Table 2:

The observations.

	Observation				Predicted	Resultsa
Star			integration		stellar	Flux,	Total	stats.	Background limit
name	Filter	,  m	time, s	Instrument	flux, mJy*	mJy	err., mJy	err., mJy	mJyb	Spc. Typec
HD 3003	N9.8	9.56	1800	TIMMI2	426	481	87	17	46	M3.5V
	N12.9	12.21	3600	TIMMI2	262	436	64	10	27
	Q2	18.75	3100	TIMMI2	112	206	140	44	148
	Si-5	11.66	3400	TReCS	288	375	34	4	10
	Q2	18.72	2400	VISIR	113	244	27	9	21
HD 23281	N12.9	12.21	3200	TIMMI2	243	339	57	10	27	M5V
	SiC	11.85	3600	VISIR	258	252	13	2	4
	Q2	18.72	3800	VISIR	104	129	9	6	13
HD 23432	N7.9	7.77	1800	TIMMI2	299	452	192	192	351	A6V
	N11.9	11.59	1800	TIMMI2	136	141	62	14	44
HD 31295	N1	8.60	1800	TIMMI2	648	851	77	13	33	M3V
HD 38206	N9.8	9.56	1800	TIMMI2	204	196	48	16	44	G3.5V
Gem	N1	8.60	1800	TIMMI2	2244	1997	167	22	56	M5.5V
Chop PA	SiC	11.85	540	VISIR	1195	701	9	4	7
268	Q2	18.72	1880	VISIR	484	590	71	6	14
Binary	N1	8.60	1800	TIMMI2	101	68	8		-
Chop PA	SiC	11.85	540	VISIR	54	46	4		-
268	Q2	18.72	1800	VISIR	22	31	17		-
HD 71155	N2	10.68	3060	TIMMI2	850	1278	215	36	98	K4.5V
	Si-5	11.60	1410	MICHELLE	722	1050	115	12	32
	Qa	18.50	2100	MICHELLE	286	398	99	13	38
	Q2	18.72	3600	VISIR	280	380	36	7	16
HD 75416	N11.9	11.59	1800	TIMMI2	144	204	88	15	48	F0V
HD 80950	N11.9	11.59	3600	TIMMI2	129	175	16	10	25	K4.5V
	SiC	11.85	1800	VISIR	124	120	23	3	7
	Q2	18.72	3760	VISIR	50	119	11	9	20
HD 141795	N12.9	12.21	1200	TIMMI2	1115	1138	119	19	49	M4.5V
	Qa	18.50	1900	MICHELLE	491	511	39	3	8
Tel	N12.9	12.21	2500	TIMMI2	254	351	23	10	25	K2V
	Q2	18.75	1800	TIMMI2	109	391	182	43	136

Notes. ^(*) The expected photospheric emission is determined by a Kurucz model profile appropriate to the spectral type of the star and scaled to the K band 2MASS magnitude as outlined in Sect. 2 unless otherwise stated in the individual source description. Errors are 1. M band TIMMI2 observations were largely non-photometric and primarily used to improve pointing accuracy and thus are not listed in this Table. ^(a) Errors are total errors (inclusive of calibration uncertainty and image noise); ^b limits are 3 upper limit to undetected object including calibration errors, or scaled to IRAS fluxes when conditions were non-photospheric. These limits are valid to within 28 of the detected source for TIMMI2 observations, 12 6 for MICHELLE, 8 1 for TReCS, and 11 4 of the source for VISIR observations; ^c the hottest spectral type of main-sequence star equidistant with the target that would have remained undetected within our field of view. See Sect. 3.2 for details of this limit.