**Table 4:** Detected sources.
Cluster	RA; Dec	z	$n_{\rm H}$	Radius	HR	Count Rate	$f_{\rm X}$	$f_{\rm bol}$	$L_{\rm bol}$	kT	Refer.	Merger
	(J2000.0)		(10²⁰				(10^-12		(10⁴⁴
	(deg)		${\rm cm}^{-2})$	(arcmin)		$\left( {\rm counts\ s}^{-1}\right)$	${\rm erg\ cm}^{-2}\ {\rm s}^{-1})$		${\rm erg\ s}^{-1})$	(keV)
RX J1252.5-3116	193.143;-31.266	0.0535	5.55	5.8	+0.80	$0.69\pm0.08$	16.09	30.33	1.95	3.8
Abell 1631	193.242;-15.379	0.0462	3.94	9.4	-0.24	$0.15\pm0.01$	3.43	5.65	0.27	2.8	A
Abell 3528	193.640;-29.126	0.0528	6.07	12.24	+0.50	$1.04\pm0.11$	24.32	47.02	2.95	4.0	B	M
Abell 3528N	193.598;-29.010	0.0528	6.07	6.01	+0.70	$0.44\pm0.04$	10.53	18.07	1.13	3.4	B
Abell 3528S	193.673;-29.231	0.0528	6.07	6.33	+0.68	$0.51\pm0.05$	12.20	20.97	1.31	3.1	B
Abell 3530	193.917;-30.367	0.0537	5.75	9.7	+0.42	$0.39\pm0.03$	9.24	16.10	1.04	3.2	C	M
Abell 1644	194.332;-17.381	0.0473	4.05	14.8	+0.49	$1.91\pm0.16$	41.28	89.21	4.45	5.0	D	M
Abell 3532	194.336;-30.375	0.0554	5.84	11.4	+0.45	$0.93\pm0.07$	21.35	43.18	2.99	4.4	A	M
Abell 3535	194.446;-28.536	0.0652	6.49	5.4	+0.11	$0.090\pm0.006$	2.14	2.99	0.21	1.8		M
Abell S0718	194.963;-33.661	0.0478	5.57	3.7	+0.56	$0.060\pm0.006$	1.43	1.89	0.097	1.1
Abell S0721	196.513;-37.642	0.0490	5.13	10.4	+0.09	$0.33\pm0.03$	7.76	12.10	0.65	2.5
Abell S0724	198.286;-32.994	0.0493	4.86	5.0	-0.90	$0.090\pm0.007$	2.05	2.75	0.15	1.3
Abell 3548	198.379;-44.063	0.0000	8.43	6.5	+0.51	$0.17\pm0.02$	4.26	6.08	0.34	1.9
Abell 3553	199.805;-37.179	0.0487	4.73	3.5	+0.33	$0.058\pm0.003$	1.35	1.79	0.095	1.1
Abell 3554	199.865;-33.497	0.0470	4.7	8.5	-0.17	$0.128\pm0.016$	2.91	3.95	0.20	1.5
Abell S0729	200.358;-35.816	0.0499	4.15	2.8	+0.39	$0.055\pm0.008$	1.27	1.67	0.093	1.1
Abell 3556	201.001;-31.656	0.0479	4.07	7.1	-0.20	$0.077\pm0.003$	1.72	3.26	0.17	3.8	E	M
Abell 1736	201.758;-27.153	0.0453	5.38	12.2	+0.38	$1.18\pm0.20$	27.54	50.17	2.27	3.5	D
Abell 3558	202.011;-31.493	0.0480	3.89	13.1	+0.60	$2.72\pm0.11$	57.87	131.0	6.68	5.5	D	M
SC 1327-312	202.514;-31.664	0.0495	3.89	11.4	+0.19	$0.55\pm0.07$	12.25	23.16	1.27	3.8	E	M
SC 1329-314	202.875;-31.812	0.0446	3.87	7.2	+0.25	$0.265\pm0.026$	5.84	11.59	0.52	4.2	E	M
RXJ1332.2-3303	203.109;-33.092	0.0470	4.08	9.6	+0.38	$0.55\pm0.06$	11.90	21.27	1.06	3.0
Abell 3562	203.446;-31.687	0.0490	3.83	14.0	+0.31	$1.35\pm0.11$	29.16	61.73	3.31	4.8	D	M
Abell 3563	203.394;-42.502	0.0000	7.82	5.4	+0.31	$0.130\pm0.013$	3.19	4.41	0.25	1.6
Abell 3570	206.708;-37.874	0.0366	4.47	6.5	+0.11	$0.159\pm0.009$	3.61	4.81	0.13	1.2
Abell 3571	206.860;-32.850	0.0391	3.91	14.0	+0.61	$5.3\pm0.5$	110.9	282.0	9.82	6.9	D
Abell S0758	213.065;-34.314	0.0380	4.78	4.4	+0.13	$0.083\pm0.009$	1.97	2.61	0.082	1.0
B1 $^{{\rm (a)}}$	196.080;-17.001	-	5.26	5.6	+0.32	$0.319\pm0.012$	7.53	11.76	0.66	2.5		M
B2 $^{{\rm (b)}}$	200.977;-14.437	-	4.56	5.2	+0.40	$0.40\pm0.03$	9.27	15.07	0.84	2.7
B3 $^{{\rm (b)}}$	208.265;-18.299	-	7.67	5.5	+0.33	$0.078\pm0.007$	1.91	2.55	0.14	1.3
B4 $^{{\rm (a)}}$	190.088;-23.131	-	6.53	3.2	+0.39	$0.075\pm0.007$	1.79	2.39	0.13	1.3		M
B5 $^{{\rm (a)}}$	195.215;-21.608	-	7.59	6.6	+0.15	$0.078\pm0.012$	1.91	2.55	0.14	1.3		M
B6 $^{{\rm (a)}}$	194.795;-21.911	-	7.49	5.6	+0.28	$0.150\pm0.008$	3.66	5.14	0.29	1.8
B7 $^{{\rm (c)}}$	203.839;-29.862	-	4.02	6.9	+0.13	$0.29\pm0.04$	6.63	10.12	0.57	2.3
B8 $^{{\rm (b)}}$	196.085;-30.593	-	5.73	8.8	+0.38	$0.209\pm0.009$	4.94	7.21	0.40	2.0		M
B9 $^{{\rm (c)}}$	213.224;-31.277	-	4.14	5.6	+0.16	$0.139\pm0.015$	3.12	4.30	0.24	1.6
B10 $^{{\rm (b)}}$	195.548;-38.760	-	6.89	4.8	+0.11	$0.073\pm0.008$	1.76	2.34	0.13	1.2
B11 $^{{\rm (c)}}$	198.339;-44.591	-	6.74	5.6	+0.17	$0.09\pm0.01$	2.15	2.89	0.16	1.4
B12 $^{{\rm (c)}}$	196.136;-43.868	-	8.32	7.0	+0.44	$0.22\pm0.02$	5.55	8.22	0.46	2.1
B13 $^{{\rm (c)}}$	195.338;-43.902	-	7.64	6.4	+0.31	$0.087\pm0.006$	2.13	2.85	0.16	1.4
B14 $^{{\rm (b)}}$	195.582;-44.535	-	7.29	4.8	+0.24	$0.081\pm0.009$	1.97	2.63	0.15	1.3

