1)"},"domain":{"xMin":42.65,"xMax":43.1},"representation":{"type":"points","intervalKind":"uncertainty","connect":true,"points":[{"x":42.65,"y":-3.17,"yLow":-3.24,"yHigh":-3.1},{"x":42.8,"y":-3.26,"yLow":-3.35,"yHigh":-3.17},{"x":42.95,"y":-3.55,"yLow":-3.68,"yHigh":-3.42},{"x":43.1,"y":-4.17,"yLow":-4.44,"yHigh":-3.9}]},"scatter":null,"selection":{"population":"narrow-band selected emitters (colour-colour, photometric and spectroscopic redshift selection), COSMOS and UDS fields","warning":"Luminosities are not corrected for dust extinction or for AGN contribution (the paper states so). 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Checks: Phi_obs recomputed from the printed numbers, volumes and bin widths to 0.002 dex; the paper's Schechter fit (log phi* = -3.31, log L* = 42.83, alpha = -1.6 fixed) reproduces the points to rms 0.72 times the printed error (largest 0.9); the infinite integral of that fit, log rho_L = 39.87, equals the 39.87 printed in the table."},{"id":"khostovan15.hizels.elf.oii.z1.47","source":"Khostovan et al. 2015 (HiZELS)","run":"[OII] luminosity function, binned (Phi_final: completeness and filter-profile corrected; not corrected for dust or AGN)","kind":"observation","relation":"elf","epoch":{"zRepresentative":1.47,"zNominal":1.47,"zMin":1.45,"zMax":1.49,"mode":"observational-bin","snapshot":null},"axes":{"xDefinition":"log10 luminosity of the [OII] emission of narrow-band selected emitters, not corrected for dust or AGN contribution","xUnit":"log10(erg s^-1)","yDefinition":"log10 comoving number density of emitters per dex of luminosity (the paper's Phi_final: corrected for completeness and for the filter profile)","yUnit":"log10(Mpc^-3 dex^-1)"},"domain":{"xMin":41.65,"xMax":42.55},"representation":{"type":"points","intervalKind":"uncertainty","connect":true,"points":[{"x":41.65,"y":-2.08,"yLow":-2.1,"yHigh":-2.06},{"x":41.8,"y":-2.28,"yLow":-2.31,"yHigh":-2.25},{"x":41.95,"y":-2.46,"yLow":-2.5,"yHigh":-2.42},{"x":42.1,"y":-2.69,"yLow":-2.75,"yHigh":-2.63},{"x":42.25,"y":-3.05,"yLow":-3.15,"yHigh":-2.95},{"x":42.4,"y":-3.55,"yLow":-3.7,"yHigh":-3.4},{"x":42.55,"y":-4.23,"yLow":-4.51,"yHigh":-3.95}]},"scatter":null,"selection":{"population":"narrow-band selected emitters (colour-colour, photometric and spectroscopic redshift selection), COSMOS and UDS fields","warning":"Luminosities are not corrected for dust extinction or for AGN contribution (the paper states so). 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The [OII] doublet is measured through a narrow band; the paper does not say how the two lines are combined. The faint-end slope of the Schechter fit is fixed, not fitted. The sample also holds galaxies mis-identified in redshift (the paper estimates the contamination, mostly H-alpha emitters). The bins sit at the bright end only (three bins); the luminosity function is poorly constrained at this epoch."},"definitions":{"line":"[OII] 3727","dustCorrection":"attenuated","dustCorrectionMethod":"none (not corrected for dust extinction or for AGN contribution)","densityFrame":"comoving","apertureDefinition":"unspecified","cosmology":{"H0":70,"Om":0.3},"population":"narrow-band selected emitters, star-forming galaxies and AGN not separated (COSMOS and UDS)"},"provenance":{"tier":"published-table","citation":"Khostovan et al. 2015, MNRAS 452, 1184 (arXiv:1503.00004), tables of the [OII] luminosity function","doi":"10.1093/mnras/stv1360","url":"https://arxiv.org/abs/1503.00004","retrieved":"2026-10-25","sourceMember":"oii_lf.tex","sourceSha256":"5fa7e020e44e319c21ae82b8547d88dd726ee7914e83e9a9993e3f05d4e1a849","quotes":{"dust":"oii_lf.tex:315","dust_statement":"oii_lf.tex:315","blend":["oii_lf.tex:139","oii_lf.tex:139"],"cosmology":"oii_lf.tex:145","comoving_volume":"oii_lf.tex:286","estimator":"oii_lf.tex:263","alpha_fixed":"oii_lf.tex:313","errors":"oii_lf.tex:662","selection":"oii_lf.tex:244"},"definitionBasis":"line: 'we present the results as the combined measurement of H-beta' (with [OIII]); the [OII] line is called [OII] 3727 in the paper's table of filters, and the text does not say that it is the blend of the doublet. imf: the paper assumes a Salpeter IMF for star formation rates, which does not enter a luminosity function. apertureDefinition: not stated in this paper."},"calibration":"validation","rankable":true,"notes":"Binned luminosity function transcribed from the paper's table (3 bins, 21 of 35 selected emitters). Checks: Phi_obs recomputed from the printed numbers, volumes and bin widths to 0.000 dex; the paper's Schechter fit (log phi* = -3.07, log L* = 42.69, alpha = -1.3 fixed) reproduces the points to rms 0.53 times the printed error (largest 0.7); the infinite integral of that fit, log rho_L = 39.73, equals the 39.74 printed in the table. The printed half widths of the second and third bins (0.075 and 0.075) do not reproduce the printed Phi_obs; the widths that do are 0.10, 0.10 and 0.20 dex, which tile the printed bin centres exactly (a misprint of the half widths in the table, not read further; the bin centres used here are not affected)."},{"id":"khostovan15.hizels.elf.oii.z4.69","source":"Khostovan et al. 2015 (HiZELS)","run":"[OII] luminosity function, binned (Phi_final: completeness and filter-profile corrected; not corrected for dust or AGN)","kind":"observation","relation":"elf","epoch":{"zRepresentative":4.69,"zNominal":4.69,"zMin":4.66,"zMax":4.72,"mode":"observational-bin","snapshot":null},"axes":{"xDefinition":"log10 luminosity of the [OII] emission of narrow-band selected emitters, not corrected for dust or AGN contribution","xUnit":"log10(erg s^-1)","yDefinition":"log10 comoving number density of emitters per dex of luminosity (the paper's Phi_final: corrected for completeness and for the filter profile)","yUnit":"log10(Mpc^-3 dex^-1)"},"domain":{"xMin":42.86,"xMax":43.16},"representation":{"type":"points","intervalKind":"uncertainty","connect":true,"points":[{"x":42.86,"y":-3.66,"yLow":-3.75,"yHigh":-3.57},{"x":43.01,"y":-3.93,"yLow":-4.06,"yHigh":-3.8},{"x":43.16,"y":-4.11,"yLow":-4.27,"yHigh":-3.95}]},"scatter":null,"selection":{"population":"narrow-band selected emitters (colour-colour, photometric and spectroscopic redshift selection), COSMOS and UDS fields","warning":"Luminosities are not corrected for dust extinction or for AGN contribution (the paper states so). The [OII] doublet is measured through a narrow band; the paper does not say how the two lines are combined. The faint-end slope of the Schechter fit is fixed, not fitted. The sample also holds galaxies mis-identified in redshift (the paper estimates the contamination, mostly H-alpha emitters). The bins sit at the bright end only (three bins); the luminosity function is poorly constrained at this epoch."},"definitions":{"line":"[OII] 3727","dustCorrection":"attenuated","dustCorrectionMethod":"none (not corrected for dust extinction or for AGN contribution)","densityFrame":"comoving","apertureDefinition":"unspecified","cosmology":{"H0":70,"Om":0.3},"population":"narrow-band selected emitters, star-forming galaxies and AGN not separated (COSMOS and UDS)"},"provenance":{"tier":"published-table","citation":"Khostovan et al. 2015, MNRAS 452, 1184 (arXiv:1503.00004), tables of the [OII] luminosity function","doi":"10.1093/mnras/stv1360","url":"https://arxiv.org/abs/1503.00004","retrieved":"2026-10-25","sourceMember":"oii_lf.tex","sourceSha256":"5fa7e020e44e319c21ae82b8547d88dd726ee7914e83e9a9993e3f05d4e1a849","quotes":{"dust":"oii_lf.tex:315","dust_statement":"oii_lf.tex:315","blend":["oii_lf.tex:139","oii_lf.tex:139"],"cosmology":"oii_lf.tex:145","comoving_volume":"oii_lf.tex:286","estimator":"oii_lf.tex:263","alpha_fixed":"oii_lf.tex:313","errors":"oii_lf.tex:662","selection":"oii_lf.tex:244"},"definitionBasis":"line: 'we present the results as the combined measurement of H-beta' (with [OIII]); the [OII] line is called [OII] 3727 in the paper's table of filters, and the text does not say that it is the blend of the doublet. imf: the paper assumes a Salpeter IMF for star formation rates, which does not enter a luminosity function. apertureDefinition: not stated in this paper."},"calibration":"validation","rankable":true,"notes":"Binned luminosity function transcribed from the paper's table (3 bins, 17 of 18 selected emitters). Checks: Phi_obs recomputed from the printed numbers, volumes and bin widths to 0.004 dex; the paper's Schechter fit (log phi* = -3.69, log L* = 42.93, alpha = -1.3 fixed) reproduces the points to rms 0.28 times the printed error (largest 0.4); the infinite integral of that fit, log rho_L = 39.35, equals the 39.35 printed in the table."},{"id":"sobral13.hizels.elf.halpha.z0.4","source":"Sobral et al. 2013 (HiZELS)","run":"H-alpha luminosity function, binned (Table 4, corrected phi)","kind":"observation","relation":"elf","epoch":{"zRepresentative":0.4,"zNominal":0.4,"zMin":0.391,"zMax":0.411,"mode":"observational-bin","snapshot":null},"axes":{"xDefinition":"log10 H-alpha line luminosity, corrected for [NII] contamination and for dust extinction (A(Halpha) = 1 mag)","xUnit":"log10(erg s^-1)","yDefinition":"log10 comoving number density of H-alpha emitters per dex of luminosity (the paper's phi corr: corrected for incompleteness and for the filter profile)","yUnit":"log10(Mpc^-3 dex^-1)"},"domain":{"xMin":40.5,"xMax":42.5},"representation":{"type":"points","intervalKind":"uncertainty","connect":true,"points":[{"x":40.5,"y":-1.66,"yLow":-1.7,"yHigh":-1.62},{"x":40.6,"y":-1.7,"yLow":-1.74,"yHigh":-1.66},{"x":40.7,"y":-1.81,"yLow":-1.85,"yHigh":-1.77},{"x":40.8,"y":-1.93,"yLow":-1.98,"yHigh":-1.88},{"x":40.9,"y":-1.96,"yLow":-2.03,"yHigh":-1.89},{"x":41,"y":-2.03,"yLow":-2.1,"yHigh":-1.96},{"x":41.1,"y":-2.12,"yLow":-2.21,"yHigh":-2.03},{"x":41.2,"y":-2.27,"yLow":-2.35,"yHigh":-2.19},{"x":41.3,"y":-2.29,"yLow":-2.38,"yHigh":-2.2},{"x":41.4,"y":-2.42,"yLow":-2.52,"yHigh":-2.32},{"x":41.5,"y":-2.46,"yLow":-2.57,"yHigh":-2.35},{"x":41.6,"y":-2.57,"yLow":-2.7,"yHigh":-2.44},{"x":41.7,"y":-2.69,"yLow":-2.88,"yHigh":-2.5},{"x":41.8,"y":-2.73,"yLow":-2.9,"yHigh":-2.56},{"x":41.9,"y":-2.88,"yLow":-3.08,"yHigh":-2.68},{"x":42,"y":-3.03,"yLow":-3.38,"yHigh":-2.68},{"x":42.2,"y":-3.56,"yLow":-4.07,"yHigh":-3.05},{"x":42.5,"y":-3.71,"yLow":-4.42,"yHigh":-3}]},"scatter":null,"selection":{"population":"narrow-band selected H-alpha emitters (rest-frame EW(Halpha+[NII]) > 25 A), COSMOS and UDS fields","warning":"Luminosities carry a constant A(Halpha) = 1 mag for every galaxy and a statistical [NII] correction (median [NII]/(Halpha+[NII]) about 0.25), not a measurement per galaxy; the paper notes the bright end deviates from a Schechter function where AGN dominate, and the points are not AGN-corrected. Errors are Poisson plus 20 per cent of the completeness correction."},"definitions":{"line":"H-alpha (without [NII])","dustCorrection":"intrinsic","dustCorrectionMethod":"constant A(Halpha) = 1 mag applied to every galaxy","densityFrame":"comoving","apertureDefinition":"fixed 3 arcsec diameter aperture at z = 0.4 (about 16 kpc, the same physical area as 2 arcsec at higher redshift)","cosmology":{"H0":70,"Om":0.3},"population":"narrow-band selected H-alpha emitters, EW(Halpha+[NII]) > 25 A rest frame (star-forming galaxies and AGN)"},"provenance":{"tier":"published-table","citation":"Sobral et al. 2013, MNRAS 428, 1128 (arXiv:1202.3436), Table 4","doi":"10.1093/mnras/sts096","url":"https://arxiv.org/abs/1202.3436","retrieved":"2026-10-23","sourceMember":"FAINT_END_C_VARIANCE.tex","sourceArchiveSha256":"d9542ddbc0c42dbb6d3d3d8d350db74a4e553a921a2c757cc6a9751225c79748","quotes":{"line_and_dust":"FAINT_END_C_VARIANCE.tex:437","nii":"FAINT_END_C_VARIANCE.tex:348","dust_constant":"FAINT_END_C_VARIANCE.tex:386","cosmology":"FAINT_END_C_VARIANCE.tex:159","aperture":["FAINT_END_C_VARIANCE.tex:168","FAINT_END_C_VARIANCE.tex:189"],"comoving":"FAINT_END_C_VARIANCE.tex:374","selection":"FAINT_END_C_VARIANCE.tex:235","errors":"FAINT_END_C_VARIANCE.tex:401"},"definitionBasis":"densityFrame is stated as '(co-moving)' for the NB_H volume (z = 1.47) in the volume section; the other epochs' volumes are computed in the same paragraph in the same way (read, not stated)"},"calibration":"validation","rankable":true,"notes":"Table 4 transcribed (18 bins, 797 sources of 1742 Halpha emitters in Table 3). Checks: the Table 5 Schechter fit (log L*=41.95, log phi*=-3.12, alpha=-1.75) reproduces the points to rms 0.90 times the printed error (rms 0.26 dex); at this epoch the printed Schechter parameters integrate to log rho_L(41.6) = 38.62, 0.37 dex below the 38.99 printed in Table 5, so that check is not used here (the paper does not say why; the points themselves agree with the printed fit); the points and the fit give the same luminosity density over the bins (log rho 39.25 and 39.11)."},{"id":"sobral13.hizels.elf.halpha.z0.84","source":"Sobral et al. 2013 (HiZELS)","run":"H-alpha luminosity function, binned (Table 4, corrected phi)","kind":"observation","relation":"elf","epoch":{"zRepresentative":0.84,"zNominal":0.84,"zMin":0.83,"zMax":0.86,"mode":"observational-bin","snapshot":null},"axes":{"xDefinition":"log10 H-alpha line luminosity, corrected for [NII] contamination and for dust extinction (A(Halpha) = 1 mag)","xUnit":"log10(erg s^-1)","yDefinition":"log10 comoving number density of H-alpha emitters per dex of luminosity (the paper's phi corr: corrected for incompleteness and for the filter profile)","yUnit":"log10(Mpc^-3 dex^-1)"},"domain":{"xMin":41.7,"xMax":42.9},"representation":{"type":"points","intervalKind":"uncertainty","connect":true,"points":[{"x":41.7,"y":-1.93,"yLow":-1.96,"yHigh":-1.9},{"x":41.85,"y":-2.02,"yLow":-2.05,"yHigh":-1.99},{"x":42,"y":-2.18,"yLow":-2.22,"yHigh":-2.14},{"x":42.15,"y":-2.43,"yLow":-2.49,"yHigh":-2.37},{"x":42.3,"y":-2.73,"yLow":-2.9,"yHigh":-2.56},{"x":42.45,"y":-3.01,"yLow":-3.18,"yHigh":-2.84},{"x":42.6,"y":-3.27,"yLow":-3.48,"yHigh":-3.06},{"x":42.75,"y":-3.79,"yLow":-4.34,"yHigh":-3.24},{"x":42.9,"y":-4.13,"yLow":-5.64,"yHigh":-2.62}]},"scatter":null,"selection":{"population":"narrow-band selected H-alpha emitters (rest-frame EW(Halpha+[NII]) > 25 A), COSMOS and UDS fields","warning":"Luminosities carry a constant A(Halpha) = 1 mag for every galaxy and a statistical [NII] correction (median [NII]/(Halpha+[NII]) about 0.25), not a measurement per galaxy; the paper notes the bright end deviates from a Schechter function where AGN dominate, and the points are not AGN-corrected. Errors are Poisson plus 20 per cent of the completeness correction."},"definitions":{"line":"H-alpha (without [NII])","dustCorrection":"intrinsic","dustCorrectionMethod":"constant A(Halpha) = 1 mag applied to every galaxy","densityFrame":"comoving","apertureDefinition":"fixed 2 arcsec diameter aperture (about 16 kpc); 3 arcsec at z = 0.4 to cover the same physical area","cosmology":{"H0":70,"Om":0.3},"population":"narrow-band selected H-alpha emitters, EW(Halpha+[NII]) > 25 A rest frame (star-forming galaxies and AGN)"},"provenance":{"tier":"published-table","citation":"Sobral et al. 2013, MNRAS 428, 1128 (arXiv:1202.3436), Table 4","doi":"10.1093/mnras/sts096","url":"https://arxiv.org/abs/1202.3436","retrieved":"2026-10-23","sourceMember":"FAINT_END_C_VARIANCE.tex","sourceArchiveSha256":"d9542ddbc0c42dbb6d3d3d8d350db74a4e553a921a2c757cc6a9751225c79748","quotes":{"line_and_dust":"FAINT_END_C_VARIANCE.tex:437","nii":"FAINT_END_C_VARIANCE.tex:348","dust_constant":"FAINT_END_C_VARIANCE.tex:386","cosmology":"FAINT_END_C_VARIANCE.tex:159","aperture":["FAINT_END_C_VARIANCE.tex:168","FAINT_END_C_VARIANCE.tex:189"],"comoving":"FAINT_END_C_VARIANCE.tex:374","selection":"FAINT_END_C_VARIANCE.tex:235","errors":"FAINT_END_C_VARIANCE.tex:401"},"definitionBasis":"densityFrame is stated as '(co-moving)' for the NB_H volume (z = 1.47) in the volume section; the other epochs' volumes are computed in the same paragraph in the same way (read, not stated)"},"calibration":"validation","rankable":true,"notes":"Table 4 transcribed (9 bins, 633 sources of 637 Halpha emitters in Table 3). Checks: the Table 5 Schechter fit (log L*=42.25, log phi*=-2.47, alpha=-1.56) reproduces the points to rms 0.61 times the printed error (rms 0.11 dex); the same fit integrated above 10^41.6 erg/s gives log rho_L = 39.74 against 39.75 printed in Table 5; the points and the fit give the same luminosity density over the bins (log rho 39.72 and 39.73)."},{"id":"sobral13.hizels.elf.halpha.z1.47","source":"Sobral et al. 2013 (HiZELS)","run":"H-alpha luminosity function, binned (Table 4, corrected phi)","kind":"observation","relation":"elf","epoch":{"zRepresentative":1.47,"zNominal":1.47,"zMin":1.45,"zMax":1.482,"mode":"observational-bin","snapshot":null},"axes":{"xDefinition":"log10 H-alpha line luminosity, corrected for [NII] contamination and for dust extinction (A(Halpha) = 1 mag)","xUnit":"log10(erg s^-1)","yDefinition":"log10 comoving number density of H-alpha emitters per dex of luminosity (the paper's phi corr: corrected for incompleteness and for the filter profile)","yUnit":"log10(Mpc^-3 dex^-1)"},"domain":{"xMin":42.1,"xMax":43.4},"representation":{"type":"points","intervalKind":"uncertainty","connect":true,"points":[{"x":42.1,"y":-2.13,"yLow":-2.23,"yHigh":-2.03},{"x":42.2,"y":-2.25,"yLow":-2.34,"yHigh":-2.16},{"x":42.3,"y":-2.34,"yLow":-2.4,"yHigh":-2.28},{"x":42.4,"y":-2.47,"yLow":-2.52,"yHigh":-2.42},{"x":42.5,"y":-2.62,"yLow":-2.67,"yHigh":-2.57},{"x":42.6,"y":-2.73,"yLow":-2.77,"yHigh":-2.69},{"x":42.7,"y":-2.91,"yLow":-2.99,"yHigh":-2.83},{"x":42.8,"y":-3.18,"yLow":-3.29,"yHigh":-3.07},{"x":42.9,"y":-3.55,"yLow":-3.73,"yHigh":-3.37},{"x":43,"y":-3.81,"yLow":-4.07,"yHigh":-3.55},{"x":43.1,"y":-4.22,"yLow":-4.6,"yHigh":-3.84},{"x":43.2,"y":-4.55,"yLow":-5.1,"yHigh":-4},{"x":43.4,"y":-4.86,"yLow":-5.41,"yHigh":-4.31}]},"scatter":null,"selection":{"population":"narrow-band selected H-alpha emitters (rest-frame EW(Halpha+[NII]) > 25 A), COSMOS and UDS fields","warning":"Luminosities carry a constant A(Halpha) = 1 mag for every galaxy and a statistical [NII] correction (median [NII]/(Halpha+[NII]) about 0.25), not a measurement per galaxy; the paper notes the bright end deviates from a Schechter function where AGN dominate, and the points are not AGN-corrected. Errors are Poisson plus 20 per cent of the completeness correction."},"definitions":{"line":"H-alpha (without [NII])","dustCorrection":"intrinsic","dustCorrectionMethod":"constant A(Halpha) = 1 mag applied to every galaxy","densityFrame":"comoving","apertureDefinition":"fixed 2 arcsec diameter aperture (about 16 kpc); 3 arcsec at z = 0.4 to cover the same physical area","cosmology":{"H0":70,"Om":0.3},"population":"narrow-band selected H-alpha emitters, EW(Halpha+[NII]) > 25 A rest frame (star-forming galaxies and AGN)"},"provenance":{"tier":"published-table","citation":"Sobral et al. 2013, MNRAS 428, 1128 (arXiv:1202.3436), Table 4","doi":"10.1093/mnras/sts096","url":"https://arxiv.org/abs/1202.3436","retrieved":"2026-10-23","sourceMember":"FAINT_END_C_VARIANCE.tex","sourceArchiveSha256":"d9542ddbc0c42dbb6d3d3d8d350db74a4e553a921a2c757cc6a9751225c79748","quotes":{"line_and_dust":"FAINT_END_C_VARIANCE.tex:437","nii":"FAINT_END_C_VARIANCE.tex:348","dust_constant":"FAINT_END_C_VARIANCE.tex:386","cosmology":"FAINT_END_C_VARIANCE.tex:159","aperture":["FAINT_END_C_VARIANCE.tex:168","FAINT_END_C_VARIANCE.tex:189"],"comoving":"FAINT_END_C_VARIANCE.tex:374","selection":"FAINT_END_C_VARIANCE.tex:235","errors":"FAINT_END_C_VARIANCE.tex:401"},"definitionBasis":"densityFrame is stated as '(co-moving)' for the NB_H volume (z = 1.47) in the volume section; the other epochs' volumes are computed in the same paragraph in the same way (read, not stated)"},"calibration":"validation","rankable":true,"notes":"Table 4 transcribed (13 bins, 499 sources of 515 Halpha emitters in Table 3). Checks: the Table 5 Schechter fit (log L*=42.56, log phi*=-2.61, alpha=-1.62) reproduces the points to rms 0.61 times the printed error (rms 0.26 dex); the same fit integrated above 10^41.6 erg/s gives log rho_L = 40.04 against 40.03 printed in Table 5; the points and the fit give the same luminosity density over the bins (log rho 39.83 and 39.84)."},{"id":"sobral13.hizels.elf.halpha.z2.23","source":"Sobral et al. 2013 (HiZELS)","run":"H-alpha luminosity function, binned (Table 4, corrected phi)","kind":"observation","relation":"elf","epoch":{"zRepresentative":2.23,"zNominal":2.23,"zMin":2.215,"zMax":2.247,"mode":"observational-bin","snapshot":null},"axes":{"xDefinition":"log10 H-alpha line luminosity, corrected for [NII] contamination and for dust extinction (A(Halpha) = 1 mag)","xUnit":"log10(erg s^-1)","yDefinition":"log10 comoving number density of H-alpha emitters per dex of luminosity (the paper's phi corr: corrected for incompleteness and for the filter profile)","yUnit":"log10(Mpc^-3 dex^-1)"},"domain":{"xMin":42,"xMax":43.6},"representation":{"type":"points","intervalKind":"uncertainty","connect":true,"points":[{"x":42,"y":-1.93,"yLow":-2.12,"yHigh":-1.74},{"x":42.15,"y":-2.07,"yLow":-2.23,"yHigh":-1.91},{"x":42.3,"y":-2.19,"yLow":-2.26,"yHigh":-2.12},{"x":42.4,"y":-2.31,"yLow":-2.36,"yHigh":-2.26},{"x":42.5,"y":-2.41,"yLow":-2.46,"yHigh":-2.36},{"x":42.6,"y":-2.5,"yLow":-2.54,"yHigh":-2.46},{"x":42.7,"y":-2.59,"yLow":-2.64,"yHigh":-2.54},{"x":42.8,"y":-2.73,"yLow":-2.79,"yHigh":-2.67},{"x":42.9,"y":-2.88,"yLow":-3.02,"yHigh":-2.74},{"x":43,"y":-3.09,"yLow":-3.26,"yHigh":-2.92},{"x":43.1,"y":-3.33,"yLow":-3.55,"yHigh":-3.11},{"x":43.2,"y":-3.67,"yLow":-3.98,"yHigh":-3.36},{"x":43.3,"y":-4.01,"yLow":-4.52,"yHigh":-3.5},{"x":43.4,"y":-4.22,"yLow":-4.9,"yHigh":-3.54},{"x":43.6,"y":-4.63,"yLow":-5.04,"yHigh":-4.22}]},"scatter":null,"selection":{"population":"narrow-band selected H-alpha emitters (rest-frame EW(Halpha+[NII]) > 25 A), COSMOS and UDS fields","warning":"Luminosities carry a constant A(Halpha) = 1 mag for every galaxy and a statistical [NII] correction (median [NII]/(Halpha+[NII]) about 0.25), not a measurement per galaxy; the paper notes the bright end deviates from a Schechter function where AGN dominate, and the points are not AGN-corrected. Errors are Poisson plus 20 per cent of the completeness correction."},"definitions":{"line":"H-alpha (without [NII])","dustCorrection":"intrinsic","dustCorrectionMethod":"constant A(Halpha) = 1 mag applied to every galaxy","densityFrame":"comoving","apertureDefinition":"fixed 2 arcsec diameter aperture (about 16 kpc); 3 arcsec at z = 0.4 to cover the same physical area","cosmology":{"H0":70,"Om":0.3},"population":"narrow-band selected H-alpha emitters, EW(Halpha+[NII]) > 25 A rest frame (star-forming galaxies and AGN)"},"provenance":{"tier":"published-table","citation":"Sobral et al. 2013, MNRAS 428, 1128 (arXiv:1202.3436), Table 4","doi":"10.1093/mnras/sts096","url":"https://arxiv.org/abs/1202.3436","retrieved":"2026-10-23","sourceMember":"FAINT_END_C_VARIANCE.tex","sourceArchiveSha256":"d9542ddbc0c42dbb6d3d3d8d350db74a4e553a921a2c757cc6a9751225c79748","quotes":{"line_and_dust":"FAINT_END_C_VARIANCE.tex:437","nii":"FAINT_END_C_VARIANCE.tex:348","dust_constant":"FAINT_END_C_VARIANCE.tex:386","cosmology":"FAINT_END_C_VARIANCE.tex:159","aperture":["FAINT_END_C_VARIANCE.tex:168","FAINT_END_C_VARIANCE.tex:189"],"comoving":"FAINT_END_C_VARIANCE.tex:374","selection":"FAINT_END_C_VARIANCE.tex:235","errors":"FAINT_END_C_VARIANCE.tex:401"},"definitionBasis":"densityFrame is stated as '(co-moving)' for the NB_H volume (z = 1.47) in the volume section; the other epochs' volumes are computed in the same paragraph in the same way (read, not stated)"},"calibration":"validation","rankable":true,"notes":"Table 4 transcribed (15 bins, 797 sources of 817 Halpha emitters in Table 3). 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The paper plots a third version, reddening-corrected with the Balmer decrement; it is not a record here."