Modelling self-similar appearance of galaxy clusters in X-rays

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Volume 539 (March 2012)

A&A, 539 (2012) A120

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Table 5

Observationally determined slopes of the L − T relation.

Relation	Slope	Comments	Reference

L_X1 − T^a	2.02 ± 0.4	35 clusters ROSAT/ASCA	Markevitch98
L_X1 − T^b	2.10 ± 0.24		Markevitch98
L_bol − T^b	2.64 ± 0.27		Markevitch98
L_bol − T	2.88 ± 0.27	24 clusters ROSAT/GINGA	Arnaud99
L_X1 − T^c	2.47 ± 0.14	88 clusters ROSAT/ASCA	Ikebe02
L_bol − T	3.72 ± 0.47	28 clusters, z = 0.4−1.3	Ettori04
L_bol − T	2.78 ± 0.55	11 clusters, z = 0.6−1.0	Maughan06
L_bol − T^f	2.80 ± 0.2	115 clusters, z = 0.1−1.3	Maughan07
L_bol − T	2.35 ± 0.33	70 clusters, z = 0.18−1.24	O’Hara07
L_bol − T^d	2.26 ± 0.33		O’Hara07
L_bol − T	2.90 ± 0.35	27 RCS & CNOC clusters	Hicks08
L_X1 − T^e	2.13 ± 0.32	37 clusters, XMM-Newton	Zhang08
L_bol − T^e	2.61 ± 0.32		Zhang08
L_X1 − T	2.24 ± 0.22	31 clusters, XMM-Newton	Pratt09
L_bol − T	2.70 ± 0.24		Pratt09
L_X1 − T^f	2.32 ± 0.13		Pratt09
L_bol − T^f	2.78 ± 0.13		Pratt09
L_bol − T	2.53 ± 0.15	14 literature samples	Reichert11

Notes. L_X1 is the temperature in the 0.1 to 2.4 keV band, L_X2 for the 0.5 to 2 keV band, and L_bol the bolometric luminosity.

^(a)

For total luminosity.

^(b)

Luminosity and temperature corrected for cool core contribution.

^(c)

Temperature was determined by allowing for an additional cool component not considered in the correlation.

^(d)

Core excised L_X and T with r ≥ 0.2r₅₀₀.

^(e)

Temperatures for r = 0.2−0.5 × r₅₀₀.

^(f)

Core excised L and T with r = 0.15−1 × r₅₀₀.

References not listed in Table 4 from top to bottom are: Markevitch (1998), Arnaud & Evrard (1999), Ikebe et al. (2002), Maughan (2007), Pratt et al. (2009).

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