Herschel-PACS photometry of faint stars for sensitivity performance assessment and establishment of faint FIR primary photometric standards

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Table 9

Evaluation of correspondence of PACS photometry with models or flux predictions (C = Cohen, H = Hammersley, G = Gordon).

HD	Other name	Model	Mode	Correspondence with model	Reason for deviation	Sect.
62509	β Gem	C	s, c	no, excess of ≈+8%	dust disk in planetary system	5.2.1
12929	α Ari	C	s	yes, better than ±3%
32887	ε Lep	C	s, c	yes, better than ±1%
198542	ω Cap	C	s	yes, better than ±1%
148387	η Dra	H	s, c	no, excess of ≈+8%	dust in binary system	5.2.1
180711	δ Dra	C	s, c	partially, ≈+3% offset for λ ≤ 100 μm
				+7% @160 μm	cirrus confusion	5.2.2
139669	θ Umi	C	s, c	partially, ≈+3% offset for λ ≤ 100 μm
				+16% @160 μm	cirrus confusion	5.2.2
41047	HR 2131	C	s, c	yes, better than ±3%
170693	42 Dra	G	s	yes, ≈–4% offset
138265	HR 5755	G	s, c	partially, ≈–2% offset for λ ≤ 100 μm
				+40% @160 μm	cirrus confusion	5.2.2
159330	HR 6540	G	s, c	partially, better than ±1% for λ ≤ 100 μm
				no flux determination @160 μm	source confusion	3.7
152222	SAO 17226	G	s, c	yes, better than ±5%
39608	SAO 249364	G	s	yes, better than 1% @70 μm
				+19% @100 μm, +105% @160 μm	background confusion	5.2.2
181597	HR 7341	H	s, c	yes, better than 4% @70 μm
				no flux determination @160 μm	below detection limit	3.6
15008	δ Hyi	G	s, c	yes, better than 4% @70 μm
				no flux determination @160 μm	below detection limit	3.6
156729	e Her	H	c	no	below detection limit
168009	HR 6847	H	c	no	below detection limit

Notes. Column “mode” specifies the PACS observing mode (s = scan map, c = chop/nod). Column “Reason for deviation” gives a short summary of the discussion in the reference sections.

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