Table 6.
Source properties.
| Source | Cat. | Scale | DL | SFRIR | SFR | M* | Mdust | log10(Ṁcool) | Pmech | Pcav | LX-ray | Mmol | tdep |
|---|---|---|---|---|---|---|---|---|---|---|---|---|---|
| (kpc/″) | (Mpc) | (M⊙ yr−1) | (M⊙ yr−1) | (1011 M⊙) | (M⊙) | (M⊙ yr−1) | (1042 erg s−1) | (1042 erg s−1) | (1044 erg s−1) | (M⊙) | 108 yr | ||
| (1) | (2) | (3) | (4) | (5) | (6) | (7) | (8) | (9) | (10) | (11) | (12) | (13) | (14) |
| M 87 | 1 | 0.082 | 16.1 | – | 0.14 ± 0.07 | 0.15 | < 1.3 × 108 | 1.29 ± 0.00 | 124.6 ± 17.6 | 6 | – | 4.7 × 105 | 0.03 |
| Centaurus | 1 | 0.208 | 43.9 | 0.13 | 0.16 ± 0.76 | 6.15 ± 0.14 | 1.6 × 106 | 0.97 ± 0.01 | 12.8 ± 0.8 | 7.4 |
1.74 | 0.9 × 108 | 5.5 |
| Abell 262 | 2 | 0.330 | 70.2 | 0.55 | 0.22 ± 0.87 | 3.31 ± 0.08 | 8.7 × 106 | 0.48 ± 0.04 | 12.4 ± 2.3 | 9.7 |
– | 3.4 × 108 | 15.2 |
| Abell 3581 | 1 | 0.435 | 94.9 | – | 0.78 ± 0.33 | 0.86 | ∼106 | 1.35 ± 0.22 | 48.2 ± 0.3 | 3.1 | – | 5.4 × 108 | 2.6 |
| 2A0335+096 | 1 | 0.700 | 150.0 | 2.09 | 0.46 ± 0.66 | 5.33 ± 0.26 | 7.3 × 105 | 2.26 ± 0.01 | 19.4 ± 2.5 | 24.0 |
9.77 | 1.1 × 109 | 23.5 |
| Hydra-A | 2 | 1.053 | 242.0 | 4.0 | 4.07 ± 2.81 | 4.18 ± 0.24 | 5.5 × 106 | 2.04 ± 0.02 | 816.5 ± 408.9 | 430.0 |
– | 5.4 × 109 | 13.2 |
| Abell S1101 | 1 | 1.094 | 251.8 | 2.30 | 1.02 ± 2.57 | 6.13 ± 0.55 | ∼107 | 2.37 ± 0.02 | 37 ± 0.9 | 780 |
1.10 | 10.8 × 108 | 10.7 |
| Abell 1795 | 1 | 1.220 | 283.9 | 8.0 | 3.45 ± 5.01 | 6.99 ± 0.52 | 6.7 × 107 | 2.27 ± 0.02 | – | 160 | 7.59 | 3.2 × 109 | 9.2 |
| RXJ1539.5 | 1 | 1.437 | 343.0 | – | 1.86 ± 1.14 | 2.3 | – | 2.19 ± 0.05 | 5.8 ± 0.7 | – | – | 1.3 × 1010 | 69.8 |
| Abell 2597 | 1 | 1.546 | 373.3 | 2.93 | 3.98 ± 2.29 | 3.24 ± 0.31 | 8.4 × 107 | 2.49 ± 0.05 | 295.1 ± 86.7 | 67.0 |
– | 2.3 × 109 | 5.8 |
| PKS 0745−191 | 1 | 1.890 | 474.1 | 17.07 | 13.48 ± 1.73 | 5 | 3.5 × 107 | 2.89 ± 0.01 | 400.2 ± 141.1 | 1700.0 |
18.41 | 4.9 × 109 | 3.6 |
| RXJ0821+0752 | 1 | 2.000 | 510.0 | 36.91 | 36.30 | 1.4 | 2.2 × 107 | – | 19.7 ± 2.5 | 13 | – | 2.3 × 1010 | 6.5 |
| Abell 1664 | 1 | 2.302 | 604.2 | 14.54 | 13.18 ± 1.09 | 2.5 | 1.3 × 107 | 2.21 ± 0.04 | 68.1 ± 3.0 | 95.2 ± 74.0 | 2.59 | 1.1 × 1010 | 8.3 |
| Abell 1835 | 1 | 3.966 | 1260.1 | 138 | 117.48 ± 1.58 | 5.7 | 1.0 × 108 | 3.07 ± 0.06 | 129.8 ± 19.2 | 1800.0 |
39.38 | 3.0 × 1010 | 4.3 |
| Phoenix-A | 1 | 6.750 | 3501.5 | 530 ± 53 | 616.59 ± 2.29 | ∼8 | – | 3.23 ± 0.08 | 10000.0 | 800–4700 | – | 2.1 × 1010 | 0.4 |
