Table 3.
Infrared excess in CCs with mid-IR spectra.
| Name | L |  |
BIC | L | τ | Tinn | Rinn | p | Gr. |  |
BIC | ΔMbol | ΔV | ΔK | ΔV | ΔK | ΔN | Remarks |
|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|
| (L⊙) | (L⊙) | (⋅10−4) | (K) | (R⋆) | (%) | (mag) | (mag) | (mag) | ||||||||||
| ζ Gem | 3204 ± 2.3 | 38.7 | −2183 | 3168 ± 4.7 | 13.7 ± 1.8 | 1546 ± 187 | 13 | 1.90 ± 0.06 | 94 | 32.5 | −4847 | −0.012 | −0.013 | −0.010 | 0.000 | −0.003 | −0.013 | |
| η Aql | 3008 ± 2.0 | 24.0 | −8050 | 2970 ± 3.9 | 9.0 ± 0.8 | 1394 ± 98 | 11 | 2.02 ± 0.05 | 90 | 19.5 | −10028 | −0.014 | −0.015 | −0.013 | 0.001 | −0.002 | −0.013 | |
| α UMi | 2413 ± 1.2 | 32.6 | −19409 | 2260 ± 10.1 | 14.1 ± 1.1 | 1091 ± 37 | 50 | 2.58 ± 0.03 | 80 | 26.8 | −27673 | −0.071 | −0.072 | −0.067 | 0.001 | −0.004 | −0.046 | |
| β Dor | 2863 ± 89 | 243.6 | 24737 | no convergence | ||||||||||||||
| δ Cep | 1984 ± 0.90 | 16.8 | −45576 | 1955 ± 6.0 | 6.2 ± 0.4 | 1218 ± 69 | 32 | 2.26 ± 0.03 | 90 | 16.7 | −45726 | −0.016 | −0.017 | −0.015 | 0.000 | −0.001 | −0.012 | |
| l Car | 12316 ± 7.9 | 31.2 | −22071 | 12313 ± 8.4 | 1.6 ± 0.9 | 2825 ± 938 | 1.8 | 2.0 f | 80 | 31.2 | −22144 | −0.000 | 0.000 | 0.000 | − | − | − | insignificant |
| AY Cen | 1864 ± 3.2 | 13.1 | −15069 | 1808 ± 6.0 | 48.6 ± 8.6 | 1590 ± 154 | 14 | 2.39 ± 0.13 | 80 | 9.4 | −16561 | −0.033 | −0.035 | −0.023 | 0.002 | −0.010 | −0.040 | |
| SU Cyg | 910 ± 0.90 | 72.7 | 8981 | 897 ± 1.3 | 3.5 ± 0.6 | 1126 ± 115 | 44 | 2.10 ± 0.10 | 80 | 54.3 | 1257 | −0.016 | −0.014 | −0.013 | 0.000 | −0.001 | −0.014 | |
| S TrA | 486 ± 0.90 | 36.2 | −4498 | 473 ± 1.0 | 2.7 ± 0.4 | 512 ± 36 | 370 | 2.88 ± 0.14 | 80 | 16.2 | −12352 | −0.029 | −0.029 | −0.029 | 0.000 | 0.000 | −0.038 | |
| V Cen | 1657 ± 2.2 | 22.1 | −10162 | 1615 ± 2.6 | 15.1 ± 1.4 | 1668 ± 122 | 11 | 1.77 ± 0.04 | 80 | 8.7 | −15908 | −0.028 | −0.029 | −0.025 | 0.001 | −0.002 | −0.029 | |
| V1334 Cyg | 1871 ± 1.7 | 25.2 | −9630 | 1845 ± 2.2 | 26.1 ± 2.5 | 3236 ± 382 | 2.1 | 1.76 ± 0.05 | 80 | 15.6 | −13564 | −0.015 | +0.054 | −0.012 | ||||
| 1764 ± 1.6 | 24.5 | −9928 | 1740 ± 2.1 | 2.8 ± 0.2 | 979 ± 48 | 63 | 1.96 ± 0.06 | 80 | 14.4 | −13915 | −0.015 | −0.015 | −0.015 | −0.002 | −0.003 | −0.017 | binary corrected | |
| RS Pup | 13778 ± 14.5 | 36.2 | −1805 | 13727 ± 16.6 | 5.4 ± 2.5 | 1300 f | 18 | 2.0 f | 90 | 36.2 | −1813 | −0.004 | −0.004 | −0.004 | − | − | − | insignificant |
Notes. Column 1 gives the name of the Cepheid. Columns 2–4 give the luminosity (for the best-fitting effective temperatue), the reduced χ2 and the BIC statistics. Columns 5–10 give the results for the best-fitting model including a dust component: luminosity, dust optical depth at 0.55 μm, temperature of the dust at the inner radius, the corresponding inner radius in stellar radii, and slope of the density law. An “f” in Cols. 7–9 means that parameter is fixed. The number in Col. 10 indicates the percentage of iron in the grain (see main text), while Cols. 11–12 give the statistics for this model. Columns 12–14 give the difference in magnitude between the standard case and the model with dust bolometrically, and in the V and K. A negative magnitude implies that the model with dust is fainter. Columns 15–17 give the difference in magnitude between the model with dust and the photosphere in the V, K and N band. A positive magnitude implies that photosphere is brighter.
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