Physical properties of MACSJ0032-arc.
|z CO||3.6314 ± 0.0005|
|μ a||62 ± 6|
|LUV/μ (L⊙) †|
|LIR/μ (L⊙) †, b|
|SFRUV + IR/μ ≃ SFRSED/μ (M⊙ yr-1) †|
|M∗/μ (M⊙) †|
|sSFR = SFR/M∗ (Gyr-1)|
|SFRradio/μ (M⊙ yr-1) †, c||58 ± 11|
|Tdust (K) d||43 ± 5|
|Mdust/μ (M⊙) †, d||(1.9 ± 0.7) × 107|
|(K km s-1 pc2) †, d||(2.54 ± 0.73) × 109|
|(K km s-1 pc2) †, e||(1.53 ± 0.37) × 109|
|(K km s-1 pc2) †, e, f||(0.70 ± 0.15) × 109|
|0.60 ± 0.17|
|0.28 ± 0.08|
|αCO (M⊙/ (K km s-1 pc2)) g||2.8−7.1|
|Mmolgas/μ (M⊙) †, h||(7.1 − 18) × 109|
|fmolgas = Mmolgas/ (Mmolgas + M∗)||0.60−0.79|
|tdepl = Mmolgas/SFR (Gyr)||0.14−0.35|
Star formation rate as derived from the 5 GHz continuum and the SFR–1.4 GHz calibration from Bell (2003). The total 5 GHz flux (Table 1) is first corrected for the flux excess observed in image E by propagating the 5 GHz–F814W color properly measured in images B, C, and D over the counter-image E.
CO luminosities inferred from the CO line integrated fluxes (FCO) in Jy km s-1 (Table 1) that have been beforehand corrected against the CMB (Sect. 4.3), and derived using the Solomon et al. (1997) formula: , where νobs is the observed CO line frequency in GHz, and DL is the luminosity distance of the galaxy in Mpc.
The total CO(6–5) line integrated flux (Table 1) is first corrected for the flux excess observed in image E by propagating the CO(6–5)–F814W color properly measured in image C over the counter-image E.
CO-to-H2 conversion factor as computed in Sect. 5.1.
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