},"definitions":{"line":"H-alpha (without [NII])","imf":"kroupa01","dustCorrection":"intrinsic","dustCorrectionMethod":"none (line luminosity before dust)","densityFrame":"comoving","apertureDefinition":"all gas and stellar particles within the halo virial radius","cosmology":{"H0":67.11,"Om":0.3175},"population":"galaxies with SFR(10 Myr) >= 0.3 Msun/yr in the 20 cMpc box (the data-release selection)"},"provenance":{"tier":"catalog-derived","citation":"SPHINX20 public data release (Katz et al. 2023; Rosdahl et al. 2018, 2022); luminosity functions derived by sim-highline","doi":null,"url":"https://github.com/HarleyKatz/SPHINX-20-data","retrieved":"2026-10-23","compilation":"https://github.com/HarleyKatz/SPHINX-20-data @ 526ebb5c90294414fc7914200478c49a99c86fd2","sourceMember":"data/all_basic_data.csv","checksumSha256":"3379131d054752a4abd8248d86898117e20ed3da2ff0c30d5acbdf6c144d9e85","paper":"arXiv:2309.03269","definitionBasis":"imf: the paper's caveats paragraph says 'we have chosen a specific stellar IMF (Kroupa-like)'; it is filled as Kroupa (2001), the nearest entry of the vocabulary, by data/definition-fills.json, as for the other SPHINX20 records (an earlier version of this note said the paper gave no sentence on the IMF; it does). The IMF is not a comparison key of this relation. line: the release lists H I 6562.80 and [N II] 6548/6583 as separate lines.","quotes":{"box":"main.tex:119","cosmology":"main.tex:122","galaxy":"main.tex:124","selection":"main.tex:76","dust_model":"main.tex:197","line_columns":"main.tex:245","galaxies":"main.tex:203","plotted_function":"main.tex:613","turnover":"main.tex:613","sight_lines":"main.tex:620","ebv":"main.tex:253","imf":"main.tex:763"},"checkAgainstFigure":{"figure":"Line luminosity functions for Halpha (top)","checksumSha256":"7c0f3c16cc33dcc1cb9d2bca4eb01e0fe63200eb7747099d080861e19366c4d1","sourceMember":"figures/Halpha_lum_func.pdf","kHalpha":2.2,"rmsDex":0.015,"bins":250},"definitionFills":["katz23-sphinx20-imf"]},"calibration":"prediction","rankable":true,"notes":"RAMSES-RT radiation hydrodynamics of reionization in a 20 cMpc box. Volume (20 cMpc)^3 and bin width 0.25 dex (the check against the figure uses the paper's 0.5 dex bins). Checks: the release's columns reproduce the function the paper plots (reddening-corrected, ten sight lines) to 0.015 dex rms over 250 plotted bins (mean -0.004) with a fitted k(Halpha) = 2.2; the plotted function lies between the dust-attenuated and intrinsic functions in 106 bin-and-sight-line cases above the turnover. The fitted coefficient is used only in that check; no value in this record depends on it (the record counts galaxies by the release's own intrinsic or dust-attenuated column). Intrinsic Halpha is the release column HI_6562.8_int; attenuated is HI_6562.8_dir_0..9. 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The paper's table labels the sSFR split in Gyr^-1 while its text and caption use yr^-1 (log sSFR = -9.5): the text and caption were followed."},"definitions":{"muAlpha":0.22,"metallicityQuantity":"gas-O/H","metallicityCalibration":"Te-anchored-strong-line (Curti+17)","sfrTimescaleMyr":"unspecified","sfrIndicator":"Halpha extinction-corrected in the fibre (Kennicutt & Evans 2012 calibration), MPA-JHU aperture corrections to total SFR","imf":"chabrier03","massDefinition":"sed-total","population":"star-forming"},"provenance":{"tier":"published-fit","citation":"Curti et al. 2020, MNRAS 491, 944 (arXiv:1910.00597), Appendix A and its table of 2D projections of the FMR","doi":"10.1093/mnras/stz2910","url":"https://arxiv.org/abs/1910.00597","retrieved":"2026-10-18","sourceMember":"fmr_new_paper.tex","figureMember":"figures/fmr_proj_lowfinal_MCMC.pdf","figureSha256":"7e52c550b0358666d571a1dd00b58de2c116d1c895a9959c06c519d9dfe3bb2a","sourceArchiveSha256":"6c6089bd07d4a5c1466489c56f9c4570a191391535fd9ec86b8742ddb34cd1a4"},"calibration":"validation","rankable":true,"notes":"Parameters as published (Appendix A table). curti20.sdss.fmr.mu0.22.low-ssfr: drawn best-fit curve (50 vertices, x 8.64..11.52) minus transcribed expression: max |diff| = 0.0126 dex (rms 0.0071); ends: drawn 8.441,8.794 vs expression 8.429,8.793"},{"id":"curti20.sdss.fmr.mu0.65.high-ssfr","source":"Curti et al. 2020","run":"sSFR > 10^-9.5 yr^-1, alpha=0.65","kind":"observation","relation":"fmr","epoch":{"zRepresentative":0.027,"zMin":0.027,"zMax":0.027,"mode":"observational-bin","snapshot":null},"axes":{"xDefinition":"mu_0.65 = log10(M*/Msun) - 0.65 log10(SFR/(Msun/yr)); MPA-JHU total stellar mass, total (aperture-corrected) Halpha SFR","xUnit":"log10(Msun)","yDefinition":"12+log10(O/H), gas-phase, Te-anchored strong-line calibrations (Curti+17), median of M*-SFR bins","yUnit":"dex"},"domain":{"xMin":8.41,"xMax":10.33},"representation":{"type":"parametric","equation":"12+log(O/H) = Z0 - (gamma/beta) log10(1 + (10^mu / 10^mu0)^-beta), mu = mu_0.65; Z0=8.74, mu0=9.9, gamma=0.32, beta=5.0","expression":"Z0-(gamma/beta)*Math.log10(1+Math.pow(10,-beta*(x-mu0)))","parameters":{"Z0":8.74,"mu0":9.9,"gamma":0.32,"beta":5,"Z0Error":0.04,"mu0Error":0.1,"gammaError":0.01,"betaError":3}},"scatter":null,"selection":{"population":"star-forming SDSS galaxies with log sSFR > -9.5 (yr^-1) (SDSS DR7 MPA-JHU, BPT star-forming, z>0.027)","warning":"Fit to median metallicities in M*-SFR bins using the MZR functional form with mu_alpha in place of M*. The paper's main FMR is Z(M*, SFR) and is not stored. x range = extent of the best-fit curve drawn in the paper's figure (not stated in the text). The redshift upper limit of the sample is not stated in this paper, so the epoch block carries only the stated lower limit z>0.027. The paper's table labels the sSFR split in Gyr^-1 while its text and caption use yr^-1 (log sSFR = -9.5): the text and caption were followed."},"definitions":{"muAlpha":0.65,"metallicityQuantity":"gas-O/H","metallicityCalibration":"Te-anchored-strong-line (Curti+17)","sfrTimescaleMyr":"unspecified","sfrIndicator":"Halpha extinction-corrected in the fibre (Kennicutt & Evans 2012 calibration), MPA-JHU aperture corrections to total SFR","imf":"chabrier03","massDefinition":"sed-total","population":"star-forming"},"provenance":{"tier":"published-fit","citation":"Curti et al. 2020, MNRAS 491, 944 (arXiv:1910.00597), Appendix A and its table of 2D projections of the FMR","doi":"10.1093/mnras/stz2910","url":"https://arxiv.org/abs/1910.00597","retrieved":"2026-10-18","sourceMember":"fmr_new_paper.tex","figureMember":"figures/fmr_proj_highfinal_MCMC.pdf","figureSha256":"13fd97fba985b36d98c6823774002efaa7da0fa53a586a55d32ca82540a7231b","sourceArchiveSha256":"6c6089bd07d4a5c1466489c56f9c4570a191391535fd9ec86b8742ddb34cd1a4"},"calibration":"validation","rankable":true,"notes":"Parameters as published (Appendix A table). curti20.sdss.fmr.mu0.65.high-ssfr: drawn best-fit curve (50 vertices, x 8.41..10.33) minus transcribed expression: max |diff| = 0.0127 dex (rms 0.0093); ends: drawn 8.250,8.736 vs expression 8.263,8.740"},{"id":"garcia24.illustris.fmr.mu0.23.linear.z0","source":"Illustris","run":"Illustris-1 (Garcia+24 FMR regression, star-forming centrals)","kind":"simulation","relation":"fmr","epoch":{"zRepresentative":0,"zNominal":0,"zMin":0,"zMax":0,"mode":"published-epoch","snapshot":null},"axes":{"xDefinition":"mu_0.23 = log10(M*/Msun) - 0.23 log10(SFR/(Msun/yr)), star-forming centrals at z=0","xUnit":"log10(Msun)","yDefinition":"12+log10(O/H) from the mass-weighted total metallicity of star-forming gas bound to the system, scaled with constant f_O = 0.35 and X = 0.76","yUnit":"dex"},"domain":{"xMin":8.54,"xMax":10.98},"representation":{"type":"parametric","equation":"12+log(O/H) = 0.693 mu_0.23 + 1.807","expression":"m*x+b","parameters":{"m":0.693,"b":1.807}},"scatter":null,"selection":{"population":"star-forming central galaxies (sSFR within 0.5 dex of the sSFMS), well resolved (M* > 1e8 Msun, 1e9 in SIMBA; gas mass > 10^8.5, 10^9.5 in SIMBA)","warning":"z=0 linear least-squares regression of 12+log(O/H) on mu_alpha for the star-forming central galaxies of the simulation, alpha = alpha_min of the minimum-scatter projection. x range is NOT stated by the paper: it is mu_alpha evaluated along the z=0 star-forming main sequence (digitized from the paper's SFMS figure) over the stellar-mass range of the paper's predicted-MZR curve (log M* 8.10-11.20), so it is narrower than the full galaxy scatter in mu_alpha. METALLICITY SCALE: the printed equation of the Illustris/TNG/EAGLE lines is identical in arXiv v1 and v2, but v1 converts the star-forming-gas metal mass fraction to O/H with f_O = 35 per cent while v2 text says f_O = 50 per cent. The equation reproduces the v1 figure (mean offset -0.011 dex) and sits 0.166 dex below the v2 figure (log10(50/35) = 0.155), so it corresponds to f_O = 35 per cent; the v2 text did not update this line. Not a directly tracked oxygen abundance (constant f_O and X scaling of the total metallicity)."},"definitions":{"muAlpha":0.23,"metallicityQuantity":"gas-O/H","metallicityCalibration":"total metallicity of star-forming gas rescaled to O/H with constant oxygen-to-metal mass fraction f_O = 0.35 and hydrogen mass fraction X = 0.76","sfrTimescaleMyr":"unspecified","imf":"chabrier03","massDefinition":"unspecified","population":"star-forming-centrals"},"provenance":{"tier":"published-fit","citation":"Garcia et al. 2024, 'Does the Fundamental Metallicity Relation Evolve with Redshift? II' (arXiv:2407.06254), eq. 'FMR_regressions'","doi":null,"url":"https://arxiv.org/abs/2407.06254","retrieved":"2026-10-18","sourceMember":"paper.tex","figureMember":"figures/fake_MZR_mega.pdf (v1), figures/Figure4.pdf and Figure2.pdf (v2)","figureSha256":"9fe321b30eb788fb48ce116a94835046ebd7f20991db5bdd02884b6866955b9d","sourceArchiveSha256":"1966844be96db2cd3a1588714c096ee5679f283d7e834376fac8fe7e98c28e50","terms":"third-party: source repository has no licence file (Garcia et al. 2024); binned values derived by sim-highline, permission not yet requested"},"calibration":"prediction","rankable":true,"notes":"Equation as printed. v1 figures (f_O=35%): formula minus drawn z=0 predicted MZR, mean/sd (dex): Illustris -0.0108/0.0027; TNG -0.0015/0.0021; EAGLE -0.0066/0.0048; SIMBA -0.0012/0.0065 v2 figures (f_O=50%): Illustris -0.1658/0.0027; TNG -0.1564/0.0021; EAGLE -0.1616/0.0048; SIMBA -0.0026/0.0133; log10(50/35) = 0.1549"},{"id":"garcia24.tng.fmr.mu0.31.linear.z0","source":"IllustrisTNG","run":"TNG100-1 (Garcia+24 FMR regression, star-forming centrals)","kind":"simulation","relation":"fmr","epoch":{"zRepresentative":0,"zNominal":0,"zMin":0,"zMax":0,"mode":"published-epoch","snapshot":null},"axes":{"xDefinition":"mu_0.31 = log10(M*/Msun) - 0.31 log10(SFR/(Msun/yr)), star-forming centrals at z=0","xUnit":"log10(Msun)","yDefinition":"12+log10(O/H) from the mass-weighted total metallicity of star-forming gas bound to the system, scaled with constant f_O = 0.35 and X = 0.76","yUnit":"dex"},"domain":{"xMin":8.65,"xMax":10.71},"representation":{"type":"parametric","equation":"12+log(O/H) = 0.368 mu_0.31 + 5.044","expression":"m*x+b","parameters":{"m":0.368,"b":5.044}},"scatter":null,"selection":{"population":"star-forming central galaxies (sSFR within 0.5 dex of the sSFMS), well resolved (M* > 1e8 Msun, 1e9 in SIMBA; gas mass > 10^8.5, 10^9.5 in SIMBA)","warning":"z=0 linear least-squares regression of 12+log(O/H) on mu_alpha for the star-forming central galaxies of the simulation, alpha = alpha_min of the minimum-scatter projection. x range is NOT stated by the paper: it is mu_alpha evaluated along the z=0 star-forming main sequence (digitized from the paper's SFMS figure) over the stellar-mass range of the paper's predicted-MZR curve (log M* 8.10-10.90), so it is narrower than the full galaxy scatter in mu_alpha. METALLICITY SCALE: the printed equation of the Illustris/TNG/EAGLE lines is identical in arXiv v1 and v2, but v1 converts the star-forming-gas metal mass fraction to O/H with f_O = 35 per cent while v2 text says f_O = 50 per cent. The equation reproduces the v1 figure (mean offset -0.001 dex) and sits 0.156 dex below the v2 figure (log10(50/35) = 0.155), so it corresponds to f_O = 35 per cent; the v2 text did not update this line. Not a directly tracked oxygen abundance (constant f_O and X scaling of the total metallicity)."},"definitions":{"muAlpha":0.31,"metallicityQuantity":"gas-O/H","metallicityCalibration":"total metallicity of star-forming gas rescaled to O/H with constant oxygen-to-metal mass fraction f_O = 0.35 and hydrogen mass fraction X = 0.76","sfrTimescaleMyr":"unspecified","imf":"chabrier03","massDefinition":"unspecified","population":"star-forming-centrals"},"provenance":{"tier":"published-fit","citation":"Garcia et al. 2024, 'Does the Fundamental Metallicity Relation Evolve with Redshift? II' (arXiv:2407.06254), eq. 'FMR_regressions'","doi":null,"url":"https://arxiv.org/abs/2407.06254","retrieved":"2026-10-18","sourceMember":"paper.tex","figureMember":"figures/fake_MZR_mega.pdf (v1), figures/Figure4.pdf and Figure2.pdf (v2)","figureSha256":"9fe321b30eb788fb48ce116a94835046ebd7f20991db5bdd02884b6866955b9d","sourceArchiveSha256":"1966844be96db2cd3a1588714c096ee5679f283d7e834376fac8fe7e98c28e50","terms":"third-party: source repository has no licence file (Garcia et al. 2024); binned values derived by sim-highline, permission not yet requested"},"calibration":"prediction","rankable":true,"notes":"Equation as printed. v1 figures (f_O=35%): formula minus drawn z=0 predicted MZR, mean/sd (dex): Illustris -0.0108/0.0027; TNG -0.0015/0.0021; EAGLE -0.0066/0.0048; SIMBA -0.0012/0.0065 v2 figures (f_O=50%): Illustris -0.1658/0.0027; TNG -0.1564/0.0021; EAGLE -0.1616/0.0048; SIMBA -0.0026/0.0133; log10(50/35) = 0.1549"},{"id":"garcia24.eagle.fmr.mu0.74.linear.z0","source":"EAGLE","run":"RefL0100N1504 (Garcia+24 FMR regression, star-forming centrals)","kind":"simulation","relation":"fmr","epoch":{"zRepresentative":0,"zNominal":0,"zMin":0,"zMax":0,"mode":"published-epoch","snapshot":null},"axes":{"xDefinition":"mu_0.74 = log10(M*/Msun) - 0.74 log10(SFR/(Msun/yr)), star-forming centrals at z=0","xUnit":"log10(Msun)","yDefinition":"12+log10(O/H) from the mass-weighted total metallicity of star-forming gas bound to the system, scaled with constant f_O = 0.35 and X = 0.76","yUnit":"dex"},"domain":{"xMin":9.47,"xMax":10.75},"representation":{"type":"parametric","equation":"12+log(O/H) = 0.38 mu_0.74 + 5.132","expression":"m*x+b","parameters":{"m":0.38,"b":5.132}},"scatter":null,"selection":{"population":"star-forming central galaxies (sSFR within 0.5 dex of the sSFMS), well resolved (M* > 1e8 Msun, 1e9 in SIMBA; gas mass > 10^8.5, 10^9.5 in SIMBA)","warning":"z=0 linear least-squares regression of 12+log(O/H) on mu_alpha for the star-forming central galaxies of the simulation, alpha = alpha_min of the minimum-scatter projection. x range is NOT stated by the paper: it is mu_alpha evaluated along the z=0 star-forming main sequence (digitized from the paper's SFMS figure) over the stellar-mass range of the paper's predicted-MZR curve (log M* 8.10-11.20), so it is narrower than the full galaxy scatter in mu_alpha. METALLICITY SCALE: the printed equation of the Illustris/TNG/EAGLE lines is identical in arXiv v1 and v2, but v1 converts the star-forming-gas metal mass fraction to O/H with f_O = 35 per cent while v2 text says f_O = 50 per cent. The equation reproduces the v1 figure (mean offset -0.007 dex) and sits 0.162 dex below the v2 figure (log10(50/35) = 0.155), so it corresponds to f_O = 35 per cent; the v2 text did not update this line. Not a directly tracked oxygen abundance (constant f_O and X scaling of the total metallicity)."},"definitions":{"muAlpha":0.74,"metallicityQuantity":"gas-O/H","metallicityCalibration":"total metallicity of star-forming gas rescaled to O/H with constant oxygen-to-metal mass fraction f_O = 0.35 and hydrogen mass fraction X = 0.76","sfrTimescaleMyr":"unspecified","imf":"chabrier03","massDefinition":"unspecified","population":"star-forming-centrals"},"provenance":{"tier":"published-fit","citation":"Garcia et al. 2024, 'Does the Fundamental Metallicity Relation Evolve with Redshift? II' (arXiv:2407.06254), eq. 'FMR_regressions'","doi":null,"url":"https://arxiv.org/abs/2407.06254","retrieved":"2026-10-18","sourceMember":"paper.tex","figureMember":"figures/fake_MZR_mega.pdf (v1), figures/Figure4.pdf and Figure2.pdf (v2)","figureSha256":"9fe321b30eb788fb48ce116a94835046ebd7f20991db5bdd02884b6866955b9d","sourceArchiveSha256":"1966844be96db2cd3a1588714c096ee5679f283d7e834376fac8fe7e98c28e50","terms":"third-party: source repository has no licence file (Garcia et al. 2024); binned values derived by sim-highline, permission not yet requested"},"calibration":"prediction","rankable":true,"notes":"Equation as printed. v1 figures (f_O=35%): formula minus drawn z=0 predicted MZR, mean/sd (dex): Illustris -0.0108/0.0027; TNG -0.0015/0.0021; EAGLE -0.0066/0.0048; SIMBA -0.0012/0.0065 v2 figures (f_O=50%): Illustris -0.1658/0.0027; TNG -0.1564/0.0021; EAGLE -0.1616/0.0048; SIMBA -0.0026/0.0133; log10(50/35) = 0.1549"},{"id":"garcia24.simba.fmr.mu0.66.linear.z0","source":"SIMBA","run":"m100n1024 (Garcia+24 FMR regression, star-forming centrals)","kind":"simulation","relation":"fmr","epoch":{"zRepresentative":0,"zNominal":0,"zMin":0,"zMax":0,"mode":"published-epoch","snapshot":null},"axes":{"xDefinition":"mu_0.66 = log10(M*/Msun) - 0.66 log10(SFR/(Msun/yr)), star-forming centrals at z=0","xUnit":"log10(Msun)","yDefinition":"12+log10(O/H) from the mass-weighted total metallicity of star-forming gas bound to the system, scaled with constant f_O = 0.5 and X = 0.76","yUnit":"dex"},"domain":{"xMin":9.4,"xMax":10.94},"representation":{"type":"parametric","equation":"12+log(O/H) = 0.364 mu_0.66 + 4.901","expression":"m*x+b","parameters":{"m":0.364,"b":4.901}},"scatter":null,"selection":{"population":"star-forming central galaxies (sSFR within 0.5 dex of the sSFMS), well resolved (M* > 1e8 Msun, 1e9 in SIMBA; gas mass > 10^8.5, 10^9.5 in SIMBA)","warning":"z=0 linear least-squares regression of 12+log(O/H) on mu_alpha for the star-forming central galaxies of the simulation, alpha = alpha_min of the minimum-scatter projection. x range is NOT stated by the paper: it is mu_alpha evaluated along the z=0 star-forming main sequence (digitized from the paper's SFMS figure) over the stellar-mass range of the paper's predicted-MZR curve (log M* 9.10-11.40), so it is narrower than the full galaxy scatter in mu_alpha. METALLICITY SCALE: f_O = 50 per cent, X = 76 per cent (v2). The v1 line for SIMBA was 0.440 mu_0.33 + 3.974 (f_O = 35 per cent); v2 text still says alpha_min = 0.33 for SIMBA in one sentence, but its equation and figure use alpha = 0.66, which the figure check confirms (alpha = 0.33 does not reproduce the drawn curve)."},"definitions":{"muAlpha":0.66,"metallicityQuantity":"gas-O/H","metallicityCalibration":"total metallicity of star-forming gas rescaled to O/H with constant oxygen-to-metal mass fraction f_O = 0.5 and hydrogen mass fraction X = 0.76","sfrTimescaleMyr":"unspecified","imf":"chabrier03","massDefinition":"unspecified","population":"star-forming-centrals"},"provenance":{"tier":"published-fit","citation":"Garcia et al. 2024, 'Does the Fundamental Metallicity Relation Evolve with Redshift? II' (arXiv:2407.06254), eq. 'FMR_regressions'","doi":null,"url":"https://arxiv.org/abs/2407.06254","retrieved":"2026-10-18","sourceMember":"paper.tex","figureMember":"figures/fake_MZR_mega.pdf (v1), figures/Figure4.pdf and Figure2.pdf (v2)","figureSha256":"3cb50554df66ebf8c7a6925aa562b9c06b2f71ce97a954563cb28d6e6041eb41","sourceArchiveSha256":"6da622ce40cca088c348d26705c83b79d482b483a463771c46722032f5527b38","terms":"third-party: source repository has no licence file (Garcia et al. 2024); binned values derived by sim-highline, permission not yet requested"},"calibration":"prediction","rankable":true,"notes":"Equation as printed. v1 figures (f_O=35%): formula minus drawn z=0 predicted MZR, mean/sd (dex): Illustris -0.0108/0.0027; TNG -0.0015/0.0021; EAGLE -0.0066/0.0048; SIMBA -0.0012/0.0065 v2 figures (f_O=50%): Illustris -0.1658/0.0027; TNG -0.1564/0.0021; EAGLE -0.1616/0.0048; SIMBA -0.0026/0.0133; log10(50/35) = 0.1549"},{"id":"mannucci10.sdss.fmr.mu0.32.poly4","source":"Mannucci et al. 2010","run":"SDSS median polynomial","kind":"observation","relation":"fmr","epoch":{"zRepresentative":0.185,"zMin":0.07,"zMax":0.3,"mode":"observational-bin","snapshot":null},"axes":{"xDefinition":"mu_0.32 = log10(M*/Msun) - 0.32 log10(SFR/(Msun/yr)); total stellar mass (Kauffmann+03, scaled 1.06 from Kroupa to Chabrier), SFR from fibre Halpha","xUnit":"log10(Msun)","yDefinition":"12+log10(O/H), gas-phase oxygen abundance (Nagao+06, Maiolino+08 strong-line calibration)","yUnit":"dex"},"domain":{"xMin":9.23,"xMax":11.43},"representation":{"type":"parametric","equation":"12+log(O/H) = 8.90 + 0.39x - 0.20x^2 - 0.077x^3 + 0.064x^4, x = mu_0.32 - 10","expression":"8.90+0.39*(x-10)-0.20*Math.pow(x-10,2)-0.077*Math.pow(x-10,3)+0.064*Math.pow(x-10,4)","parameters":{}},"scatter":{"value":0.05,"unit":"dex","meaning":"residual dispersion of individual SDSS galaxies around the 3D FMR in the central part, as stated for the FMR (not for this projection)"},"selection":{"population":"SDSS DR7 emission-line galaxies, AGN removed (BPT), H-alpha S/N>25, 0.07<z<0.30; fit to the median metallicity in mu_0.32","warning":"Fit to the medians of SDSS galaxies in mu_0.32. x range is the span of mu_0.32 over the cells of the paper's Table 1 (computed from bin centres, not stated by the paper). zRepresentative 0.185 is the midpoint of the 0.07-0.30 selection window, not a measured median. The paper's 3 arcsec fibre SFRs are not aperture corrected."},"definitions":{"muAlpha":0.32,"metallicityQuantity":"gas-O/H","metallicityCalibration":"Nagao+06 / Maiolino+08 strong-line calibrations (average of N2 and R23 metallicities)","sfrTimescaleMyr":"unspecified","sfrIndicator":"Halpha (3 arcsec fibre, Balmer-decrement dust correction, Kennicutt 1998 conversion)","imf":"chabrier03","massDefinition":"sed-total","population":"star-forming"},"provenance":{"tier":"published-fit","citation":"Mannucci et al. 2010, MNRAS 408, 2115 (arXiv:1005.0006)","doi":"10.1111/j.1365-2966.2010.17291.x","url":"https://arxiv.org/abs/1005.0006","retrieved":"2026-10-18","sourceMember":"fmr4.tex","sourceArchiveSha256":"1edb3e3bd44d9d843d249e2aa1b0fd463bc6f916517607665a82cca95512f560"},"calibration":"validation","rankable":true,"notes":"Polynomial as published (eq. 'cfr2', first). poly(10)=8.900 (quoted constant term 8.90); poly(10.8)=9.0708 -> 9.07 vs quoted plateau 9.07; poly over 10.7-11.4 in 0.1 steps = [9.06, 9.07, 9.07, 9.08, 9.08, 9.08, 9.08, 9.09]. Table 1: 185 median cells, mu_0.32 span 9.23..11.43, N-weighted rms of polynomial minus cell median = 0.0153 dex."},{"id":"mannucci10.sdss-highz.fmr.mu0.32.linear-lowmu","source":"Mannucci et al. 2010","run":"linear branch mu<10.2","kind":"observation","relation":"fmr","epoch":{"zRepresentative":0.07,"zMin":0.07,"zMax":2.5,"mode":"analytic-evolution","snapshot":null},"axes":{"xDefinition":"mu_0.32 = log10(M*/Msun) - 0.32 log10(SFR/(Msun/yr)); total stellar mass (Kauffmann+03, scaled 1.06 from Kroupa to Chabrier), SFR from fibre Halpha","xUnit":"log10(Msun)","yDefinition":"12+log10(O/H), gas-phase oxygen abundance (Nagao+06, Maiolino+08 strong-line calibration)","yUnit":"dex"},"domain":{"xMin":9.23,"xMax":10.2},"representation":{"type":"parametric","equation":"12+log(O/H) = 8.90 + 0.47x, x = mu_0.32 - 10, valid for mu_0.32 < 10.2","expression":"8.90+0.47*(x-10)","parameters":{}},"scatter":null,"selection":{"population":"star-forming galaxies of any mass and SFR, SDSS plus the z=0.5-2.5 literature samples compiled in the paper","warning":"Published as the relation followed 'at any redshift up to z=2.5'; the paper gives no relation for 10.2<mu_0.32<10.5. Evolution is stored as analytic-evolution with zRepresentative = zMin because the expression has no redshift dependence."