1. ULXs @ non-X-ray wavelengths Manfred Pakull 0bservatoire Astronomique de Strasbourg coll: Roberto Soria, Christian Motch, Fabien Grisé ULX and Middle Weight Black Holes, May 24-26, ESAC, Spain

2. Outline -- Ultraluminous X-ray sources proper -- ULXs and stellar environment -- ULX feedback: photoionisation -- ULX feedback: shocks; wind/jet inflated ULX bubbles -- Rosetta Stone S26 in NGC 7793 -- ULXBs = jet inflated « beambags » like SS433/W50

3. NGC1313 X-2 (Thesis Grisé) ‏ VLT/FORS1 : H ,V,B HST/ACS : F814W,F555W, F435W 5“ N E N E 10“

4. Color-magnitude diagrams of the stars around NGC 1313 X-2 Counterpart Mv ~ -4.5 (Grisé et al) Cluster age: Ramsey et al 2006: > 10 MyrsE(B-V) = 0 Liu et al 2007< 10 Myrs= 0.33 Grisé et al 2008 20 Myrs= 0.10

5. Optical Spectrum of X-2 Pakull et al 2006 HeII λ 4686  RV( 4686) ~ 300 km/s, if disk emission -> no IMBH !

6. Photometry of N1313 X-2 Liu et al 2009: Periodic (?) variation with P= 6 days Not confirmed by ground-based photom (Grisé et al. 2009) ‏

7. Holy grail Measure orbital period and radial velocity curve(s) ‏ of ULX (and companion) ‏ Determine masses: stellar BHs or IMBH ? We are close ! (c.f. C. Motch et al.; T. Roberts et al. this conf.) ‏

8. Feedback I. X-ray photoionization

9. X-ray ionized nebula: XIN Halpern & Grindlay 1980 Kallman & McCray 1982 Different frm HII regions: no sharp Stroemgren spheres; ‘warm’ neutrals  strong [OI], [SII] ‘warm’ He++ zone:  HeII 4686 emission ‘Te ~10 4 K; line width < 20 km/s

10. Holmberg II ULX 2 nd XIN after LMC X-1 (Pakull & Angebault 1989) nebular HeII 4686 emission at the position of the ULX (Pakull & Mirioni 2002) ‏ Zanstra He+ LyC photon counting L HeII 4686  L X nebula indeed “sees” L X ~ 10 40 erg/s -> no beaming here ! Foot nebula

11. Xray ionized nebula in Holmberg II From Laurent Mirioni’s thesis; nebula is density-bound (optically thin) beyond heel Chandra position coincident with He III region confirmed by Kaaret et al 04

12. [OIV] 25.9  emission in Holmberg II X-1 Spitzer observations: Berghea et al 2009 note: IP (O++) ~ IP(He+) ~ 54 eV

13. Orocz et al 2007: 70 Mo OB + 16 Mo BH in dense HII B208f: XIN M33 X-7 Strasbourg students Maggi, Morgan and Master student Xian Hua: Measure XUV (0.054 – ~0.1 KeV) emission of well-behaved BH X-ray binary using CLOUDY modeling; PL and TB wrong ! 4686

14. NGC 5408 HeII 4686 Nebula: Pakull & Mirioni 2003 Spectra: Kaaret et al 2009: XIN! 4686: Nebular & STELLAR H 

15. Feedback II. Shocks by wind/jets

16. ULX IC 342 X-1 "Tooth" nebula situated in spiral arm has a diameter of 220pc Pakull & Mirioni 2002; Roberts et al 2003; SNR-like spectrum: [SII]/H  =1.2 [OI] 6300/ H  =0.4 shock (or X-ray) ionization Detection of supersonic expansion (see later) Roberts et al 2003 INTEGRAL field spectrograph: [OIII]-contours Cont 5000 H  [OIII]-contours

17. ULXB NGC 1313 X-2 H  VLT * bubble diameter ~ 26’’ = 400 pc (!) ‏

18. The ‘SNR’ MH9-11 in HolmbergIX Holmberg IX X-1: Lx ~10 40 erg/s Miller (1995): X-ray superluminous SNR; but X-ray variable point source! Note small cluster incl. ULX counterpart; SE: shock breakout (?) SE Subaru B Ha [OIII] B 30 " = 500 pc

19. ULX (Swartz, Soria, in prep)‏ 30 pc HST/ACS - brightest ‘SNR’ (10 39 erg/s) ‏ - ‘colliding SNRs’ (Blair & Fesen 94, BF & Schlegel 01) ‏ - X-ray variable  ULX (Roberts & Colbert 03, poster Fengyun Rao !) ‏ - v ex =225 km/s; t ~3 10 4 yrs; (Dunne et al. 00) ‏ The youth of the bubble excludes nature as a remnant of SN explosion that created compact accreting star in ULX [after SN explosion nuclear timescale expansion of donor star before Roche lobe overflow mass transfer can take place] NGC 6946 MF16 no HNR !

