APEX and NOEMA observations of H2S in nearby luminous galaxies and the ULIRG Mrk 231 - A possible relation between dense gas properties and molecular outflows

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Table B.1.

APEX results.

Source	Molecule	Line peak (T_A, peak)^b	I	Δv	rms
		(mK)	(K kms⁻¹)	(kms⁻¹)	(mK)
NGC 3256	CH₃OH	> 2.1 ± 0.2	> 0.06 ± 0.03	238 ± 43	0.20
	H₂S	1.2 ± 0.7	0.28 ± 0.03	216 ± 61	0.20
	HCN	16.9 ± 0.4	2.26 ± 0.06	182 ± 7	0.38
	HCO⁺	21.6 ± 0.4	4.17 ± 0.06	186 ± 4	0.38
	SO	1.2 ± 0.4	0.13 ± 0.03	85 ± 4	0.38
	HNC	4.4 ± 2.0	> 1.02 ± 0.04	284 ± 145	0.38

NGC 1068	CH₃OH	> 0.7 ± 0.2	> 0.18 ± 0.04	303 ± 185	0.35
	H₂S	1.4 ± 0.3	0.40 ± 0.06	267 ± 60	0.35
	HCN	28.4 ± 0.6	7.41 ± 0.10	253 ± 6	0.60
	HCO⁺	20.7 ± 0.6	5.32 ± 0.11	250 ± 8	0.60
	SO	1.0 ± 0.5	0.14 ± 0.04	133 ± 73	0.60
	HNC	7.6 ± 0.9	> 0.73 ± 0.06	104 ± 18	0.60

IC 860	CH₃CN	1.4 ± 0.5	0.39 ± 0.09	192 ± 87	0.52
	HCN	2.2 ± 0.3	0.82 ± 0.15	357 ± 63	0.80

NGC 4418	CH₃CN	1.3 ± 0.3	0.27 ± 0.11	216 ± 56	0.41
	H₂S	1.6 ± 0.4	0.25 ± 0.11	126 ± 39	0.41
	H₂CS	1.7 ± 0.5	> 0.11 ± 0.03	—	0.41
	HCN	6.4 ± 0.4	1.45 ± 0.10	200 ± 16	0.67
	HCO⁺	5.3 ± 0.5	0.84 ± 0.08	151 ± 15	0.67
	SO	0.9 ± 0.5	0.18 ± 0.07	166 ± 15	0.67
	HNC	3.3 ± 0.5	> 0.70 ± 0.07	251 ± 103	0.67

Circinus	CH₃OH	> 2.0 ± 1.0	> 0.16 ± 0.04	63 ± 37	0.37
	H₂S	3.0 ± 0.4	0.78 ± 0.06	241 ± 33	0.37
	HCN	24.0 ± 1.0	6.0 ± 0.1	233 ± 11	0.81
	HCO⁺	29.5 ± 1.0	7.0 ± 0.1	238 ± 9	0.81
	SO	4.2 ± 1.0	0.16 ± 0.08	38 ± 9	0.81
	HNC	—	> 0.93 ± 0.08	—	0.81

NGC 1097	CH₃OH	> 0.8 ± 0.2	> 0.04 ± 0.04	18 ± 273	0.30
	H₂S	0.5 ± 0.3	0.11 ± 0.04	157 ± 89	0.30
	HCN	5.9 ± 0.3	2.38 ± 0.10	409 ± 26	0.51
	HCO⁺	4.9 ± 0.3	1.97 ± 0.09	405 ± 29	0.51
	HNC	2.4 ± 1.0	> 0.33 ± 0.05	126 ± 63	0.51

NGC 4945	CH₃OH	7.2 ± 1.1	> 1.92 ± 0.08	238 ± 43	0.46
	CH₃CN	2.8 ± 0.3	0.96 ± 0.08	345 ± 39	0.46
	H₂S	4.8 ± 0.5	1.49 ± 0.07	295 ± 35	0.46
	H₂CS	1.4 ± 0.5	0.46 ± 0.07	275 ± 38	0.46
	HCN	95.5 ± 7.1	31.3 ± 0.2	325 ± 28	1.0
	HCO⁺	85.6 ± 5.4	30.1 ± 0.2	337 ± 25	1.0
	SO	—	0.24 ± 0.16	—	1.0
	HOC⁺	5.5 ± 1.0	1.75 ± 0.16	322 ± 69	1.0
	HNC	38.3 ± 2.8	13.3 ± 0.2	339 ± 28	1.0

NGC 253	CH₃OH	9.5 ± 1.4	> 1.93 ± 0.07	183 ± 45	0.48
	CH₃CN	4.7 ± 1.0	1.05 ± 0.08	208 ± 35	0.48
	H₂S	10.4 ± 1.1	3.09 ± 0.06	187 ± 24	0.48
	H₂CS	0.7 ± 1.1	0.12 ± 0.05	126 ± 23	0.48
	HCN	161.4 ± 3.7	33.5 ± 0.14	203 ± 5	0.87
	HCO⁺	165.3 ± 2.8	33.7 ± 0.14	197 ± 4	0.87
	SO	6.2 ± 0.6	1.00 ± 0.10	162 ± 20	0.87
	HOC⁺	6.1 ± 0.9	1.03 ± 0.11	157 ± 27	0.87
	HNC	> 42.9 ± 0.8	> 3.91 ± 0.10	135 ± 5	0.87

NGC 1377	HCN	1.3 ± 0.4	0.76 ± 0.1	135 ± 45	0.60

M 83	CH₃OH	0.9 ± 0.3	> 0.29 ± 0.03	377 ± 242	0.51
	H₂S	2.6 ± 0.4	0.31 ± 0.05	107 ± 19	0.51
	HCN	34.0 ± 0.9	3.95 ± 0.13	106 ± 3	0.96
	HCO⁺	36.0 ± 0.9	4.21 ± 0.13	108 ± 3	0.96
	HOC⁺	1.1 ± 0.9	0.39 ± 0.14	273 ± 3	0.96

NGC 4826	H₂S	0.9 ± 0.2	0.27 ± 0.09	288 ± 58	0.27
	HCN	5.5 ± 0.6	1.54 ± 0.11	273 ± 31	0.66
	HCO⁺	4.9 ± 0.4	1.38 ± 0.13	270 ± 22	0.66

NGC 5128	-	-	-	-	-

Notes. Integrated line intensities are calculated using the formula I_line = ∑_iI_idv, where I is the intensity at each velocity and dv is the velocity resolution.The errors are calculated using , where σ is the rms, v_res is the velocity resolution, N_L is the number of channels that contribute to the line, and N_B is the number of channels that are outside the line. The rms noise levels are given in Table 1. NGC 5128 has strong continuum emission, and its noise levels could not be measured.

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