H2O emission in high-z ultra-luminous infrared galaxies

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Volume 551 (March 2013)

A&A, 551 (2013) A115

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Table 4

Observed parameters of the H₂O emission lines and continuum emission.

Source	Line^a	ν_obs^b	S_ν pk^c	S_ν^c	S_νH₂O pk^d	ΔV_H₂O	I_H₂O pk^d	I_H₂O^d	L_H₂O^e
		[GHz]	[mJy/beam]	[mJy]	[mJy/beam]	[km s^-1]	[Jy km s^-1/beam]	[Jy km s^-1]	[10⁷ L_⊙]

SDP.81	2	244.5000	12.5	27.0 ± 1.2	10.7± 1.9	140 ± 50	1.6	1.8 ± 0.5	32 ± 9
NA.v1.144	1	234.8343	9.4	16.4 ± 0.7	22.8 ± 1.7	200 ± 50	4.9	7.5 ± 0.9	57 ± 7
SDP.9	1	292.1425	17.4	21.7 ± 0.9	20.3/37.8 ± 2.9^f	410 ± 50	11.3	14.4 ± 1.1	60 ± 5
NB.v1.78	2	240.2896	15.4	36.9 ± 0.4	5.0 ± 0.8	510 ± 90	2.7	6.7 ± 1.3	122 ± 24
G12.v2.30	2	231.9458	4.9	21.0 ± 0.8	4.5/4.5 ± 0.7^f	690 ± 80	2.7	6.5 ± 1.2	128 ± 24
G15.v2.779	1	143.3837	5.9	7.3 ± 0.2	3.2/6.6 ± 0.5^f	890 ± 140	3.4	4.1 ± 0.6	94 ± 9
SDP.17b	2	298.8646	28.6	37.9 ± 1.1	22.9 ± 2.6	300 ± 30	7.2	7.8 ± 0.9	85 ± 10

Notes.

^(a)

Lines 1 and 2 correspond to the H₂O (2₁₁ − 2₀₂) (ν_rest = 752.03 GHz, E_up = 137 K) and (2₀₂ − 1₁₁) (ν_rest = 987.93 GHz, E_up = 101 K) transitions, respectively.

^(b)

ν_obs is the frequency corresponding to the zero of the velocity scale of the spectra of Fig. 1.

^(c)

S_νpk corresponds to the peak continuum flux density (mJy/beam); S_ν refers to the total spatially integrated continuum flux density (mJy).

^(d)

S_νH₂O pk corresponds to the peak H₂O flux density (mJy/beam); I_H₂O pk is the peak H₂O velocity-integrated flux density (flux in one beam, in Jy km s^-1/beam) and I_H₂O the spatially integrated H₂O line flux (in Jy km s^-1). The values derived for SDP.81 and G12.v2.30. are underestimated (see text).

^(e)

μL_H₂O is the apparent luminosity of the observed H₂O line using the relations given in, e.g., Solomon et al. (1992).

^(f)

In the cases of SDP.9, G12.v2.30 and G15.v2.779, the H₂O emission lines are double-peaked and the parameters in the table refer to double Gaussian fits.

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