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Table 1.

Sample: ALMA and MUSE data used in our analysis.

Cluster ID BCG ID ALMA ID project z CO(1-0) CO(2-1) CO(3-2) MUSE
(1) (2) (3) (4) (5) (6)
New ALMA observations
Centaurus NGC4696 2015.1.01198.S 0.01016 ... ...
RXJ1539.5−8335 2MASXJ15393387−8335215 2015.1.01198.S 0.07576 ... ...
Abell S1101 ESO 291−G009 2015.1.01198.S 0.05639 ... ...

ALMA archive
PKS 0745−191 PKS 0745−191 2012.1.00837.S 0.10280 ...
Abell 1664 2MASXJ13034252−2414428 2011.0.00374.S 0.12797 ... ...
Abell 1835 2MASXJ14010204+0252423 2011.0.00374.S 0.25200 ... ...
Abell 2597 PKS 2322−12 2012.1.00988.S 0.08210 ... ...
M 87 M 87 2013.1.00862.S 0.00436 ... ... ...
Abell 1795 Abell 1795 2015.1.00623.S 0.06326 ... ...
Phoenix-A SPT-CLJ2344-4243 2013.1.01302.S 0.59600 ... ... ...
RXJ0820.9+0752 2MASXJ08210226+0751479 2016.1.01269.S 0.10900 ...
2A0335+096 2MASXJ03384056+0958119 2012.1.00837.S 0.03634 ...
Abell 3581 IC4374 2015.1.00644.S 0.02180 ... ...
Abell 262 NGC 708 2015.1.00598.S 0.01619 ... ... ...
Hydra-A Hydra-A 2016.1.01214.S 0.05435 ... ...

Notes. (1) Source name, the actual target studied in this paper is the central brightest cluster galaxy of the cluster. (2) Central brightest cluster galaxy name. (3) ALMA project ID of the observations analyzed. (4) The redshifts z of the BCGs which were derived from optical features (stellar absorption lines). (5) The lines observed with ALMA used in our study. (6) The availability of MUSE data for each source.

References. Centaurus from Postman & Lauer (1995); RXJ1539.5−8335 from Huchra et al. (2012); Abell S1101 from da Costa et al. (1991); PKS 0745−191 from Russell et al. (2016); Abell 1664 from Pimbblet et al. (2006); Abell 1835 from Crawford et al. (1999); Abell 2597 from Tremblay et al. (2016); M 87 from Simionescu et al. (2018); Abell 1795 from Russell et al. (2017b); Phoenix-A from Russell et al. (2016); RXJ0820.9+0752 from Crawford et al. (1995); 2A0335+096 from McNamara et al. (1990); Abell 3581 from Canning et al. (2013); Hydra from Rose et al. (2019).

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