1. Supersoft sources in M 31: Comparing the XMM-Newton Deep Survey, ROSAT and Chandra catalogues Holger Stiele SuperSoft X-ray Sources – New Developments ESAC Madrid 20.05.2009

2. 20. May. 2009Holger Stiele2 The Large Program Collaboration PI: W.Pietsch (MPE) MPE: V. Burwitz, M. Freyberg, J. Greiner, F. Haberl, H. Stiele And: R. Barnard (The Open University), D. Hatzidimitriou (University of Crete), M. Hernanz (CSIC-IEEC), G. Israel (INAF), U. Kolb (The Open University), A. Kong (National Tsing Hua University), P. Plucinsky (Harvard-Smithsonian Centre for Astrophysics), P. Reig (IESL), G. Sala (UPC/IEEC), M. Sasaki (Harvard-Smithsonian Centre for Astrophysics), L. Shaw Greening (The Open University), L. Stella (INAF), B. Williams (Pennsylvania State University) 19 scientists from 7 countries

3. 20. May. 2009Holger Stiele3Outline The XMM-Newton Deep Survey catalogue  Supersoft sources optical novae Comparing the XMM-Newton Deep Survey, ROSAT and Chandra catalogues  The catalogues  The method  The results

4. 20. May. 2009Holger Stiele4Image of Deep survey (“outer ring”) and archival (“major axis”) data ( see Pietsch et al. 2005 ) Fields with high background repeated Optical extent indicated by D 25 ellipse 0.2 – 1 keV 1 – 2 keV 2 – 12 keV SSSs; fgstars + SNRs; hard (AGNs,XRBs,Crab like SNR) Extended sources  mostly background galaxy clusters

5. 20. May. 2009Holger Stiele5 Hardness Ratios i= 1…4 B1: 0.2-0.5 keV B2: 0.5-1.0 keV B3: 1.0-2.0 keV B4: 2.0-4.5 keV B5: 4.5- 12 keV  fg star + AGN  Gal/GlC = X-ray colour  XRB  SSS  SNR Extent Time variability Cross correlations with optical and radio source catalogues Further classification methods: HR2 versus HR1  separate SSS; thermal SNRs and fg stars SSS

6. 20. May. 2009Holger Stiele6 X-ray Sources in M 31 Field: Identification and Classification identified classified SSS 43 SNR 25 38 Globular clusters 36 17 XRB10 22 foreground stars22243 AGN 3 49 Galaxies 4 21 Galaxy clusters 1 1 Hard 1289 Without127  1951 + SSS 43

7. 20. May. 2009Holger Stiele7 Supersoft Sources Definition: –Radiation with effective temperature of 10 to 100 eV –Luminosities: ~10 36-39 erg s -1 HR1 < 0 and HR2 - EHR2 < -0.96 or HR2 not defined, HR3, HR4 not defined 43 SSSs, 27 “new”

8. 20. May. 2009Holger Stiele8 Flux Distribution Period 217s Trudolyubov & Priedhorsky 2008 Period 865.5s (Nova?) Osborne et al. 2001 M31N2007-06b M31N2005-01c 7.3  10 36 erg/s Blackbody “model” with T bb = 50 eV N H = 6.6  10 20 cm -2 Unabs. fluxes erg cm -2 s -1 Number of sources M31N 2001-11a Novae

9. 20. May. 2009Holger Stiele9 Optical Novae Major class of SSSs in centre of M 31: optical novae ( Pietsch et al. 2005, 2007 ) Outer regions: not deep enough optical and no X- ray monitoring for novae/SSSs  only snapshots (X-rays)  only random detections  difficult to determine general properties of disk nova population 2005-01b 1997-10c 2005-09b 2005-01c 2007-06b 1997-10c SSSs Novae

