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TABLE 4Nominal HR 8799 bcde Photometry Considered Here

Filter z J H Ks [3.3] L′ [4.05] M ′

λ (µm) 1.03 1.25 1.633 2.146 3.3 3.776 4.051 4.68

Planetb 18.24 ± 0.29 16.52 ± 0.14 15.08 ± 0.13 14.05 ± 0.08 13.22 ± 0.11 12.60 ± 0.10 11.84 ± 0.18 13.07 ± 0.30c > 16.48 14.65 ± 0.17 14.18 ± 0.17 13.13 ± 0.08 12.22 ± 0.11 11.74 ± 0.08 10.99 ± 0.08 12.05 ± 0.14d >15.03 15.26 ± 0.43 14.23 ± 0.22 13.11 ± 0.12 12.02 ± 0.11 11.58 ± 0.09 10.89 ± 0.14 11.67 ± 0.35e – > 13.2 13.88 ± 0.22 12.89 ± 0.26 12.02 ± 0.21 11.57 ± 0.12 10.74 ± 0.20 > 10.09

Note. — The (nominal) HR 8799 bcde photometry considered here. The z band photometry come from Currie et al. (2011a), J bandphotometry for HR 8799 bcd come from Marois et al. (2008a) while upper limits come from Oppenheimer et al. (2013), the H band and[3.3] photometry come from Skemer et al. (2012), the Ks band photometry come from Marois et al. (2008a) for HR 8799 bcd and fromCurrie et al. (2011a) for HR 8799 e, the L′ and [4.05] photometry come from this work and the M ′ photometry come from Galicher et al.(2011).

TABLE 5Statistical Tests Comparing HR 8799 bcde photometry

Photometry b and c b and d b and e c and d c and e d and e

Nominal (0.98 [0.42], 0.99+) (0.32 [0.39], 0.99+ ) (0.14 [0.36], 0.99+) (0.59 [0.92],0.66) (0.02 [0.82], 0.66) (0.27 [0.91], 0.31)Keck 2005 H band (0.98 [0.42], 0.99+) (0.42 [0.38], 0.99+) (0.14 [0.36], 0.99+) (0.64 [0.90],0.77) (0.01 [0.83], 0.59) (0.19 [0.96], 0.11)P1640 J and H band (0.10 [0.43], 0.99+) (0.58 [0.38], 0.99+) (0.74 [0.35], 0.99+) (0.35 [0.87],0.77) (0.64 [0.80], 0.92) (0.27 [0.92], 0.28)

Note. — Confidence limits at which two pairs of planets’ (scaled) photometry differ as determined from the goodness-of-fit statistic given the number of degrees of freedom – Ndata

- 2 for scaled photometry, Ndata -1 for non-scaled photometry – and the χ2 value. For HR 8799 bcd comparisons, Ndata = 7 while comparisons with HR 8799 e have Ndata = 5. Thedifferent rows indicate the nominal case, using photometry listed in Table 4, the Currie et al. (2012b) H-band photometry, and the Oppenheimer et al. (2013) J and H photometry.The two entries (enclosed by parentheses) list the correlation from scaling the planets’ fluxes with respect to one another (left entry) and the nominal correlation (no scaling of thespectra) (right entry). A value closer to one means that the photometry significantly differ (e.g. 0.95 = the planets’ photometry differ at the 2-σ/95% confidence limit). The “[]” values

enclose the scaling factor applied to the second planet in each listed pair that minimizes χ2.

TABLE 6Atmospheric Models

Figure Panel Planet Teff (K) log(g) Cloud Type Chemistry Reference

8 top-left HR 8799 b 900 4.0 A60 equilibrium 1,2middle-left ” 850 4.0 AE30 equilibrium 3bottom-left ” 850 4.3 AE60 100×CO, 0.01×CH4 4top-right HR 8799 d 1000 4.0 A60 equilibrium 1,2

middle-right ” 975 4.0 AE60 equilibrium 3bottom-right ” 1000 4.0 AE60 100×CO, 0.01×CH4 4

9 top-left HR 8799 b 900 4.0 0.85×A60, 0.15×E60 equilibrium 5bottom-left HR 8799 c 1000 4.0 0.7×A60, 0.3×E60 equilibrium 5top-right HR 8799 d 1000 4.0 0.9×A60, 0.1×AE60 equilibrium 5

bottom-right HR 8799 e 1000 4.0 0.75×A60, 0.25×E60 equilibrium 5

Note. — References: 1) Burrows et al. (2006), 2) Currie et al. (2011a), 3) Madhusudhan et al. (2011), 4) Skemer et al.(2012), 5) this work.

Fig. 1.— Keck/NIRC2 L′ images of HR 8799 from 2012 data (left) and archival 2010 data (right) reduced using A-LOCI. HR 8799 bcdeare all easily identifiable.

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