Astron. Astrophys. 351, 413-432 (1999)

Appendix

We note down individual clusters with overlays of significance contour plots superposed on the Digitized Sky Survey ⁴ optical images and radial profiles. A significance contour plot is made from an X-ray image smoothed with a Gaussian filter with a of after subtracting the background. The lowest contour levels is . In each radial profile, the solid line and the dashed line respectively represent the result of fitting with standard model and ENF98 model. The dotted line represents the point spread function at the position of each X-ray center.

MS 0015.9+1609 (Cl 0016+16)

One correlation was found between the brightest point source in the HRI field of view and objects cataloged in ROSID: QSO0015+162. As Neumann & Böhringer(1997, henceforth NB97) mentioned, there are two observations for this cluster. Each exposure time was 70 ksec and 2 ksec. NB97 merged two observational data referring the position of the QSO. However, since 1)there is only one source available for the pointing check of 2 dimensional position and 2) 70 ksec exposure time is long enough compared with ksec exposure time, we used only the data of 70 ksec exposure time to avoid systematic error which comes from merging 2 dimensional data referring only one source position. Our result of standard model fitting to HRI data is slightly different from NB97's result of the model fitting to HRI data (but consistent with it within 90% errors) and rather consistent with their results of that of PSPC data. The position of QSO0015+162 on HRI is (, )(J2000). The position of X-ray center on HRI is (, )(J2000)

Fig. 2. The contour plot of MS 0015.9+1609 (Cl 0016+16). The lowest contour is and the step size is .

Fig. 3. The radial profile of MS 0015.9+1609 (Cl 0016+16).

MS 0302.7+1658 (Cl 0302+1658)

One observation was performed for this cluster. No correlation was found between sources higher than 3 in the HRI field of view and objects cataloged in HRASSCAT or ROSID. The position of the X-ray center on HRI is (, 0)(J2000). The position of the X-ray peak is consistent with that of the brightest cluster member galaxy within the HRI pointing accuracy.

Fig. 4. The contour plot of MS 0302.7+1658 (Cl 0302+1658). The step size is .

Fig. 5. The radial profile of MS 0302.7+1658 (Cl 0302+1658).

MS 0353.6-3642 (S 400)

One observation was performed for this cluster. No correlation was found between sources higher than 3 in the HRI field of view and objects cataloged in HRASSCAT or ROSID. This cluster does not show a significant X-ray peak, i.e. the X-ray center, we therefore defined the X-ray center as source count rate weighted mean position of sources around pointing center. The source count rates are calculated by the EXSAS command "DETECT/SOURCES".

Fig. 6. The contour plot of MS 0353.6+3642 (S 400). The step size is .

Fig. 7. The radial profile of MS 0353.6-3642 (S 400).

MS 0451.5+0250 (Abel 520)

One observation was performed for this cluster. No correlation was found between the sources higher than 3 in the HRI field of view and objects cataloged in HRASSCAT or ROSID. This cluster does not show a significant X-ray peak, i.e. the X-ray center, we therefore define the X-ray center as source count rate weighted mean position of sources around pointing center. The source count rates were calculated by the EXSAS command "DETECT/SOURCES".

Fig. 8. The contour plot of MS 0451.5+0250 (Abel 520). The step size is .

Fig. 9. The radial profile of MS 0451.5+0250 (Abel 520).

MS 0735.6+7421 (ZwCl 0735.7+7421)

One observation was performed for this cluster. No correlation was found between sources higher than 3 in the HRI field of view and objects cataloged in HRASSCAT or ROSID. The position of the X-ray center is consistent with that of the brightest cluster member galaxy within the HRI pointing accuracy.

Fig. 10. The contour plot of MS 0735.6+7421 (ZwCl 0735.7+7421). The step size in the contour plot is .

Fig. 11. The radial profile of MS 0735.6+7421 (ZwCl 0735.7+7421).

MS 1006.0+1202 (ZwCl 1006.1+1201)

Three observations were performed for this cluster. Each exposure time was 3 ksec, 20 ksec, and 65 ksec. No correlation was found between sources higher than 3 in the HRI field of view and objects cataloged in HRASSCAT or ROSID. We used only the data of 65 ksec exposure time to avoid systematic error in merging the data without any references because 65 ksec exposure seemed long enough. This cluster does not show a significant X-ray peak, i.e. the X-ray center, we therefore defined the X-ray center as source count rate weighted mean position of sources around pointing center. The source count rates were calculated by the EXSAS command "DETECT/SOURCES".

Fig. 12. The contour plot of MS 1006.0+1202 (ZwCl 1006.1+1201). The step size is .

Fig. 13. The radial profile of MS 1006.0+1202 (ZwCl 1006.1+1201).

MS 1008.1-1224

One observation was performed for this cluster. No correlation was found between sources higher than 3 in the HRI field of view and objects cataloged in HRASSCAT or ROSID. X-ray center (J2000.0) is (, ).

Fig. 14. The contour plot of MS 1008.1-1224. The step size is .

Fig. 15. The radial profile of MS 1008.1-1224.

MS 1224.7+2007

Four observations were performed for this cluster. Each exposure time was 14 ksec, 24 ksec, 5 ksec, and 13 ksec. No correlation was found between sources higher than 3 in the HRI field of view and objects cataloged in both HRASSCAT and ROSID. One, and the only one, cataloged bright point source was available for comparison of pointing accuracy in each image. We therefore used only the data of 24 ksec exposure time which was the longest one among them, to avoid systematic error which came from merging data referring only one source position. X-ray center (J2000.0) is (, 0).

Fig. 16. The contour plot of MS 1224.7+2007. The step size is .