},"definitions":{"muAlpha":0.32,"metallicityQuantity":"gas-O/H","metallicityCalibration":"Nagao+06 / Maiolino+08 strong-line calibrations (average of N2 and R23 metallicities)","sfrTimescaleMyr":"unspecified","sfrIndicator":"Halpha (3 arcsec fibre, Balmer-decrement dust correction, Kennicutt 1998 conversion)","imf":"chabrier03","massDefinition":"sed-total","population":"star-forming"},"provenance":{"tier":"published-fit","citation":"Mannucci et al. 2010, MNRAS 408, 2115 (arXiv:1005.0006)","doi":"10.1111/j.1365-2966.2010.17291.x","url":"https://arxiv.org/abs/1005.0006","retrieved":"2026-10-18","sourceMember":"fmr4.tex","sourceArchiveSha256":"1edb3e3bd44d9d843d249e2aa1b0fd463bc6f916517607665a82cca95512f560"},"calibration":"validation","rankable":true,"notes":"Linear branch as published. Table 1 cells with mu<10.2 and N>200: least-squares slope dZ/dmu = 0.390 (the paper's linear branch, 0.47, was fitted to the SDSS plus high-z samples, so the SDSS-only slope is not expected to equal it); N-weighted rms of 8.90+0.47x minus the Table 1 cell medians with mu<10.2 = 0.025 dex"},{"id":"mannucci10.sdss-highz.fmr.mu0.32.plateau","source":"Mannucci et al. 2010","run":"plateau branch mu>10.5","kind":"observation","relation":"fmr","epoch":{"zRepresentative":0.07,"zMin":0.07,"zMax":2.5,"mode":"analytic-evolution","snapshot":null},"axes":{"xDefinition":"mu_0.32 = log10(M*/Msun) - 0.32 log10(SFR/(Msun/yr)); total stellar mass (Kauffmann+03, scaled 1.06 from Kroupa to Chabrier), SFR from fibre Halpha","xUnit":"log10(Msun)","yDefinition":"12+log10(O/H), gas-phase oxygen abundance (Nagao+06, Maiolino+08 strong-line calibration)","yUnit":"dex"},"domain":{"xMin":10.5,"xMax":11.43},"representation":{"type":"parametric","equation":"12+log(O/H) = 9.07, valid for mu_0.32 > 10.5","expression":"9.07","parameters":{}},"scatter":null,"selection":{"population":"star-forming galaxies of any mass and SFR, SDSS plus the z=0.5-2.5 literature samples compiled in the paper","warning":"Constant branch of the same published relation; see the linear-lowmu record. Upper x limit is the span of mu_0.32 over the cells of the paper's Table 1."},"definitions":{"muAlpha":0.32,"metallicityQuantity":"gas-O/H","metallicityCalibration":"Nagao+06 / Maiolino+08 strong-line calibrations (average of N2 and R23 metallicities)","sfrTimescaleMyr":"unspecified","sfrIndicator":"Halpha (3 arcsec fibre, Balmer-decrement dust correction, Kennicutt 1998 conversion)","imf":"chabrier03","massDefinition":"sed-total","population":"star-forming"},"provenance":{"tier":"published-fit","citation":"Mannucci et al. 2010, MNRAS 408, 2115 (arXiv:1005.0006)","doi":"10.1111/j.1365-2966.2010.17291.x","url":"https://arxiv.org/abs/1005.0006","retrieved":"2026-10-18","sourceMember":"fmr4.tex","sourceArchiveSha256":"1edb3e3bd44d9d843d249e2aa1b0fd463bc6f916517607665a82cca95512f560"},"calibration":"validation","rankable":true,"notes":"Plateau as published. Table 1 cells with mu>10.5 (77 cells): N-weighted mean median-metallicity = 9.0583 vs quoted 9.07 (agreement to 0.015 dex only; the plateau value is a rounded fit parameter); the SDSS polynomial evaluates to 9.07 at mu_0.32=10.8."},{"id":"sanders21.sdss-stacks.fmr.mu0.60.cubic","source":"Sanders et al. 2021","run":"z~0 cubic fit to Andrews & Martini stacks","kind":"observation","relation":"fmr","epoch":{"zRepresentative":0.08,"zMin":0.027,"zMax":0.25,"mode":"observational-bin","snapshot":null},"axes":{"xDefinition":"mu_0.60 = log10(M*/Msun) - 0.60 log10(SFR/(Msun/yr)); median M* and median SFR of each stack, SFR from Halpha (Hao+11 calibration), Chabrier IMF","xUnit":"log10(Msun)","yDefinition":"12+log10(O/H), strong-line ratios ([OII], Hbeta, [OIII], [NeIII]) with z~0 calibrations anchored to direct-method (Te) metallicities, DIG-corrected","yUnit":"dex"},"domain":{"xMin":8.25,"xMax":11.125},"representation":{"type":"parametric","equation":"12+log(O/H) = 8.80 + 0.188 y - 0.220 y^2 - 0.0531 y^3, y = mu_0.60 - 10","expression":"8.80+0.188*(x-10)-0.220*Math.pow(x-10,2)-0.0531*Math.pow(x-10,3)","parameters":{}},"scatter":{"value":0.05,"unit":"dex","meaning":"intrinsic scatter of the FMR at z=0 quoted in the paper text ('approximately 0.05 dex', citing Mannucci+10, Cresci+19, Curti+20); not measured for this fit"},"selection":{"population":"Andrews & Martini 2013 SDSS stacks in M*-SFR bins with at least 5 galaxies, DIG-corrected line fluxes; z~0.08","warning":"Cubic fit to z~0 stacks only; the paper reports that its z~2.3 and z~3.3 stacks fall on it without being fitted. x range is the extent of the curve drawn in the paper's figure (not stated in the text). The redshift range 0.027<z<0.25 is that of the Andrews & Martini stacks (their paper, Sec. 2), zRepresentative 0.08 is the paper's 'z~0.08'. The cubic turns over (maximum 8.84 at mu=10.38) and decreases beyond it, which is the shape drawn. SFRs are not DIG-corrected; metallicities are NOT the Andrews & Martini direct-method values but strong-line values calibrated to them."},"definitions":{"muAlpha":0.6,"metallicityQuantity":"gas-O/H","metallicityCalibration":"strong-line calibrations (O32, R23, [NeIII]/[OII] etc.) anchored to direct-method (Te) metallicities of SDSS stacks and dwarfs (Sanders+21 z~0 set), DIG-corrected","sfrTimescaleMyr":"unspecified","sfrIndicator":"Halpha (dust-corrected Balmer lines), Hao+11 calibration renormalised to Chabrier IMF, not DIG-corrected","imf":"chabrier03","massDefinition":"sed-total","population":"star-forming"},"provenance":{"tier":"published-fit","citation":"Sanders et al. 2021, ApJ 914, 19 (arXiv:2009.07292), eq. 'fmr' (Sec. 'The fundamental metallicity relation at z=0-3.3')","doi":"10.3847/1538-4357/abf4c1","url":"https://arxiv.org/abs/2009.07292","retrieved":"2026-10-18","sourceMember":"ms.tex","figureMember":"z0z2z3_fmr_combined.pdf","figureSha256":"f1487bc79a304f869eaf653d2aa1e00e409e63780a95c3b668187bffe2341da6","sourceArchiveSha256":"8fb01530d79223ee3f224e5980196df4e42a8ecb9cbfd7cab3fd29249482877e"},"calibration":"validation","rankable":true,"notes":"Cubic as published. drawn black best-fit cubic (100 vertices, x 8.25..11.125) minus transcribed cubic: max |diff| = 0.0023 dex (rms 0.0020); ends: drawn 8.080,8.656 vs cubic 8.082,8.657 cubic maximum 8.837 at mu_0.60 = 10.38 (the paper: flattening above mu_0.60 = 10.0)"},{"id":"furlong15.eagle-l100n1504.gsmf-single-schechter.z0.1","source":"EAGLE","run":"Ref-L100N1504 (single Schechter fit)","kind":"simulation","relation":"gsmf","epoch":{"zRepresentative":0.1,"zNominal":0.1,"zMin":0.1,"zMax":0.1,"mode":"published-epoch","snapshot":null},"axes":{"xDefinition":"log10 stellar mass","xUnit":"log10(Msun)","yDefinition":"log10 galaxy number density per dex (single Schechter fit, converted from per-dM)","yUnit":"log10(cMpc^-3 dex^-1)"},"domain":{"xMin":8,"xMax":12},"representation":{"type":"parametric","equation":"Phi_dex = ln(10) exp(-M/M*) phi1 (M/M*)^(alpha1+1)","expression":"log10(Math.LN10*Math.exp(-Math.pow(10,x-logMstar))*phi1*Math.pow(10,(x-logMstar)*(alpha1+1)))","parameters":{"logMstar":11.14,"phi1":0.00084,"alpha1":-1.43,"logMstarError":0.09,"phi1Error":0.00013000000000000002,"alpha1Error":0.01}},"scatter":null,"selection":{"population":"all galaxies","warning":"Least-squares fit by Furlong et al. 2015 to 0.2 dex bins of the Ref-L100N1504 GSMF between 10^8 and 10^12 Msun, Poisson-weighted. Phi* is per unit M/M* (cMpc^-3) as tabulated; the record converts to per dex. Fit, not the simulation curve itself; the fit degeneracies between M* and Phi* are noted by the authors."},"definitions":{"massDefinition":"aperture-30pkpc","imf":"chabrier03","cosmology":{"H0":67.77,"Om":0.307},"densityFrame":"comoving","population":"all"},"provenance":{"tier":"published-fit","citation":"Furlong et al. 2015, MNRAS 450, 4486, Appendix A Table (Schechter fits)","doi":"10.1093/mnras/stv852","url":"https://arxiv.org/abs/1410.3485","retrieved":"2026-10-05","sourceMember":"Appendix.tex table:Schechter (arXiv source, transcribed)"},"calibration":"target","rankable":true,"notes":"Transcribed from the paper's table; spot-checked against published values in the script."},{"id":"furlong15.eagle-l100n1504.gsmf-single-schechter.z0.5","source":"EAGLE","run":"Ref-L100N1504 (single Schechter fit)","kind":"simulation","relation":"gsmf","epoch":{"zRepresentative":0.5,"zNominal":0.5,"zMin":0.5,"zMax":0.5,"mode":"published-epoch","snapshot":null},"axes":{"xDefinition":"log10 stellar mass","xUnit":"log10(Msun)","yDefinition":"log10 galaxy number density per dex (single Schechter fit, converted from per-dM)","yUnit":"log10(cMpc^-3 dex^-1)"},"domain":{"xMin":8,"xMax":12},"representation":{"type":"parametric","equation":"Phi_dex = ln(10) exp(-M/M*) phi1 (M/M*)^(alpha1+1)","expression":"log10(Math.LN10*Math.exp(-Math.pow(10,x-logMstar))*phi1*Math.pow(10,(x-logMstar)*(alpha1+1)))","parameters":{"logMstar":11.11,"phi1":0.00084,"alpha1":-1.45,"logMstarError":0.08,"phi1Error":0.00012,"alpha1Error":0.01}},"scatter":null,"selection":{"population":"all galaxies","warning":"Least-squares fit by Furlong et al. 2015 to 0.2 dex bins of the Ref-L100N1504 GSMF between 10^8 and 10^12 Msun, Poisson-weighted. Phi* is per unit M/M* (cMpc^-3) as tabulated; the record converts to per dex. Fit, not the simulation curve itself; the fit degeneracies between M* and Phi* are noted by the authors."},"definitions":{"massDefinition":"aperture-30pkpc","imf":"chabrier03","cosmology":{"H0":67.77,"Om":0.307},"densityFrame":"comoving","population":"all"},"provenance":{"tier":"published-fit","citation":"Furlong et al. 2015, MNRAS 450, 4486, Appendix A Table (Schechter fits)","doi":"10.1093/mnras/stv852","url":"https://arxiv.org/abs/1410.3485","retrieved":"2026-10-05","sourceMember":"Appendix.tex table:Schechter (arXiv source, transcribed)"},"calibration":"prediction","rankable":true,"notes":"Transcribed from the paper's table; spot-checked against published values in the script."},{"id":"furlong15.eagle-l100n1504.gsmf-single-schechter.z1","source":"EAGLE","run":"Ref-L100N1504 (single Schechter fit)","kind":"simulation","relation":"gsmf","epoch":{"zRepresentative":1,"zNominal":1,"zMin":1,"zMax":1,"mode":"published-epoch","snapshot":null},"axes":{"xDefinition":"log10 stellar mass","xUnit":"log10(Msun)","yDefinition":"log10 galaxy number density per dex (single Schechter fit, converted from per-dM)","yUnit":"log10(cMpc^-3 dex^-1)"},"domain":{"xMin":8,"xMax":12},"representation":{"type":"parametric","equation":"Phi_dex = ln(10) exp(-M/M*) phi1 (M/M*)^(alpha1+1)","expression":"log10(Math.LN10*Math.exp(-Math.pow(10,x-logMstar))*phi1*Math.pow(10,(x-logMstar)*(alpha1+1)))","parameters":{"logMstar":11.06,"phi1":0.00074,"alpha1":-1.48,"logMstarError":0.08,"phi1Error":0.0001,"alpha1Error":0.01}},"scatter":null,"selection":{"population":"all galaxies","warning":"Least-squares fit by Furlong et al. 2015 to 0.2 dex bins of the Ref-L100N1504 GSMF between 10^8 and 10^12 Msun, Poisson-weighted. Phi* is per unit M/M* (cMpc^-3) as tabulated; the record converts to per dex. Fit, not the simulation curve itself; the fit degeneracies between M* and Phi* are noted by the authors."},"definitions":{"massDefinition":"aperture-30pkpc","imf":"chabrier03","cosmology":{"H0":67.77,"Om":0.307},"densityFrame":"comoving","population":"all"},"provenance":{"tier":"published-fit","citation":"Furlong et al. 2015, MNRAS 450, 4486, Appendix A Table (Schechter fits)","doi":"10.1093/mnras/stv852","url":"https://arxiv.org/abs/1410.3485","retrieved":"2026-10-05","sourceMember":"Appendix.tex table:Schechter (arXiv source, transcribed)"},"calibration":"prediction","rankable":true,"notes":"Transcribed from the paper's table; spot-checked against published values in the script."},{"id":"furlong15.eagle-l100n1504.gsmf-single-schechter.z2","source":"EAGLE","run":"Ref-L100N1504 (single Schechter fit)","kind":"simulation","relation":"gsmf","epoch":{"zRepresentative":2,"zNominal":2,"zMin":2,"zMax":2,"mode":"published-epoch","snapshot":null},"axes":{"xDefinition":"log10 stellar mass","xUnit":"log10(Msun)","yDefinition":"log10 galaxy number density per dex (single Schechter fit, converted from per-dM)","yUnit":"log10(cMpc^-3 dex^-1)"},"domain":{"xMin":8,"xMax":12},"representation":{"type":"parametric","equation":"Phi_dex = ln(10) exp(-M/M*) phi1 (M/M*)^(alpha1+1)","expression":"log10(Math.LN10*Math.exp(-Math.pow(10,x-logMstar))*phi1*Math.pow(10,(x-logMstar)*(alpha1+1)))","parameters":{"logMstar":10.91,"phi1":0.00045000000000000004,"alpha1":-1.57,"logMstarError":0.08,"phi1Error":0.00007000000000000001,"alpha1Error":0.01}},"scatter":null,"selection":{"population":"all galaxies","warning":"Least-squares fit by Furlong et al. 2015 to 0.2 dex bins of the Ref-L100N1504 GSMF between 10^8 and 10^12 Msun, Poisson-weighted. Phi* is per unit M/M* (cMpc^-3) as tabulated; the record converts to per dex. Fit, not the simulation curve itself; the fit degeneracies between M* and Phi* are noted by the authors."},"definitions":{"massDefinition":"aperture-30pkpc","imf":"chabrier03","cosmology":{"H0":67.77,"Om":0.307},"densityFrame":"comoving","population":"all"},"provenance":{"tier":"published-fit","citation":"Furlong et al. 2015, MNRAS 450, 4486, Appendix A Table (Schechter fits)","doi":"10.1093/mnras/stv852","url":"https://arxiv.org/abs/1410.3485","retrieved":"2026-10-05","sourceMember":"Appendix.tex table:Schechter (arXiv source, transcribed)"},"calibration":"prediction","rankable":true,"notes":"Transcribed from the paper's table; spot-checked against published values in the script."},{"id":"furlong15.eagle-l100n1504.gsmf-single-schechter.z3","source":"EAGLE","run":"Ref-L100N1504 (single Schechter fit)","kind":"simulation","relation":"gsmf","epoch":{"zRepresentative":3,"zNominal":3,"zMin":3,"zMax":3,"mode":"published-epoch","snapshot":null},"axes":{"xDefinition":"log10 stellar mass","xUnit":"log10(Msun)","yDefinition":"log10 galaxy number density per dex (single Schechter fit, converted from per-dM)","yUnit":"log10(cMpc^-3 dex^-1)"},"domain":{"xMin":8,"xMax":12},"representation":{"type":"parametric","equation":"Phi_dex = ln(10) exp(-M/M*) phi1 (M/M*)^(alpha1+1)","expression":"log10(Math.LN10*Math.exp(-Math.pow(10,x-logMstar))*phi1*Math.pow(10,(x-logMstar)*(alpha1+1)))","parameters":{"logMstar":10.78,"phi1":0.00022,"alpha1":-1.66,"logMstarError":0.11,"phi1Error":0.00005,"alpha1Error":0.01}},"scatter":null,"selection":{"population":"all galaxies","warning":"Least-squares fit by Furlong et al. 2015 to 0.2 dex bins of the Ref-L100N1504 GSMF between 10^8 and 10^12 Msun, Poisson-weighted. Phi* is per unit M/M* (cMpc^-3) as tabulated; the record converts to per dex. Fit, not the simulation curve itself; the fit degeneracies between M* and Phi* are noted by the authors."},"definitions":{"massDefinition":"aperture-30pkpc","imf":"chabrier03","cosmology":{"H0":67.77,"Om":0.307},"densityFrame":"comoving","population":"all"},"provenance":{"tier":"published-fit","citation":"Furlong et al. 2015, MNRAS 450, 4486, Appendix A Table (Schechter fits)","doi":"10.1093/mnras/stv852","url":"https://arxiv.org/abs/1410.3485","retrieved":"2026-10-05","sourceMember":"Appendix.tex table:Schechter (arXiv source, transcribed)"},"calibration":"prediction","rankable":true,"notes":"Transcribed from the paper's table; spot-checked against published values in the script."},{"id":"furlong15.eagle-l100n1504.gsmf-single-schechter.z4","source":"EAGLE","run":"Ref-L100N1504 (single Schechter fit)","kind":"simulation","relation":"gsmf","epoch":{"zRepresentative":4,"zNominal":4,"zMin":4,"zMax":4,"mode":"published-epoch","snapshot":null},"axes":{"xDefinition":"log10 stellar mass","xUnit":"log10(Msun)","yDefinition":"log10 galaxy number density per dex (single Schechter fit, converted from per-dM)","yUnit":"log10(cMpc^-3 dex^-1)"},"domain":{"xMin":8,"xMax":12},"representation":{"type":"parametric","equation":"Phi_dex = ln(10) exp(-M/M*) phi1 (M/M*)^(alpha1+1)","expression":"log10(Math.LN10*Math.exp(-Math.pow(10,x-logMstar))*phi1*Math.pow(10,(x-logMstar)*(alpha1+1)))","parameters":{"logMstar":10.6,"phi1":0.00012,"alpha1":-1.74,"logMstarError":0.15,"phi1Error":0.00004,"alpha1Error":0.02}},"scatter":null,"selection":{"population":"all galaxies","warning":"Least-squares fit by Furlong et al. 2015 to 0.2 dex bins of the Ref-L100N1504 GSMF between 10^8 and 10^12 Msun, Poisson-weighted. Phi* is per unit M/M* (cMpc^-3) as tabulated; the record converts to per dex. Fit, not the simulation curve itself; the fit degeneracies between M* and Phi* are noted by the authors."},"definitions":{"massDefinition":"aperture-30pkpc","imf":"chabrier03","cosmology":{"H0":67.77,"Om":0.307},"densityFrame":"comoving","population":"all"},"provenance":{"tier":"published-fit","citation":"Furlong et al. 2015, MNRAS 450, 4486, Appendix A Table (Schechter fits)","doi":"10.1093/mnras/stv852","url":"https://arxiv.org/abs/1410.3485","retrieved":"2026-10-05","sourceMember":"Appendix.tex table:Schechter (arXiv source, transcribed)"},"calibration":"prediction","rankable":true,"notes":"Transcribed from the paper's table; spot-checked against published values in the script."},{"id":"furlong15.eagle-l100n1504.gsmf-double-schechter.z0.1","source":"EAGLE","run":"Ref-L100N1504 (double Schechter fit)","kind":"simulation","relation":"gsmf","epoch":{"zRepresentative":0.1,"zNominal":0.1,"zMin":0.1,"zMax":0.1,"mode":"published-epoch","snapshot":null},"axes":{"xDefinition":"log10 stellar mass","xUnit":"log10(Msun)","yDefinition":"log10 galaxy number density per dex (double Schechter fit, converted from per-dM)","yUnit":"log10(cMpc^-3 dex^-1)"},"domain":{"xMin":8,"xMax":12},"representation":{"type":"parametric","equation":"Phi_dex = ln(10) exp(-M/M*) [phi1 (M/M*)^(alpha1+1) + phi2 (M/M*)^(alpha2+1)]","expression":"log10(Math.LN10*Math.exp(-Math.pow(10,x-logMstar))*(phi1*Math.pow(10,(x-logMstar)*(alpha1+1))+phi2*Math.pow(10,(x-logMstar)*(alpha2+1))))","parameters":{"logMstar":10.95,"phi1":0.00145,"alpha1":-1.31,"phi2":0,"alpha2":-2.22,"logMstarError":0.03,"phi1Error":0.00012,"alpha1Error":0.03,"phi2Error":0,"alpha2Error":0.22}},"scatter":null,"selection":{"population":"all galaxies","warning":"Least-squares fit by Furlong et al. 2015 to 0.2 dex bins of the Ref-L100N1504 GSMF between 10^8 and 10^12 Msun, Poisson-weighted. Phi* is per unit M/M* (cMpc^-3) as tabulated; the record converts to per dex. Fit, not the simulation curve itself; the fit degeneracies between M* and Phi* are noted by the authors. 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Not rankable: the sample is a selection of rotators and the velocity definition is not the observational one."},{"id":"glowacki20.simba.btfr.box100.polyex.z0","source":"SIMBA","run":"m100n1024, V_polyex fit","kind":"simulation","relation":"btfr","epoch":{"zRepresentative":0,"zNominal":0,"zMin":0,"zMax":0,"mode":"published-epoch","snapshot":null},"axes":{"xDefinition":"log10 rotation velocity, V_polyex (polyex model velocity)","xUnit":"log10(km/s)","yDefinition":"log10 baryonic mass M_bar","yUnit":"log10(Msun)"},"domain":{"xMin":2.1461,"xMax":2.4771},"representation":{"type":"parametric","equation":"log10 M_bar = m log10 V + b (orthogonal maximum-likelihood fit)","expression":"m*x+b","parameters":{"m":3.76,"b":1.64,"log10b200":10.3,"scatterOrthogonalDex":0.056}},"scatter":null,"selection":{"population":"SIMBA galaxies at z=0 with sSFR and HI-mass cuts and M*>5.8e8 Msun (see paper), 100 Mpc/h box only","warning":"Linear fit of Glowacki et al. 2020 over 140 < V < 300 km/s using the V_polyex (polyex model velocity); the stellar mass-to-light adjustment to Upsilon*=0.5 follows the SPARC comparison section. 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Not rankable: the sample is a selection of rotators and the velocity definition is not the observational one."},{"id":"glowacki20.simba.btfr.hires.2re.z0","source":"SIMBA","run":"hires, V_2Re fit","kind":"simulation","relation":"btfr","epoch":{"zRepresentative":0,"zNominal":0,"zMin":0,"zMax":0,"mode":"published-epoch","snapshot":null},"axes":{"xDefinition":"log10 rotation velocity, V_2Re (velocity at twice the effective radius)","xUnit":"log10(km/s)","yDefinition":"log10 baryonic mass M_bar","yUnit":"log10(Msun)"},"domain":{"xMin":2,"xMax":2.4771},"representation":{"type":"parametric","equation":"log10 M_bar = m log10 V + b (orthogonal maximum-likelihood fit)","expression":"m*x+b","parameters":{"m":4.8,"b":-0.29,"log10b200":10.76,"scatterOrthogonalDex":0.052}},"scatter":null,"selection":{"population":"SIMBA galaxies at z=0 with sSFR and HI-mass cuts and M*>5.8e8 Msun (see paper), high-resolution box only (8x better mass resolution)","warning":"Linear fit of Glowacki et al. 2020 over 100 < V < 300 km/s using the V_2Re (velocity at twice the effective radius); the stellar mass-to-light adjustment to Upsilon*=0.5 follows the SPARC comparison section. 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The figure itself (individual galaxies) is not extracted."},"definitions":{"imf":"chabrier03","cosmology":{"H0":68,"Om":0.3},"massDefinition":"baryonic mass as defined in the paper","population":"rotation-supported galaxies (sSFR and HI cuts)","velocityDefinition":"V_2Re (velocity at twice the effective radius)"},"provenance":{"tier":"published-fit","citation":"Glowacki et al. 2020, MNRAS 498, 3687 (arXiv:2003.03402), BTFR best-fit parameters","doi":"10.1093/mnras/staa2616","url":"https://arxiv.org/abs/2003.03402","retrieved":"2026-10-05","checksumSha256":"8f712eee1964c3f68459ea94a04903f2e8fc4e40dc339ea9c641e346957533cc","sourceMember":"main.tex table:btfr_fits (arXiv source, transcribed)","extractionMethod":"transcribed from the arXiv LaTeX table; m, b and b200 cross-checked in the script (m log10(200) + b = log10 b200 within 0.03 dex)","definitionFills":["dave20-simba-imf"]},"calibration":"prediction","rankable":false,"notes":"Transcribed from the paper's table and spot-checked against quoted values in the script. Not rankable: the sample is a selection of rotators and the velocity definition is not the observational one."},{"id":"glowacki20.simba.btfr.hires.max.z0","source":"SIMBA","run":"hires, V_max fit","kind":"simulation","relation":"btfr","epoch":{"zRepresentative":0,"zNominal":0,"zMin":0,"zMax":0,"mode":"published-epoch","snapshot":null},"axes":{"xDefinition":"log10 rotation velocity, V_max (peak of the rotation curve)","xUnit":"log10(km/s)","yDefinition":"log10 baryonic mass M_bar","yUnit":"log10(Msun)"},"domain":{"xMin":2,"xMax":2.4771},"representation":{"type":"parametric","equation":"log10 M_bar = m log10 V + b (orthogonal maximum-likelihood fit)","expression":"m*x+b","parameters":{"m":5.07,"b":-1.11,"log10b200":10.57,"scatterOrthogonalDex":0.034}},"scatter":null,"selection":{"population":"SIMBA galaxies at z=0 with sSFR and HI-mass cuts and M*>5.8e8 Msun (see paper), high-resolution box only (8x better mass resolution)","warning":"Linear fit of Glowacki et al. 2020 over 100 < V < 300 km/s using the V_max (peak of the rotation curve); the stellar mass-to-light adjustment to Upsilon*=0.5 follows the SPARC comparison section. Velocity definitions differ between the four fits, so compare like with like. The figure itself (individual galaxies) is not extracted."},"definitions":{"imf":"chabrier03","cosmology":{"H0":68,"Om":0.3},"massDefinition":"baryonic mass as defined in the paper","population":"rotation-supported galaxies (sSFR and HI cuts)","velocityDefinition":"V_max (peak of the rotation curve)"},"provenance":{"tier":"published-fit","citation":"Glowacki et al. 2020, MNRAS 498, 3687 (arXiv:2003.03402), BTFR best-fit parameters","doi":"10.1093/mnras/staa2616","url":"https://arxiv.org/abs/2003.03402","retrieved":"2026-10-05","checksumSha256":"8f712eee1964c3f68459ea94a04903f2e8fc4e40dc339ea9c641e346957533cc","sourceMember":"main.tex table:btfr_fits (arXiv source, transcribed)","extractionMethod":"transcribed from the arXiv LaTeX table; m, b and b200 cross-checked in the script (m log10(200) + b = log10 b200 within 0.03 dex)","definitionFills":["dave20-simba-imf"]},"calibration":"prediction","rankable":false,"notes":"Transcribed from the paper's table and spot-checked against quoted values in the script. Not rankable: the sample is a selection of rotators and the velocity definition is not the observational one."},{"id":"glowacki20.simba.btfr.hires.flat.z0","source":"SIMBA","run":"hires, V_flat fit","kind":"simulation","relation":"btfr","epoch":{"zRepresentative":0,"zNominal":0,"zMin":0,"zMax":0,"mode":"published-epoch","snapshot":null},"axes":{"xDefinition":"log10 rotation velocity, V_flat (flat part of the rotation curve)","xUnit":"log10(km/s)","yDefinition":"log10 baryonic mass M_bar","yUnit":"log10(Msun)"},"domain":{"xMin":2,"xMax":2.4771},"representation":{"type":"parametric","equation":"log10 M_bar = m log10 V + b (orthogonal maximum-likelihood fit)","expression":"m*x+b","parameters":{"m":4.24,"b":0.98,"log10b200":10.72,"scatterOrthogonalDex":0.067}},"scatter":null,"selection":{"population":"SIMBA galaxies at z=0 with sSFR and HI-mass cuts and M*>5.8e8 Msun (see paper), high-resolution box only (8x better mass resolution)","warning":"Linear fit of Glowacki et al. 2020 over 100 < V < 300 km/s using the V_flat (flat part of the rotation curve); the stellar mass-to-light adjustment to Upsilon*=0.5 follows the SPARC comparison section. 