Physical conditions of molecular gas in the Circinus galaxy Multi-J CO and Ci 3PP0 observations

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Table 3

CO line intensities.

Transitions	Beam = 18′′			Beam = 45′′

	W_line^a	F_line		W_line	F_line	L′_line/L′_{CO3 − 2}
	Kkms^-1	Jy kms^-1	–	Kkms^-1	Jy kms^-1	–

¹²COJ = 1 → 0	–	–	–	180 ± 35^b	3.51 × 10³	1
¹²COJ = 2 → 1	–	–	–	144 ± 25^b	1.42 × 10⁴	0.83 ± 0.20
¹²COJ = 3 → 2	310 ± 20	0.97 × 10⁴	1	140 ± 20	2.49 × 10⁴	0.79 ± 0.16
¹²COJ = 4 → 3	240 ± 20	1.17 × 10⁴	0.77 ± 0.2	80 ± 15	2.51 × 10⁴	0.44 ± 0.09
¹²COJ = 6 → 5	140 ± 15	1.44 × 10⁴	0.45 ± 0.08	35 ± 5	2.48 × 10⁴	0.19 ± 0.03
¹²COJ = 7 → 6	55 ± 7	0.97 × 10⁴	0.18 ± 0.03	19 ± 5	1.73 × 10⁴	0.11 ± 0.03

¹³COJ = 1 → 0	–	–	–	13 ± 2.5	230	0.07 ± 0.02
¹³COJ = 2 → 1	–	–	–	12.5 ± 2.5	1300	0.07 ± 0.02
¹³COJ = 3 → 2	24 ± 5	740	0.07 ± 0.02	9.5 ± 3.0^c	1850	0.05 ± 0.02

Ci 1→0	100 ± 25	5 × 10³		45 ± 10	1.4 × 10⁴

Notes.

^(a)

The integrated line intensities are calculated from in the velocity range from 200 kms^-1 to 700kms^-1.

^(b)

We take aperture efficiencies of η_mb = 0.7 and 0.6 for ¹²COJ = 1 → 0 and ¹²COJ = 2 → 1 for SEST.

^(c)

We convolve the ¹³COJ = 3 → 2 emission to a resolution of 45′′, assuming that the distribution of ¹³COJ = 3 → 2 is the same as that of ¹²COJ = 3 → 2.

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