The SMC–LMC modulus difference, Δμ0, derived in various ways. The values corrected for metallicity and/or other population effects, Δμ0cor, are also listed. Their errors include the uncertainty of this correction. References are indicated in the last column.
| Method | Δμ0 | Δμ0cor | Notes | Ref. |
| Type II Cepheids (WV) | 0.40 ± 0.07 | – | (1) | This work |
| 0.39 ± 0.05 | – | (2) | This work | |
| Classical Cepheids | 0.48 ± 0.01 | 0.43 ± 0.05 | (1,3,4) | This work |
| 0.48 ± 0.01 | 0.43 ± 0.05 | (2,3,4) | This work | |
| 0.48 ± 0.04 | 0.43 ± 0.06 | (1,3) | Groenewegen (2000) | |
| 0.51 ± 0.02 | 0.46 ± 0.05 | (2,3) | Groenewegen (2000) | |
| 0.41 ± 0.20 | 0.39 ± 0.20 | (1) | Bono et al. (2010) | |
| 0.45 ± 0.12 | 0.44 ± 0.12 | (2) | Bono et al. (2010) | |
| RR Lyrae variables | 0.327 ± 0.002 | 0.363 ± 0.04 | (1,5) | Szewczyk et al. (2009) |
| Red clump giants | 0.47 ± 0.03 | 0.43 | (1,6) | Pietrzyński, Gieren & Udalski (2003) |
| 0.38 ± 0.02 | 0.45 ± 0.10 | (2) | Pietrzyński et al. (2003) | |
| Tip of RGB | – | 0.40 ± 0.12 | (2,7) | Sakai et al. (2004) |
| Pulsating M giants | 0.41 ± 0.02 | – | (1,8) | Tabur et al. (2010) |
| Eclipsing binaries | – | 0.5 ± 0.15 | (9) | – |
| Method | Δμ0 | Δμ0cor | Notes | Ref. |
| Type II Cepheids (WV) | 0.40 ± 0.07 | – | (1) | This work |
| 0.39 ± 0.05 | – | (2) | This work | |
| Classical Cepheids | 0.48 ± 0.01 | 0.43 ± 0.05 | (1,3,4) | This work |
| 0.48 ± 0.01 | 0.43 ± 0.05 | (2,3,4) | This work | |
| 0.48 ± 0.04 | 0.43 ± 0.06 | (1,3) | Groenewegen (2000) | |
| 0.51 ± 0.02 | 0.46 ± 0.05 | (2,3) | Groenewegen (2000) | |
| 0.41 ± 0.20 | 0.39 ± 0.20 | (1) | Bono et al. (2010) | |
| 0.45 ± 0.12 | 0.44 ± 0.12 | (2) | Bono et al. (2010) | |
| RR Lyrae variables | 0.327 ± 0.002 | 0.363 ± 0.04 | (1,5) | Szewczyk et al. (2009) |
| Red clump giants | 0.47 ± 0.03 | 0.43 | (1,6) | Pietrzyński, Gieren & Udalski (2003) |
| 0.38 ± 0.02 | 0.45 ± 0.10 | (2) | Pietrzyński et al. (2003) | |
| Tip of RGB | – | 0.40 ± 0.12 | (2,7) | Sakai et al. (2004) |
| Pulsating M giants | 0.41 ± 0.02 | – | (1,8) | Tabur et al. (2010) |
| Eclipsing binaries | – | 0.5 ± 0.15 | (9) | – |
Notes. (1) Based on near-IR photometry, Ks or K. (2) Based on optical photometry, I or W(VI). (3) Our adopted metallicity correction, 0–0.1 mag, was used to derive Δμ0cor. (4) Only those with 0.4 < log P < 1.0 were used. (5) Taking the means of the values based on different calibrations discussed in Szewczyk et al. (2009). (6) The population correction suggested by Salaris & Girardi (2002) was used. (7) A metallicity correction was derived using the colour of the RGB. (8) Tabur et al. (2010) concluded that the metallicity effect is negligible. (9) This value is a rough estimate (see text).
