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Table C.2.

obscured QSO sample.

Target RA & Dec (J2000) z Jup rJup, 1 LCO (1010 K km s−1 pc2) Mgas (1010 M) log(Mstar) (M) log(LIR) (L) ref NH (1022 cm−2) log(LX) erg s−1 ref.
(1) (2) (3) (4) (5) (6) (7) (8) (9) (10) (11) (12) (13)
no.682 03:32:59 −27:45:22 1.155 2 0.8 < 0.84 < 3.02 10.6 11.92 K17 < 1 42.43 Lu17
W0410-0913 04:10:10 −09:13:05 3.592 4 0.87 16.28 ± 1.44 13.1 ± 1.15∘ 13.72 ± 0.03 F18 < 46.08 V17
X2522 09:57:28 +02:25:42 1.532 2 0.8 < 1.67 < 6.00 11.3 12.5 K17 < 0.8 45.03 M16
X5308 09:59:22 +01:36:18 1.285 2 0.8 < 1.06 < 3.82 11.0 12.02 K17 < 2 44.28 M16
C1148 10:00:04 +02:13:07 1.563 2 0.8 < 1.66 < 5.98 11.1 12.2 K17 > 2.7 44.42 M16
COSMOS22995 10:00:17 +02:24:52 2.469 1 1.0 < 1.3 < 1.3 11.08 12.3 Sp16 33 ± 17 43.91 Br14
COSB011 10:00:38 +02:08:22 1.827 sled 5.89 ± 1.16 4.71 ± 0.93∘ 13.13 A08 1 − 10 44.02 A08
C152 10:00:39 +02:37:19 1.188 2 0.8 < 0.53 < 1.91 10.4 11.52 K17 < 2.6 43.9 M16
C92 10:01:09 +02:22:55 1.581 2 0.8 2.64 ± 0.25 9.5 ± 0.9 11.2 12.8 K17 43.73 M16
C103 10:01:10 +02:27:17 1.433 2 0.8 < 0.66 < 2.38 10.7 11.82 K17 < 1.6 44.15 M16
C1591 10:01:43 +02:33:31 1.238 2 0.8 1.67 ± 0.4 6.0 ± 1.4 11.3 12.62 K17 44.25 M16
C488 10:01:47 +02:02:37 1.171 2 0.8 < 0.42 < 1.51 10.3 11.62 K17 44.25 M16
XID2028 10:02:11 +01:37:06 1.592 sled 1.43 ± 0.63 1.14 ± 0.50∘ 11.65 ± 0.35 B18 0.7 ± 0.02 45.32 P15
HS1002 10:05:17 +43:46:09 2.102 1 1.0 11.9 ± 3.4 9.5 ± 2.7∘ 13.08 ± 0.08 C08,S16
SDSS J1148+5251 11:48:16 +52:51:50 6.418 2 1.0 3.2 ± 0.3 2.6 ± 0.2∘ 13.16 St15 45.18 ± 0.12 G17
RXJ121803 12:18:04 +47:08:51 1.742 2 1.0 < 2.47 < 1.97∘ 12.8 ± 0.4 C08 S05
ULASJ1234 12:34:27 +09:07:54 2.503 3 0.8 4.4 ± 0.8 3.5 ± 0.6∘ 13.24 ± 0.12 Ba17 0.89 ± 0.09 45.13 Ba14
SMMJ123606 12:36:06 +62:10:24 2.505 3 0.52 2.86 ± 0.82 2.86 ± 0.82 10.3 12.81 Bo13 43.52 L10
SMMJ123618 12:36:18 +62:15:51 1.996 4 0.41 4.6 ± 0.6 4.6 ± 0.6 10.7 12.9 Bo13 < 7.4 L10
SMMJ123707 12:37:07 +62:14:08 2.487 3 0.52 6.53 ± 1.53 6.53 ± 1.53 10.8 12.59 Bo13 43.50 L10
