| Experiment | Value (ppm) |
|---|---|
| midHolocene | 264.4 |
| lgm | 190 |
| past1000 | Time varying Meinshausen et al., CMIP6 GMD special issue |
| lig127k | 275 |
| midPliocene-eoi400 | 400 |
| LDv1-LGMspin | Same as lgm |
| LDv1-transpin LDv1 | Transient, as per Bereiter et al. (2015) [ Bereiter et al data access ] (md5sum = c54a033d8cbf588bc2b95d3b92ff9b1c) |
| PDGv1-PGMspin | 191 |
| PDGv1 | CO2 = Transient, as per the spline of Koehler et al. (2017): [ Access to data ] |
| Experiment | Value (ppb) |
|---|---|
| midHolocene | 597 |
| lgm | 375 |
| past1000 | Time varying Meinshausen et al., CMIP6 GMD special issue |
| lig127k | 685 |
| midPliocene-eoi400 | Same as in CMIP6 piControl |
| LDv1-LGMspin | Same as lgm |
| LDv1-transpin LDv1 | Transient, as per Loulergue et al. (2008) Get reference and data below! |
| PDGv1-PGMspin | 385 |
| PDGv1 | Transient, as per the spline of Koehler et al. (2017): [ Access to data ] |
338187b58a48d8cb5496f0d7c98528bb| Experiment | Value (ppb) |
|---|---|
| midHolocene | 262 |
| lgm | 200 |
| past1000 | Time varying Meinshausen et al., CMIP6 GMD special issue |
| lig127k | 255 |
| midPliocene-eoi400 | Same as in CMIP6 piControl |
| LDv1-LGMspin | Same as lgm |
| LDv1-transpin LDv1 | Transient, as per Schilt et al. (2010) Get reference and data below! |
| PDGv1-PGMspin | 201 |
| PDGv1 | Linear increase from 201 ppb at 140 ka to 218.74 ppb at 134.5 ka then transient, as per the spline of Koehler et al. (2017): [ Access to data ] |
a99f2d791256774f3296871aaf4ee9bd| Experiment | Value |
|---|---|
| midHolocene | 0 |
| lgm | 0 |
| past1000 | 0 |
| lig127k | 0 |
| midPliocene-eoi400 | Same as in CMIP6 piControl |
| LDv1-LGMspin LDv1-transpin LDv1 | Same as lgm |
| PDGv1-PGMspin PDGv1 | 0 |
| Experiment | Value |
|---|---|
| midHolocene lgm lig127k midPliocene-eoi400 LDv1-LGMspin LDv1-transpin LDv1 PDGv1-PGMspin PDGv1 | Same as in CMIP6 piControl |
| past1000 | For models without interactive ozone chemistry, we suggest that O3 modulation is derived in a similar way from the modulation of the UV part of the solar spectrum as in the historical simulations (c.f. Matthes et al., CMIP6 GMD special issue 2016) |