Скачать презентацию Supersoft sources in M 31 Comparing the XMM-Newton Скачать презентацию Supersoft sources in M 31 Comparing the XMM-Newton

dec62f1b53654878499c37647758c39d.ppt

  • Количество слайдов: 24

Supersoft sources in M 31: Comparing the XMM-Newton Deep Survey, ROSAT and Chandra catalogues Supersoft sources in M 31: Comparing the XMM-Newton Deep Survey, ROSAT and Chandra catalogues Holger Stiele Super. Soft X-ray Sources – New Developments ESAC 20. May. 2009 Madrid 20. 05. 2009 Holger Stiele

The Large Program Collaboration 19 scientists from 7 countries • PI: W. Pietsch (MPE) The Large Program Collaboration 19 scientists from 7 countries • 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) 20. May. 2009 Holger Stiele 2

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

Image • of Deep survey (“outer ring”) and archival (“major axis”) data (see Pietsch Image • 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 ke. V • 20. May. 2009 Holger Stiele 1 – 2 ke. V 2 – 12 ke. V SSSs; fgstars + SNRs; hard (AGNs, XRBs, Crab like SNR) Extended sources mostly background galaxy clusters 4

Hardness Ratios = X-ray colour i= 1… 4 SSS HR 2 versus HR 1 Hardness Ratios = X-ray colour i= 1… 4 SSS HR 2 versus HR 1 separate SSS; thermal SNRs and fg stars B 1: 0. 2 -0. 5 ke. V B 2: 0. 5 -1. 0 ke. V B 3: 1. 0 -2. 0 ke. V B 4: 2. 0 -4. 5 ke. V B 5: 4. 5 - 12 ke. V Further classification methods: • Extent Yfg star XRB + AGN SSS Gal/Gl. C SNR • Time variability • Cross correlations with optical and radio source catalogues 20. May. 2009 Holger Stiele 5

X-ray Sources in M 31 Field: Identification and Classification identified • • SSS SNR X-ray Sources in M 31 Field: Identification and Classification identified • • SSS SNR Globular clusters XRB • • • foreground stars AGN Galaxies Galaxy clusters Hard Without 20. May. 2009 25 36 10 22 3 4 1 + Holger Stiele classified 43 38 17 22 243 49 21 1 1289 127 1951 6

Supersoft Sources • Definition: – Radiation with effective temperature of 10 to 100 e. Supersoft Sources • Definition: – Radiation with effective temperature of 10 to 100 e. V – Luminosities: ~1036 -39 erg s-1 • HR 1 < 0 and HR 2 - EHR 2 < -0. 96 or HR 2 not defined, HR 3, HR 4 not defined • 43 SSSs, 27 “new” 20. May. 2009 Holger Stiele 7

Flux Distribution Blackbody “model” with Tbb = 50 e. V NH = 6. 6 Flux Distribution Blackbody “model” with Tbb = 50 e. V NH = 6. 6 1020 cm-2 Period 217 s Number of sources Unabs. fluxes Novae Trudolyubov & Priedhorsky 2008 M 31 N 2001 -11 a M 31 N 2005 -01 c erg cm-2 s-1 M 31 N 2007 -06 b Period 865. 5 s (Nova? ) Osborne et al. 2001 20. May. 2009 7. 3 1036 erg/s Holger Stiele 8

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

Optical Novae (II) M 31 N a. opt. det. Not vis. Distance 1994 -09 Optical Novae (II) M 31 N a. opt. det. Not vis. Distance 1994 -09 a 2591 d 3583 d 3. 1” 1. 6 1036 1995 -11 c 1486 d --- 2. 1” 1. 68 1037 1996 -08 b 1880 d --- 1. 1” 5. 6 1036 1997 -08 b 1589 d 2514 d 2. 3” 0. 7 1036 1997 -10 c 982 d 1167 d 1. 9” 1998 -06 a 1119 d 2235 d 1. 1” 1. 7 1036 1999 -10 a 1751 d --- 1. 6” 2. 12 1037 2000 -07 a 170 d --- 1. 3” 1. 35 1037 2001 -10 f 84 d 1009 d 0. 9” 3. 7 1037 2001 -11 a 53 d --- 0. 5” 2005 -01 b 535 d 1073 d 4. 3” 45 1. 0 1037 2005 -01 c 703 d --- 0. 9” 40. 23 1. 2 1038 2005 -09 b 299 d 690 d 0. 57” 35 5. 4 1038 2007 -06 b 20. May. 2009 See talk of M. Henze Holger Stiele Tbb (e. V) 41 LX (erg/s) 5. 9 1037 Smirnova et al. 2006 Pietsch et al. 2007 10

