The role of molecular gas in the nuclear regions of IRAS 00183-7111 - ALMA and X-ray investigations of an ultraluminous infrared galaxy

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Table 2.

Properties of ALMA line detections extracted from image analysis.

	ν_rest^a (GHz)	ν_obs^b (GHz)	Peak flux^c (mJy beam⁻¹)	rms^d (mJy beam⁻¹)	S_line^e (Jy km s⁻¹)	FWHM^f (km s⁻¹)	Luminosity^g (K km s⁻¹ pc²)
CO	115.271	86.73	5.5 ± 0.6 (32σ)	0.17	2.56 ± 0.26	400 ± 27	1.42 × 10¹⁰
HCN	354.505	266.72	5.9 ± 1.1 (6σ)	1.0	0.40 ± 0.08	~66	~10⁹

Notes.

^(a)

Rest-frame frequency of molecular lines.

^(b)

Observed frequency of the line peak.

^(c)

Observed line peak flux with the detection significance in parentheses.

^(d)

1σ rms noise level computed in line-free regions.

^(e)

Integrated flux density of the line derived from a 2D Gaussian fit of the emitting region.

^(f)

Measured line FWHM.

^(g)

Molecular line luminosity derived from the measured flux density.

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