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Ultraluminous X-ray Sources Counterparts & Bubbles

: . Ultraluminous X-ray Sources Counterparts & Bubbles . Manfred Pakull, Fabien Grisé 0bservatoire Astronomique de Strasbourg coll: C. Motch, R. Soria, I. Smith, A. Kubota, T. Tsuru. X-rays from Nearby Galaxies, ESAC Sept 5-7, 2007. ULX Bubbles. LMC X-1 / N159F . Only bright XRB that

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Ultraluminous X-ray Sources Counterparts & Bubbles

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  1. : Ultraluminous X-ray Sources Counterparts & Bubbles Manfred Pakull, Fabien Grisé 0bservatoire Astronomique de Strasbourg coll: C. Motch, R. Soria, I. Smith, A. Kubota, T. Tsuru... X-rays from Nearby Galaxies, ESAC Sept 5-7, 2007

  2. ULX Bubbles

  3. LMC X-1 / N159F Only bright XRB that was known to be located in HII region Discovery of first X-ray ionized nebula XIN (HeIII region) Pakull&Angebault 1986

  4. SS433 & Cyg X-1 Mechanically inflated bubbles due to XRB jets (or SNR ?) (radio-images) ! note different scale ! Gallo et al 2005 6 pc

  5. ULX IC 342 X-1 • "Tooth" nebula situated in spiral arm has a diameter of 220pc (Pakull & Mirioni 2002; Roberts et al 2003; Grisé et al 2006 • SNR-like spectrum: [SII]/H=1.2 [OI]6300/ H=0.4 • X-ray or shock ionization ? • Detection of supersonic expansion (see later) from Laurent Mirioni’s thesis

  6. ULX in Holmberg IX (M81 X-9) • Discovered by Miller 1995: very lum. SNR • But variable compact source • diameter = 250 pc, away from young star-burst region • Contrary to claim by Miller H/H is normal, [OI]6300/H=0.2 • Blue star/group near X-ray position (see later)

  7. ULX NGC 1313 X-2 Previously candidate for galactic neutron star ! location far away (9kpc) from nucleus of N1313 no nearby starburst diameter 400 pc Laurent Mirioni’s thesis

  8. What powers ULX Bubbles ? 1- Photoionized by ULX (or companion star or cluster) ?  XUV luminosity of the source 2a - SNR (HNR) of star that created ULX ? 2b - inflated by wind/jet from ULX (or superbubble inflated by cluster) ?  age, explosion energy Eo, or wind/jet luminosity

  9. X-ray photoionization

  10. Strömgren spheres around O stars Even hottest massive stars (O2,3 V) do not emit substantial He+ Ly cont (hn > 54 eV) i.e., no He++ ions • no nebular HeIIl4686 emission very thin skin of ‘warm’ OI atoms i.e., [OI]l6300/Ha < 0.03

  11. X-ray ionized nebula Halpern & Grindlay 1980 no sharp Stroemgren spheres; ‘warm’ He++ zone:  HeIIl4686 emission ‘warm’ neutrals  strong [OI] , [SII]

  12. Holmberg II X-1: 2nd XIN nebular HeII l4686 emission at the position of the ULX (Pakull & Mirioni 2002) ‘Heel’ of Foot nebula

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

  14. Holmberg II X-1 seen by HST High-resolution imaging with ACS camera on HST by Kaaret et al 2004: Confirmation of nebular morphology (ionisation structure); Counterpart: V=21.9, Mv ~ -5.6

  15. HeII4686 X-ray photon counting X-ray photoionization models (CLOUDY) show good agreement with Zanstra photon counting for l4686 flux; i.e. LHeII4686  LX if the nebula indeed “sees” the total isotropic X-ray luminosity, i.e. LX ~ 1040erg/s no, or only little, X-ray beaming

  16. Shock ionization

  17. A few elements of shock physics Adiabatic, non-radiative shock ( no B field) n1 = 4 n0; v1= 3/4 vs ; P1 = 3/4r0 vs2; T1 ~ 105 K v1002 Isothermal, fully radiative shock (no B field) n2 = M2 n0; v2 = vs; P2 = r0 vs2; T2=T0 Precursor Dopita & Sutherland 95: vs = 400 km/s

