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Table 6

Observationally determined slopes of the L − M relation.

Relation Slope Comments Reference
LX1 − M200a 1.61 ± 0.09 106 cluster, ROSAT/ASCA Reiprich02
LX1 − M200a 1.46 ± 0.11 63 cluster, ROSAT/ASCA Reiprich02
Lbol − M200a 1.84 ± 0.09 106 cluster, ROSAT/ASCA Reiprich02
Lbol − M200 1.90 ± 0.49 11 clusters, z = 0.6−1.0 Maughan06
Lbol − M500 1.96 ± 0.10 115 clusters, z = 0.1−1.3 Maughan07
Lbol − M500b 1.63 ± 0.08 Maughan07
LX2 − M500b 1.45 ± 0.07 Maughan07
Lbol − M500 1.03 ± 0.28 13 RCS Clusters, z = 0.6−1.1 Hicks08
Lbol − M500 2.33 ± 0.70 37 clusters, XMM-Newton Zhang08
LX2 − M500 1.61 ± 0.14 17 cluster, Chandra Vikhlinin09
LX1 − MY,500c 1.53 ± 0.10 31 clusters, XMM-Newton Pratt09
Lbol − MY,500c 1.81 ± 0.10 Pratt09
LX1 − MY,500d 1.62 ± 0.11 Pratt09
Lbol − MY,500d 1.90 ± 0.11 Pratt09
LX1 − M500 1.64 ± 0.12 31 clusters, XMM-Newton Arnaud10
LX1 − M500d 1.76 ± 0.13 Arnaud10
Lbol − M500 1.51 ± 0.09 14 literature samples Reichert11

Notes. LX1 is the temperature in the 0.1 to 2.4 keV band, LX2 for the 0.5 to 2 keV band, and Lbol is the bolometric luminosity.

(a)

Quoted is the BCES orthogonal fit.

(b)

Core excised luminosity, r = 0.15−1 × r500.

(c)

MY is the mass estimated from the YX − M relation.

(d)

Corrected for Malmquist bias.

References not listed in Tables 4 and 5 from are: Reiprich & Böhringer (2002), Arnaud et al. (2010).

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