Table 7
Circumstellar model excess ratios.
| Excess ratios | Temp | Ossenkopf et al. (1992)-O-richCold | Suh (1999)-SILC | Rosenthal et al. (2000) | ||||||
|---|---|---|---|---|---|---|---|---|---|---|
| curve_1 | curve_2 | curve_3 | curve_4 | curve_5 | curve_6 | curve_7 | curve_8 | curve_9 | ||
| [K] | (max_0.25) | (max_0.75) | (max_2.00) | (max_0.25) | (max_0.75) | (max_2.00) | (peak_1.4) | (peak_0.4) | (peak_0.2) | |
| E(Ks−A) E(Ks−D) |
3200 | 0.990 | 0.964 | 0.895 | 1.144 | 0.979 | 0.899 | 0.889 | 0.882 | 0.905 |
| E(Ks−C) E(Ks−D) |
3200 | 0.624 | 0.905 | 0.854 | 0.966 | 0.979 | 0.923 | 0.548 | 0.906 | 0.956 |
| E(Ks−E) E(Ks−D) |
3200 | 0.871 | 0.971 | 0.983 | 0.417 | 0.880 | 0.869 | 0.715 | 0.967 | 1.000 |
| E(Ks−W1) E(Ks−W3) |
3200 | 1.321 | 0.790 | 0.404 | 1.219 | 0.806 | 0.413 | 1.738 | 0.693 | 0.608 |
| E(Ks−W2) E(Ks−W3) |
3200 | 1.674 | 1.046 | 0.677 | 1.499 | 1.040 | 0.671 | 2.368 | 0.943 | 0.828 |
| E(Ks−W4) E(Ks−W3) |
3200 | 1.367 | 1.089 | 1.132 | 0.687 | 0.983 | 1.006 | 1.467 | 1.121 | 1.078 |
| E(Ks−[3.6]) E(Ks−[5.8]) |
3200 | 0.779 | 0.759 | 0.504 | 0.781 | 0.779 | 0.519 | 0.701 | 0.701 | 0.701 |
| E(Ks−[4.5]) E(Ks−[5.8]) |
3200 | 0.921 | 0.923 | 0.733 | 0.898 | 0.925 | 0.734 | 0.872 | 0.872 | 0.872 |
| E(Ks−[8.0]) E(Ks−[5.8]) |
3200 | 0.926 | 1.002 | 1.210 | 0.991 | 1.009 | 1.219 | 0.806 | 1.006 | 1.060 |
| E(Ks−A) E(Ks−D) |
2600 | 0.969 | 0.958 | 0.891 | 1.125 | 0.972 | 0.894 | 0.858 | 0.875 | 0.903 |
| E(Ks−C) E(Ks−D) |
2600 | 0.614 | 0.905 | 0.853 | 0.969 | 0.979 | 0.923 | 0.539 | 0.905 | 0.956 |
| E(Ks−E) E(Ks−D) |
2600 | 0.869 | 0.971 | 0.982 | 0.400 | 0.878 | 0.869 | 0.709 | 0.968 | 1.001 |
| E(Ks−W1) E(Ks−W3) |
2600 | 1.365 | 0.799 | 0.408 | 1.257 | 0.815 | 0.416 | 1.798 | 0.695 | 0.608 |
| E(Ks−W2) E(Ks−W3) |
2600 | 1.726 | 1.051 | 0.680 | 1.539 | 1.043 | 0.672 | 2.442 | 0.944 | 0.826 |
| E(Ks−W4) E(Ks−W3) |
2600 | 1.398 | 1.093 | 1.138 | 0.685 | 0.986 | 1.009 | 1.490 | 1.123 | 1.078 |
| E(Ks−[3.6]) E(Ks−[5.8]) |
2600 | 0.781 | 0.763 | 0.507 | 0.781 | 0.782 | 0.521 | 0.703 | 0.703 | 0.703 |
| E(Ks−[4.5]) E(Ks−[5.8]) |
2600 | 0.920 | 0.924 | 0.734 | 0.898 | 0.926 | 0.736 | 0.873 | 0.873 | 0.873 |
| E(Ks−[8.0]) E(Ks−[5.8]) |
2600 | 0.920 | 1.001 | 1.212 | 0.985 | 1.008 | 1.223 | 0.793 | 1.004 | 1.060 |
Notes. Circumstellar excess ratios were calculated with the MSX, WISE, and GLIMPSE filter response curves, with a stellar spectrum (Allard et al. 2011) and an extinction curve. The columns curve_1, curve_2, and curve_3 refer to the circumstellar extinction curves obtained with DUSTY and the cold O-rich silicates by Ossenkopf et al. (1992) adopting a maximum size of 0.25, 0.75, and 2.0 μm, respectively (see text). The columns curve_4, curve_5, and curve_6 refer to the circumstellar extinction curves obtained with DUSTY and the cold silicates (SILC) by Suh (1999) adopting a maximum size of 0.25, 0.75, and 2.0 μm, respectively, (see text). The spectrum of a naked star of 3200 K is used to obtain the naked star colours in the upper part of the table (first 9 rows). In the lower part of the table, the spectrum of a naked star of 2600 K is used. For comparison, the columns curve_7, curve_8, and curve_9 refer to the parametric formula for Galactic interstellar extinction by Rosenthal et al. (2000) normalized at 2.12 μm with the silicate peak set at 1.4, 0.4, and 0.2, respectively.
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