Table 1
Color-excess ratios.
| ⟨E(J−λ) /E(J−Ks)⟩ | λ (μm) | Demographic |
|
|
||
| 0 | J (1.2) | – |
| 0.66 ± 0.05 | H(1.7) | Type II Cepheids |
| 0.67 ± 0.01 | H(1.7) | RR Lyrae |
| 0.70 ± 0.01 | H(1.7) | classical Cepheids |
| 0.63 ± 0.01 | H(1.7) | O stars |
| 1 | Ks (2.2) | – |
| 1.28 ± 0.04 | W1 (3.4) | classical Cepheids |
| 1.25 ± 0.02 | W1 (3.4) | Type II Cepheids |
| 1.31 ± 0.05 | W1 (3.4) | RR Lyrae |
| 1.33 ± 0.02 | W1 (3.4) | O stars |
| 1.27 ± 0.01 | S1(3.6) | Type II Cepheids |
| 1.25 ± 0.02 | S1 (3.6) | RR Lyrae |
| 1.28 ± 0.01 | S1 (3.6) | O stars |
| 1.33 ± 0.02 | S2(4.5) | RR Lyrae |
| 1.37 ± 0.09 | S2(4.5) | O stars |
| ∗ 1.54 ± 0.01 | W2(4.6) | O stars |
| 1.35 ± 0.01 | S3(5.8) | Type II Cepheids |
| 1.30 ± 0.02 | S3(5.8) | RR Lyrae |
| 1.48 ± 0.06 | S3(5.8) | O stars |
| 1.46 ± 0.06 | W4 (22) | classical Cepheids |
|
|
||
| ⟨E(V−λ) /E(B−V)⟩ | ||
|
|
||
| 2.26 ± 0.03 | J (1.2) | O stars |
| 2.24 ± 0.09 | J (1.2) | classical Cepheids |
| 2.58 ± 0.04 | H (1.7) | O stars |
| 2.54 ± 0.06 | H (1.7) | classical Cepheids |
| 2.77 ± 0.06 | Ks (2.2) | O stars |
| 2.70 ± 0.06 | Ks (2.2) | classical Cepheids |
| 2.94 ± 0.06 | W1 (3.4) | O stars |
| 2.74 ± 0.02 | W1 (3.4) | classical Cepheids |
| 3.04 ± 0.05 | S1 (3.6) | O stars |
| 3.13 ± 0.01 | S2 (4.5) | O stars |
| 2.98 ± 0.04 | W2 (4.6) | O stars |
| 3.24 ± 0.06 | S3 (5.8) | O stars |
| 3.10 ± 0.26 | W4 (22) | classical Cepheids |
Notes. Near-infrared observations are on the 2MASS system, and Sx and Wx signify Spitzer and WISE data, respectively. Contamination from the environment encircling O stars is probable beyond J−5.8 μm, and the lower-resolution J−4.6 μm (W2) passband relative to the bracketing Spitzer filters (S1, S2). The uncertainties cited reflect the spread between the fitting algorithms (see Sect. 2.2).
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