The X-ray Universe September 2005, El Escorial, Madrid, Spain Extended Sources in the XMM-Newton slew survey V. Lazaro a, R. Saxton a, A.M.Read c,M.P. Esquej a, M.J. Freyberg b, B. Altieri a,D. Bermejo a V. Lazaro a, R. Saxton a, A.M.Read c,, M.P. Esquej a, M.J. Freyberg b, B. Altieri a,D. Bermejo a a European Space Agency (ESA), European Space Astronomy Centre (ESAC), Villafranca, Apartado 50727, Madrid, Spain b Max-Planck-Institut für extraterrestrische Physik, Giessenbachstrasse 1, Garching, Germany c Dept. of Physics and Astronomy, Leicester University, Leicester LE1 7RH, U.K. Clusters of Galaxies ESACProcessing Introduction The XMM-Newton slew survey project will catalogue of the order of 4000 sources from 15% of the sky, with a limiting flux of about ergs s -1 cm -2 in the keV energy band. About 10% of these sources are reported to be extended by the source detection software. Categories represented are:  Clusters of galaxies  Nearby galaxies  Supernova Remnants Equatorial coordinates of extended sources on the sky The low background and great sensitivity of the EPIC- pn camera on XMM-Newton gives useful limits for the detection of extended sources. This poster attempts to illustrate the potential of the slew survey as a tool for analysing flux-limited samples of clusters of galaxies and other sources of spatially extended X-ray emission. EMASK Detection Mask EBOXDETECT (local mode) Eboxdetect Local Mode Source List ESPLINEMAP Spline Background Map EBOXDETECT (map mode) Eboxdetect Map Mode Source List EMLDETECT Emldetect Source List Exposure Image dmlextmin | extentmodel | ml_id_src | scts | ext | det_ml | ext_ml | bg_map | exp_map | ra | dec | gaussian | 1 | | | | | | | | | beta | 1 | | | | | | | | | gaussian | 1 | | | | | | | | | beta | 1 | | | | | | | | | gaussian | 1 | | | | | | | | | beta | 1 | | | | | | | | | gaussian | 1 | | | | | | | | | beta | 1 | | | | | | | | | gaussian | 1 | | | | | | | | | beta | 1 | | | | | | | | | gaussian | 1 | | | | | | | | | beta | 1 | | | | | | | | | gaussian | 1 | | 0 | | 0 | | | | | gaussian | 2 | | 0 | | 0 | | | | | beta | 1 | | 0 | | 0 | | | | | beta | 2 | | 0 | | 0 | | | | This is the processing schema for source detection. To identify the best parameters to use for detecting extended sources within the slew data, a set of training images, consisting of known extended sources, were identified. The software was run on these images varying the dmlextmin parameter and the extent model. It was found that the actual value of dmlextmin wasn’t important as long as it didn’t exceed 10. Using a beta model generally gave a greater extent size and more counts. An example for the cluster Abell 3581 is shown below. A smoothed slew image of the SNR Puppis-A compared with a 7ks ROSAT HRI observation. The blue circles represent the individual detections made by the source search software, illustrating how difficult it is to automatically parameterise very extended sources. Slew X-ray contours of the VELA SNR overlaid on an optical image X-ray contours of two close SNRs in the Small Magellenic Cloud overlaid on a DSS image Supernova Remnants Cross-correlations with the Abell and Zwicky catalogues show 34 known clusters in the slew survey. These are clearly detected as extended objects even with a 14 second exposure time. For the very brightest examples spectral imaging is possible. As the survey is flux limited the cluster luminosity is limited as a function of red- shift (Fig. 5). We can also look at the relationship between X-ray flux and the optical strength of a cluster (Fig. 6). Abell 3581 An energy coded smoothed image of Abell Red represents soft (0.2-2 keV) photons and blue the hard (2-12 keV) photons. XMM-Slew Comparison of cluster survey areas and depths