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

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Table 6

CO detections toward the central position of Circinus in the literature

Transition	Telescope	Resolution	W_mb	Flux	η_mb
		(′′)	Kkms^-1	Jykms^-1

¹²COJ = 1 → 0^a	SEST	43′′	128 ± 1.2	2650	0.77
¹²COJ = 1 → 0^b	SEST	41′′	185 ± 15	3350	0.67
¹²COJ = 1 → 0^c	MOPRA	45′′	145	–	–
¹²COJ = 1 → 0^d	SEST	45′′	156	3050	0.72
¹²COJ = 1 → 0^e	SEST	45′′	180 ± 10	3500	–
¹²COJ = 1 → 0^f	SEST	45′′	150 ± 30	2850	0.7
Adopted	–	45′′	180 ± 10	3500	–

¹³COJ = 1 → 0^a	SEST	43′′	11.2 ± 0.2	230	0.77
¹³COJ = 1 → 0^b	SEST	43′′	11 ± 1.5	210	0.68
¹³COJ = 1 → 0^d	SEST	45′′	13	250	0.72
¹³COJ = 1 → 0^e	SEST	45′′	12 ± 1	230	–
Adopted	SEST	45′′	11.2	230	–

¹²COJ = 2 → 1^d	SEST	45′′	125	12300	0.6
¹²COJ = 2 → 1^e	SEST	22′′	220 ± 20	5400	0.6
¹²COJ = 2 → 1^g	SEST	38′′	177	13000	0.6
Adopted	SEST	45′′	144	14200ⁱ	–

¹³COJ = 2 → 1^d	SEST	45′′	12.5	1280	0.60
¹³COJ = 2 → 1^e	SEST	22′′	24 ± 4	590	0.6
¹³COJ = 2 → 1^g	SEST	38′′	19	1390	0.6
Adopted	SEST	45′′	12.5	1300	–

¹²COJ = 3 → 2^d	SEST	45′′	70	20400	0.33
¹²COJ = 3 → 2^e	SEST	15′′	230 ± 20	7400	0.33
¹²COJ = 3 → 2^g	APEX	45′′	140 ± 20	25000	0.73
Adopted	APEX	45′′	140 ± 20	25000	–

¹²COJ = 4 → 3^h	NANTEN-2	38′′	58	12600	0.5
¹²COJ = 3 → 2^g	APEX	45′′	80 ± 15	25000	0.6
Adopted	APEX	45′′	80 ± 15	25000	–

Notes. The line fluxes are derived from by adopting the telescope efficiencies of the SEST with 27 Jy/K, 41 Jy/K, and 98 Jy/K at 115 GHz, 230 GHz, and 346 GHz, respectively. For the NANTEN-2 4 m telescope, a Jy/K factor for T_mb of 216 has been assumed.

^(a)

Aalto et al. (1991);

^(b)

Israel et al. (1992);

^(c)

Elmouttie et al. (1997);

^(d)

Curran et al. (1998);

^(e)

Curran et al. (2001a);

^(f)

Curran et al. (2001b);

^(g)

this work;

^(h)

Hitschfeld et al. (2007);

⁽ⁱ⁾

We adopt the CO J = 2→1 to 1→0 line ratio in the 45′′ region, and the integrated intensity of ¹²COJ = 1 → 0 in Curran et al. (2008).

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