Table 1.
Physical properties of the targeted sample and observing log.
| ID | Object | Redshift (a) |  (b) |
 (c) |
SFR (d) | Mdust(e) | Seeing (f) | Exp. time | SBlimLyα | Type |
|---|---|---|---|---|---|---|---|---|---|---|
| [M⊙ yr−1] | [108 M⊙] | [arcsec] | [min] | [ × 10−18] (g) | ||||||
| 1 | BR1202 − 0725 | 4.6942 ± 0.0003 ([C II]) | 47.7 | 13.7 ± 0.2 | 5000 ± 2300 | 23.6 ± 3.1 | 1.1 | 126 | 3.2 (i) | QSO+SMG |
| 2 | G09 − 0902 + 0101 | 3.120 | 46.5 | 13.2 ± 0.1 | 1600 ± 370 | 17.4 ± 3.6 | 1.0 | 44 | 3.1 | SMG hosting a QSO (h) |
| 3 | G15 − 1444 − 0044 | 3.375 | 46.6 | 13.3 ± 0.1 | 2000 ± 460 | 19.7 ± 2.9 | 1.0 | 44 | 3.3 | SMG hosting a QSO (h) |
| 4 | ALESS61.1 | 4.4189 ± 0.0004 (CO(4-3)) | – | 12.6 ± 0.1 | 400 ± 90 | 4.8 ± 0.9 | 1.3 | 86 | 2.5 | SMG |
| 5 | ALESS65.1 | 4.4445 ± 0.0005 (CO(4-3)) | – | 12.6 ± 0.1 | 400 ± 90 | 4.7 ± 1.1 | 1.2 | 86 | 2.2 | SMG |
Notes.
Redshifts from Carilli et al. (2013), Fu et al. (2017) and Birkin et al. (2021). In brackets we report the line used for precise redshift estimates. For G09-0902+0101 and G15-1444-0044, the redshifts are the best values from Lyke et al. (2020), whose uncertainties are on the order of a few hundred km s−1.
Bolometric luminosities computed from the observed luminosities at 1450 Å using the relation by Runnoe et al. (2012).
IR luminosities at 8 − 1000 μm due to star formation recomputed in this work, and consistent within uncertainties with values in Wagg et al. (2012), Fu et al. (2017) and Birkin et al. (2021). For BR1202-0725 we only use the data points for the QSO from Omont et al. (1996a) and Iono et al. (2006).
SFR computed using the formula 
(Fu et al. 2017). The errors reflect only the uncertainty on the IR luminosities.
Dust masses computed assuming a modified blackbody with dust emissivity spectral index β = 2.0 and fixing the dust temperature only for BR1202-0725 as we only use two data points not covering the SED peak (Tdust = 68 K; Leech et al. 2001). For the other sources we found Tdust ∼ 55 K.
The seeing is estimated by fitting a 2D Moffat model to point sources in each field (see Appendix A).
2σ SB detection level within 1 square arcsecond and 30 Å at the expected Lyα wavelengths, in units of erg s−1 cm−2 arcsec−2.
The host-galaxies are submillimeter bright with the flux at 870 μm of S870 = 14.4 and 6.0 mJy for G09-0902+0101 and G15-1444-0044, respectively (Fu et al. 2017).
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