Warm debris disks candidates in transiting planets systems

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Table 2

Parameters of the selected objects.

Name

SpT

a_planet[AU]

d_star[pc]

χ₁₂

χ₂₂

T_dust[K]

R_dust[AU]

f = L_dust/L_∗[10^-5]

Quality flag (1) – Single isolated clean PSF

KIC 2853093/KOI 1099

0.573

1300

7.1 ± 1.0

6.1

58.7 ± 28.2

2.2

200

1.0

6.5

KIC 4918309/KOI 1582

0.626

1020

2.7 ± 0.7

2.2

<46.4

...

>150

<1.9

<5.4

KIC 6422367/KOI 559

0.052

660

2.5 ± 0.4

4.0

<40.2

...

>150

<2.7

<4.7

KIC 6924203/KOI 1370

0.071

910

2.1 ± 0.6

2.2

<39.7

...

>150

<2.4

<3.7

KIC 9008220/KOI 466

0.087

1100

2.1 ± 0.5

2.2

<31.8

...

>150

<2.1

<2.9

KIC 9703198/KOI 469

0.095

1200

3.2 ± 0.5

4.2

<30.7

...

>175

<2.6

<2.7

KIC 10526549/KOI 746

0.080

570

1.7 ± 0.4

2.1

<30.1

...

>125

<2.6

<5.2

Quality flag (2) – Possible source confusion or weak detection at W3 or W4

WASP-46

0.024

520

1.5 ± 0.3

3.3

<6.7

...

>175

<2.2

<0.4

KIC 3547091/KOI 1177

0.043

1080

2.9 ± 0.9

2.2

<55.5

...

>150

<2.0

<5.6

KIC 3732821/KOI 1207

0.111

720

2.4 ± 0.6

2.6

<56.5

...

>125

<3.6

<10.0

KIC 4545187/KOI 223

0.041, 0.226

600

1.9 ± 0.3

2.6

<20.9

...

>150

<2.0

<2.8

KIC 6665695/KOI 561

0.058

430

1.1 ± 0.2

0.8

12.8 ± 5.7

2.2

100

4.8

1.9

KIC 8414716/KOI 910

0.057

850

2.5 ± 0.7

2.2

<79.8

...

>125

<2.0

<14.8

Notes. The candidates are separated in two groups based on the visual inspection process. SpT and a_planet from Borucki et al. (2011); Anderson et al. (2011). For WASP-46, we use T_eff = 5750 K and A_V = 0. Stellar distances are calculated deriving the absolute J magnitude from the T_eff or the J − K color.T_dust is the temperature of a blackbody fitted to the W3 and W4 bands. The disk radius R_dust is derived assuming large dust grains. f = L_dust/L_∗ is derived from the fitted blackbody. KIC 4545187 is a multiple planet system.

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