Photometric observations and excess emission from Fomalhaut. The excess fluxes (|$F_\mathrm{disc})$| were obtained by subtracting the star’s photosphere flux from total observed fluxes (except for ALMA-imaging-derived disc fluxes, denoted by a), which are obtained from the corresponding references. For the photosphere fluxes, we use a stellar SED modelled with PHOENIX (Allard, Homeier & Freytag 2012) (provided by Kennedy, personal communication), which was fitted using the method described in Yelverton et al. (2019) and Yelverton, Kennedy & Su (2020).
| |$\lambda$| (|$\mathrm{{\mu }m}$|) . | |$F_\mathrm{total}$| (Jy) . | |$F_\mathrm{disc}$| (Jy) . | Observatory . |
|---|---|---|---|
| 18 | |$5.338 \pm 0.114$| | |$0.348 \pm 0.117$| | AKARI1 |
| 23 | |$4.04 \pm 0.22$| | |$0.596 \pm 0.213$| | WISE2 |
| 25 | |$4.81 \pm 0.385$| | |$0.867 \pm 0.385$| | IRAS3 |
| 37.1 | |$4.10 \pm 0.28$| | |$2.94 \pm 0.28$| | SOFIA4 |
| 60 | |$9.02 \pm 1.08$| | |$8.433 \pm 1.08$| | IRAS3 |
| 70 | |$10.8 \pm 0.90$| | |$10.47 \pm 0.90$| | Herschel5 |
| 100 | |$11.2 \pm 1.46$| | |$11.03 \pm 1.46$| | IRAS3 |
| 160 | |$6.20 \pm 0.6$| | |$6.14 \pm 0.6$| | Herschel5 |
| 250 | |$2.70 \pm 0.3$| | |$2.68 \pm 0.3$| | Herschel5 |
| 350 | |$1.10 \pm 0.1$| | |$1.088 \pm 0.1$| | Herschel5 |
| 450 | |$0.595 \pm 0.035$| | |$0.588 \pm 0.035$| | JCMT/SCUBA6 |
| 450 | |$0.475 \pm 0.021$| | |$0.468 \pm 0.021$| | JCMT/SCUBA-27 |
| 500 | |$0.500 \pm 0.050$| | |$0.494 \pm 0.050$| | Herschel5 |
| 850 | |$0.097 \pm 0.005$| | |$0.095 \pm 0.005$| | JCMT/SCUBA6 |
| 850 | |$0.0912 \pm 0.0025$| | |$0.089 \pm 0.0025$| | JCMT/SCUBA-27 |
| 1300 | – | |$0.0247 \pm 0.0025$|a | ALMA8 |
| 1300 | – | |$0.0308 \pm 0.0041$|a,b | ALMA9 |
| |$\lambda$| (|$\mathrm{{\mu }m}$|) . | |$F_\mathrm{total}$| (Jy) . | |$F_\mathrm{disc}$| (Jy) . | Observatory . |
|---|---|---|---|
| 18 | |$5.338 \pm 0.114$| | |$0.348 \pm 0.117$| | AKARI1 |
| 23 | |$4.04 \pm 0.22$| | |$0.596 \pm 0.213$| | WISE2 |
| 25 | |$4.81 \pm 0.385$| | |$0.867 \pm 0.385$| | IRAS3 |
| 37.1 | |$4.10 \pm 0.28$| | |$2.94 \pm 0.28$| | SOFIA4 |
| 60 | |$9.02 \pm 1.08$| | |$8.433 \pm 1.08$| | IRAS3 |
| 70 | |$10.8 \pm 0.90$| | |$10.47 \pm 0.90$| | Herschel5 |
| 100 | |$11.2 \pm 1.46$| | |$11.03 \pm 1.46$| | IRAS3 |
| 160 | |$6.20 \pm 0.6$| | |$6.14 \pm 0.6$| | Herschel5 |
| 250 | |$2.70 \pm 0.3$| | |$2.68 \pm 0.3$| | Herschel5 |
| 350 | |$1.10 \pm 0.1$| | |$1.088 \pm 0.1$| | Herschel5 |
| 450 | |$0.595 \pm 0.035$| | |$0.588 \pm 0.035$| | JCMT/SCUBA6 |
| 450 | |$0.475 \pm 0.021$| | |$0.468 \pm 0.021$| | JCMT/SCUBA-27 |
| 500 | |$0.500 \pm 0.050$| | |$0.494 \pm 0.050$| | Herschel5 |
| 850 | |$0.097 \pm 0.005$| | |$0.095 \pm 0.005$| | JCMT/SCUBA6 |
| 850 | |$0.0912 \pm 0.0025$| | |$0.089 \pm 0.0025$| | JCMT/SCUBA-27 |
| 1300 | – | |$0.0247 \pm 0.0025$|a | ALMA8 |
| 1300 | – | |$0.0308 \pm 0.0041$|a,b | ALMA9 |
1Ishihara et al. (2010), 2Wright et al. (2010), 3Helou & Walker (1988), 4Adams et al. (2018), 5Acke et al. (2012), 6Holland et al. (2003), 7Holland et al. (2017), 8MacGregor et al. (2017), 9White et al. (2017).
Direct fluxes from just the outer planetesimal belt.
95 per cent confidence interval instead of 1σ error.
