Molecular gas content in strongly lensed z ~ 1.5−3 star-forming galaxies with low infrared luminosities

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Volume 577 (May 2015)

A&A, 577 (2015) A50

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Table 2

Observation summary.

Source	Coordinates		T _on−source	CO	ν _obs ^a	Synthesized beam^b		Bandwidth^c	rms^d
	RA (J2000)	DEC (J2000)	(hours)	line	(GHz)	Size (″)	PA (°)	(MHz)	(mJy)

A68-C0	00:37:07.404	+09:09:26.57	5.2	2–1	89.131	6.41 × 5.53	174	15	0.72
A68-HLS115	00:37:09.503	+09:09:03.80	4.6	2–1	89.128	5.94 × 5.79	111	15	0.71
MACS0451-arc	04:51:57.093	+00:06:10.44	30.2	3–2	114.768	5.45 × 4.12	163	19	0.84
A2218-Mult	16:35:48.919	+66:12:13.81	9.2	3–2	84.258	6.35 × 5.90	90	15	0.77
A68-h7^e	00:37:01.41	+09:10:22.31	5.5	3–2	109.777			24	0.94

Notes.

^(a)

Observed line frequency used for tuning.

^(b)

Beam resulting after combining all available imaging with natural weighting. These are the beam sizes and position angles displayed in Fig. 3.

^(c)

Bandwidth achieved after resampling the PdBI data to a resolution of 50 km s^-1 and the 30 m telescope data to a resolution of 65 km s^-1. Such resampling perfectly suits observed CO lines with full widths at half maximum > 200 km s^-1.

^(d)

Noise per beam obtained for the specified bandwidth and averaged over the full 3.6 GHz spectral range after excluding channels where CO emission is detected.

^(e)

Source observed at the 30 m single dish telescope, while all the other sources were observed with the PdBI.

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