Table 4
Available constraints on the near- and mid-infrared excess around Vega.
| Wavelength | F meas | Excess | Instruments |
| [μm] | [Jy] | [%] | |
|
|
|||
| 1.26 | 1574 ± 34 | 2.4 ± 2.9% | Catalina1, UKIRT2 |
| 1.60 | 1055 ± 32 | -2.4 ± 3.6% | Catalina1 |
| 1.65 | – | 1.23 ± 0.53% | IOTA/IONIC |
| 2.12 | – | 1.29 ± 0.19% | CHARA/FLUOR3 |
| 2.12 | – |
|
PTI4 |
| 2.20 | 655 ± 14 | 4.1 ± 3.0% | Catalina1, UKIRT2 |
| 3.54 | 283 ± 6 | 3.1 ± 3.0% | Catalina1, UKIRT2 |
| 4.80 | 167 ± 8 | 7.1 ± 5.1% | Catalina1, UKIRT2 |
| 10 | 40.0 ± 3 | 6.0 ± 4.5% | Various5 |
| 10.5 | 33.7 ± 0.33 | 0.0 ± 5.0% | IRS spectrum |
| 10.6 | – | 0.2 ± 0.7% | MMT/BLINC6 |
| 12 | 27.0 ± 0.3 | 1.2 ± 5.0% | IRAS7 |
| 12.5 | 23.89 ± 0.39 | 0.0 ± 5.0% | IRS spectrum |
Notes. The superscript on the name of the instrument in the last column gives the reference: (1) Campins et al. (1985), (2) Blackwell et al. (1983), (3) Absil et al. (2008), (4) Ciardi et al. (2001), (5) Rieke et al. (1985), (6) Liu et al. (2004), (7) Cohen et al. (1992), with the absolute photometric error estimated by Aumann et al. (1984). The interferometric data from IONIC, FLUOR, PTI, and BLINC only sample a specific part of the inner disc, while the photometric studies include Vega’s entire environment.
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