Column (1): source name. The last 14 sources labeled with B followed by increasing identification numbers are the new X-ray detections. (a) Confirmed cluster. (b) Possible cluster. (c) Non cluster source. Column (2): RA and Dec (J2000). Column (3): redshift. Column (4); Galactic HI column density in units of $10^{20}\ {\rm cm}^{-2}$ (Dickey & Lockman 1990). Column (5): source radius (arcmin). Column (6): hardness ratio. Column (7): source count rate in the $0.5{-}2.0\ {\rm keV}$ energy band and its error. Columns (8)-(9): $f_{\rm X}$ in the $0.1{-}2.4\ {\rm keV}$ energy band and the bolometric flux, both in units of $10^{-12}\ {\rm erg\ cm}^{-2}\ {\rm s}^{-1}$ . Column (10): bolometric luminosity in units of $10^{44}\ {\rm erg\ s}^{-1}$ ; for the new X-ray detections a redshift z=0.05 has been assumed. Column (11): cluster average temperature in keV. Column (12): literature reference for the cluster temperature: A (Wu et al. 1999), B (Schindler 1996), C (Ettori et al. 1997), D (Markevitch 1998), E (Hanami et al. 1999). Column (13): flag for clusters showing signatures of merger.

Source LaTeX | All tables | In the text

	1 Introduction
	2 The Shapley super-cluster
	3 A complete X-ray analysis of the Shapley area
	4 The detection algorithm
	5 Cluster detection
	6 Clusters detected in the Shapley region
	7 New X-ray detections
	8 Cluster number density
	9 The X-ray luminosity function
	10 The cumulative mass profile
	11 Results and discussion
	References
	Online Material
	Appendix A: Optical properties of B1, B4-B9 and B11-B14