Jet inflated bubbles: facts (and fiction) Manfred W. Pakull, Observatoire de Strasbourg coll. Roberto Soria, Christian Motch, and others HEPROIII, Barcelona, June 27-July 1, 2011 S26 in NGC 7793: Chandra/ESO press release

Outline -- bubble nebulae around Ultraluminous X-ray sources -- microquasars and interaction with IS medium -- Rosetta Stone S26 in NGC 7793: micro FRII-type source with reliably measured jet power

Ultraluminous X-ray sources (ULX) X-2 NGC 1313 Lx > erg/s = Ledd (20 Mo) Various hypotheses (XRB) super-Eddington beamed emission IMBH ( Mo) I will show: ULX also emit winds/jets with L mech ~ L x

NGC 1313 X-2 H  VLT * bubble diameter ~ 26’’ = 400 pc (!) ‏ Optical spectra: shock ionised Vs ~ 100 km/s Pakull & Mirioni 2002, Pakull et al. 2006

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 ? see poster of D. Cseh from Laurent Mirioni’s thesis CFHT, H 

The ‘SNR’ around HolmbergIX X-1 Holmberg IX X-1 = M81 X-9: Lx ~10 40 erg/s; Grisé et al 2011 Miller (1995): X-ray superluminous SNR; but X-ray variable point source! SE: shock breakout (?) SE Subaru B Ha [OIII] B 30 " = 500 pc

Estimate: >~ 25 % ULX blow observable bubbles If ULX photon emission strongly beamed, than there should be many ULXB with ULXs that are beamed away from us, are presently inactive or have not yet been discovered (200x300) pc ‘SNR’ #1 in NGC 5585 (Matonick & Fesen 1997) is optically selected ULX ! Chandra ULX !

Kinematics of ULX bubbles Holm IXNGC1313 X-2 IC 342 X-1 Holm II HH [NII] 6584 V exp = 80 – 150 km/s >> 10 km/s (c s for T~10 4 K) ‏ NS

Energetics of ULX Bubbles Bubble radii R ~200 pc (i.e. >> SNR) Expansion velocity vs ~ 80 – 150 km/s IS densities n ~ cm -3 wind/jet driven bubble with power Lw (Weaver et al 1977) R = 0.76 (L w /  ) 1/5 t 3/5 ; t = 3/5 R/v L w = erg/s R x v x n fully radiative shock with v s implies for total radiative lumisosity & H  Luminosity L rad = 27/77 x L w ; L  = f(v s ) x L w t~10 6 yrs; Lw~ erg/s ~ Lx (ULX) ; E o ~10 53 erg/s (SS433/W50 - like; Pakull & Mirioni 2002; Pakull & Grisé 2006)

Galactic  QSO: Cyg X-1 Russell et al pc Gallo et al. 2005: thermal radio emission [OIII]: P J ~ 4 x10 36 – erg/s P J ~ 30 – 100 % L bol; compact source too radio faint:. ‘’dark’’ outflow 100x smaller than W50 ~100x weaker jet

 QSO SS433 & W50 mechanically inflated Bubble W50 (SNR??) with ‘ears’ due to v = 0.26c jets L mech = L J ~ erg/s 200 pc ASCA image (Kotani 1998) ‏ Begelman’s ‘beambags’ i.e. linear triple XRS radio-image SS433 seen from far away…

Discovery of a 2nd S433/W50- type object Pakull & Grisé 2008 in “Population explosion” Pakull, Soria, Motch 2010 Nature Soria, Pakull, et al 2020 MNRAS after ~ 30 years of effort from many people…

“SNR” S26 in NGC 7793 (d=3.9 Mpc) S26: Blair & Long 1997; faint ROSAT source: Read & Pietsch pc HRHR