20. Kinematics of ULX bubbles Holm IXNGC1313 X-2 IC 342 X-1 Holm II HH [NII] 6584 V exp = 80 – 250 km/s >> 20 km/s (T~10 4 K thermal v) ‏

21. Energetics of ULX Bubbles Bubble radii up to ~200 pc (ie. >> SNR) Expansion velocity ~ 80 – 250 km/s if due to SN explosion; Sedov /snowplow : E 0 ~ 2 10 52 erg R 100 3 v 100 2 n ; t ~ 1 10 6 yrs, E 0 ~ 5 10 53 erg n (shock H  luminosity: I  ~ v exp 2.3 n --> n = 0.1-1.0 cm -3 ) ‏  HNR nature of ULXB unlikely if wind/jet driven bubble (Castor 1975, Weaver et al 1977): Lw ~ 5 10 39 erg/s R 100 2 v 100 3 n t ~ 1 10 6 yrs (3 10 4 yr for NGC6946X-1); Lw ~ 10 39-40 erg/s for all ULXB Lw = ½ Mdot v out 2 ~ jet mechanical luminosity of SS433; i.e. v out should be mildly relativistic (~ 0.3 c) ‏

22. Interstellar Bubble Castor, McCray, Weaver 1975, Weaver et al. 1977 E_therm = 5/11 L w t E_kin = 15/77 L w t E_rad = 27/77 L w t  E_i = 77/77 L w t (from Chu, 2009)‏ + non- thermal particles 10 7 - 10 8 K

23. Problem: strong winds or large- scale jets not readily seen in ULXB

24. Estimate: >~ 25 % ULX blow bubbles If ULX photon emission strongly beamed, than there should be many ULXB with ULXs that are beamed away from us Are there unrecognized ULXB from active, presently inactive, or misaligned ULXs ? Search for point-like XRS among large SNRs candidates

25. Optical [SII]/H  > 0.4 selected surveys of SNRs in large nearby galaxies (outside LG) Matonick & Fesen 1997: N5204, N5585, N6946, M81, M101; N2403 Blair & Long 1997: N300, N7793 HH [SII] [SII]-H 

26. some very large SNR candidates… Lozinskaya & Moiseev 2007 Log  - logD for SNR S1-N5585 10 100 300 pc IC 10: Bubble around XRB WR + 30 Mo BH (LM 2007)‏ NGC 5585 S1: new ULX (Pakull & Grisé 2008)‏

27. very large SNR in NGC 5585 Matonick & Fesen (1997) noted huge (200x300) pc ‘SNR’ in NGC 5585 5.0 300 pc

28. very large ‘SNR’ is ULXB ! 5.0 Matonick & Fesen (1997) noted huge (200x300) pc ‘SNR’ in NGC 5585 300 pc Chandra: point source (~ 5 10 39 erg/s) ‏ as in many previously identified ‘SNRs’ Ho IX, NGC 6946X-1; M81X-6 …

29.  QSO SS433 & W50 mechanically inflated Bubble W50 with ‘ears’ due to v=0.26c jets (+SNR ?) radio-image 200 pc ASCA image (Kotani 98) ‏ Begelman’s ‘beambags’ i.e. linear triple

30. ss433film VLBA; credit: NRAO/AUI/NSF

31. Problem: no large-scale jets readily seen in ULXB (or other  QSO)

32. …but non-thermal radio emission around some ULX Hol II X-1 again L R ~ Cas A extended emission i.e. not  QSO-like ~ only 1% of P J in SS433 is enough to power radio lobes (very small fraction of P J go into relativistic electrons and B fields Neal Miller, Mushotzky, Neff 2005 HeII 4686

33. some very large SNR candidates… NGC 7793 S26 Log  - logD for SNR S1-N5585 10 100 300 pc

34. S26 = optical/Xray = P8 0.2-8 keV0.2-1 keV 250pc N7793: Chandra archive; 50 ks; PI: Pannuti X + Ha S26: Blair & Long 1997 P8: Read and Pietsch 1999

35. 0.3- 1.0 keV 1.0 - 2.0 keV 2.0 – 8.0 keV

36. Pakull, Soria & Motch, Nature in press H  contours from CTIO L x ~ 5E36 erg/s L x ~ 7E36 erg/s L x ~ 1.1E37 erg/s  ~ 1.5 kT ~ 0.3-0.8 keV

37. S26 and FR II radio galaxies Soria et al 2009; 2010 submitted ATCA 9.02 GHz 1000 : 1

38. compare with FRII CygA Cyg A: Chandra high S/N NGC 7793 S26: Chandra 50ks

39. compare with FRII CygA Cyg A: Chandra low S/N NGC7793-S26: Chandra 50ks

40. Radio galaxy basic model Heinz 2000, Thesis AGN: hot T~10 7-8 K cluster gas weak cocoon shock S26: warm 10 3-4 K ISM: strong cocoon shock

41. S26 in HeII 4686 emission -> v ~ 275 km/s S26 in HeII 4686 emission -> v s ~ 275 km/s opt. counterpart of central souce: Mv~-5 (WR) star

42. but finally...

43. V ~ V ~ 250 km/s V exp ~ V s ~ 250 km/s ESO VLT Oct. 2009

44. S26/P8 summary Pakull, Soria & Motch 2010, Nature in press Morphology : FRII radio galaxy: radio and X-ray lobes, hot spots + optical lobes  inflation of the lobes by a jet (power P J ) ‏ Size: 300 x 150 pc, i.e. typical ULXB Supersonic expansion with 250 km/s (!); consistent with shock-excited 4686 emission M V ~ -5 (WR) optical counterpart Age = 2/5 R/v ~ 2 10 5 yrs E(rel. electrons) << E(thermal), E(kin) ‏ P J ~ 5 10 40 erg/s (>> Lx ~ 2 10 37 erg/s) ‏ Similar to, but much more powerful than SS433/W50

45. Heinz 2002 Heinz & Sunyaev, 2003  QSO and ULX

46. Thank you