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

ROSAT PSPC Survey • PSPC survey covering the entire galaxy twice 560 X-ray sources 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 ke. V, and ~ 1 ke. V – ROSAT observations taken about > 10 yr earlier than XMM-Newton observations ( investigation of long term variability) 20. May. 2009 Holger Stiele 12

Chandra Observations • Observation of selected fields, especially central region • Kong et al. 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, Voss & Gilfanov 2007 Very soft sources Di Stefano et al. 2004 – Three energy bands: S: 0. 1 -1. 1 ke. V; M: 1. 1 -2 ke. V; H: 2 -7 ke. V Several criteria to select SSSs and QSSs – Important difference: Only one band below ~1 ke. V Contamination of SSS class with foreground stars, SNRs and soft AGNs – Temporal distance to XMMNewton observations: centre and Field 2: < 1 yr Fields 1+3: > ~ 4 yr Image: Di Stefano et al. 2004 20. May. 2009 Holger Stiele 13

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

XMM-Newton SSS to ROSAT PSPC Surveys • 43 XMM-Newton SSS, 12 brighter than ROSAT 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) 20. May. 2009 Holger Stiele 15

XMM-Newton SSS to Chandra Surveys • 9 XMM-Newton SSSs have Chandra counterparts: – 6 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 M 31 N 1999 -10 c, M 31 N 2001 -11 a)) – 1 variable 20. May. 2009 Holger Stiele 16

ROSAT SSSs to XMM-Newton Deep Survey • 34 ROSAT SSS, 4 not in observed ROSAT SSSs to XMM-Newton Deep Survey • 34 ROSAT SSS, 4 not in observed XMM-Newton field • 14 correlations with XMM-Newton sources • 3 SSS confirmed with XMM-Newton 5 Fg Star cand 1 Fg Star 1 SNR 1 Galaxy 2 1 No class. (2 XMM) most of these sources not highly variable (fvar < 5) • 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) 20. May. 2009 Holger Stiele 17

Chandra VSSs to XMMNewton Deep Survey • 20 Chandra SSSs – 15 correlations with Chandra VSSs to XMMNewton Deep Survey • 20 Chandra SSSs – 15 correlations with XMM-Newton sources: 5 Confirmed SSSs 2 Fg Star cand. 3 Confirmed fg Stars 1 SNR cand. 2 Confirmed SNRs 2 XRB cnad. – 5 not detected with XMM-Newton (4 transients (Di Stefano et al. 2004, 2 of them novae), 1 faint) 20. May. 2009 Holger Stiele 18

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

What do we learn? • 3 sources detected in all 3 missions visible for What do we learn? • 3 sources detected in all 3 missions visible for more than a decade: – Two are located in the central field: • XMMM 31 J 004318. 8+412017 = r 3 -8 = [SHL 2001] 235: foreground polar? (Williams et al. 2006) • XMMM 31 J 004252. 5+411540 = r 2 -12 = [SHL 2001] 203 = [PFJ 93] 58 = [TF 91] 69: 217 s period (Trudolyubov et al. 2008) – XMMM 31 J 003840. 5+401956 = s 2 -26 = [SHL 2001] 27: r 3 -8 r 2 -12 s 2 -26 20. May. 2009 ROSAT: ~22 -25 brighter XMM: June 2006 – Jan. 2008 in 3 Chandra observations (2000 -2001) only once visible variable (Di Stefano et al. 2004) Holger Stiele ROSAT Chandra XMMNewton 20

What do we learn? (II) • Of 12 XMM-Newton sources with brightness above ROSAT 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 20. May. 2009 Holger Stiele 21

What do we learn? (III) • Two interesting sources: – XMMM 31 J 004307. What do we learn? (III) • Two interesting sources: – XMMM 31 J 004307. 1+411810 = r 3 -115: Chandra and XMM-Newton observations between 2000 -end 2001: SSS XMM-Newton observation Jan. 2002: hard spectrum (Pietsch et al. 2005) – XMMM 31 J 004247. 9+411549 = r 1 -25: Chandra r 3 -115 r 1 -25 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 20. May. 2009 Holger Stiele 22

Summary 1. Deep XMM-Newton survey of M 31 1951 X-ray sources, 43 Supersoft sources Summary 1. Deep XMM-Newton survey of M 31 1951 X-ray sources, 43 Supersoft sources 2. Optical novae are an important class of SSSs in M 31 (5 in addition to Pietsch et al. 2005, 2007) 3. Correlation with ROSAT PSPC surveys and Chandra catalogues 4. 3 persistent SSSs 5. SSSs are a highly variable source class 6. Many ROSAT and Chandra SSSs get other classes from XMM-Newton observations 7. Two sources that show supersoft-hard transition between Chandra and XMM-Newton observations 20. May. 2009 Holger Stiele 23

The large program collaboration: • PI: W. Pietsch (MPE) • MPE: V. Burwitz, M. 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) 20. May. 2009 Holger Stiele 24