Photometric observations and excess emission from Fomalhaut. The excess fluxes (|$F_\mathrm{disc})$| were obtained by subtracting the star’s photosphere flux from total observed fluxes (except for ALMA-imaging-derived disc fluxes, denoted by a), which are obtained from the corresponding references. For the photosphere fluxes, we use a stellar SED modelled with PHOENIX (Allard, Homeier & Freytag 2012) (provided by Kennedy, personal communication), which was fitted using the method described in Yelverton et al. (2019) and Yelverton, Kennedy & Su (2020).
| |$\lambda$| (|$\mathrm{{\mu }m}$|) . | |$F_\mathrm{total}$| (Jy) . | |$F_\mathrm{disc}$| (Jy) . | Observatory . |
|---|---|---|---|
| 18 | |$5.338 \pm 0.114$| | |$0.348 \pm 0.117$| | AKARI1 |
| 23 | |$4.04 \pm 0.22$| | |$0.596 \pm 0.213$| | WISE2 |
| 25 | |$4.81 \pm 0.385$| | |$0.867 \pm 0.385$| | IRAS3 |
| 37.1 | |$4.10 \pm 0.28$| | |$2.94 \pm 0.28$| | SOFIA4 |
| 60 | |$9.02 \pm 1.08$| | |$8.433 \pm 1.08$| | IRAS3 |
| 70 | |$10.8 \pm 0.90$| | |$10.47 \pm 0.90$| | Herschel5 |
| 100 | |$11.2 \pm 1.46$| | |$11.03 \pm 1.46$| | IRAS3 |
| 160 | |$6.20 \pm 0.6$| | |$6.14 \pm 0.6$| | Herschel5 |
| 250 | |$2.70 \pm 0.3$| | |$2.68 \pm 0.3$| | Herschel5 |
| 350 | |$1.10 \pm 0.1$| | |$1.088 \pm 0.1$| | Herschel5 |
| 450 | |$0.595 \pm 0.035$| | |$0.588 \pm 0.035$| | JCMT/SCUBA6 |
| 450 | |$0.475 \pm 0.021$| | |$0.468 \pm 0.021$| | JCMT/SCUBA-27 |
| 500 | |$0.500 \pm 0.050$| | |$0.494 \pm 0.050$| | Herschel5 |
| 850 | |$0.097 \pm 0.005$| | |$0.095 \pm 0.005$| | JCMT/SCUBA6 |
| 850 | |$0.0912 \pm 0.0025$| | |$0.089 \pm 0.0025$| | JCMT/SCUBA-27 |
| 1300 | – | |$0.0247 \pm 0.0025$|a | ALMA8 |
| 1300 | – | |$0.0308 \pm 0.0041$|a,b | ALMA9 |
| |$\lambda$| (|$\mathrm{{\mu }m}$|) . | |$F_\mathrm{total}$| (Jy) . | |$F_\mathrm{disc}$| (Jy) . | Observatory . |
|---|---|---|---|
| 18 | |$5.338 \pm 0.114$| | |$0.348 \pm 0.117$| | AKARI1 |
| 23 | |$4.04 \pm 0.22$| | |$0.596 \pm 0.213$| | WISE2 |
| 25 | |$4.81 \pm 0.385$| | |$0.867 \pm 0.385$| | IRAS3 |
| 37.1 | |$4.10 \pm 0.28$| | |$2.94 \pm 0.28$| | SOFIA4 |
| 60 | |$9.02 \pm 1.08$| | |$8.433 \pm 1.08$| | IRAS3 |
| 70 | |$10.8 \pm 0.90$| | |$10.47 \pm 0.90$| | Herschel5 |
| 100 | |$11.2 \pm 1.46$| | |$11.03 \pm 1.46$| | IRAS3 |
| 160 | |$6.20 \pm 0.6$| | |$6.14 \pm 0.6$| | Herschel5 |
| 250 | |$2.70 \pm 0.3$| | |$2.68 \pm 0.3$| | Herschel5 |
| 350 | |$1.10 \pm 0.1$| | |$1.088 \pm 0.1$| | Herschel5 |
| 450 | |$0.595 \pm 0.035$| | |$0.588 \pm 0.035$| | JCMT/SCUBA6 |
| 450 | |$0.475 \pm 0.021$| | |$0.468 \pm 0.021$| | JCMT/SCUBA-27 |
| 500 | |$0.500 \pm 0.050$| | |$0.494 \pm 0.050$| | Herschel5 |
| 850 | |$0.097 \pm 0.005$| | |$0.095 \pm 0.005$| | JCMT/SCUBA6 |
| 850 | |$0.0912 \pm 0.0025$| | |$0.089 \pm 0.0025$| | JCMT/SCUBA-27 |
| 1300 | – | |$0.0247 \pm 0.0025$|a | ALMA8 |
| 1300 | – | |$0.0308 \pm 0.0041$|a,b | ALMA9 |
1Ishihara et al. (2010), 2Wright et al. (2010), 3Helou & Walker (1988), 4Adams et al. (2018), 5Acke et al. (2012), 6Holland et al. (2003), 7Holland et al. (2017), 8MacGregor et al. (2017), 9White et al. (2017).
Direct fluxes from just the outer planetesimal belt.
95 per cent confidence interval instead of 1σ error.
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