XMM-Newton slew sources A quick analysis Refiz Duro ESAC, Madrid 2009

Find new variable sources Aims Find new variable sources Quick, automatic analysis of slew data with results provided to the user

Agenda XMM-Newton slew data description Comparison to ROSAT data Results Conclusion

Slew data Slews: images taken while the telescope is changing its position from one pointed observation to the next Slew speed of 90 deg/hour EPIC-pn data Shallow survey of the sky. Image properties: 0.2 – 2.0 keV (soft energy band) Median exposure time: ~6.2 seconds (min ~ 1s, max~12s) Images roughly 1 degree by 0.5 degree

Source searching SAS (Science Analysis Software) tasks: eslewchain (create images, exposure maps) emask (area for source searching) eboxdetect (source searching) esplinemap (constructs background map) emldetect (info on the sources) Tables with the sources and their properties More details in Saxton et al. 2008

Comparison to ROSAT Aim: find variable sources ROSAT – X-ray all sky survey (RASS) (done in 1991/92) – soft X-ray: 0.2-2.4 keV Bright, faint & point source catalogues Expected factor of difference between XMM-Newton and ROSAT fluxes for a non-variable source is 6.4 (Spectral model of an absorbed power-law with slope 2.4 and NH=3*10^20cm^(-2)) Larger/smaller factors suggest a variable source

Results Table 1: XMM-Newton sources compared to ROSAT source counterparts. Table 2: Upper limits table. Sources which were expected to be found in the slew images based on the coordinates from RASS, but which were not detected in the analysis.

Conclusion Quickly analyzed X-ray slew data Results presented on the web New variable sources