A. Putze et al.: An MCMC technique to sample transport and source parameters of Galactic cosmic rays. II. Fig. C.1. Posterior PDFs of the model parameters (using the Binary S pace Partitioning step—see Paper I, and the B/C constraint). The diagonals show the 1D marginalised PDF of the ind icated parameters, and the red line results from a Gaussian fi t to the histogram. Off-diagonal plots show the 2D marg inalised posterior PDFs for the parameters in the same colu mn and same line, respectively. The colour code corresponds t o the regions of increasing probability (from paler to darker s hades), and the two contours (smoothed) delimit regions containing respectively 68% and 95% (inner and outer conto ur) of the PDF. Left panel: PDFs for { V$_{c}$, δ, K$_{0}$, V$_{a}$ } . R ight panel: the same PDFs but shown for a different combinatio n of the parameters { V$_{c}$, δ, K$_{0}$/L × 50 $^{δ}$, V$_{a}$ / √ K$_{0}$ × 3 δ (4 − δ $^{2}$)(4 − δ ) } . parameter, and a small asymmetry for the V$_{a}$ parameter. The right p anel shows the same PDFs, but for the following combinatio ns of the transport parameters: A last combination is for the local bubble parameter r$_{h}$ : √ K$_{0}$ × 3 δ (4 − δ $^{2}$)(4 − δ ) These for ms are inspired by the known degeneracies be- tween para meters. For instance, in diffusion models, the secondary to primary ratio is expected to remain un- changed as long as the effective grammage 〈 x 〉 of the model is left unchanged. For pure diffusion, we obtain (Jones et a l. 2001; Maurin et al. 2006) for the grammage 〈 x 〉 = Σ vL / (2 K ) = Σ L/ (2 cK$_{0}$ ( R / 1GV) $^{δ}$), where Σ is the surface de nsity. Apart from the K$_{0}$ − L degeneracy, the parameters K$_{0}$ and δ are correlated. We find that the com- bination K$_{0}$ × 50 δ is appropriate for removing the K$_{0}$ PDF’s tail (see F ig. C.1). The origin of the value 50 is unclear. It may be rela ted to the energy range covered by B/C HEAO- 3 data on which the fits are based. The combination used for V$_{a}$ [Eq. (C.2)] comes directly from the form of the reac- celeration t erm Eq. (5). Reacceleration only plays a role at low energy, so we can take R δ ≈ 1 and end up with the combinatio n presented in Eq. (C.2). The independent ac- ceptance f$_{i}$$_{nd}$ , defined in Paper I as the ratio of the number of indepen dent samples to the total step number, increases from 1/3 t o 1/2 by using the above described parameter combinations for the four parameter model presented in Fig. C.1. Unless specified otherwise, the reference B/C dataset used throughout the paper is denoted dataset F: it consists of i) low-energy data taken by the IMP7-8 (Garcia-Munoz et al. 1987), the Voyager 1&2 (Lukasiak et al. 1999), and the ACE-CRIS (de Nolfo et al. 2006) spacecrafts; ii) intermediate energies acquired by HEA0-3 data (Engelmann et al. 1990); and iii) higher energy data from Spacelab (Swordy et al. 1990) and the published CREAM data (Ahn et al. 2008). Other existing data are discarded either because of their too large error bars, or because of their inconsistency with the above data (see Paper I). For $^{10}$Be/$^{9}$Be, the data are taken from balloon flights (Hagen et al. 1977; Buffington et al. 1978; Webber & Kish 1979), including the ISOMAX balloon- borne instrument (Hams et al. 2004), and from the IMP-7/8 (Garcia-Munoz et al. 1977), ISEE-3 (Wiedenbeck & Greiner 1980), Ulysses (Connell 1998), This c omes from the form of Eq. (10), where the flux damp- ing for radioactive species (due to the local bubble) is ef- fective only at low energy ( γ ≈ 1, R ≈ 1). Appendix D: Datasets for CR measurements D.1. B/C ratio D.2. Isotopic and elemental ratios of radioactive species K$_{0}$ ←→ K$_{0}$ L × 50 δ (C.1) V$_{a}$ ←→ V$_{a}$ (C.2) r$_{h}$ ←→ r$_{h}$ √$_{K}$$_{0}$ . (C.3) 18 19 20 0 0.5 1  [km/s] c V 0.8 0.9 18 19 20 0.8 0.9 0 5 10 0.004 0.006 0.008 18 19 20 0.8 0.9 0.004 0.006 0.008 0.004 0.006 0.008 0 200 400 600 /Myr] 2  [kpc 0 K 35 40 45 18 19 20 0.8 0.9 35 40 45 0.004 0.006 0.008 35 40 45 35 40 45 0 0.1 0.2 Va [km/s] Burn­In length: 2.9 Correlation Length: 5.8 : 135156/400000 = 33.789% ind f /d.o.f: 1.47 min 2 Chain analysis Binary space partitioning step Model III-F 18 19 20 0 0.5 1  [km/s] c V 0.8 0.9 18 19 20 0.8 0.9 0 5 10 0.032 0.034 0.036 18 19 20 0.8 0.9 0.032 0.034 0.036 0.032 0.034 0.036 0 200 400  [kpc/Myr] /L*50 0 K 100 110 18 19 20 0.8 0.9 100 110 0.032 0.034 0.036 100 110 100 110 0 0.05 0.1 0.15 /kpc] Myr  [km/s  ) )(4 -  2 (4 - Burn­In length: 3.0 Correlation Length: 1.9 : 209947/400000 = 52.487% ind f /d.o.f: 1.47 min 2 Chain analysis Binary space partitioning step Model III-F 19