Fig. 17. The radial profile of MS 1224.7+2007.

MS 1333.3+1725

One observation was performed for this cluster. One correlation was found between sources higher than 3 in the HRI field of view and objects cataloged in HRASSCAT and ROSID: QSO1333+177.

As the contour plot and the radial profile show, this object is not a cluster but an X-ray point source. Therefore this object was excluded from the sample.

Fig. 18. The contour plot of MS 1333.3+1725. The step size is .

Fig. 19. The radial profile of MS 1333.3+1725.

MS 1358.4+6245 (ZwCl 1358.1+6245)

Two observations ware performed for this cluster. Each exposure time was 14 ksec and 16 ksec. One correlation was found between sources higher than 3 in the HRI field of view and objects cataloged in HRASSCAT: J135903.4+621239. However, J135903.4+621239 locates near the edge of HRI field of view and was not usable for the reference of the pointing accuracy check. There was also a bright source not cataloged and thus only one point source near the pointing center available for the reference of the pointing accuracy check. Since the exposure times of two observations were comparable to each other and each exposure time is not long enough, we chose the way to merge two files believing that pointing of each observation is completely identical. The difference of position of the point source near the pointing center is in RA and in DEC and therefore we can say that these two positions are identical within the HRI pointing accuracy. Position of the X-ray center on HRI is (, )(J2000). The position of the X-ray center is consistent with that of the brightest cluster member galaxy within the HRI pointing accuracy.

Fig. 20. The contour plot of MS 1358.4+6245 (ZwCl 1358.1+6245). The step size is .

Fig. 21. The radial profile of MS 1358.4+6245 (ZwCl 1358.1+6245)

MS 1455.0-2232 (1E 1455+2232)

Three observations were performed for this cluster. Each exposure time was 4 ksec, 4 ksec, and 7 ksec. No correlation was found between sources higher than 3 in the HRI field of view and objects cataloged in HRASSCAT or ROSID. Since the exposure times of three observations were comparable to each other and each exposure time is not long enough, we chose the way to merge three files believing that the pointing of each observation was completely identical. The position of the X-ray center on HRI is (, )(J2000). The position of the X-ray center is consistent with that of the brightest cluster member galaxy within the HRI pointing accuracy.

Fig. 22. The contour plot of MS 1455.0-2232 (1E 1455+2232). The step size is .

Fig. 23. The radial profile of MS 1455.0-2232 (1E 1455+2232).

MS 1512.4+3647

One observation was performed for this cluster. Two correlations were found between sources higher than 3 in the HRI field of view and objects cataloged in ROSID: QSO1512+370 and HD135657. The position of the X-ray center on HRI is (, )(J2000). The position of the X-ray center is consistent with that of the brightest cluster member galaxy within the HRI pointing accuracy.

Fig. 24. The contour plot of MS 1512.4+3647. The step size is .

Fig. 25. The radial profile of MS 1512.4+3647.

MS 1621.5+2640

One observation was performed for this cluster. No correlation was found between sources higher than 3 in the HRI field of view and objects cataloged in HRASSCAT or ROSID. The HRI image of MS 1621.5+2640 shows double peaks and therefore we defined the X-ray center as the position of the second brightest cluster member galaxy. (First brightest cluster member galaxy locates about away from X-ray center (Ellingson et al. 1997).) This position is near the center of double X-ray peaks. This cluster shows very poor signal-to-noise ratio. Forcing standard model fitting gave unusual values for its best-fit (Morris et al. 1998). We also fit the PSPC data, which has the lower background than HRI , and only to give us unacceptable value same as the case of HRI . PSPC data showed that the position where the tail of radial profile from HRI meets the background was still in the cluster source region on the PSPC image. Therefore model fitting to HRI data is not applicable. This cluster is excluded from the arc statistics.

Fig. 26. The contour plot of MS 1621.5+2640. The step size is .

Fig. 27. The radial profile of MS 1621.5+2640.

MS 1910.5+6736

One observation was performed for this cluster. No correlation was found between sources higher than 3 in the HRI field of view and objects cataloged in HRASSCAT or ROSID. The position of the X-ray center on HRI is (, 0)(J2000).

Fig. 28. The contour plot of MS 1910.5+6736. The step size is .

Fig. 29. The radial profile of MS 1910.5+6736.

MS 2053.7-0449

One observation was performed for this cluster. No correlation was found between sources higher than 3 in the HRI field of view and objects cataloged in HRASSCAT or ROSID.

In spite of 5 ksec pointing, we could have no source photons of MS 2053.7-0449. This indicates the low signal-to-noise ratio of this cluster. We gave the upper limit of the central surface brightness assuming for analytical calculation. This cluster was excluded from our GLA statistics with the ENF98-NFW model and the MSS98-NFW model. For the GLA statistics with Isothermal model, core radius was assumed to be .

Fig. 30. The contour plot of MS 2053.7-0449. The step size is .

MS 2137.3-2353

Two observations were performed for this cluster. Each exposure time was 2 ksec and 14 ksec. No correlation was found between sources higher than 3 in the HRI field of view and objects cataloged in HRASSCAT or ROSID. Since 14 ksec exposure time is long enough comparing with ksec exposure time, we used only the data of 14 ksec exposure time to avoid systematic error which came from merging data with no references. The position of the X-ray center on HRI is (, )(J2000). The position of the X-ray center is consistent with that of the brightest cluster member galaxy within the HRI pointing accuracy.

Fig. 31. The contour plot of MS 2137.3-2353. The step size is .

Fig. 32. The radial profile of MS 2137.3-2353.

© European Southern Observatory (ESO) 1999

Online publication: November 3, 1999
helpdesk.link@springer.de