Table 4.
Dark matter halo mass results for all groups.
Structure | σOD(a) | M*, max(b) | Total M* | Mh(2a) | Mh(3) | Mh(4) | Mh best (c) | Rvir(d) | Mh(1) | Mh(2b) | Mh(5) |
---|---|---|---|---|---|---|---|---|---|---|---|
[1011 M⊙] | [1011 M⊙] | log M⊙ | log M⊙ | log M⊙ | log M⊙ | [pkpc] | log M⊙ | log M⊙ | log M⊙ | ||
HPC1001 | 7.7 | 1.0 ± 0.2 | 2.4 ± 0.2 | ![]() |
![]() |
![]() |
13.3 ± 0.3 | 181 ± 42 | > 12.8 | 12.8 ± 0.3 | ![]() |
COS-SBCX3 | 6.0 | 0.5 ± 0.1 | 1 ± 0.1 | ![]() |
![]() |
![]() |
12.8 ± 0.3 | 141 ± 33 | ![]() |
12.2 ± 0.4 | ![]() |
COS-SBCX4 | 6.0 | 1.6 ± 0.4 | 4.4 ± 0.6 | ![]() |
![]() |
![]() |
13.3 ± 0.3 | 229 ± 53 | > 13.1 | 13.2 ± 0.3 | ![]() |
COS-SBCX1 | 7.0 | 2.5 ± 0.6 | 8.6 ± 0.6 | > 13.6 | ![]() |
![]() |
13.7 ± 0.3 | 331 ± 70 | > 13.8 | 13.7 ± 0.2 | ![]() |
COS-SBCX7 | 5.6 | 1.3 ± 0.3 | 4.5 ± 0.6 | ![]() |
![]() |
![]() |
13.6 ± 0.3 | 308 ± 71 | ![]() |
13.3 ± 0.2 | ![]() |
COS-SBC3 | 4.6 | 3.2 ± 0.7 | 5.2 ± 0.7 | ![]() |
![]() |
![]() |
13.7 ± 0.3 | 337 ± 71 | > 14.1 | 13.3 ± 0.2 | ![]() |
COS-SBC6 | 4.6 | 1.3 ± 0.3 | 2.5 ± 0.2 | ![]() |
![]() |
![]() |
13.4 ± 0.3 | 271 ± 57 | ![]() |
12.9 ± 0.3 | ![]() |
COS-SBC4 | 7.4 | 1.6 ± 0.6 | 7.9 ± 0.4 | > 13.5 | ![]() |
![]() |
13.7 ± 0.3 | 429 ± 90 | > 13.0 | 13.8 ± 0.2 | ![]() |
Notes. Lower limits are at 1σ significance.
M*, max is the stellar mass of the most massive central spectroscopically confirmed member galaxy.
The best estimate halo mass is the average of Mh(2a), Mh(3), and Mh(4), and the uncertainty is estimated by the average scatter between the methods (Fig. 3).
Virial radius of Mh Best, using the Mh − Rvir relation from Goerdt et al. (2010).
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