SMMJ123711 12:37:11 +62:13:31 1.995 3 0.52 8.2 ± 1.7 8.2 ± 1.7 11.5 12.83 Bo13 43.36 L10
SMMJ1237 12:37:16 +62:03:23 2.057 3 1.0 < 0.62 < 0.5∘ 12.71 ± 0.4 C08 0.17 44.02 Y09
RXJ1249 12:49:13 −05:59:19 2.240 1 1.0 5.1 ± 1.2 4.1 ± 1.0∘ 12.84 ± 0.08 C08,S16 44.92 S10
SMMJ1312 13:12:22 +42:38:13 2.554 3 1.0 1.2 ± 0.4 1.0 ± 0.3∘ 12.5 ± 0.4 C08 < 1.26 44.6 Bo14
VCV J140955 14:09:55 +56:28:27 2.576 1 1.0 8.6 ± 2.3 6.9 ± 1.8∘ 13.31 ± 0.02 C08,S16
3C 298 14:19:08 +06:28:35 1.438 3 0.97 1.15 ± 0.11 0.92 ± 0.09∘ 12.75 ± 0.01 Va17 21.4 ± 0.2 46.12 S08
ULASJ1539 15:39:10 +05:57:50 2.658 3 1.0 5.46 ± 0.94 4.36 ± 0.75∘ 10.9 ± 0.27 12.82 F14 4 ± 2 45.12 M17
J154359 15:43:59 +53:59:03 2.369 1 1.0 2.9 ± 0.7 2.3 ± 0.6∘ 12.86 ± 0.10 C08,S16 2 45.46 Y09
HS1611 16:12:39 +47:11:57 2.403 3 1.0 5.2 ± 0.8 4.2 ± 0.6∘ 13.1 ± 0.4 C08
SMMJ163650 16:36:50 +40:57:34 2.383 3 0.52 11.4 ± 0.7 11.4 ± 0.7 11.0 13.24 Bo13
MMJ163655 16:36:55 +40:59:10 2.607 3 1.0 < 0.8 < 0.6∘ 12.8 ± 0.4 C08 32 ± 6 44.89 M03
SMMJ163706 16:37:06 +40:53:15 2.377 3 0.52 3.8 ± 0.7 3.8 ± 0.7 11.1 12.76 Bo13
J164914 16:49:14 +53:03:16 2.270 3 1.0 < 2.2 < 1.8∘ 12.9 ± 0.4 C08 < 0.79 45.51
MIPS8342 17:14:11 +60:11:09 1.562 2 1.0 2.32 ± 0.25 1.86 ± 0.20 12.56 Y10 < 43.45 B10
MIPS8196 17:15:10 +60:09:54 2.586 3 1.0 < 1.70 < 1.36 13.0 Y10 < 43.78 B10
MIPS8327 17:15:35 +60:28:25 2.441 3 1.0 1.31 ± 0.21 1.04 ± 0.17 12.84 Y10
MIPS429 17:16:11 +59:12:13 2.213 3 1.0 2.97 ± 0.50 2.38 ± 0.40 12.73 Y10
AMS12 17:18:22 +59:01:54 2.767 3 1.0 4.4 ± 0.4 3.5 ± 0.3 11.48 ± 0.04 13.52 ± 0.10 S12
MIPS16080 17:18:44 +60:01:16 2.007 3 1.0 2.08 ± 0.37 1.66 ± 0.30 12.72 Y10 < 43.7 B10
MIPS15949 17:21:09 +60:15:01 2.122 3 1.0 2.79 ± 0.29 2.23 ± 0.23 12.91 Y10
MIPS16059 17:24:28 +60:15:33 2.326 3 1.0 1.80 ± 0.55 1.44 ± 0.43 12.88 Y10
VHSJ2101 21:01:19 −59:43:44 2.313 3 0.8 1.78 ± 0.11 1.44 ± 0.09 12.93 ± 0.15 Ba17
ULASJ2315 23:15:56 +01:43:50 2.560 3 0.8 4.31 ± 0.21 3.44 ± 0.16 13.61 ± 0.03 Ba17 0.71 ± 0.44 45.52 M17
Compton Thick QSOs

