Table 2.
Estimated properties of the CO emissions.
| Object | ICO | ΔVFWHM | zCO |  |
μS160 μm | Log μSFR | Log MBH | η | μSF |
|---|---|---|---|---|---|---|---|---|---|
| [K km s−1] | [km s−1] | [K km s−1 pc2] | [mJy] | [M⊙ yr−1] | [M0⊙] | ||||
| (1) | (2) | (3) | (4) | (5) | (6) | (7) | (8) | (9) | (10) |
| PSJ0147+4630 | 0.75 ± 0.07 | 272 ± 30 | 2.3637 | 11.06 ± 0.24 | – | – | 10.05 ± 0.35a | 0.11 ± 0.29a | – |
| SDSS J0924+0219 | 0.65 ± 0.12 | 211 ± 46 | 1.5251 | 11.0 ± 0.28 | 49.26 ± 10.58 | 3.31 ± 0.28 | 7.93 ± 0.34b | 0.04 ± 0.03b | 23.5c |
| SDSS J1330+1810 | 0.42 ± 0.06 | 219 ± 36 | 1.3945 | 10.75 ± 0.26 | 76.47 ± 12.46 | 3.40 ± 0.27 | 9.19 ± 0.02d | 0.02 ± 0.02d | 24 ± 1e |
| H1413+117 | 2.78 ± 0.19 | 528 ± 42 | 2.5585 | 11.68 ± 0.23 | 123.26 ± 32.17 | 4.26 ± 0.28 | 9.12 ± 0.01b | 0.28 ± 0.06b | 10.3e |
| J2145+6345 | 0.54 ± 0.09 | 216 ± 45 | 1.5652 | 10.95 ± 0.28 | – | – | – | – | – |
| PMNJ0134-0931 | < 0.92 (3σ) | 289 | – | < 11.11 (3σ) | – | – | – | – | – |
| COSMOS5921+0638 | < 0.92 (3σ) | 289 | – | < 11.35 (3σ) | – | – | – | – | – |
| SDSS J1004+4112 | < 0.87 (3σ) | 289 | – | < 11.24 (3σ) | – | – | – | – | – |
| J1042+1641 | < 0.99 (3σ) | 289 | – | < 11.22 (3σ) | – | – | 9.60 ± 0.1f | 0.05 ± 0.01f | 43 ± 1e |
| HE1113-0641 | < 1.68 (3σ) | 289 | – | < 11.24 (3σ) | – | – | – | – | – |
| SDSS J1138+0314 | < 0.82 (3σ) | 289 | – | < 11.12 (3σ) | 42.30 ± 4.25 | 3.75 ± 0.26 | 7.69 ± 0.33b | 0.43 ± 0.36b | – |
| HST14113+5211 | < 0.70 (3σ) | 289 | – | < 11.16 (3σ) | < 36.38 | < 3.82 | – | – | – |
| B1422+231 | < 0.66 (3σ) | 289 | – | < 11.31 (3σ) | 7.96 ± 0.88 | 3.43 ± 0.26 | 9.72 ± 0.38g | 0.45 ± 0.31g | 24.22h |
| SDSS J1433+6007 | < 1.22 (3σ) | 289 | – | < 11.38 (3σ) | – | – | – | – | – |
| J1817+2729 | < 0.82 (3σ) | 289 | – | < 11.29 (3σ) | – | – | – | – | – |
| B1933+503 | < 1.57 (3σ) | 289 | – | < 11.46 (3σ) | 160.95 ± 22.3 | 3.95 ± 0.27 | – | – | – |
| SDSS J2222+2745 | < 1.63 (3σ) | 289 | – | < 11.52 (3σ) | – | – | – | – | – |
Notes. (1) Object name. (2) CO J = 1-0 line luminosity converted from the high J-level emission line, assuming the line ratio as R12 = 1.2, R13 = 1.8 (Tacconi et al. 2018), which is not corrected for the gravitational lensing magnification. For nondetection objects, the flux is estimated to be three times the standard deviation of the continuum as the upper limit, and the FWHM is assumed as the average of the five detected objects (289 km s−1). (3) FWHM of detected CO emission lines. (4) The inferred redshift from the CO emission lines. (5) The inferred CO J1-0 luminosity without the magnification correction. (6) Flux density at 160 μm, which is inferred from the best-fit SED. (7) Star formation rate estimated from 160 μm luminosity based on the Eq. (25) in Calzetti et al. (2010). (8) The SMBH masses collected from the literature, which are corrected for the magnifications. (9) The Eddington ratio. (10) Magnification factors estimated from high-resolution CO emissions from the literature. Except for B1422+231, whose magnification was estimated from millimeter-continuum observations. a This work, b Sluse et al. (2012), c Badole et al. (2020), d Frias Castillo et al. (2024), e Stacey et al. (2022), f Matsuoka et al. (2018), g Assef et al. (2011), h Wen & Kemball (2022).
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