Main observed and derived properties of our galaxies.
|ID||z||μ||β||LUV × μ||Library of||LIR × μ||SFRIR||Tdust|
|[1012L⊙]||best FIR fit||[1012L⊙]||[M⊙ yr-1]||[K]|
|A68/C0||1.5854||30||0.19 ± 0.02||R09||3.55 ± 0.2||20.4 (19.2−21.5)||34.5|
|A68/h7||2.15||3||0.22 ± 0.01||R09||315 (294−330)||43.3|
|A68/HLS115||1.5859||15||0.1 ± 0.01||CE01||59.0 (56.3−61.7)||37.5|
|MACS0451 north||2.013||49||0.55 ± 0.01||CE01||12.8(12.2-13.4)||49.2|
|MACS0451 full arc||′′||′′||′′||1.2 ± 0.03||M10||32.1 (31.3−32.8)*||50−80*|
|cB58||2.73||30||CE01||9.12 ± 0.21||52.4 (51.2−53.6)||50.1a|
|Cosmic Eye||3.07||28||2.57 ± 0.06||R09||58.8 (54.9−61.6)||46.3a|
Notes. β stands for the UV slope at 2000 Å, measured from 1800 to 2200 Å. The values of β presented are the averages of the best Calzetti-based solution and the best SMC one. The LIR values are produced by integrating the [8, 1000 μm] interval on the best-fit SED’s shown here in the column on their left. The values of SFRIR are then obtained via the Kennicutt (1998) calibration from the intrinsic (de-lensed) LIRvalues. Errors and values in parenthesis represent the 68% confidence levels from our MC runs. For the peculiar case of the MACS0451 arc, we show quantities of the northern part (that seems to be starburst-dominated), and for the whole arc (that may be AGN contaminated, hence the asterisks) for convenience and to illustrate the flux ratios between the north segment and the whole arc. See Sect. 5.1.5 for further discussion. Uncertainties on the temperatures are on the order of ± 1 K, with the exception of the Cosmic Eye for which it is ± 3 K, because of the uncertainties on the SPIRE photometry and de-blending.
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