Table 4
Spectral slopes of the detected excesses.
| HD | a | σ a | a 2000 K | a 1500 K | a 1000 K | a 500 K |
|
|
||||||
| 2262 | –0.63 | 1.49 | 1.01 | 1.48 | 2.28 | 3.46 |
| 7788 | 0.04 | 1.67 | 2.06 | 3.11 | 5.00 | (8.46) |
| 14412 | –0.93 | 1.69 | 1.27 | 1.95 | 3.14 | (4.94) |
| 20794 | 0.50 | 2.41 | 1.94 | 2.98 | 4.80 | (7.99) |
| 28355 | –1.13 | 1.41 | 1.33 | 1.96 | (3.12) | (5.25) |
| 39060 | 0.11 | 1.89 | 1.41 | 2.09 | 3.32 | 5.42 |
| 104731 | 0.39 | 1.38 | 0.82 | 1.23 | 1.97 | 3.30 |
| 108767 | 1.47 | 1.35 | 1.14 | 1.63 | 2.50 | 4.00 |
| 210302 | 4.61 | 2.15 | 1.37 | 2.06 | 3.32 | 5.63 |
|
|
||||||
| 172555 | 8.02 | 2.12 | (1.37) | 2.12 | 3.65 | 7.25 |
| 182572 | 3.97 | 1.06 | (0.29) | (0.48) | 0.87 | 1.81 |
| 210049 | 10.50 | 3.10 | (0.58) | (0.94) | 1.74 | 3.81 |
Notes. Slopes and uncertainties are listed in % /μm. In addition to the measured values, we list for all targets the spectral slopes of purely thermal excesses with black body temperatures of 2000 K, 1500 K, 1000 K, and 500 K. For targets marked in bold face, constraints on the emission mechanism or the black body temperature are possible. Measured slopes marked in bold face are significantly different from a zero slope, i.e., with scattered light emission, while black body slopes in parentheses can be ruled out. The three last targets are the tentative detections of circumstellar excess based on the spectral analysis, but are not detected as broad band excesses by our original approach.
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