  18. A few elements of shock physics Adiabatic, non-radiative shock ( no B field) n1 = 4 n0; v1= 3/4 vs ; P1 = 3/4r0 vs2; T1 ~ 105 K v1002 Isothermal, fully radiative shock (no B field) n2 = M2 n0; v2 = vs; P2 = r0 vs2; T2=T0 Precursor Dopita & Sutherland 95 vs = 400 km/s [0I] 6300

  19. A few elements of shock physics Adiabatic, non-radiative shock ( no B field) n1 = 4 n0; v1= 3/4 vs ; P1 = 3/4r0 vs2; T1 ~ 105 K v1002 Isothermal, fully radiative shock (no B field) n2 = M2 n0; v2 = vs; P2 = r0 vs2; T2=T0 For fully radiative shocks a certain fraction of the dissipated energy (‘shock luminosity’ [erg/cm2/s]) L = ½ r vs3 is radiated as H recombination radiation, i.e., Lb (~0.003 x L) Lb = 7.4x10-6 v22.4 n0 erg/cm2/s

  20. Shock diagnostics 1 10 3 1 .3 5007/b [OIII]l5007/Hb ratio as function of schock vel. vs (Dopita et al 1984)

  21. Shock diagnostics 2: uncomplete shocks Raymond at al. 1988 Distance from shock Distance from shock 100 10 1 0.1 1.0 0.0 OIIIl5007/ Hb • high • [OIII]l5007/ Hb • ratios (>6) • uncomplete shocks (not XIN !) high [OI]l6300/ Hb ratios (>0.1)  complete shocks OIIIl5007 Hb OIl6300/Hb

  22. Holmberg IX X-1 Nebula Subaru Ha[OIII]B 30 " = 500 pc SE shock ionized nebula; breakout towards SE with incomplete shocks

  23. ULX IC 342 X-1 Subaru observations (Grisé et al) Roberts et al, MNRAS (2003) INTEGRAL field spectrograph: Contl5000 Ha [OIII]-contours - ‘high-ionization’ cones are not confirmed - l5007/ Ha varies as function of vs and of completeness ! - i.e., no indication of non-isotropic X-ray emission

  24. Holm IX NGC1313 X-2 H [NII] 6584 IC 342 X-1 Holm II Kinematics of ULX Nebulae Vexp = 80 – 150 km/s

  25. E W Pakull & Mirioni 2002 NGC1313-X2 nebula • Size ~ 570 x 400 pc • V ~ 100 km/s • n ~ 0.2 cm-3 • E ~ 1.0 x 1053 erg courtesy D. Wang see Ramsey et al 2006

  26. Photo- or shock- ionization ? (with kind regards from the AGN/Liner community) NGC 6946 X-1/MF16, a compact bubble with strong HeII 4686 emission that cannot easily be explained as XIN; i.e., Lx(observed) appears much too low; Abolmasov et al. 2006 NGC 1313 X-1: high [OI]6300/Ha ratio in nebular neighbourhood (Pakull&Mirioni 2002) NGC 4485/90: new IR spectral diagnostic proposed by Vazquez et al 2007

  27. Spitzer IR diagnostics for six ULXs in NGC 4485/90 Vazquez et al 2007 IR diagnostic diagram: regions around 5/6 ULX appear to have higher ionization than normal HII regions; i.e. AGN-like

  28. Energetics of ULX Bubbles Sedov –Taylor (SNR kin Energy E0, adiabatic) • R ~ 12.8 pc (E51/n )1/5 t42/5 • V ~ 500 km/s (E51/n )1/5 t4-3/5 • t ~ 6 105 yrs R100/V100 • E0 ~ 2 1052 erg R1003 V1002 n Wind/jet fed bubble (mech. luminosity LW ) • R ~ 26.2 pc (L36/n )1/5 t43/5 • V ~ 15.4 km/s (L36/n )1/5 t4-2/5 • t ~ 4 105 yrs R100/V100 • LW ~ 4 1039 erg/s R1002 V1003n density n from Ib = 7.4x10-6 v22.4n erg/s/cm2

  29. Energetics of ULX Bubbles: SNR Direct application of previous relations yields: t ~ 106yrs (robust); n ~ 0.3 – 10 cm-3 (from Ha intensity) E0~1053 erg • ~100 SNRs in 106yrs (excluded !), or hypernova ( that created ULX) ?

