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P1640 J and H band

(0.98 [0.42], 0.99+)(0.10 [0.43], 0.99+)(0.42 [0.38], 0.99+)(0.58 [0.38], 0.99+)(0.14 [0.36], 0.99+)(0.74 [0.35], 0.99+)(0.64 [0.90],0.77)(0.35 [0.87],0.77)(0.01 [0.83], 0.59)(0.64 [0.80], 0.92)(0.19 [0.96], 0.11)(0.27 [0.92], 0.28)

SEICA (Second-generation Exoplanet Imager with Coronagraphic Adaptive Optics)
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. The
different 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 .

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TABLE 6
Atmospheric Models

FigurePanel

PlanetTef f (K)log(g)

Cloud TypeChemistry

Reference8

top-leftmiddle-leftbottom-left
top-right
middle-rightbottom-right
top-leftbottom-left
top-rightbottom-right

HR 8799 b””
HR 8799 d””
HR 8799 bHR 8799 c
HR 8799 dHR 8799 e900
850
850
1000975
1000
900
1000
1000
1000

4.0
4.0
4.3
4.0
4.0
4.0
4.0
4.0
4.0
4.0A60
AE30
AE60
A60
AE60
AE60
0.85×A60, 0.15×E60
0.7×A60, 0.3×E60
0.9×A60, 0.1×AE60
0.75×A60, 0.25×E60

equilibrium
equilibrium
100×CO, 0.01×CH4
equilibrium
equilibrium
100×CO, 0.01×CH4
equilibrium
equilibrium
equilibrium
equilibrium

1,23
4
1,23
45
555196'1’(60’’)

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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.

HR8799 (Currie+2014)
c 10MJ
1’’.1

b 7MJ
1’’.7+
#
10-5

e 9MJ0’’.4

QcZP`[ uZadP%8u]TYu
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@HLFKJ
CQdY`TY3C0&EJ
d 10MJ0’’.7uFig. 1.— Keck/NIRC2 L′ images of HR 8799 from 2012 data (left) and archival 2010 data (right) reduced using A-LOCI. HR 8799 bcdeHGA)

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