Table 4: Available constraints on the near- and mid-infrared excess around Vega. References: (1) Campins et al. (1985); (2) Blackwell et al. (1983); (3) Rieke et al. (1985); (4) Liu et al. (2004); (5) Cohen et al. (1992), with the absolute photometric error estimated by Aumann et al. (1984). The photometric data in references (1), (2) and (3) have been compared to the most recent Kurucz photospheric model of Vega (Bohlin & Gilliland 2004), which has a typical uncertainty of 2% in the infrared (this uncertainty has been added to the estimated errors on the measurements). Note that the interferometric data from FLUOR and BLINC only sample a specific part of the inner disk, while the photometric studies include Vega's entire environment.
Wavelength Excess Instruments References
1.26 $\mu $m $2.4 \pm 2.9$% Catalina, UKIRT (1), (2)
1.60 $\mu $m $-2.4 \pm 3.6$% Catalina (1)
2.12 $\mu $m $1.29 \pm 0.19$% CHARA/FLUOR This study
2.20 $\mu $m $4.1 \pm 3.0$% Catalina, UKIRT (1), (2)
3.54 $\mu $m $3.1 \pm 3.0$% Catalina, UKIRT (1), (2)
4.80 $\mu $m $7.1 \pm 5.1$% Catalina, UKIRT (1), (2)
10 $\mu $m $6 \pm 4.5$% Various (3)
10.6 $\mu $m $0.2 \pm 0.7$% MMT/BLINC (4)
12 $\mu $m $1.2 \pm 5$% IRAS (5)

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