“SNR” S26 in NGC 7793 = triple XRS Chandra archive; 50 ks; PI: Pannuti X-ray

keV keV 2.0 – 8.0 keV Contours: H 

Pakull, Soria & Motch, 2010 Nature L x ~ 5E36 erg/s L x ~ 7E36 erg/s L x ~ 1.1E37 erg/s  ~ 1.5 kT ~ keV Mx ~ few 100 Mo

S26: V exp ~ V s ~ 250 km/s >> c s ESO VLT long-slit spectro HST H  (Soria et al. in prep) night-sky 23 mag counterpart Optical spectra: shocks Optical spectra: complete shocks  fully radiative bubble with R~100 pc, v ~ 250 km/s  fully radiative bubble with R~100 pc, v s ~ 250 km/s t = 2 10 yrs; t = yrs; L J = 5 x erg/s (>> Lx)

+ 9 GHz radio contours  = 0.7; opt. thin syn. S26: X-ray/ radio image X-ray Hot Spots lead radio HS

S26 and FR II radio galaxies similar morphologyities Soria et al MNRAS ATCA 9 GHz 1 : 1000 O – X-ray sources

S26 and FR II radio galaxies important difference S26: highly supersonic expansion of cocoon into ISM i.e. M >> 1  radiative shock radio galaxies: M~1 expansion into hot (kT ~ keV) IGM  pdV work (4pV cavity enthalpy) warm ISMhot IGM: cluster gas

Assume magnetic field ~ in equipartition with relativistic energy density In hot spots, In hot spots, jet energy transferred to: relativistic electrons (~ 1—1E5): = 1 radiating relativistic electrons (  ~ 1—1E5): = 1 radiating relativistic protons and He nuclei : = k non-radiating relativistic protons and He nuclei : = k non-radiating B/ 8 B 2 / 8  thermal gas radiating thermal gas radiating    = E (rel + B) / E(total) (<< 1)    = E (rel + B) / E(total) (<< 1) Calculate synchrotron emission and radio flux density from P, n, t Calculate synchrotron emission and radio flux density from P J, n, t  only a fraction { } = of the jet power is. transferred to relativistic electrons  only a fraction { } = a few E(-3) of the jet power is. transferred to relativistic electrons What about the radio lobes of S26? Compare with observed radio flux density predicted:  predicted: S = 1020 {  1.85 /(1+k)} mJy 5 –0.7 (see also Heinz 2002, Bordas et al 2009) (see also Heinz 2002, Bordas et al 2009) S26 radio flux S = 2.1 mJy 5 –0.7 ; 5 =  5 GHz

S26 and radio galaxies Calibration of { } = f (k,  is long-standing problem, also for AGN (eg, Willott et al 1999) S26 is a rare object with direct estimates of both proxies S26

Cavagnolo et al (2010): relation between radio lobe luminosity P(1.4GHz) and power injected into the bubble, for a sample of AGN Power into relativistic electrons ~ (1/100) of the total jet power S26 { } =1

Conclusions ULX bubbles indicate mechanical power ~ 1E39 - 1E40 erg/s ~ Lx t ~ 1E6 yrs ; Etot ~ 1E53 erg t ~ 1E6 yrs ; Etot ~ 1E53 erg (Beware of fake jets/shocks) S26 in NGC 7793: super-SS433/W50 system with hot spots (->jets) Largest and most powerful microquasar system (160 x 290 pc) Linear size ~ 2.5 x SS433 Linear size ~ 2.5 x SS433 Radio luminosity ~ 3 x Cas A Radio luminosity ~ 3 x Cas A Jet power ~ a few E 40 erg/s (>> Ledd of accr. BH.) Much of the jet power used to inflate fully radiative bubble, (L = 27/77 L); only ~ 1% goes into synchrot-emitting electrons (L rad = 27/77 L Jet ); only ~ 1% goes into synchrot-emitting electrons Rare example of kinetically-dominated high state BH in the local universe; analogy with recently discovered/advocated (Punsly 2007, 08, 11) sample of kinetically dominated quasars ?

Thank you