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The figure itself (individual galaxies) is not extracted."},"definitions":{"imf":"chabrier03","cosmology":{"H0":68,"Om":0.3},"massDefinition":"baryonic mass as defined in the paper","population":"rotation-supported galaxies (sSFR and HI cuts)","velocityDefinition":"V_flat (flat part of the rotation curve)"},"provenance":{"tier":"published-fit","citation":"Glowacki et al. 2020, MNRAS 498, 3687 (arXiv:2003.03402), BTFR best-fit parameters","doi":"10.1093/mnras/staa2616","url":"https://arxiv.org/abs/2003.03402","retrieved":"2026-10-05","checksumSha256":"8f712eee1964c3f68459ea94a04903f2e8fc4e40dc339ea9c641e346957533cc","sourceMember":"main.tex table:btfr_fits (arXiv source, transcribed)","extractionMethod":"transcribed from the arXiv LaTeX table; m, b and b200 cross-checked in the script (m log10(200) + b = log10 b200 within 0.03 dex)","definitionFills":["dave20-simba-imf"]},"calibration":"prediction","rankable":false,"notes":"Transcribed from the paper's table and spot-checked against quoted values in the script. Not rankable: the sample is a selection of rotators and the velocity definition is not the observational one."},{"id":"glowacki20.simba.btfr.hires.polyex.z0","source":"SIMBA","run":"hires, V_polyex fit","kind":"simulation","relation":"btfr","epoch":{"zRepresentative":0,"zNominal":0,"zMin":0,"zMax":0,"mode":"published-epoch","snapshot":null},"axes":{"xDefinition":"log10 rotation velocity, V_polyex (polyex model velocity)","xUnit":"log10(km/s)","yDefinition":"log10 baryonic mass M_bar","yUnit":"log10(Msun)"},"domain":{"xMin":2,"xMax":2.4771},"representation":{"type":"parametric","equation":"log10 M_bar = m log10 V + b (orthogonal maximum-likelihood fit)","expression":"m*x+b","parameters":{"m":4.47,"b":0.38,"log10b200":10.67,"scatterOrthogonalDex":0.035}},"scatter":null,"selection":{"population":"SIMBA galaxies at z=0 with sSFR and HI-mass cuts and M*>5.8e8 Msun (see paper), high-resolution box only (8x better mass resolution)","warning":"Linear fit of Glowacki et al. 2020 over 100 < V < 300 km/s using the V_polyex (polyex model velocity); the stellar mass-to-light adjustment to Upsilon*=0.5 follows the SPARC comparison section. Velocity definitions differ between the four fits, so compare like with like. The figure itself (individual galaxies) is not extracted."},"definitions":{"imf":"chabrier03","cosmology":{"H0":68,"Om":0.3},"massDefinition":"baryonic mass as defined in the paper","population":"rotation-supported galaxies (sSFR and HI cuts)","velocityDefinition":"V_polyex (polyex model velocity)"},"provenance":{"tier":"published-fit","citation":"Glowacki et al. 2020, MNRAS 498, 3687 (arXiv:2003.03402), BTFR best-fit parameters","doi":"10.1093/mnras/staa2616","url":"https://arxiv.org/abs/2003.03402","retrieved":"2026-10-05","checksumSha256":"8f712eee1964c3f68459ea94a04903f2e8fc4e40dc339ea9c641e346957533cc","sourceMember":"main.tex table:btfr_fits (arXiv source, transcribed)","extractionMethod":"transcribed from the arXiv LaTeX table; m, b and b200 cross-checked in the script (m log10(200) + b = log10 b200 within 0.03 dex)","definitionFills":["dave20-simba-imf"]},"calibration":"prediction","rankable":false,"notes":"Transcribed from the paper's table and spot-checked against quoted values in the script. Not rankable: the sample is a selection of rotators and the velocity definition is not the observational one."},{"id":"habouzit21.illustris1.bh.z0","source":"Illustris","run":"Illustris-1 (median, Habouzit+21)","kind":"simulation","relation":"bh","epoch":{"zRepresentative":0,"zNominal":0,"zMin":0,"zMax":0,"mode":"published-epoch","snapshot":null},"axes":{"xDefinition":"log10 total stellar mass of the host galaxy","xUnit":"log10(Msun)","yDefinition":"log10 black hole mass","yUnit":"log10(Msun)"},"domain":{"xMin":9.126,"xMax":11.838},"representation":{"type":"points","intervalKind":"scatter","connect":true,"points":[{"x":9.126,"y":5.3175,"yLow":5.1931,"yHigh":5.679},{"x":9.367,"y":5.6659,"yLow":5.3568,"yHigh":6.1402},{"x":9.619,"y":6.0961,"yLow":5.693,"yHigh":6.5376},{"x":9.87,"y":6.4517,"yLow":6.0408,"yHigh":6.861},{"x":10.119,"y":6.7752,"yLow":6.3355,"yHigh":7.1895},{"x":10.366,"y":7.0982,"yLow":6.6739,"yHigh":7.5488},{"x":10.614,"y":7.5095,"yLow":7.0318,"yHigh":7.9751},{"x":10.862,"y":7.9166,"yLow":7.3551,"yHigh":8.3734},{"x":11.108,"y":8.3749,"yLow":7.892,"yHigh":8.7701},{"x":11.352,"y":8.8832,"yLow":8.484,"yHigh":9.2163},{"x":11.595,"y":9.2845,"yLow":9.037,"yHigh":9.5553},{"x":11.838,"y":9.6509,"yLow":9.4265,"yHigh":9.8176}]},"scatter":null,"selection":{"population":"BH-hosting galaxies with M* >= 5e8 Msun (all BHs in the volume)","warning":"Median M_BH in stellar-mass bins with more than 5 galaxies (coloured line, Illustris-1) and the 15th-85th percentile band (offsets read from the lower panel and added to the median) at z=0, read from the vector paths of Habouzit et al. 2021; no table exists. Bins with 5 or fewer galaxies are drawn in the paper as individual points and are not extracted. Galaxies with M* below 5e8 Msun are excluded. 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Transcription cross-checked: M500 from R500 agrees with the M500-Y_X relation used by the papers (mean -0.0080, max 0.0193 dex); the relation refit from these points reproduces the published fit (see fit records)."},{"id":"arnaud10.rexcess.ysz.ysph500.points","source":"Arnaud et al. 2010 (REXCESS)","run":"Y_sph(R500), 31 REXCESS clusters","kind":"observation","relation":"ysz","epoch":{"zRepresentative":0.1181,"zMin":0.0564,"zMax":0.1832,"mode":"observational-bin","snapshot":null},"axes":{"xDefinition":"log10 M500 (mass inside the radius at which the mean density is 500 times the critical density at the cluster redshift; computed from the tabulated R500 and z; R500 iterated from the M500-Y_X relation)","xUnit":"log10(Msun)","yDefinition":"log10 spherically integrated Compton parameter Y_sph(R500) = (sigma_T/m_e c^2) int_0^R500 4 pi P(r) r^2 dr, physical (not E(z)-scaled)","yUnit":"log10(Mpc^2)"},"domain":{"xMin":13.9822,"xMax":14.9246},"representation":{"type":"points","intervalKind":"uncertainty","connect":false,"points":[{"x":13.9822,"y":-5.6253,"yLow":-5.6576,"yHigh":-5.5952},{"x":13.986,"y":-5.644,"yLow":-5.6615,"yHigh":-5.6271},{"x":14.0012,"y":-5.5735,"yLow":-5.5901,"yHigh":-5.5575},{"x":14.085,"y":-5.4461,"yLow":-5.466,"yHigh":-5.4271},{"x":14.1083,"y":-5.3862,"yLow":-5.4023,"yHigh":-5.3706},{"x":14.1185,"y":-5.3979,"yLow":-5.4191,"yHigh":-5.3778},{"x":14.126,"y":-5.3197,"yLow":-5.3382,"yHigh":-5.3019},{"x":14.1928,"y":-5.2132,"yLow":-5.2321,"yHigh":-5.1952},{"x":14.2086,"y":-5.2007,"yLow":-5.2269,"yHigh":-5.1759},{"x":14.2774,"y":-5.0969,"yLow":-5.1186,"yHigh":-5.0762},{"x":14.3244,"y":-5.0044,"yLow":-5.0205,"yHigh":-4.9889},{"x":14.3533,"y":-4.945,"yLow":-4.965,"yHigh":-4.9259},{"x":14.354,"y":-4.9404,"yLow":-4.9602,"yHigh":-4.9215},{"x":14.3567,"y":-4.9212,"yLow":-4.9382,"yHigh":-4.9048},{"x":14.4125,"y":-4.8256,"yLow":-4.8416,"yHigh":-4.8102},{"x":14.4286,"y":-4.8097,"yLow":-4.8242,"yHigh":-4.7956},{"x":14.4318,"y":-4.7886,"yLow":-4.8049,"yHigh":-4.7729},{"x":14.5165,"y":-4.6554,"yLow":-4.672,"yHigh":-4.6394},{"x":14.5568,"y":-4.5832,"yLow":-4.5962,"yHigh":-4.5706},{"x":14.5846,"y":-4.5528,"yLow":-4.5702,"yHigh":-4.5361},{"x":14.5875,"y":-4.5045,"yLow":-4.5243,"yHigh":-4.4855},{"x":14.5963,"y":-4.5143,"yLow":-4.5376,"yHigh":-4.4921},{"x":14.6207,"y":-4.466,"yLow":-4.52,"yHigh":-4.4179},{"x":14.6347,"y":-4.4283,"yLow":-4.4425,"yHigh":-4.4145},{"x":14.6413,"y":-4.4101,"yLow":-4.4306,"yHigh":-4.3904},{"x":14.6923,"y":-4.3063,"yLow":-4.3325,"yHigh":-4.2815},{"x":14.6967,"y":-4.3429,"yLow":-4.3565,"yHigh":-4.3298},{"x":14.7305,"y":-4.2526,"yLow":-4.2708,"yHigh":-4.2351},{"x":14.8669,"y":-4.0545,"yLow":-4.067,"yHigh":-4.0424},{"x":14.8679,"y":-4.0031,"yLow":-4.0241,"yHigh":-3.983},{"x":14.9246,"y":-3.9355,"yLow":-3.9469,"yHigh":-3.9245}]},"scatter":null,"selection":{"population":"31 REXCESS clusters","warning":"Y_sph(R500) per cluster from the REXCESS pressure profiles (31 rows, including RXC J2157.4-0747 that the paper calls bimodal and excludes from the profile analysis) in units of 10^-5 Mpc^2; error bars are the table's 1-sigma errors. Y_sph is the SPHERICAL integral (proportional to the gas thermal energy), not the cylindrical Y_SZ D_A^2. R500 and M500 are from the M500-Y_X relation (hydrostatic-calibrated relaxed clusters), so M500 and Y are not independent of Y_X. M500 is computed from R500 and z."},"definitions":{"haloMassDefinition":"M500crit","massMethod":"M500-Y_X relation (Arnaud+07), calibrated on hydrostatic masses of relaxed clusters; computed from R500 iterated with it","cosmology":{"H0":70,"Om":0.3},"sampleSelection":"REXCESS: 31 nearby clusters selected from REFLEX by X-ray luminosity only (\"selected by luminosity only, in such a way as to have close to homogeneous coverage of luminosity space\"), 0.0564 <= z <= 0.1832; 'Pratt+09: M_Y = mass from the M500-Y_X relation of Arnaud+07'","population":"all","szScaling":"none (physical Y_sph); the paper's relation uses h(z)^(-2/3) Y_sph","szAperture":"spherical, R500","szDefinition":"Y_sph (spherical), not Y_SZ D_A^2 (cylindrical)","pressureProfile":"measured REXCESS pressure profiles (deprojected X-ray electron density times spectroscopic temperature)"},"provenance":{"tier":"published-table","citation":"Arnaud et al. 2010, A&A 517, A92 (arXiv:0910.1234)","doi":"10.1051/0004-6361/200913416","url":"https://arxiv.org/abs/0910.1234","retrieved":"2026-10-18","figure":"table:pnfw (Cluster physical parameters; column Y_sph(R500))","sourceMember":"prexcess_sub.tex","sourceArchiveSha256":"b9a965ef37d1ecedeb5f6fdb6f3c1d6beff0d62f6b5f383c937c3e63ff4833b9","extractionMethod":"values parsed from the LaTeX table(s); M500 computed from tabulated R500 and z with the paper's definition (footnote of Sect. Scaling in Pratt+09)"},"calibration":"validation","rankable":true,"notes":"One point per cluster (31). Transcription cross-checked: M500 from R500 agrees with the M500-Y_X relation used by the papers (mean -0.0080, max 0.0193 dex); the relation refit from these points reproduces the published fit (see fit records)."},{"id":"pratt09.rexcess.lxm.bol-L1.bcesyx","source":"Pratt et al. 2009 (REXCESS fit)","run":"bol-L1: bolometric [0.01-100] keV, with core (R < R500), BCES (Y|X)","kind":"observation","relation":"lxm","epoch":{"zRepresentative":0.1181,"zNominal":0.1181,"zMin":0.0564,"zMax":0.1832,"mode":"analytic-evolution","snapshot":null},"axes":{"xDefinition":"log10 M500 (mass inside the radius at which the mean density is 500 times the critical density at the cluster redshift; computed from the tabulated R500 and z; R500 iterated from the M500-Y_X relation)","xUnit":"log10(Msun)","yDefinition":"log10 X-ray luminosity L1 (bolometric [0.01-100] keV, R < R500); the published h(z)^(-7/3) scaling is re-applied at the epoch, so this is the physical luminosity","yUnit":"log10(erg s^-1)"},"domain":{"xMin":13.99,"xMax":14.9},"representation":{"type":"parametric","equation":"h(z)^(-7/3) L = C (M500 / 2e14 Msun)^alpha, C = 1.81 x 10^44 erg/s, alpha = 1.81  [BCES (Y|X); Pratt+09 table lxrel (bolometric)]","expression":"(7/6)*log10(0.3*(1+z)**3+0.7)+logC+alpha*(x-logM0)","parameters":{"logC":44.25768,"alpha":1.81,"logM0":14.30103},"ageCosmology":{"H0":70,"Om":0.3}},"scatter":null,"selection":{"population":"REXCESS clusters","warning":"Published power-law fit of the raw REXCESS L1-M_Y relation (bolometric [0.01-100] keV, with core (R < R500)); fit method BCES (Y|X). 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Malmquist-bias-corrected rows of the same table are not stored. M is M_Y, the M500 derived from Y_X with the relation of Arnaud+07, so L-M is a Y_X-mass relation. 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Intrinsic scatter is not given for L-M because M is derived from Y_X (table footnote a)."},"definitions":{"haloMassDefinition":"M500crit","massMethod":"M500-Y_X relation (Arnaud+07), calibrated on hydrostatic masses of relaxed clusters; computed from R500 iterated with it","cosmology":{"H0":70,"Om":0.3},"sampleSelection":"REXCESS: 31 nearby clusters selected from REFLEX by X-ray luminosity only (\"selected by luminosity only, in such a way as to have close to homogeneous coverage of luminosity space\"), 0.0564 <= z <= 0.1832; 'Pratt+09: M_Y = mass from the M500-Y_X relation of Arnaud+07'","population":"all","xrayBand":"bolometric [0.01-100] keV","coreTreatment":"core-excised","luminosityAperture":"0.15-1 R500","luminosityScaling":"h(z)^-7/3 = E(z)^-7/3 applied in the fit (E^2 = 0.3 (1+z)^3 + 0.7)","fitMethod":"BCES orthogonal","malmquistBiasCorrection":"none (raw relation of the REXCESS sample)","massDefinition":"M500 from the M500-Y_X relation (M_Y)"},"provenance":{"tier":"published-fit","citation":"Pratt et al. 2009, A&A 498, 361 (arXiv:0809.3784)","doi":"10.1051/0004-6361/200810994","url":"https://arxiv.org/abs/0809.3784","retrieved":"2026-10-18","sourceArchiveSha256":"d3e149ed63839e172348b14a97b7a9221549631534be33a001b83d177e5c66ea"},"calibration":"validation","rankable":true,"notes":"Verified: refitting the 31 table values (M500 computed from R500, z) with orthogonal regression gives alpha = 1.798, C = 1.081 x 10^44 erg/s against the paper's 1.8, 1.08 (negligible measurement errors, so BCES reduces to these)."},{"id":"pratt09.rexcess.lxm.soft-L1.bcesyx","source":"Pratt et al. 2009 (REXCESS fit)","run":"soft-L1: [0.1-2.4] keV (ROSAT band), with core (R < R500), BCES (Y|X)","kind":"observation","relation":"lxm","epoch":{"zRepresentative":0.1181,"zNominal":0.1181,"zMin":0.0564,"zMax":0.1832,"mode":"analytic-evolution","snapshot":null},"axes":{"xDefinition":"log10 M500 (mass inside the radius at which the mean density is 500 times the critical density at the cluster redshift; computed from the tabulated R500 and z; R500 iterated from the M500-Y_X relation)","xUnit":"log10(Msun)","yDefinition":"log10 X-ray luminosity L[0.1-2.4]_1 ([0.1-2.4] keV (ROSAT band), R < R500); the published h(z)^(-7/3) scaling is re-applied at the epoch, so this is the physical luminosity","yUnit":"log10(erg s^-1)"},"domain":{"xMin":13.99,"xMax":14.9},"representation":{"type":"parametric","equation":"h(z)^(-7/3) L = C (M500 / 2e14 Msun)^alpha, C = 1.03 x 10^44 erg/s, alpha = 1.53  [BCES (Y|X); Pratt+09 table lxrelsoft ([0.1-2.4] keV)]","expression":"(7/6)*log10(0.3*(1+z)**3+0.7)+logC+alpha*(x-logM0)","parameters":{"logC":44.01284,"alpha":1.53,"logM0":14.30103},"ageCosmology":{"H0":70,"Om":0.3}},"scatter":null,"selection":{"population":"REXCESS clusters","warning":"Published power-law fit of the raw REXCESS L[0.1-2.4]_1-M_Y relation ([0.1-2.4] keV (ROSAT band), with core (R < R500)); fit method BCES (Y|X). Malmquist-bias-corrected rows of the same table are not stored. M is M_Y, the M500 derived from Y_X with the relation of Arnaud+07, so L-M is a Y_X-mass relation. Intrinsic scatter is not given for L-M because M is derived from Y_X (table footnote a)."},"definitions":{"haloMassDefinition":"M500crit","massMethod":"M500-Y_X relation (Arnaud+07), calibrated on hydrostatic masses of relaxed clusters; computed from R500 iterated with it","cosmology":{"H0":70,"Om":0.3},"sampleSelection":"REXCESS: 31 nearby clusters selected from REFLEX by X-ray luminosity only (\"selected by luminosity only, in such a way as to have close to homogeneous coverage of luminosity space\"), 0.0564 <= z <= 0.1832; 'Pratt+09: M_Y = mass from the M500-Y_X relation of Arnaud+07'","population":"all","xrayBand":"[0.1-2.4] keV (ROSAT band)","coreTreatment":"with core","luminosityAperture":"R < R500","luminosityScaling":"h(z)^-7/3 = E(z)^-7/3 applied in the fit (E^2 = 0.3 (1+z)^3 + 0.7)","fitMethod":"BCES (Y|X)","malmquistBiasCorrection":"none (raw relation of the REXCESS sample)","massDefinition":"M500 from the M500-Y_X relation (M_Y)"},"provenance":{"tier":"published-fit","citation":"Pratt et al. 2009, A&A 498, 361 (arXiv:0809.3784)","doi":"10.1051/0004-6361/200810994","url":"https://arxiv.org/abs/0809.3784","retrieved":"2026-10-18","sourceArchiveSha256":"d3e149ed63839e172348b14a97b7a9221549631534be33a001b83d177e5c66ea"},"calibration":"validation","rankable":true,"notes":"Verified: refitting the 31 table values (M500 computed from R500, z) with ordinary least squares in log-log gives alpha = 1.527, C = 1.033 x 10^44 erg/s against the paper's 1.53, 1.03 (negligible measurement errors, so BCES reduces to these)."},{"id":"pratt09.rexcess.lxm.soft-L1.bcesorth","source":"Pratt et al. 2009 (REXCESS fit)","run":"soft-L1: [0.1-2.4] keV (ROSAT band), with core (R < R500), BCES orthogonal","kind":"observation","relation":"lxm","epoch":{"zRepresentative":0.1181,"zNominal":0.1181,"zMin":0.0564,"zMax":0.1832,"mode":"analytic-evolution","snapshot":null},"axes":{"xDefinition":"log10 M500 (mass inside the radius at which the mean density is 500 times the critical density at the cluster redshift; computed from the tabulated R500 and z; R500 iterated from the M500-Y_X relation)","xUnit":"log10(Msun)","yDefinition":"log10 X-ray luminosity L[0.1-2.4]_1 ([0.1-2.4] keV (ROSAT band), R < R500); the published h(z)^(-7/3) scaling is re-applied at the epoch, so this is the physical luminosity","yUnit":"log10(erg s^-1)"},"domain":{"xMin":13.99,"xMax":14.9},"representation":{"type":"parametric","equation":"h(z)^(-7/3) L = C (M500 / 2e14 Msun)^alpha, C = 0.98 x 10^44 erg/s, alpha = 1.71  [BCES orthogonal; Pratt+09 table lxrelsoft ([0.1-2.4] keV)]","expression":"(7/6)*log10(0.3*(1+z)**3+0.7)+logC+alpha*(x-logM0)","parameters":{"logC":43.99123,"alpha":1.71,"logM0":14.30103},"ageCosmology":{"H0":70,"Om":0.3}},"scatter":null,"selection":{"population":"REXCESS clusters","warning":"Published power-law fit of the raw REXCESS L[0.1-2.4]_1-M_Y relation ([0.1-2.4] keV (ROSAT band), with core (R < R500)); fit method BCES orthogonal. Malmquist-bias-corrected rows of the same table are not stored. M is M_Y, the M500 derived from Y_X with the relation of Arnaud+07, so L-M is a Y_X-mass relation. Intrinsic scatter is not given for L-M because M is derived from Y_X (table footnote a)."},"definitions":{"haloMassDefinition":"M500crit","massMethod":"M500-Y_X relation (Arnaud+07), calibrated on hydrostatic masses of relaxed clusters; computed from R500 iterated with it","cosmology":{"H0":70,"Om":0.3},"sampleSelection":"REXCESS: 31 nearby clusters selected from REFLEX by X-ray luminosity only (\"selected by luminosity only, in such a way as to have close to homogeneous coverage of luminosity space\"), 0.0564 <= z <= 0.1832; 'Pratt+09: M_Y = mass from the M500-Y_X relation of Arnaud+07'","population":"all","xrayBand":"[0.1-2.4] keV (ROSAT band)","coreTreatment":"with core","luminosityAperture":"R < R500","luminosityScaling":"h(z)^-7/3 = E(z)^-7/3 applied in the fit (E^2 = 0.3 (1+z)^3 + 0.7)","fitMethod":"BCES orthogonal","malmquistBiasCorrection":"none (raw relation of the REXCESS sample)","massDefinition":"M500 from the M500-Y_X relation (M_Y)"},"provenance":{"tier":"published-fit","citation":"Pratt et al. 2009, A&A 498, 361 (arXiv:0809.3784)","doi":"10.1051/0004-6361/200810994","url":"https://arxiv.org/abs/0809.3784","retrieved":"2026-10-18","sourceArchiveSha256":"d3e149ed63839e172348b14a97b7a9221549631534be33a001b83d177e5c66ea"},"calibration":"validation","rankable":true,"notes":"Verified: refitting the 31 table values (M500 computed from R500, z) with orthogonal regression gives alpha = 1.706, C = 0.985 x 10^44 erg/s against the paper's 1.71, 0.98 (negligible measurement errors, so BCES reduces to these)."},{"id":"pratt09.rexcess.lxm.soft-L2.bcesyx","source":"Pratt et al. 2009 (REXCESS fit)","run":"soft-L2: [0.1-2.4] keV (ROSAT band), core-excised ([0.15-1] R500), BCES (Y|X)","kind":"observation","relation":"lxm","epoch":{"zRepresentative":0.1181,"zNominal":0.1181,"zMin":0.0564,"zMax":0.1832,"mode":"analytic-evolution","snapshot":null},"axes":{"xDefinition":"log10 M500 (mass inside the radius at which the mean density is 500 times the critical density at the cluster redshift; computed from the tabulated R500 and z; R500 iterated from the M500-Y_X relation)","xUnit":"log10(Msun)","yDefinition":"log10 X-ray luminosity L[0.1-2.4]_2 ([0.1-2.4] keV (ROSAT band), 0.15-1 R500); the published h(z)^(-7/3) scaling is re-applied at the epoch, so this is the physical luminosity","yUnit":"log10(erg s^-1)"},"domain":{"xMin":13.99,"xMax":14.9},"representation":{"type":"parametric","equation":"h(z)^(-7/3) L = C (M500 / 2e14 Msun)^alpha, C = 0.63 x 10^44 erg/s, alpha = 1.49  [BCES (Y|X); Pratt+09 table lxrelsoft ([0.1-2.4] keV)]","expression":"(7/6)*log10(0.3*(1+z)**3+0.7)+logC+alpha*(x-logM0)","parameters":{"logC":43.79934,"alpha":1.49,"logM0":14.30103},"ageCosmology":{"H0":70,"Om":0.3}},"scatter":null,"selection":{"population":"REXCESS clusters","warning":"Published power-law fit of the raw REXCESS L[0.1-2.4]_2-M_Y relation ([0.1-2.4] keV (ROSAT band), core-excised ([0.15-1] R500)); fit method BCES (Y|X). Malmquist-bias-corrected rows of the same table are not stored. M is M_Y, the M500 derived from Y_X with the relation of Arnaud+07, so L-M is a Y_X-mass relation. Intrinsic scatter is not given for L-M because M is derived from Y_X (table footnote a). The row is printed in the paper as 'L[0.1-2.4]_1-M_Y' but sits in the 0.15<R<R500 block of the survey-band table (a typo); it is read as L[0.1-2.4]_2 and the refit of the L_2 values reproduces it."},"definitions":{"haloMassDefinition":"M500crit","massMethod":"M500-Y_X relation (Arnaud+07), calibrated on hydrostatic masses of relaxed clusters; computed from R500 iterated with it","cosmology":{"H0":70,"Om":0.3},"sampleSelection":"REXCESS: 31 nearby clusters selected from REFLEX by X-ray luminosity only (\"selected by luminosity only, in such a way as to have close to homogeneous coverage of luminosity space\"), 0.0564 <= z <= 0.1832; 'Pratt+09: M_Y = mass from the M500-Y_X relation of Arnaud+07'","population":"all","xrayBand":"[0.1-2.4] keV (ROSAT band)","coreTreatment":"core-excised","luminosityAperture":"0.15-1 R500","luminosityScaling":"h(z)^-7/3 = E(z)^-7/3 applied in the fit (E^2 = 0.3 (1+z)^3 + 0.7)","fitMethod":"BCES (Y|X)","malmquistBiasCorrection":"none (raw relation of the REXCESS sample)","massDefinition":"M500 from the M500-Y_X relation (M_Y)"},"provenance":{"tier":"published-fit","citation":"Pratt et al. 2009, A&A 498, 361 (arXiv:0809.3784)","doi":"10.1051/0004-6361/200810994","url":"https://arxiv.org/abs/0809.3784","retrieved":"2026-10-18","sourceArchiveSha256":"d3e149ed63839e172348b14a97b7a9221549631534be33a001b83d177e5c66ea"},"calibration":"validation","rankable":true,"notes":"Verified: refitting the 31 table values (M500 computed from R500, z) with ordinary least squares in log-log gives alpha = 1.488, C = 0.627 x 10^44 erg/s against the paper's 1.49, 0.63 (negligible measurement errors, so BCES reduces to these)."},{"id":"pratt09.rexcess.lxm.soft-L2.bcesorth","source":"Pratt et al. 2009 (REXCESS fit)","run":"soft-L2: [0.1-2.4] keV (ROSAT band), core-excised ([0.15-1] R500), BCES orthogonal","kind":"observation","relation":"lxm","epoch":{"zRepresentative":0.1181,"zNominal":0.1181,"zMin":0.0564,"zMax":0.1832,"mode":"analytic-evolution","snapshot":null},"axes":{"xDefinition":"log10 M500 (mass inside the radius at which the mean density is 500 times the critical density at the cluster redshift; computed from the tabulated R500 and z; R500 iterated from the M500-Y_X relation)","xUnit":"log10(Msun)","yDefinition":"log10 X-ray luminosity L[0.1-2.4]_2 ([0.1-2.4] keV (ROSAT band), 0.15-1 R500); the published h(z)^(-7/3) scaling is re-applied at the epoch, so this is the physical luminosity","yUnit":"log10(erg s^-1)"},"domain":{"xMin":13.99,"xMax":14.9},"representation":{"type":"parametric","equation":"h(z)^(-7/3) L = C (M500 / 2e14 Msun)^alpha, C = 0.62 x 10^44 erg/s, alpha = 1.52  [BCES orthogonal; Pratt+09 table lxrelsoft ([0.1-2.4] keV)]","expression":"(7/6)*log10(0.3*(1+z)**3+0.7)+logC+alpha*(x-logM0)","parameters":{"logC":43.79239,"alpha":1.52,"logM0":14.30103},"ageCosmology":{"H0":70,"Om":0.3}},"scatter":null,"selection":{"population":"REXCESS clusters","warning":"Published power-law fit of the raw REXCESS L[0.1-2.4]_2-M_Y relation ([0.1-2.4] keV (ROSAT band), core-excised ([0.15-1] R500)); fit method BCES orthogonal. Malmquist-bias-corrected rows of the same table are not stored. M is M_Y, the M500 derived from Y_X with the relation of Arnaud+07, so L-M is a Y_X-mass relation. Intrinsic scatter is not given for L-M because M is derived from Y_X (table footnote a). The row is printed in the paper as 'L[0.1-2.4]_1-M_Y' but sits in the 0.15<R<R500 block of the survey-band table (a typo); it is read as L[0.1-2.4]_2 and the refit of the L_2 values reproduces it."