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

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

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

4. 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

5. 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

6. Comparison to ROSAT Aim: find variable sources
ROSAT – X-ray all sky survey (RASS) (done in 1991/92) – soft X-ray: 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

7. 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.

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