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Table 3

CO emission properties.

Source z CO CO S / N det a FWHM CO b F CO b c M gas d f gas d
line (km s-1) (Jy km s-1) (109 K km s-1 pc2) (1010M)

A68-C0 1.5854 2–1 11 334 ± 76 1.89 ± 0.28 2.6 ± 0.4 1.2 0.38
A68-HLS115 1.5859 2–1 14 267 ± 18 2.00 ± 0.30 5.5 ± 0.9 2.4 0.75
MACS0451-arc 2.0118 3–2 4–5 261 ± 41 1.27 ± 0.32 1.0 ± 0.3 0.4 0.62
A2218-Mult 3.104 3–2 undetected < 0.62 e < 3.8 < 1.7
A68-h7 2.1529 3–2 3–4 282 ± 61 1.12 ± 0.22 16.9 ± 3.3 7.4 0.33
MS 1512-cB58 2.727 1–0 174 0.052 ± 0.013 f 0.6 ± 0.15 0.3 0.41
Cosmic Eye 3.074 1–0 200 0.077 ± 0.013 f 1.2 ± 0.2 0.5 0.18

Notes.

(a)

Signal-to-noise ratio of the CO emission detection.

(b)

Full widths half maximum and “observed” CO(21) or CO(32) line integrated fluxes in Jy km s-1 and their 1σ errors, as derived from fitting Gaussian function(s) to the observed CO profile.

(c)

Lensing-corrected CO(10) integrated line luminosities obtained with the following prescriptions: (1) the Solomon et al. (1997) formula , where νobs is the observed line frequency in GHz and DL is the luminosity distance in Mpc; (2) the correction factors and adopted for SFGs to account for the CO(21) and CO(32) transitions being slightly subthermally excited (see Sect. 4); and (3) the lensing magnification correction, μ, given in Table 1.

(d)

Molecular gas masses, , obtained by assuming the “Galactic” CO–H2 conversion factor XCO = 2 × 1020 cm-2/ (K km s-1), or α = 4.36 M/ (K km s-1 pc2) including the correction factor of 1.36 for helium. The molecular gas fraction is expressed as fgas = Mgas/ (Mgas + M). Both quantities correspond to intrinsic values corrected from magnification factors.

(e)

4σ upper limit estimated by assuming a full width half maximum FWHMCO = 200 km s-1 for the undetected CO(32) line.

(f)

“Observed” CO(10) integrated line fluxes and their 1σ errors from Riechers et al. (2010).

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