},"definitions":{"haloMassDefinition":"M500crit","massMethod":"M500-Y_X relation (Arnaud+07), calibrated on hydrostatic masses of relaxed clusters; computed from R500 iterated with it","cosmology":{"H0":70,"Om":0.3},"sampleSelection":"REXCESS: 31 nearby clusters selected from REFLEX by X-ray luminosity only (\"selected by luminosity only, in such a way as to have close to homogeneous coverage of luminosity space\"), 0.0564 <= z <= 0.1832; 'Pratt+09: M_Y = mass from the M500-Y_X relation of Arnaud+07'","population":"all","xrayBand":"[0.1-2.4] keV (ROSAT band)","coreTreatment":"core-excised","luminosityAperture":"0.15-1 R500","luminosityScaling":"h(z)^-7/3 = E(z)^-7/3 applied in the fit (E^2 = 0.3 (1+z)^3 + 0.7)","fitMethod":"BCES orthogonal","malmquistBiasCorrection":"none (raw relation of the REXCESS sample)","massDefinition":"M500 from the M500-Y_X relation (M_Y)"},"provenance":{"tier":"published-fit","citation":"Pratt et al. 2009, A&A 498, 361 (arXiv:0809.3784)","doi":"10.1051/0004-6361/200810994","url":"https://arxiv.org/abs/0809.3784","retrieved":"2026-10-18","sourceArchiveSha256":"d3e149ed63839e172348b14a97b7a9221549631534be33a001b83d177e5c66ea"},"calibration":"validation","rankable":true,"notes":"Verified: refitting the 31 table values (M500 computed from R500, z) with orthogonal regression gives alpha = 1.523, C = 0.621 x 10^44 erg/s against the paper's 1.52, 0.62 (negligible measurement errors, so BCES reduces to these)."},{"id":"arnaud10.rexcess.ysz.ysph500.fit","source":"Arnaud et al. 2010 (REXCESS fit)","run":"Y_sph(R500)-M500, fit to the REXCESS data","kind":"observation","relation":"ysz","epoch":{"zRepresentative":0.1181,"zNominal":0.1181,"zMin":0.0564,"zMax":0.1832,"mode":"analytic-evolution","snapshot":null},"axes":{"xDefinition":"log10 M500 (mass inside the radius at which the mean density is 500 times the critical density at the cluster redshift; computed from the tabulated R500 and z; R500 iterated from the M500-Y_X relation)","xUnit":"log10(Msun)","yUnit":"log10(Mpc^2)","yDefinition":"log10 spherically integrated Compton parameter Y_sph(R500); the published h(z)^(-2/3) scaling is re-applied at the epoch, so this is the physical Y_sph"},"domain":{"xMin":13.99,"xMax":14.9},"representation":{"type":"parametric","equation":"h(z)^(-2/3) Y_sph(R500) = 10^-4.739 [M500 / (3e14 h70^-1 Msun)]^1.790 h70^-5/2 Mpc^2  (Arnaud+10 eq. mysz500)","expression":"(1/3)*log10(0.3*(1+z)**3+0.7)+logA+alpha*(x-logM0)","parameters":{"logA":-4.739,"alpha":1.79,"logM0":14.47712},"ageCosmology":{"H0":70,"Om":0.3}},"scatter":null,"selection":{"population":"REXCESS clusters","warning":"Published power-law fit to the REXCESS Y_sph(R500) - M500 data. Y_sph is the spherical integral inside R500, not Y_SZ D_A^2. M500 comes from the M500-Y_X relation, so the relation 'does not contain more information than the Y_sph-Y_X relation' (paper). The paper's units carry h70 factors (h70 = 1 here)."},"definitions":{"haloMassDefinition":"M500crit","massMethod":"M500-Y_X relation (Arnaud+07), calibrated on hydrostatic masses of relaxed clusters; computed from R500 iterated with it","cosmology":{"H0":70,"Om":0.3},"sampleSelection":"REXCESS: 31 nearby clusters selected from REFLEX by X-ray luminosity only (\"selected by luminosity only, in such a way as to have close to homogeneous coverage of luminosity space\"), 0.0564 <= z <= 0.1832; 'Pratt+09: M_Y = mass from the M500-Y_X relation of Arnaud+07'","population":"all","szScaling":"h(z)^(-2/3) = E(z)^(-2/3) applied in the fit (E^2 = 0.3 (1+z)^3 + 0.7)","szAperture":"spherical, R500","szDefinition":"Y_sph (spherical)","h70":"H0 = 70, so h70 = 1 and units are Msun and Mpc^2"},"provenance":{"tier":"published-fit","citation":"Arnaud et al. 2010, A&A 517, A92 (arXiv:0910.1234)","doi":"10.1051/0004-6361/200913416","url":"https://arxiv.org/abs/0910.1234","retrieved":"2026-10-18","sourceArchiveSha256":"b9a965ef37d1ecedeb5f6fdb6f3c1d6beff0d62f6b5f383c937c3e63ff4833b9"},"calibration":"validation","rankable":true,"notes":"Verified: refitting the 31 table values (M500 from R500 and z, Y_sph(R500) / E(z)^(2/3)) with orthogonal regression gives slope 1.791 and log A = -4.739 (OLS: 1.789, -4.739), against the paper's 1.790 +/- 0.015 and -4.739 +/- 0.003."},{"id":"arnaud10.rexcess.ysz.ycyl500.universal","source":"Arnaud et al. 2010 (universal profile)","run":"Y_SZ D_A^2-M500, universal GNFW pressure profile, cylindrical, R500 aperture (Y_SZ D_A^2 within R500)","kind":"observation","relation":"ysz","epoch":{"zRepresentative":0.1181,"zNominal":0.1181,"zMin":0.0564,"zMax":0.1832,"mode":"analytic-evolution","snapshot":null},"axes":{"xDefinition":"log10 M500 (mass inside the radius at which the mean density is 500 times the critical density at the cluster redshift; computed from the tabulated R500 and z; R500 iterated from the M500-Y_X relation)","xUnit":"log10(Msun)","yUnit":"log10(Mpc^2)","yDefinition":"log10 Y_SZ D_A^2, cylindrical, R500 aperture (Y_SZ D_A^2 within R500); the published h(z)^(-2/3) scaling is re-applied at the epoch, so this is the physical value"},"domain":{"xMin":13.99,"xMax":14.9},"representation":{"type":"parametric","equation":"h(z)^(-2/3) Y_SZ D_A^2 = B (M500 / (3e14 h70^-1 Msun))^1.78 h70^-1 Mpc^2, log10 B = -4.665 (2.925e-5 x J(1) = 0.7398)  (Arnaud+10 eqs. mysz, Jx)","expression":"(1/3)*log10(0.3*(1+z)**3+0.7)+logB+alpha*(x-logM0)","parameters":{"logB":-4.665,"alpha":1.78,"logM0":14.47712},"ageCosmology":{"H0":70,"Om":0.3}},"scatter":null,"selection":{"population":"REXCESS clusters","warning":"Model relation built by the authors from the universal GNFW pressure profile (REXCESS data plus simulations at large radii) with the mass scaling slope fixed to 1.78 from the M500-Y_X relation; extent R_b = 5 R500 assumed for the cylindrical integral. The paper estimates an uncertainty of +/-0.06 on the slope and +/-0.024 dex on the normalisation. Not a direct measurement of Y_SZ."},"definitions":{"haloMassDefinition":"M500crit","massMethod":"M500-Y_X relation (Arnaud+07), calibrated on hydrostatic masses of relaxed clusters; computed from R500 iterated with it","cosmology":{"H0":70,"Om":0.3},"sampleSelection":"REXCESS: 31 nearby clusters selected from REFLEX by X-ray luminosity only (\"selected by luminosity only, in such a way as to have close to homogeneous coverage of luminosity space\"), 0.0564 <= z <= 0.1832; 'Pratt+09: M_Y = mass from the M500-Y_X relation of Arnaud+07'","population":"all","szScaling":"h(z)^(-2/3) = E(z)^(-2/3) applied in the fit","szAperture":"cylindrical, R500 aperture (Y_SZ D_A^2 within R500)","szDefinition":"Y_SZ D_A^2 (cylindrical) derived from the universal pressure profile with the slope fixed at 1.78","h70":"H0 = 70, so h70 = 1"},"provenance":{"tier":"published-fit","citation":"Arnaud et al. 2010, A&A 517, A92 (arXiv:0910.1234)","doi":"10.1051/0004-6361/200913416","url":"https://arxiv.org/abs/0910.1234","retrieved":"2026-10-18","sourceArchiveSha256":"b9a965ef37d1ecedeb5f6fdb6f3c1d6beff0d62f6b5f383c937c3e63ff4833b9"},"calibration":"validation","rankable":true,"notes":"Verified: the normalisation reproduces the quoted number log B = -4.665 from 2.925e-5 x 0.7398 to 4 digits (quoted constants of the paper: eq. y500, J(1), I(5))."},{"id":"arnaud10.rexcess.ysz.ytot.universal","source":"Arnaud et al. 2010 (universal profile)","run":"Y_SZ D_A^2-M500, universal GNFW pressure profile, total signal, cylindrical aperture 5 R500 (equivalently Y_sph(5 R500))","kind":"observation","relation":"ysz","epoch":{"zRepresentative":0.1181,"zNominal":0.1181,"zMin":0.0564,"zMax":0.1832,"mode":"analytic-evolution","snapshot":null},"axes":{"xDefinition":"log10 M500 (mass inside the radius at which the mean density is 500 times the critical density at the cluster redshift; computed from the tabulated R500 and z; R500 iterated from the M500-Y_X relation)","xUnit":"log10(Msun)","yUnit":"log10(Mpc^2)","yDefinition":"log10 Y_SZ D_A^2, total signal, cylindrical aperture 5 R500 (equivalently Y_sph(5 R500)); the published h(z)^(-2/3) scaling is re-applied at the epoch, so this is the physical value"},"domain":{"xMin":13.99,"xMax":14.9},"representation":{"type":"parametric","equation":"h(z)^(-2/3) Y_SZ D_A^2 = B (M500 / (3e14 h70^-1 Msun))^1.78 h70^-1 Mpc^2, log10 B = -4.491 (2.925e-5 x I(5) = 1.1037)  (Arnaud+10 eqs. mysz, Jx)","expression":"(1/3)*log10(0.3*(1+z)**3+0.7)+logB+alpha*(x-logM0)","parameters":{"logB":-4.491,"alpha":1.78,"logM0":14.47712},"ageCosmology":{"H0":70,"Om":0.3}},"scatter":null,"selection":{"population":"REXCESS clusters","warning":"Model relation built by the authors from the universal GNFW pressure profile (REXCESS data plus simulations at large radii) with the mass scaling slope fixed to 1.78 from the M500-Y_X relation; extent R_b = 5 R500 assumed for the cylindrical integral. 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Verification: the expression with these parameters reproduces the paper's plotted best-fit curve for this bin (rms 0.0024 dex, max 0.0045 dex over [9.01, 11.3]), and the six tabulated gammas span 0.92-1.28 as the abstract's 'low mass power-law slope ranges from 0.9-1.3'.","definitions":{"massDefinition":"sed-total","imf":"unspecified","cosmology":"unspecified","population":"star-forming","sfrIndicator":"total SFR = SFR_IR + SFR_UV, L_IR from Herschel / Spitzer 24 micron / NRK","sfrTimescaleMyr":"unspecified","sfrStatistic":"median"}},{"id":"lee15.cosmos.sfms.z0.63-0.78","source":"Lee et al. 2015 (COSMOS, Herschel/Spitzer/NRK)","run":"best-fit curve, median SFR in 30 stellar-mass bins","kind":"observation","relation":"sfms","epoch":{"zRepresentative":0.7,"zMin":0.63,"zMax":0.78,"mode":"observational-bin","snapshot":null},"axes":{"xDefinition":"log10 stellar mass (SED fitting with BC03 models, Ilbert+13 catalogue; IMF not stated in the paper)","xUnit":"log10(Msun)","yDefinition":"log10 of the median total SFR = 8.6e-11 (L_IR + 2.3 nu L_nu(2300 A)) of star-forming galaxies in a stellar-mass bin; L_IR from Herschel, Spitzer 24 micron or the NRK method (ladder of indicators)","yUnit":"log10(Msun/yr)"},"domain":{"xMin":9,"xMax":11.3},"representation":{"type":"parametric","equation":"S = S0 - log[1 + (10^M / 10^M0)^-gamma], S = log SFR, M = log10 M*/Msun (Eq. 2, Table 1)","expression":"S0-Math.log10(1+Math.pow(10,-gamma*(x-M0)))","parameters":{"S0":1.23,"M0":9.93,"gamma":1.11,"S0Error":0.016,"M0Error":0.031,"gammaError":0.025}},"scatter":{"value":0.36,"unit":"dex","meaning":"standard deviation of the SFRs in each stellar-mass bin, 'sigma ~ 0.36 dex in all bins' (population scatter, not an uncertainty of the curve)"},"selection":{"population":"mass-complete star-forming galaxies, Ks<24 UltraVISTA/COSMOS2015-predecessor catalogue; 'quiescent' = M_NUV-M_r > 3(M_r-M_J)+1 and M_NUV-M_r > 3.1, except IR-detected 'quiescent' galaxies, which are kept as star-forming","warning":"Six equally populated redshift bins; fit to the medians of 30 equally populated mass bins above a 'conservative mass limit' log M* = 9.0; the plotted curve ends at 11.3 (digitised). Reduced chi^2 = 1.48. IMF, cosmology and SFR averaging timescale are not stated in the paper."},"provenance":{"tier":"published-fit","citation":"Lee et al. 2015, ApJ 801, 80 (arXiv:1501.01080), Eq. 2 and Table 1","doi":null,"url":"https://arxiv.org/abs/1501.01080","retrieved":"2026-10-18"},"calibration":"validation","rankable":true,"notes":"Table parsed from the arXiv source. Verification: the expression with these parameters reproduces the paper's plotted best-fit curve for this bin (rms 0.0019 dex, max 0.005 dex over [9.01, 11.3]), and the six tabulated gammas span 0.92-1.28 as the abstract's 'low mass power-law slope ranges from 0.9-1.3'.","definitions":{"massDefinition":"sed-total","imf":"unspecified","cosmology":"unspecified","population":"star-forming","sfrIndicator":"total SFR = SFR_IR + SFR_UV, L_IR from Herschel / Spitzer 24 micron / NRK","sfrTimescaleMyr":"unspecified","sfrStatistic":"median"}},{"id":"lee15.cosmos.sfms.z0.78-0.93","source":"Lee et al. 2015 (COSMOS, Herschel/Spitzer/NRK)","run":"best-fit curve, median SFR in 30 stellar-mass bins","kind":"observation","relation":"sfms","epoch":{"zRepresentative":0.85,"zMin":0.78,"zMax":0.93,"mode":"observational-bin","snapshot":null},"axes":{"xDefinition":"log10 stellar mass (SED fitting with BC03 models, Ilbert+13 catalogue; IMF not stated in the paper)","xUnit":"log10(Msun)","yDefinition":"log10 of the median total SFR = 8.6e-11 (L_IR + 2.3 nu L_nu(2300 A)) of star-forming galaxies in a stellar-mass bin; L_IR from Herschel, Spitzer 24 micron or the NRK method (ladder of indicators)","yUnit":"log10(Msun/yr)"},"domain":{"xMin":9.3,"xMax":11.3},"representation":{"type":"parametric","equation":"S = S0 - log[1 + (10^M / 10^M0)^-gamma], S = log SFR, M = log10 M*/Msun (Eq. 2, Table 1)","expression":"S0-Math.log10(1+Math.pow(10,-gamma*(x-M0)))","parameters":{"S0":1.35,"M0":9.96,"gamma":1.28,"S0Error":0.014,"M0Error":0.025,"gammaError":0.034}},"scatter":{"value":0.36,"unit":"dex","meaning":"standard deviation of the SFRs in each stellar-mass bin, 'sigma ~ 0.36 dex in all bins' (population scatter, not an uncertainty of the curve)"},"selection":{"population":"mass-complete star-forming galaxies, Ks<24 UltraVISTA/COSMOS2015-predecessor catalogue; 'quiescent' = M_NUV-M_r > 3(M_r-M_J)+1 and M_NUV-M_r > 3.1, except IR-detected 'quiescent' galaxies, which are kept as star-forming","warning":"Six equally populated redshift bins; fit to the medians of 30 equally populated mass bins above a 'conservative mass limit' log M* = 9.3; the plotted curve ends at 11.3 (digitised). Reduced chi^2 = 1.84. IMF, cosmology and SFR averaging timescale are not stated in the paper."},"provenance":{"tier":"published-fit","citation":"Lee et al. 2015, ApJ 801, 80 (arXiv:1501.01080), Eq. 2 and Table 1","doi":null,"url":"https://arxiv.org/abs/1501.01080","retrieved":"2026-10-18"},"calibration":"validation","rankable":true,"notes":"Table parsed from the arXiv source. Verification: the expression with these parameters reproduces the paper's plotted best-fit curve for this bin (rms 0.0012 dex, max 0.0027 dex over [9.31, 11.3]), and the six tabulated gammas span 0.92-1.28 as the abstract's 'low mass power-law slope ranges from 0.9-1.3'.","definitions":{"massDefinition":"sed-total","imf":"unspecified","cosmology":"unspecified","population":"star-forming","sfrIndicator":"total SFR = SFR_IR + SFR_UV, L_IR from Herschel / Spitzer 24 micron / NRK","sfrTimescaleMyr":"unspecified","sfrStatistic":"median"}},{"id":"lee15.cosmos.sfms.z0.93-1.11","source":"Lee et al. 2015 (COSMOS, Herschel/Spitzer/NRK)","run":"best-fit curve, median SFR in 30 stellar-mass bins","kind":"observation","relation":"sfms","epoch":{"zRepresentative":0.99,"zMin":0.93,"zMax":1.11,"mode":"observational-bin","snapshot":null},"axes":{"xDefinition":"log10 stellar mass (SED fitting with BC03 models, Ilbert+13 catalogue; IMF not stated in the paper)","xUnit":"log10(Msun)","yDefinition":"log10 of the median total SFR = 8.6e-11 (L_IR + 2.3 nu L_nu(2300 A)) of star-forming galaxies in a stellar-mass bin; L_IR from Herschel, Spitzer 24 micron or the NRK method (ladder of indicators)","yUnit":"log10(Msun/yr)"},"domain":{"xMin":9.3,"xMax":11.3},"representation":{"type":"parametric","equation":"S = S0 - log[1 + (10^M / 10^M0)^-gamma], S = log SFR, M = log10 M*/Msun (Eq. 2, Table 1)","expression":"S0-Math.log10(1+Math.pow(10,-gamma*(x-M0)))","parameters":{"S0":1.53,"M0":10.1,"gamma":1.26,"S0Error":0.017,"M0Error":0.029,"gammaError":0.032}},"scatter":{"value":0.36,"unit":"dex","meaning":"standard deviation of the SFRs in each stellar-mass bin, 'sigma ~ 0.36 dex in all bins' (population scatter, not an uncertainty of the curve)"},"selection":{"population":"mass-complete star-forming galaxies, Ks<24 UltraVISTA/COSMOS2015-predecessor catalogue; 'quiescent' = M_NUV-M_r > 3(M_r-M_J)+1 and M_NUV-M_r > 3.1, except IR-detected 'quiescent' galaxies, which are kept as star-forming","warning":"Six equally populated redshift bins; fit to the medians of 30 equally populated mass bins above a 'conservative mass limit' log M* = 9.3; the plotted curve ends at 11.3 (digitised). Reduced chi^2 = 0.62. IMF, cosmology and SFR averaging timescale are not stated in the paper."},"provenance":{"tier":"published-fit","citation":"Lee et al. 2015, ApJ 801, 80 (arXiv:1501.01080), Eq. 2 and Table 1","doi":null,"url":"https://arxiv.org/abs/1501.01080","retrieved":"2026-10-18"},"calibration":"validation","rankable":true,"notes":"Table parsed from the arXiv source. Verification: the expression with these parameters reproduces the paper's plotted best-fit curve for this bin (rms 0.0052 dex, max 0.0064 dex over [9.31, 11.3]), and the six tabulated gammas span 0.92-1.28 as the abstract's 'low mass power-law slope ranges from 0.9-1.3'.","definitions":{"massDefinition":"sed-total","imf":"unspecified","cosmology":"unspecified","population":"star-forming","sfrIndicator":"total SFR = SFR_IR + SFR_UV, L_IR from Herschel / Spitzer 24 micron / NRK","sfrTimescaleMyr":"unspecified","sfrStatistic":"median"}},{"id":"lee15.cosmos.sfms.z1.11-1.3","source":"Lee et al. 2015 (COSMOS, Herschel/Spitzer/NRK)","run":"best-fit curve, median SFR in 30 stellar-mass bins","kind":"observation","relation":"sfms","epoch":{"zRepresentative":1.19,"zMin":1.11,"zMax":1.3,"mode":"observational-bin","snapshot":null},"axes":{"xDefinition":"log10 stellar mass (SED fitting with BC03 models, Ilbert+13 catalogue; IMF not stated in the paper)","xUnit":"log10(Msun)","yDefinition":"log10 of the median total SFR = 8.6e-11 (L_IR + 2.3 nu L_nu(2300 A)) of star-forming galaxies in a stellar-mass bin; L_IR from Herschel, Spitzer 24 micron or the NRK method (ladder of indicators)","yUnit":"log10(Msun/yr)"},"domain":{"xMin":9.3,"xMax":11.3},"representation":{"type":"parametric","equation":"S = S0 - log[1 + (10^M / 10^M0)^-gamma], S = log SFR, M = log10 M*/Msun (Eq. 2, Table 1)","expression":"S0-Math.log10(1+Math.pow(10,-gamma*(x-M0)))","parameters":{"S0":1.72,"M0":10.31,"gamma":1.07,"S0Error":0.024,"M0Error":0.043,"gammaError":0.028}},"scatter":{"value":0.36,"unit":"dex","meaning":"standard deviation of the SFRs in each stellar-mass bin, 'sigma ~ 0.36 dex in all bins' (population scatter, not an uncertainty of the curve)"},"selection":{"population":"mass-complete star-forming galaxies, Ks<24 UltraVISTA/COSMOS2015-predecessor catalogue; 'quiescent' = M_NUV-M_r > 3(M_r-M_J)+1 and M_NUV-M_r > 3.1, except IR-detected 'quiescent' galaxies, which are kept as star-forming","warning":"Six equally populated redshift bins; fit to the medians of 30 equally populated mass bins above a 'conservative mass limit' log M* = 9.3; the plotted curve ends at 11.3 (digitised). Reduced chi^2 = 1.24. IMF, cosmology and SFR averaging timescale are not stated in the paper."},"provenance":{"tier":"published-fit","citation":"Lee et al. 2015, ApJ 801, 80 (arXiv:1501.01080), Eq. 2 and Table 1","doi":null,"url":"https://arxiv.org/abs/1501.01080","retrieved":"2026-10-18"},"calibration":"validation","rankable":true,"notes":"Table parsed from the arXiv source. Verification: the expression with these parameters reproduces the paper's plotted best-fit curve for this bin (rms 0.0079 dex, max 0.0133 dex over [9.31, 11.3]), and the six tabulated gammas span 0.92-1.28 as the abstract's 'low mass power-law slope ranges from 0.9-1.3'.","definitions":{"massDefinition":"sed-total","imf":"unspecified","cosmology":"unspecified","population":"star-forming","sfrIndicator":"total SFR = SFR_IR + SFR_UV, L_IR from Herschel / Spitzer 24 micron / NRK","sfrTimescaleMyr":"unspecified","sfrStatistic":"median"}},{"id":"leja22.prospector.sfms.ridge.evolution","source":"Leja et al. 2022 (COSMOS-2015 + 3D-HST, Prospector-alpha)","run":"ridge, broken power law","kind":"observation","relation":"sfms","epoch":{"zRepresentative":1,"zMin":0.2,"zMax":3,"mode":"analytic-evolution","snapshot":null},"axes":{"xDefinition":"log10 stellar mass from Prospector-alpha SED fitting (Chabrier IMF)","xUnit":"log10(Msun)","yDefinition":"log10 SFR averaged over the most recent 100 Myr, ridge (mode of the SFR distribution at fixed mass and redshift) of the full galaxy population, no star-forming pre-selection","yUnit":"log10(Msun/yr)"},"domain":{"xMin":8.82,"xMax":11.3},"representation":{"type":"parametric","equation":"log SFR = a (M - Mt) + c for M > Mt and b (M - Mt) + c for M <= Mt, M = log10 M*/Msun; each of a, b, c, Mt = X0 + X1 z + X2 z^2 (Eq. 3-4, Table 1)","expression":"((a0+a1*z+a2*z*z)*(x-(Mt0+Mt1*z+Mt2*z*z))*(x>(Mt0+Mt1*z+Mt2*z*z)?1:0)+(b0+b1*z+b2*z*z)*(x-(Mt0+Mt1*z+Mt2*z*z))*(x>(Mt0+Mt1*z+Mt2*z*z)?0:1)+(c0+c1*z+c2*z*z))","parameters":{"a0":0.03746,"a1":0.3448,"a2":-0.1156,"a0Error":0.01739,"a1Error":0.0297,"a2Error":0.0107,"b0":0.9605,"b1":0.0499,"b2":-0.05984,"b0Error":0.01,"b1Error":0.01518,"b2Error":0.00482,"c0":0.2516,"c1":1.118,"c2":-0.2006,"c0Error":0.0082,"c1Error":0.013,"c2Error":0.0039,"Mt0":10.22,"Mt1":0.3826,"Mt2":-0.04491,"Mt0Error":0.01,"Mt1Error":0.0188,"Mt2Error":0.00613}},"scatter":null,"selection":{"population":"all galaxies (no star-forming pre-selection); the ridge is the density peak of the star-forming sequence","warning":"Fit to the normalizing-flow density field over 0.2<z<3.0, mass-complete samples (COSMOS-2015 at 0.2<z<0.8, 3D-HST at 0.5<z<3.0; limits from Leja+20, raised by 0.1-0.25 dex at some redshifts). Mass range shown in the paper's fit figure is log M* = 8.82 to 11.3; this range is read from the digitised plot, the paper does not state it. Deviations of the fit from the density field are <~0.1 dex (paper). SED-based SFRs and masses (Prospector-alpha, nonparametric continuity SFH) sit 0.2-0.5 dex below UV+IR based sequences, see the paper's Section 5."},"provenance":{"tier":"published-fit","citation":"Leja et al. 2022, ApJ 936, 165 (arXiv:2110.04314), Eqs. 3-4 and Table 1","doi":null,"url":"https://arxiv.org/abs/2110.04314","retrieved":"2026-10-18"},"calibration":"validation","rankable":true,"notes":"Coefficients parsed from the arXiv source Table 1. Verification: the expression with the quoted coefficients reproduces the six solid fit lines of the paper's parameterized-moments figure (z=0.3, 0.6, 1.0, 1.5, 2.0, 2.7) with rms 0.002-0.004 dex (max 0.006), and a free fit of z to each line returns the legend redshift to <=0.012. The plotted lines start at log M* = {\"0.3\": 8.99, \"0.6\": 8.82, \"1.0\": 9.07, \"1.5\": 9.64, \"2.0\": 9.86, \"2.7\": 10.08} (by redshift; the mass-complete limits) and end at 11.3. Cosmology: Om = Omega_b + Omega_c = 0.0464 + 0.235 = 0.2814 (WMAP9, H0=69.7). The paper does not say here whether the stellar mass is the surviving or the formed mass.","definitions":{"massDefinition":"sed-total","imf":"chabrier03","cosmology":{"H0":69.7,"Om":0.2814},"population":"all","sfrIndicator":"Prospector-alpha SED fit to 0.2-24 micron photometry","sfrTimescaleMyr":100,"sfrStatistic":"mode"}},{"id":"leja22.prospector.sfms.mean.evolution","source":"Leja et al. 2022 (COSMOS-2015 + 3D-HST, Prospector-alpha)","run":"mean, broken power law","kind":"observation","relation":"sfms","epoch":{"zRepresentative":1,"zMin":0.2,"zMax":3,"mode":"analytic-evolution","snapshot":null},"axes":{"xDefinition":"log10 stellar mass from Prospector-alpha SED fitting (Chabrier IMF)","xUnit":"log10(Msun)","yDefinition":"log10 SFR averaged over the most recent 100 Myr, mean SFR (not mean log SFR) of the full galaxy population including quiescent galaxies","yUnit":"log10(Msun/yr)"},"domain":{"xMin":8.82,"xMax":11.3},"representation":{"type":"parametric","equation":"log SFR = a (M - Mt) + c for M > Mt and b (M - Mt) + c for M <= Mt, M = log10 M*/Msun; each of a, b, c, Mt = X0 + X1 z + X2 z^2 (Eq. 3-4, Table 1)","expression":"((a0+a1*z+a2*z*z)*(x-(Mt0+Mt1*z+Mt2*z*z))*(x>(Mt0+Mt1*z+Mt2*z*z)?1:0)+(b0+b1*z+b2*z*z)*(x-(Mt0+Mt1*z+Mt2*z*z))*(x>(Mt0+Mt1*z+Mt2*z*z)?0:1)+(c0+c1*z+c2*z*z))","parameters":{"a0":-0.06707,"a1":0.3684,"a2":-0.1047,"a0Error":0.00821,"a1Error":0.0128,"a2Error":0.0044,"b0":0.8552,"b1":-0.101,"b2":-0.001816,"b0Error":0.0068,"b1Error":0.0107,"b2Error":0.00329,"c0":0.2148,"c1":0.8137,"c2":-0.08052,"c0Error":0.0045,"c1Error":0.0069,"c2Error":0.00219,"Mt0":10.29,"Mt1":-0.1284,"Mt2":0.1203,"Mt0Error":0.01,"Mt1Error":0.0135,"Mt2Error":0.0044}},"scatter":null,"selection":{"population":"all galaxies including quiescent","warning":"Fit to the normalizing-flow density field over 0.2<z<3.0, mass-complete samples (COSMOS-2015 at 0.2<z<0.8, 3D-HST at 0.5<z<3.0; limits from Leja+20, raised by 0.1-0.25 dex at some redshifts). Mass range shown in the paper's fit figure is log M* = 8.82 to 11.3; this range is read from the digitised plot, the paper does not state it. Deviations of the fit from the density field are <~0.1 dex (paper). SED-based SFRs and masses (Prospector-alpha, nonparametric continuity SFH) sit 0.2-0.5 dex below UV+IR based sequences, see the paper's Section 5."