Notes. (1) Source name. (2) Category. Cat. 1: extended filaments, Cat 2: nuclear emission with disk-like morphologies and kinematics (see text for details). (3) Scale conversion of angular size to physical size. (4) Luminosity distance. (5) The SFR estimated from IR observations as given in the literature. (6) SFR from McDonald et al. (2018) – they estimated the SFR values in a variety of robust methods taking into account the AGN contamination. Phoenix: The spectrally decomposed AGN component. For the rest of the sample they determine SFRs based on an ensemble of measurements from the literature, principally from IR dust emission, optical lines, stellar continuum and optical SED fitting. (7) Mass of the stellar population collected from literature – using apparent K-band luminosities taken from the 2MASS Extended Source Catalog, the galactic extinction, evolution, and K-corrections were applied. Then McDonald et al. (2018) used the M/LK relation (Bell et al. 2003) for Centaurus, Abell 262, Hydra-A, 2A0335+096, Abell S1101, Abell 1796, Abell 2597 from Main et al. (2016), for Phoenix from Lidman et al. (2012), PKS 0745−191 from Donahue et al. (2011). Finally for Abell 3581, Abell 1664, Abell 1835, PKS 0745−191, RXJ0821+0752 WISE observations. (8) Dust mass collected from the literature, for Centaurus from Mittal et al. (2011), Hydra-A, 2A0335+096, RXJ0821+0752, Abell 2597, Abell 1664, Abell 1835 from Edge (2001), Abell 262, Abell 1795, PKS 0745−191 from Salomé & Combes (2003) using Tdust of 35 K, M 87 and Abell S1101 (McDonald et al. 2015), Phoenix-A. (9) Classical cooling rate are from McDonald et al. (2018), calculated inside the rcool (radius within the cooling time is less than 3 Gyr). Integrating the gas density within a sphere bounded by this radius provides an estimate of the total mass available for cooling, which is then divided by the cooling time. (10) Mechanical power: inferred from the AGN radio luminosity correlation (Bîrzan et al. 2004; Pulido et al. 2018). (11) The cavity power were obtained from Rafferty et al. (2006), Hlavacek-Larrondo et al. (2015), Pulido et al. (2018). (12) Bolometric X-ray luminosity (0.1 – 100 keV) from Chandra observations (Cavagnolo et al. 2009). (13) Molecular mass estimated from ALMA observations, assuming a XCO factor of 2 × 1020 cm−2 (K km s−1)−1 for all the systems. (14) Depletion time are calculated based on SFR and the molecular mass from ALMA observations. References. Centaurus (Mittal et al. 2011) from Herschel (36″) and Spitzer (65″) observations, Abell 262 (O’Dea et al. 2008), 2A0335+096 (O’Dea et al. 2008) from IR photometry within a 6″ aperture, which excludes both the companion galaxy and the filament, PKS 0745−191, RXJ0821+0752, Abell 1664, Abell 1835 using Spitzer photometry using different apertures depending the band from 12″, 26″, 35″ (see O’Dea et al. 2008; Quillen et al. 2008), Abell S1101 from Herschel PACS and SPIRE imaging McDonald et al. (2015), Hydra-A and Abell 1795 from Hoffer et al. (2012), Abell 1835 (McNamara et al. 2006), Abell 2597 (Donahue et al. 2007), Phoenix-A (Tozzi et al. 2015).
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