SW022513 02:25:13 −04:39:19 3.427 4 1.0 8.4 ± 1.2 6.72 ± 0.96 11.3-11.6 12.5-13.3 P11 ≳100 44.78 P11
SW022550 02:25:50 −04:21:49 3.867 4 1.0 5.8 ± 1.0 4.64 ± 0.80 11.2-11.9 12.5-13.2 P11 ≳100 < 45.5 P11
XID403 03:32:29 −27:56:19 4.762 2 1.0 2.0 ± 0.4 1.6 ± 0.3 10.8 ± 0.22 12.78 ± 0.07 G14 140 ± 70 44.40 G14
GMASS953 03:32:31 −27:46:23 2.225 3 0.1 2.1 ± 0.2 1.7 ± 0.1 11.3 ± 0.1 12.33 ± 0.04 Po17 340−150+370 43.61 DM

Notes. Molecular gas: For each target we report the upper level of the CO transition, Jup, and the excitation correction, rJup, 1 (see Notes in Table C.1). For COSB011 and XID2028, the CO(1-0) luminosity was derived extrapolating the ground-state transition flux from the QSOs SLEDs. We also indicate the luminosity-to-gas-mass conversion factors used to derive the gas mass in the different papers, as follows: : αCO = 3.6; : αCO = 1.0; ∘: αCO = 0.8. The sample of dusty AGN comprises a large number of sources associated with evidence of multiphase outflows: broad and shifted components in the [O III] emission lines (e.g. Coppin et al. 2008; Perna et al. 2015a; Polletta et al. 2011) and in molecular CO lines (e.g. Banerji et al. 2017; Brusa et al. 2018; Fan et al. 2018; Stefan et al. 2015) are usually found in these targets. For a small number of sources there are also indications of ongoing mergers (W0149+2350, SMMJ030227, 3C 298). For these sources, characterised by complex CO line profiles, we report in the Table (and in the figures) the total molecular luminosities and masses obtained integrating over all the different kinematic components. X-ray luminosities and Column densities: X-ray luminosities refer to the 2–10 keV rest-frame absorption-corrected luminosities; column densities are derived from X-ray spectroscopic analysis for all but no. 226 and no. 682, for which NH is derived from the hardness ratio, following the prescriptions in Elvis et al. (2012). To our knowledge, the only CT sources with molecular line observations are XID403 (from C10, G14), SW022513, and SW022550 (from P11), and GMASS953 (from T18). The source C1148 (from K17), detected with 20 net counts in X-ray, is a candidate CT source (see Sect. 4.1). The few CT sources at z > 1 are tabulated in the lower part of the table. Stellar masses and IR luminosities: A08, B18, E14, F18, G14, K17, St15 (from Leipski et al. 2013), St17, Po17 (from T18), Va17 (from Podigachoski et al. 2015), and Y10 host galaxy properties are obtained with a two-component (AGN+galaxy) SED fit; their IR luminosities refer therefore to the only stellar component. B13: IR luminosities are obtained from the 1.4 GHz continuum. Ba17: IR luminosities are obtained using a modified greybody model assuming dust temperature and dust emissivity values (T = [41, 47]; β = [1.6, 1.95]), and rescaling the model to match the 3mm observations. C08: stellar mass from Wardlow (2011); LIR assuming a dust temperature of T = 40 K and a dust emissivity factor of νβ, with β = 1.5, rescaling a modified greybody model to match the 850 or 1200 μm photometry. F14: stellar IR luminosity is obtained with a two-component (AGN+galaxy) SED fit, but is not well constrained due to the lack of data above the 22 μm. P11: stellar IR luminosities are obtained with a two-component (AGN+galaxy) SED fit, but is not well constrained due to the lack of data between 24 μm and 1.2mm. Mstar from H-band luminosity. S12: IR luminosity is obtained by fitting the far-IR SED with a greybody model. Sp16: SFR and stellar mass from 3D-HST catalogue (Momcheva et al. 2015, i.e. without considering AGN component). The source is undetected in any Herschel/PACS or SPIRE bands. The infrared luminosity is derived from SFR, using the following prescription: LIR = SFR × 1010 L (Kennicutt 1998, correcting for a Chabrier IMF). Y10: these sources are undetected in SPIRE bands; far-IR emission is constrained using upper limits and mid-IR Spitzer spectra. Column (1): target name; Column (2): coordinates; Column (3): redshift; Column (4): Jup refers to the upper level of the (JupJup − 1) CO transition; Column (5): the excitation correction defined as rJup, 1 = CO(JupJup − 1)/CO(1 → 0); Column (6): CO(1-0) luminosity; Column (7): gas mass; Column (8): stellar mass; Column (9): 8–1000 μm IR luminosity; Column (10): reference for the paper from which we derived CO and far-IR measurements, as well as assumed excitation correction and αCO conversion factors. Columns (11) and (12): column density and 2–10 keV rest-frame absorption-corrected luminosities derived from X-ray spectroscopic analysis (see below). Column (13): reference for the paper from which we derived X-ray properties.

References. Aravena et al. (2008, A08); Banerji et al. (2017, Ba17); Banerji et al. (2014, Ba14); Bauer et al. (2010, B10); Bothwell et al. (2013, Bo13); Bongiorno (2014, Bo14); Brightman et al. (2014, Br14); Brusa et al. (2018, B18); Coppin et al. (2008, C08); Coppin et al. (2010, C10); Della Mura et al. (in prep., DM); Emonts et al. (2014, E14); Fan et al. (2018, F18); Feruglio et al. (2014, F14); Gallerani et al. (2017, G17); Gilli et al. (2014, G14); Kakkad et al. (2017, K17:); Laird et al. (2010, L10); Luo et al. (2017, Lu17); Marchesi et al. (2016, M16); Martocchia et al. (2017, M17); Perna et al. (2015a, P15); Polletta et al. (2011, P11); Popping et al. (2017, Po17); Siemiginowska et al. (2008, S08); Schumacher et al. (2012, S12); Sharon et al. (2016, S16); Spilker et al. (2016, Sp16); Stefan et al. (2015, St15); Stevens et al. (2005, S05); Streblyanska et al. (2010, S10); Talia et al. (2018, T18);Vayner et al. (2017, Va17); Vito et al. (2017, Vi17); Yan et al. (2010, Y10); Young et al. (2009, Y09).

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