Subarcsecond imaging of the water emission in Arp 220

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Table 1

Water line properties.

Line	ν _rest	E _upper	Telescope	Beam	^∫S dv^a, ^b		Date of	Reference^c
	[GHz]	[K]			[Jy km s^-1]		observation

H₂O 6₁₆ − 5₂₃	22.23508	609	VLA	0.79′′ × 0.71′′	0.34	0.17	March 2011–June 2012	1
H₂O 3₁₃ − 2₂₀	183.31009	205	IRAM 30 m	14′′	55.7^d		January 2005	2
			IRAM 30 m	14′′	56.9		April, May 2014	3
			APEX	35′′	50 ± 6		July, September 2015	4
			ALMA	35′′	56.0		July 2016	3
			ALMA	0.79′′ × 0.71′′	13.7	47.8	July 2016	3
H₂O 5₁₅ − 4₂₂	325.15292	470	IRAM 30 m	8′′	39.8		December 2012	3
			IRAM 30 m	8′′	42.3		April, May 2014	3
			ALMA	8′′	45.4		June, July 2014	3
			ALMA	0.79′′ × 0.71′′	9.1	25.3	June, July 2014	3

Notes.

^(a)

When two values are given, the left column denotes the contamination-corrected integrated intensities measured in Arp 220 East, the right column is for Arp 220 West. A single value given represents the uncorrected integrated intensities for a region that encompasses both nuclei.

^(b)

The integrated intensities given for the interferometric observations are the contamination-corrected values.

^(c)

(1) Zschaechner et al. (2016), (2) Cernicharo et al. (2006b), (3) this work, (4) Galametz et al. (2016).

^(d)

Derived from the luminosity given in their Table 1.

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