  30. Supernovae – Hypernovae Nomoto et al. 2003

  31. Energetics of ULX Bubbles winds/jets Direct application of previous relations yields: t ~ 106yrs (robust); E0~1053 erg • ~100 SNRs in 106yrs (excluded !), or hypernova (->ULX?) or wind/jet fed :  LW ~ few 1039 erg/s; Mdot<10-6Msol /yr; • vW,j ~few 0.1 c (mildly relativistic jet velocity); but unlike SS433, jets are not directly observed !

  32. Energetics of ULX Bubbles Direct application of previous relations yields: t ~ 106yrs (robust); E0~1053 erg • ~100 SNRs in 106yrs (excluded !), hypernova (->ULX?) or • LJ~few 1039 erg/s; Mdot<10-6Msol /yr; i.e., we predict vJ ~ few 0.1 c, probably dark jets However: • much smaller IS density (n~0.01 like in excavated wind-driven superbubbles) would lessen E0. and LJ. • vs(optical) not necessarily = vexp of blastwave (X-ray); remember that IS medium is cloudy, like in real SNR

  33. ULX Bubbles: possible Misconceptions & Promises • High [OIII]5007/Hb ratio does not necessarily imply (beamed) X-ray ionization • filamantary HII regions don’t necessarily imply jets • If most ULXs do create (wind/jet driven) bubbles: then presently inactive ULX and hypothetical beamed ULX pointed away from us should still be optically visible by their bubbles ; • conversely, lack of many large shocked nebulae implies that ULX emission is NOT beamed

  34. NGC 1313 X-2 NGC 1313 field H H Inactive ULX bubbles ? If most ULX blow energetic bubbles, than there should exist bubbles that were created by presently inactive ULX, or by beamed ULX that do not point towards us. Search for such objects has revealed only few candidates  little beaming, certainly W/4p > 1/10 !

  35. . ULX Optical Counterparts c.f. talk by Fabien Grisé Optical data have suggested O star optical counterparts  MXRB; holy grail: observe RV curve to derive masses and decide between stellar BHB vs. IMBHs models

  36. HeII4686 Holmberg IX X-1 counterpart Brightest object in cluster has stellar HeII l4686 emission

  37. HeII 4686 NGC 1313 X-2 cluster Pakull et al. 2005: it is the blue component C1 of double C (Zampieri 2004,06 07)

  38. HeII 4686 HeII 4686 Stellar4686 emission from ULX Upper: SUBARU spectrum of the 22.8 mag optical counter- part of Hol IX X-1. The stellar 4686 has EW = 9A Lower: ESO-VLT spectrum of 23.4 mag NGC 1313 X-2. Stellar 4686 EW = 10 A. ULX counterparts resemble very luminous (Mv ~ -5) LMXB, i.e. X-ray heated accretion disks(not SS433-like: there EWs several 100 A !!) Hol IX nebular NGC 1313 X-2 nebular

  39. ULX optical counterparts: LMXB – like accretion disks ULXs 1313X-2, HoIX Van Paradijs & McClintock 1994: X-ray heated disks: Lv ~ Lx1/2 a ~ Lx1/2 Porb2/3 M1/3 ~ S HeII l4686 luminosity ~ LX Æhigh intrinsic Lx, no beaming at work here

  40. RV variation in NGC1313 X-2 (?) dotted line corresponds to RV of HI gas near XRS HeII 4686: RV = 300 km/s in 20 d if confirmed  Mx < 50 M (i.e., not IMBH !)

  41. What have we learnt ? fancies • ULX are IMBH ! …less and less likely • ULX are Blazars ! no: largely isotropic emitters • ULX are thermal-  (short) phases of binary evolution ! no: stable nuclear-  transfer • Counterparts are O stars ! no: probably accretion disks

  42. What have we learnt ? facts • A significant fraction of ULX have nebulae, but there are not many X-ray inactive “ULX bubbles”. • Some ULX photoionize nebulae allowing (via HeII4686 photon counting) to estimate total Lx and thus possibly excluding beaming (Hol II, MF16). • Extent and supersonic expansion velocity of ULX bubbles allows to measure energetics (>20 x ESNR)  clues to their formation or recent (relativistic) mass-loss history; lifetime > 1 Myr • Direct measurements of ULX mass (via RV curve of accretion disk HeII4686 emission) appears now feasible (but very hard to realize !)

  43. FIN

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