Table 2
IR excess derived by SPIPS.
| Star | Δmag(K) | Δmag(L) | Δmag(N) |
|---|---|---|---|
| X Sgr | 0.056 ± 0.032 | 0.058 ± 0.017 | 0.058 ± 0.013 |
| U Aql | 0.016 ± 0.022 | 0.024 ± 0.012 | 0.036 ± 0.014 |
| η Aql | 0.037 ± 0.022 | 0.085 ± 0.023 | 0.091 ± 0.007 |
| β Dor | 0.040 ± 0.014 | 0.080 ± 0.025 | 0.095 ± 0.016 |
| ζ Gem | 0.023 ± 0.032 | 0.060 ± 0.014 | 0.148 ± 0.017 |
| TT Aql | −0.006 ± 0.035 | 0.019 ± 0.017 | 0.000 ± 0.014 |
| T Mon | 0.048 ± 0.034 | 0.115 ± 0.031 | 0.094 ± 0.015 |
| U Car | 0.096 ± 0.024 | 0.110 ± 0.025 | 0.142 ± 0.010 |
Notes. The IR excess in the K, L, and N band is derived as the difference between the median magnitude observed in each photometric band and the magnitude of the atmosphere model (see the blue bars in Fig. 2). A positive value of Δ mag represents an excess, and a negative value indicates absorption.
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