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Table 7.

Properties of individual star-forming clumps in the Emerald.

Source RA Dec μS850 SFR μ ICO(4 − 3) Mgas v FWHM αvir
(J2000) (J2000) (mJy) (M yr−1) (Jy km s−1) (109M) (km s−1) (km s−1)
1.2 N 11:27:14.67 +42:28:23.9 7.8 ± 0.6 100 ± 8 14.2 (2.3 ± 0.2)×10−1 5.0 ± 0.5 44 ± 9 374 ± 38 2.9 ± 0.6
1.2 S (m) 11:27:14.70 +42:28:23.0 8.1 ± 0.6 41 ± 3 35.0 (5.0 ± 0.5)×10−2 1.0 ± 0.1 334 ± 28 199 ± 17 1.4 ± 0.3
1.2 S (b) (5.0 ± 0.6)×10−2 1.2 ± 0.1 135 ± 17 333 ± 43 5.3 ± 1.1

Notes. We list observed values for continuum flux densities, S850, and intrinsic values for line fluxes, star-formation rates and gas masses. The local magnification factors are listed in column μ. Error bars give the rms for the continuum and uncertainties in the fit for emission-line data. For the clumps where we identify a secondary line component, we also list the velocity offset and FWHM line width at the position of that clump. The virial parameters, αvir, quantify the relative contribution from gravitational binding and turbulent energy.

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