},"provenance":{"tier":"published-fit","citation":"Leja et al. 2022, ApJ 936, 165 (arXiv:2110.04314), Eqs. 3-4 and Table 1","doi":null,"url":"https://arxiv.org/abs/2110.04314","retrieved":"2026-10-18"},"calibration":"validation","rankable":true,"notes":"Coefficients parsed from the arXiv source Table 1. Verification: the expression with the quoted coefficients reproduces the six solid fit lines of the paper's parameterized-moments figure (z=0.3, 0.6, 1.0, 1.5, 2.0, 2.7) with rms 0.002-0.004 dex (max 0.006), and a free fit of z to each line returns the legend redshift to <=0.012. The plotted lines start at log M* = {\"0.3\": 8.99, \"0.6\": 8.82, \"1.0\": 9.07, \"1.5\": 9.64, \"2.0\": 9.86, \"2.7\": 10.08} (by redshift; the mass-complete limits) and end at 11.3. Cosmology: Om = Omega_b + Omega_c = 0.0464 + 0.235 = 0.2814 (WMAP9, H0=69.7). The paper does not say here whether the stellar mass is the surviving or the formed mass.","definitions":{"massDefinition":"sed-total","imf":"chabrier03","cosmology":{"H0":69.7,"Om":0.2814},"population":"all","sfrIndicator":"Prospector-alpha SED fit to 0.2-24 micron photometry","sfrTimescaleMyr":100,"sfrStatistic":"mean"}},{"id":"schreiber15.goods-candels-cosmos.sfms.evolution","source":"Schreiber et al. 2015 (Herschel stacking)","run":null,"kind":"observation","relation":"sfms","epoch":{"zRepresentative":2,"zMin":0.3,"zMax":5,"mode":"analytic-evolution","snapshot":null},"axes":{"xDefinition":"log10 stellar mass (FAST, Bruzual & Charlot 2003, Salpeter IMF, delayed-exponential SFHs)","xUnit":"log10(Msun)","yDefinition":"log10 of the mode of the SFR distribution of star-forming galaxies, SFR = SFR_UV (uncorrected, Daddi+04) + SFR_IR (Kennicutt98), Salpeter IMF, from mean Herschel stacks corrected to the mode (about -0.1 dex)","yUnit":"log10(Msun/yr)"},"domain":{"xMin":9.74,"xMax":11.21},"representation":{"type":"parametric","equation":"log10 SFR_MS = m - m0 + a0 r - a1 [max(0, m - m1 - a2 r)]^2, m = log10(M*/1e9 Msun), r = log10(1+z) (Eq. 7)","expression":"(x-9)-m0+a0*Math.log10(1+z)-a1*Math.pow(Math.max(0,(x-9)-m1-a2*Math.log10(1+z)),2)","parameters":{"m0":0.5,"a0":1.5,"a1":0.3,"m1":0.36,"a2":2.5,"m0Error":0.07,"a0Error":0.15,"a1Error":0.08,"m1Error":0.3,"a2Error":0.6}},"scatter":{"value":0.3,"unit":"dex","meaning":"non-varying dispersion of log SFR at fixed mass and redshift from scatter stacking (0.30 +-0.06 Herschel; 0.33 +-0.03 COSMOS UltraVISTA), not an uncertainty of the curve"},"selection":{"population":"mass-complete star-forming galaxies selected with the UVJ criterion (U-V>1.3, V-J<1.6, U-V>0.88(V-J)+0.49 = quiescent), GOODS-N/S, UDS, COSMOS CANDELS H-band and GOODS-N/COSMOS UltraVISTA Ks-band catalogues","warning":"The fit was made to the filled circles of Fig. 8 (stacked mass/redshift bins with 0.3<z<5.0 in six redshift bins); the stacks span log M* = 9.74 to 11.21, so the expression is an extrapolation outside this mass range and outside 0.3<z<5.0. The paper's text says the catalogue is mass-complete above 2e10 Msun and extends to z=4. Abstract: flattening at log M* > 10.5. Quiescent galaxies, not AGN, are excluded."},"provenance":{"tier":"published-fit","citation":"Schreiber et al. 2015, A&A 575, A74 (arXiv:1409.5433), Eq. 7","doi":null,"url":"https://arxiv.org/abs/1409.5433","retrieved":"2026-10-18"},"calibration":"validation","rankable":true,"notes":"Analytic redshift evolution (variable z in the expression). Verification: parameters parsed from the arXiv source; the expression, evaluated at the legend bin centres, reproduces the six grey best-fit curves of the paper's Fig. 8 with rms 0.007-0.016 dex and maximum 0.04 dex (digitisation of vector paths, axes calibrated on tick marks).","definitions":{"massDefinition":"sed-total","imf":"salpeter55","cosmology":{"H0":70,"Om":0.3},"population":"star-forming","sfrIndicator":"UV (uncorrected, 1500 A) + IR (Herschel stacks, CE01 templates), L_IR from 24-500 micron stacks","sfrTimescaleMyr":100,"sfrTimescaleBasis":"'assume that the SFR remained constant over the last 100 Myr'","sfrStatistic":"mode","sfrStatisticBasis":"'in all the following we refer to the SFR of the main sequence as the mode of the distribution'"}},{"id":"tomczak16.zfourge.sfms.all.evolution","source":"Tomczak et al. 2016 (ZFOURGE)","run":"all galaxies (star-forming plus quiescent)","kind":"observation","relation":"sfms","epoch":{"zRepresentative":2,"zMin":0.5,"zMax":4,"mode":"analytic-evolution","snapshot":null},"axes":{"xDefinition":"log10 stellar mass (FAST, Bruzual & Charlot 2003, Chabrier IMF, solar metallicity)","xUnit":"log10(Msun)","yDefinition":"log10 UV+IR SFR (Psi = 1.09e-10 (L_IR + 2.2 L_UV), Chabrier IMF) of the median UV luminosity plus stacked 24-160 micron IR luminosity in bins of mass and redshift","yUnit":"log10(Msun/yr)"},"domain":{"xMin":8.62,"xMax":11.38},"representation":{"type":"parametric","equation":"log Psi = s0 - log[1 + (M*/M0)^-gamma] (Eq. 1, Lee+15 form); s0 = a + b z + c z^2 and log M0 = a + b z + c z^2 (Eq. 2-3), gamma constant (fixed-gamma fit)","expression":"(s00+s01*z+s02*z*z)-Math.log10(1+Math.pow(10,-gamma*(x-(logM00+logM01*z+logM02*z*z))))","parameters":{"s00":0.195,"s01":1.157,"s02":-0.143,"logM00":9.244,"logM01":0.753,"logM02":-0.09,"gamma":1.118}},"scatter":null,"selection":{"population":"all galaxies (star-forming plus quiescent), ZFOURGE (CDFS, COSMOS, UDS) with Spitzer 24 micron and Herschel 100/160 micron stacking","warning":"Valid for 0.5<z<4 and the stacked mass ranges; the authors warn that the parameterization 'may not extrapolate well outside of the z and/or stellar mass ranges used here'. Digitised start of the fitted lines (log M*, by z bin): {\"0.5-0.75\": 8.62, \"0.75-1.0\": 8.62, \"1.0-1.25\": 8.62, \"1.25-1.5\": 8.62, \"1.5-2.0\": 9.12, \"2.0-2.5\": 9.38, \"2.5-3.0\": 9.62, \"3.0-4.0\": 9.88}; end 11.38. The SFR of each bin is built from the median UV luminosity and the stacked IR luminosity of the bin. The 'all galaxies' relation includes quiescent galaxies (the turnover mass may be influenced by the growing quiescent population, as the authors note)."},"provenance":{"tier":"published-fit","citation":"Tomczak et al. 2016, ApJ 817, 118 (arXiv:1510.06072), Eqs. 1-3","doi":null,"url":"https://arxiv.org/abs/1510.06072","retrieved":"2026-10-18"},"calibration":"validation","rankable":true,"notes":"Coefficients parsed from the arXiv source. Verification: the expression reproduces the eight redshift-parameterised curves of the paper's Fig. 7 at the bin-centre redshifts with rms 0.0003-0.0032 dex (max 0.005) and a free fit of z returns the bin centres; it matches the paper's Table 4 stacked SFRs with rms 0.083 dex over all 80 stacks (including bins below the completeness limit).","definitions":{"massDefinition":"sed-total","imf":"chabrier03","cosmology":{"H0":70,"Om":0.3},"population":"all","sfrIndicator":"UV+IR (Bell05 conversion scaled to Chabrier; L_IR from Wuyts08 template fitted to stacked 24-160 micron photometry)","sfrTimescaleMyr":"unspecified","sfrStatistic":"unspecified","sfrStatisticNote":"'we aim to measure the average star-formation rate of galaxies in bins of z and stellar mass'; median L_UV, stacked L_IR"}},{"id":"tomczak16.zfourge.sfms.sf.evolution","source":"Tomczak et al. 2016 (ZFOURGE)","run":"UVJ-selected star-forming galaxies","kind":"observation","relation":"sfms","epoch":{"zRepresentative":2,"zMin":0.5,"zMax":4,"mode":"analytic-evolution","snapshot":null},"axes":{"xDefinition":"log10 stellar mass (FAST, Bruzual & Charlot 2003, Chabrier IMF, solar metallicity)","xUnit":"log10(Msun)","yDefinition":"log10 UV+IR SFR (Psi = 1.09e-10 (L_IR + 2.2 L_UV), Chabrier IMF) of the median UV luminosity plus stacked 24-160 micron IR luminosity in bins of mass and redshift","yUnit":"log10(Msun/yr)"},"domain":{"xMin":8.62,"xMax":11.38},"representation":{"type":"parametric","equation":"log Psi = s0 - log[1 + (M*/M0)^-gamma] (Eq. 1, Lee+15 form); s0 = a + b z + c z^2 and log M0 = a + b z + c z^2 (Eq. 2-3), gamma constant (fixed-gamma fit)","expression":"(s00+s01*z+s02*z*z)-Math.log10(1+Math.pow(10,-gamma*(x-(logM00+logM01*z+logM02*z*z))))","parameters":{"s00":0.448,"s01":1.22,"s02":-0.174,"logM00":9.458,"logM01":0.865,"logM02":-0.132,"gamma":1.091}},"scatter":null,"selection":{"population":"UVJ-selected star-forming galaxies, ZFOURGE (CDFS, COSMOS, UDS) with Spitzer 24 micron and Herschel 100/160 micron stacking","warning":"Valid for 0.5<z<4 and the stacked mass ranges; the authors warn that the parameterization 'may not extrapolate well outside of the z and/or stellar mass ranges used here'. Digitised start of the fitted lines (log M*, by z bin): {\"0.5-0.75\": 8.62, \"0.75-1.0\": 8.62, \"1.0-1.25\": 8.62, \"1.25-1.5\": 8.62, \"1.5-2.0\": 9.12, \"2.0-2.5\": 9.38, \"2.5-3.0\": 9.62, \"3.0-4.0\": 9.88}; end 11.38. The SFR of each bin is built from the median UV luminosity and the stacked IR luminosity of the bin. The 'all galaxies' relation includes quiescent galaxies (the turnover mass may be influenced by the growing quiescent population, as the authors note)."},"provenance":{"tier":"published-fit","citation":"Tomczak et al. 2016, ApJ 817, 118 (arXiv:1510.06072), Eqs. 1-3","doi":null,"url":"https://arxiv.org/abs/1510.06072","retrieved":"2026-10-18"},"calibration":"validation","rankable":true,"notes":"Coefficients parsed from the arXiv source. Verification: the expression reproduces the eight redshift-parameterised curves of the paper's Fig. 8 at the bin-centre redshifts with rms 0.0003-0.0032 dex (max 0.005) and a free fit of z returns the bin centres; it matches the paper's Table 4 stacked SFRs with rms 0.074 dex over all 80 stacks (including bins below the completeness limit).","definitions":{"massDefinition":"sed-total","imf":"chabrier03","cosmology":{"H0":70,"Om":0.3},"population":"star-forming","sfrIndicator":"UV+IR (Bell05 conversion scaled to Chabrier; L_IR from Wuyts08 template fitted to stacked 24-160 micron photometry)","sfrTimescaleMyr":"unspecified","sfrStatistic":"unspecified","sfrStatisticNote":"'we aim to measure the average star-formation rate of galaxies in bins of z and stellar mass'; median L_UV, stacked L_IR"}},{"id":"whitaker14.3dhst.sfms.bpl.z0.5-1","source":"Whitaker et al. 2014 (3D-HST/CANDELS)","run":"broken power law, median stacks","kind":"observation","relation":"sfms","epoch":{"zRepresentative":0.75,"zMin":0.5,"zMax":1,"mode":"observational-bin","snapshot":null},"axes":{"xDefinition":"log10 stellar mass (FAST, Bruzual & Charlot 2003, Chabrier IMF, emission-line corrected)","xUnit":"log10(Msun)","yDefinition":"log10 UV+IR SFR (Psi = 1.09e-10 (L_IR + 2.2 L_UV) Lsun, Chabrier IMF) of the median 24um-stack plus median UV luminosity of star-forming galaxies in the mass bin","yUnit":"log10(Msun/yr)"},"domain":{"xMin":8.4,"xMax":11.1},"representation":{"type":"parametric","equation":"log Psi = a [log(M*/Msun) - 10.2] + b, with a = a_low below and a_high above log M* = 10.2 (Eq. 2, Table 2)","expression":"b+alow*Math.min(x-10.2,0)+ahigh*Math.max(x-10.2,0)","parameters":{"alow":0.94,"ahigh":0.14,"b":1.11,"alowError":0.03,"ahighError":0.08,"bError":0.03}},"scatter":null,"selection":{"population":"UVJ-selected star-forming galaxies above the 90% mass-completeness limits, 3D-HST v4.0 / CANDELS (five fields)","warning":"Fit to median stacked UV+IR SFRs in 0.2 dex mass bins; the SFR of each bin includes MIPS-undetected galaxies through stacking. The paper does not measure the intrinsic scatter. The break mass 10.2 is fixed. zRepresentative is the bin centre. The paper's quadratic (Table 1) is not stored: its two-decimal coefficients do not reproduce the paper's own Table 3 (see M1 notes)."},"provenance":{"tier":"published-fit","citation":"Whitaker et al. 2014, ApJ 795, 104 (arXiv:1407.1843), Eq. 2 and Table 2","doi":null,"url":"https://arxiv.org/abs/1407.1843","retrieved":"2026-10-18"},"calibration":"validation","rankable":true,"notes":"Coefficients parsed from the arXiv source Table 2; mass range is the range of the tabulated stacks in Table 3 (8.4 to 11.1). Verification: mean a_low of the four bins = 0.97 (paper quotes 0.97+-0.06); a refit to Table 3 reproduces Table 2 within 1 sigma.","definitions":{"massDefinition":"sed-total","imf":"chabrier03","cosmology":{"H0":70,"Om":0.3},"population":"star-forming","sfrIndicator":"UV+IR (Spitzer/MIPS 24 um stacking for L_IR, rest-frame 2800 A for L_UV)","sfrTimescaleMyr":100,"sfrTimescaleBasis":"'This conversion implicitly assumes that galaxies continuously form stars over timescales of 100 Myr or longer.' (lower bound)","sfrStatistic":"median","massBasis":"stellar masses include a correction for emission-line contamination"}},{"id":"whitaker14.3dhst.sfms.bpl.z1-1.5","source":"Whitaker et al. 2014 (3D-HST/CANDELS)","run":"broken power law, median stacks","kind":"observation","relation":"sfms","epoch":{"zRepresentative":1.25,"zMin":1,"zMax":1.5,"mode":"observational-bin","snapshot":null},"axes":{"xDefinition":"log10 stellar mass (FAST, Bruzual & Charlot 2003, Chabrier IMF, emission-line corrected)","xUnit":"log10(Msun)","yDefinition":"log10 UV+IR SFR (Psi = 1.09e-10 (L_IR + 2.2 L_UV) Lsun, Chabrier IMF) of the median 24um-stack plus median UV luminosity of star-forming galaxies in the mass bin","yUnit":"log10(Msun/yr)"},"domain":{"xMin":8.8,"xMax":11.3},"representation":{"type":"parametric","equation":"log Psi = a [log(M*/Msun) - 10.2] + b, with a = a_low below and a_high above log M* = 10.2 (Eq. 2, Table 2)","expression":"b+alow*Math.min(x-10.2,0)+ahigh*Math.max(x-10.2,0)","parameters":{"alow":0.99,"ahigh":0.51,"b":1.31,"alowError":0.04,"ahighError":0.07,"bError":0.02}},"scatter":null,"selection":{"population":"UVJ-selected star-forming galaxies above the 90% mass-completeness limits, 3D-HST v4.0 / CANDELS (five fields)","warning":"Fit to median stacked UV+IR SFRs in 0.2 dex mass bins; the SFR of each bin includes MIPS-undetected galaxies through stacking. The paper does not measure the intrinsic scatter. The break mass 10.2 is fixed. zRepresentative is the bin centre. The paper's quadratic (Table 1) is not stored: its two-decimal coefficients do not reproduce the paper's own Table 3 (see M1 notes)."},"provenance":{"tier":"published-fit","citation":"Whitaker et al. 2014, ApJ 795, 104 (arXiv:1407.1843), Eq. 2 and Table 2","doi":null,"url":"https://arxiv.org/abs/1407.1843","retrieved":"2026-10-18"},"calibration":"validation","rankable":true,"notes":"Coefficients parsed from the arXiv source Table 2; mass range is the range of the tabulated stacks in Table 3 (8.8 to 11.3). Verification: mean a_low of the four bins = 0.97 (paper quotes 0.97+-0.06); a refit to Table 3 reproduces Table 2 within 1 sigma.","definitions":{"massDefinition":"sed-total","imf":"chabrier03","cosmology":{"H0":70,"Om":0.3},"population":"star-forming","sfrIndicator":"UV+IR (Spitzer/MIPS 24 um stacking for L_IR, rest-frame 2800 A for L_UV)","sfrTimescaleMyr":100,"sfrTimescaleBasis":"'This conversion implicitly assumes that galaxies continuously form stars over timescales of 100 Myr or longer.' (lower bound)","sfrStatistic":"median","massBasis":"stellar masses include a correction for emission-line contamination"}},{"id":"whitaker14.3dhst.sfms.bpl.z1.5-2","source":"Whitaker et al. 2014 (3D-HST/CANDELS)","run":"broken power law, median stacks","kind":"observation","relation":"sfms","epoch":{"zRepresentative":1.75,"zMin":1.5,"zMax":2,"mode":"observational-bin","snapshot":null},"axes":{"xDefinition":"log10 stellar mass (FAST, Bruzual & Charlot 2003, Chabrier IMF, emission-line corrected)","xUnit":"log10(Msun)","yDefinition":"log10 UV+IR SFR (Psi = 1.09e-10 (L_IR + 2.2 L_UV) Lsun, Chabrier IMF) of the median 24um-stack plus median UV luminosity of star-forming galaxies in the mass bin","yUnit":"log10(Msun/yr)"},"domain":{"xMin":9.2,"xMax":11.5},"representation":{"type":"parametric","equation":"log Psi = a [log(M*/Msun) - 10.2] + b, with a = a_low below and a_high above log M* = 10.2 (Eq. 2, Table 2)","expression":"b+alow*Math.min(x-10.2,0)+ahigh*Math.max(x-10.2,0)","parameters":{"alow":1.04,"ahigh":0.62,"b":1.49,"alowError":0.05,"ahighError":0.06,"bError":0.02}},"scatter":null,"selection":{"population":"UVJ-selected star-forming galaxies above the 90% mass-completeness limits, 3D-HST v4.0 / CANDELS (five fields)","warning":"Fit to median stacked UV+IR SFRs in 0.2 dex mass bins; the SFR of each bin includes MIPS-undetected galaxies through stacking. The paper does not measure the intrinsic scatter. The break mass 10.2 is fixed. zRepresentative is the bin centre. The paper's quadratic (Table 1) is not stored: its two-decimal coefficients do not reproduce the paper's own Table 3 (see M1 notes)."},"provenance":{"tier":"published-fit","citation":"Whitaker et al. 2014, ApJ 795, 104 (arXiv:1407.1843), Eq. 2 and Table 2","doi":null,"url":"https://arxiv.org/abs/1407.1843","retrieved":"2026-10-18"},"calibration":"validation","rankable":true,"notes":"Coefficients parsed from the arXiv source Table 2; mass range is the range of the tabulated stacks in Table 3 (9.2 to 11.5). Verification: mean a_low of the four bins = 0.97 (paper quotes 0.97+-0.06); a refit to Table 3 reproduces Table 2 within 1 sigma.","definitions":{"massDefinition":"sed-total","imf":"chabrier03","cosmology":{"H0":70,"Om":0.3},"population":"star-forming","sfrIndicator":"UV+IR (Spitzer/MIPS 24 um stacking for L_IR, rest-frame 2800 A for L_UV)","sfrTimescaleMyr":100,"sfrTimescaleBasis":"'This conversion implicitly assumes that galaxies continuously form stars over timescales of 100 Myr or longer.' (lower bound)","sfrStatistic":"median","massBasis":"stellar masses include a correction for emission-line contamination"}},{"id":"whitaker14.3dhst.sfms.bpl.z2-2.5","source":"Whitaker et al. 2014 (3D-HST/CANDELS)","run":"broken power law, median stacks","kind":"observation","relation":"sfms","epoch":{"zRepresentative":2.25,"zMin":2,"zMax":2.5,"mode":"observational-bin","snapshot":null},"axes":{"xDefinition":"log10 stellar mass (FAST, Bruzual & Charlot 2003, Chabrier IMF, emission-line corrected)","xUnit":"log10(Msun)","yDefinition":"log10 UV+IR SFR (Psi = 1.09e-10 (L_IR + 2.2 L_UV) Lsun, Chabrier IMF) of the median 24um-stack plus median UV luminosity of star-forming galaxies in the mass bin","yUnit":"log10(Msun/yr)"},"domain":{"xMin":9.3,"xMax":11.5},"representation":{"type":"parametric","equation":"log Psi = a [log(M*/Msun) - 10.2] + b, with a = a_low below and a_high above log M* = 10.2 (Eq. 2, Table 2)","expression":"b+alow*Math.min(x-10.2,0)+ahigh*Math.max(x-10.2,0)","parameters":{"alow":0.91,"ahigh":0.67,"b":1.62,"alowError":0.06,"ahighError":0.06,"bError":0.02}},"scatter":null,"selection":{"population":"UVJ-selected star-forming galaxies above the 90% mass-completeness limits, 3D-HST v4.0 / CANDELS (five fields)","warning":"Fit to median stacked UV+IR SFRs in 0.2 dex mass bins; the SFR of each bin includes MIPS-undetected galaxies through stacking. The paper does not measure the intrinsic scatter. The break mass 10.2 is fixed. zRepresentative is the bin centre. The paper's quadratic (Table 1) is not stored: its two-decimal coefficients do not reproduce the paper's own Table 3 (see M1 notes)."},"provenance":{"tier":"published-fit","citation":"Whitaker et al. 2014, ApJ 795, 104 (arXiv:1407.1843), Eq. 2 and Table 2","doi":null,"url":"https://arxiv.org/abs/1407.1843","retrieved":"2026-10-18"},"calibration":"validation","rankable":true,"notes":"Coefficients parsed from the arXiv source Table 2; mass range is the range of the tabulated stacks in Table 3 (9.3 to 11.5). Verification: mean a_low of the four bins = 0.97 (paper quotes 0.97+-0.06); a refit to Table 3 reproduces Table 2 within 1 sigma.","definitions":{"massDefinition":"sed-total","imf":"chabrier03","cosmology":{"H0":70,"Om":0.3},"population":"star-forming","sfrIndicator":"UV+IR (Spitzer/MIPS 24 um stacking for L_IR, rest-frame 2800 A for L_UV)","sfrTimescaleMyr":100,"sfrTimescaleBasis":"'This conversion implicitly assumes that galaxies continuously form stars over timescales of 100 Myr or longer.' (lower bound)","sfrStatistic":"median","massBasis":"stellar masses include a correction for emission-line contamination"}},{"id":"shen20.bhmd.fitA.zi7","source":"Shen et al. 2020","run":"Shen et al. 2020 (integrated bolometric QLF, global fit A, z_i=7)","kind":"observation","relation":"bhmd","epoch":{"zRepresentative":3.185,"zNominal":0,"zMin":0,"zMax":6.37,"mode":"observational-bin","snapshot":null},"axes":{"xDefinition":"redshift","xUnit":"redshift","yDefinition":"log10 cosmic black-hole mass density integrated from the bolometric QLF","yUnit":"log10(Msun cMpc^-3)"},"domain":{"xMin":0,"xMax":6.37},"representation":{"type":"points","intervalKind":"unspecified","connect":true,"points":[{"x":0,"y":5.7155},{"x":0.07,"y":5.7136},{"x":0.14,"y":5.7109},{"x":0.21,"y":5.7072},{"x":0.28,"y":5.7023},{"x":0.35,"y":5.6961},{"x":0.42,"y":5.6884},{"x":0.49,"y":5.6791},{"x":0.56,"y":5.668},{"x":0.63,"y":5.6552},{"x":0.7,"y":5.6405},{"x":0.77,"y":5.624},{"x":0.84,"y":5.6056},{"x":0.91,"y":5.5854},{"x":0.98,"y":5.5634},{"x":1.05,"y":5.5396},{"x":1.12,"y":5.5141},{"x":1.19,"y":5.4869},{"x":1.26,"y":5.4582},{"x":1.33,"y":5.428},{"x":1.4,"y":5.3963},{"x":1.47,"y":5.3633},{"x":1.54,"y":5.329},{"x":1.61,"y":5.2934},{"x":1.68,"y":5.2567},{"x":1.75,"y":5.219},{"x":1.82,"y":5.1802},{"x":1.89,"y":5.1405},{"x":1.96,"y":5.1},{"x":2.03,"y":5.0586},{"x":2.1,"y":5.0165},{"x":2.17,"y":4.9737},{"x":2.24,"y":4.9303},{"x":2.31,"y":4.8863},{"x":2.38,"y":4.8418},{"x":2.45,"y":4.7969},{"x":2.52,"y":4.7515},{"x":2.59,"y":4.7057},{"x":2.66,"y":4.6596},{"x":2.73,"y":4.6133},{"x":2.8,"y":4.5667},{"x":2.87,"y":4.5198},{"x":2.94,"y":4.4729},{"x":3.01,"y":4.4258},{"x":3.08,"y":4.3786},{"x":3.15,"y":4.3313},{"x":3.22,"y":4.284},{"x":3.29,"y":4.2367},{"x":3.36,"y":4.1895},{"x":3.43,"y":4.1423},{"x":3.5,"y":4.0952},{"x":3.57,"y":4.0482},{"x":3.64,"y":4.0014},{"x":3.71,"y":3.9547},{"x":3.78,"y":3.9082},{"x":3.85,"y":3.8619},{"x":3.92,"y":3.8159},{"x":3.99,"y":3.7701},{"x":4.06,"y":3.7245},{"x":4.13,"y":3.6792},{"x":4.2,"y":3.6343},{"x":4.27,"y":3.5895},{"x":4.34,"y":3.5451},{"x":4.41,"y":3.501},{"x":4.48,"y":3.4572},{"x":4.55,"y":3.4137},{"x":4.62,"y":3.3705},{"x":4.69,"y":3.3276},{"x":4.76,"y":3.285},{"x":4.83,"y":3.2426},{"x":4.9,"y":3.2005},{"x":4.97,"y":3.1585},{"x":5.04,"y":3.1168},{"x":5.11,"y":3.0751},{"x":5.18,"y":3.0336},{"x":5.25,"y":2.9921},{"x":5.32,"y":2.9506},{"x":5.39,"y":2.909},{"x":5.46,"y":2.8673},{"x":5.53,"y":2.8252},{"x":5.6,"y":2.7829},{"x":5.67,"y":2.74},{"x":5.74,"y":2.6965},{"x":5.81,"y":2.6523},{"x":5.88,"y":2.607},{"x":5.95,"y":2.5606},{"x":6.02,"y":2.5127},{"x":6.09,"y":2.463},{"x":6.16,"y":2.4112},{"x":6.23,"y":2.3566},{"x":6.3,"y":2.2988},{"x":6.37,"y":2.2369}]},"scatter":null,"selection":{"population":"all AGN (global fit A of the bolometric QLF, 43 <= log L_bol <= 48)","warning":"Model curve integrated by the authors from z_i=7 (zero initial mass density) down to z with eps_r=0.1; the grey/coloured shaded +-2x eps_r bands are not extracted; points are the vertices of the plotted path inside the frame (the curve leaves the frame below log rho=2.2 at high z). 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Scatter quoted in the text: sigma(log Sigma_1)~0.25 dex (SFGs), 0.14 dex (quiescent)."