10. 20. May. 2009Holger Stiele10 Optical Novae (II) M31Na. opt.det.Not vis.DistanceT bb (eV)L X (erg/s) 1994-09a2591 d3583 d3.1” 1.6  10 36 1995-11c1486 d---2.1” 1.68  10 37 1996-08b1880 d---1.1” 5.6  10 36 1997-08b1589 d2514 d2.3” 0.7  10 36 1997-10c982 d1167 d1.9”  415.9  10 37 1998-06a1119 d2235 d1.1” 1.7  10 36 1999-10a1751 d---1.6” 2.12  10 37 2000-07a170 d---1.3” 1.35  10 37 2001-10f84 d1009 d0.9” 3.7  10 37 2001-11a53 d---0.5”Smirnova et al. 2006 2005-01b535 d1073 d4.3”  451.0  10 37 2005-01c703 d---0.9”  40.231.2  10 38 2005-09b299 d690 d0.57” 2007-06b  See talk of M. Henze Pietsch et al. 2007  355.4  10 38

11. 20. May. 2009Holger Stiele11 Comparing the XMM- Newton Deep Survey, ROSAT and Chandra catalogues XMM-Newton Deep Survey 1951 sources 43 Supersoft sources

12. 20. May. 2009Holger Stiele12 ROSAT PSPC Survey PSPC survey covering the entire galaxy twice  560 X-ray sources Supper et al. 1997, 2001 Supersoft sources selected from Greiner 2000 and Kahabka 1999 : –Similar selection criterion (as used for XMM-Newton) –Two hardness ratios (based on standard ROSAT energy bands) –band separation energies at ~ 0.5 keV, and ~ 1 keV –ROSAT observations taken about > 10 yr earlier than XMM-Newton observations (  investigation of long term variability)

13. 20. May. 2009Holger Stiele13 Chandra Observations Observation of selected fields, especially central region Kong et al. 2002, Kaaret 2002, Di Stefano et al. 2004, Williams et al. 2004, 2006, Very soft sources Di Stefano et al. 2004 –Three energy bands: S: 0.1-1.1 keV; M: 1.1-2 keV; H: 2-7 keV  Several criteria to select SSSs and QSSs – Important difference:  Contamination of SSS class with – Temporal distance to XMM- Only one band below ~1 keV foreground stars, SNRs and soft AGNs Newton observations: centre and Field 2: ~ 4yr Image: Di Stefano et al. 2004 Voss & Gilfanov 2007

14. 20. May. 2009Holger Stiele14Method Two step process: First step: Were the XMM-Newton SSSs detected in previous surveys? XMM – Newton SSS Full ROSAT PSPC Full Chandra Second step: How many ROSAT/Chandra SSSs are detected with XMM-Newton? ROSAT SSS Chandra VSS Full XMM Deep Survey

15. 20. May. 2009Holger Stiele15 XMM-Newton SSS to ROSAT PSPC Surveys 43 XMM-Newton SSS, 12 brighter than ROSAT detection threshold (~5.3  10 -15 erg cm -2 s -1 ): –2 also found as ROSAT SSSs –10 not detected with ROSAT: 6 recent novae, 1 transient, 1 variable  2 must be transient/highly variable 31 XMM-Newton SSS with fluxes below ROSAT detection threshold: –1 also found as ROSAT SSSs (~factor 22-25 brighter in ROSAT observations) –3 chance coincidences –27 remaining sources: 7 recent novae, 1 transient ( Di Stefano et al. 2004 )

16. 20. May. 2009Holger Stiele16 XMM-Newton SSS to Chandra Surveys 9 XMM-Newton SSSs have Chandra counterparts: –6 are also classified as SSSs from Chandra –8 of the 9 sources are located in the centre of M 31 34 sources do not have Chandra counterparts: –7 are in regions not covered with Chandra –10 are novae (4 after 2005, 6 no Chandra detections ( see Pietsch et al. 2005, 2007 and M31N1999-10c, M31N2001-11a )) –1 variable

17. 20. May. 2009Holger Stiele17 ROSAT SSSs to XMM-Newton Deep Survey 34 ROSAT SSS, 4 not in observed XMM-Newton field 14 correlations with XMM-Newton sources 16 ROSAT SSS without XMM-Newton counterparts: 1 nova  Where are the novae? No systematic search/monitoring campaign in the years before 1990  number of known optical novae very low (see talk of W. Pietsch) 3SSS confirmed with XMM-Newton 5Fg Star cand1Fg Star 1SNR1Galaxy 2 1No class. ( 2 XMM ) most of these sources not highly variable (fvar < 5)

18. 20. May. 2009Holger Stiele18 Chandra VSSs to XMM- Newton Deep Survey 20 Chandra SSSs –15 correlations with XMM-Newton sources: –5 not detected with XMM-Newton (4 transients ( Di Stefano et al. 2004, 2 of them novae), 1 faint) 5Confirmed SSSs2Fg Star cand. 3Confirmed fg Stars1SNR cand. 2Confirmed SNRs2XRB cnad.

