Table 2.
Multiwavelength properties of the BGG sample.
| BGG | M(H2) | log(M⋆) | SFR | CCT | min(tcool/tff) | tcool/teddy | Core type | Tsys | K1 | K10 | R500 | M500 | Radio | LLS | X-ray | Notes | |
|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|
| (108 M⊙) | (M⊙) | (M⊙ yr−1) | (Gyr) | T profile | Hudson | (keV) | (keV cm−2) | (keV cm−2) | (kpc) | (1013 M⊙) | (kpc) | ||||||
| (1) | (2) | (3) | (4) | (5) | (6) | (7) | (8) | (9) | (10) | (11) | (12) | (13) | (14) | (15) | (16) | (17) | (18) |
| NGC 193 | < 1.35 | 10.92 | – | – | – | – | CC | – | 0.88 |
11.31 | 24.3 | 432 | 2.33 | JET | 80 | GRP | Shock |
| NGC 410 | < 1.17 | 11.37 | – | 0.102 | 18.2 | 0.5 | CC | SCC | 0.98 ± 0.02 | 4.50 | 34.5 | 458 | 2.78 | pnt | ≤11 | GRP | |
| NGC 584 | < 0.11 | 10.62 | 0.024 | – | – | – | – | – | – | < 270.62 | > 272.7 | – | – | pnt | ≤3 | – | |
| NGC 677 | < 2.25 | 10.91 | – | 2.042 | 47.9 | 1.69 | CC | WCC | 0.79 ± 0.01 | 5.82 | 31.9 | 406 | 1.94 | Diffuse | 30 | GRP | |
| NGC 777 | < 2.08 | 11.32 | 0.014 | 0.314 | 39.2 | 1.0 | NCC | SCC | 0.89 ± 0.02 | 23.84 | 34.8 | 434 | 2.37 | pnt | ≤8 | GRP | |
| NGC 924 | 0.52 ± 0.10 | 10.76 | 0.545 | – | – | – | – | – | – | < 403.08 | > 406.1 | – | – | pnt | ≤4 | – | |
| NGC 940 | 61.0 ± 2.15 | 10.94 | 2.0 | – | – | – | – | – | 0.41 |
< 548.74 | > 552.9 | 282 | 0.65 | pnt | ≤6 | pnt | |
| NGC 978 | < 0.70 | 11.08 | 0.157 | 1.421 | 80.6* | – | (NCC) | WCC | 0.49 |
7.29 | 23.6 | 312 | 0.87 | pnt | ≤3 | gal | |
| NGC 1060 | < 0.78 | 11.42 | 5.6 | 0.132 | 10.4 | 0.6 | CC | SCC | 1.02 ± 0.01 | 11.20 | 41.8 | 468 | 2.97 | jet | 14 | GRP | Merger |
| NGC 1453 | < 0.78 | 11.16 | 0.217 | 0.390 | 64.4 | 1.6 | NCC | SCC | 0.74 ± 0.03 | 14.08 | 40.4 | 392 | 1.74 | pnt | ≤11 | GRP | |
| NGC 1587 | 2.30 ± 0.48 | 11.01 | – | 0.101 | 31.6* | 0.5 | NCC | SCC | 0.37 |
1.22 | 15.3 | 267 | 0.55 | diffuse | 22 | GRP | |
| NGC 4008 | < 0.73 | 10.90 | 0.128 | 0.199 | 16.9* | 0.7 | (NCC) | SCC | 0.56 |
9.98 | 20.5 | 336 | 1.09 | pnt | ≤7 | gal | |
| NGC 4169 | 1.44 ± 0.34 | 10.89 | 4.972 | – | – | – | – | – | 0.71 |
< 744.33 | > 750.0 | 384 | 1.63 | pnt | ≤3 | pnt | |
| NGC 4261 | 0.112 ± 0.005⋆ | 11.05 | 0.034 | 0.097 | 15.0 | 1.2 | CC | SCC | 1.36 |
3.91 | 39.1 | 552 | 4.83 | JET | 80 | GRP | |
| NGC 5846 | 0.14 ± 0.06 | 10.83 | 0.019 | 0.138 | 14.7 | 0.8 | CC | SCC | 0.95 ± 0.01 | 7.07 | 25.6 | 452 | 2.65 | jet | 12 | GRP | Sloshing |
| NGC 6658 | < 0.71 | 10.76 | – | – | – | – | – | – | 0.29 |
< 586.82 | > 591.3 | 233 | 0.36 | – | – | pnt | |
| NGC 7619 | < 0.33 | 11.21 | 0.255 | 0.135 | 24.5 | 0.7 | CC | SCC | 1.00 ± 0.01 | 6.62 | 36.4 | 464 | 2.88 | pnt | ≤6 | GRP | Merger |
| ESO 507-25 | 4.23 ± 0.56 | 10.95 | 0.497 | – | – | – | – | – | – | < 331.42 | > 333.9 | – | – | Diffuse | 11 | – | |
Notes. (1) BGG name. (2) Molecular gas mass from single-dish IRAM and APEX observations (O’Sullivan et al. 2015; O’Sullivan et al. 2018b). ⋆ From ALMA observations (Boizelle et al. 2021). (3) Stellar mass (O’Sullivan et al. 2005; O’Sullivan et al. 2018b). (4) Star formation rate (O’Sullivan et al. 2005; O’Sullivan et al. 2018b). (5) Central cooling time at 10 kpc. (6). min tcool/tff values. Systems where no deprojected profile was available are marked with an asterisk and were calculated at 10 kpc (O’Sullivan et al. 2017). (7) Values of tcool/teddy, where tcool is measure at 10 kpc (O’Sullivan et al. 2017). The eddy turn-over timescale, teddy, has been measured following Olivares et al. (2019). (8) and (9) Type core indicates the classification of groups as cool-core and non-cool-core based on their temperature profiles, and based on the classification of Hudson et al. (2010) as strong (SCC), weak (WCC), and non-cool-core (NCC). Taken from O’Sullivan et al. (2017). Entries in brackets indicate systems where only a projected temperature profile with < 3 bins is available. (10) System temperature O’Sullivan et al. (2017). (11) Entropy measured at 1 kpc based on X-ray profiles from O’Sullivan et al. (2017). (12) Entropy measured at 10 kpc O’Sullivan et al. (2017). (13) R500 refer to the radii at which the cluster mass density is 500 times the critical density of the universe. (14) Total mass within R500. (15) Radio morphology from Kolokythas et al. (2018). The physical scale of the radio emission moves from few kpcs with an (i) point-like (pnt) radio source with sizes ≤11 kpc, (ii) diffuse emission (diffuse) with no clear jet or lobe structure, (iii) small-scale (< 20 kpc) jets (jet) confined within the stellar body of the host galaxy, and (iv) large-scale (> 20 kpc) jets (JET) extending beyond the host galaxy and into the IGrM. (16) The largest linear size (LLS) of the radio source, taken from Kolokythas et al. (2018). (17) X-ray morphology classification and notes from O’Sullivan et al. (2017). For systems where thermal emission was detected, we classified the extent of the gas halo as either group-like (GRP) (extent > 65 kpc), galaxy-like (Gal) (extent ∼10–65 kpc) or point-like (point) (unresolved, extent smaller than the XMM PSF). Although somewhat arbitrary, these classifications give a simple picture of the scale of the emission. (18) X-ray features.
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