Observations of Herbig Ae/Be stars with Herschel/PACS - The atomic and molecular contents of their protoplanetary discs

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Table 4

Atomic line strengths in units of 10^-18 W/m² with 1σ continuum rms between brackets in the case of a detection or 3σ upper limits.


Star	[O i]	[O i]	[C ii]
λ (μm)	63.18	145.53	157.75


AB Aur	851.2 (21.5)	44.6 (14.7)	51.0 (8.3)
HD 31648	94.9 (3.5)	<7.8	<9.7
HD 35187	32.8 (4.8)	<4.6	<5.9
HD 36112	37.3 (2.4)	<6.3	<9.6
CQ Tau	47.9 (4.0)	<3.8	<11.3
HD 97048	1592.5 (4.3)	65.6 (2.6)	106.8 (6.3)
HD 100453	61.6 (7.5)	<6.1	<15.4
HD 100546	6043.4 (13.4)	194.7 (9.9)	203.8 (8.6)
HD 104237	79.1 (3.5)	<5.9	<7.6
HD 135344B	47.9 (5.8)	<4.6	<6.4
HD 139614	44.5 (6.1)	<4.7	<8.3
HD 141569A	245.3 (4.8)	24.9 (1.4)	11.4 (2.1)
HD 142527	52.3 (3.8)	<11.6	<28.7
HD 142666	18.9 (3.1)	<4.7	<9.0
HD 144668	140.2 (4.3)	<5.8	<5.4
HD 150193	24.6 (2.8)	<6.6	<5.3
KK Oph	172.8 (5.0)	6.2 (1.3)	9.2 (1.2)
51 Oph	53.3 (2.5)	<5.1	<6.8
HD 163296	208.4 (4.2)	<4.0	ABS^a
HD 169142	91.5 (4.4)	<3.6	<8.0

49 Cet	< 10.0	< 6.3	< 9.1
HD 32297	< 7.4	< 4.2	< 7.1
HR 1998	< 7.0	< 5.1	< 6.6
HR 4796A	< 6.3	< 3.8	< 5.4
HD 158352	< 8.2	n.a.	< 3.8

Notes. For HD 158352, not all settings were observed, therefore we write “n.a.” (not available) when the spectrum is lacking.

^(a)

An absorption feature is observed in the spectrum, that is caused by the subtraction of stronger emission in the chop-off position.

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