19. 20. May. 2009Holger Stiele19 Chandra VSSs to XMM- Newton Deep Survey 23 Chandra QSSs –12 correlations with XMM-Newton sources: –11 not detected with XMM-Newton (1 outside XMM field, 5 transients ( Di Stefano et al. 2004 ), 1 in crowded centre, 2 faint) 3Confirmed fg Stars 3Fg Star cand.1Fg Star 1Bg Gal cand.2 2No class.

20. 20. May. 2009Holger Stiele20 What do we learn? 3 sources detected in all 3 missions  visible for more than a decade: – Two are located in the central field: XMMM31 J004318.8+412017 = r3-8 = [SHL2001] 235: foreground polar? ( Williams et al. 2006 ) XMMM31 J004252.5+411540 = r2-12 = [SHL2001] 203 = [PFJ93] 58 = [TF91] 69: 217s period ( Trudolyubov et al. 2008 ) – XMMM31 J003840.5+401956 = s2-26 = [SHL2001] 27: r2-12 r3-8 s2-26 ROSAT: ~22-25  brighter XMM: June 2006 – Jan. 2008 in 3 Chandra observations (2000-2001) only once visible  variable ( Di Stefano et al. 2004 ) ROSAT Chandra XMM- Newton

21. 20. May. 2009Holger Stiele21 What do we learn? (II) Of 12 XMM-Newton sources with brightness above ROSAT threshold, only 2 observed by ROSAT  underlines variability of the source class on long time scales (~83% variable, cf. Greiner et al. 2004 ) ROSAT as well as Chandra SSSs contain sources of other classes

22. 20. May. 2009Holger Stiele22 What do we learn? (III) Two interesting sources: –XMMM31 J004307.1+411810 = r3-115: Chandra and XMM-Newton observations between 2000-end 2001: SSS XMM-Newton observation Jan. 2002: hard spectrum ( Pietsch et al. 2005 ) –XMMM31 J004247.9+411549 = r1-25: Chandra observations between 2000-end 2001: SSS XMM-Newton observation July 2004: hard spectrum optical counterpart within 1.2” (‘regular or semi-regular red variable’ Fliri et al. 2006 )  Nature unclear: X-ray transient (BH primary) or symbiotic r1-25 r3-115

23. 20. May. 2009Holger Stiele23Summary Deep XMM-Newton survey of M 31  1951 X-ray sources, 43 Supersoft sources Optical novae are an important class of SSSs in M 31 (5 in addition to Pietsch et al. 2005, 2007 ) Correlation with ROSAT PSPC surveys and Chandra catalogues 3 persistent SSSs SSSs are a highly variable source class Many ROSAT and Chandra SSSs get other classes from XMM-Newton observations Two sources that show supersoft-hard transition between Chandra and XMM-Newton observations

24. 20. May. 2009Holger Stiele24 The large program collaboration: PI: W.Pietsch (MPE) MPE: V. Burwitz, M. Freyberg, J. Greiner, F. Haberl, H. Stiele And: R. Barnard (The Open University), D. Hatzidimitriou (University of Crete), M. Hernanz (CSIC-IEEC), G. Israel (INAF), U. Kolb (The Open University), A. Kong (National Tsing Hua University), P. Plucinsky (Harvard-Smithsonian Centre for Astrophysics), P. Reig (IESL), G. Sala (UPC/IEEC), M. Sasaki (Harvard-Smithsonian Centre for Astrophysics), L. Shaw Greening (The Open University), L. Stella (INAF), B. Williams (Pennsylvania State University)