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Table 3
Comparison of the best fits of the gas-mass fraction, stellar mass fraction, and baryon-mass fraction as a function of the cluster total mass between different samples.
| Sample | Best fit | Intrinsic scatter |
|
|
||
| 19 clusters | fgas,500 = 10 − (0.93 ± 0.32)(M500/ [1014M⊙] ) − (0.03 ± 0.64) | (26 ± 4)% |
| 19 clusters-A2029-A2065 | fgas,500 = 10 − (1.10 ± 0.16)(M500/ [1014M⊙] )0.38 ± 0.36 | (23 ± 17)% |
| 19 clusters and Sun+09 | fgas,500 = 10 − (1.07 ± 0.02)(M500/ [1014M⊙] )0.30 ± 0.07 | (26 ± 8)% |
| Pratt+09 | fgas,500 = 10 − (1.029 ± 0.013)h-1.5(z)(M500/ [2 × 1014M⊙] )(0.21 ± 0.03)h-1.5(z) | (12 ± 2)% |
| Sun+09 (Tier 1 groups + clusters) |
|
– |
| Andreon (2010) | fgas,500 = 10 − (0.97 ± 0.02)(M500/ [1014.5M⊙] )0.15 ± 0.03 | (14 ± 2)% |
|
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| 19 clusters | f∗,500 = 10 − (1.53 ± 0.05)(M500/ [1014M⊙] ) − (0.49 ± 0.09) | (20 ± 4)% |
| 19 clusters-A2029-A2065 | f ∗ ,500 = 10 − (1.56 ± 0.05)(M500/ [1014M⊙] ) − (0.39 ± 0.09) | (15 ± 29)% |
| Lin+03 |
|
– |
| Gonzalez+07 | f ∗ ,500 = 107.57 ± 0.08)M500 − (0.64 ± 0.13) | – |
| Giodini+09 | f∗,500 = (0.050 ± 0.001)(M500/ [5 × 1013M⊙] ) − (0.26 ± 0.09) | 0.35 dex |
| Giodini+09 and Lin+03 | f∗,500 = (0.050 ± 0.001)(M500/ [5 × 1013M⊙] ) − (0.37 ± 0.04) | 0.50 dex |
| Andreon (2010) | f∗,500 ∝ (M500/ [1014.5M⊙] ) − (0.55 ± 0.08) | (41 ± 5)% |
|
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||
| 19 clusters | fb,500 = 10 − (0.73 ± 0.24)(M500/ [1014M⊙] ) − (0.30 ± 0.48) | (45 ± 6)% |
| 19 clusters-A2029-A2065 | fb,500 = 10 − (0.96 ± 0.25)(M500/ [1014M⊙] )0.22 ± 0.57 | (29 ± 14)% |
| Lin+03 |
|
– |
| Giodini+09 | fb,500 = (0.123 ± 0.003)(M500/ [2 × 1014M⊙] )0.09 ± 0.03 | – |
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