},{"id":"barro17.candels-goodss.sigma1.q.z1.4-2.2","source":"Barro et al. 2017 (CANDELS GOODS-S)","run":"quiescent galaxies, 1.4<z<2.2, log-linear fit","kind":"observation","relation":"sigma1","epoch":{"zRepresentative":1.8,"zNominal":1.8,"zMin":1.4,"zMax":2.2,"mode":"observational-bin","snapshot":null},"axes":{"xDefinition":"log10 stellar mass (FAST SED fit, Chabrier IMF)","xUnit":"log10(Msun)","yDefinition":"log10 stellar surface density within 1 kpc, Sigma_1kpc = M(<1 kpc)/(pi (1 kpc)^2)","yUnit":"log10(Msun/kpc^2)"},"domain":{"xMin":10,"xMax":11.5},"representation":{"type":"parametric","equation":"log Sigma_1 = beta*(log M* - 10.5) + log B","expression":"beta*(x-10.5)+logB","parameters":{"beta":0.64,"logB":9.74}},"scatter":{"value":0.14,"unit":"dex","meaning":"sigma(log Sigma_1) quoted in the text (ms.tex:500), all redshifts"},"selection":{"population":"quiescent (DeltaSFR < -0.7 dex below the SFR main sequence)","warning":"Domain = extent of the fit line plotted in Fig. 2B (SFG 9.0-11.6, quiescent 10.0-11.5); the paper says the fit uses galaxies down to log M*=9 (~70% complete). The plotted thick lines use slopes 0.85 (SFG) and 0.65 (quiescent) in all panels and differ from the tabulated fits by up to 0.10 dex over the plotted range; the table is used here. zRepresentative is the bin midpoint. Sigma_1 is derived assuming the stellar mass profile follows a Sersic fit (paper Eq. gammaeq). Single-field (GOODS-S), not volume limited."},"definitions":{"imf":"chabrier03","cosmology":{"H0":70,"Om":0.3},"massDefinition":"sed-total","sigma1Definition":"Sigma_1kpc=M(<1 kpc)/pi (1 kpc)^2, M(<1 kpc) from stellar mass profiles (multi-band HST SED fits, with a Sersic-dependent correction for PSF smearing within 1 kpc)","population":"quiescent"},"provenance":{"tier":"published-fit","citation":"Barro et al. 2017, ApJ 840, 47 (arXiv:1509.00469), Table 'Power Law Fits' (Sigma_1 columns), 1.4<z<2.2","doi":"10.3847/1538-4357/aa6b05","url":"https://arxiv.org/abs/1509.00469","retrieved":"2026-10-18","sourceArchiveSha256":"07485144467a1082df44b88961546ae628a902b25a42d5507507d43902c2afd6","sourceMember":"etab1.tex rows 15-18","figureCheck":"fig2b.eps panel lines, 667bf4a22c6c8dca423471815a754f86fb03e710092b53d48edd88f92dd32a47"},"calibration":"validation","rankable":true,"notes":"beta and log B as tabulated (errors: see etab1.tex); Fig. 2B thick-line check performed. Scatter quoted in the text: sigma(log Sigma_1)~0.25 dex (SFGs), 0.14 dex (quiescent)."},{"id":"barro17.candels-goodss.sigma1.sf.z2.2-3","source":"Barro et al. 2017 (CANDELS GOODS-S)","run":"star-forming galaxies, 2.2<z<3, log-linear fit","kind":"observation","relation":"sigma1","epoch":{"zRepresentative":2.6,"zNominal":2.6,"zMin":2.2,"zMax":3,"mode":"observational-bin","snapshot":null},"axes":{"xDefinition":"log10 stellar mass (FAST SED fit, Chabrier IMF)","xUnit":"log10(Msun)","yDefinition":"log10 stellar surface density within 1 kpc, Sigma_1kpc = M(<1 kpc)/(pi (1 kpc)^2)","yUnit":"log10(Msun/kpc^2)"},"domain":{"xMin":9,"xMax":11.6},"representation":{"type":"parametric","equation":"log Sigma_1 = beta*(log M* - 10.5) + log B","expression":"beta*(x-10.5)+logB","parameters":{"beta":0.89,"logB":9.33}},"scatter":{"value":0.25,"unit":"dex","meaning":"sigma(log Sigma_1) quoted in the text (ms.tex:500), all redshifts"},"selection":{"population":"star-forming (DeltaSFR >= -0.7 dex from the SFR main sequence)","warning":"Domain = extent of the fit line plotted in Fig. 2B (SFG 9.0-11.6, quiescent 10.0-11.5); the paper says the fit uses galaxies down to log M*=9 (~70% complete). The plotted thick lines use slopes 0.85 (SFG) and 0.65 (quiescent) in all panels and differ from the tabulated fits by up to 0.10 dex over the plotted range; the table is used here. zRepresentative is the bin midpoint. Sigma_1 is derived assuming the stellar mass profile follows a Sersic fit (paper Eq. gammaeq). Single-field (GOODS-S), not volume limited."},"definitions":{"imf":"chabrier03","cosmology":{"H0":70,"Om":0.3},"massDefinition":"sed-total","sigma1Definition":"Sigma_1kpc=M(<1 kpc)/pi (1 kpc)^2, M(<1 kpc) from stellar mass profiles (multi-band HST SED fits, with a Sersic-dependent correction for PSF smearing within 1 kpc)","population":"star-forming"},"provenance":{"tier":"published-fit","citation":"Barro et al. 2017, ApJ 840, 47 (arXiv:1509.00469), Table 'Power Law Fits' (Sigma_1 columns), 2.2<z<3","doi":"10.3847/1538-4357/aa6b05","url":"https://arxiv.org/abs/1509.00469","retrieved":"2026-10-18","sourceArchiveSha256":"07485144467a1082df44b88961546ae628a902b25a42d5507507d43902c2afd6","sourceMember":"etab1.tex rows 15-18","figureCheck":"fig2b.eps panel lines, 667bf4a22c6c8dca423471815a754f86fb03e710092b53d48edd88f92dd32a47"},"calibration":"validation","rankable":true,"notes":"beta and log B as tabulated (errors: see etab1.tex); Fig. 2B thick-line check performed. Scatter quoted in the text: sigma(log Sigma_1)~0.25 dex (SFGs), 0.14 dex (quiescent)."},{"id":"barro17.candels-goodss.sigma1.q.z2.2-3","source":"Barro et al. 2017 (CANDELS GOODS-S)","run":"quiescent galaxies, 2.2<z<3, log-linear fit","kind":"observation","relation":"sigma1","epoch":{"zRepresentative":2.6,"zNominal":2.6,"zMin":2.2,"zMax":3,"mode":"observational-bin","snapshot":null},"axes":{"xDefinition":"log10 stellar mass (FAST SED fit, Chabrier IMF)","xUnit":"log10(Msun)","yDefinition":"log10 stellar surface density within 1 kpc, Sigma_1kpc = M(<1 kpc)/(pi (1 kpc)^2)","yUnit":"log10(Msun/kpc^2)"},"domain":{"xMin":10,"xMax":11.5},"representation":{"type":"parametric","equation":"log Sigma_1 = beta*(log M* - 10.5) + log B","expression":"beta*(x-10.5)+logB","parameters":{"beta":0.67,"logB":9.8}},"scatter":{"value":0.14,"unit":"dex","meaning":"sigma(log Sigma_1) quoted in the text (ms.tex:500), all redshifts"},"selection":{"population":"quiescent (DeltaSFR < -0.7 dex below the SFR main sequence)","warning":"Domain = extent of the fit line plotted in Fig. 2B (SFG 9.0-11.6, quiescent 10.0-11.5); the paper says the fit uses galaxies down to log M*=9 (~70% complete). The plotted thick lines use slopes 0.85 (SFG) and 0.65 (quiescent) in all panels and differ from the tabulated fits by up to 0.10 dex over the plotted range; the table is used here. zRepresentative is the bin midpoint. Sigma_1 is derived assuming the stellar mass profile follows a Sersic fit (paper Eq. gammaeq). Single-field (GOODS-S), not volume limited."},"definitions":{"imf":"chabrier03","cosmology":{"H0":70,"Om":0.3},"massDefinition":"sed-total","sigma1Definition":"Sigma_1kpc=M(<1 kpc)/pi (1 kpc)^2, M(<1 kpc) from stellar mass profiles (multi-band HST SED fits, with a Sersic-dependent correction for PSF smearing within 1 kpc)","population":"quiescent"},"provenance":{"tier":"published-fit","citation":"Barro et al. 2017, ApJ 840, 47 (arXiv:1509.00469), Table 'Power Law Fits' (Sigma_1 columns), 2.2<z<3","doi":"10.3847/1538-4357/aa6b05","url":"https://arxiv.org/abs/1509.00469","retrieved":"2026-10-18","sourceArchiveSha256":"07485144467a1082df44b88961546ae628a902b25a42d5507507d43902c2afd6","sourceMember":"etab1.tex rows 15-18","figureCheck":"fig2b.eps panel lines, 667bf4a22c6c8dca423471815a754f86fb03e710092b53d48edd88f92dd32a47"},"calibration":"validation","rankable":true,"notes":"beta and log B as tabulated (errors: see etab1.tex); Fig. 2B thick-line check performed. Scatter quoted in the text: sigma(log Sigma_1)~0.25 dex (SFGs), 0.14 dex (quiescent)."},{"id":"fang13.sdss.sigma1.green-red.fit","source":"Fang et al. 2013 (SDSS)","run":"central green+red galaxies, z<0.075, least-squares fit","kind":"observation","relation":"sigma1","epoch":{"zRepresentative":0.04,"zNominal":0.04,"zMin":0.005,"zMax":0.075,"mode":"observational-bin","snapshot":null},"axes":{"xDefinition":"log10 total stellar mass (MPA/JHU DR7)","xUnit":"log10(Msun)","yDefinition":"log10 average stellar surface mass density within a circular aperture of radius 1 kpc, Sigma_1","yUnit":"log10(Msun/kpc^2)"},"domain":{"xMin":9.75,"xMax":11.25},"representation":{"type":"parametric","equation":"log Sigma_1 = 9.29 + 0.64 (log M* - 10.25)","expression":"a+b*(x-10.25)","parameters":{"a":9.29,"b":0.64}},"scatter":{"value":0.16,"unit":"dex","meaning":"1 sigma scatter of green and red galaxies about the relation"},"selection":{"population":"central, green valley + red sequence","warning":"SDSS DR7 central galaxies (most massive group member, Yang+12), 0.005<z<0.075, b/a>0.6, green-valley and red-sequence (NUV-r>4) galaxies only, 9.75<log M*<11.25, volume-limited per 0.25 dex mass bin; blue-cloud galaxies lie below the ridge and are excluded from the fit. Not a relation for all galaxies. zRepresentative is the midpoint of 0.005<z<0.075 (not a median). The drawn line in Fig. 4 spans log M* 9-11.5; the fit uses the 9.75-11.25 sample. IMF and cosmology are not stated in the paper. Sigma_1 is from SDSS i-band surface-brightness profiles converted with a g-i colour M/L calibrated on the MPA/JHU masses, so it inherits SDSS seeing (HWHM 0.7 arcsec ~ 1 kpc at z=0.075)."},"definitions":{"imf":"unspecified","cosmology":"unspecified","massDefinition":"sed-total","population":"central green-valley and red-sequence","sigma1Definition":"average surface mass density within a circular aperture of radius 1 kpc, computed by directly integrating the mass profiles from the innermost point out to R=1 kpc"},"provenance":{"tier":"published-fit","citation":"Fang et al. 2013, ApJ 776, 63 (arXiv:1308.5224), fit to Fig. 4 (Sigma_1 vs M*)","doi":"10.1088/0004-637X/776/1/63","url":"https://arxiv.org/abs/1308.5224","retrieved":"2026-10-18","sourceArchiveSha256":"e41adaecc34114a227801cbe2cd9dde2f6636ea11a3012a0fac4cab893c3ee9f","sourceMember":"ms_v2.tex lines 193-197 (Eq. sd1_mass_eqn)","figureCheck":"f4.pdf checksum 74a767bba87193408ac509cb73d31a2d3c2b466ab1dcf231d35da980c16e159f"},"calibration":"validation","rankable":true,"notes":"Fit 9.29(+0.10,-0.10) + 0.64(+0.23,-0.20)(log M* - 10.25), 1 sigma scatter 0.16 dex (bootstrap 16-84%). Drawn line in f4.pdf reproduces the closed form to 0.006 dex at all vertices."},{"id":"fang13.sdss.sigmam.sigma1kpc.green-red.fit","source":"Fang et al. 2013 (SDSS)","run":"central green+red galaxies, sigma scaled to 1 kpc, z<0.075, least-squares fit","kind":"observation","relation":"sigmam","epoch":{"zRepresentative":0.04,"zNominal":0.04,"zMin":0.005,"zMax":0.075,"mode":"observational-bin","snapshot":null},"axes":{"xDefinition":"log10 total stellar mass (MPA/JHU DR7)","xUnit":"log10(Msun)","yDefinition":"log10 SDSS fibre velocity dispersion scaled to a circular aperture of radius 1 kpc, sigma_1","yUnit":"log10(km/s)"},"domain":{"xMin":9.75,"xMax":11.25},"representation":{"type":"parametric","equation":"log sigma_1 = 2.09 + 0.29 (log M* - 10.25)","expression":"a+b*(x-10.25)","parameters":{"a":2.09,"b":0.29}},"scatter":{"value":0.09,"unit":"dex","meaning":"1 sigma vertical scatter of green and red galaxies about the relation"},"selection":{"population":"central, green valley + red sequence","warning":"SDSS DR7 central galaxies (most massive group member, Yang+12), 0.005<z<0.075, b/a>0.6, green-valley and red-sequence (NUV-r>4) galaxies only, 9.75<log M*<11.25, volume-limited per 0.25 dex mass bin; blue-cloud galaxies lie below the ridge and are excluded from the fit. Not a relation for all galaxies. The aperture is 1 kpc (not R_e and not the 3 kpc of Zahid+16): fibre dispersions were scaled with sigma ~ R^-0.66 (Cappellari+06). zRepresentative is the midpoint of the redshift range. IMF and cosmology not stated."},"definitions":{"imf":"unspecified","cosmology":"unspecified","massDefinition":"sed-total","population":"central green-valley and red-sequence","sigmaDefinition":"SDSS fibre (3 arcsec) stellar velocity dispersion scaled to a circular aperture of radius 1 kpc with sigma ~ R^-0.66 (Cappellari+06); 1D line of sight","sigmaDimension":"1D line of sight, scaled to 1 kpc aperture","sigmaWeighting":"unspecified"},"provenance":{"tier":"published-fit","citation":"Fang et al. 2013, ApJ 776, 63 (arXiv:1308.5224), fit to Fig. 11 (sigma_1 vs M*)","doi":"10.1088/0004-637X/776/1/63","url":"https://arxiv.org/abs/1308.5224","retrieved":"2026-10-18","sourceArchiveSha256":"e41adaecc34114a227801cbe2cd9dde2f6636ea11a3012a0fac4cab893c3ee9f","sourceMember":"ms_v2.tex lines 339-344","figureCheck":"f11.pdf checksum c346c1996fdf5b5c5c56ba9bd1d77a40630a59692ed888c52910d096116e6b57"},"calibration":"validation","rankable":true,"notes":"Fit 2.09(+0.05,-0.08) + 0.29(+0.13,-0.10)(log M* - 10.25); 1 sigma scatter 0.09 dex. Drawn line in f11.pdf reproduces the closed form to 0.004 dex at all vertices."},{"id":"zahid16.sdss.sigmam.fit","source":"Zahid et al. 2016 (SDSS)","run":"SDSS DR12 quiescent, broken power-law fit","kind":"observation","relation":"sigmam","epoch":{"zRepresentative":0.11,"zNominal":0.11,"zMin":0.02,"zMax":0.2,"mode":"observational-bin","snapshot":null},"axes":{"xDefinition":"log10 stellar mass (SED fit, Chabrier IMF)","xUnit":"log10(Msun)","yDefinition":"log10 central line-of-sight stellar velocity dispersion (fibre, corrected to a 3 kpc aperture)","yUnit":"log10(km/s)"},"domain":{"xMin":9.362,"xMax":11.656},"representation":{"type":"parametric","equation":"log sigma = log sigma_b + alpha*(log M - log Mb), alpha = alpha1 (M<=Mb), alpha2 (M>Mb)","expression":"logSigb+(x<=logMb?alpha1:alpha2)*(x-logMb)","parameters":{"logMb":10.26,"logSigb":2.073,"alpha1":0.403,"alpha2":0.293}},"scatter":null,"selection":{"population":"quiescent (Dn4000>1.5), median log sigma in equally populated mass bins","warning":"Domain = extent of the best-fit line plotted in Fig. 5 (log M* 9.36-11.66); the paper fits all bins. Quiescent galaxies only (SDSS: M*>1e9 Msun, 0.02<z<0.2, Dn4000>1.5; SHELS: R<20.6, M*>10^9.5 Msun, Dn4000>1.5). The relation is for the median log sigma in equally populated stellar-mass bins, so it is not a relation for star-forming/disc galaxies, whose stellar kinematics are partly ordered rotation. 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Cosmology (Om, OL, h) = (0.27, 0.73, 0.71)."},{"id":"vanderwel14.size.late.z2.25","source":"van der Wel et al. 2014","run":"late-type","kind":"observation","relation":"size","epoch":{"zRepresentative":2.25,"zMin":2,"zMax":2.5,"mode":"observational-bin","snapshot":null},"axes":{"xDefinition":"log10 stellar mass, Chabrier IMF","xUnit":"log10(Msun)","yDefinition":"log10 major-axis effective radius at rest-frame 5000 A (late-type (UVJ star-forming))","yUnit":"log10(kpc)"},"domain":{"xMin":9.48,"xMax":11.5},"representation":{"type":"parametric","equation":"R_eff/kpc = A (M/5e10 Msun)^alpha","expression":"logA+alpha*(x-log10(5e10))","parameters":{"logA":0.55,"logAError":0.01,"alpha":0.22,"alphaError":0.01}},"scatter":{"value":0.19,"unit":"dex","meaning":"intrinsic scatter in log R_eff (Table 1)"},"selection":{"population":"late-type (UVJ star-forming)","warning":"UVJ-based type split with 10% assumed misclassification; fit mass limits >3e9 Msun (late) and >2e10 Msun (early). 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Cosmology (Om, OL, h) = (0.27, 0.73, 0.71)."},{"id":"vanderwel14.size.late.z2.75","source":"van der Wel et al. 2014","run":"late-type","kind":"observation","relation":"size","epoch":{"zRepresentative":2.75,"zMin":2.5,"zMax":3,"mode":"observational-bin","snapshot":null},"axes":{"xDefinition":"log10 stellar mass, Chabrier IMF","xUnit":"log10(Msun)","yDefinition":"log10 major-axis effective radius at rest-frame 5000 A (late-type (UVJ star-forming))","yUnit":"log10(kpc)"},"domain":{"xMin":9.48,"xMax":11.5},"representation":{"type":"parametric","equation":"R_eff/kpc = A (M/5e10 Msun)^alpha","expression":"logA+alpha*(x-log10(5e10))","parameters":{"logA":0.51,"logAError":0.01,"alpha":0.18,"alphaError":0.02}},"scatter":{"value":0.19,"unit":"dex","meaning":"intrinsic scatter in log R_eff (Table 1)"},"selection":{"population":"late-type (UVJ star-forming)","warning":"UVJ-based type split with 10% assumed misclassification; fit mass limits >3e9 Msun (late) and >2e10 Msun (early). 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Cosmology (Om, OL, h) = (0.27, 0.73, 0.71)."},{"id":"vanderwel14.size.early.z0.75","source":"van der Wel et al. 2014","run":"early-type","kind":"observation","relation":"size","epoch":{"zRepresentative":0.75,"zMin":0.5,"zMax":1,"mode":"observational-bin","snapshot":null},"axes":{"xDefinition":"log10 stellar mass, Chabrier IMF","xUnit":"log10(Msun)","yDefinition":"log10 major-axis effective radius at rest-frame 5000 A (early-type (UVJ quiescent))","yUnit":"log10(kpc)"},"domain":{"xMin":10.3,"xMax":11.5},"representation":{"type":"parametric","equation":"R_eff/kpc = A (M/5e10 Msun)^alpha","expression":"logA+alpha*(x-log10(5e10))","parameters":{"logA":0.42,"logAError":0.01,"alpha":0.71,"alphaError":0.03}},"scatter":{"value":0.11,"unit":"dex","meaning":"intrinsic scatter in log R_eff (Table 1)"},"selection":{"population":"early-type (UVJ quiescent)","warning":"UVJ-based type split with 10% assumed misclassification; fit mass limits >3e9 Msun (late) and >2e10 Msun (early). 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Cosmology (Om, OL, h) = (0.27, 0.73, 0.71)."},{"id":"vanderwel14.size.early.z1.25","source":"van der Wel et al. 2014","run":"early-type","kind":"observation","relation":"size","epoch":{"zRepresentative":1.25,"zMin":1,"zMax":1.5,"mode":"observational-bin","snapshot":null},"axes":{"xDefinition":"log10 stellar mass, Chabrier IMF","xUnit":"log10(Msun)","yDefinition":"log10 major-axis effective radius at rest-frame 5000 A (early-type (UVJ quiescent))","yUnit":"log10(kpc)"},"domain":{"xMin":10.3,"xMax":11.5},"representation":{"type":"parametric","equation":"R_eff/kpc = A (M/5e10 Msun)^alpha","expression":"logA+alpha*(x-log10(5e10))","parameters":{"logA":0.22,"logAError":0.01,"alpha":0.76,"alphaError":0.04}},"scatter":{"value":0.12,"unit":"dex","meaning":"intrinsic scatter in log R_eff (Table 1)"},"selection":{"population":"early-type (UVJ quiescent)","warning":"UVJ-based type split with 10% assumed misclassification; fit mass limits >3e9 Msun (late) and >2e10 Msun (early). 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The paper prints numbers that the extracted curves reproduce: 18 curves: six redshifts, three treatments; solid curves below L_FUV = 10^28.5: median -2.39, range -2.41 to -2.29 (paper: about -2.4); solid curves at L_FUV = 10^29 to 10^29.3 (z = 10 to 13): median -1.94 (paper: about -2); dotted curves at the faint end: lowest value -2.87 (paper: about -2.8); dotted curves of z = 10 and 11 above 10^29.3: -2.52, -2.76, -2.57, -2.36, mean -2.55 (paper: about -2.5 at 10^29.5); dashed curves up to 10^29: median -2.54 (paper: about -2.5); dust minus nebular curve at L_FUV = 10^29 to 10^29.1: mean 0.55 over 8 values (paper: dust reddens the slope by about 0.5)."},{"id":"wilkins22.flares.uvbeta.stellar.z15","source":"FLARES","run":"40 resimulated regions (EAGLE AGNdT9 model), stellar continuum only (dotted line)","kind":"simulation","relation":"uvbeta","epoch":{"zRepresentative":15,"zNominal":15,"zMin":15,"zMax":15,"mode":"published-epoch","snapshot":null},"axes":{"xDefinition":"absolute UV magnitude M_UV converted from the plotted far-UV luminosity L_FUV (the paper does not say whether it is the intrinsic or the dust-attenuated luminosity; AB, 10 pc)","xUnit":"mag (AB)","yDefinition":"UV-continuum slope beta, f_lambda ~ lambda^beta, median of galaxies in bins of L_FUV: unprocessed starlight: stellar emission only, no nebular emission, no dust","yUnit":"dimensionless"},"domain":{"xMin":-20.593,"xMax":-17.468},"representation":{"type":"points","intervalKind":"unspecified","connect":true,"points":[{"x":-20.593,"y":-2.6633},{"x":-19.968,"y":-2.7978},{"x":-19.343,"y":-2.8183},{"x":-18.718,"y":-2.8644},{"x":-18.093,"y":-2.8379},{"x":-17.468,"y":-2.7567}]},"scatter":null,"selection":{"population":"FLARES galaxies of the 40 resimulated regions; whether the median is weighted by the region weights is not stated","warning":"Median beta of the FLARES galaxies at z = 15 in bins of L_FUV (the figure has no band or error bars), unprocessed starlight: stellar emission only, no nebular emission, no dust, read from the vector paths of Wilkins et al. 2023 and converted to M_UV with the exact AB conversion M_UV = 51.5948 - 2.5 log10(L_FUV / erg s^-1 Hz^-1). 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The paper prints numbers that the extracted curves reproduce: 18 curves: six redshifts, three treatments; solid curves below L_FUV = 10^28.5: median -2.39, range -2.41 to -2.29 (paper: about -2.4); solid curves at L_FUV = 10^29 to 10^29.3 (z = 10 to 13): median -1.94 (paper: about -2); dotted curves at the faint end: lowest value -2.87 (paper: about -2.8); dotted curves of z = 10 and 11 above 10^29.3: -2.52, -2.76, -2.57, -2.36, mean -2.55 (paper: about -2.5 at 10^29.5); dashed curves up to 10^29: median -2.54 (paper: about -2.5); dust minus nebular curve at L_FUV = 10^29 to 10^29.1: mean 0.55 over 8 values (paper: dust reddens the slope by about 0.5)."},{"id":"wilkins22.flares.uvbeta.dust.z14","source":"FLARES","run":"40 resimulated regions (EAGLE AGNdT9 model), stellar plus nebular emission and dust (solid line)","kind":"simulation","relation":"uvbeta","epoch":{"zRepresentative":14,"zNominal":14,"zMin":14,"zMax":14,"mode":"published-epoch","snapshot":null},"axes":{"xDefinition":"absolute UV magnitude M_UV converted from the plotted far-UV luminosity L_FUV (the paper does not say whether it is the intrinsic or the dust-attenuated luminosity; AB, 10 pc)","xUnit":"mag (AB)","yDefinition":"UV-continuum slope beta, f_lambda ~ lambda^beta, median of galaxies in bins of L_FUV: stellar plus nebular emission, attenuated by dust (the paper: 'that which would be observed')","yUnit":"dimensionless"},"domain":{"xMin":-21.218,"xMax":-17.468},"representation":{"type":"points","intervalKind":"unspecified","connect":true,"points":[{"x":-21.218,"y":-1.8407},{"x":-20.593,"y":-1.8843},{"x":-19.968,"y":-2.2414},{"x":-19.343,"y":-2.332},{"x":-18.718,"y":-2.3902},{"x":-18.093,"y":-2.3999},{"x":-17.468,"y":-2.4113}]},"scatter":null,"selection":{"population":"FLARES galaxies of the 40 resimulated regions; whether the median is weighted by the region weights is not stated","warning":"Median beta of the FLARES galaxies at z = 14 in bins of L_FUV (the figure has no band or error bars), stellar plus nebular emission, attenuated by dust (the paper: 'that which would be observed'), read from the vector paths of Wilkins et al. 2023 and converted to M_UV with the exact AB conversion M_UV = 51.5948 - 2.5 log10(L_FUV / erg s^-1 Hz^-1). 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The paper prints numbers that the extracted curves reproduce: 18 curves: six redshifts, three treatments; solid curves below L_FUV = 10^28.5: median -2.39, range -2.41 to -2.29 (paper: about -2.4); solid curves at L_FUV = 10^29 to 10^29.3 (z = 10 to 13): median -1.94 (paper: about -2); dotted curves at the faint end: lowest value -2.87 (paper: about -2.8); dotted curves of z = 10 and 11 above 10^29.3: -2.52, -2.76, -2.57, -2.36, mean -2.55 (paper: about -2.5 at 10^29.5); dashed curves up to 10^29: median -2.54 (paper: about -2.5); dust minus nebular curve at L_FUV = 10^29 to 10^29.1: mean 0.55 over 8 values (paper: dust reddens the slope by about 0.5)."},{"id":"wilkins22.flares.uvbeta.nebular.z13","source":"FLARES","run":"40 resimulated regions (EAGLE AGNdT9 model), stellar plus nebular emission (dashed line)","kind":"simulation","relation":"uvbeta","epoch":{"zRepresentative":13,"zNominal":13,"zMin":13,"zMax":13,"mode":"published-epoch","snapshot":null},"axes":{"xDefinition":"absolute UV magnitude M_UV converted from the plotted far-UV luminosity L_FUV (the paper does not say whether it is the intrinsic or the dust-attenuated luminosity; AB, 10 pc)","xUnit":"mag (AB)","yDefinition":"UV-continuum slope beta, f_lambda ~ lambda^beta, median of galaxies in bins of L_FUV: starlight reprocessed by gas: stellar plus nebular emission, no dust","yUnit":"dimensionless"},"domain":{"xMin":-21.218,"xMax":-17.468},"representation":{"type":"points","intervalKind":"unspecified","connect":true,"points":[{"x":-21.218,"y":-2.5105},{"x":-20.593,"y":-2.5393},{"x":-19.968,"y":-2.5453},{"x":-19.343,"y":-2.54},{"x":-18.718,"y":-2.5358},{"x":-18.093,"y":-2.5535},{"x":-17.468,"y":-2.5652}]},"scatter":null,"selection":{"population":"FLARES galaxies of the 40 resimulated regions; whether the median is weighted by the region weights is not stated","warning":"Median beta of the FLARES galaxies at z = 13 in bins of L_FUV (the figure has no band or error bars), starlight reprocessed by gas: stellar plus nebular emission, no dust, read from the vector paths of Wilkins et al. 2023 and converted to M_UV with the exact AB conversion M_UV = 51.5948 - 2.5 log10(L_FUV / erg s^-1 Hz^-1). 