The role of molecular gas in galaxy transition in compact groups

U. Lisenfeld; K. Alatalo; C. Zucker; P. N. Appleton; S. Gallagher; P. Guillard; K. Johnson

doi:10.1051/0004-6361/201730898

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Volume 607 (November 2017)

A&A, 607 (2017) A110

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Table 1

Integrated CO intensities.

Galaxy	rms^a	I _CO(1−0)	△ V_CO(1−0) ^b
	[mK]	[K km s^-1]	[km s^-1]

HCG 01b	1.58	1.41 ± 0.15	410
HCG 05a	1.51	5.73 ± 0.12	275
HCG 19c	3.24	<0.77	300^c
HCG 28a	1.97	2.16 ± 0.22	570
HCG 32d	1.27	0.83 ± 0.14	590
HCG 39a	1.16	0.97 ± 0.15	800
HCG 45a	1.08	1.98 ± 0.17	1120
HCG 45b	1.08	0.62 ± 0.14*	800
HCG 46b	1.35	0.91 ± 0.12	370
HCG 47c	1.89	2.47 ± 0.18	434
HCG 51b	2.90	3.58 ± 0.27	415
HCG 52a	1.32	0.79 ± 0.14	536
HCG 54a^d	3.37	<0.80	300
HCG 57b	1.87	1.37 ± 0.22	634
HCG 57e	1.85	1.22 ± 0.19	489
HCG 60b	0.93	1.09 ± 0.12	715
HCG 64a	2.44	1.71 ± 0.23	423
HCG 70a	2.12	<0.51	300^c
HCG 70b	2.45	2.69 ± 0.27	564
HCG 70c	1.55	1.04 ± 0.14	375
HCG 71a	2.36	6.71 ± 0.24	470
HCG 75c	1.28	0.54 ± 0.12*	389
NGC 0070	3.53	<0.85	300^c
NGC 4410NED01	3.09	5.11 ± 0.35	604
NGC 4614	1.94	1.56 ± 0.15	295
NGC 6961	2.50	<0.60	300
MCG + 02-36-018	1.75	0.73 ± 0.11	200

Notes.

^(a)

Root-mean-square noise level at a velocity resolution of ~21 km s^-1.

^(b)

Zero-level line width. The uncertainty is roughly given by the velocity resolution.

^(c)

Assumed linewidth for the non-detections.

^(d)

HCG 54a was excluded from the subsequent statistical analysis because of its low recession velocity.

^(*)

Tentative detection (S/N between 4 and 5).

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