A peculiar class of debris disks from Herschel/DUNES - A steep fall off in the far infrared

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Table 2

Observational results obtained in this work^a.

Source	HIP 103389		HIP 107350		HIP 114948

	Reduction 1	Reduction 2	Reduction 1	Reduction 2	Reduction 1	Reduction 2

F_{PACS 70} [mJy]	47.4 ± 2.7	44.0 ± 2.3	...	...	...	...
F_{MIPS 70} [mJy]	46.6 ± 3.8		28.4 ± 2.5		68.7 ± 3.0
F_{PACS 100} [mJy]	23.7 ± 1.4	26.3 ± 1.7	11.0 ± 0.9	15.1 ± 1.3	42.5 ± 2.2	40.8 ± 1.6
F_{PACS 160} [mJy]	5.0 ± 1.3	7.7 ± 2.5	4.4 ± 1.5	4.4 ± 2.3	12.7 ± 1.9	13.3 ± 2.2

F_{⋆,70 μm}^b [mJy]	13.8		13.4		15.0
F_{⋆,100 μm}^b [mJy]	6.8		6.6		7.3
F_{⋆,160 μm}^b [mJy]	2.7		2.6		2.9

Δ_100,70	1.94 ± 0.32	1.44 ± 0.33	2.66 ± 0.45	1.77 ± 0.49	1.35 ± 0.26	1.46 ± 0.23
Δ_160,100	3.31 ± 0.69	2.61 ± 0.82	1.95 ± 0.88	2.62 ± 1.30	2.57 ± 0.44	2.38 ± 0.43
Δ_160,70	2.72 ± 0.39	2.11 ± 0.46	2.25 ± 0.53	2.26 ± 0.74	2.04 ± 0.22	1.99 ± 0.25

FWHM_{PACS 100}^c

RA_{PACS 100}
Dec_{PACS 100}
RA_optical
Dec_optical

Notes. Uncertainties of the flux measurements are total uncertainties including sky noise and calibration uncertainties. Δ_ν₁,ν₂ is the spectral index measured from ν₁ and ν₂ (Sect 3), identified with the corresponding PACS bands.

^(a)

The Spitzer/MIPS 70 μm photometry is also listed, since these data complement the Herschel observations and are important to illustrate the unusual behavior of the SEDs. These data are published by Beichman et al. (2006, HIP 103389 and HIP 114948) and Bryden et al. (2006, HIP 107350) and have been re-reduced in the context of DUNES (Eiroa et al., in prep.).

^(b)

Predicted stellar photosphere using a PHOENIX/GAIA synthetic stellar model (Eiroa et al., in prep.).

^(c)

FWHM as measured from the PACS images at 100 μm using a 2D Gaussian fit.

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