Table 1.
Properties of the Planck’s dusty GEMS that were part of our CO emission-line survey with EMIR.
| Source | RA (J2000) | Dec (J2000) | zspec | μdust | μgas | Δμ/μ | LFIR (1012 L⊙) | r1/2 (kpc) |
|---|---|---|---|---|---|---|---|---|
| PLCK_G045.1+61.1 | 15:02:36.04 | +29:20:51 | 3.4286 ± 0.0003 | 19.1 ± 1.2a | 15.5 ± 0.7 | < 10% | 4.4 ± 0.3 | ... |
| PLCK_G080.2+49.8 | 15:44:33.25 | +50:23:45 | 2.5984 ± 0.0001 | 14.7 ± 0.8 | 15.9 ± 1.5 | < 30% | 3.1 ± 0.2 | ... |
| PLCK_G092.5+42.9 | 16:09:17.76 | +60:45:21 | 3.2557 ± 0.0002 | 15.4 ± 1.0 | 12.0 ± 0.6 | < 10% | 16.1 ± 1.2 | ... |
| PLCK_G102.1+53.6 | 14:29:17.98 | +59:21:09 | 2.9170 ± 0.0003 | 7.1 ± 0.2 | 6.9 ± 0.3 | < 5% | 5.0 ± 0.3 | ... |
| PLCK_G113.7+61.0 | 13:23:02.88 | +55:36:01 | 2.4166 ± 0.0002 | 11.2 ± 0.7 | 9.7 ± 0.5 | < 5% | 8.8 ± 0.7 | ... |
| PLCK_G138.6+62.0 | 12:02:07.68 | +53:34:40 | 2.4420 ± 0.0002 | ∼20b | ∼20b | ... | 4.5 ± 2.3 | ... |
| PLCK_G145.2+50.9 | 10:53:22.56 | +60:51:49 | 3.5487 ± 0.0003 | 7.6 ± 0.5 | 8.9 ± 0.5 | < 10% | 28.7 ± 2.2 | ... |
| PLCK_G165.7+67.0 | 11:27:14.60 | +42:28:25 | 2.2362 ± 0.0003 | 29.4 ± 5.9 | 24.1 ± 4.8 | < 30% | 3.5 ± 0.7 | 1.4 |
| PLCK_G200.6+46.1 | 09:32:23.67 | +27:25:00 | 2.9726 ± 0.0004 | ∼15b | ∼15b | ... | 3.8 ± 1.3 | ... |
| PLCK_G231.3+72.2 | 11:39:21.60 | +20:24:53 | 2.8589 ± 0.0003 | 7.9 ± 0.3 | 6.0 ± 0.5 | < 10% | 9.5 ± 0.5 | ... |
| PLCK_G244.8+54.9 | 10:53:53.04 | +05:56:21 | 3.0054 ± 0.0001 | 21.8 ± 0.6c | 22.0 ± 1.3c | < 5% | 12.2 ± 0.4 | 0.6 |
Notes. The source positions are those used to point the IRAM 30-m telescope for the single-dish spectroscopic observations. Here zspec is the best spectroscopic redshift inferred from single Gaussian fits to the lowest-J CO emission lines detected with EMIR, between Jup = 3 and Jup = 5. The quantity μdust is the luminosity-weighted magnification factor of the 880-μm dust continuum, mostly obtained from the highest resolution SMA maps, either in the EXT or VEXT configuration. μgas is the luminosity-weighted magnification factor of the gas component in the GEMS derived from our CO Jup = 4–6 interferometry using IRAM/PdBI. Both factors are inferred from detailed strong lensing models that will be presented in a forthcoming paper (Cañameras et al., in prep.), with errors showing their ±1σ statistical uncertainties. Expected systematics on the magnification factors are listed in the column headed Δμ/μ (see further details in the text). The quantity LFIR is the delensed value of the total FIR luminosity (8–1000 μm) presented in C15, including statistical uncertainties on μ. Finally, r1/2 is the intrinsic half-light radius of the dust continuum from the source.
Computed from the ALMA 0.7-mm continuum map at 0.42″ × 0.28″ beam size presented in Nesvadba et al. (2016).
Rough estimate of μ from the scaling relation between LFIR and Tdust in unlensed SMGs (see C15 for details), for the sources without detailed lensing models.
The magnification factors of the Ruby are inferred from the ALMA very extended baseline observations of the 3-mm dust continuum and CO(4–3) line emission presented in Cañameras et al. (2017a).
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