The SMC–LMC modulus difference, Δμ0, derived in various ways. The values corrected for metallicity and/or other population effects, Δμ0cor, are also listed. Their errors include the uncertainty of this correction. References are indicated in the last column.
| Method | Δμ0 | Δμ0cor | Notes | Ref. |
| Type II Cepheids (WV) | 0.40 ± 0.07 | – | (1) | This work |
| 0.39 ± 0.05 | – | (2) | This work | |
| Classical Cepheids | 0.48 ± 0.01 | 0.43 ± 0.05 | (1,3,4) | This work |
| 0.48 ± 0.01 | 0.43 ± 0.05 | (2,3,4) | This work | |
| 0.48 ± 0.04 | 0.43 ± 0.06 | (1,3) | Groenewegen (2000) | |
| 0.51 ± 0.02 | 0.46 ± 0.05 | (2,3) | Groenewegen (2000) | |
| 0.41 ± 0.20 | 0.39 ± 0.20 | (1) | Bono et al. (2010) | |
| 0.45 ± 0.12 | 0.44 ± 0.12 | (2) | Bono et al. (2010) | |
| RR Lyrae variables | 0.327 ± 0.002 | 0.363 ± 0.04 | (1,5) | Szewczyk et al. (2009) |
| Red clump giants | 0.47 ± 0.03 | 0.43 | (1,6) | Pietrzyński, Gieren & Udalski (2003) |
| 0.38 ± 0.02 | 0.45 ± 0.10 | (2) | Pietrzyński et al. (2003) | |
| Tip of RGB | – | 0.40 ± 0.12 | (2,7) | Sakai et al. (2004) |
| Pulsating M giants | 0.41 ± 0.02 | – | (1,8) | Tabur et al. (2010) |
| Eclipsing binaries | – | 0.5 ± 0.15 | (9) | – |
| Method | Δμ0 | Δμ0cor | Notes | Ref. |
| Type II Cepheids (WV) | 0.40 ± 0.07 | – | (1) | This work |
| 0.39 ± 0.05 | – | (2) | This work | |
| Classical Cepheids | 0.48 ± 0.01 | 0.43 ± 0.05 | (1,3,4) | This work |
| 0.48 ± 0.01 | 0.43 ± 0.05 | (2,3,4) | This work | |
| 0.48 ± 0.04 | 0.43 ± 0.06 | (1,3) | Groenewegen (2000) | |
| 0.51 ± 0.02 | 0.46 ± 0.05 | (2,3) | Groenewegen (2000) | |
| 0.41 ± 0.20 | 0.39 ± 0.20 | (1) | Bono et al. (2010) | |
| 0.45 ± 0.12 | 0.44 ± 0.12 | (2) | Bono et al. (2010) | |
| RR Lyrae variables | 0.327 ± 0.002 | 0.363 ± 0.04 | (1,5) | Szewczyk et al. (2009) |
| Red clump giants | 0.47 ± 0.03 | 0.43 | (1,6) | Pietrzyński, Gieren & Udalski (2003) |
| 0.38 ± 0.02 | 0.45 ± 0.10 | (2) | Pietrzyński et al. (2003) | |
| Tip of RGB | – | 0.40 ± 0.12 | (2,7) | Sakai et al. (2004) |
| Pulsating M giants | 0.41 ± 0.02 | – | (1,8) | Tabur et al. (2010) |
| Eclipsing binaries | – | 0.5 ± 0.15 | (9) | – |
Notes. (1) Based on near-IR photometry, Ks or K. (2) Based on optical photometry, I or W(VI). (3) Our adopted metallicity correction, 0–0.1 mag, was used to derive Δμ0cor. (4) Only those with 0.4 < log P < 1.0 were used. (5) Taking the means of the values based on different calibrations discussed in Szewczyk et al. (2009). (6) The population correction suggested by Salaris & Girardi (2002) was used. (7) A metallicity correction was derived using the colour of the RGB. (8) Tabur et al. (2010) concluded that the metallicity effect is negligible. (9) This value is a rough estimate (see text).
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