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The paper prints numbers that the extracted curves reproduce: 18 curves: six redshifts, three treatments; solid curves below L_FUV = 10^28.5: median -2.39, range -2.41 to -2.29 (paper: about -2.4); solid curves at L_FUV = 10^29 to 10^29.3 (z = 10 to 13): median -1.94 (paper: about -2); dotted curves at the faint end: lowest value -2.87 (paper: about -2.8); dotted curves of z = 10 and 11 above 10^29.3: -2.52, -2.76, -2.57, -2.36, mean -2.55 (paper: about -2.5 at 10^29.5); dashed curves up to 10^29: median -2.54 (paper: about -2.5); dust minus nebular curve at L_FUV = 10^29 to 10^29.1: mean 0.55 over 8 values (paper: dust reddens the slope by about 0.5)."},{"id":"wilkins22.flares.uvbeta.dust.z11","source":"FLARES","run":"40 resimulated regions (EAGLE AGNdT9 model), stellar plus nebular emission and dust (solid line)","kind":"simulation","relation":"uvbeta","epoch":{"zRepresentative":11,"zNominal":11,"zMin":11,"zMax":11,"mode":"published-epoch","snapshot":null},"axes":{"xDefinition":"absolute UV magnitude M_UV converted from the plotted far-UV luminosity L_FUV (the paper does not say whether it is the intrinsic or the dust-attenuated luminosity; AB, 10 pc)","xUnit":"mag (AB)","yDefinition":"UV-continuum slope beta, f_lambda ~ lambda^beta, median of galaxies in bins of L_FUV: stellar plus nebular emission, attenuated by dust (the paper: 'that which would be observed')","yUnit":"dimensionless"},"domain":{"xMin":-22.468,"xMax":-17.468},"representation":{"type":"points","intervalKind":"unspecified","connect":true,"points":[{"x":-22.468,"y":-1.9832},{"x":-21.843,"y":-1.7095},{"x":-21.218,"y":-1.9501},{"x":-20.593,"y":-2.0182},{"x":-19.968,"y":-2.1629},{"x":-19.343,"y":-2.3114},{"x":-18.718,"y":-2.3808},{"x":-18.093,"y":-2.3955},{"x":-17.468,"y":-2.4007}]},"scatter":null,"selection":{"population":"FLARES galaxies of the 40 resimulated regions; whether the median is weighted by the region weights is not stated","warning":"Median beta of the FLARES galaxies at z = 11 in bins of L_FUV (the figure has no band or error bars), stellar plus nebular emission, attenuated by dust (the paper: 'that which would be observed'), read from the vector paths of Wilkins et al. 2023 and converted to M_UV with the exact AB conversion M_UV = 51.5948 - 2.5 log10(L_FUV / erg s^-1 Hz^-1). 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The paper prints numbers that the extracted curves reproduce: 18 curves: six redshifts, three treatments; solid curves below L_FUV = 10^28.5: median -2.39, range -2.41 to -2.29 (paper: about -2.4); solid curves at L_FUV = 10^29 to 10^29.3 (z = 10 to 13): median -1.94 (paper: about -2); dotted curves at the faint end: lowest value -2.87 (paper: about -2.8); dotted curves of z = 10 and 11 above 10^29.3: -2.52, -2.76, -2.57, -2.36, mean -2.55 (paper: about -2.5 at 10^29.5); dashed curves up to 10^29: median -2.54 (paper: about -2.5); dust minus nebular curve at L_FUV = 10^29 to 10^29.1: mean 0.55 over 8 values (paper: dust reddens the slope by about 0.5)."},{"id":"wilkins22.flares.uvbeta.nebular.z11","source":"FLARES","run":"40 resimulated regions (EAGLE AGNdT9 model), stellar plus nebular emission (dashed line)","kind":"simulation","relation":"uvbeta","epoch":{"zRepresentative":11,"zNominal":11,"zMin":11,"zMax":11,"mode":"published-epoch","snapshot":null},"axes":{"xDefinition":"absolute UV magnitude M_UV converted from the plotted far-UV luminosity L_FUV (the paper does not say whether it is the intrinsic or the dust-attenuated luminosity; AB, 10 pc)","xUnit":"mag (AB)","yDefinition":"UV-continuum slope beta, f_lambda ~ lambda^beta, median of galaxies in bins of L_FUV: starlight reprocessed by gas: stellar plus nebular emission, no dust","yUnit":"dimensionless"},"domain":{"xMin":-22.468,"xMax":-17.468},"representation":{"type":"points","intervalKind":"unspecified","connect":true,"points":[{"x":-22.468,"y":-2.5435},{"x":-21.843,"y":-2.4671},{"x":-21.218,"y":-2.4956},{"x":-20.593,"y":-2.5098},{"x":-19.968,"y":-2.5271},{"x":-19.343,"y":-2.5181},{"x":-18.718,"y":-2.5266},{"x":-18.093,"y":-2.5393},{"x":-17.468,"y":-2.5463}]},"scatter":null,"selection":{"population":"FLARES galaxies of the 40 resimulated regions; whether the median is weighted by the region weights is not stated","warning":"Median beta of the FLARES galaxies at z = 11 in bins of L_FUV (the figure has no band or error bars), starlight reprocessed by gas: stellar plus nebular emission, no dust, read from the vector paths of Wilkins et al. 2023 and converted to M_UV with the exact AB conversion M_UV = 51.5948 - 2.5 log10(L_FUV / erg s^-1 Hz^-1). 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The paper does not give the wavelength window of beta (betaWindow unspecified) and does not say whether the plotted L_FUV is intrinsic or dust attenuated, so a comparison with observed M_UV may shift the bright end by the far-UV attenuation. The bright-end bins hold few galaxies."},"definitions":{"betaWindow":"unspecified","dustTreatment":"intrinsic","dustModel":"no dust","betaMethod":"unspecified","stellarPopulation":"starlight reprocessed by gas: stellar plus nebular emission, no dust","imf":"chabrier03","cosmology":{"H0":67.77,"Om":0.307},"xVariable":"far-UV luminosity L_FUV converted to M_UV","uvBand":"far-UV (1500 A), L_FUV","statistic":"median","population":"all galaxies of the resimulated regions"},"provenance":{"tier":"digitized-figure","citation":"Wilkins et al. 2023, MNRAS 519, 3118 (arXiv:2204.09431), UV continuum slope against far-UV luminosity, stellar plus nebular emission (dashed line), z=10","doi":"10.1093/mnras/stac3280","url":"https://arxiv.org/abs/2204.09431","retrieved":"2026-10-25","figure":"Average UV continuum slope against UV luminosity and redshift","panel":"z=10, stellar plus nebular emission (dashed line)","checksumSha256":"d33df324aae1a8aeed5ca5101078a989986fd2718ba75bc4725e613d593ac3c9","sourceMember":"figures/beta2.pdf","extractionMethod":"vector path vertices from the figure PDF (PyMuPDF get_drawings), transformed through axes calibrated on labelled tick marks","axisCalibrationPixels":{"xTicks":[[76.49,28],[157.95,29],[239.4,30]],"yTicks":[[25.65,-1.6],[54.66,-1.8],[83.67,-2],[112.67,-2.2],[141.68,-2.4],[170.69,-2.6],[199.7,-2.8]],"labels":"x: numeric tick labels 28 to 30; y: labels 1.6 to 2.8 read with the separate minus glyph"},"digitizationUncertaintyDex":0.02,"quotes":{"treatments":"observational.tex:99","caption":"observational.tex:110","faint":"observational.tex:97","bright":"observational.tex:97","stellar":"observational.tex:99","dust":"observational.tex:99"},"definitionBasis":"dustTreatment and the stellar-population content are from the figure caption ('the solid line also including dust (i.e. that which would be observed)'). betaWindow and betaMethod: not stated in this paper. imf and cosmology: as in the other FLARES records of this dataset (the paper's SED-modelling section refers to FLARES II)."},"calibration":"prediction","rankable":false,"notes":"Vector-path extraction; exact to PDF coordinate precision. The paper prints numbers that the extracted curves reproduce: 18 curves: six redshifts, three treatments; solid curves below L_FUV = 10^28.5: median -2.39, range -2.41 to -2.29 (paper: about -2.4); solid curves at L_FUV = 10^29 to 10^29.3 (z = 10 to 13): median -1.94 (paper: about -2); dotted curves at the faint end: lowest value -2.87 (paper: about -2.8); dotted curves of z = 10 and 11 above 10^29.3: -2.52, -2.76, -2.57, -2.36, mean -2.55 (paper: about -2.5 at 10^29.5); dashed curves up to 10^29: median -2.54 (paper: about -2.5); dust minus nebular curve at L_FUV = 10^29 to 10^29.1: mean 0.55 over 8 values (paper: dust reddens the slope by about 0.5)."},{"id":"wilkins22.flares.uvbeta.stellar.z10","source":"FLARES","run":"40 resimulated regions (EAGLE AGNdT9 model), stellar continuum only (dotted line)","kind":"simulation","relation":"uvbeta","epoch":{"zRepresentative":10,"zNominal":10,"zMin":10,"zMax":10,"mode":"published-epoch","snapshot":null},"axes":{"xDefinition":"absolute UV magnitude M_UV converted from the plotted far-UV luminosity L_FUV (the paper does not say whether it is the intrinsic or the dust-attenuated luminosity; AB, 10 pc)","xUnit":"mag (AB)","yDefinition":"UV-continuum slope beta, f_lambda ~ lambda^beta, median of galaxies in bins of L_FUV: unprocessed starlight: stellar emission only, no nebular emission, no dust","yUnit":"dimensionless"},"domain":{"xMin":-22.468,"xMax":-17.468},"representation":{"type":"points","intervalKind":"unspecified","connect":true,"points":[{"x":-22.468,"y":-2.361},{"x":-21.843,"y":-2.5696},{"x":-21.218,"y":-2.6224},{"x":-20.593,"y":-2.6576},{"x":-19.968,"y":-2.7117},{"x":-19.343,"y":-2.7469},{"x":-18.718,"y":-2.8034},{"x":-18.093,"y":-2.8007},{"x":-17.468,"y":-2.7423}]},"scatter":null,"selection":{"population":"FLARES galaxies of the 40 resimulated regions; whether the median is weighted by the region weights is not stated","warning":"Median beta of the FLARES galaxies at z = 10 in bins of L_FUV (the figure has no band or error bars), unprocessed starlight: stellar emission only, no nebular emission, no dust, read from the vector paths of Wilkins et al. 2023 and converted to M_UV with the exact AB conversion M_UV = 51.5948 - 2.5 log10(L_FUV / erg s^-1 Hz^-1). The paper does not give the wavelength window of beta (betaWindow unspecified) and does not say whether the plotted L_FUV is intrinsic or dust attenuated, so a comparison with observed M_UV may shift the bright end by the far-UV attenuation. The bright-end bins hold few galaxies."},"definitions":{"betaWindow":"unspecified","dustTreatment":"intrinsic","dustModel":"no dust","betaMethod":"unspecified","stellarPopulation":"unprocessed starlight: stellar emission only, no nebular emission, no dust","imf":"chabrier03","cosmology":{"H0":67.77,"Om":0.307},"xVariable":"far-UV luminosity L_FUV converted to M_UV","uvBand":"far-UV (1500 A), L_FUV","statistic":"median","population":"all galaxies of the resimulated regions"},"provenance":{"tier":"digitized-figure","citation":"Wilkins et al. 2023, MNRAS 519, 3118 (arXiv:2204.09431), UV continuum slope against far-UV luminosity, stellar continuum only (dotted line), z=10","doi":"10.1093/mnras/stac3280","url":"https://arxiv.org/abs/2204.09431","retrieved":"2026-10-25","figure":"Average UV continuum slope against UV luminosity and redshift","panel":"z=10, stellar continuum only (dotted line)","checksumSha256":"d33df324aae1a8aeed5ca5101078a989986fd2718ba75bc4725e613d593ac3c9","sourceMember":"figures/beta2.pdf","extractionMethod":"vector path vertices from the figure PDF (PyMuPDF get_drawings), transformed through axes calibrated on labelled tick marks","axisCalibrationPixels":{"xTicks":[[76.49,28],[157.95,29],[239.4,30]],"yTicks":[[25.65,-1.6],[54.66,-1.8],[83.67,-2],[112.67,-2.2],[141.68,-2.4],[170.69,-2.6],[199.7,-2.8]],"labels":"x: numeric tick labels 28 to 30; y: labels 1.6 to 2.8 read with the separate minus glyph"},"digitizationUncertaintyDex":0.02,"quotes":{"treatments":"observational.tex:99","caption":"observational.tex:110","faint":"observational.tex:97","bright":"observational.tex:97","stellar":"observational.tex:99","dust":"observational.tex:99"},"definitionBasis":"dustTreatment and the stellar-population content are from the figure caption ('the solid line also including dust (i.e. that which would be observed)'). betaWindow and betaMethod: not stated in this paper. imf and cosmology: as in the other FLARES records of this dataset (the paper's SED-modelling section refers to FLARES II)."},"calibration":"prediction","rankable":false,"notes":"Vector-path extraction; exact to PDF coordinate precision. The paper prints numbers that the extracted curves reproduce: 18 curves: six redshifts, three treatments; solid curves below L_FUV = 10^28.5: median -2.39, range -2.41 to -2.29 (paper: about -2.4); solid curves at L_FUV = 10^29 to 10^29.3 (z = 10 to 13): median -1.94 (paper: about -2); dotted curves at the faint end: lowest value -2.87 (paper: about -2.8); dotted curves of z = 10 and 11 above 10^29.3: -2.52, -2.76, -2.57, -2.36, mean -2.55 (paper: about -2.5 at 10^29.5); dashed curves up to 10^29: median -2.54 (paper: about -2.5); dust minus nebular curve at L_FUV = 10^29 to 10^29.1: mean 0.55 over 8 values (paper: dust reddens the slope by about 0.5)."},{"id":"wilkins22.flares.uvlf.observed.z15","source":"FLARES","run":"40 resimulated regions (EAGLE AGNdT9 model), dust attenuated","kind":"simulation","relation":"uvlf","epoch":{"zRepresentative":15,"zNominal":15,"zMin":15,"zMax":15,"mode":"published-epoch","snapshot":null},"axes":{"xDefinition":"absolute UV magnitude M_UV from the far-UV luminosity, dust attenuated (AB)","xUnit":"mag (AB)","yDefinition":"log10 UV luminosity function per magnitude","yUnit":"log10(cMpc^-3 mag^-1)"},"domain":{"xMin":-19.655,"xMax":-17.905},"representation":{"type":"points","intervalKind":"unspecified","connect":true,"points":[{"x":-19.655,"y":-6.4225},{"x":-19.405,"y":-5.3242},{"x":-19.155,"y":-5.6282},{"x":-18.905,"y":-4.8045},{"x":-18.655,"y":-4.6792},{"x":-18.405,"y":-4.5748},{"x":-18.155,"y":-4.4225},{"x":-17.905,"y":-4.5274}]},"scatter":null,"selection":{"population":"all galaxies in the weighted combination of the resimulated regions","warning":"Observed far-UV luminosity function of FLARES at z=15, read from the vector paths of Wilkins et al. 2023. Conversions (exact): M_UV = 51.5948 - 2.5 log10(L_FUV / erg s^-1 Hz^-1) (AB, 10 pc), and log phi per magnitude = log phi per dex + log10(0.4). Binned in 0.1 dex of log L_FUV; bright-end bins hold few galaxies and are noisy. The paper also tabulates space densities in 0.2 dex bins without saying whether they are attenuated or intrinsic; those are not used."},"definitions":{"imf":"chabrier03","cosmology":{"H0":67.77,"Om":0.307},"densityFrame":"comoving","uvBand":"far-UV (1500 A), L_FUV","dustCorrection":"dust attenuated (SED modelling with a line-of-sight dust model)","population":"all"},"provenance":{"tier":"digitized-figure","citation":"Wilkins et al. 2023, MNRAS 519, 3118 (arXiv:2204.09431), far-UV luminosity function at z=15 to 10, observed, z=15","doi":"10.1093/mnras/stac3280","url":"https://arxiv.org/abs/2204.09431","retrieved":"2026-10-05","figure":"Observed and intrinsic far-UV luminosity function at z=15 to 10","panel":"z=15, solid line","checksumSha256":"e54af1794498ade1adb10e076ad226b87b58a9c4205c03c03b21c317839b1958","sourceMember":"figures/UVLF_panel.pdf","extractionMethod":"vector path vertices from the figure PDF (PyMuPDF get_drawings), transformed through axes calibrated on labelled tick marks","axisCalibrationPixels":"x: numeric tick labels snapped to ticks (log L_FUV); y: log phi per dex labels paired with ticks (minus glyphs are separate); x converted to M_UV, y to per magnitude","digitizationUncertaintyDex":0.02},"calibration":"prediction","rankable":false,"notes":"Vector-path extraction; exact to PDF coordinate precision, so uncertainty is the plotted line, not marker tracing."},{"id":"wilkins22.flares.uvlf.intrinsic.z15","source":"FLARES","run":"40 resimulated regions (EAGLE AGNdT9 model), intrinsic","kind":"simulation","relation":"uvlf","epoch":{"zRepresentative":15,"zNominal":15,"zMin":15,"zMax":15,"mode":"published-epoch","snapshot":null},"axes":{"xDefinition":"absolute UV magnitude M_UV from the far-UV luminosity, intrinsic (AB)","xUnit":"mag (AB)","yDefinition":"log10 UV luminosity function per magnitude","yUnit":"log10(cMpc^-3 mag^-1)"},"domain":{"xMin":-19.905,"xMax":-17.905},"representation":{"type":"points","intervalKind":"unspecified","connect":true,"points":[{"x":-19.905,"y":-5.4646},{"x":-19.655,"y":-6.2257},{"x":-19.405,"y":-6.4122},{"x":-19.155,"y":-5.0472},{"x":-18.905,"y":-4.8969},{"x":-18.655,"y":-4.9631},{"x":-18.405,"y":-4.4073},{"x":-18.155,"y":-4.4306},{"x":-17.905,"y":-4.6506}]},"scatter":null,"selection":{"population":"all galaxies in the weighted combination of the resimulated regions","warning":"Intrinsic far-UV luminosity function of FLARES at z=15, read from the vector paths of Wilkins et al. 2023. Conversions (exact): M_UV = 51.5948 - 2.5 log10(L_FUV / erg s^-1 Hz^-1) (AB, 10 pc), and log phi per magnitude = log phi per dex + log10(0.4). Binned in 0.1 dex of log L_FUV; bright-end bins hold few galaxies and are noisy. The paper also tabulates space densities in 0.2 dex bins without saying whether they are attenuated or intrinsic; those are not used."},"definitions":{"imf":"chabrier03","cosmology":{"H0":67.77,"Om":0.307},"densityFrame":"comoving","uvBand":"far-UV (1500 A), L_FUV","dustCorrection":"none (intrinsic)","population":"all"},"provenance":{"tier":"digitized-figure","citation":"Wilkins et al. 2023, MNRAS 519, 3118 (arXiv:2204.09431), far-UV luminosity function at z=15 to 10, intrinsic, z=15","doi":"10.1093/mnras/stac3280","url":"https://arxiv.org/abs/2204.09431","retrieved":"2026-10-05","figure":"Observed and intrinsic far-UV luminosity function at z=15 to 10","panel":"z=15, dashed line","checksumSha256":"e54af1794498ade1adb10e076ad226b87b58a9c4205c03c03b21c317839b1958","sourceMember":"figures/UVLF_panel.pdf","extractionMethod":"vector path vertices from the figure PDF (PyMuPDF get_drawings), transformed through axes calibrated on labelled tick marks","axisCalibrationPixels":"x: numeric tick labels snapped to ticks (log L_FUV); y: log phi per dex labels paired with ticks (minus glyphs are separate); x converted to M_UV, y to per magnitude","digitizationUncertaintyDex":0.02},"calibration":"prediction","rankable":false,"notes":"Vector-path extraction; exact to PDF coordinate precision, so uncertainty is the plotted line, not marker tracing."},{"id":"wilkins22.flares.uvlf.observed.z14","source":"FLARES","run":"40 resimulated regions (EAGLE AGNdT9 model), dust attenuated","kind":"simulation","relation":"uvlf","epoch":{"zRepresentative":14,"zNominal":14,"zMin":14,"zMax":14,"mode":"published-epoch","snapshot":null},"axes":{"xDefinition":"absolute UV magnitude M_UV from the far-UV luminosity, dust attenuated (AB)","xUnit":"mag (AB)","yDefinition":"log10 UV luminosity function per magnitude","yUnit":"log10(cMpc^-3 mag^-1)"},"domain":{"xMin":-20.155,"xMax":-17.905},"representation":{"type":"points","intervalKind":"unspecified","connect":true,"points":[{"x":-20.155,"y":-6.803},{"x":-19.905,"y":-6.5632},{"x":-19.655,"y":-5.6876},{"x":-19.405,"y":-5.0968},{"x":-19.155,"y":-4.8214},{"x":-18.905,"y":-4.9557},{"x":-18.655,"y":-4.4038},{"x":-18.405,"y":-4.1801},{"x":-18.155,"y":-3.8645},{"x":-17.905,"y":-4.1181}]},"scatter":null,"selection":{"population":"all galaxies in the weighted combination of the resimulated regions","warning":"Observed far-UV luminosity function of FLARES at z=14, read from the vector paths of Wilkins et al. 2023. Conversions (exact): M_UV = 51.5948 - 2.5 log10(L_FUV / erg s^-1 Hz^-1) (AB, 10 pc), and log phi per magnitude = log phi per dex + log10(0.4). Binned in 0.1 dex of log L_FUV; bright-end bins hold few galaxies and are noisy. The paper also tabulates space densities in 0.2 dex bins without saying whether they are attenuated or intrinsic; those are not used."},"definitions":{"imf":"chabrier03","cosmology":{"H0":67.77,"Om":0.307},"densityFrame":"comoving","uvBand":"far-UV (1500 A), L_FUV","dustCorrection":"dust attenuated (SED modelling with a line-of-sight dust model)","population":"all"},"provenance":{"tier":"digitized-figure","citation":"Wilkins et al. 2023, MNRAS 519, 3118 (arXiv:2204.09431), far-UV luminosity function at z=15 to 10, observed, z=14","doi":"10.1093/mnras/stac3280","url":"https://arxiv.org/abs/2204.09431","retrieved":"2026-10-05","figure":"Observed and intrinsic far-UV luminosity function at z=15 to 10","panel":"z=14, solid line","checksumSha256":"e54af1794498ade1adb10e076ad226b87b58a9c4205c03c03b21c317839b1958","sourceMember":"figures/UVLF_panel.pdf","extractionMethod":"vector path vertices from the figure PDF (PyMuPDF get_drawings), transformed through axes calibrated on labelled tick marks","axisCalibrationPixels":"x: numeric tick labels snapped to ticks (log L_FUV); y: log phi per dex labels paired with ticks (minus glyphs are separate); x converted to M_UV, y to per magnitude","digitizationUncertaintyDex":0.02},"calibration":"prediction","rankable":false,"notes":"Vector-path extraction; exact to PDF coordinate precision, so uncertainty is the plotted line, not marker tracing."},{"id":"wilkins22.flares.uvlf.intrinsic.z14","source":"FLARES","run":"40 resimulated regions (EAGLE AGNdT9 model), intrinsic","kind":"simulation","relation":"uvlf","epoch":{"zRepresentative":14,"zNominal":14,"zMin":14,"zMax":14,"mode":"published-epoch","snapshot":null},"axes":{"xDefinition":"absolute UV magnitude M_UV from the far-UV luminosity, intrinsic (AB)","xUnit":"mag (AB)","yDefinition":"log10 UV luminosity function per magnitude","yUnit":"log10(cMpc^-3 mag^-1)"},"domain":{"xMin":-20.405,"xMax":-17.905},"representation":{"type":"points","intervalKind":"unspecified","connect":true,"points":[{"x":-20.405,"y":-6.5093},{"x":-20.155,"y":-5.8474},{"x":-19.905,"y":-6.325},{"x":-19.655,"y":-5.9577},{"x":-19.405,"y":-4.8543},{"x":-19.155,"y":-4.9452},{"x":-18.905,"y":-5.0347},{"x":-18.655,"y":-4.6251},{"x":-18.405,"y":-3.925},{"x":-18.155,"y":-3.9539},{"x":-17.905,"y":-3.8483}]},"scatter":null,"selection":{"population":"all galaxies in the weighted combination of the resimulated regions","warning":"Intrinsic far-UV luminosity function of FLARES at z=14, read from the vector paths of Wilkins et al. 2023. Conversions (exact): M_UV = 51.5948 - 2.5 log10(L_FUV / erg s^-1 Hz^-1) (AB, 10 pc), and log phi per magnitude = log phi per dex + log10(0.4). Binned in 0.1 dex of log L_FUV; bright-end bins hold few galaxies and are noisy. The paper also tabulates space densities in 0.2 dex bins without saying whether they are attenuated or intrinsic; those are not used."},"definitions":{"imf":"chabrier03","cosmology":{"H0":67.77,"Om":0.307},"densityFrame":"comoving","uvBand":"far-UV (1500 A), L_FUV","dustCorrection":"none (intrinsic)","population":"all"},"provenance":{"tier":"digitized-figure","citation":"Wilkins et al. 2023, MNRAS 519, 3118 (arXiv:2204.09431), far-UV luminosity function at z=15 to 10, intrinsic, z=14","doi":"10.1093/mnras/stac3280","url":"https://arxiv.org/abs/2204.09431","retrieved":"2026-10-05","figure":"Observed and intrinsic far-UV luminosity function at z=15 to 10","panel":"z=14, dashed line","checksumSha256":"e54af1794498ade1adb10e076ad226b87b58a9c4205c03c03b21c317839b1958","sourceMember":"figures/UVLF_panel.pdf","extractionMethod":"vector path vertices from the figure PDF (PyMuPDF get_drawings), transformed through axes calibrated on labelled tick marks","axisCalibrationPixels":"x: numeric tick labels snapped to ticks (log L_FUV); y: log phi per dex labels paired with ticks (minus glyphs are separate); x converted to M_UV, y to per magnitude","digitizationUncertaintyDex":0.02},"calibration":"prediction","rankable":false,"notes":"Vector-path extraction; exact to PDF coordinate precision, so uncertainty is the plotted line, not marker tracing."},{"id":"wilkins22.flares.uvlf.observed.z13","source":"FLARES","run":"40 resimulated regions (EAGLE AGNdT9 model), dust attenuated","kind":"simulation","relation":"uvlf","epoch":{"zRepresentative":13,"zNominal":13,"zMin":13,"zMax":13,"mode":"published-epoch","snapshot":null},"axes":{"xDefinition":"absolute UV magnitude M_UV from the far-UV luminosity, dust attenuated (AB)","xUnit":"mag (AB)","yDefinition":"log10 UV luminosity function per magnitude","yUnit":"log10(cMpc^-3 mag^-1)"},"domain":{"xMin":-20.405,"xMax":-17.905},"representation":{"type":"points","intervalKind":"unspecified","connect":true,"points":[{"x":-20.405,"y":-6.7942},{"x":-20.155,"y":-5.4285},{"x":-19.905,"y":-6.2631},{"x":-19.655,"y":-5.1651},{"x":-19.405,"y":-4.7038},{"x":-19.155,"y":-4.3889},{"x":-18.905,"y":-4.183},{"x":-18.655,"y":-3.8189},{"x":-18.405,"y":-3.7411},{"x":-18.155,"y":-3.5482},{"x":-17.905,"y":-3.5478}]},"scatter":null,"selection":{"population":"all galaxies in the weighted combination of the resimulated regions","warning":"Observed far-UV luminosity function of FLARES at z=13, read from the vector paths of Wilkins et al. 2023. 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